Ranzani 1, 40127, Bologna, Italy.), AG(Astronomy
Department, University of Virginia, Charlottesville,
VA 22903.), AH(INAF, Osservatorio Astronomico di
Roma, Via Frascati 33, I-00040, Monteporzio,
Italy.), AI(INAF, Osservatorio Astronomico di
Padova, Vicolo dell'Osservatorio, 5, I-35122 Padova,
Italy.), AJ(INAF, Osservatorio Astronomico di Roma,
Via Frascati 33, I-00040, Monteporzio, Italy.),
AK(INAF, Osservatorio Astronomico di Padova, Vicolo
dell'Osservatorio, 5, I-35122 Padova, Italy.),
AL(Max-Planck-Institut für extraterrestrische Physik
(MPE), Giessenbachstrasse 1, 85748 Garching,
Germany.), AM(Max-Planck-Institut für
extraterrestrische Physik (MPE), Giessenbachstrasse
1, 85748 Garching, Germany.), AN(INAF, Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040,
Monteporzio, Italy.), AO(INAF-Osservatorio
Astronomico di Bologna, via Ranzani 1, 40127,
Bologna, Italy.), AP(INAF, Osservatorio Astronomico
di Roma, Via Frascati 33, I-00040, Monteporzio,
Italy.), AQ(INAF, Osservatorio Astronomico di
Padova, Vicolo dell'Osservatorio, 5, I-35122 Padova,
Italy.), AR(INAF, Osservatorio Astronomico di Roma,
Via Frascati 33, I-00040, Monteporzio, Italy.),
AS(INAF, Osservatorio Astronomico di Roma, Via
Frascati 33, I-00040, Monteporzio, Italy.), AT(INAF,
Osservatorio Astronomico di Trieste, Via G. B.
Tiepolo 11, I-34131 Trieste, Italy.), AU(INAF,
Osservatorio Astronomico di Padova, Vicolo
dell'Osservatorio, 5, I-35122 Padova, Italy.),
AV(INAF, Osservatorio Astronomico di Trieste, Via G.
B. Tiepolo 11, I-34131 Trieste, Italy.), AW(INAF,
Osservatorio Astronomico di Roma, Via Frascati 33,
I-00040, Monteporzio, Italy.), AX(INAF, Osservatorio
Astronomico di Trieste, Via G. B. Tiepolo 11,
I-34131 Trieste, Italy.), AY(INAF, Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040,
Monteporzio, Italy.), AZ(INAF, Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040,
Monteporzio, Italy.), BA(INAF, Osservatorio
Astronomico di Arcetri, Largo E. Fermi 5, I-50125,
Firenze, Italy.)
Publication: The Astrophysical Journal, Volume 679, Issue 1, pp.
712-719. (ApJ Homepage)
Publication Date: 05/2008
Origin: UCP
ApJ Keywords: Stars: Blue Stragglers, galaxies: clusters:
individual (M53), Galaxy: Globular Clusters:
General, Stars: Evolution
Abstract Copyright: (c) 2008: The American Astronomical Society
DOI: 10.1086/587689
Bibliographic Code: 2008ApJ...679..712B
Abstract
We used a proper combination of high-resolution and wide-field
multiwavelength observations collected at three different telescopes
(HST, LBT, and CFHT) to probe the blue straggler star (BSS) population
in the globular cluster M53. Almost 200 BSSs have been identified over
the entire cluster extension. The radial distribution of these stars has
been found to be bimodal (similar to that of several other clusters)
with a prominent dip at ~60" (~2rc) from the cluster center.
This value turns out to be a factor of 2 smaller than the radius of
avoidance (ravoid, the radius within which all the stars of
~1.2 Msolar have sunk to the core because of dynamical
friction effects in a Hubble time). While in most of the clusters with a
bimodal BSS radial distribution, ravoid has been found to be
located in the region of the observed minimum, this is the second case
(after NGC 6388) where this discrepancy is noted. This evidence suggests
that in a few clusters the dynamical friction seems to be somehow less
efficient than expected. We have also used this database to construct
the radial star density profile of the cluster; this is the most
extended and accurate radial profile ever published for this cluster,
including detailed star counts in the very inner region. The star
density profile is reproduced by a standard King Model with an extended
core (~25") and a modest value of the concentration parameter (c=1.58).
A deviation from the model is noted in the most external region of the
cluster (at r>6.5' from the center). This feature needs to
be further investigated in order to address the possible presence of a
tidal tail in this cluster.
Based on observations with MegaPrime/MegaCam, a joint project of CFHT
and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is
operated by the National Research Council (NRC) of Canada, the Institute
National des Sciences de l'Univers of the Centre National de la
Recherche Scientifique of France, and the University of Hawaii. Based on
observations with the NASA/ESA HST, obtained at the Space Telescope
Science Institute, which is operated by AURA, Inc., under NASA contract
NAS5-26555. Also based on data acquired using the Large Binocular
Telescope (LBT). The LBT is an international collaboration among
institutions in the United States, Italy, and Germany. LBT Corporation
partners are The University of Arizona on behalf of the Arizona
university system; Istituto Nazionale di Astrofisica, Italy; LBT
Beteiligungsgesellschaft, Germany, representing the Max-Planck Society,
the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio
State University; and The Research Corporation, on behalf of The
University of Notre Dame, University of Minnesota and University of
Virginia. This research used the facilities of the Canadian Astronomy
Data Centre operated by the National Research Council of Canada with the
support of the Canadian Space Agency.
Title: The Spitzer MIPSGAL Asteroid Survey
Authors: Ryan, Erin L.; Carey, S.; Mizuno, D.;
Woodward, C.; MIPSGAL Science Team
Affiliation: AA(Univ. of Minnesota), AB(Spitzer Science Center),
AC(Boston College), AD(Univ. of Minnesota), AE()
Publication: American Astronomical Society, AAS Meeting #212,
#4.04
Publication Date: 05/2008
Origin: AAS
Abstract Copyright: (c) 2008: American Astronomical Society
Bibliographic Code: 2008AAS...212.0404R
Abstract
We present the first asteroid results from the Spitzer MIPSGAL Legacy
program. This program represents the first mid-infrared data set which
samples the ecliptic plane to
a consistent depth of 1 mJy at 24 micron for ecliptic latitudes of -0.7
to 14.2 degrees.
Our results include asteroid number counts as a function of ecliptic
latitude (ranging from 40 asteroids per square degree at 0 degrees
latitude to 10 asteroids per square degree at 15 degrees latitude) and
diameter/albedo determinations for all known asteroids in the field
(approximately 650). The asteroid number counts will also be compared to
other programs by the authors, including an optical survey with the LBT
and mid-infrared observations from the Spitzer IRAC instrument.
This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory (JPL),
California Institute of Technology under
a contract with NASA. Support for this work was provided by NASA in part
through an award issued by JPL/Caltech.
Title: The performance of the blue prime focus large
binocular camera at the large binocular telescope
Authors: Giallongo, E.; Ragazzoni, R.; Grazian, A.;
Baruffolo, A.; Beccari, G.; de Santis, C.;
Diolaiti, E.; di Paola, A.; Farinato, J.;
Fontana, A.; Gallozzi, S.; Gasparo, F.;
Gentile, G.; Green, R.; Hill, J.; Kuhn, O.;
Pasian, F.; Pedichini, F.; Radovich, M.;
Salinari, P.; Smareglia, R.; Speziali, R.;
Testa, V.; Thompson, D.; Vernet, E.; Wagner, R. M.
Affiliation: AA(INAF - Osservatorio Astronomico di Roma, via
Frascati 33, 00040 Monteporzio, Italy
), AB(INAF - Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy), AC(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AD(INAF - Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy), AE(INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AF(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AG(INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AH(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AI(INAF - Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy), AJ(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AK(INAF -!
Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AL(INAF - Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34131 Trieste, Italy), AM(INAF - Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy), AN(Large Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721-0065, USA), AO(Large Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721-0065, USA), AP(Large Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721-0065, USA), AQ(INAF - Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34131 Trieste, Italy), AR(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AS(INAF - Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy), AT(INAF - Osservatorio Astronomico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy), AU(INAF - Osservato!
rio Astronomico di Trieste, via G. B. Tiepolo 11, 34131 Triest!
e, Italy
), AV(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AW(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy), AX(Large Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721-0065, USA), AY(INAF - Osservatorio Astronomico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy ; European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany), AZ(Large Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721-0065, USA)
Publication: Astronomy and Astrophysics, Volume 482, Issue 1,
2008, pp.349-357 (A&A Homepage)
Publication Date: 04/2008
Origin: EDP
Keywords: instrumentation: detectors, methods: data analysis,
techniques: image processing, surveys, galaxies:
photometry
DOI: 10.1051/0004-6361:20078402
Bibliographic Code: 2008A&A...482..349G
Abstract
Aims. We present the characteristics and some early scientific results
of the first instrument at the Large Binocular Telescope (LBT), the
Large Binocular Camera (LBC). Each LBT telescope unit will be equipped
with similar prime focus cameras. The blue channel is optimized for
imaging in the UV-B bands and the red channel for imaging in the VRIz
bands. The corrected field-of-view of each camera is approximately 30
arcmin in diameter, and the chip area is equivalent to a 23×23
arcmin2 field. In this paper we also present the
commissioning results of the blue channel. Methods: The scientific and
technical performance of the blue channel was assessed by measurement of
the astrometric distortion, flat fielding, ghosts, and photometric
calibrations. These measurements were then used as input to a data
reduction pipeline applied to science commissioning data. Results: The
measurements completed during commissioning show that the technical
performance of the blue channel is in agreement with original
expectations. Since the red camera is very similar to the blue one we
expect similar performance from the commissioning that will be performed
in the following months in binocular configuration. Using deep UV image,
acquired during the commissioning of the blue camera, we derived faint
UV galaxy-counts in a ~ 500 sq. arcmin sky area to U(Vega) = 26.5. These
galaxy counts imply that the blue camera is the most powerful UV imager
presently available and in the near future in terms of depth and extent
of the field-of-view. We emphasize the potential of the blue camera to
increase the robustness of the UGR multicolour selection of Lyman break
galaxies at redshift z ~ 3.
Title: Discovery of the Dust-Enshrouded Progenitor of SN
2008S with Spitzer
Authors: Prieto, J. L.; Kistler, M. D.; Thompson, T. A.;
Yuksel, H.; Kochanek, C. S.; Stanek, K. Z.;
Beacom, J. F.; Martini, P.; Pasquali, A.;
Bechtold, J.
Publication: eprint arXiv:0803.0324
Publication Date: 03/2008
Origin: ARXIV
Keywords: Astrophysics
Comment: ApJ letters, in press; corrected a typo
Bibliographic Code: 2008arXiv0803.0324P
Abstract
We report the discovery of the progenitor of the recent type IIn SN
2008S in the nearby galaxy NGC 6946. Surprisingly, it was not found in
deep, pre-explosion optical images of its host galaxy taken with the
Large Binocular Telescope, but only through examination of archival
Spitzer mid-IR data. A source coincident with the SN 2008S position is
clearly detected in the 4.5, 5.8, and 8.0 micron IRAC bands, showing no
evident variability in the three years prior to the explosion, yet is
undetected at 3.6 and 24 micron. The distinct presence of ~440 K dust,
along with stringent LBT limits on the optical fluxes, suggests that the
progenitor of SN 2008S was engulfed in a shroud of its own dust. The
inferred luminosity of 3.5x10^4 Lsun implies a modest mass of ~10 Msun.
We conclude that objects like SN 2008S are not exclusively associated
with the deaths or outbursts of very massive eta Carinae-like objects.
This conclusion holds based solely on the optical flux limits even if
our identification of the progenitor with the mid-IR source is
incorrect.
Title: LBT Discovery of a Yellow Supergiant Eclipsing
Binary in the Dwarf Galaxy Holmberg IX
Authors: Prieto, J. L.; Stanek, K. Z.; Kochanek, C. S.;
Weisz, D. R.; Baruffolo, A.; Bechtold, J.;
Burwitz, V.; De Santis, C.; Gallozzi, S.;
Garnavich, P. M.; Giallongo, E.; Hill, J. M.;
Pogge, R. W.; Ragazzoni, R.; Speziali, R.;
Thompson, D. J.; Wagner, R. M.
Affiliation: AA(Department of Astronomy, Ohio State University,
Columbus, OH 43210.), AB(Department of Astronomy,
Ohio State University, Columbus, OH 43210.),
AC(Department of Astronomy, Ohio State University,
Columbus, OH 43210.), AD(Department of Astronomy,
University of Minnesota, Minneapolis, MN 55455.),
AE(INAF, Osservatorio Astronomico di Padova, I-35122
Padova, Italy.), AF(Steward Observatory, University
of Arizona, Tucson, AZ 85721.),
AG(Max-Planck-Institut für extraterrestrische
Physik, Giessenbachstraße, 85741 Garching,
Germany.), AH(INAF, Osservatorio Astronomico di
Roma, I-00040 Monteporzio, Italy.), AI(INAF,
Osservatorio Astronomico di Roma, I-00040
Monteporzio, Italy.), AJ(University of Notre Dame,
Notre Dame, IN 46556-5670.), AK(INAF, Osservatorio
Astronomico di Roma, I-00040 Monteporzio, Italy.),
AL(LBT Observatory, University of Arizona, Tucson,
AZ 85721-0065.), AM(Department of Astronomy, Ohio
State University, Columbus, OH 43210.), AN(INAF,
Osservatorio Astronomico di Padova, I-35122 Padova,
Italy.), AO(INAF, Osservatorio Astronomico di Roma,
I-00040 Monteporzio, Italy.), AP(LBT Observatory,
University of Arizona, Tucson, AZ 85721-0065.),
AQ(Department of Astronomy, Ohio State University,
Columbus, OH 43210.; LBT Observatory, University of
Arizona, Tucson, AZ 85721-0065.)
Publication: The Astrophysical Journal, Volume 673, Issue 1, pp.
L59-L62. (ApJ Homepage)
Publication Date: 01/2008
Origin: UCP
ApJ Keywords: Stars: Binaries: Eclipsing
Abstract Copyright: (c) 2008: The American Astronomical Society
DOI: 10.1086/527415
Bibliographic Code: 2008ApJ...673L..59P
Abstract
In a variability survey of M81 using the Large Binocular Telescope we
have discovered a peculiar eclipsing binary (MV~-7.1) in the
field of the dwarf galaxy Holmberg IX. It has a period of 271 days, and
the light curve is well fit by an overcontact model in which both stars
are overflowing their Roche lobes. It is composed of two yellow
supergiants (V-I~=1 mag, Teff~=4800 K), rather than the far
more common red or blue supergiants. Such systems must be rare. While we
failed to find any similar systems in the literature, we did, however,
note a second example. The SMC F0 supergiant R47 is a bright
(MV~-7.5) periodic variable whose All Sky Automated Survey
(ASAS) light curve is well fit as a contact binary with a 181 day
period. We propose that these systems are the progenitors of supernovae
like SN 2004et and SN 2006ov, which appeared to have yellow progenitors.
The binary interactions (mass transfer, mass loss) limit the size of the
supergiant to give it a higher surface temperature than an isolated star
at the same core evolutionary stage. We also discuss the possibility of
this variable being a long-period Cepheid.
Based on data acquired using the Large Binocular Telescope (LBT). The
LBT is an international collaboration among institutions in the United
States, Italy and Germany. LBT Corporation partners are The University
of Arizona on behalf of the Arizona university system; Istituto
Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany,
representing the Max-Planck Society, the Astrophysical Institute
Potsdam, and Heidelberg University; The Ohio State University, and The
Research Corporation, on behalf of The University of Notre Dame,
University of Minnesota, and University of Virginia.
Title: A Deep Large Binocular Telescope View of the Canes
Venatici I Dwarf Galaxy
Authors: Martin, Nicolas F.; Coleman, Matthew G.;
De Jong, Jelte T. A.; Rix, Hans-Walter;
Bell, Eric F.; Sand, David J.; Hill, John M.;
Thompson, David; Burwitz, Vadim;
Giallongo, Emanuele; Ragazzoni, Roberto;
Diolaiti, Emiliano; Gasparo, Federico;
Grazian, Andrea; Pedichini, Fernando; Bechtold, Jill
Affiliation: AA(Max-Planck-Institut für Astronomie, Heidelberg,
Germany;
.), AB(Max-Planck-Institut für Astronomie, Heidelberg, Germany; .), AC(Max-Planck-Institut für Astronomie, Heidelberg, Germany; .), AD(Max-Planck-Institut für Astronomie, Heidelberg, Germany; .), AE(Max-Planck-Institut für Astronomie, Heidelberg, Germany; .), AF(Steward Observatory,!
University of Arizona, Tucson, AZ.; Chandra Fellow.), AG(Large Binocular Telescope Observatory, University of Arizona, Tucson, AZ.), AH(Large Binocular Telescope Observatory, University of Arizona, Tucson, AZ.), AI(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany.), AJ(INAF, Osservatorio Astronomico di Roma, Monteporzio, Italy.), AK(INAF, Osservatorio Astronomico di Padova, Padova, Italy.), AL(INAF, Osservatorio Astronomico di Bologna, Bologna, Italy.), AM(INAF, Osservatorio Astronomico di Trieste, Trieste, Italy.), AN(INAF, Osservatorio Astronomico di Roma, Monteporzio, Italy.), AO(INAF, Osservatorio Astronomico di Roma, Monteporzio, Italy.), AP(Steward Observatory, University of Arizona, Tucson, AZ.)
Publication: The Astrophysical Journal, Volume 672, Issue 1, pp.
L13-L16. (ApJ Homepage)
Publication Date: 01/2008
Origin: UCP
ApJ Keywords: galaxies: individual (Canes Venatici I), Galaxies:
Stellar Content, Galaxies: Local Group
Abstract Copyright: (c) 2008: The American Astronomical Society
DOI: 10.1086/525559
Bibliographic Code: 2008ApJ...672L..13M
Abstract
We present the first deep color-magnitude diagram of the Canes Venatici
I (CVn I) dwarf galaxy from observations with the wide-field Large
Binocular Camera on the Large Binocular Telescope. Reaching down to the
main-sequence turnoff of the oldest stars, it reveals a dichotomy in the
stellar populations of CVn I: it harbors an old (>~10 Gyr),
metal-poor ([Fe/H]~-2.0), and spatially extended population along with a
much younger (~1.4-2.0 Gyr), 0.5 dex more metal-rich, and spatially more
concentrated population. These young stars are also offset by
64+40-20 pc to the east of the galaxy center. The
data suggest that this young population, which represents ~3%-5% of the
stellar mass of the galaxy within its half-light radius, should be
identified with the kinematically cold stellar component found in a
recent spectroscopic survey. CVn I therefore follows the behavior of the
other remote MW dwarf spheroidals, which all contain intermediate-age
and/or young populations: a complex star formation history is possible
in extremely low mass galaxies.
Based on data acquired using the Large Binocular Telescope (LBT). The
LBT is an international collaboration among institutions in the United
States, Italy, and Germany. LBT Corporation partners are the University
of Arizona on behalf of the Arizona university system; Istituto
Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany,
representing the Max-Planck Society, the Astrophysical Institute
Potsdam, and Heidelberg University; Ohio State University, and the
Research Corporation, on behalf of the University of Notre Dame, the
University of Minnesota, and the University of Virginia.
Title: Isopistonic angle for multi-aperture interferometers
from isoplanatic angle
Authors: Elhalkouj, T.; Ziad, A.; Petrov, R. G.;
Lazrek, M.; Elazhari, Y.; Benkhaldoun, Z.
Affiliation: AA(Université Cady-Ayyad Faculté des sciences LPHEA,
40000 Marrakech, Morocco
), AB(Université de Nice Sophia-Antipolis UMR 6525, Parc Valrose, 06108 Nice, France), AC(Université de Nice Sophia-Antipolis UMR 6525, Parc Valrose, 06108 Nice, France), AD(Université Cady-Ayyad Faculté des sciences LPHEA, 40000 Marrakech, Morocco), AE(École Normale Supérieure, route d'Essaouira, Laboratoire d'optique et optoélectronique, 4000 Marrakech, Morocco), AF(Université Cady-Ayyad Faculté des sciences LPHEA, 40000 Marrakech, Morocco)
Publication: Astronomy and Astrophysics, Volume 477, Issue 1,
January I 2008, pp.337-344 (A&A Homepage)
Publication Date: 01/2008
Origin: EDP
Keywords: instrumentation: interferometers, atmospheric
effects
DOI: 10.1051/0004-6361:20078173
Bibliographic Code: 2008A&A...477..337E
Abstract
Context: Extending the potential of multi-aperture telescopes toward the
higher magnitudes necessary for extragalactic science needs an off-axis
reference source to cophase the interferometric array. Aims: The
off-axis reference star and the science source must be within the
isopistonic angle, and evaluating this parameter is crucial for
estimating the potential of long-baseline interferometers for faint
sources, differential astrometry, and phase-reference imaging. Methods:
We derived an analytical method of deducing the isopistonic angle from
the standard atmospheric optical parameters, and used a full description
of the atmospheric turbulence to validate numerical integrations.
Results: We used the analytical expression for the isopistonic angle for
predictions concerning the VLT, Keck, and LBT interferometers, as well
as for an array of small apertures in the Antarctica site Dome C,
indicating that is might be a unique site on earth for interferometric
observations of faint sources.
Title: Basic Concepts and Parameters of Astronomical AO
Systems
Authors: Esposito, S.; Pinna, E.
Affiliation: AA(INAF $,1rs(B Osservatorio Astrofisico di Arcetri, L.go
E. Fermi), AB(INAF $,1rs(B Osservatorio Astrofisico di
Arcetri, L.go E. Fermi)
Publication: Jets from Young Stars II, Lecture Notes in Physics,
Volume 742. ISBN 978-3-540-68031-4. Springer-Verlag
Berlin Heidelberg, 2008, p. 45
Publication Date: 00/2008
Origin: SPRINGER
Abstract Copyright: (c) 2008: Springer-Verlag Berlin Heidelberg
Bibliographic Code: 2008LNP...742...45E
Abstract
The paper describes the basic concepts and parameters of astronomical
adaptive optic (AO) systems. In particular, the paper introduces and
discusses the main parameters and error sources that determine the
performances of an AO system. From this discussion, the current
limitations of AO systems are derived. Following this, the
laser-generated reference star method is described, being the best
technique to solve the main limitation of Astronomical AO system, namely
the limited sky coverage. Then advantages and disadvantages of such
technique are given. Using the considered matter, the case of LBT, the
first 8m class telescope using a deformable secondary mirror, is
described. The LBT AO system performances in the single telescope case
are briefly outlined. Then some concepts of optical interferometry are
reported. They are used to analyze the definition of homothetic
interferometer, the LBT case, and explain its differences from the
Michelson stellar interferometer configuration. Finally a short
description of the LBT interferometric instruments is given.
Title: GRB080310, late-time photometry with LBT.
Authors: Hill, J.; Ragazzoni, R.; Baruffolo, A.;
Garnavich, P.
Publication: GRB Coordinates Network, Circular Service, 7523, 1
(2008)
Publication Date: 00/2008
Origin: SIMBAD
Bibliographic Code: 2008GCN..7523....1H
Abstract
Not Available
Title: GRB080310, LBT and MDM photometry.
Authors: Wegner, G.; Garnavich, P.; Prieto, J. L.;
Stanek, K. Z.
Publication: GRB Coordinates Network, Circular Service, 7423, 1
(2008)
Publication Date: 00/2008
Origin: SIMBAD
Bibliographic Code: 2008GCN..7423....1W
Abstract
Not Available
Title: GRB080310, optical observations with the LBT.
Authors: Garnavich, P.; Prieto, J. L.; Pogge, R.
Publication: GRB Coordinates Network, Circular Service, 7409, 1
(2008)
Publication Date: 00/2008
Origin: SIMBAD
Bibliographic Code: 2008GCN..7409....1G
Abstract
Not Available
Title: GRB080310, optical observations with LBT.
Authors: Garnavich, P.; Dame, N.; Prieto, J. L.; Pogge, R.
Publication: GRB Coordinates Network, Circular Service, 7390, 1
(2008)
Publication Date: 00/2008
Origin: SIMBAD
Bibliographic Code: 2008GCN..7390....1G
Abstract
Not Available
Title: Go Long, Go Deep: Finding Optical Jet Breaks for
Swift-Era GRBs with the LBT
Authors: Dai, X.; Garnavich, P. M.; Prieto, J. L.;
Stanek, K. Z.; Kochanek, C. S.; Bechtold, J.;
Bouche, N.; Buschkamp, P.; Diolaiti, E.;
Fan, X.; Giallongo, E.; Gredel, R.;
Hill, J. M.; Jiang, L.; McClellend, C.;
Milne, P.; Pedichini, F.; Pogge, R. W.;
Ragazzoni, R.; Rhoads, J.; Smareglia, R.;
Thompson, D.; Wagner, R. M.
Publication: eprint arXiv:0712.2239
Publication Date: 12/2007
Origin: ARXIV
Keywords: Astrophysics
Comment: submitted to ApJ Letters, 16 pages, 3 figures
Bibliographic Code: 2007arXiv0712.2239D
Abstract
Using the 8.4m Large Binocular Telescope, we observed six GRB afterglows
from 2.8 hours to 30.8 days after the burst triggers to systematically
probe the late time behaviors of afterglows including jet breaks,
flares, and supernova bumps. We detected five afterglows with Sloan r'
magnitudes ranging from 23.0--26.3 mag. The depth of our observations
allows us to extend the temporal baseline for measuring jet breaks by
another decade in time scale. We detected two jet breaks and a third
candidate, all of which are not detectable without deep, late time
optical observations. In the other three cases, we do not detect the jet
breaks either because of contamination from the host galaxy light, the
presence of a supernova bump, or the intrinsic faintness of the optical
afterglow. This suggests that the basic picture that GRBs are collimated
is still valid and that the apparent lack of Swift jet breaks is due to
poorly sampled afterglow light curves, particularly at late times.
Title: Comet 17P/Holmes
Authors: Wagner, R. M.; Starrfield, S.; Schwarz, G.;
Larson, S.; Kaitchuck, R.; Childers, J.; Turner, G.
Publication: IAU Circ., 8887, 2 (2007). Edited by Green, D. W.
E. (IAUC Homepage)
Publication Date: 10/2007
Origin: CBAT
Objects: 17P
Bibliographic Code: 2007IAUC.8887....2W
Abstract
IAUC 8887 available at Central Bureau for Astronomical Telegrams.
Title: Observational Results from the 2007 March 18 Pluto
Stellar Occultation
Authors: Pasachoff, Jay M.; Babcock, B. A.;
Souza, S. P.; McKay, A. J.; Person, M. J.;
Elliot, J. L.; Gulbis, A. A.; Zuluaga, C. A.;
Hill, J. M.; Ryan, E. V.; Ryan, W. H.
Affiliation: AA(Williams College), AB(Williams College),
AC(Williams College), AD(Williams College), AE(MIT),
AF(MIT), AG(MIT), AH(MIT), AI(LBTO), AJ(Magdalena
Ridge Obs), AK(Magdalena Ridge Obs)
Publication: American Astronomical Society, DPS meeting #39,
#62.03
Publication Date: 10/2007
Origin: AAS
Abstract Copyright: (c) 2007: American Astronomical Society
Bibliographic Code: 2007DPS....39.6203P
Abstract
Our consortium observed the 5-minute occultation by Pluto of the star we
call P445.3 (2UCAC 25823784, UCAC magnitude 15.3; McDonald and Elliot,
2000, AJ 120, 1599) from sites in the American southwest on 2007 March
17/18 (18 March, UT). Shadow velocity was 6.8 km/s. The 2007 occultation
grazed the atmosphere. We were able to use one of the 8.4-m mirrors of
the Large Binocular Telescope Observatory, still in its engineering
stage, though only with its facility guide camera and not with our
Portable Occultation, Eclipse, and Transit System (POETS)
CCD/GPS/computer instruments (Souza et al., 2006, PASP 118, 1550).
Because of the accurate GPS timing, we were able to align the light
curve obtained, which included only the second half of the occultation,
with results from other telescopes, including the visible, beamsplit
light curve obtained by our group with the 6.5-m MMT (Person et al.,
2007, this meeting). We also used, with POETS, the 2.4-m Magdalena Ridge
Observatory near Socorro, New Mexico; a partial light curve was obtained
despite variable cloudiness throughout the 80 min observation. The
location of this telescope was the farthest into the occultation path,
and thus led to the deepest incursion into Pluto's atmosphere of the
starlight of the major telescopes we used. Light curves were generated
by frame-by-frame synthetic-aperture photometry. The large increase in
atmospheric pressure we had earlier measured at the 2002 occultation
compared with measurements at the first successful Pluto occultation, in
1988, has ceased, as shown by both the 2006 and the current, 2007
measurements.
Acknowledgments: We thank Richard Green for granting Director's
Discretionary time for the LBT observations. This work was partially
funded by NASA Planetary Astronomy grants NNG05GG75G, NNG04GE48G,
NNG04GF25G, and NNH04ZSS001N to Williams College and to MIT.
Title: Observation Preparation and Support Software for
LINC-NIRVANA
Authors: Pavlov, A.; Berwein, J.; Gässler, W.; Briegel, F.
Publication: Astronomical Data Analysis Software and Systems XVI
ASP Conference Series, Vol. 376, proceedings of the
conference held 15-18 October 2006 in Tucson,
Arizona, USA. Edited by Richard A. Shaw, Frank Hill
and David J. Bell., p.665
Publication Date: 10/2007
Origin: ASP
Bibliographic Code: 2007ASPC..376..665P
Abstract
LINC-NIRVANA is a near-infrared imaging interferometer for the Large
Binocular Telescope (LBT). The fixed geometry of the telescope and the
adaptive optics of the instrument put special constraints on the
observation and scheduling process. The observation and support
software, currently under development at MPIA, is a tool to support an
observer in the complex process of preparing and scheduling the
observations for LINC-NIRVANA. Our final goal is to create a coherent
software that guides a scientific project through all stages of the
LINC-NIRVANA observation program preparation to achieve high observation
efficiency and scientific results with the instrument.
Title: LINC-NIRVANA Instrument Control Software
Authors: Kittmann, F.; Gässler, W.; Briegel, F.; Berwein, J.
Publication: Astronomical Data Analysis Software and Systems XVI
ASP Conference Series, Vol. 376, proceedings of the
conference held 15-18 October 2006 in Tucson,
Arizona, USA. Edited by Richard A. Shaw, Frank Hill
and David J. Bell., p.661
Publication Date: 10/2007
Origin: ASP
Bibliographic Code: 2007ASPC..376..661K
Abstract
LINC-NIRVANA (LN) is a German-Italian beam combiner for the LBT. The
instrument exploits its full capability by means of Multi-Conjugate
Adaptive Optics and an IR Fringe and Flexure Tracker. Any of these
systems must run stand alone with full supported user interaction. In
addition they have to work together in a failure tolerant fashion. The
commanding and synchronization of all systems is done by observation
procedures based on Python scripts in the ICS. An alarm and notification
system (Briegel et al. 2007) collects the status and feedback of each
system non hierarchical and in parallel. We will present the software
architecture and the operational flow of LN.
Title: The Large Binocular Telescope: Really a Binocular
Now
Authors: Hill, J. M.
Publication: Astronomical Data Analysis Software and Systems XVI
ASP Conference Series, Vol. 376, proceedings of the
conference held 15-18 October 2006 in Tucson,
Arizona, USA. Edited by Richard A. Shaw, Frank Hill
and David J. Bell., p.643
Publication Date: 10/2007
Origin: ASP
Bibliographic Code: 2007ASPC..376..643H
Abstract
The Large Binocular Telescope (LBT) uses two 8.4~m diameter primary
mirrors mounted side-by-side to produce a collecting area equivalent to
an 11.8~m circular aperture. A unique feature of LBT is that the light
from the two primary mirrors can be combined to produce phased array
imaging of an extended field. This coherent imaging along with adaptive
optics gives the telescope the diffraction-limited resolution of a
22.65~m telescope. First light with a single primary mirror and a prime
focus imager was achieved in 2005 October. The second of two 8.4~m
borosilicate honeycomb primary mirrors was installed in the telescope in
2005 October and was aluminized in 2006 January. Binocular operation
with two prime focus cameras is planned for early 2007. The telescope
will use two F/15 adaptive secondaries to correct atmospheric
turbulence. These adaptive mirrors are now being integrated with their
electro-mechanics.
Title: Lifecycle Management for SOA-Based Composite
Applications
Authors: Berwein, J.; Briegel, F.; Kittmann, F.;
Pavlov, A.; G"Assler, W.
Publication: Astronomical Data Analysis Software and Systems XVI
ASP Conference Series, Vol. 376, proceedings of the
conference held 15-18 October 2006 in Tucson,
Arizona, USA. Edited by Richard A. Shaw, Frank Hill
and David J. Bell., p.535
Publication Date: 10/2007
Origin: ASP
Bibliographic Code: 2007ASPC..376..535B
Abstract
LINC-NIRVANA is a Fizeau interferometer for the Large Binocular
Telescope (LBT). The instrument combines the two 8.4-m telescopes into
one image plane. Due to the instrumental and operational complexity of
LINC-NIRVANA, a software architecture is required that enables control,
test and maintenance of individual instrument components. Therefore
LINC-NIRVANA applied a composite application based on a service oriented
architecture (SOA), which provides service distribution of stand-alone
applications, within a heterogeneous environment. We present a software
tool and the software architecture to manage the lifecycle of
distributed services.
Title: Logging and Exception Management for SOA-Based
Composite Applications
Authors: Briegel, F.; Berwein, J.; Kittmann, F.; Gässler, W.
Publication: Astronomical Data Analysis Software and Systems XVI
ASP Conference Series, Vol. 376, proceedings of the
conference held 15-18 October 2006 in Tucson,
Arizona, USA. Edited by Richard A. Shaw, Frank Hill
and David J. Bell., p.377
Publication Date: 10/2007
Origin: ASP
Bibliographic Code: 2007ASPC..376..377B
Abstract
LINC-NIRVANA is a Fizeau interferometer for the Large Binocular
Telescope (LBT). The instrument combines the two 8.4-m telescopes into
one image plane. Due to the high instrumental and operational complexity
of LINC-NIRVANA, a software architecture is required that enables
controlling, testing and maintainance of individual instrument
components (Briegel et al. 2006). Service-oriented architecture (SOA) is
an architectural approach to building composite applications from
reusable services. A composite application consists of functionality
drawn from several different sources within an SOA. The problem is
trouble-shooting composite applications. For efficient troubleshooting,
operators need an end-to-end, cross-platform logging and exception
handling system where the logging and exception information of every
unit can be retrieved, displayed and handled.
Title: WiBSI: A Wide-Bandwidth Sub-millimeter
Interferometer for the LBT
Authors: Bussmann, R. S.; Drouet D'Aubigny, C. Y.;
Walker, C. K.
Publication: From Z-Machines to ALMA: (Sub)Millimeter
Spectroscopy of Galaxies ASP Conference Series, Vol.
375, proceedings of the conference held 12-14
January, 2006 at the North American ALMA Science
Center, National Radio Astronomy Observatory,
Charlottesville, Virginia, United States. Edited by
Andrew J. Baker, Jason Glenn, Andrew I. Harris,
Jeffrey G. Mangum and Min S. Yun., p.221
Publication Date: 10/2007
Origin: ASP
Bibliographic Code: 2007ASPC..375..221B
Abstract
We describe a unique 350 $,1'<(Bm beam combiner designed for use on the
Large Binocular Telescope (LBT) on Mt. Graham that can be used with
either coherent or incoherent detectors. The LBT consists of two 8.4 m
optical quality primary mirrors on a common azimuth-elevation mount with
a center-to-center distance between the primaries of 14.4 m, allowing
angular resolution of 2 arcsec × 6 arcsec at 350 $,1'<(Bm. Unlike
the case of traditional radio interferometers, here the beams are
combined quasi-optically without the need for a digital correlator.
Therefore, the instantaneous bandwidth is limited only by the
capabilities of the detector.
Title: The Elongated Structure of the Hercules Dwarf
Spheroidal Galaxy from Deep Large Binocular
Telescope Imaging
Authors: Coleman, Matthew G.; de Jong, Jelte T. A.;
Martin, Nicolas F.; Rix, Hans-Walter;
Sand, David J.; Bell, Eric F.;
Pogge, Richard W.; Thompson, David J.;
Hippelein, H.; Giallongo, E.; Ragazzoni, R.;
DiPaola, Andrea; Farinato, Jacopo;
Smareglia, Riccardo; Testa, Vincenzo;
Bechtold, Jill; Hill, John M.;
Garnavich, Peter M.; Green, Richard F.
Affiliation: AA(Max-Planck-Institut für Astronomie, Königstuhl
17, D-69117 Heidelberg, Germany.),
AB(Max-Planck-Institut für Astronomie, Königstuhl
17, D-69117 Heidelberg, Germany.),
AC(Max-Planck-Institut für Astronomie, Königstuhl
17, D-69117 Heidelberg, Germany.),
AD(Max-Planck-Institut für Astronomie, Königstuhl
17, D-69117 Heidelberg, Germany.), AE(Steward
Observatory, University of Arizona, Tucson, AZ
85721.; Chandra Fellow.), AF(Max-Planck-Institut für
Astronomie, Königstuhl 17, D-69117 Heidelberg,
Germany.), AG(Department of Astronomy, Ohio State
University, 140 West 18th Avenue, Columbus, OH
43210-1173.), AH(Large Binocular Telescope
Observatory, University of Arizona, 933 North Cherry
Avenue, Tucson, AZ 85721-0065.),
AI(Max-Planck-Institut für Astronomie, Königstuhl
17, D-69117 Heidelberg, Germany.), AJ(INAF,
Osservatorio Astronomico di Roma, via Frascati 33,
I-00040 Monteporzio, Italy.), AK(INAF, Osservatorio
Astronomico di Roma, via Frascati 33, I-00040
Monteporzio, Italy.), AL(INAF, Osservatorio
Astronomico di Roma, via Frascati 33, I-00040
Monteporzio, Italy.), AM(INAF, Osservatorio
Astronomico di Padova, vicolo dell'Osservatorio, 5,
35122 Padova, Italy.), AN(INAF, Osservatorio
Astronomico di Trieste, via G. B. Tiepolo, 11, 34131
Trieste, Italy.), AO(INAF, Osservatorio Astronomico
di Roma, via Frascati 33, I-00040 Monteporzio,
Italy.), AP(Steward Observatory, University of
Arizona, Tucson, AZ 85721.), AQ(Large Binocular
Telescope Observatory, University of Arizona, 933
North Cherry Avenue, Tucson, AZ 85721-0065.),
AR(Harvard-Smithsonian Center for Astrophysics, 60
Garden Street, Cambridge MA 02138.), AS(Large
Binocular Telescope Observatory, University of
Arizona, 933 North Cherry Avenue, Tucson, AZ
85721-0065.)
Publication: The Astrophysical Journal, Volume 668, Issue 1, pp.
L43-L46. (ApJ Homepage)
Publication Date: 10/2007
Origin: UCP
ApJ Keywords: galaxies: individual (Hercules dwarf spheroidal
galaxy), Galaxies: Kinematics and Dynamics
Abstract Copyright: (c) 2007: The American Astronomical Society
DOI: 10.1086/522672
Bibliographic Code: 2007ApJ...668L..43C
Abstract
We present a deep, wide-field photometric survey of the newly discovered
Hercules dwarf spheroidal galaxy (dSph), based on data from the Large
Binocular Telescope. Images in B, V, and r were obtained with the Large
Binocular Camera covering a 23'×23' field of
view to a magnitude of ~25.5 (5 $,1'C(B). This permitted the
construction of color-magnitude diagrams that reach approximately 1.5
mag below the Hercules main-sequence turnoff. Three-filter photometry
allowed us to preferentially select probable Hercules member stars and
to examine the structure of this system at a previously unattained
level. We find that the Hercules dwarf is highly elongated (3:1),
considerably more so than any other dSph satellite of the Milky Way,
except the disrupting Sagittarius dwarf. Although we cannot rule out
that the unusual structure is intrinsic to Hercules as an equilibrium
system, our results suggest tidal disruption as a likely cause of this
highly elliptical structure. Given the relatively large galactocentric
distance of this system (132+/-12 kpc), signs of tidal disruption would
require the Hercules dwarf to be on a highly eccentric orbit around the
Milky Way.
Based on data acquired using the Large Binocular Telescope (LBT). The
LBT is an international collaboration among institutions in the US,
Italy, and Germany. LBT Corporation partners are the University of
Arizona, on behalf of the Arizona university system; Istituto Nazionale
di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany,
representing the Max Planck Society, the Astrophysical Institute
Potsdam, and Heidelberg University; Ohio State University; and the
Research Corporation, on behalf of the University of Notre Dame, the
University of Minnesota, and the University of Virginia.
Title: Advances in the reconstruction of LBT LINC-NIRVANA
images
Authors: La Camera, A.; Desiderá, G.; Arcidiacono, C.;
Boccacci, P.; Bertero, M.
Affiliation: AA(INAF - Osservatorio Astrofisico di Arcetri, Lgo.
E. Fermi 5, 50125 Firenze, Italy
), AB(DISI, Università di Genova, Via Dodecaneso 35, 16146 Genova, Italy), AC(INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy), AD(DISI, Università di Genova, Via Dodecaneso 35, 16146 Genova, Italy), AE(DISI, Università di Genova, Via Dodecaneso 35, 16146 Genova, Italy)
Publication: Astronomy and Astrophysics, Volume 471, Issue 3,
September I 2007, pp.1091-1097 (A&A Homepage)
Publication Date: 09/2007
Origin: EDP
Keywords: techniques: interferometric, thechniques: image
processing, methods: data analysis, methods:
numercial
DOI: 10.1051/0004-6361:20077380
Bibliographic Code: 2007A&A...471.1091L
Abstract
Context: LINC-NIRVANA, the Fizeau interferometer of the Large Binocular
Telescope (LBT), will require routine use of image reconstruction
methods for data reduction. To this purpose our group has already
developed the software package AIRY (Astronomical Image Restoration in
interferometrY). Aims: Observations of a target, with different
orientations of the baseline of LINC-NIRVANA, will provide images with
different orientations with respect to the CCD camera. This rotation
effect was not taken into account in our previous work. Therefore in
this paper we propose a method able to compensate for the rotation of
the field of view. Moreover we investigate acceleration techniques for
reducing the computational burden of multiple image deconvolution.
Methods: The basic method is a suitable modification of the
Richardson-Lucy algorithm, also implementing an approach we proposed for
reducing boundary effects. Acceleration techniques, proposed by Biggs
& Andrews, are extended and applied to this new algorithm. Finally a
method for estimating the unknown point spread function (PSF) by
extracting and extrapolating the image of a reference star is developed
and implemented. Results: The method introduced for compensating object
rotation and reducing boundary effects, as well as its accelerated
versions, are tested on simulated LINC-NIRVANA images, using the VLT
image of the Crab Nebula as test object. The results are very promising.
Moreover the method for PSFs extraction is tested on simulated images,
derived from the LBT image of the galaxy NGC 6946 and obtained by
convolving this image with PSFs computed by means of the numerical code
LOST (Layer Oriented Simulation Tool).
Title: First Results From the Large Binocular Telescope:
Deep Photometry of New dSphs
Authors: Coleman, Matthew G.; de Jong, Jelte
Publication: eprint arXiv:0708.2612
Publication Date: 08/2007
Origin: ARXIV
Keywords: Astrophysics
Comment: Four pages, two figures. To appear in the
proceedings of "Galaxies in the Local Volume",
Astrophysics and Space Science, editors B.
Koribalski and H. Jerjen
Bibliographic Code: 2007arXiv0708.2612C
Abstract
This contribution describes photometry for two Galactic dSphs obtained
with the Large Binocular Telescope to a magnitude of ~25.5. Using the
Large Binocular Camera, a purpose-built wide-field imager for the LBT,
we have examined the structure and star formation histories of two
newly-discovered Local Group members, the Hercules dSph and the Leo T
dSph/dIrr system. We have constructed a structural map for the Hercules
system using three-filter photometry to V ~ 25.5. This is the first deep
photometry for this system, and it indicates that Hercules is unusually
elongated, possibly indicating distortion due to the Galactic tidal
field. We have also derived the first star formation history for the Leo
T system, and find that its oldest population of stars (age ~ 13 Gyr)
were relatively metal-rich, with [Fe/H] ~ -1.5.
Title: The Large Binocular Camera at LBT
Authors: Giallongo, E.
Publication: Astronomische Nachrichten, Vol.328, Issue 7, July,
2007. Published by Wiley-VCH Verlag GmbH & Co. KGaA,
Weinheim, Germany, 2007, p.630 (AN Homepage)
Publication Date: 07/2007
Origin: ADS
Bibliographic Code: 2007AN....328Q.630G
Abstract
Not Available
Title: The Laser Guide Star Facility for the LBT
Authors: Rabien, S.
Publication: Astronomische Nachrichten, Vol.328, Issue 7, July,
2007. Published by Wiley-VCH Verlag GmbH & Co. KGaA,
Weinheim, Germany, 2007, p.631 (AN Homepage)
Publication Date: 07/2007
Origin: ADS
Bibliographic Code: 2007AN....328..631R
Abstract
Not Available
Title: SERPIL/LINUS: a design study for a Near-Infrared
Interferometric Integral Field Spectrometer for the
LBT
Authors: Mueller Sanchez, F.; Gal, C.; Eisenhauer, F.;
Krabbe, A.; Herbst, T.
Publication: Astronomische Nachrichten, Vol.328, Issue 7, July,
2007. Published by Wiley-VCH Verlag GmbH & Co. KGaA,
Weinheim, Germany, 2007, p.628 (AN Homepage)
Publication Date: 07/2007
Origin: ADS
Bibliographic Code: 2007AN....328..628M
Abstract
Not Available
Title: Feedback in galaxy cores: a LBT Key Science Project
proposal
Authors: Bomans, D.
Publication: Astronomische Nachrichten, Vol.328, Issue 7, July,
2007. Published by Wiley-VCH Verlag GmbH & Co. KGaA,
Weinheim, Germany, 2007, p.628 (AN Homepage)
Publication Date: 07/2007
Origin: ADS
Bibliographic Code: 2007AN....328..628B
Abstract
Not Available
Title: LUCIFER: a NIR Spectrograph and Imager for the LBT
Authors: Mandel, Holger; Seifert, Walter;
Lenzen, Rainer; Hofmann, Reiner; Jütte, Marcus;
Weiser, Peter; Appenzeller, Immo;
Bomans, Dominik; Buschkamp, Peter;
Dettmar, Ralf-Jürgen; Feiz, Carmen;
Gemperlein, Hans; Germeroth, André;
Grimm, Bernhard; Heidt, Jochen;
Knierim, Volker; Laun, Werner;
Lehmitz, Michael; Luks, Thomas; Mall, Ulrich;
Polsterer, Peter Müller Kai; Schimmelmann, Jan;
Weisz, Harald; Quirrenbach, Andreas
Publication: Astronomische Nachrichten, Vol.328, Issue 7, July,
2007. Published by Wiley-VCH Verlag GmbH & Co. KGaA,
Weinheim, Germany, 2007, p.626 (AN Homepage)
Publication Date: 07/2007
Origin: ADS
Bibliographic Code: 2007AN....328..626M
Abstract
Not Available
Title: LMIRCam 3-5 micron Imager for the LBT Combined Focus
Authors: Wilson, J. C.; Hinz, P.; Kenworthy, M.;
Skrutskie, M.; Jones, T. J.; Nelson, M.;
Woodward, C. E.; Garnavich, P.
Publication: Proceedings of the conference In the Spirit of
Bernard Lyot: The Direct Detection of Planets and
Circumstellar Disks in the 21st Century. June 04 -
08, 2007. University of California, Berkeley, CA,
USA. Edited by Paul Kalas.
Publication Date: 06/2007
Origin: AUTHOR
Bibliographic Code: 2007lyot.confE..51W
Abstract
LMIRCam is a 3-5 micron Fizeau imaging channel for use at the combined
focus of the Large Binocular Telescope (LBT). LMIRCam is being developed
by the University of Virginia, University of Minnesota, Notre Dame and
the University of Arizona. It will reside within the 10 micron Nulling
Interferometric Camera (NIC). We present this instrument's predicted
science capabilities, instrument design, and its potential use as a test
bed for complex coronographic methods.
Title: The Elongated Structure of the Hercules dSph from
Deep LBT Imaging
Authors: Coleman, Matthew G.; De Jong, Jelte T. A.;
Martin, Nicolas F.; Rix, Hans-Walter;
Sand, David J.; Bell, Eric F.;
Pogge, Richard W.; Thompson, David J.;
Hippelein, H.; Giallongo, E.; Ragazzoni, R.;
DiPaola, Andrea; Farinato, Jacopo;
Smareglia, Riccardo; Testa, Vincenzo;
Bechtold, Jill; Hill, John M.;
Garnavich, Peter M.; Green, Richard F.
Publication: eprint arXiv:0706.1669
Publication Date: 06/2007
Origin: ARXIV
Keywords: Astrophysics
Comment: Submitted to ApJ (Letters). 5 pages, 3 figures
Bibliographic Code: 2007arXiv0706.1669C
Abstract
We present a deep, wide-field photometric survey of the newly-discovered
Hercules dwarf spheroidal galaxy, based on data from the Large Binocular
Telescope. Images in B, V and r were obtained with the Large Binocular
Camera covering a 23' times 23' field of view to a magnitude of ~25.5 (5
sigma). This permitted the construction of colour-magnitude diagrams
that reach approximately 1.5 magnitudes below the Hercules main sequence
turnoff. Three-filter photometry allowed us to preferentially select
probable Hercules member stars, and examine the structure of this system
at a previously unattained level. We find that the Hercules dwarf is
highly elongated (3:1), considerably more so than any other dSph
satellite of the Milky Way except the disrupting Sagittarius dwarf.
While we cannot rule out that the unusual structure is intrinsic to
Hercules as an equilibrium system, our results suggest tidal disruption
as a likely cause of this highly elliptical structure. Given the
relatively large Galactocentric distance of this system (132 +/- 12
kpc), signs of tidal disruption would require the Hercules dwarf to be
on a highly eccentric orbit around the Milky Way.
Title: Signatures of Planets in Debris Disks
Authors: Moro-Martin, Amaya; Malhotra, Renu; Wolf, Sebastian
Publication: Workshop on Dust in Planetary Systems (ESA SP-643).
September 26-30 2005, Kauai, Hawaii. Editors:
Krueger, H. and Graps, A., p.113-122
Publication Date: 01/2007
Origin: ADS
Bibliographic Code: 2007ESASP.643..113M
Abstract
Main sequence stars are commonly surrounded by debris disks, formed by
cold far-IR-emitting dust that is thought to be continuously replenished
by a reservoir of undetected dust-producing planetesimals. In a
planetary system with a belt of planetesimals (like the Solar System's
Kuiper Belt) and one or more interior giant planets, as the particles
spiral inward due to Poynting-Robertson (PR) drag they can get trapped
in the mean motion resonances (MMRs) with the planets. This process can
create structure in the dust disk, as the particles accumulate at
certain semimajor axes. Sufficiently massive planets may also scatter
and eject dust particles out of a planetary system, creating a dust
depleted region inside the orbit of the planet, a feature that is common
in most of the spatially debris disks observed so far. We have studied
the efficiency of particle ejection and the resulting dust density
contrast inside and outside the orbit of the planet, as a function of
the planet's mass and orbital elements and the particle size.Because the
debris disk structure is sensitive to long period planets, complementing
a parameter space not covered by radial velocity and transit surveys,
its study can help us learn about the diversity of planetary systems.
Presently, the Spitzer Space Telescope is carrying out observations of
debris disks most of which are spatially unresolved. It is interesting
therefore to study how the structure carved by planets affects the shape
of the disk's Spectral Energy Distribution (SED), and consequently if
the SED can be used to infer the presence of planets. We have
numerically calculated the 3-D equilibrium spatial density distributions
of dust disks originated by a belt of planetesimals similar to the
Kuiper Belt (KB) in the presence of interior giant planets in different
planetary configurations (with planet masses ranging from 1-10 MJup in
circular orbits with semimajor axis between 1--30 AU). For each of these
systems we calculate its SED for a representative sample of chemical
compositions. We discuss what types of planetary systems can be
distinguishable from one another and the main parameter degeneracies in
the model SEDs. We find that the SEDs are degenerated, and therefore to
unambiguously constrain the planet location we need to obtain high
resolution images able to spatially resolve the disk. In the future,
observatories like ALMA, LBT, SAFIR, TPF and JWST will be able to image
the dust in planetary systems analogous to our own.
Title: Technological developments at the LBT: the prime
focus camera.
Authors: Di Paola, A.; Pedichini, F.; Speziali, R.;
Baruffolo, A.; Diolaiti, E.; Farinato, J.;
Gallozzi, S.; Gentile, G.; Giallongo, E.;
Ragazzoni, R.; Vernet, E.
Affiliation: AA( Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040 Monte
Porzio Catone, Italy), AB( Istituto Nazionale di
Astrofisica - Osservatorio Astronomico di Roma, Via
Frascati 33, I-00040 Monte Porzio Catone, Italy),
AC( Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040 Monte
Porzio Catone, Italy), AD(Istituto Nazionale di
Astrofisica - Osservatorio Astronomico di Padova,
Vicolo dell'Osservatorio 5, I-32122 Padova, Italy),
AE(Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Bologna, Via Ranzani 1, I-40127
Bologna, Italy), AF(Istituto Nazionale di
Astrofisica - Osservatorio Astronomico di Padova,
Vicolo dell'Osservatorio 5, I-32122 Padova, Italy),
AG( Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040 Monte
Porzio Catone, Italy), AH(Istituto Nazionale di
Astrofisica - Osservatorio Astronomico di Padova,
Vicolo dell'Osservatorio 5, I-32122 Padova, Italy),
AI( Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040 Monte
Porzio Catone, Italy), AJ(Istituto Nazionale di
Astrofisica - Osservatorio Astronomico di Padova,
Vicolo dell'Osservatorio 5, I-32122 Padova, Italy),
AK(Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Padova, Vicolo dell'Osservatorio 5,
I-32122 Padova, Italy)
Publication: Memorie della Societa Astronomica Italiana, v.78,
p.704 (2007)
Publication Date: 00/2007
Origin: MmSAI
Keywords: LBC, camera, LBT, prime focus, CCD, controllers, LN2
cryostat, control software
Abstract Copyright: (c) 2007: SAIt
Bibliographic Code: 2007MmSAI..78..704D
Abstract
This paper show the technological solutions adopted to build the blue (U
and B bands) and red (V, R, I and Z bands) of the prime focus imagers at
the LBT. We specially described the functional caracteristics and
performances of the cryogenic and CCD control systems and the instrument
management system.
Title: GRB 070419A, deep LBT photometry and possible
supernova detection.
Authors: Hill, J.; Garnavich, P.; Kuhn, O.;
Bouche, N.; Buschkamp, P.; Fan, X.; Dai, X.;
Prieto, J.; Stanek, K. Z.; Milne, P.;
Bechtold, J.; Wagner, R. M.; Rhoads, J.
Publication: GRB Coordinates Network, Circular Service, 6486, 1
(2007)
Publication Date: 00/2007
Origin: SIMBAD
Bibliographic Code: 2007GCN..6486....1H
Abstract
Not Available
Title: GRB 070518, deep LBT photometry.
Authors: Garnavich, P.; Dame, N.; Bouche, N.;
Buschkamp, P.; Kuhn, O.; Fan, X.; Dai, X.;
Prieto, J.; Stanek, K. Z.; Hill, J.;
Bechtold, J.; Kern, J.; Wagner, R. M.; Rhoads, J.
Publication: GRB Coordinates Network, Circular Service, 6462, 1
(2007)
Publication Date: 00/2007
Origin: SIMBAD
Bibliographic Code: 2007GCN..6462....1G
Abstract
Not Available
Title: GRB 070419A, deep LBT photometry.
Authors: Garnavich, P.; Fan, X.; Dai, X.; Prieto, J.;
Stanek, K. Z.; Hill, J.; Bechtold, J.;
Wagner, R. M.; Rhoads, J.
Publication: GRB Coordinates Network, Circular Service, 6406, 1
(2007)
Publication Date: 00/2007
Origin: SIMBAD
Bibliographic Code: 2007GCN..6406....1G
Abstract
Not Available
Title: GRB 070412, deep LBT imaging.
Authors: Prieto, J.; Garnavich, P.; Hill, J.; Fan, X.;
Harris, J.; Bechtold, J.; Dai, X.;
Martini, P.; Stanek, K. Z.; Wagner, R. M.;
Rhoads, J.; Pian, E.
Publication: GRB Coordinates Network, Circular Service, 6374, 1
(2007)
Publication Date: 00/2007
Origin: SIMBAD
Bibliographic Code: 2007GCN..6374....1P
Abstract
Not Available
Title: GRB 070411, further deep LBT photometry.
Authors: Garnavich, P.; Prieto, J.; Hill, J.; Fan, X.;
Dai, X.; Stanek, K. Z.; Wagner, R. M.;
Rhoads, J.; Bechtold, J.; Gredel, R.; Grazian, A.
Publication: GRB Coordinates Network, Circular Service, 6351, 1
(2007)
Publication Date: 00/2007
Origin: SIMBAD
Bibliographic Code: 2007GCN..6351....1G
Abstract
Not Available
Title: GRB 070411, deep LBT photometry.
Authors: Prieto, J.; Garnavich, P.; Hill, J.; Fan, X.;
Harris, J.; Dai, X.; Martini, P.;
Stanek, K. Z.; Wagner, R. M.; Rhoads, J.;
Herbert-Fort, S.
Publication: GRB Coordinates Network, Circular Service, 6346, 1
(2007)
Publication Date: 00/2007
Origin: SIMBAD
Bibliographic Code: 2007GCN..6346....1P
Abstract
Not Available
Title: Fizeau Interferometry with the LBT Astronomy on the
Way to ELTs
Authors: Gaessler, W.; Herbst, T. M.; Ragazzoni, R.;
Eckart, A.; Weigelt, G.; The Linc-Nirvana Team
Publication: Exploring the Cosmic Frontier: Astrophysical
Instruments for the 21st Century. ESO Astrophysics
Symposia, European Southern Observatory series.
Edited by Andrei P. Lobanov, J. Anton Zensus,
Catherine Cesarsky and Phillip J. Diamond. Series
editor: Bruno Leibundgut, ESO. ISBN
978-3-540-39755-7. Published by Springer-Verlag,
Berlin and Heidelberg, Germany, 2007, p.55
Publication Date: 00/2007
Origin: SPRINGER; ADS
Abstract Copyright: (c) 2007: Springer
Bibliographic Code: 2007ecf..book...55G
Abstract
Not Available
Title: Deconvolution of multiple images with high dynamic
range and an application to LBT LINC-NIRVANA
Authors: Anconelli, B.; Bertero, M.; Boccacci, P.;
Desiderà, G.; Carbillet, M.; Lanteri, H.
Affiliation: AA(DISI, Università di Genova, via Dodecaneso 35,
16146 Genova, Italy
), AB(DISI, Università di Genova, via Dodecaneso 35, 16146 Genova, Italy), AC(DISI, Università di Genova, via Dodecaneso 35, 16146 Genova, Italy), AD(DISI, Università di Genova, via Dodecaneso 35, 16146 Genova, Italy), AE(Laboratoire Universitaire d'Astrophysique de Nice, UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France), AF(Laboratoire Universitaire d'Astrophysique de Nice, UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France)
Publication: Astronomy and Astrophysics, Volume 460, Issue 1,
December II 2006, pp.349-355 (A&A Homepage)
Publication Date: 12/2006
Origin: EDP
Keywords: methods: numerical, techniques: image processing
DOI: 10.1051/0004-6361:20065836
Bibliographic Code: 2006A&A...460..349A
Abstract
Context: .The standard Richardson-Lucy method (RLM) does not work well
in the deconvolution of astronomical images containing objects with very
different angular scales and magnitudes. Therefore, modifications of
RLM, applicable to this kind of objects, must be investigated.
Aims: .We recently proposed a regularization of RLM which provides
satisfactory results in the case of particular test objects with high
dynamic range. In this paper we extend this method to the case of
multiple image deconvolution, having in mind application to the
reconstruction of the images provided by Fizeau interferometers such as
LINC-NIRVANA, the German-Italian beam combiner for the Large Binocular
Telescope.
Methods: .RLM is an iterative method for the
minimization of the Csiszár divergence, a problem equivalent to
maximum likelihood estimation in the case of photon noise. In our
approach, the problem is regularized by adding a suitable penalization
term to the Csiszár divergence and an iterative method converging
to the minimum of the resulting functional is derived from the so-called
split gradient method (SGM).
Results: .The method is tested on a
model of young binary star consisting of a core binary surrounded by a
dusty circumbinary ring. The results are quite good in the case of exact
knowledge of the point spread functions (PSF). However, in the case of
approximate knowledge of the PSFs, the accuracy of the reconstruction
depends on the difference of magnitude between the ring and the central
binary.
Title: Status and Plans for the Large Binocular Telescope
Authors: Green, R. F.
Affiliation: AA(Large Binocular Telescope Observatory, Tucson,
United States)
Publication: Astronomical Facilities of the Next Decade, 26th
meeting of the IAU, Special Session 1, 16-17 August,
2006 in Prague, Czech Republic, SPS1, #23
Publication Date: 08/2006
Origin: IAU
Bibliographic Code: 2006IAUSS...1E..23G
Abstract
The Large Binocular Telescope (LBT) is in commissioning, with the
initiation of science operations planned for 2007. The telescope
contains two 8.4-m diameter borosilicate honeycomb primary mirrors,
supported actively to control bending modes. The secondary mirrors will
provide adaptive optics correction through rapid modulation of the
surface of a Zerodur face sheet 91 cm in diameter and 1.5 mm thick. The
initial complement of facility instruments comprises capabilities used
in pairs on common fields of view. The Large Binocular Cameras are
wide-field 36 Mpix mosaics at prime focus optimized for blue and for red
performance. The Multi-Object Double Spectrographs will be fed at
straight-through Gregorian foci through custom cut focal plane masks.
The ambitious LUCIFER near-IR spectrographs at bent Gregorian will have
exchangeable cold focal plan masks. Ultimately, two instruments will
combine the two beams through Fizeau interferometry. One, LBTI, is
optimized for mid-IR, and will have a nulling capability for
coronagraphic work. The other, LINC-NIRVANA, will employ three levels of
adaptive correction to achieve interferometric resolution down to 1
micron. The 23-m tip-to-tip dimension affords resolution as good as 10
mas. LBTO is supported by a consortium of institutions from Arizona,
Italy, Germany, and the U.S. It is truly an international project and
the first of the next generation of large ground-based telescopes.
Title: V723 Cassiopeiae
Authors: Ness, J.-U.; Starrfield, S.; Schwarz, G.;
Vanlandingham, K.; Wagner, R. M.; Lyke, J.;
Woodward, C. E.; Lynch, D. K.; Krautter, J.;
Schmitt, J. H. M. M.
Publication: Central Bureau Electronic Telegrams, 598, 1 (2006).
Edited by Green, D. W. E.
Publication Date: 08/2006
Origin: CBAT
Objects: V723 Cas
Bibliographic Code: 2006CBET..598....1N
Abstract
CBET 598 available at Central Bureau for Astronomical Telegrams.
Title: The Large Binocular Telescope mount control system
architecture
Authors: Ashby, David S.; McKenna, Dan;
Brynnel, Joar G.; Sargent, Tom; Cox, Dan;
Little, John; Powell, Keith; Holmberg, Gene
Affiliation: AA(Large Binocular Telescope Observatory, Univ. of
Arizona (USA)), AB(Steward Observatory, Univ. of
Arizona (USA)), AC(Large Binocular Telescope
Observatory, Univ. of Arizona (USA)), AD(Steward
Observatory, Univ. of Arizona (USA)), AE(Steward
Observatory, Univ. of Arizona (USA)), AF(Large
Binocular Telescope Observatory, Univ. of Arizona
(USA)), AG(Steward Observatory, Univ. of Arizona
(USA)), AH(Steward Observatory, Univ. of Arizona
(USA))
Publication: Advanced Software and Control for Astronomy. Edited
by Lewis, Hilton; Bridger, Alan. Proceedings of the
SPIE, Volume 6274, pp. 627423 (2006). (SPIE
Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671983
Bibliographic Code: 2006SPIE.6274E..66A
Abstract
The Large Binocular Telescope (LBT) features dual 8.4 m diameter mirrors
in a common elevation-over-azimuth mount. The LBT moves in elevation on
two large crescent-shaped C-rings that are supported by radial
hydrostatic bearing pads located near the four corners of the
rectangular azimuth frame. The azimuth frame, in turn, is supported by
four hydrostatic bearing pads and uses hydrodynamic roller bearings for
centering. Each axis is gear driven by four large electric motors. In
addition to precision optical motor encoders, each axis is equipped with
Farrand Inductosyn strip encoders which yield 0.005 arcsecond
resolution. The telescope weighs 580 metric tons and is designed to
track with 0.03 arcsecond or better servo precision under wind speeds as
high as 24 km/hr. Though the telescope is still under construction, the
Mount Control System (MCS) has been routinely exercised to achieve First
Light. The authors present a description of the unique, DSP-based
synchronous architecture of the MCS and its capabilities.
Title: The LINC-NIRVANA fringe and flexure tracker: piston
control strategies
Authors: Rost, Steffen; Bertram, Thomas;
Straubmeier, Christian; Wang, Yeping;
Eckart, Andreas
Affiliation: AA(Univ. of Cologne (Germany)), AB(Univ. of Cologne
(Germany)), AC(Univ. of Cologne (Germany)), AD(Univ.
of Cologne (Germany)), AE(Univ. of Cologne
(Germany))
Publication: Advanced Software and Control for Astronomy. Edited
by Lewis, Hilton; Bridger, Alan. Proceedings of the
SPIE, Volume 6274, pp. 62741P (2006). (SPIE
Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671741
Bibliographic Code: 2006SPIE.6274E..53R
Abstract
The Fringe and Flexure Tracking System (FFTS) is designed to correct the
atmospheric piston variations and the instrumental flexure during the
NIR interferometric image acquisition of the LINC-NIRVANA camera at the
LBT. The interferometric image quality depends on the performance of
these corrections. Differential piston and flexure effects will be
detected and corrected in a real-time closed loop by analyzing the PSF
of a guide star at a frequency of up to several hundred Hz. A dedicated
piston mirror will then be moved in a corresponding manner by a piezo
actuator. The FFTS is expected to provide a residual piston of better
then 0.1 $,1';(B at the central wavelength of the science band. Thus,
the required correction bandwidth is 10-20 Hz as differential piston
simulations of different seeing conditions indicate. Therefore, a
sampling frequency of 100-200 Hz is required to correct OPD variations.
The upper limit for the loop frequency is the resonance frequency of the
mirror and the response function respectively. The piston mirror as the
actuator and the FFTS detector as the sensor feedback are embedded in a
very complex system. Many control loop aspects like sampling
frequencies, delays, controller algorithm and control bandwidth have to
be identified. With accurate simulations of the system the limits of
atmospheric and instrumental conditions for reliable closed loops can be
determined against the respective control parameters. We present
strategies for the closed-loop control of the piston correction which
are suitable to achieve the 0.1 $,1';(B requirement and the optimal
overall imaging performance with a sufficient "all-purpose" control
stability.
Title: The LINC-NIRVANA fringe and flexure tracker: Linux
real-time solutions
Authors: Wang, Yeping; Bertram, Thomas;
Straubmeier, Christian; Rost, Steffen;
Eckart, Andreas
Affiliation: AA(Univ. of Cologne (Germany)), AB(Univ. of Cologne
(Germany)), AC(Univ. of Cologne (Germany)), AD(Univ.
of Cologne (Germany)), AE(Univ. of Cologne
(Germany))
Publication: Advanced Software and Control for Astronomy. Edited
by Lewis, Hilton; Bridger, Alan. Proceedings of the
SPIE, Volume 6274, pp. 62741O (2006). (SPIE
Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671616
Bibliographic Code: 2006SPIE.6274E..52W
Abstract
The correction of atmospheric differential piston and instrumental
flexure effects is mandatory for optimum interferometric performance of
the LBT NIR interferometric imaging camera LINC-NIRVANA. The task of the
Fringe and Flexure Tracking System (FFTS) is to detect and correct these
effects in a real-time closed loop. On a timescale of milliseconds,
image data of the order of 4K bytes has to be retrieved from the FFTS
detector, analyzed, and the results have to be sent to the control
system. The need for a reliable communication between several processes
within a confined period of time calls for solutions with good real-time
performance. We investigated two soft real-time options for the Linux
platform. The design we present takes advantage of several features that
follow the POSIX standard with improved real-time performance, which
were implemented in the new Linux kernel (2.6.12). Several concepts,
such as synchronization, shared memory, and preemptive scheduling are
considered and the performance of the most time-critical parts of the
FFTS software is tested.
Title: The LINC-NIRVANA Common Software
Authors: Briegel, Florian; Berwein, Jürgen;
Kittmann, Frank; Volchkov, Valentin;
Mohr, Lars; Gaessler, Wolfgang;
Bertram, Thomas; Rost, Steffen; Wang, Yeping
Affiliation: AA(Max-Planck-Institute for Astronomy (Germany)),
AB(Max-Planck-Institute for Astronomy (Germany)),
AC(Max-Planck-Institute for Astronomy (Germany)),
AD(Max-Planck-Institute for Astronomy (Germany)),
AE(Max-Planck-Institute for Astronomy (Germany)),
AF(Max-Planck-Institute for Astronomy (Germany)),
AG(Univ. of Cologne (Germany)), AH(Univ. of Cologne
(Germany)), AI(Univ. of Cologne (Germany))
Publication: Advanced Software and Control for Astronomy. Edited
by Lewis, Hilton; Bridger, Alan. Proceedings of the
SPIE, Volume 6274, pp. 62741M (2006). (SPIE
Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671373
Bibliographic Code: 2006SPIE.6274E..50B
Abstract
The MPIA is leading an international consortium of institutes in
building an instrument called LINC-NIRVANA, the LBT INterferometric
Camera and Near-IR / Visible Adaptive INterferometer for Astronomy.
LINC-NIRVANA is a Fizeau interferometer for the Large Binocular
Telescope doing imaging in the near infrared (J, H, K - band).
Multi-conjugated adaptive objects is used to increase sky coverage and
to get diffraction limited images over a 2 arcminute field of view. The
LN Common Software provides a software infrastructure common to all
partners and consists of a documented collection of common patterns in
control systems and of services, which implement those patterns. The
heart of LCSW is an object model of controlled devices, implemented as
ICE network objects. A code generator creates application from templates
for these network objects.
Title: Lucifer VR: a virtual instrument for the LBT
Authors: Polsterer, Kai L.; Jütte, Marcus;
Knierim, Volker; Lehmitz, Michael; Mandel, Holger
Affiliation: AA(Ruhr-Univ. Bochum (Germany)), AB(Ruhr-Univ.
Bochum (Germany)), AC(Ruhr-Univ. Bochum (Germany)),
AD(Max-Planck Institut für Astronomie (Germany)),
AE(Landessternwarte Heidelberg (Germany))
Publication: Advanced Software and Control for Astronomy. Edited
by Lewis, Hilton; Bridger, Alan. Proceedings of the
SPIE, Volume 6274, pp. 62740M (2006). (SPIE
Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671279
Bibliographic Code: 2006SPIE.6274E..19P
Abstract
Lucifer VR is a virtually realized instrument that was build in order to
allow improved pre-integration software tests, training of observers as
well as providing educational access. Beside testing the instrument
hardware in combination with e.g. a telescope simulator, software tests
need to be done. A virtual instrument closes the gap between regression
tests and testing the control software with the integrated instrument.
Lucifer VR allows much earlier tests and reduces the amount of time
needed to combine the software with the hardware. By modeling the
instrument in a simulator, motion times can be calculated very easily
and the position of all instrument units can be traced. Especially when
using complex mechanisms like a MOS unit a virtual instrument makes
software development less time consuming. Lucifer VR consists of three
parts; one for handling the communication, another to simulate the
hardware and finally a part to visualize the whole instrument in three
dimensions.
Title: CFRP structure for the LBT instrument LINC-NIRVANA
Authors: Rohloff, Ralf-Rainer; Münch, Norbert;
Böhm, Armin; Schlossmacher, Wolfram;
Schöppinger, Carsten; Neugeboren, Hartmut;
Wittke, Henrik; Wichmann, Henning
Affiliation: AA(Max-Planck-Institut für Astronomie (Germany)),
AB(Max-Planck-Institut für Astronomie (Germany)),
AC(Max-Planck-Institut für Astronomie (Germany)),
AD(Ingenieurbüro Schlossmacher (Germany)), AE(INVENT
GmbH (Germany)), AF(INVENT GmbH (Germany)),
AG(INVENT GmbH (Germany)), AH(INVENT GmbH (Germany))
Publication: Optomechanical Technologies for Astronomy. Edited
by Atad-Ettedgui, Eli; Antebi, Joseph; Lemke,
Dietrich. Proceedings of the SPIE, Volume 6273, pp.
62730Z (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671314
Bibliographic Code: 2006SPIE.6273E..30R
Abstract
This paper describes the development of a Carbon Fiber-Reinforced
Plastics (CFRP) structure for the interferometric instrument
LINC-NIRVANA (LN) at the Large Binocular Telescope (LBT) Arizona, USA.
This structure carries all components between the two "bent" Gregorian
foci of the individual telescopes necessary to combine the light of the
two arms coherently. Especially developed for aerospace and defence,
CFRP materials now find widespread use across a number of other
applications where their special properties are beneficial. We will
profit in LN from the good rigidity, high strength, low thermal
expansion, low mass and high damping properties of CFRP. An extended
Finite Element Analysis was performed to simulate the properties of the
structure for different telescope positions and different temperatures.
We built a 560 mm x 550 mm x 385 mm test piece of the LN optical bench
for flexure tests to confirm the results of the Finite Element Analysis.
The complete LN instrument with a mass of 7.5 tons will be mounted at a
tilting unit to simulate the different telescope positions.
Title: The aluminizing system for the 8.4 meter diameter
LBT primary mirrors
Authors: Atwood, Bruce; Pappalardo, Daniel;
O'Brien, Thomas; Hill, John M.; Mason, Jerry;
Belville, Ralph; Steinbrecher, David;
Brewer, David; Teiga, Ed; Sabol, Barry;
Howard, James; Miglietta, L.
Affiliation: AA(The Ohio State Univ. (USA)), AB(The Ohio State
Univ. (USA)), AC(The Ohio State Univ. (USA)), AD(LBT
Observatory, Univ. of Arizona (USA)), AE(The Ohio
State Univ. (USA)), AF(The Ohio State Univ. (USA)),
AG(The Ohio State Univ. (USA)), AH(The Ohio State
Univ. (USA)), AI(The Ohio State Univ. (USA)), AJ(New
Mexico Institute of Mining and Technology (USA)),
AK(LBT Observatory, Univ. of Arizona (USA)),
AL(Osservatorio Astrofisico d'Arcetri (Italy))
Publication: Optomechanical Technologies for Astronomy. Edited
by Atad-Ettedgui, Eli; Antebi, Joseph; Lemke,
Dietrich. Proceedings of the SPIE, Volume 6273, pp.
62730T (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.672998
Bibliographic Code: 2006SPIE.6273E..25A
Abstract
The recently commissioned system for aluminizing the 8.408 meter
diameter Large Binocular Telescope mirrors has a variety of unusual
features. Among them are aluminizing the mirror in the telescope, the
mirror is horizon pointing when aluminized, boron nitride crucibles are
used for the sources, only 28 sources are used, the sources are powered
with 280 Volts at 20 kHz, high vacuum is produced with a LN2 cooled
charcoal cryo-panel, an inflatable edge seal is used to isolate the
rough vacuum behind the mirror from the high vacuum space, and a burst
disk is mounted in the center hole to protect the mirror from
overpressure. We present a description of these features. Results from
aluminizing both primary mirrors are presented.
Title: Design and manufacture of 8.4 m primary mirror
segments and supports for the GMT
Authors: Martin, H. M.; Angel, J. R. P.; Burge, J. H.;
Cuerden, B.; Davison, W. B.; Johns, M.;
Kingsley, J. S.; Kot, L. B.; Lutz, R. D.;
Miller, S. M.; Shectman, S. A.;
Strittmatter, P. A.; Zhao, C.
Affiliation: AA(Steward Observatory, Univ. of Arizona (USA)),
AB(Steward Observatory, Univ. of Arizona (USA)),
AC(Steward Observatory, Univ. of Arizona (USA) and
College of Optical Sciences, Univ. of Arizona
(USA)), AD(Steward Observatory, Univ. of Arizona
(USA)), AE(Steward Observatory, Univ. of Arizona
(USA)), AF(Carnegie Observatories (USA)), AG(Steward
Observatory, Univ. of Arizona (USA)), AH(Steward
Observatory, Univ. of Arizona (USA)), AI(Steward
Observatory, Univ. of Arizona (USA)), AJ(Steward
Observatory, Univ. of Arizona (USA)), AK(Carnegie
Observatories (USA)), AL(Steward Observatory, Univ.
of Arizona (USA)), AM(College of Optical Sciences,
Univ. of Arizona (USA))
Publication: Optomechanical Technologies for Astronomy. Edited
by Atad-Ettedgui, Eli; Antebi, Joseph; Lemke,
Dietrich. Proceedings of the SPIE, Volume 6273, pp.
62730E (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.672149
Bibliographic Code: 2006SPIE.6273E..13M
Abstract
The design, manufacture and support of the primary mirror segments for
the GMT build on the successful primary mirror systems of the MMT,
Magellan and Large Binocular telescopes. The mirror segment and its
support system are based on a proven design, and the experience gained
in the existing telescopes has led to significant refinements that will
provide even better performance in the GMT. The first 8.4 m segment has
been cast at the Steward Observatory Mirror Lab, and optical processing
is underway. Measurement of the off-axis surface is the greatest
challenge in the manufacture of the segments. A set of tests that meets
the requirements has been defined and the concepts have been developed
in some detail. The most critical parts of the tests have been
demonstrated in the measurement of a 1.7 m off-axis prototype. The
principal optical test is a full-aperture, high-resolution null test in
which a hybrid reflective-diffractive null corrector compensates for the
14 mm aspheric departure of the off-axis segment. The mirror support
uses the same synthetic floatation principle as the MMT, Magellan, and
LBT mirrors. Refinements for GMT include 3-axis actuators to accommodate
the varying orientations of segments in the telescope.
Title: Beyond conventional G-SCIDAR: the ground-layer in
high vertical resolution
Authors: Egner, Sebastian E.; Masciadri, Elena;
McKenna, Dan; Herbst, T. M.
Affiliation: AA(Max-Planck-Institute for Astronomy (Germany)),
AB(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AC(Steward Observatory (USA)),
AD(Max-Planck-Institute for Astronomy (Germany))
Publication: Advances in Adaptive Optics II. Edited by
Ellerbroek, Brent L.; Bonaccini Calia, Domenico.
Proceedings of the SPIE, Volume 6272, pp. 627256
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671380
Bibliographic Code: 2006SPIE.6272E.164E
Abstract
By using the SCIDAR instrument at the VATT on the top of Mt. Graham and
a very wide binary star with a separtion of 35", the vertical structure
of the turbulence in the first few hundred meters above the telescope
was measured. When using such a binary and analysing the
cross-correlation images, a vertical resolution for the turbulence
profile of a few tens of meters can be achieved near the ground. This
permits to determine the inner structure and the wind sheer of the
single turbulent layers inside the ground-layer. We present the
principles and the data-reduction process of this method and show first
results obtained with this method at Mt. Graham. As an application, we
estimate the fraction of the turbulence between the dome of the VATT and
the primary mirror of the LBT.
Title: MANU-CHAO: a laboratory ground-layer adaptive optics
experiment
Authors: Egner, Sebastian E.; Gaessler, Wolfgang;
Ragazzoni, Roberto; LeRoux, Brice;
Herbst, T. M.; Farinato, J.; Diolaiti, E.;
Arcidiacono, C.
Affiliation: AA(Max Planck Institute for Astronomy (Germany)),
AB(Max Planck Institute for Astronomy (Germany)),
AC(INAF, Osservatorio Astrofisico di Padova
(Italy)), AD(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AE(Max Planck Institute for
Astronomy (Germany)), AF(INAF, Osservatorio
Astrofisico di Padova (Italy)), AG(INAF,
Osservatorio Astrofisico di Bologna (Italy)),
AH(INAF, Osservatorio Astrofisico di Padova (Italy))
Publication: Advances in Adaptive Optics II. Edited by
Ellerbroek, Brent L.; Bonaccini Calia, Domenico.
Proceedings of the SPIE, Volume 6272, pp. 62724X
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671608
Bibliographic Code: 2006SPIE.6272E.156E
Abstract
We present a laboratory setup of a Ground-Layer Adaptive Optics system.
This system is a scaled-down version of the MCAO system of MAD (a MCAO
system for the VLT) / LINC-NIRVANA (a Fizeau Imager for the LBT) and
measures the wavefront aberrations with 4 pyramids in a layer-oriented
fashion with optical co-addition. The laboratory setup contains besides
the wavefront-sensing unit a telescope-simulator, a dynamic turbulence
generator and a Deformable Mirror for the wavefront correction. We
describe the overall system and its single components, open- and
closed-loop measurements of the characteristics of a system working in
GLAO mode and first results when using a Kalman filter for the control
of the wavefront reconstruction process.
Title: Integration, testing, and laboratory
characterization of the mid-high layer wavefront
sensor for LINC-NIRVANA
Authors: Lombini, Matteo; Foppiani, Italo;
Diolaiti, Emiliano; Farinato, Jacopo;
Ragazzoni, Roberto; Bregoli, Giovanni;
Ciattaglia, Costantino; Cosentino, Giuseppe;
Innocenti, Giancarlo; Schreiber, Laura;
Arcidiacono, Carmelo; De Bonis, Fulvio;
Egner, Sebastian; Gaessler, Wolfgang;
Herbst, Tom; Kuerster, Martin;
Schmidt, Johannes; Soci, Roberto;
Rossettini, Pierfrancesco; Tomelleri, Raffaele
Affiliation: AA(INAF, Osservatorio Astronomico di Bologna (Italy)
and INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AB(INAF, Osservatorio Astronomico di
Bologna (Italy) and INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AC(INAF, Osservatorio
Astronomico di Bologna (Italy)), AD(INAF,
Osservatorio Astrofisico di Arcetri (Italy) and
INAF, Osservatorio Astronomico di Padova (Italy)),
AE(INAF, Osservatorio Astronomico di Padova
(Italy)), AF(INAF, Osservatorio Astronomico di
Bologna (Italy)), AG(INAF, Osservatorio Astronomico
di Bologna (Italy)), AH(Univ. degli Studi di Bologna
(Italy)), AI(INAF, Osservatorio Astronomico di
Bologna (Italy)), AJ(Univ. degli Studi di Bologna
(Italy)), AK(INAF, Osservatorio Astrofisico di
Arcetri (Italy) and INAF, Osservatorio Astronomico
di Padova (Italy)), AL(Max-Planck-Institut für
Astronomie (Germany)), AM(Max-Planck-Institut für
Astronomie (Germany)), AN(Max-Planck-Institut für
Astronomie (Germany)), AO(Max-Planck-Institut für
Astronomie (Germany)), AP(Max-Planck-Institut für
Astronomie (Germany)), AQ(Max-Planck-Institut für
Astronomie (Germany)), AR(Max-Planck-Institut für
Astronomie (Germany)), AS(Tomelleri s.r.l. (Italy)),
AT(Tomelleri s.r.l. (Italy))
Publication: Advances in Adaptive Optics II. Edited by
Ellerbroek, Brent L.; Bonaccini Calia, Domenico.
Proceedings of the SPIE, Volume 6272, pp. 62724P
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671600
Bibliographic Code: 2006SPIE.6272E.149L
Abstract
The Mid-High Wavefront Sensors (MHWS) are components of the adaptive
optics system of LINC-NIRVANA, the Fizeau interferometer that will be
mounted at the LBT. These sensors, one for each telescope arm, will
measure the atmospheric turbulence in the high altitude layers, using up
to 8 reference stars in a 2 arcmin Field of View, and they will be
coupled with two Ground Layer WFSs that will measure the lower part of
the atmospheric turbulence using up to 12 stars over an annular Field of
View from 2 to 6 arcmin in diameter. We will describe the
opto-mechanical layout of the MHWS and the Assembly, Integration and
Test (AIT) phase of the first sensor in the laboratory of the Bologna
Observatory.
Title: The MCAO wavefront sensing system of LINC-NIRVANA:
status report
Authors: Farinato, Jacopo; Ragazzoni, Roberto;
Arcidiacono, Carmelo; Giorgia, Gentile;
Diolaiti, Emiliano; Foppiani, Italo;
Lombini, Matteo; Schreiber, Laura;
Lorenzetti, Dario; D'Alessio, Francesco;
Li Causi, Gianluca; Pedichini, Fernando;
Vitali, Fabrizio; Herbst, Tom; Kürster, Martin;
Bizenberger, Peter; Briegel, Florian;
De Bonis, Fulvio; Egner, Sebastian;
Gässler, Wolfgang; Mohr, Lars; Pavlov, Alexei;
Rohloff, Ralf Rainer; Soci, Roberto
Affiliation: AA(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AB(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AC(INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AD(INAF, Osservatorio
Astrofisico di Arcetri (Italy)), AE(INAF,
Osservatorio Astronomico di Bologna (Italy)),
AF(INAF, Osservatorio Astronomico di Bologna
(Italy)), AG(INAF, Osservatorio Astronomico di
Bologna (Italy)), AH(INAF, Osservatorio Astronomico
di Bologna (Italy)), AI(INAF, Osservatorio
Astronomico di Roma (Italy)), AJ(INAF, Osservatorio
Astronomico di Roma (Italy)), AK(INAF, Osservatorio
Astronomico di Roma (Italy)), AL(INAF, Osservatorio
Astronomico di Roma (Italy)), AM(INAF, Osservatorio
Astronomico di Roma (Italy)), AN(Max-Planck-Institut
für Astronomie (Germany)), AO(Max-Planck-Institut
für Astronomie (Germany)), AP(Max-Planck-Institut
für Astronomie (Germany)), AQ(Max-Planck-Institut
für Astronomie (Germany)), AR(Max-Planck-Institut
für Astronomie (Germany)), AS(Max-Planck-Institut
für Astronomie (Germany)), AT(Max-Planck-Institut
für Astronomie (Germany)), AU(Max-Planck-Institut
für Astronomie (Germany)), AV(Max-Planck-Institut
für Astronomie (Germany)), AW(Max-Planck-Institut
für Astronomie (Germany)), AX(Max-Planck-Institut
für Astronomie (Germany))
Publication: Advances in Adaptive Optics II. Edited by
Ellerbroek, Brent L.; Bonaccini Calia, Domenico.
Proceedings of the SPIE, Volume 6272, pp. 627229
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.673083
Bibliographic Code: 2006SPIE.6272E..70F
Abstract
LINC-NIRVANA is an infrared camera that will work in Fizeau
interferometric way at the Large Binocular Telescope (LBT). The two
beams that will be combined in the camera are corrected by an MCAO
system, aiming to cancel the turbulence in a scientific field of view of
2 arcminutes. The MCAO wavefront sensors will be two for each arm, with
the task to sense the atmosphere at two different altitudes (the ground
one and a second height variable between a few kilometers and a maximum
of 15 kilometers). The first wavefront sensor, namely the Ground layer
Wavefront sensor (GWS), will drive the secondary adaptive mirror of LBT,
while the second wavefront sensor, namely the Mid High layer Wavefront
Sensor (MHWS) will drive a commercial deformable mirror which will also
have the possibility to be conjugated to the same altitude of the
correspondent wavefront sensor. The entire system is of course
duplicated for the two telescopes, and is based on the Multiple Field of
View (MFoV) Layer Oriented (LO) technique, having thus different FoV to
select the suitable references for the two wavefront sensor: the GWS
will use the light of an annular field of view from 2 to 6 arcminutes,
while the MHWS will use the central 2 arcminutes part of the FoV. After
LINC-NIRVANA has accomplished the final design review, we describe the
MFoV wavefront sensing system together with its current status.
Title: High SNR measurement of interaction matrix on-sky
and in lab
Authors: Esposito, S.; Tubbs, R.; Puglisi, A.;
Oberti, S.; Tozzi, A.; Xompero, M.; Zanotti, D.
Affiliation: AA(Osservatorio Astrofisico di Arcetri (Italy)),
AB(Osservatorio Astrofisico di Arcetri (Italy)),
AC(Osservatorio Astrofisico di Arcetri (Italy)),
AD(European Southern Observatory (Germany)),
AE(Osservatorio Astrofisico di Arcetri (Italy)),
AF(Osservatorio Astrofisico di Arcetri (Italy)),
AG(Osservatorio Astrofisico di Arcetri (Italy))
Publication: Advances in Adaptive Optics II. Edited by
Ellerbroek, Brent L.; Bonaccini Calia, Domenico.
Proceedings of the SPIE, Volume 6272, pp. 62721C
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.673514
Bibliographic Code: 2006SPIE.6272E..41E
Abstract
The fundamental task of AO system calibration is the acquisition of the
Interaction Matrix (IM). This task is usually performed in a laboratory
or at the telescope using a reference fiber illuminating both deformable
mirror and wavefront sensor. The problem of measuring the IM on a bright
reference star has been attacked by some authors. The principal problem
of this measurement is to achieve a high SNR when atmospheric turbulence
is present. This is very difficult if sensor signals are simply time
averaged to get rid of the turbulence effects. The paper presents a new
technique to perform an on sky measurement of the IM with high SNR and
reducing the overall measurement time by an order of magnitude. This
technique can be very useful for AO systems using large size DMs like
MMT, LBT and possibly VLT and OWL. In these cases fiber-based IM
measurements require challenging optical set-up that in some cases, like
for OWL, are unpractical to build. The technique is still relevant for
classical small DM AO systems that could be calibrated on sky avoiding
misregistration errors. Finally this technique is valuable for
laboratory measurements when the IM of an AO system has to be measured
with great accuracy against external disturbances like bench vibrations,
local turbulence effects and so on. Again IM measurement SNR is
increased and the overall measurement time can be significantly reduced.
The paper will introduce and detail the technique physical principle and
quantify with numerical simulations the SNR improvement achieved using
this technique. Finally laboratory results obtained during the test of
the LBT AO system prototype are given and compared to simulations.
Title: Deformable secondary mirrors for the LBT adaptive
optics system
Authors: Martin, H. M.; Brusa Zappellini, G.;
Cuerden, B.; Miller, S. M.; Riccardi, A.;
Smith, B. K.
Affiliation: AA(Steward Observatory, Univ. of Arizona (USA)),
AB(Large Binocular Telescope Observatory, Univ. of
Arizona (USA)), AC(Steward Observatory, Univ. of
Arizona (USA)), AD(Steward Observatory, Univ of
Arizona (USA)), AE(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AF(Steward Observatory, Univ. of
Arizona (USA))
Publication: Advances in Adaptive Optics II. Edited by
Ellerbroek, Brent L.; Bonaccini Calia, Domenico.
Proceedings of the SPIE, Volume 6272, pp. 62720U
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.672698
Bibliographic Code: 2006SPIE.6272E..26M
Abstract
We describe the manufacture of thin shells for the deformable secondary
mirrors of the LBT adaptive optics system. The secondary mirrors are
thin shells, 910 mm in diameter and 1.6 mm thick. Each mirror will have
its shape controlled by 672 voice-coil actuators. The main requirement
for manufacture of the shell is smoothness on scales too small to be
adjusted by the actuators. An additional requirement is that the rear
surface match the reference body within 30 $,1'<(Bm peak-to-valley. A
technique was developed for producing smooth surfaces on the very
aspheric surfaces of the shells. We figure the optical surfaces on a
thick disk of Zerodur, then turn the disk over and thin it to 1.6 mm
from the rear surface. Figuring is done primarily with a 30 cm diameter
stressed lap, which bends actively to match the local curvature of the
aspheric surface. For the thinning operation, the mirror is blocked with
pitch, optical surface down, onto a granite disk with a matching convex
surface. Because the shell may bend during the blocking operation and as
its thickness is reduced to 1.6 mm, figuring of the rear surface is
guided by precise thickness measurements over the surface of the shell.
This method guarantees that both surfaces of the finished shell will
satisfy their requirements when corrected with small actuator forces.
Following the thinning operation, we edge the shell to its final
dimensions, remove it from the blocking body, and coat the rear surface
with aluminum to provide a set of conductive plates for capacitive
sensors.
Title: First light AO system for LBT: toward on-sky
operation
Authors: Esposito, S.; Tozzi, A.; Puglisi, A.;
Pinna, E.; Riccardi, A.; Busoni, S.;
Busoni, L.; Stefanini, P.; Xompero, M.;
Zanotti, D.; Pieralli, F.
Affiliation: AA(Osservatorio Astrofisico di Arcetri (Italy)),
AB(Osservatorio Astrofisico di Arcetri (Italy)),
AC(Osservatorio Astrofisico di Arcetri (Italy)),
AD(Osservatorio Astrofisico di Arcetri (Italy)),
AE(Osservatorio Astrofisico di Arcetri (Italy)),
AF(Osservatorio Astrofisico di Arcetri (Italy)),
AG(Osservatorio Astrofisico di Arcetri (Italy)),
AH(Osservatorio Astrofisico di Arcetri (Italy)),
AI(Osservatorio Astrofisico di Arcetri (Italy)),
AJ(Osservatorio Astrofisico di Arcetri (Italy)),
AK(Osservatorio Astrofisico di Arcetri (Italy))
Publication: Advances in Adaptive Optics II. Edited by
Ellerbroek, Brent L.; Bonaccini Calia, Domenico.
Proceedings of the SPIE, Volume 6272, pp. 62720A
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.673509
Bibliographic Code: 2006SPIE.6272E...8E
Abstract
The paper is describing the present status of the LBT first light AO
system. The system design started in January 2002 and is now approaching
the final test in the Arcetri solar tower. Two key features of this
single conjugate AO system are the use of an adaptive secondary mirror
having 672 actuators and a pyramid wavefront sensor with a maximum
sampling of 30x30 subapertures. The paper is reporting about the
adaptive secondary mechanical electrical and optical integration, and
the wavefront sensor unit integration and acceptance test. Finally some
lab test of the AO system done using an adaptive secondary prototype
with 45 actuators, the so called P45 are described. The aim of these
test was to get an estimate of the system limiting magnitude and to
demonstrate the feasibility of a new technique able to measure AO system
interaction matrix in a shortest time and with higher SNR with respect
to the classical interaction matrix measurement. We are planning to use
such a technique to calibrate the AO system in Arcetri and later at the
LBT telescope.
Title: Observation preparation software for LINC-NIRVANA
Authors: Pavlov, Aleksei; Gässler, Wolfgang;
Arcidiacono, Carmelo; Berwein, Jürgen;
Briegel, Florian; Schinnerer, Eva; Herbst, Tom
Affiliation: AA(Max-Planck-Institut für Astronomie (Germany)),
AB(Max-Planck-Institut für Astronomie (Germany)),
AC(INAF - Osservatorio Astrofisico di Arcetri
(Italy)), AD(Max-Planck-Institut für Astronomie
(Germany)), AE(Max-Planck-Institut für Astronomie
(Germany)), AF(Max-Planck-Institut für Astronomie
(Germany)), AG(Max-Planck-Institut für Astronomie
(Germany))
Publication: Observatory Operations: Strategies, Processes, and
Systems. Edited by Silva, David R.; Doxsey, Rodger
E.. Proceedings of the SPIE, Volume 6270, pp.
627011 (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671376
Bibliographic Code: 2006SPIE.6270E..34P
Abstract
LINC-NIRVANA is a Fizeau Interferometer using the two 8.4 m mirrors of
LBT in the combined focus. The images can be obtained in K, H and J Band
over a 10" × 10" Field of View by means of Multi-Conjugated
Adaptive Optics (MCAO) and a Fringe and Flexure Tracker System (FFTS).
In interferometry, the planning of observations is much more tightly
connected to the reduction of data than in traditional astronomy. Such
observations need to be carefully prepared, taking into account the
constraints imposed by scientific objectives as well as features of the
instrument. The Observation Preparation Software (OPS), currently under
development at MPIA, is a tool to support an astronomer (observer) in
the complex process of preparing the observations for LINC-NIRVANA. The
main goal of this tool is to provide the observer with an idea what he
or she can do and what to expect under given conditions.
Title: Reactive scheduling for LINC-NIRVANA
Authors: Berwein, Juergen; Pavlov, Aleksei;
Briegel, Florian; Gaessler, Wolfgang; Storz, Clemens
Affiliation: AA(Max-Planck-Institut für Astronomie (Germany)),
AB(Max-Planck-Institut für Astronomie (Germany)),
AC(Max-Planck-Institut für Astronomie (Germany)),
AD(Max-Planck-Institut für Astronomie (Germany)),
AE(Max-Planck-Institut für Astronomie (Germany))
Publication: Observatory Operations: Strategies, Processes, and
Systems. Edited by Silva, David R.; Doxsey, Rodger
E.. Proceedings of the SPIE, Volume 6270, pp.
627010 (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671261
Bibliographic Code: 2006SPIE.6270E..33B
Abstract
LINC-NIRVANA is a Fizeau interferometer for the LBT. The instrument
combines the two 8.4 m telescopes into one image plane. The fixed
geometry of the telescope and the adaptive optics of the instrument put
constraints on the observation schedule. Environmental changes
influences the execution of observations. We present a robust and
reactive scheduling strategy to achieve high observation efficiency and
scientific results with our instrument.
Title: The LINC-NIRVANA patrol camera
Authors: Lorenzetti, Dario; D'Alessio, Francesco;
Li Causi, Gianluca; Vitali, Fabrizio;
Pedichini, Fernando; Speziali, Roberto;
Diolaiti, Emiliano; Farinato, Jacopo;
Ragazzoni, Roberto; Briegel, Florian;
De Bonis, Fulvio; Gaessler, Wolfgang; Soci, Roberto
Affiliation: AA(INAF, Osservatorio Astronomico di Roma (Italy)),
AB(INAF, Osservatorio Astronomico di Bologna
(Italy)), AC(INAF, Osservatorio Astronomico di Roma
(Italy)), AD(INAF, Osservatorio Astronomico di Roma
(Italy)), AE(INAF, Osservatorio Astronomico di Roma
(Italy)), AF(INAF, Osservatorio Astronomico di Roma
(Italy)), AG(INAF, Osservatorio Astronomico di
Bologna (Italy)), AH(INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AI(INAF, Osservatorio
Astrofisico di Arcetri (Italy)),
AJ(Max-Planck-Institut für Astronomie (Germany)),
AK(Max-Planck-Institut für Astronomie (Germany)),
AL(Max-Planck-Institut für Astronomie (Germany)),
AM(Max-Planck-Institut für Astronomie (Germany))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 62695C
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.668881
Bibliographic Code: 2006SPIE.6269E.169L
Abstract
LINC-NIRVANA is the IR Fizeau interferometric imager of the Large
Binocular Telescope (LBT) in Arizona. Here we describe in particular the
design, realization and preliminary tests of the so-called Patrol
Camera. It can image (in the range 600-900 nm) the same 2 arcmin FoV
seen by the Medium- High-Wavefront Sensor (MHWS), adequately sampled to
provide the MHWS star enlargers with the positions of the FoV stars with
an accuracy of 0.1 arcsec. To this aim a diffraction-limited performance
is not required, while a distortion free focal plane is needed to
provide a suitable astrometric output. Two identical systems will be
realized, one for each single arm, which corresponds to each single
telescope. We give here the details concerning the optical and
mechanical design, as well as the CCD and the control system. The
interfaces with LINC-NIRVANA are also presented both in terms of
matching the carbon fiber optical bench and developing of suitable
software procedures. Since the major components have been already
gathered, the laboratory tests and the integration are currently in
progress.
Title: The LINC-NIRVANA IR cryostat
Authors: Laun, W.; Baumeister, H.; Bizenberger, P.
Affiliation: AA(Max Planck Institut für Astronomie (Germany)),
AB(Max Planck Institut für Astronomie (Germany)),
AC(Max Planck Institut für Astronomie (Germany))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 626956
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671642
Bibliographic Code: 2006SPIE.6269E.163L
Abstract
The MPIA is leading an international consortium of institutes building
an instrument called LINC-NIRVANA. The instrument will combine the light
from the two 8.4 m primary mirrors of the LBT. The beam combiner will
operate at wavelengths between 1.1 and 2.4 microns, using a Hawaii2
detector. A volume of about 1.6 m high with a diameter of about 0.65 m
is required for the cold optics. The size of the instrument and the high
requirements on vibrations brought us to a new approach for the cooling
of the cryostat, which has never been tried in astronomy. The cryostat
will be cooled by a flow of Helium gas. The cooler which cools the gas
will be placed far away on a different level in the telescope building.
The cold helium will be fed through long vacuum isolated transfer lines
to the instrument cryostat. Inside the cryostat a tube will be wrapped
around the mounting structure of the cold optics. The first hardware
arrived at the MPIA in 2005 and the system will soon be tested in our
labs.
Title: LIINUS/SERPIL: a design study for interferometric
imaging spectroscopy at the LBT
Authors: Gál, C.; Müller-Sánchez, F.; Krabbe, A.;
Eisenhauer, F.; Iserlohe, C.; Haug, M.;
Herbst, T. M.
Affiliation: AA(Univ. of Cologne (Germany)), AB(Max-Plank
Institute for extraterrestrial Physics (Germany)),
AC(Univ. of Cologne (Germany)), AD(Max-Plank
Institute for extraterrestrial Physics (Germany)),
AE(Univ. of Cologne (Germany)), AF(Max-Plank
Institute for extraterrestrial Physics (Germany)),
AG(Max-Planck Institute for Astronomy (Germany))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 62693O
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.670220
Bibliographic Code: 2006SPIE.6269E.116G
Abstract
LIINUS/SERPIL is a design study to augment LBTs interferometric beam
combiner camera LINC-NIRVANA with imaging spectroscopy. The FWHM of the
interferometric main beam at 1.5 micron will be about 10 mas, offering
unique imaging and spectroscopic capabilities well beyond the angular
resolution of current 8-10m telescopes. At 10 mas angular scale, e.g.,
one resolution element at the distance of the Galactic Center
corresponds to the average diameter of the Pluto orbit (79 AU), hence
the size of the solar system. Taking advantage of the LBT
interferometric beam with an equivalent maximum diameter of 23 m,
LIINUS/SERPIL is an ideal precursor instrument for (imaging)
spectrographs at extremely large full aperture telescopes. LIINUS/SERPIL
will be built upon the LINC-NIRVANA hardware and LIINUS/SERPIL could
potentially be developed on a rather short timescale. The study
investigates several concepts for the optical as well as for the
mechanical design. We present the scientific promises of such an
instrument together with the current status of the design study.
Title: LUCIFER status report: Summer 2006
Authors: Mandel, H. G.; Appenzeller, I.; Seifert, W.;
Baumeister, H.; Dettmar, R.-J.; Feiz, C.;
Gemperlein, H.; Germeroth, A.; Grimm, B.;
Heidt, J.; Herbst, T.; Hofmann, R.;
Jütte, M.; Knierim, V.; Laun, W.; Luks, T.;
Lehmitz, M.; Lenzen, R.; Polsterer, K.;
Quirrenbach, A.; Rohloff, R.-R.;
Rosenberger, J.; Weiser, P.; Weisz, H.
Affiliation: AA(Landessternwarte Heidelberg-Königstuhl
(Germany)), AB(Landessternwarte
Heidelberg-Königstuhl (Germany)),
AC(Landessternwarte Heidelberg-Königstuhl
(Germany)), AD(Max-Planck-Institut für Astronomie
(Germany)), AE(Ruhr-Univ. Bochum (Germany)),
AF(Landessternwarte Heidelberg-Königstuhl
(Germany)), AG(Max-Planck-Institut für
Extraterrestrische Physik (Germany)),
AH(Landessternwarte Heidelberg-Königstuhl
(Germany)), AI(Max-Planck-Institut für Astronomie
(Germany)), AJ(Landessternwarte
Heidelberg-Königstuhl (Germany)),
AK(Max-Planck-Institut für Astronomie (Germany)),
AL(Max-Planck-Institut für Extraterrestrische Physik
(Germany)), AM(Ruhr-Univ. Bochum (Germany)),
AN(Ruhr-Univ. Bochum (Germany)),
AO(Max-Planck-Institut für Astronomie (Germany)),
AP(Ruhr-Univ. Bochum (Germany)),
AQ(Max-Planck-Institut für Astronomie (Germany)),
AR(Max-Planck-Institut für Astronomie (Germany)),
AS(Ruhr-Univ. Bochum (Germany)), AT(Landessternwarte
Heidelberg-Königstuhl (Germany)),
AU(Max-Planck-Institut für Astronomie (Germany)),
AV(Landessternwarte Heidelberg-Königstuhl
(Germany)), AW(Fachhochschule Mannheim (Germany)),
AX(Max-Planck-Institut für Extraterrestrische Physik
(Germany))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 62693F
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671067
Bibliographic Code: 2006SPIE.6269E.107M
Abstract
LUCIFER (LBT NIR Spectrograph Utility with Camera and Integral-Field
Unit for Extragalactic Research) is a NIR spectrograph and imager for
the LBT (Large Binocular Telescope) working in the wavelength range from
0.9 to 2.5 microns. Two instruments are built by a consortium of five
German institutes (Landessternwarte Heidelberg (LSW), Max Planck
Institut for Astronomy (MPIA), Max Planck Institut for Extraterrestric
Physics (MPE), Astronomical Institut of the Ruhr-University Bochum
(AIRUB) and Fachhochschule for Technics and Design Mannheim (FHTG). All
major components for the first instrument have been manufactured or are
in the final stage of procurement. While integration and testing of
LUCIFER 1 started in spring 2006 at the MPIA in Heidelberg, the cryostat
for LUCIFER 2 has been sent to the MPE in Garching for system
integration tests of the MOS-unit and testing of the mask cabinet
exchange. The control electronics for the basic instrument has been
manufactured, the MOS control electronics has been integrated and is
being debugged. The MOS control software is under development by AIRUB.
Fabrication and integration of components for LUCIFER 2 have started.
Title: MegaMIR: a Fizeau thermal infrared camera for the
LBTI
Authors: Mainzer, A. K.; Young, Erick; Hong, John;
Hinz, Phil; Werner, Mike; Gorjian, Varoujan;
Ressler, Michael E.
Affiliation: AA(Jet Propulsion Lab. (USA)), AB(Univ. of Arizona
(USA)), AC(Jet Propulsion Lab. (USA)), AD(Univ. of
Arizona (USA)), AE(Jet Propulsion Lab. (USA)),
AF(Jet Propulsion Lab. (USA)), AG(Jet Propulsion
Lab. (USA))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 626910
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.670380
Bibliographic Code: 2006SPIE.6269E..33M
Abstract
The Megapixel Mid-infrared Instrument (MegaMIR) is a proposed
Fizeau-mode camera for the Large Binocular Telescope operating at
wavelengths between 5 and 28 $,1'<(Bm. The camera will be used in
conjunction with the Large Binocular Telescope Interferometer (LBTI), a
cryogenic optical system that combines the beams from twin 8.4-m
telescopes in a phase coherent manner. Unlike other interferometric
systems, the co-mounted telescopes on the LBT satisfy the sine
condition, providing diffraction-limited resolution over the 40" field
of view of the camera. With a 22.8-m baseline, MegaMIR will yield 0.1"
angular resolution, making it the highest resolution wide field imager
in the thermal infrared for at least the next decade. MegaMIR will
utilize a newly developed 1024 x 1024 pixel Si:As detector array that
has been optimized for use at high backgrounds. This new detector is a
derivative of the Wide-field Infrared Survey Explorer (WISE)
low-background detector. The combination of high angular resolution and
wide field imaging will be a unique scientific capability for astronomy.
Key benefits will be realized in planetary science, galactic, and
extra-galactic astronomy. High angular resolution is essential to
disentangle highly complex sources, particularly in star formation
regions and external galaxies, and MegaMIR provides this performance
over a full field of view. Because of the great impact being made by
space observatories like the Spitzer Space Telescope, the number of
available targets for study has greatly increased in recent years, and
MegaMIR will allow efficient follow up science.
Title: The multi-object double spectrographs for the Large
Binocular Telescope
Authors: Pogge, R. W.; Atwood, B.; Belville, S. R.;
Brewer, D. F.; Byard, P. L.; DePoy, D. L.;
Derwent, M. A.; Eastwood, J.; Gonzalez, R.;
Krygier, A.; Marshall, J. R.; Martini, P.;
Mason, J. A.; O'Brien, T. P.; Osmer, P. S.;
Pappalardo, D. P.; Steinbrecher, D. P.;
Teiga, E. J.; Weinberg, D. H.
Affiliation: AA(The Ohio State Univ. (USA)), AB(The Ohio State
Univ. (USA)), AC(The Ohio State Univ. (USA)), AD(The
Ohio State Univ. (USA)), AE(The Ohio State Univ.
(USA)), AF(The Ohio State Univ. (USA)), AG(The Ohio
State Univ. (USA)), AH(The Ohio State Univ. (USA)),
AI(The Ohio State Univ. (USA)), AJ(The Ohio State
Univ. (USA)), AK(The Ohio State Univ. (USA)), AL(The
Ohio State Univ. (USA)), AM(The Ohio State Univ.
(USA)), AN(The Ohio State Univ. (USA)), AO(The Ohio
State Univ. (USA)), AP(The Ohio State Univ. (USA)),
AQ(The Ohio State Univ. (USA)), AR(The Ohio State
Univ. (USA)), AS(The Ohio State Univ. (USA))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 62690I
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.670704
Bibliographic Code: 2006SPIE.6269E..16P
Abstract
Ohio State is building two identical Multi-Object Double Spectrographs
(MODS), one for each of the f/15 Gregorian foci of the Large Binocular
Telescope (LBT). Each MODS is a high-throughput optical low- to
medium-resolution CCD spectrometer operating in the 320-1000nm range
with a 6.5-arcminute field-of-view. A dichroic distributes the science
beam into separately-optimized red and blue channels that provide for
direct imaging and up to 3 spectroscopic modes per channel. The
identical MODS instruments may be operated together with digital data
combination as a single instrument giving the LBT an effective aperture
of 11.8-meter, or separately configured to flexibly use the twin
8.4-meter apertures. This paper describes progress on the integration
and testing of MODS1, and plans for the deployment of MODS2 by the end
of 2008 at the LBT.
Title: LINC-NIRVANA: optical design of an interferometric
imaging camera
Authors: Bizenberger, P.; Diolaiti, E.; Egner, S.;
Herbst, T. M.; Ragazzoni, R.; Reymann, D.; Xu, W.
Affiliation: AA(Max Planck Institute for Astronomy (Germany)),
AB(Osservatorio Astronomico di Bologna (Italy)),
AC(Max Planck Institute for Astronomy (Germany)),
AD(Max Planck Institute for Astronomy (Germany)),
AE(Osservatorio Astrofisico di Arcetri (Italy)),
AF(Max Planck Institute for Astronomy (Germany)),
AG(Optical System Engineering (Germany))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 62690D
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671569
Bibliographic Code: 2006SPIE.6269E..11B
Abstract
Combining the two 8.4 m telescopes of the Large Binocular Telescope
1(LBT) offers the unique possibility to achieve diffraction
limited images with 23 m spatial resolution. This requires an
interferometric superposition of the two telescope beams in a
Fizeau-type interferometer. LINC-NIRVANA delivers a 10 arcsec x 10
arcsec panoramic field of view with 5 mas pixel size. In addition to
delivering diffraction limited, single-telescope images, the optics have
several additional constraints imposed by interferometric operation. In
this paper, we describe the evolution of the optical design and how the
individual optical subsystems were developed in parallel to provide
optimal combined performance. We also present an alignment strategy to
setup the optics and to achieve zero optical path difference.
Title: An overview of instrumentation for the Large
Binocular Telescope
Authors: Wagner, R. Mark
Affiliation: AA(Large Binocular Telescope Observatory, The Ohio
State Univ. (USA))
Publication: Ground-based and Airborne Instrumentation for
Astronomy. Edited by McLean, Ian S.; Iye, Masanori.
Proceedings of the SPIE, Volume 6269, pp. 626909
(2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.670636
Bibliographic Code: 2006SPIE.6269E...7W
Abstract
An overview of instrumentation for the Large Binocular Telescope is
presented. Optical instrumentation includes the Large Binocular Camera
(LBC), a pair of wide-field (27' × 27') mosaic CCD imagers at the
prime focus, and the Multi-Object Double Spectrograph (MODS), a pair of
dual-beam blue-red optimized long-slit spectrographs mounted at the
straight-through F/15 Gregorian focus incorporating multiple slit masks
for multi-object spectroscopy over a 6' field and spectral resolutions
of up to 8000. Infrared instrumentation includes the LBT Near-IR
Spectroscopic Utility with Camera and Integral Field Unit for
Extragalactic Research (LUCIFER), a modular near-infrared (0.9-2.5
$,1'<(Bm) imager and spectrograph pair mounted at a bent interior focal
station and designed for seeing-limited (FOV: 4' × 4') imaging,
long-slit spectroscopy, and multi-object spectroscopy utilizing cooled
slit masks and diffraction limited (FOV: 0'.5 × 0'.5) imaging and
long-slit spectroscopy. Strategic instruments under development for the
remaining two combined focal stations include an interferometric
cryogenic beam combiner with near-infrared and thermal-infrared
instruments for Fizeau imaging and nulling interferometry (LBTI) and an
optical bench near-infrared beam combiner utilizing multi-conjugate
adaptive optics for high angular resolution and sensitivity
(LINC-NIRVANA). In addition, a fiber-fed bench spectrograph (PEPSI)
capable of ultra high resolution spectroscopy and spectropolarimetry (R
= 40,000-300,000) will be available as a principal investigator
instrument. The availability of all these instruments mounted
simultaneously on the LBT permits unique science, flexible scheduling,
and improved operational support.
Title: The LINC-NIRVANA fringe and flexure tracker: image
analysis concept and fringe tracking performance
estimate
Authors: Bertram, Thomas; Arcidiacono, Carmelo;
Straubmeier, Christian; Rost, Steffen;
Wang, Yeping; Eckart, Andreas
Affiliation: AA(Univ. of Cologne (Germany)), AB(INAF -
Osservatorio di Arcetri (Italy)), AC(Univ. of
Cologne (Germany)), AD(Univ. of Cologne (Germany)),
AE(Univ. of Cologne (Germany)), AF(Univ. of Cologne
(Germany))
Publication: Advances in Stellar Interferometry. Edited by
Monnier, John D.; Schöller, Markus; Danchi, William
C.. Proceedings of the SPIE, Volume 6268, pp.
62683P (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671542
Bibliographic Code: 2006SPIE.6268E.117B
Abstract
The correction of atmospheric differential piston and instrumental
flexure effects is mandatory for interferometric operation of the LBT
NIR interferometric imaging camera LINC-NIRVANA. The task of the Fringe
and Flexure Tracking System (FFTS) is to detect and correct these
effects in real-time. In the fringe tracking concept that we present,
differential piston information is gathered in the image plane by
analyzing the PSF of a reference star anywhere in the large field of
view of the LBT. We have developed and tested a fast PSF analysis
algorithm that allows to clearly identify differential piston even in
the case of low S/N. We present performance estimates of the algorithm.
Since the performance of the FFTS algorithm has a strong impact on the
overall sky coverage of LINC-NIRVANA, we studied the required limiting
magnitudes of the fringe tracking reference star for different
scenarios. As the FFTS may not necessarily operate on the science
target, but rather uses a suitable reference star at a certain angular
distance to the science target, differences between piston values at the
two positions add to the residual piston of the FFTS. We have dealt with
the question of differential piston angular anisoplanatism and studied a
possible improvement of the isopistonic patch size by the use of
multi-conjugate adaptive optics (MCAO). In its final stage, LINC-NIRVANA
will be equipped with such a system.
Title: The LINC-NIRVANA fringe and flexure tracker:
cryo-ambient mechanical design
Authors: Bertram, Thomas; Baumeister, Harald;
Laun, Werner; Straubmeier, Christian;
Rost, Steffen; Wang, Yeping; Eckart, Andreas
Affiliation: AA(Univ. of Cologne (Germany)), AB(Max Planck
Institute for Astronomy (Germany)), AC(Max Planck
Institute for Astronomy (Germany)), AD(Univ. of
Cologne (Germany)), AE(Univ. of Cologne (Germany)),
AF(Univ. of Cologne (Germany)), AG(Univ. of Cologne
(Germany))
Publication: Advances in Stellar Interferometry. Edited by
Monnier, John D.; Schöller, Markus; Danchi, William
C.. Proceedings of the SPIE, Volume 6268, pp.
62683L (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671378
Bibliographic Code: 2006SPIE.6268E.114B
Abstract
The correction of atmospheric differential piston and instrumental
flexure effects is mandatory for interferometric operation of the LBT
NIR interferometric imaging camera LINC-NIRVANA. The task of the Fringe
and Flexure Tracking System (FFTS) is to detect and correct these
effects in a real-time closed loop. Being a Fizeau-Interferometer, the
LBT provides a large field of view (FoV). The FFTS can make use of the
large FoV and increase the sky coverage of the overall instrument if it
is able to acquire the light of a suitable fringe tracking reference
star within the FoV. For this purpose, the FFTS detector needs to be
moved to the position of the reference star PSF in the curved focal
plane and needs to precisely follow its trajectory as the field rotates.
Sub-pixel (1 pixel = 18.5 micron) positioning accuracy is required over
a travel range of 200mm x 300mm x 70mm. Strong are the constraints
imposed by the need of a cryogenic environment for the moving detector.
We present a mechanical design, in which the Detector Positioning Unit
(DPU) is realized with off-the-shelf micro-positioning stages, which can
be kept at ambient temperature. A moving baffle will prevent the
intrusion of radiation from the ambient temperature environment into the
cryogenic interior of the camera. This baffle consists of two nested
disks, which synchronously follow any derotation - or repositioning
trajectory of the DPU. The detector, its fanout board and a filter wheel
are integrated into a housing that is mounted on top of the DPU and that
protects the FFTS detector from stray light. Long and flexible copper
bands allow heat transfer from the housing to the LINC-NIRVANA heat
exchanger.
Title: Aperture synthesis imaging with the LBT:
reconstruction of diffraction-limited images from
LBT LINC-NIRVANA data using the Richardson-Lucy and
regularized building block method
Authors: Hofmann, Karl-Heinz; Driebe, Thomas;
Heininger, Mathias; Schertl, Dieter; Weigelt, Gerd
Affiliation: AA(Max-Planck-Institut für Radioastronomie
(Germany)), AB(Max-Planck-Institut für
Radioastronomie (Germany)), AC(Max-Planck-Institut
für Radioastronomie (Germany)),
AD(Max-Planck-Institut für Radioastronomie
(Germany)), AE(Max-Planck-Institut für
Radioastronomie (Germany))
Publication: Advances in Stellar Interferometry. Edited by
Monnier, John D.; Schöller, Markus; Danchi, William
C.. Proceedings of the SPIE, Volume 6268, pp.
62683H (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.671535
Bibliographic Code: 2006SPIE.6268E.111H
Abstract
The regularized and space-variant Building Block method allow the
reconstruction of diffraction-limited aperture-synthesis images from
Large Binocular Telescope (LBT) LINC-NIRVANA data. Images with the
diffraction-limited resolution of a 22.8 m single-dish telescope can be
reconstructed if raw images are taken at several different hour angles.
Computer-generated and laboratory LBT interferograms were simulated that
are similar to the data which can be obtained with the LINC-NIRVANA beam
combiner instrument. From the simulated interferograms,
diffraction-limited images were reconstructed with the regularized
Building Block method, which is an extension of the Building Block
method. We compare the Building Block reconstructions to images obtained
with the Richardson-Lucy (RL) method and the Ordered Subsets Expectation
Maximization (OSEM) method. Our image reconstruction studies were
performed with computer-simulated J-band and laboratory H-band raw data
of a galaxy with simulated total magnitudes of J = 16 to 18 and H = 16
to 19, respectively. One of the faintest structures in the images has a
brightness of J~25. The simulated reference stars within the isoplanatic
patch have magnitudes of J = 20 - 21 and H = 19. All three methods are
able to reconstruct diffraction-limited images of similar quality.
Title: Interferometric observations of the galactic center:
LBT and VLTI
Authors: Eckart, Andreas; Schödel, Rainer;
Straubmeier, Christian; Bertram, Thomas;
Pott, Jörg-Uwe; Muzic, Koraljka;
Meyer, Leonhard; Moultaka, Jihane;
Viehmann, Thomas; Rost, Steffen; Herbst, Tom
Affiliation: AA(Univ. of Cologne (Germany)), AB(Univ. of Cologne
(Germany)), AC(Univ. of Cologne (Germany)), AD(Univ.
of Cologne (Germany)), AE(Univ. of Cologne (Germany)
and European Southern Observatory (Germany)),
AF(Univ. of Cologne (Germany)), AG(Univ. of Cologne
(Germany)), AH(Univ. of Cologne (Germany)), AI(Univ.
of Cologne (Germany)), AJ(Univ. of Cologne
(Germany)), AK(Max-Planck-Institut für Astronomie
(Germany))
Publication: Advances in Stellar Interferometry. Edited by
Monnier, John D.; Schöller, Markus; Danchi, William
C.. Proceedings of the SPIE, Volume 6268, pp.
62681J (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.670283
Bibliographic Code: 2006SPIE.6268E..49E
Abstract
Current and future opportunities for interferometric observations of the
Galactic Center in the near- and mid-infrared (NIR/MIR) wavelength
domain are highlighted. Main emphasis is being put on the Large
Binocular Telescope (LBT) and the Very Large Telescope Interferometer
(VLTI). The Galactic Center measurements of stellar orbits and strongly
variable NIR and X-ray emission from Sagittarius A* (SgrA*) at the
center of the Milky Way have provided the strongest evidence so far that
the dark mass concentration at this position is associated with a super
massive black hole. Similar dark mass concentrations seen in many
galactic nuclei are most likely super massive black holes as well. High
angular resolution interferometric observations in the NIR/MIR will
provide key information on the central massive black hole and the
stellar cluster it is embedded in. These observations have already
started: Recent results on the luminous dust enshrowded star IRS3 using
MIDI at the VLTI are presented and future scientific possibilities in
the GC using MIDI at the VLTI in the MIR and GRAVITY in the NIR are
highlighted. As a NIR wide field interferometric imager offering an
angular resolution of about 10 milliarcseconds LINC/NIRVANA at the Large
Binocular Telescope will be an ideal instrument for imaging galactic
nuclei including the center of the Milky Way.
Title: The imaging fringe and flexure tracker of
LINC-NIRVANA: basic opto-mechanical design and
principle of operation
Authors: Straubmeier, Christian; Bertram, Thomas;
Eckart, Andreas; Rost, Steffen; Wang, Yeping;
Herbst, Tom; Ragazzoni, Roberto; Weigelt, Gerd
Affiliation: AA(Univ. of Cologne (Germany)), AB(Univ. of Cologne
(Germany)), AC(Univ. of Cologne (Germany)), AD(Univ.
of Cologne (Germany)), AE(Univ. of Cologne
(Germany)), AF(Max-Planck-Institut für Astronomie
(Germany)), AG(Osservatorio Astrofisico di Arcetri
(Italy)), AH(Max-Planck-Institut für Radioastronomie
(Germany))
Publication: Advances in Stellar Interferometry. Edited by
Monnier, John D.; Schöller, Markus; Danchi, William
C.. Proceedings of the SPIE, Volume 6268, pp.
62681I (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.670160
Bibliographic Code: 2006SPIE.6268E..48S
Abstract
LINC-NIRVANA is the interferometric near-infrared imaging camera for the
Large Binocular Telescope (LBT). Being able to observe at wavelength
bands from J to K (suppported by an adaptive optics system operating at
visible light) LINC-NIRVANA will provide an unique and unprecedented
combination of high angular resolution (~ 9 milliarcseconds at
1.25$,1'<(Bm), wide field of view (~ 100 arcseconds2 at
1.25$,1'<(Bm), and large collecting area (~ 100m2). One of the
major contributions of the 1. Physikalische Institut of the University
of Cologne to this project is the development and provision of the
Fringe and Flexure Tracking System (FFTS). In addition to the single-eye
adaptive optics systems the FFTS is a crucial component to ensure a
time-stable wavefront correction over the full aperture of the
double-eye telescope, a mandatory pre-requisite for interferometric
observations. Using a independent HAWAII 1 detector array at a combined
focus close to the science detector, the Fringe and Flexure Tracking
System analyses the complex two-dimensional interferometric point spread
function (PSF) of a suitably bright reference source at frame rates of
up to several hundred Hertz. By fitting a parameterised theoretical
model PSF to the preprocessed image-data the FFTS determines the amount
of pistonic phase difference and angular misalignment between the
wavefronts of the two optical paths of LINC-NIRVANA. For every exposure
the corrective parameters are derived in real-time and transmitted to a
dedicated piezo-electric fast linear mirror for simple path lengths
adjustments, and/or to the adaptive optics systems of the single-eye
telescopes for more complicated corrections. In this paper we present
the basic concept and currect status of the opto-mechanical design of
the Fringe and Flexure Tracker, the operating principle of the fringe
and flexure tracking loops, and the encouraging result of a laboratory
test of the piston control loop.
Title: The Large Binocular Telescope main axis encoders:
mounting hardware, read heads, and tape installation
Authors: Callahan, S.; Ashby, D.; Hair, T.;
Brynnel, J.; Donovan, S.; Dionies, F.
Affiliation: AA(Large Binocular Telescope Observatory (USA)),
AB(Large Binocular Telescope Observatory (USA)),
AC(Large Binocular Telescope Observatory (USA)),
AD(Large Binocular Telescope Observatory (USA)),
AE(Large Binocular Telescope Observatory (USA)),
AF(Large Binocular Telescope Observatory (USA))
Publication: Ground-based and Airborne Telescopes. Edited by
Stepp, Larry M.. Proceedings of the SPIE, Volume
6267, pp. 62673B (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.670508
Bibliographic Code: 2006SPIE.6267E.109C
Abstract
The Large Binocular Telescope Observatory (LBT) encoded their elevation
and azimuth axis with Farrand Inductosyn tape encoders. The authors
present the unique design requirements to achieve high precision
tracking and pointing. This paper describes the mechanical hardware used
to meet these goals. The telescope elevation axis uses two tapes to
encode 14m diameter tracks machined into the optical support structure.
Each elevation tape is encoded with two custom read heads machined to
fit the surfaces. The read heads are mounted on spring loaded flexures
with rollers to insure consistent alignment of the heads to the tapes
and to allow for radial run out. The azimuth is encoded with two tapes
set end to end. Four custom read heads have been installed on similar
flexures. The tape mounting hardware has been designed to maintain
uniform and constant tension over the lifetime of the tape. We also
describe the equipment and procedures used during installation to insure
uniform tension of the tape in the track.
Title: Exoplanet imaging with the Giant Magellan Telescope
Authors: Angel, Roger; Codona, Johanan L.; Hinz, Phil;
Close, Laird
Affiliation: AA(Steward Observatory, Univ. of Arizona (USA)),
AB(Steward Observatory, Univ. of Arizona (USA)),
AC(Steward Observatory, Univ. of Arizona (USA)),
AD(Steward Observatory, Univ. of Arizona (USA))
Publication: Ground-based and Airborne Telescopes. Edited by
Stepp, Larry M.. Proceedings of the SPIE, Volume
6267, pp. 62672A (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.672251
Bibliographic Code: 2006SPIE.6267E..73A
Abstract
Over the next decade, we can expect that some imaging of extrasolar
planets will be possible with the high-resolution LBT and present 8 m
class telescopes. But it will be limited by sensitivity and contrast
ratio to self-luminous planets of the nearest young stars. When the
Giant Magellan Telescope (GMT) comes on-line, it will have because of
much larger light grasp and sharper PSF, the potential for imaging many
new planets as well as, for the first time, imaging planets of known
msini. It will also be capable of starting atmospheric studies through
spectrophotometry. The full angular resolution of the GMT (that of D=24
m filled aperture) will be exploited with coronagraphy and nulling
interferometry. The new coronagraphic technique of phase apodization
being pioneered at the MMT will enable very high contrast at angular
separations $,1y%(B3$,1';(B/D. To reach the highest contrast levels, the
AO system is being designed not to minimize wavefront error, but to
shape the corrected wavefront so as to cancel speckles in the search
region. Interferometric measurements of complex amplitude in the focal
plane make this possible, regardless of whether the speckles originate
from errors in diffraction or phase. New control algorithms are being
developed to minimize the decorrelation time as well as the intensity of
residual speckles, so that they average out to the smoothest possible
background halo. In this way, detections at 1.65 $,1'<(Bm at the 5$,1'C
(Blevel of planets at 10-8 contrast at 50 mas separation should
be possible. The low background AO system of the GMT, made with its
deformable secondary, will allow also high contrast imaging with high
sensitivity at 5 $,1'<(Bm, down to 100 mas separation.
Title: The Large Binocular Telescope
Authors: Hill, John M.; Green, Richard F.; Slagle, James H.
Affiliation: AA(Univ. of Arizona, Large Binocular Telescope
Observatory (USA)), AB(Univ. of Arizona, Large
Binocular Telescope Observatory (USA)), AC(Univ. of
Arizona, Large Binocular Telescope Observatory
(USA))
Publication: Ground-based and Airborne Telescopes. Edited by
Stepp, Larry M.. Proceedings of the SPIE, Volume
6267, pp. 62670Y (2006). (SPIE Homepage)
Publication Date: 07/2006
Origin: SPIE
Abstract Copyright: (c) 2006: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.669832
Bibliographic Code: 2006SPIE.6267E..31H
Abstract
The Large Binocular Telescope (LBT) Project is a collaboration between
institutions in Arizona, Germany, Italy, Indiana, Minnesota, Ohio and
Virginia. The telescope on Mt. Graham in southeastern Arizona uses two
8.4-meter diameter primary mirrors mounted side-by-side to produce a
collecting area equivalent to an 11.8-meter circular aperture. A unique
feature of LBT is that the light from the two primary mirrors can be
combined to produce phased array imaging of an extended field. This
coherent imaging along with adaptive optics gives the telescope the
diffraction-limited resolution of a 22.65-meter telescope. The first
primary mirror was aluminized in April 2005. First light with a single
primary mirror and a prime focus imager was achieved in October 2005. We
describe here some of the technical challenges met and solved on the way
to First Light. The second of two 8.4-meter borosilicate honeycomb
primary mirrors has been installed in the telescope in October 2005 and
was aluminized in January 2006. Binocular operation with two prime focus
cameras is planned for Fall 2006. The telescope uses two F/15 adaptive
secondaries to correct atmospheric turbulence. The first of these
adaptive mirrors is now being integrated with its electro-mechanics.
Title: Design of the Telemetry Control System for the Large
Binocular Telescope
Authors: de La Peña, M. D.; Axelrod, T.
Publication: Astronomical Data Analysis Software and Systems XV
ASP Conference Series, Vol. 351, Proceedings of the
Conference Held 2-5 October 2005 in San Lorenzo de
El Escorial, Spain. Edited by Carlos Gabriel,
Christophe Arviset, Daniel Ponz, and Enrique Solano.
San Francisco: Astronomical Society of the Pacific,
2006., p.727
Publication Date: 07/2006
Origin: ASP
Bibliographic Code: 2006ASPC..351..727D
Abstract
The Telemetry Control Subsystem (TEL) of the Large Binocular Telescope
(LBT) is responsible for capturing sets of time-sampled telescope
control system data, referred to as streams. These streams can
originate in any of the LBT telescope control subsystems and are
delivered over a dedicated 1 Gbit/s network to a telemetry archive. The
telescope control subsystems are autonomous entities which control
telescope hardware through low-level interfaces (e.g., enclosure, mirror
cell, pointing and mount control, etc.).
The stream type, characterized according to the main associated
subsystem, and the sets of variables which comprise a telemetry stream
are currently pre-defined in a MySQL database. A graphical user
interface developed in Qt provides the functionality which allows the
user to start a pre-defined stream, set the parameters under which the
stream should be initiated, and the option to generate a graphical view
of the data stream. The graphics are handled by MATLAB and its
accompanying GUI builder, GUIDE. The actual data stream is written out
to a series of Hierarchical Data Format (HDF) files; the HDF files serve
as the stream archive which is tracked by the MySQL database.
Title: Application of iterative blind deconvolution to the
reconstruction of LBT LINC-NIRVANA images
Authors: Desiderá, G.; Anconelli, B.; Bertero, M.;
Boccacci, P.; Carbillet, M.
Affiliation: AA(DISI, Università di Genova, via Dodecaneso 35,
16146 Genova, Italy
), AB(DISI, Università di Genova, via Dodecaneso 35, 16146 Genova, Italy), AC(DISI, Università di Genova, via Dodecaneso 35, 16146 Genova, Italy), AD(DISI, Università di Genova, via Dodecaneso 35, 16146 Genova, Italy), AE(Laboratoire Universitaire d'Astrophysique de Nice, UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France)
Publication: Astronomy and Astrophysics, Volume 452, Issue 2,
June III 2006, pp.727-734 (A&A Homepage)
Publication Date: 06/2006
Origin: EDP
Keywords: methods: numerical, techniques: image processing
DOI: 10.1051/0004-6361:20054481
Bibliographic Code: 2006A&A...452..727D
Abstract
Context: .The paper is about methods for multiple image deconvolution
and their application to the reconstruction of the images acquired by
the Fizeau interferometer, denoted LINC-NIRVANA, under development for
the Large Binocular Telescope (LBT). The multiple images of the same
target are obtained with different orientations of the baseline.
Aims: .To propose and develop a blind method for dealing with cases
where no knowledge or very poor knowledge of the point spread functions
(PSF) is available.
Methods: .The approach is an iterative one
where object and PSFs are alternately updated using deconvolution
methods related to the standard Richardson-Lucy method. It is basically
an extension, to the multiple image case, of iterative blind
deconvolution methods proposed in the case of a single image.
Results: .The method is applied to simulated LBT LINC-NIRVANA images and
its limitations are investigated. The algorithm has been implemented in
the module BLI of the software package AIRY (Astronomical Image
Reconstruction in interferometrY), available under request. The
preliminary results we have obtained are promising but an extensive
simulation program is still necessary for a full understanding of the
applicability of the method in the practice of the reconstruction of
LINC-NIRVANA images.
Title: Reduction of boundary effects in multiple image
deconvolution with an application to LBT
LINC-NIRVANA
Authors: Anconelli, B.; Bertero, M.; Boccacci, P.;
Carbillet, M.; Lanteri, H.
Affiliation: AA(DISI, Università di Genova, Via Dodecaneso 35,
16146 Genova, Italy), AB(DISI, Università di Genova,
Via Dodecaneso 35, 16146 Genova, Italy), AC(DISI,
Università di Genova, Via Dodecaneso 35, 16146
Genova, Italy), AD(Laboratoire Universitaire
d'Astrophysique de Nice, UMR 6525, Parc Valrose,
06108 Nice Cedex 02, France), AE(Laboratoire
Universitaire d'Astrophysique de Nice, UMR 6525,
Parc Valrose, 06108 Nice Cedex 02, France)
Publication: Astronomy and Astrophysics, Volume 448, Issue 3,
March IV 2006, pp.1217-1224 (A&A Homepage)
Publication Date: 03/2006
Origin: EDP
Keywords: methods: data analysis, methods: numerical
DOI: 10.1051/0004-6361:20053848
Bibliographic Code: 2006A&A...448.1217A
Abstract
Our approach proposed in a previous paper for the reduction of boundary
effects in the deconvolution of astronomical images by the
Richardson-Lucy method (RLM) is extended here to the problem of multiple
image deconvolution and applied to the reconstruction of the images of
LINC-NIRVANA, the German-Italian beam combiner for the Large Binocular
Telescope (LBT). We investigate the multiple image RLM, its accelerated
version ordered subsets expectation maximization (OSEM), and the
regularized versions of these twomethods. In addition we show how the
approach can be extended to the iterative space reconstruction algorithm
(ISRA), which is an iterative method converging to non-negative least
squares solutions. Numerical simulations indicate that the approach can
provide excellent results with aconsiderable reduction of the boundary
effects.
Title: V723 Cassiopeiae
Authors: Ness, J.-U.; Starrfield, S.; Schwarz, G.;
Vanlandingham, K.; Wagner, R. M.; Lyke, J.;
Woodward, C. E.; Lynch, D. K.; Krautter, J.
Publication: IAU Circ., 8676, 2 (2006). Edited by Green, D. W.
E. (IAUC Homepage)
Publication Date: 02/2006
Origin: CBAT
Objects: V723 Cas
Bibliographic Code: 2006IAUC.8676....2N
Abstract
IAUC 8676 available at Central Bureau for Astronomical Telegrams.
Title: V723 Cassiopeiae
Authors: Ness, J.-U.; Starrfield, S.; Schwarz, G.;
Vanlandingham, K.; Wagner, R. M.; Lyke, J.;
Woodward, C. E.; Lynch, D. K.
Publication: Central Bureau Electronic Telegrams, 404, 1 (2006).
Edited by Green, D. W. E.
Publication Date: 02/2006
Origin: CBAT
Objects: V723 Cas
Bibliographic Code: 2006CBET..404....1N
Abstract
CBET 404 available at Central Bureau for Astronomical Telegrams.
Title: The Future of Astrometric Education
Authors: van Altena, W.; Stavinschi, M.
Affiliation: AA(Yale University, USA.)
Publication: Third International Meeting of Dynamic Astronomy in
Latin America (Eds. Carlos Abad, Ángel Bongiovanni,
& Yaneth Guillén) Revista Mexicana de Astronomía y
Astrofísica (Serie de Conferencias) Vol. 25, pp.
61-62 (2006) (http://www.astroscu.unam.mx/~rmaa/)
(RMxAC Homepage)
Publication Date: 01/2006
Origin: RMXAC
Keywords: Astrometry, Sociology of Astronomy
Abstract Copyright: (C) 2006; Instituto de Astronomía, Universidad
Nacional Autónoma de México
Comment: ISBN: 9703228038
Bibliographic Code: 2006RMxAC..25...61A
Abstract
Astrometry is poised to enter an era of unparalleled growth and
relevance due to the wealth of highly accurate data expected from the
SIM and GAIA space missions. Innovative ground-based telescopes are
planned, such as the LSST, which will provide less precise data, but for
many more stars. The potential for studies of the structure, kinematics
and dynamics of our Galaxy as well as for the physical nature of stars
and the cosmological distance scale is without equal in the history of
astronomy. It is therefore ironic that worldwide it is possible to
obtain an extensive education in astrometry only in St. Petersburg and
Paris and in two years not one course in astrometry will be taught in
the US. Who will ensure the astrometric quality control for the JWT,
SIM, GAIA, LSST, to say nothing about the current large ground-based
facilities, such as the VLT, Gemini, Keck, NOAO, Magellan, LBT, etc.?
We propose a renewal of astrometric education in the universities to
prepare qualified scientists so that the scientific returns from the
investment of billions of dollars in these unique facilities will be
maximized. The funding agencies are providing outstanding facilities.
The universities, national and international observatories and agencies
should acknowledge their responsibility to hire qualified full-time
astrometric scientists to teach students and to supervise existing and
planned astronomical facilities so that quality data will be obtained
and analyzed.
A temporary solution to this problem is proposed in the form of a series
of international summer schools in Astrometry. The Michelson Science
Center of the SIM project will hold an astrometry summer school in 2005
to begin this process. A one-semester syllabus is suggested as a means
of meeting the needs of Astronomy by educating students in astrometric
techniques that might be most valuable for careers associated with
modern astrophysics.
Title: Ground-based direct detection of close-in
extra-solar planets with nulling and high order
adaptive optics
Authors: Langlois, M.; Burrows, A.; Hinz, P.
Affiliation: AA(Laboratoire d'Astophysique de Marseille, 2 place
Le Verrier, 13248 Marseille, France
), AB(Steward Observatory, Tucson, AZ 85719, USA), AC(Steward Observatory, Tucson, AZ 85719, USA)
Publication: Astronomy and Astrophysics, Volume 445, Issue 3,
January III 2006, pp.1143-1149 (A&A Homepage)
Publication Date: 01/2006
Origin: EDP
Keywords: stars: planetary systems, instrumentation:
interferometers, instrumentation: high angular
resolution, instrumentation: adaptive optics
DOI: 10.1051/0004-6361:20042384
Bibliographic Code: 2006A&A...445.1143L
Abstract
Ground-based direct detection of extra-solar planets is very challenging
due to high planet to star brightness contrasts. For giant close-in
planets, such as have been discovered by the radial velocity method,
closer than 0.1 AU, the reflected light is predicted to be fairly high
yielding a contrast ratio ranging from 10-4 to
10-5 at near infra-red wavelengths. In this paper, we
investigate direct detection of reflected light from such planets using
nulling interferometry, and high-order adaptive optics in conjunction
with large double aperture ground-based telescopes. In this
configuration, at least 10-3 suppression of the entire
stellar Airy pattern with small loss of planet flux as close as 0.03
arcsec is achievable. Distinguishing residual starlight from the planet
signal is achieved by using the center of gravity shift method or
multicolor differential imaging. Using these assumptions, we derive
exposure times from a few minutes to several hours for direct detection
of many of the known extra-solar planets with several short-baseline
double aperture telescopes such as the Large Binocular Telescope (LBT),
the Very Large Telescope (VLT) and the Keck Telescope.
Title: Interferometry with the Large Binocular Telescope
Authors: Herbst, T.
Publication: Visions for Infrared Astronomy, Instrumentation,
Mesure, Métrologie vol 6/1-4, 2006. Proc. of the
Conference held in Paris, March 20-22, 2006.
Publisher: Lavoisier, pp.263-269
Publication Date: 00/2006
Origin: AUTHOR
Keywords: large binocular telescope, interferometry, nulling,
Fizeau.
Bibliographic Code: 2006via..conf..263H
Abstract
The Large Binocular Telescope (LBT) will soon be entering science
operations. Designed as a flexible, multipurpose facility, the LBT will
show its greatest strengths as an interferometer. This paper presents an
update on the construction of the telescope, and explains the science
and technology driving the two planned interferometric instruments.
Title: NIR/Optical observations of the GOODS-S field .
Tracing the mass assembly history of galaxies
Authors: Grazian, A.; Fontana, A.; De Santis, C.;
Salimbeni, S.; Nonino, M.; Giallongo, E.;
Gallozzi, S.; Menci, N.; Vanzella, E.; Cristiani, S.
Affiliation: AA( INAF - Osservatorio Astronomico di Roma, Via
Frascati 33, I-0040 Monte Porzio Catone, Roma, Italy
), AB( INAF - Osservatorio Astronomico di Roma, Via Frascati 33, I-0040 Monte Porzio Catone, Roma, Italy ), AC( INAF - Osservatorio Astronomico di Roma, Via Frascati 33, I-0040 Monte Porzio Catone, Roma, Italy ), AD( INAF - Osservatorio Astronomico di Roma, Via Frascati 33, I-0040 Monte Porzio Catone, Roma, Italy ), AE(INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34131, Trieste, Italy.!
), AF( INAF - Osservatorio Astronomico di Roma, Via Frascati 33, I-0040 Monte Porzio Catone, Roma, Italy ), AG( INAF - Osservatorio Astronomico di Roma, Via Frascati 33, I-0040 Monte Porzio Catone, Roma, Italy ), AH( INAF - Osservatorio Astronomico di Roma, Via Frascati 33, I-0040 Monte Porzio Catone, Roma, Italy ), AI(INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34131, Trieste, Italy.), AJ(INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34131, Trieste, Italy.)
Publication: Memorie della Societa Astronomica Italiana
Supplement, v.9, p.301 (2006)
Publication Date: 00/2006
Origin: MmSAI
Keywords: Galaxies:distances and redshift, Galaxies:
evolution, Galaxies: high redshift, Galaxies:
photometry
Abstract Copyright: (c) 2006: SAIt
Bibliographic Code: 2006MSAIS...9..301G
Abstract
The GOODS Survey (Great Observatory Origin Deep Survey) is providing
unprecedented valuable data in the optical-NIR bands to investigate
galaxies up to the extreme redshifts (z$,1$|(B7) over a relatively large
area of the sky. The survey is the result of a combined effort of space
observatories (HST, Spitzer) as well as ground based telescopes (Keck,
VLT). Using this public dataset, and focusing in particular on the VLT
data in the Chandra Deep Field South region, we have produced a high
quality multicolor catalog (from the U to the Ks band) for $,1$|(B14000
galaxies over an area of 135 sq. arcmin, complete to both Z(AB)=26 and
Ks(AB)=24 magnitudes. To optimally match the HST high resolution images
with the ground-based ones, we have designed a software for high
precision photometry (ConvPhot) and an SQL database to manage properly
this Multi Wavelength Catalog. This survey will give a uniquely
comprehensive history of galaxies, from early epochs to the relatively
recent past: at this purpose, we are focusing the attention on the
Distant Red Galaxy (DRG) population at z$,1$|(B1-3 to shed light on
their still unclear nature and to avoid cosmic variance thanks to the
large and deep area investigated. We will finally discuss how this work
is useful to prepare future surveys with the LBC instrument at the LBT
telescope.
Title: STREGA@VST: Structure and Evolution of the Galaxy .
Authors: Marconi, M.; Musella, I.; Ripepi, V.;
De Martino, D.; Silvotti, R.; Capaccioli, M.;
Cappellaro, E.; Cignoni, M.; Dall'Ora, M.;
Di Criscienzo, M.; Iodice, E.; Ruoppo, A.;
Bono, G.; Brocato, E.; Caputo, F.;
Carollo, D.; Castellani, M.; Castellani, V.;
Cioni, M. R.; Degli Innocenti, S.; Momany, Y.;
Monelli, M.; Piotto, G.; Prada Moroni, P. G.;
Raimondo, G.
Affiliation: AA( Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Capodimonte, Via Moiariello 16,
I-80131 Napoli, Italy
), AB( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AC( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AD( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AE( Istituto Nazionale di Astrofisica - Osservat!
orio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AF( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ; Università``Federico II'' di Napoli, Italy), AG( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AH( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AI( Istituto Nazi!
onale di
Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AJ( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ; Università``Tor Vergata'' di Roma, Italy), AK( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ), AL( Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli, Italy ; Università``Federico II'' di Napoli, Italy), AM(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Roma, Italy), AN(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Collurania - Teramo, Italy), AO(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Roma, Italy), AP(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Torino, Italy), AQ(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Roma, Italy), AR(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Roma, Italy), AS(Institute for Astronomy - Royal Observatory, Edinburgh, United Kingdom), AT(Universitàdi Pisa, Italy), AU(Universitàdi Padova, Italy), AV(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Roma, Italy), AW(Universitàdi Padova, Italy), AX(Universitàdi Pisa, Italy), AY(Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Collurania - Teramo, It!
aly)
Publication: Memorie della Societa Astronomica Italiana
Supplement, v.9, p.253 (2006)
Publication Date: 00/2006
Origin: MmSAI
Keywords: Stars: variables: RR Lyr, Stars: white dwarfs,
Stars: cataclysmic variables, Galaxy: evolution,
Galaxy: structure
Abstract Copyright: (c) 2006: SAIt
Bibliographic Code: 2006MSAIS...9..253M
Abstract
In this article we present the survey STREGA, that has been proposed as
part of the VST GTO (VLT Survey Telescope Guarantee Time of Observation)
that will be given to the INAF-OAC in exchange for the construction of
the telescope (see Alcalàet al., this volume). This survey will
cover an area of about 150 sq. deg., searching for the southern portion
of the Fornax stream, also allowing to study the properties of Disk and
Halo White Dwarfs and interacting binaries in different fields at
increasing galactic latitudes and to provide an ideal database for star
counts and for the comparison with Galactic model predictions. The final
aim is to constrain the structure and the evolutionary properties of the
Milky Way. For the Fornax Stream this proposal is coordinated with a LBT
Science Verification Pilot Project (P.I.: G. Bono).
Title: Future prospects for AGN and galaxy surveys with the
LBT Large Binocular Camera
Authors: Grazian, A.
Affiliation: Istituto Nazionale di Astrofisica - Osservatorio
Astronomico di Roma, Via Frascati 33, I-00040 Monte
Porzio Catone, Italy
Publication: Memorie della Societa Astronomica Italiana, v.77,
p.720 (2006)
Publication Date: 00/2006
Origin: MmSAI
Keywords: Instrumentation: detectors, Telescopes, Surveys,
quasars: general, Galaxies: high-redshift,
Cosmology: observations
Abstract Copyright: (c) 2006: SAIt
Bibliographic Code: 2006MmSAI..77..720G
Abstract
The Large Binocular Camera (LBC) is a wide field of view instrument at
the prime focus of the twin 8.4 meter Large Binocular Telescope. The
Blue channel of LBC has been already installed at the telescope and the
first light images have been successfully obtained on October 12th,
2005. LBC is able to provide faint images of the sky down to the level
of the Hubble Deep Fields, but in an area that is 150 times larger. A
number of high-quality scientific programs requiring extremely deep
images in the near UV wavelength are highlighted, which become feasible
with this powerful instrument.
Title: High-resolution image reconstruction: the case of
the Large Binocular Telescope (LBT)
Authors: Bertero, M.; Anconelli, B.; Boccacci, P.;
Desiderà, G.; Carbillet, M.; Lanteri, H.
Affiliation: AA(DISI $,1rs(B Università di Genova, Via Dodecaneso 35,
16146 Genova, Italy), AB(DISI $,1rs(B Università di
Genova, Via Dodecaneso 35, 16146 Genova, Italy),
AC(DISI $,1rs(B Università di Genova, Via Dodecaneso 35,
16146 Genova, Italy), AD(DISI $,1rs(B Università di
Genova, Via Dodecaneso 35, 16146 Genova, Italy),
AE(DISI $,1rs(B Università di Genova, Via Dodecaneso 35,
16146 Genova, Italy), AF(LUAN $,1rs(B Université de Nice,
UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France)
Publication: EAS Publications Series, Volume 22, 2006, pp.35-67
Publication Date: 00/2006
Origin: EDP
DOI: 10.1051/eas:2006124
Bibliographic Code: 2006EAS....22...35B
Abstract
In this paper we give a survey of the methods we have developed for
multiple image deconvolution, with application to the reconstruction of
the images of the Large Binocular Telescope (LBT). We first describe the
main features of LBT and of the Fizeau interferometer, denoted
LINC-NIRVANA, that will be one of the basic instruments of the
telescope. It will allow to reach the resolution of a 22.8 m mirror by
combining different images taken with different orientations of the
baseline. Next we discuss the problem of multiple image deconvolution,
that is crucial for obtaining a unique high-resolution image from the
multiple images provided by LINC-NIRVANA. We present the state-of-the
art of the methods based on the Richardson-Lucy (RL) approach and we
discuss topics such as computational efficiency, correction of boundary
effects and super-resolution. Then, in the perspective of going beyond
RL, we extend to the problem of multiple image deconvolution the split
gradient method (SGM) that is a general approach to the design of
iterative methods for the constrained minimization of regularized
functionals. Finally we present an application of SGM to the regularized
reconstruction of objects with high-dynamic range. The different methods
are illustrated with examples taken from the many numerical experiments
we performed on this problem.
Title: Development of relative thermal stress index (RTSI)
for Monitoring and Management of Dry Deciduous
Ecosystem
Authors: Gupta, R. K.; Vijayan, D.
Publication: 36th COSPAR Scientific Assembly. Held 16 - 23 July
2006, in Beijing, China. Meeting abstract from the
CDROM, #295
Publication Date: 00/2006
Origin: ADS
Bibliographic Code: 2006cosp...36..295G
Abstract
Gir wildlife sanctuary located between 20 r 57 to 21 r 20 N and 70 r 28
to 71 r 13 E is the last home of Asiatic lions Its biodiversity
comprises of 450 recorded flowering plant species 32 species of mammals
26 species of reptiles about 300 species of birds and more than 2000
species of insects As per 1995 census it has 304 lions and 268 leopards
The movement of wildlife to thermally comfortable zones to reduce stress
conditions forces the changes in management plan with reference to
change in localized water demand This necessitates the use of space
based thermal data available from AVHRR MODIS etc to monitor temperature
of Gir-ecosystem for meso-scale level operational utility As the time
scale of the variability of NDVI parameter is much higher than that for
lower boundary temperature LBT the dense patch in riverine forest having
highest NDVI value would not experience change in its vigour with the
change in the season NDVI value of such patch would be near invariant
over the year and temperature of this pixel could serve as reference
temperature for developing the concept of relative thermal stress index
RTSI which is defined as RTSI T p -T r T max -T r wherein T r T max and
T p refer to LBT over the maximum NDVI reference point maximum LBT
observed in the Gir ecosystem and the temperature of the pixel in the
image respectively RTSI images were computed from AVHRR images for
post-monsoon leaf-shedded and summer seasons Scatter plot between RTSI
and NDVI for summer seasons
Title: High-Resolution with Large Ground-Based Optical/IR
Telescopes
Authors: Wittkowski, M.; Glindemann, A.; Paresce, F.
Publication: Future Directions in High Resolution Astronomy: The
10th Anniversary of the VLBA, ASP Conference
Proceedings, Vol. 340. Edited by J. Romney and M.
Reid. San Francisco: Astronomical Society of the
Pacific, 2005., p.626
Publication Date: 12/2005
Origin: ASP
Bibliographic Code: 2005ASPC..340..626G
Abstract
The Keck Interferometer on Mauna Kea and ESO's Very Large Telescope
Interferometer (VLTI) on Cerro Paranal (2635 m) in Northern Chile both
saw first fringes in 2001. In the meantime, MIDI, the mid-infrared
science instrument of the VLTI, also had first fringes. Using the VLTI
test siderostats and the VLTI near-infrared commissioning instrument
VINCI, 300 hours of shared-risk science programs were executed. A few
years from now, the Large Binocular Telescope (LBT) in Arizona will be
the third large telescope interferometer, providing a large field of
view by using a Fizeau beam combination. Here, we compare the general
concepts of these three interferometers, and describe the VLTI in detail
discussing the layout of the interferometer, its current status, and the
general philosophy as a facility observatory.
Title: Reconstruction of aperture-synthesis images from LBT
LINC-NIRVANA data using the Richardson-Lucy and
space-variant Building Block method
Authors: Hofmann, K.-H.; Driebe, T.; Heininger, M.;
Schertl, D.; Weigelt, G.
Affiliation: AA(Max-Planck-Institut für Radioastronomie (MPIfR),
Auf dem Hügel 69, 53121 Bonn, Germany
), AB(Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany), AC(Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany), AD(Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany), AE(Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany)
Publication: Astronomy and Astrophysics, Volume 444, Issue 3,
December IV 2005, pp.983-993 (A&A Homepage)
Publication Date: 12/2005
Origin: EDP
Keywords: instrumentation: interferometers, instrumentation:
high angular resolution, techniques: image
processing, techniques: high angular resolution,
techniques: miscellaneous
DOI: 10.1051/0004-6361:20053480
Bibliographic Code: 2005A&A...444..983H
Abstract
We present a new method, the regularized and space-variant Building
Block method, which is able to reconstruct diffraction-limited
aperture-synthesis images from Large Binocular Telescope (LBT)
LINC-NIRVANA data. Images with the diffraction-limited resolution of a
22.8 m single-dish telescope can be derived if raw images are taken at
several different hour angles. We simulated computer-generated and
laboratory LBT interferograms that are similar to the data which can be
obtained with the LINC-NIRVANA beam combiner instrument. From the
simulated data, diffraction-limited images were reconstructed with the
regularized Building Block method, which is an extension of the Building
Block method (Hofmann & Weigelt 1993, A&A, 278, 328). We compare
the Building Block reconstructions to images obtained with the
Richardson-Lucy (RL) method (Richardson 1972, J. Opt. Soc. Am., 62, 55;
Lucy 1974, AJ, 79, 745) and the Ordered Subsets Expectation Maximization
(OSEM) method (Hudson & Larkin 1994, IEEE Trans. Med. Imag., 13,
601; Bertero & Boccacci 2000, A&AS, 144, 181). Our image
reconstruction studies were performed with computer-simulated J-band and
laboratory H-band raw data of a galaxy with simulated total magnitudes
of J = 16m to 18m and H = 16m to 19^m,
respectively. One of the faintest structures in the images has a
brightness of J $,1$|(B 25^m. The simulated reference stars within the
isoplanatic patch have magnitudes of J = 20^m{-}21m and H =
19^m. All three methods are able to reconstruct diffraction-limited
images with almost the same quality. Furthermore, raw data with
space-variant point spread functions were simulated, and
diffraction-limited images were reconstructed using the space-variant
version of the Building Block method.
Title: Signatures of Planets in Spatially Resolved Debris
Disks
Authors: Moro-Martin, Amaya
Publication: Proceedings of the Miniworkshop on Nearby Resolved
Debris Disks. October 19-20, 2005. Space Telescope
Science Institute, Baltimore, MD, USA. Edited by
Inga Kamp, Margaret Meixner, p.26
Publication Date: 10/2005
Origin: AUTHOR
Bibliographic Code: 2005nrdd.conf...26M
Abstract
The presence of debris disks around many main sequence stars indicate
that plantesimal formation is a common by-product of the star formation
process. In systems where massive planets are located interior to the
dust-producing planetesimal region, the gravitational interaction of the
dust particles with the planet can create structure in the dust disk.
Because this structure is sensitive to long period planets,
complementing a parameter space not covered by radial velocity and
transit surveys, its study can help us learn about the diversity of
planetary systems. In anticipation of future high-resolution
high-sensitivity observations of spatially resolved debris disks with
e.g. ALMA, LBT, SAFIR, TPF and JWST, we numerically calculate the 3-D
equilibrium spatial density distributions of dust disks originated by a
belt of planetesimals similar to the Kuiper Belt (KB) in the presence of
interior giant planets in different planetary configurations (with
planet masses ranging from 1-10 MJup in circular orbits with
semimajor axis between 1-30 AU). For each of these modeled disks we use
a 3-D radiative transfer code to obtain their brightness density
distributions at different wavelengths that will help us to interpret
future observations of these dusty ``fingerprints'' in terms of
planetary architecture.
Title: The Future of Astrometric Education
Authors: van Altena, W.; Stavinschi, M.
Publication: Astrometry in the Age of the Next Generation of
Large Telescopes, ASP Conference Series, Vol. 338,
Proceedings of a meeting held 18-20 October 2004 at
Lowell Observatory, Flagstaff, Arizona, USA. Edited
by P. Kenneth Seidelmann and Alice K. B. Monet. San
Francisco: Astronomical Society of the Pacific,
2005., p.311
Publication Date: 10/2005
Origin: ASP
Bibliographic Code: 2005ASPC..338..311V
Abstract
Astrometry is poised to enter an era of unparalleled growth and
relevance due to the wealth of highly accurate data expected from the
SIM and GAIA space missions. Innovative ground-based telescopes, such as
the LSST, are planned which will provide less precise data, but for many
more stars. The potential for studies of the structure, kinematics and
dynamics of our Galaxy as well as for the physical nature of stars and
the cosmological distance scale is without equal in the history of
astronomy. It is therefore ironic that in two years not one course in
astrometry will be taught in the US, leaving all astrometric education
to Europe, China and Latin America. Who will ensure the astrometric
quality control for the JWT, SIM, GAIA, LSST, to say nothing about the
current large ground-based facilities, such as the VLT, Gemini, Keck,
NOAO, Magellan, LBT, etc.? Hipparcos and the HST were astrometric
successes due only to the dedicated work of specialists in astrometry
who fought to maintain the astrometric characteristics of those
satellites and their data pipelines.
We propose a renewal of astrometric education in the universities to
prepare qualified scientists so that the scientific returns from the
investment of billions of dollars in these unique facilities will be
maximized. The funding agencies are providing outstanding facilities.
The universities, national and international observatories and agencies
should acknowledge their responsibility to hire qualified full-time
astrometric scientists to teach students, and to supervise existing and
planned astronomical facilities so that quality data will be obtained
and analyzed.
A temporary solution to this problem is proposed in the form of a series
of international summer schools in Astrometry. The Michelson Science
Center of the SIM project has offered to hold an astrometry summer
school in 2005 to begin this process. A one-semester syllabus is
suggested as a means of meeting the needs of Astronomy by educating
students in astrometric techniques that might be most valuable for
careers associated with modern astrophysics.
Title: T-spheres as a limit of Lemaitre-Tolman-Bondi
solutions
Authors: Zaslavskii, O. B.
Publication: eprint arXiv:gr-qc/0509043
Publication Date: 09/2005
Origin: ARXIV
Comment: 6 pages. 1 Reference added. To appear in Phys. Rev.
D; Phys.Rev. D72 (2005) 067501
Bibliographic Code: 2005gr.qc.....9043Z
Abstract
In the Tolman model there exist two quite different branches of
solutions - generic Lemaitre-Tolman-Bondi (LTB) ones and T-spheres as a
special case. We show that, nonetheless, T-spheres can be obtained as a
limit of the class of LTB solutions having no origin and extending to
infinity with the areal radius approaching constant. It is shown that
all singularities of T-models are inherited from those of corresponding
LBT solutions. In doing so, the disc type singularity of a T-sphere is
the analog of shell-crossing.
Title: Nulling interferometry and adaptive optics control
system optimization
Authors: Ferrario, Damien; Wildi, François
Affiliation: AA(West Switzerland Univ. of Applied Sciences
(Switzerland)), AB(West Switzerland Univ. of Applied
Sciences (Switzerland) and Steward Observatory
(USA))
Publication: Techniques and Instrumentation for Detection of
Exoplanets II. Edited by Coulter, Daniel R.
Proceedings of the SPIE, Volume 5905, pp. 237-248
(2005). (SPIE Homepage)
Publication Date: 08/2005
Origin: SPIE
Abstract Copyright: (c) 2005: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.617850
Bibliographic Code: 2005SPIE.5905..237F
Abstract
We present a study of the LBT nulling interferometer (LBTI) performance
considered from the control systems point of view. Focusing first on the
fast path length corrector controller within the LBTI, we show that a
simple modification of the controller algorithm reduces the modal
tracking error by 50% or more depending on the system dynamics. WE show
that this translates into a null depth improvement by a factor larger
than 5. Next, we consider coupling the LBTI real-time controller to that
of the AO to take advantage of the high order information that is
available on the LBTI phase sensor and we show that here again, the
global performance can be improved, albeit more modestly by 20%-30%.
Title: The Fringe and Flexure Tracking System for the LBT
interferometric camera LINC-NIRVANA.
Authors: Bertram, T.; Straubmeier, C.; Rost, S.; Eckart, A.
Publication: Astron. Nachr., 326, 560-561 (2005) (AN Homepage)
Publication Date: 08/2005
Origin: SIMBAD
Bibliographic Code: 2005AN....326..560B
Abstract
Not Available
Title: PMAS: The Potsdam Multi-Aperture Spectrophotometer.
I. Design, Manufacture, and Performance
Authors: Roth, Martin M.; Kelz, Andreas;
Fechner, Thomas; Hahn, Thomas;
Bauer, Svend-Marian; Becker, Thomas;
Böhm, Petra; Christensen, Lise; Dionies, Frank;
Paschke, Jens; Popow, Emil; Wolter, Dieter;
Schmoll, Jürgen; Laux, Uwe; Altmann, Werner
Affiliation: AA(Visiting Astronomer, German-Spanish Astronomical
Centre, Calar Alto, jointly operated by the
Max-Planck-Institute for Astronomy, Heidelberg, with
the Spanish National Commission for Astronomy.;
Visiting Astronomer, Special Astrophysical
Observatory, Selentchuk, Russia.), AB(Visiting
Astronomer, German-Spanish Astronomical Centre,
Calar Alto, jointly operated by the
Max-Planck-Institute for Astronomy, Heidelberg, with
the Spanish National Commission for Astronomy.),
AC(), AD(), AE(), AF(Visiting Astronomer,
German-Spanish Astronomical Centre, Calar Alto,
jointly operated by the Max-Planck-Institute for
Astronomy, Heidelberg, with the Spanish National
Commission for Astronomy.; Visiting Astronomer,
Special Astrophysical Observatory, Selentchuk,
Russia.), AG(Visiting Astronomer, German-Spanish
Astronomical Centre, Calar Alto, jointly operated by
the Max-Planck-Institute for Astronomy, Heidelberg,
with the Spanish National Commission for
Astronomy.), AH(Visiting Astronomer, German-Spanish
Astronomical Centre, Calar Alto, jointly operated by
the Max-Planck-Institute for Astronomy, Heidelberg,
with the Spanish National Commission for
Astronomy.), AI(Astrophysikalisches Institut
Potsdam, An der Sternwarte 16, D-14482 Potsdam,
Germany;
), AJ(Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany; ), AK(Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany; ), AL(Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany; ), AM(Astronomical Instrument Group, Department of Physics, University of Durham, Rochester Building, South Road, Durham DH1 3LE, UK), AN(Thüringer Landessternwarte Tautenburg, Sternwar!
te 5, Tautenburg D-07778, Germany), AO(Konstruktionsbüro Altmann, Passau, Germany)
Publication: The Publications of the Astronomical Society of the
Pacific, Volume 117, Issue 832, pp. 620-642. (PASP
Homepage)
Publication Date: 06/2005
Origin: UCP
PASP Keywords: Instrumentation: Spectrographs, Techniques:
Spectroscopic
Abstract Copyright: (c) 2005: The Astronomical Society of the Pacific
DOI: 10.1086/429877
Bibliographic Code: 2005PASP..117..620R
Abstract
We describe the design, manufacture, commissioning, and performance of
PMAS, the Potsdam Multi-Aperture Spectrophotometer. PMAS is a dedicated
integral field spectrophotometer optimized to cover the optical
wavelength regime of 0.35-1 $,1'<(Bm. It is based on the lens array-fiber
bundle principle of operation. The instrument employs an all-refractive
fiber spectrograph, built with CaF2 optics, to provide good
transmission and high image quality over the entire nominal wavelength
range. A set of user-selectable reflective gratings provides low to
medium spectral resolution of approximately 1.5, 3.2, and 7 Å in
first order, depending on the groove density (1200, 600, 300 grooves
mm-1). While the standard integral field unit (IFU) uses a
16×16 element lens array, which provides seeing-limited sampling
in a relatively small field of view (FOV) in one of three magnifications
(8" × 8", 12" × 12", or 16" × 16"), a recently
retrofitted bare fiber bundle IFU (PPak: PMAS fiber pack) expands the
FOV to a hexagonal area with a footprint of 65" × 74". Other
special features include a cryogenic CCD camera for field acquisition
and guiding, a nod-shuffle mode for beam switching and improved sky
background subtraction, and a scanning Fabry-Pérot etalon in
combination with the standard IFU (PYTHEAS mode). PMAS was initially
designed and built as an experimental traveling instrument with optical
interfaces to various telescopes (Calar Alto 3.5 m, ESO VLT, LBT). It is
offered as a common-user instrument at Calar Alto under contract to MPIA
Heidelberg since 2002.
Title: Restoration of interferometric images. III.
Efficient Richardson-Lucy methods for LINC-NIRVANA
data reduction
Authors: Anconelli, B.; Bertero, M.; Boccacci, P.;
Carbillet, M.; Lanteri, H.
Affiliation: AA(INFM and DISI, Universitàdi Genova, via
Dodecaneso 35, 16146 Genova, Italy), AB(INFM and
DISI, Universitàdi Genova, via Dodecaneso 35, 16146
Genova, Italy
), AC(INFM and DISI, Universitàdi Genova, via Dodecaneso 35, 16146 Genova, Italy), AD(Laboratoire Universitaire d'Astrophysique de Nice, UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France), AE(Laboratoire Universitaire d'Astrophysique de Nice, UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France)
Publication: Astronomy and Astrophysics, v.430, p.731-738 (2005)
(A&A Homepage)
Publication Date: 02/2005
Origin: A&A
A&A Keywords: techniques: image processing, techniques:
interferometric
DOI: 10.1051/0004-6361:20041493
Bibliographic Code: 2005A&A...430..731A
Abstract
In previous papers we proposed methods and software for the restoration
of images provided by Fizeau interferometers such as LINC-NIRVANA (LN),
the German-Italian beam combiner for the Large Binocular Telescope
(LBT). It will provide multiple images of the same target corresponding
to different orientations of the baseline. Therefore LN will require
routinely the use of multiple-image deconvolution methods in order to
produce a unique high-resolution image. As a consequence of the
complexity of astronomical images, two kinds of methods will be
required: first a quick-look method, namely a method that is
computationally efficient, allowing a rapid overview and identification
of the object being observed; second an ad hoc method designed for that
particular object and as accurate as possible. In this paper we
investigate the possibility of using Richardson-Lucy-like (RL-like)
methods, namely methods designed for the maximization of the likelihood
function in the case of Poisson noise, as possible quick-look methods.
To this purpose we propose new techniques for accelerating the Ordered
Subsets - Expectation Maximization (OS-EM) method, investigated in our
previous papers; moreover, we analyze approaches based on the fusion of
the multiple images into a single one, so that one can use single-image
deconvolution methods which are presumably more efficient than the
multiple-image ones. The results are encouraging and all the methods
proposed in this paper have been implemented in our software package
AIRY.
Title: PEPSI, the High-Resolution Optical-IR Spectrograph
for the LBT
Authors: Andersen, Michael; Strassmeier, Klaus;
Hoffman, Axel; Woche, Manfred; Spano, Paolo
Publication: High Resolution Infrared Spectroscopy in Astronomy,
Proceedings of an ESO Workshop held at Garching,
Germany, 18-21 November 2003. Edited by H.U. Käufl,
R. Siebenmorgen, and A. Moorwood. Garching,
Germany, 2005., pp. 57-61
Publication Date: 00/2005
Origin: AUTHOR
DOI: 10.1007/10995082_7
Bibliographic Code: 2005hris.conf...57A
Abstract
PEPSI is a high resolution fibre feed optical-IR polarimetric echelle
spectrograph for the Large Binocular Telescope (LBT). PEPSI utilizes the
two 8.4m LBT apertures to simultaneously record four polarization states
at a resolution of 120.000. The extension of the coverage towards the IR
is mainly motivated by the larger Zeeman splitting of IR lines, which
would allow to study weaker/fainter magnetic structures on stars. The
two optical arms, which also have an integral light mode with R up to
300.000, are under construction, while the IR arm is being designed.
Title: A Web-based Clearing-house for Community Telescope
Information and Access
Authors: Garmany, C. D.; Boroson, T. A.
Affiliation: AA(NOAO), AB(NOAO)
Publication: American Astronomical Society Meeting 205, #48.08;
Bulletin of the American Astronomical Society, Vol.
36, p.1416
Publication Date: 12/2004
Origin: AAS
Abstract Copyright: (c) 2004: American Astronomical Society
Bibliographic Code: 2004AAS...205.4808G
Abstract
Where can one find information on all available community telescopes and
their instrumentation? With the growth of a very diverse set of
ground-based O/IR telescopes and instruments there is an increasing need
for corresponding information on these facilities, as has been pointed
out by the 2nd community workshop on the ground-based O/IR system (May
2004). In response, NOAO has agreed to develop a web site for the
community that summarizes all publicly available observing opportunities
and acts as a clearing -house for information.
While much of the information is currently available on the web, it
requires consolidation. Observing opportunities include not only those
scheduled through NOAO, but other facilities as well. In particular,
PREST (Program for Research and Education with Small Telescopes), a new
NSF initiative, will provide community access to smaller (< 2.5 m)
telescopes . We envision a web site that includes NOAO facilities, the
TSIP program (which provides public time on Keck, HET, MMT, Magellan,
LBT), and other telescopes giving public access through NOAO: WIYN,
SOAR, SMARTS. Facilities that provide public access but not through
NOAO, will also be included. The site should include time available, how
and when to apply, instrument and detector capabilities, selection
criteria, typical weather, lodging accommodations, and technical
assistance or training available at the telescope. Also, feedback from
observers on the performance of the facilities will be made available to
potential proposers.
As we develop this site, we welcome input from the astronomical
community on how to make it most useful to astronomers.
Title: The fringe and flexure tracking system for
LINC-NIRVANA: basic design and principle of
operation
Authors: Straubmeier, Christian; Bertram, Thomas;
Eckart, Andreas; Wang, Yibing; Zealouk, Lahbib;
Herbst, Thomas M.; Andersen, David R.;
Ragazzoni, Roberto; Weigelt, Gerd P.
Publication: New Frontiers in Stellar Interferometry, Proceedings
of SPIE Volume 5491. Edited by Wesley A. Traub.
Bellingham, WA: The International Society for
Optical Engineering, 2004., p.1486 (SPIE Homepage)
Publication Date: 10/2004
Origin: ADS
Bibliographic Code: 2004SPIE.5491.1486S
Abstract
LINC-NIRVANA is the interferometric near-infrared imaging camera for the
Large Binocular Telescope (LBT). Operating at JHK bands LINC-NIRVANA
will provide an unique and unprecedented combination of high angular
resolution (~9 milliarcseconds at 1.25 $,1'<(Bm), wide field of view (~100
arcseconds2 at 1.25 $,1'<(Bm), and large collecting area (~100 m2). One of
the major contributions of the I. Physikalische Institut of the
University of Cologne to this project is the development of the Fringe
and Flexure Tracking System (FFTS). In close cooperation with the
Adaptive Optics systems of LINC-NIRVANA the FFTS is a fundamental
component to ensure a complete and time-stable wavefront correction at
the position of the science detector in order to allow for long
integration times at interferometric angular resolutions. Using a
dedicated near-infrared detector array at a combined focus close to the
science detector, the Fringe and Flexure Tracking System analyses the
interferometric point spread function (PSF) of a suitably bright
reference source at frame rates of several hundred Hertz up to 1 kHz. By
fitting a parameterized theoretical model PSF to the preprocessed
image-data the FFTS determines the amount of pistonic phase difference
and the amount of an angular misalignment between the wavefronts of the
two optical paths of LINC-NIRVANA. For every exposure the correcting
parameters are derived in real-time and transmitted to the respective
control electronics, or the Adaptive Optics systems of the single-eye
telescopes, which will adjust their optical elements accordingly. In
this paper we present the opto-mechanical hardware design, the principle
of operation of the software control algorithms, and the results of
first numerical simulations and laboratory experiments of the
performance of this Fringe and Flexure Tracking System.
Title: The LINC-NIRVANA fringe and flexure tracking system:
differential piston simulation and detection
Authors: Bertram, Thomas; Andersen, David R.;
Arcidiacono, Carmelo; Straubmeier, Christian;
Eckart, Andreas; Beckmann, Udo; Herbst, Thomas M.
Publication: New Frontiers in Stellar Interferometry, Proceedings
of SPIE Volume 5491. Edited by Wesley A. Traub.
Bellingham, WA: The International Society for
Optical Engineering, 2004., p.1454 (SPIE Homepage)
Publication Date: 10/2004
Origin: ADS
Bibliographic Code: 2004SPIE.5491.1454B
Abstract
The correction of atmospherical differential piston and instrumental
flexure effects is mandatory for full interferometric performance of the
LBT NIR interferometric imaging camera LINC-NIRVANA. This is the task of
the Fringe and Flexure Tracking System (FFTS), which is part of the
contribution of the I. Physikalische Institut of the University of
Cologne to the project. Differential piston and flexure effects will be
detected and corrected in a real-time closed loop by analyzing the PSF
of a guide star at a frequency of up to several hundred Hz. Numerous
critical design parameters for both FFTS hardware and control loop have
to be derived from simulations. Detailed knowledge of the special shape
of the LBT interferometric PSF as a function of a variety of parameters
is required to design the fringe tracking control loop. In this paper we
will show the results of our software that allows us to generate
polychromatic interferometric PSFs for a number of different scenarios.
Our fringe detection algorithm is based on an analytic model which is
fitted to the acquired PSF. We present the results of the evaluation of
the algorithm in terms of speed and residual piston, as well as the
first successful implementation of the algorithm in a closed loop
system. Simulations of the time evolution of differential piston have
been performed in order to investigate necessary correction frequencies
and the variation of differential piston across the usable field of
view. These simulations are based on the Layer Oriented Adaptive Optics
performance simulator "LOST" of the Osservatorio Astriofisico di
Arcetri.
Title: The fringe and flexure tracking detector of the LBT
LINC-NIRVANA beam-combiner instrument
Authors: Beckmann, Udo; Behrend, Jan;
Bohnhardt, Hermann; Connot, Claus;
Driebe, Thomas M.; Heininger, Matthias;
Herbst, Thomas M.; Hofmann, Karl-Heinz;
Nussbaum, Edmund; Schertl, Dieter;
Solscheid, Walter; Straubmeier, Christian;
Weigelt, Gerd P.
Publication: New Frontiers in Stellar Interferometry, Proceedings
of SPIE Volume 5491. Edited by Wesley A. Traub.
Bellingham, WA: The International Society for
Optical Engineering, 2004., p.1445 (SPIE Homepage)
Publication Date: 10/2004
Origin: ADS
Bibliographic Code: 2004SPIE.5491.1445B
Abstract
LINC-NIRVANA is a near-infrared (1-2.4 micron) beam-combiner instrument
for the Large Binocular Telescope (LBT). LINC-NIRVANA is being built by
a consortium of groups at the Max-Planck-Institut fur Astronomie in
Heidelberg, the Osservatorio Astrofisico di Arcetri in Florence, the
Universitat zu Koln, and the Max-Planck-Institut fur Radioastronomie in
Bonn. The MPI fur Radioastronomie is responsible for the near-infrared
detector for the fringe and flexure tracking system (FFTS). We describe
the design and construction of the detector control electronics as well
as the first laboratory measurements of performance parameters of the
NIR detector for the fringe and flexure tracking system of the LBT
LINC-NIRVANA instrument. This detector has to record LBT interferograms
of suitable reference stars in the FOV at a frame rate of the order of
200 frames per second using, for example, 32 × 32-pixel subframes.
Moreover, special noise reduction techniques have to be applied. The
fringe-tracker interferograms are required for monitoring and
closed-loop correction of the atmospheric optical path difference of the
two LBT wavefronts (see C. Straubmeier et al., "A fringe and flexure
tracking system for LINC-NIRVANA: basic design and principle of
operation"). We will describe our laboratory measurements of maximum
frame rate, readout noise, photometric stability, and other important
parameters together with first measurements of laboratory simulations of
LBT interferograms.
Title: Deconvolution methods for LINC/NIRVANA data
reduction
Authors: Anconelli, Barbara; Bertero, Mario;
Boccacci, Patrizia; Carbillet, Marcel;
Lanteri, Henri; Correia, Serge
Publication: New Frontiers in Stellar Interferometry, Proceedings
of SPIE Volume 5491. Edited by Wesley A. Traub.
Bellingham, WA: The International Society for
Optical Engineering, 2004., p.932 (SPIE Homepage)
Publication Date: 10/2004
Origin: ADS
Bibliographic Code: 2004SPIE.5491..932A
Abstract
LINC/NIRVANA (LN) is the German-Italian beam combiner for the Large
Binocular Telescope (LBT). It is a Fizeau interferometer and it will
provide multiple images of the same target corresponding to different
orientations of the baseline. For each one of these images the
resolution is not uniform over the field since it is the resolution of a
22.8m mirror in the direction of the baseline and that of a 8.4m mirror
in the orthogonal one. Therefore a unique high-resolution image can only
be obtained by means of deconvolution methods. Four-years ongoing work
of our group on this problem has already clarified the effects of
partial adaptive optics corrections and partial coverage of the u,v
plane and has produced the Software Package AIRY, a set of modules
IDL-based and CAOS-compatible, which can be used for simulation and/or
deconvolution of multiple images from the LBT instrument LN. In this
paper we present a general approach to the design of methods for the
simultaneous deconvolution of multiple images of the same object. These
can include both quick-look methods, to be used for routinely process LN
images, and ad-hoc methods for specific classes of astronomical objects.
We describe several examples of these methods whose implementation and
validation is in progress. Finally we present the last version of the
Software Package AIRY.
Title: Large Binocular Telescope Interferometer: the
universal beam combiner
Authors: Hinz, Philip M.; Connors, Tom; McMahon, Tom;
Cheng, Andrew; Peng, Chien Y.;
Hoffmann, William; McCarthy, Donald, Jr.;
Angel, Roger
Publication: New Frontiers in Stellar Interferometry, Proceedings
of SPIE Volume 5491. Edited by Wesley A. Traub.
Bellingham, WA: The International Society for
Optical Engineering, 2004., p.787 (SPIE Homepage)
Publication Date: 10/2004
Origin: ADS
Bibliographic Code: 2004SPIE.5491..787H
Abstract
The Large Binocular Telescope with its single mount design and adaptive
optics integrated into the secondary mirrors, provides a unique platform
for mid-infrared interferometry. The Large Binocular Telescope
Interferometer is designed to take advantage of this platform,
specifically for extrasolar planet detection in preparation for the
Terrestrial Planet Finder mission. The instrument consists of three
components: a general purpose or Universal Beam Combiner (UBC) which
preserves the sine condition of the array, a nulling interferometer for
the LBT (NIL) to overlap the two beams and sense phase variations, and a
nulling-optimized mid-infrared camera (NOMIC) for detection of the final
images. Here we focus on the design and tolerancing of the UBC. The
components of the system are currently being fabricated and the
instrument is planned to be integrated with the LBT in 2006.
Title: Interferometry on the Large Binocular Telescope
Authors: Herbst, Thomas M.; Hinz, Philip M.
Publication: New Frontiers in Stellar Interferometry, Proceedings
of SPIE Volume 5491. Edited by Wesley A. Traub.
Bellingham, WA: The International Society for
Optical Engineering, 2004., p.383 (SPIE Homepage)
Publication Date: 10/2004
Origin: ADS
Bibliographic Code: 2004SPIE.5491..383H
Abstract
The Large Binocular Telescope (LBT) will be a unique interferometric
facility when it is completed in 2005. The telescope incorporates two,
8.4-meter diameter primary mirrors on a single mounting. With 14.4 meter
center-to-center spacing, this interferometer provides the equivalent
collecting area of a 12-meter telescope, and, depending on the beam
combination scheme, the spatial resolution of a 14.4 or 22.8-meter
telescope. We report on the status of two initial interferometric
instruments planned for the LBT. A group based at the University of
Arizona is constructing LBTI, a thermal infrared beam combiner focusing
on nulling, but allowing thermal imaging as well. This instrument will
search for and measure zodiacal light in candidate stellar systems in
preparation for the Terrestrial Planet Finder (TPF) and Darwin missions.
There is also a program to search for young Jupiters. A second group,
based in Heidelberg, Arcetri, Cologne, and Bonn, is building
LINC-NIRVANA, a near-infrared Fizeau-mode beam combiner with
multi-conjugated adaptive optics (MCAO). Fizeau interferometry preserves
phase information and allows true imagery over a wide field of view.
Using state-of-the-art detector arrays, coupled with advanced
atmospheric correction strategies, LINC-NIRVANA will enable a broad
variety of scientific programs that require the ultimate in sensitivity,
field-of-view, and spatial resolution.
Title: LBT adaptive secondary units construction: a
progress report
Authors: Gallieni, Daniele; Anaclerio, Vincenzo;
Ripamonti, Angelo; Biasi, Roberto;
Andrighettoni, Mario; Veronese, Daniele;
Ponzo, Walter
Affiliation: AA(ADS International Srl (Italy)), AB(ADS
International Srl (Italy)), AC(ADS International Srl
(Italy)), AD(MICROGATE Srl (Italy)), AE(MICROGATE
Srl (Italy)), AF(MICROGATE Srl (Italy)),
AG(MICROGATE Srl (Italy))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
1600-1605 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.553191
Bibliographic Code: 2004SPIE.5490.1600G
Abstract
The two 911mm-diameter adaptive secondary mirrors for the Large
Binocular Telescope (LBT) are in an advanced construction phase. We
present here the general layout of the two units and the relevant steps
of their construction, in particular the mechanics and the control
electronics.
Title: The adaptive secondary mirrors for the Large
Binocular Telescope: a progress report
Authors: Riccardi, Armando; Brusa, Guido;
Xompero, Marco; Zanotti, Daniela;
Del Vecchio, Ciro; Salinari, Piero;
Ranfagni, Piero; Gallieni, Daniele;
Biasi, Roberto; Andrighettoni, Mario;
Miller, Steve; Mantegazza, Paolo
Affiliation: AA(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AB(Steward Observatory/Univ. of Arizona
(USA)), AC(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AD(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AE(INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AF(INAF, Osservatorio
Astrofisico di Arcetri (Italy)), AG(INAF,
Osservatorio Astrofisico di Arcetri (Italy)), AH(ADS
International Srl (Italy)), AI(MICROGATE Srl
(Italy)), AJ(MICROGATE Srl (Italy)), AK(Steward
Observatory/Univ. of Arizona (USA)), AL(Politecnico
di Milano (Italy))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
1564-1571 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551578
Bibliographic Code: 2004SPIE.5490.1564R
Abstract
The two 911mm-diameter adaptive secondary (AS) mirrors for the Large
Binocular telescope (LBT) are currently under manufacturing process.
Each unit has 672 electro-magnetic force actuators. They control the
figure of the Gregorian secondary 1.6mm-thick mirrors with an internal
loop using the signal of co-located capacitive sensors. The obtained
computational power of the on-board control electronics allows to use it
as real-time computer for wavefront reconstruction. We present the
progress in manufacturing and assembling of the first telescope unit,
the progress in software production, the status of the testing
facilities and an update on the latest modification of the design.
Title: Dedicated flexible electronics for adaptive
secondary control
Authors: Biasi, Roberto; Andrighettoni, Mario;
Riccardi, Armando; Biliotti, Valdemaro;
Fini, Luca; Mantegazza, Paolo; Gallieni, Daniele
Affiliation: AA(MICROGATE Srl (Italy)), AB(MICROGATE Srl
(Italy)), AC(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AD(INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AE(INAF, Osservatorio
Astrofisico di Arcetri (Italy)), AF(Politecnico di
Milano (Italy)), AG(ADS International Srl (Italy))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
1502-1513 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.553181
Bibliographic Code: 2004SPIE.5490.1502B
Abstract
In the frame of the Large Binocular Telescope (LBT) adaptive secondary
project, we developed a new dedicated electronics that controls the thin
shell by means of 672 force actuators and capacitive sensor, while
performing also the Real Time Reconstructor (RTR) computations. Within
the adaptive optics system, the Slope Computer is also implemented using
the same electronics, directly interfaced to the wavefront sensor CCD
output by means of built-in fast parallel I/O channels. The system
design has been tailored to balance the computational power, in the
range of hundreds of Gigaflops, with an effective and time-deterministic
real-time communication scheme. Diagnostic and maintenance are performed
through an additional, fully independent communication line. Modularity,
flexibility and remote in-system reconfigurability make this compact
electronic suitable for real time adaptive optics control systems within
a wide range of size and complexity, up to several thousands of
actuators. In this paper we describe the general hardware and software
architecture and the application results of this electronics within the
LBT first light adaptive optics system.
Title: Off-the-shelf real-time computers for
next-generation adaptive optics
Authors: Hippler, Stefan; Looze, Douglas P.;
Gaessler, Wolfgang
Affiliation: AA(Max-Planck-Institut fur Astronomie (Germany)),
AB(Univ. of Massachusetts/Amherst (USA)),
AC(Max-Planck-Institut fur Astronomie (Germany))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
1402-1413 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550036
Bibliographic Code: 2004SPIE.5490.1402H
Abstract
The performance of adaptive optics systems for existing as well as
future giant telescopes heavily depends on the number of active
wavefront compensating elements, the spatial, and the temporal sampling
of the distorted incoming wavefront. In a phase-A study for an extreme
adaptive optics system for the VLT (CHEOPS) as well as for LINC-NIRVANA
a fizeau interferometer aboard LBT with a multi-conjugated adaptive
optics system, we investigate how today's off-the-shelf computers
compare in terms of floating point computing power, memory bandwidth,
input/output bandwidth and real-time behavior. We address questions like
how level three cache can impact the memory bandwidth, what
matrix-vector multiplication performance is achievable, and what can we
learn from standard benchmarks running on different architectures.
Title: LINC-NIRVANA: mechanical challanges of the MCAO
wavefront sensor
Authors: Soci, Roberto; Ragazzoni, Roberto;
Herbst, Thomas M.; Farinato, Jacopo;
Gaessler, Wolfgang; Baumeister, Harald;
Rohloff, Ralf-Rainer; Diolaiti, Emiliano;
Xu, Wenli; Andersen, David R.;
Egner, Sebastian E.; Arcidiacono, Carmelo;
Lombini, Matteo; Ebert, Monica; Boehm, Armin;
Muench, Norbert; Xompero, Marco
Affiliation: AA(Max-Planck-Institut fur Astronomie (Germany)),
AB(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AC(Max-Planck-Institut fur Astronomie
(Germany)), AD(Osservatorio Astrofisico di Arcetri
(Italy)), AE(Max-Planck-Institut fur Astronomie
(Germany)), AF(Max-Planck-Institut fur Astronomie
(Germany)), AG(Max-Planck-Institut fur Astronomie
(Germany)), AH(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AI(Max-Planck-Institut fur
Astronomie (Germany)), AJ(Max-Planck-Institut fur
Astronomie (Germany)), AK(Max-Planck-Institut fur
Astronomie (Germany)), AL(INAF, Osservatorio
Astrofisico di Arcetri (Italy)), AM(INAF,
Osservatorio Astrofisico di Arcetri (Italy)),
AN(Max-Planck-Institut fur Astronomie (Germany)),
AO(Max-Planck-Institut fur Astronomie (Germany)),
AP(Max-Planck-Institut fur Astronomie (Germany)),
AQ(INAF, Osservatorio Astrofisico di Arcetri
(Italy))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
1286-1295 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551674
Bibliographic Code: 2004SPIE.5490.1286S
Abstract
Several multi-conjugate adaptive optics (MCAO) systems using the
layer-oriented approach are under construction and will soon be tested
at different facilities in several instruments. One of these instruments
is LINC-NIRVANA, a Fizeau interferometer for the Large Binocular
Telescope (LBT). This instrument uses a ground layer wavefront sensor
(GWS) and a combined mid-high layer wavefront sensor (MHWS) with
different fields of view (concept of multiple field of view), a 2-6
arcmin annular ring for the GWS and a 2 arcmin diameter central field of
view for the MHWS. Both sensors are Pyramid wavefront sensors which
optically co-add light from multiple natural guide stars. The
opto-mechanical problems concerning these sensors are related to the
fast focal ratio of the beam on the pyramids coupled with the available
pixelscale of detectors. This leads to very tight requirements on the
moving systems (linear stages) for the star enlargers (SE) used to pick
off the light of individual stars. As there are 40 star enlargers in the
overall system, additional efforts were put into the alignment system of
the optics of the star enlargers and the reduction in size of the star
enlargers to minimize the distance between available guide stars.
Title: LINC-NIRVANA: the single arm MCAO experiment
Authors: Egner, Sebastian E.; Gaessler, Wolfgang;
Herbst, Tom M.; Ragazzoni, Roberto;
Stuik, Remko; Andersen, D. A.; Arcidiacono, C.;
Baumeister, H.; Beckmann, U.; Behrend, J.;
Bertram, T.; Bizenberger, P.; Boehnhardt, H.;
Diolaiti, E.; Driebe, T.; Eckhardt, A.;
Farinato, J.; Kuerster, M.; Laun, W.;
Ligori, S.; Naranjo, Vianak; Nußbaum, E.;
Rix, H.-W.; Rohloff, R.-R.; Salinari, Piero;
Soci, R.; Straubmeier, C.; Vernet-Viard, E.;
Weigelt, Gerd P.; Weiss, R.; Xu, W.
Affiliation: AA(Max-Planck-Institut fur Astronomie (Germany)),
AB(Max-Planck-Institut fur Astronomie (Germany)),
AC(Max-Planck-Institut fur Astronomie (Germany)),
AD(Max-Planck-Institut fur Astronomie (Germany) and
INAF, Osservatorio Astrofisico di Arcetri (Italy)),
AE(Leiden Observatory (Netherlands)),
AF(Max-Planck-Institut fur Astronomie (Germany)),
AG(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AH(Max-Planck-Institut fur Astronomie
(Germany)), AI(Max-Planck-Institut fur
Radioastronomie (Germany)), AJ(Max-Planck-Institut
fur Radioastronomie (Germany)), AK(Univ. zu Koln
(Germany)), AL(Max-Planck-Institut fur Astronomie
(Germany)), AM(Max-Planck-Institut fur Astronomie
(Germany)), AN(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AO(Max-Planck-Institut fur
Astronomie (Germany)), AP(Univ. zu Koln (Germany)),
AQ(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AR(Max-Planck-Institut fur Astronomie
(Germany)), AS(Max-Planck-Institut fur Astronomie
(Germany)), AT(Max-Planck-Institut fur Astronomie
(Germany)), AU(Max-Planck-Institut fur Astronomie
(Germany)), AV(Max-Planck-Institut fur
Radioastronomie (Germany)), AW(Max-Planck-Institut
fur Astronomie (Germany)), AX(Max-Planck-Institut
fur Astronomie (Germany)), AY(INAF, Osservatorio
Astrofisico di Arcetri (Italy)),
AZ(Max-Planck-Institut fur Astronomie (Germany)),
BA(Univ. zu Koln (Germany)), BB(INAF, Osservatorio
Astrofisico di Arcetri (Italy)),
BC(Max-Planck-Institut fur Radiostronomie
(Germany)), BD(Max-Planck-Institut fur Astronomie
(Germany)), BE(Max-Planck-Institut fur Astronomie
(Germany))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
924-933 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550046
Bibliographic Code: 2004SPIE.5490..924E
Abstract
LINC-NIRVANA is an imaging interferometer for the Large Binocular
Telescope (LBT) and will make use of multi-conjugated adaptive optics
(MCAO) with two 349 actuators deformable mirrors (DM), two 672 actuator
deformable secondary mirrors and a total of 4 wavefront sensors (WFS) by
using 8 or 12 natural guide stars each. The goal of the MCAO is to
increase sky coverage and achieve a medium Strehl-ratio over the 2
arcmin field of view. To test the concepts and prototypes, a laboratory
setup of one MCAO arm is being built. We present the layout of the MCAO
prototype, planned and accomplished tests, especially for the used
Xinetics DMs, and a possible setup for a test on sky with an existing 8m
class telescope.
Title: Numerical simulation studies for the first-light
adaptive optics system of the Large Binocular
Telescope
Authors: Carbillet, Marcel; Riccardi, Armando;
Esposito, Simone
Affiliation: AA(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AB(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AC(INAF, Osservatorio Astrofisico
di Arcetri (Italy))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
721-732 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551448
Bibliographic Code: 2004SPIE.5490..721C
Abstract
We present our latest results concerning the simulation studies
performed for the first-light adaptive optics (AO) system of the Large
Binocular Telescope (LBT), namely WLBT. After a brief description of the
"raw" performance evaluation results, in terms of Strehl ratios attained
in the various considered bands (from V to K), we focus on the
"scientific" performance that will be obtained when considering the
subsequent instrumentation that will benefit from the correction given
by the AO system WLBT and the adaptive secondary mirrors LBT 672. In
particular, we discuss the performance of the coupling with the
instrument LUCIFER, working at near-infrared bands, in terms of
signal-to-noise values and limiting magnitudes, and in both the cases of
spectroscopy and photometric detection. We also give the encircled
energies that are expected in the visible bands, result relevant in one
hand for the instrument PEPSI, and in other hand for the "technical
viewer" that will be on board the WLBT system itself.
Title: LINC-NIRVANA: how to get a 23-m wavefront nearly
flat
Authors: Gaessler, Wolfgang; Ragazzoni, Roberto;
Herbst, Thomas M.; Andersen, David R.;
Arcidiacono, Carmelo; Baumeister, Harald;
Beckmann, Udo; Behrend, Jan; Bertram, Thomas;
Bizenberger, Peter; Bohnhardt, Hermann;
Briegel, F.; Diolaiti, Emiliano;
Driebe, Thomas M.; Eckhardt, A.;
Egner, Sebastian E.; Farinato, Jacopo;
Heininger, Matthias; Kürster, M.; Laun, Werner;
Ligori, Sebastiano; Naranjo, Vianak;
Nussbaum, Edmund; Rix, Hans-Walter;
Rohloff, Ralf-Rainer; Salinari, Piero;
Soci, Roberto; Storz, Clemens;
Straubmeier, Christian; Vernet-Viard, Elise;
Weigelt, Gerd P.; Weiss, Robert; Xu, Wenli
Affiliation: AA(Max-Planck-Institut fur Astronomie (Germany)),
AB(Max-Planck-Institut fur Astronomie (Germany) and
INAF, Osservatorio Astrofisico di Arcetri (Italy)),
AC(Max-Planck-Institut fur Astronomie (Germany)),
AD(Max-Planck-Institut fur Astronomie (Germany)),
AE(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AF(Max-Planck-Institut fur Astronomie
(Germany)), AG(Max-Planck-Institut fur
Radioastronomie (Germany)), AH(Max-Planck-Institut
fur Radioastronomie (Germany)), AI(Univ. zu Koln
(Germany)), AJ(Max-Planck-Institut fur Astronomie
(Germany)), AK(Max Planck Institut fur Astronomie
(Germany)), AL(Max-Planck-Institut fur Astronomie
(Germany)), AM(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AN(Max-Planck-Institut fur
Radioastronomie (Germany)), AO(Univ. zu Koln
(Germany)), AP(Max-Planck-Institut fur Astronomie
(Germany)), AQ(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AR(Max-Planck-Institut fur
Radioastronomie (Germany)), AS(Max-Planck-Institut
fur Astronomie (Germany)), AT(Max-Planck-Institut
fur Astronomie (Germany)), AU(Max-Planck-Institut
fur Astronomie (Germany)), AV(Max-Planck-Institut
fur Astronomie (Germany)), AW(Max-Planck-Institut
fur Radioastronomie (Germany)),
AX(Max-Planck-Institut fur Astronomie (Germany)),
AY(Max-Planck-Institut fur Astronomie (Germany)),
AZ(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), BA(Max-Planck-Institut fur Astronomie
(Germany)), BB(Max-Planck-Institut fur Astronomie
(Germany)), BC(Univ. zu Koln (Germany)), BD(INAF,
Osservatorio Astrofisico di Arcetri (Italy)),
BE(Max-Planck-Institut fur Radioastronomie
(Germany)), BF(Max-Planck-Institut fur Astronomie
(Germany)), BG(Max-Planck-Institut fur Astronomie
(Germany))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
527-534 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551908
Bibliographic Code: 2004SPIE.5490..527G
Abstract
On the way to the Extremely Large Telescopes (ELT) the Large Binocular
Telescope (LBT) is an intermediate step. The two 8.4m mirrors create a
masked aperture of 23m. LINC-NIRVANA is an instrument taking advantage
of this opportunity. It will get, by means of Multi-Conjugated Adaptive
Optics (MCAO), a moderate Strehl Ratio over a 2 arcmin field of view,
which is used for Fizeau (imaging) interferometry in J,H and K. Several
MCAO concepts, which are proposed for ELTs, will be proven with this
instrument. Studies of sub-systems are done in the laboratory and the
option to test them on sky are kept open. We will show the
implementation of the MCAO concepts and control aspects of the
instrument and present the road map to the final installation at LBT.
Major milestones of LINC-NIRVANA, like preliminary design review or
final design review are already done or in preparation. LINC-NIRVANA is
one of the few MCAO instruments in the world which will see first light
and go into operation within the next years.
Title: Can we use adaptive optics for UHR spectroscopy with
PEPSI at the LBT?
Authors: Sacco, Germano G.; Pallavicini, Roberto;
Spano, Paolo; Andersen, Michael;
Woche, Manfred F.; Strassmeier, Klaus G.
Affiliation: AA(INAF, Osservatorio Astronomico di Palermo (Italy)
and Univ. degli Studi di Palermo (Italy)), AB(INAF,
Osservatorio Astronomico di Palermo (Italy)),
AC(INAF, Osservatorio Astronomico di Palermo (Italy)
and Univ. degli Studi di Palermo (Italy)),
AD(Astrophysikalisches Institut Potsdam (Germany)),
AE(Astrophysikalisches Institut Potsdam (Germany)),
AF(Astrophysikalisches Institut Potsdam (Germany))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
398-408 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550373
Bibliographic Code: 2004SPIE.5490..398S
Abstract
We investigate the potential of using adaptive optics (AO) in the V, R,
and I bands to reach ultra-high resolution (UHR, R >= 200,000) in
echelle spectrographs at 8-10m telescopes. In particular, we investigate
the possibility of implementing an UHR mode for the fiber-fed
spectrograph PEPSI (Potsdam Echelle Polarimetric and Spectrographic
Instrument) being developed for the Large Binocular Telescope (LBT). By
simulating the performances of the advanced AO system that will be
available at first light at the LBT, and by using first-order estimates
of the spectrograph performances, we calculate the total efficiency and
signal to noise ratio (SNR) of PEPSI in the AO mode for stars of
different magnitudes, different fiber core sizes, and different
fractions of incident light diverted to the wavefront sensor. We
conclude that AO can provide a significant advantage, of up to a factor
~2 in the V, R and I bands, for stars brighter than mR ~ 12 -
13. However, if these stars are observed at UHR in non-AO mode, slit
losses caused by the need to use a very narrow slit can be compensated
more effectively by the use of image slicers.
Title: Integration and test of the first light AO system
for LBT
Authors: Esposito, Simone; Tozzi, Andrea;
Puglisi, Alfio T.; Pinna, Enrico;
Stefanini, Paolo; Giorgetti, Gabriele;
Camiciottoli, Fabrizio; Salinari, Piero;
Bianchi, Paolo; Storm, Jesper
Affiliation: AA(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AB(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AC(INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AD(INAF, Osservatorio
Astrofisico di Arcetri (Italy)), AE(INAF,
Osservatorio Astrofisico di Arcetri (Italy)),
AF(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AG(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AH(INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AI(Istituto Nazionale di Ottica
Applicata (Italy)), AJ(Astrophysikalisches Institut
Potsdam (Germany))
Publication: Advancements in Adaptive Optics. Edited by Domenico
B. Calia, Brent L. Ellerbroek, and Roberto
Ragazzoni. Proceedings of the SPIE, Volume 5490, pp.
228-235 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551724
Bibliographic Code: 2004SPIE.5490..228E
Abstract
The paper describes the single conjugate AO system called WLBT to be
mounted at LBT in late summer 2004. The WLBT is part of the Acquisition,
Guiding & Wavefront sensing unit (AGW) attached to the front bent
Gregorian foci derotator. The two key features of this system are the
use of a pyramid wavefront sensor with variable sampling between 30x30
and 5x5 sub apertures plus the use of an adaptive secondary mirror
having 672 actuators as wavefront corrector. The AO system is mainly
working as atmospheric disturbance correction system in the near
infrared (J,H and K band). However due to the large number of actuators
and sub apertures, it can obtain good performance even in R and I band.
The paper reports about development and integration of the system final
unit in the lab. Then some initial tests aimed to do a system
characterization are reported. The results we obtained are used to give
an estimation of the performance that the system can reach at the
telescope in terms of limiting magnitude.
Title: Active optics and force optimization for the first
8.4-m LBT mirror
Authors: Martin, Hubert M.; Cuerden, Brian;
Dettmann, Lee R.; Hill, John M.
Affiliation: AA(Steward Observatory/Univ. of Arizona (USA)),
AB(Steward Observatory/Univ. of Arizona (USA)),
AC(Steward Observatory/Univ. of Arizona (USA)),
AD(Large Binocular Telescope Observatory/Univ. of
Arizona (USA))
Publication: Ground-based Telescopes. Edited by Oschmann,
Jacobus M., Jr. Proceedings of the SPIE, Volume
5489, pp. 826-837 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550464
Bibliographic Code: 2004SPIE.5489..826M
Abstract
We describe the active support system for the 8.4 m LBT primary mirrors
and the use of this system to optimize the mirror figure in the lab
before installation in the telescope. We figured the mirror, mounted on
passive supports, to an accuracy of 18 nm rms surface after subtraction
of spherical aberration and several flexible bending modes that would be
corrected with the active supports. After installing the mirror on its
active supports, we optimized the 160 support forces based on
interferometric wavefront measurements and a finite-element model of
mirror bending. We verified the accuracy of the model and determined a
scale factor-the model is stiffer than the real mirror-by measuring a
number of bending modes using forces calculated from the model. We then
optimized the forces to obtain an accuracy of 28 nm rms surface. The
optimization included correcting 200 nm of spherical aberration (Zernike
coefficient of surface error) with a maximum correction force of 26 N.
Title: The Large Binocular Telescope project
Authors: Hill, John M.; Salinari, Piero
Affiliation: AA(Large Binocular Telescope Observatory/Univ. of
Arizona (USA)), AB(INAF, Osservatorio Astrofisico di
Arcetri (Italy))
Publication: Ground-based Telescopes. Edited by Oschmann,
Jacobus M., Jr. Proceedings of the SPIE, Volume
5489, pp. 603-614 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550556
Bibliographic Code: 2004SPIE.5489..603H
Abstract
The Large Binocular Telescope (LBT) Project is a collaboration between
institutions in Arizona, Germany, Italy, and Ohio. The telescope uses
two 8.4-meter diameter primary mirrors mounted side-by-side to produce a
collecting area equivalent to an 11.8-meter circular aperture. A unique
feature of LBT is that the light from the two primary mirrors can be
combined to produce phased array imaging of an extended field. This
coherent imaging gives the telescope the diffraction-limited resolution
of a 22.65-meter telescope. The first of two 8.4-meter borosilicate
honeycomb primary mirrors has been installed in the telescope on Mt.
Graham in southeastern Arizona. First Light is planned for later this
year with one primary mirror and a prime focus imager. The second of the
two primaries is being polished at the Steward Observatory Mirror Lab in
Tucson and will be installed in the telescope in the Fall of 2005. The
telescope uses two F/15 adaptive secondaries to correct atmospheric
turbulence.
Title: The scaling relationship between telescope cost and
aperture size for very large telescopes
Authors: van Belle, Gerard T.; Meinel, Aden B.;
Meinel, Marjorie P.
Affiliation: AA(Michelson Science Ctr. (USA)), AB(Jet Propulsion
Lab. (USA)), AC(Jet Propulsion Lab. (USA))
Publication: Ground-based Telescopes. Edited by Oschmann,
Jacobus M., Jr. Proceedings of the SPIE, Volume
5489, pp. 563-570 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.552181
Bibliographic Code: 2004SPIE.5489..563V
Abstract
Cost data for ground-based telescopes of the last century are analyzed
for trends in the relationship between aperture size and cost. We find
that for apertures built prior to 1980, costs scaled as aperture size to
the 2.8 power, which is consistent with the previous finding of Meinel
(1978). After 1980, 'traditional' monolithic mirror telescope costs have
scaled as aperture to the 2.5 power. The large multiple mirror
telescopes built or in construction during this time period (Keck, LBT,
GTC) appear to deviate from this relationship with significant cost
savings as a result, although it is unclear what power law such
structures follow. We discuss the implications of the current
cost-aperture size data on the proposed large telescope projects of the
next ten to twenty years. Structures that naturally tend towards the 2.0
power in the cost-aperture relationship will be the favorable choice for
future extremely large apertures; our expectation is that space-based
structures will ultimately gain economic advantage over ground-based
ones.
Title: The acquisition, guiding, and wavefront sensing
units for the Large Binocular Telescope
Authors: Storm, Jesper; Seifert, Walter;
Bauer, Svend-Marian; Dionies, Frank;
Fechner, Thomas; Krämer, Felix; Möstl, Günter;
Popow, Emil; Esposito, Simone; Hill, John M.;
Salinari, Piero
Affiliation: AA(Astrophysikalisches Institut Potsdam (Germany)),
AB(Landessternwarte Heidelberg-Königstuhl
(Germany)), AC(Astrophysikalisches Institut Potsdam
(Germany)), AD(Astrophysikalisches Institut Potsdam
(Germany)), AE(Astrophysikalisches Institut Potsdam
(Germany)), AF(Astrophysikalisches Institut Potsdam
(Germany)), AG(Astrophysikalisches Institut Potsdam
(Germany)), AH(Astrophysikalisches Institut Potsdam
(Germany)), AI(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AJ(Large Binocular Telescope
Observatory/Univ. of Arizona (USA)), AK(INAF,
Osservatorio Astrofisico di Arcetri (Italy))
Publication: Ground-based Telescopes. Edited by Oschmann,
Jacobus M., Jr. Proceedings of the SPIE, Volume
5489, pp. 374-381 (2004). (SPIE Homepage)
Publication Date: 10/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551126
Bibliographic Code: 2004SPIE.5489..374S
Abstract
We present the final opto-mechanical design of the Large Binocular
Telescope (LBT) Acquisition, Guiding and Wavefront Sensing Units
(AGW-units) together with the laboratory test performance of the units.
The units will be installed at the LBT shortly after this conference, at
several of the different Gregorian focal positions available. Each
AGW-unit consists of a probe with a camera and a wavefront sensor
located in front of the science instrument. The probe can move in two
axes allowing it to patrol a field off-axis to the science field. A
dichroic beam-splitter on the probe transmits the blue light to the
acquisition and guide camera and the red light is reflected into a
Shack-Hartmann wavefront sensor. The guide camera is equipped with a
2.5x focal reducer giving a field of view of 28"x28" on a 512x1024
frame-transfer CCD. The 12x12 sub-pupil wavefront sensor uses a micro
lenslet array made using an ion-exchange technique on a flat substrate
with diffraction limited performance.
Title: A robotic reflective Schmidt telescope for Dome C
Authors: Strassmeier, K. G.; Andersen, M. I.; Steinbach, M.
Affiliation: AA(Astrophysical Institute Potsdam (AIP), An der
Sternwarte 16, 14482 Potsdam, Germany),
AB(Astrophysical Institute Potsdam (AIP), An der
Sternwarte 16, 14482 Potsdam, Germany),
AC(Ingenieurbüro Steinbach-Könitzer-Lopez,
Wildenbruchstr. 15, 07745 Jena, Germany)
Publication: Astronomische Nachrichten, Vol.325, Issue 6,
p.626-630 (AN Homepage)
Publication Date: 10/2004
Origin: AN
Keywords: telescopes: robotic, techniques: wide field-CCD
photometry, stars: activity, Antarctica (Dome C)
Abstract Copyright: (c) 2004: WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
DOI: 10.1002/ansa.200410303
Bibliographic Code: 2004AN....325..626S
Abstract
This paper lays out a wide-field robotic Schmidt telescope (RST) for the
Antarctic site Dome C. The telescope is based on 80/120cm reflective
Schmidt optics, built originally for a space project, and a mosaic of
four 7.5k×7.5k 8-$,1'<(Bm thinned CCDs from the PEPSI/LBT wafer run.
The telescope's total field of view (FOV) would be 5o
circular (minimum 3o× 3o square) with a
plate scale of 0.7 arcsec per pixel. Limiting magnitude is expected to
be V=21.5mag in 60 sec for a field of 9 square degrees.
Title: The MPIA detector system for the LBT instruments
LUCIFER and LINC-NIRVANA
Authors: Ligori, Sebastiano; Lenzen, Rainer;
Mandel, Holger; Grimm, Bernhard; Mall, Ulrich
Affiliation: AA(Max-Planck-Institut für Astronomie (Germany)),
AB(Max-Planck-Institut für Astronomie (Germany)),
AC(Landessternwarte Heidelberg-Königstuhl
(Germany)), AD(Max-Planck-Institut für Astronomie
(Germany)), AE(Max-Planck-Institut für Astronomie
(Germany))
Publication: Optical and Infrared Detectors for Astronomy.
Edited by James D. Garnett and James W. Beletic.
Proceedings of the SPIE, Volume 5499, pp. 108-118
(2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.549571
Bibliographic Code: 2004SPIE.5499..108L
Abstract
We describe the detector subsystem developed at MPIA to operate the
Rockwell Hawaii-2 detectors used in the LUCIFER and LINC-NIRVANA
instruments for the Large Binocular Telescope (LBT). To fully exploit
the capabilities of the LBT, the detector subsystem must meet,
especially in the case of the low background applications foreseen for
LUCIFER, very stringent requirements in terms of stability and read
noise. A read-out electronics has been developed at MPIA, which is able
to read the 32 outputs of the Hawaii-2 detector, as well as the 4
reference signals available in this chip. The noise figure associated to
the electronics alone is negligible with respect to the intrinsic read
noise of the detector, while the cloking patterns and the value of the
bias voltages applied to the chip are optimized in order to maximize the
signal to noise ratio in the different operating modes. We present the
results of the tests performed with the LUCIFER science detector; in
particular, we describe the main properties of the detector: read noise,
dark current, linearity, and long term stability, and what are the
read-out schemes foreseen for different observational modes. We discuss
also how the reference outputs can be used in order to correct for
thermal drifts, and how effective those outputs are in removing higher
frequency noise components.
Title: LBT-AdOpt control software
Authors: Fini, Luca; Puglisi, Alfio; Riccardi, Armando
Affiliation: AA(INAF, Osservatorio Astrofisico di Arcetri
(Italy)), AB(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AC(INAF, Osservatorio Astrofisico
di Arcetri (Italy))
Publication: Advanced Software, Control, and Communication
Systems for Astronomy. Edited by Lewis, Hilton;
Raffi, Gianni. Proceedings of the SPIE, Volume
5496, pp. 528-537 (2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.552972
Bibliographic Code: 2004SPIE.5496..528F
Abstract
The LBT-AdOpt subsystem is a complex machine which includes several
software controlled parts. It is essentially divided into two parts: a
real-time loop which implements the actual adaptive optics control loop,
from the wavefront sensor to the deformable secondary mirror, and a
supervisor which performs a number of coordination and diagnostics
tasks. The coordination and diagnostics task are essential for the
proper operation of the system both as an aid for the preparation of
observations and because only a continuous monitoring of dynamic system
parameters can guarantee optimal performances and system safety during
the operation. In the paper we describe the overall software
architecture of the LBT-AdOpt supervisor and we discuss the
functionalities required for a proper operation.
Title: The LBT double prime focus camera control software
Authors: Di Paola, Andrea; Baruffolo, Andrea;
Gallozzi, Stefano; Pedichini, Fernando;
Speziali, Roberto
Affiliation: AA(INAF, Rome Astronomical Observatory (Italy)),
AB(INAF, Padua Astronomical Observatory (Italy)),
AC(INAF, Rome Astronomical Observatory (Italy)),
AD(INAF, Rome Astronomical Observatory (Italy)),
AE(INAF, Rome Astronomical Observatory (Italy))
Publication: Advanced Software, Control, and Communication
Systems for Astronomy. Edited by Lewis, Hilton;
Raffi, Gianni. Proceedings of the SPIE, Volume
5496, pp. 477-488 (2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.555423
Bibliographic Code: 2004SPIE.5496..477D
Abstract
The LBT double prime focus camera (LBC) is composed of twin CCD mosaic
imagers. The instrument is designed to match the double channel
structure of the LBT telescope and to exploit parallel observing mode by
optimizing one camera at blue and the other at red side of the visible
spectrum. Because of these facts, the LBC activity will likely consist
of simultaneous multi-wavelength observation of specific targets, with
both channels working at the same time to acquire and download images at
different rates. The LBC Control Software is responsible for
coordinating these activities by managing scientific sensors and all the
ancillary devices such as rotators, filter wheels, optical correctors
focusing, house-keeping information, tracking and Active Optics
wavefront sensors. The result is obtained using four dedicated PCs to
control the four CCD controllers and one dual processor PC to manage all
the other aspects including instrument operator interface. The general
architecture of the LBC Control Software is described as well as
solutions and details about its implementation.
Title: The development process of the LUCIFER control
software
Authors: Juette, Marcus; Polsterer, Kai L.;
Lehmitz, Michael; Knierim, Volker
Affiliation: AA(Ruhr-Univ. Bochum (Germany)), AB(Ruhr-Univ.
Bochum (Germany)), AC(Landessternwarte
Heidelberg-Konigstuhl (Germany)), AD(Ruhr-Univ.
Bochum (Germany))
Publication: Advanced Software, Control, and Communication
Systems for Astronomy. Edited by Lewis, Hilton;
Raffi, Gianni. Proceedings of the SPIE, Volume
5496, pp. 469-476 (2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551166
Bibliographic Code: 2004SPIE.5496..469J
Abstract
In this paper we present the software development process and history of
the LUCIFER (LBT NIR spectroscopic Utility with Camera and Integral-
Field Unit for Extragalactic Research) multi-mode near-infrared
instrument, which is one of the first light instruments of the LBT on
Mt. Graham, Arizona. The software is realised as a distributed system in
Java using its remote method invocation service (RMI). We describe the
current status of the software and give an overview of the planned
computer hardware architecture.
Title: UML modeling of the LINC-NIRVANA control software
Authors: Gaessler, Wolfgang; Bertram, Thomas;
Briegel, F.; Driebe, Thomas M.;
Heininger, Matthias; Nussbaum, Edmund;
Storz, Clemens; Wang, J.; Zealouk, Lahbib;
Herbst, Thomas M.; Ragazzoni, Roberto;
Eckhardt, A.; Weigelt, Gerd P.
Affiliation: AA(Max-Planck-Institut fur Astronomie (Germany)),
AB(Univ. zu Koln (Germany)), AC(Max-Planck-Institut
fur Astronomie (Germany)), AD(Max-Planck-Institut
fur Radioastronomie (Germany)),
AE(Max-Planck-Institut fur Radioastronomie
(Germany)), AF(Max-Planck-Institut fur
Radioastronomie (Germany)), AG(Max-Planck-Institut
fur Astronomie (Germany)), AH(Univ. zu Koln
(Germany)), AI(Univ. zu Koln (Germany)),
AJ(Max-Planck-Institut fur Astronomie (Germany)),
AK(Max-Planck-Institut fur Astronomie (Germany) and
INAF, Osservatorio Astrofisico di Arcetri (Italy)),
AL(Univ. zu Koln (Germany)), AM(Max-Planck-Institut
fur Radioastronomie (Germany))
Publication: Advanced Software, Control, and Communication
Systems for Astronomy. Edited by Lewis, Hilton;
Raffi, Gianni. Proceedings of the SPIE, Volume
5496, pp. 79-87 (2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551756
Bibliographic Code: 2004SPIE.5496...79G
Abstract
LINC-NIRVANA is a Fizeau interferometer for the Large Binocular
Telescope (LBT) doing imaging in the near infrared (J,H,K - band).
Multi-conjugated adaptive optics is used to increase sky coverage and to
get diffraction limited images over a 2 arcminute field of view. The
control system consists of five independent loops, which are mediated
through a master control. Due to the configuration, LINC-NIRVANA has no
delay line like other interferometers. To remove residual atmospheric
piston, the system must control both the primary and secondary mirrors,
in addition to a third, dedicated piston mirror. This leads to a complex
and interlocked control scheme and software. We will present parts of
the instrument software design, which was developed in an
object-oriented manner using UML. Several diagram types were used to
structure the overall system and to evaluate the needs and interfaces of
each sub-system to each other.
Title: Conceptual design and structural analysis for an
8.4-m telescope
Authors: Mendoza, Manuel; Farah, Alejandro;
Ruiz Schneider, Elfego
Affiliation: AA(Instituto de Astronomía, Univ. Nacional Autónoma
de México (Mexico)), AB(Instituto de Astronomía,
Univ. Nacional Autónoma de México (Mexico)),
AC(Instituto de Astronomía, Univ. Nacional Autónoma
de México (Mexico))
Publication: Astronomical Structures and Mechanisms Technology.
Edited by Antebi, Joseph; Lemke, Dietrich.
Proceedings of the SPIE, Volume 5495, pp. 526-536
(2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.563388
Bibliographic Code: 2004SPIE.5495..526M
Abstract
This paper describes the conceptual design of the optics support
structures of a telescope with a primary mirror of 8.4 m, the same size
as a Large Binocular Telescope (LBT) primary mirror. The design goal is
to achieve a structure for supporting the primary and secondary mirrors
and keeping them joined as rigid as possible. With this purpose an
optimization with several models was done. This iterative design process
includes: specifications development, concepts generation and
evaluation. Process included Finite Element Analysis (FEA) as well as
other analytical calculations. Quality Function Deployment (QFD) matrix
was used to obtain telescope tube and spider specifications. Eight
spiders and eleven tubes geometric concepts were proposed. They were
compared in decision matrixes using performance indicators and
parameters. Tubes and spiders went under an iterative optimization
process. The best tubes and spiders concepts were assembled together.
All assemblies were compared and ranked according to their performance.
Title: Handling and transporting the 8.4-m mirrors for the
Large Binocular Telescope
Authors: Davison, Warren B.; Warner, Stephen H.;
Williams, Joseph T.; Lutz, Randall D.;
Hill, John M.; Slagle, Jim H.
Affiliation: AA(Steward Observatory/Univ. of Arizona (USA)),
AB(Steward Observatory/Univ. of Arizona (USA)),
AC(Multiple Mirror Telescope Observatory/Univ. of
Arizona (USA)), AD(Steward Observatory/Univ. of
Arizona (USA)), AE(Large Binocular Telescope
Observatory/Univ. of Arizona (USA)), AF(Large
Binocular Telescope Observatory/Univ. of Arizona
(USA))
Publication: Astronomical Structures and Mechanisms Technology.
Edited by Antebi, Joseph; Lemke, Dietrich.
Proceedings of the SPIE, Volume 5495, pp. 453-462
(2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.549808
Bibliographic Code: 2004SPIE.5495..453D
Abstract
The Large Binocular Telescope has two 8.4 meter mirrors, one of which is
now in the telescope. Handling and moving the 8.4-meter honeycomb
mirrors calls for moving 16 metric ton mirrors while maintaining very
low stresses. We have now handled the first LBT mirror off the furnace,
turned on edge, cleaned out, turned upside down, on the grinder, turned
again, put on a polishing cell, moved under the polishing machine,
lifted with a vacuum lifting fixture, moved to the telescope cell, to a
transportation box, down the highway, onto a multi-axle trailer on edge,
up Mount Graham, into the telescope building, back into the telescope
cell and up through a hatch onto the telescope itself. The second LBT
mirror is in the polishing stage. We have designed and manufactured many
pieces of specialized equipment to handle the task. This equipment must
be able to handle the mirrors without exceeding 0.7 MPa (100 psi) stress
in the glass.
Title: The Giant Magellan Telescope (GMT) structure
Authors: Gunnels, Steve; Davison, Warren B.;
Cuerden, Brian; Hertz, Edward
Affiliation: AA(Paragon Engineering (USA)), AB(Steward
Observatory/Univ. of Arizona (USA)), AC(Steward
Observatory/Univ. of Arizona (USA)),
AD(Harvard-Smithsonian Ctr. for Astrophysics (USA))
Publication: Astronomical Structures and Mechanisms Technology.
Edited by Antebi, Joseph; Lemke, Dietrich.
Proceedings of the SPIE, Volume 5495, pp. 168-179
(2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550266
Bibliographic Code: 2004SPIE.5495..168G
Abstract
A concept design has been developed for the Giant Magellan Telescope
(GMT). The project is a collaboration by a group of U.S. universities
and research institutions to build a 21.5-meter equivalent aperture
optical-infrared telescope in Chile. The segmented primary mirror
consists of seven 8.4-meter diameter borosilicate honeycomb mirrors that
will be cast by the Steward Observatory Mirror Laboratory. The fast
primary optics allow the use of unusually compact telescope and
enclosure structures. A wide range of secondary trusses has been
considered for the alt-az mount. The chosen truss employs carbon fiber
and steel and, due to its unique geometry, achieves high stiffness with
minimal wind area and primary obscuration. The mount incorporates
hydrostatic supports and a C-ring elevation structure similar in concept
to those implemented on the Magellan 6.5-m and LBT dual 8.4-m
telescopes. Extensive finite element analysis has been used to optimize
the telescope structure, achieving a lowest telescope resonant frequency
of ~5 Hz. The design allows for removal and replacement of any of the 7
subcells for off-telescope mirror coating with no risk to the other
mirrors. A wide range of instruments can be used which mount to the top
or underside of a large instrument platform below the primary mirror
cells. Large instruments are interchanged during the day while small and
medium-sized instruments can be enabled quickly during the night. The
large Gregorian instruments will incorporate astatic supports to
minimize flexure and hysteresis.
Title: The Large Binocular Camera image simulator:
predicting the performances of LBC
Authors: Grazian, Andrea; Fontana, Adriano;
De Santis, Cristian; Gallozzi, Stefano;
Giallongo, Emanuele
Affiliation: AA(INAF, Osservatorio Astronomico di Roma (Italy)),
AB(INAF, Osservatorio Astronomico di Roma (Italy)),
AC(INAF, Osservatorio Astronomico di Roma (Italy)),
AD(INAF, Osservatorio Astronomico di Roma (Italy)),
AE(INAF, Osservatorio Astronomico di Roma (Italy))
Publication: Optimizing Scientific Return for Astronomy through
Information Technologies. Edited by Quinn, Peter
J.; Bridger, Alan. Proceedings of the SPIE, Volume
5493, pp. 186-197 (2004). (SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.552980
Bibliographic Code: 2004SPIE.5493..186G
Abstract
The LBC (Large Binocular Camera) Image Simulator is a package for
generating artificial images in the typical FITS format. It operates on
real or artificial images, simulating the expected performances of real
instruments including several observing conditions (filters, air-mass,
flat-field, exposure time) and creating images with the LBC instrumental
artifacts (optical deformations, noise, CCD architectures). This
simulator can be used also to produce artificial images for other
existing and future telescopes, since it is very flexible on its
structure. The main aim of LBCSIM is to support the development of
pipeline and data analysis procedure able to cope with wide field
imaging and fast reduction of huge amount of photometric data. The
software consists of three stand alone programs written in C language,
using IRAF and running under Linux OS. The LBC Image Simulator is built
with particular attention to the Virtual Observatory and Data Grid
applications. In this paper, we first describe the software, the
performances and several tests carried out before the public release and
some examples for the users. In particular, we compared the Hubble Deep
Field South (HDFS) as seen by FORS1 with a simulated image and found
that the agreement is good. Then, we use this software to predict the
expected performances of the LBC instrument by means of realistic
simulations of deep field observations with the LBT telescope.
Title: LUCIFER: status and results of the hardware testing
Authors: Seifert, Walter; Laun, Werner;
Lehmitz, Michael; Mandel, Holger;
Schuetze, Andreas; Seltmann, Andreas
Affiliation: AA(Landessternwarte Heidelberg-Konigstuhl
(Germany)), AB(Max-Planck-Institut fur Astronomie
(Germany)), AC(Landessternwarte
Heidelberg-Konigstuhl (Germany)),
AD(Landessternwarte Heidelberg-Konigstuhl
(Germany)), AE(Landessternwarte
Heidelberg-Konigstuhl (Germany)),
AF(Landessternwarte Heidelberg-Konigstuhl (Germany))
Publication: Ground-based Instrumentation for Astronomy. Edited
by Alan F. M. Moorwood and Iye Masanori. Proceedings
of the SPIE, Volume 5492, pp. 1343-1350 (2004).
(SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551288
Bibliographic Code: 2004SPIE.5492.1343S
Abstract
LUCIFER (LBT NIR-Spectroscopic Utility with Camera and Integral-Field
Unit for Extragalactic Research) is a NIR spectrograph and imager
(wavelength range 0.9 to 2.5 micron) for the Large Binocular Telescope
(LBT) on Mt. Graham, Arizona. It is built by a consortium of five German
institutes and will be one of the first light instruments for the LBT.
Later, a second copy for the second mirror of the telescope will follow.
Both instruments will be mounted at the bent Gregorian foci of the two
individual telescope mirrors. The instrument is equipped with three
exchangeable cameras for imaging and spectroscopy: two of them are
optimized for seeing-limited conditions, the third camera for the
diffraction-limited case with the LBT adaptive secondary mirror working.
The spectral resolution will allow for OH suppression. Up to 33
exchangeable masks will be available for longslit and multi-object
spectroscopy (MOS) over the full field of view (FOV). The detector will
be a Rockwell HAWAII-2 HgCdTe-array. Extensive tests were done for all
the electro-mechanical functions. Those include the grating selection
and the grating tilt unit and the drive for the fold mirror to
compensate for image movement due to flexure. Furthermore several
optical and opto-mechanical units were tested. The procedures and
results of the tests are presented in detail and compared with the
specifications.
Title: LUCIFER status report, summer 2004
Authors: Mandel, Holger; Appenzeller, Immo;
Seifert, Walter; Baumeister, Harald;
Bizenberger, Peter; Dettmar, Ralf-Juergen;
Gemperlein, Hans; Grimm, Bernhard;
Herbst, Tom M.; Hofmann, Reiner; Jutte, Marcus;
Laun, Werner; Lehmitz, Michael;
Ligori, Sebastiano; Lenzen, Rainer;
Polsterer, Kai; Rohloff, Ralf-Rainer;
Schuetze, Andreas; Seltmann, Andreas;
Weiser, Peter; Weisz, Harald; Xu, Wenli
Affiliation: AA(Landessternwarte Heidelberg-Konigstuhl
(Germany)), AB(Landessternwarte
Heidelberg-Konigstuhl (Germany)),
AC(Landessternwarte Heidelberg-Konigstuhl
(Germany)), AD(Max-Planck-Institut fur Astronomie
(Germany)), AE(Max-Planck-Institut fur Astronomie
(Germany)), AF(Ruhr-Univ. Bochum (Germany)),
AG(Max-Planck-Institut fur extraterrestrische Physik
(Germany)), AH(Max-Planck-Institut fur Astronomie
(Germany)), AI(Max-Planck-Institut fur Astronomie
(Germany)), AJ(Max-Planck-Institut fur
extraterrestrische Physik (Germany)), AK(Ruhr-Univ.
Bochum (Germany)), AL(Max-Planck-Institut fur
Astronomie (Germany)), AM(Landessternwarte
Heidelberg-Konigstuhl (Germany)),
AN(Max-Planck-Institut fur Astronomie (Germany)),
AO(Max-Planck-Institut fur Astronomie (Germany)),
AP(Ruhr-Univ. Bochum (Germany)),
AQ(Max-Planck-Institut fur Astronomie (Germany)),
AR(Landessternwarte Heidelberg-Konigstuhl
(Germany)), AS(Landessternwarte
Heidelberg-Konigstuhl (Germany)), AT(Fachhochschule
Mannheim (Germany)), AU(Max-Planck-Institut fur
extraterrestrische Physik (Germany)),
AV(Max-Planck-Institut fur Astronomie (Germany))
Publication: Ground-based Instrumentation for Astronomy. Edited
by Alan F. M. Moorwood and Iye Masanori. Proceedings
of the SPIE, Volume 5492, pp. 1208-1217 (2004).
(SPIE Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.551302
Bibliographic Code: 2004SPIE.5492.1208M
Abstract
LUCIFER (LBT NIR Spectrograph Utility with Camera and Integral-Field
Unit for Extragalactic Research) is a NIR spectrograph and imager for
the LBT (Large Binocular Telescope) working in the wavelength range from
0.9 to 2.5 microns. The instrument is to be built by a consortium of
five german institutes (Landessternwarte Heidelberg (LSW), Max Planck
Institut for Astronomy (MPIA), Max Planck Institut for Extraterrestric
Physics (MPE), Astronomical Institut of the Ruhr-University Bochum
(AIRUB) and Fachhochschule for Technics and Design Mannheim (FHTG)).
LUCIFER will be one of the first light instruments of the LBT and will
be available to the community at the end of 2005. A copy of the
instrument for the second LBT mirror follows about one year later. The
paper presents a brief status report of the procured and built hardware,
of the workpackages already carried out and summarizes the ongoing work
in progress.
Title: Optical alignment of the LBT prime focus camera
Authors: Diolaiti, Emiliano; Farinato, Jacopo;
Ragazzoni, Roberto; Vernet, Elise;
Arcidiacono, Carmelo; Faccin, Fabio
Affiliation: AA(INAF, Osservatorio Astronomico di Bologna
(Italy)), AB(INAF, Osservatorio Astrofisico di
Arcetri (Italy)), AC(INAF, Osservatorio Astrofisico
di Arcetri (Italy)), AD(INAF, Osservatorio
Astrofisico di Arcetri (Italy)), AE(Univ. degli
Studi di Firenze (Italy)), AF(Univ. degli Studi di
Padova (Italy))
Publication: Ground-based Instrumentation for Astronomy. Edited
by Alan F. M. Moorwood and Iye Masanori. Proceedings
of the SPIE, Volume 5492, pp. 513-524 (2004). (SPIE
Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.552224
Bibliographic Code: 2004SPIE.5492..513D
Abstract
While this paper is written, the Blue channel of the double prime focus
camera for the Large Binocular Telescope is being commissioned at the
telescope. We report here on the optical alignment of the prime focus
corrector, a rather challenging activity, due to the tight alignment
tolerances and to the size of the lenses. Furthermore we describe the
current plans about the alignment of the prime focus corrector with the
primary mirror of the telescope, which is foreseen in the next few
months.
Title: Optical design of the PEPSI high-resolution
spectrograph at LBT
Authors: Andersen, Michael I.; Spano, Paolo;
Woche, Manfred; Strassmeier, Klaus G.; Beckert, Erik
Affiliation: AA(Astrophysikalisches Institut Potsdam (Germany)),
AB(INAF, Osservatorio Astronomico di Palermo
(Italy)), AC(Astrophysikalisches Institut Potsdam
(Germany)), AD(Astrophysikalisches Institut Potsdam
(Germany)), AE(Fraunhofer Institut fur Angewandte
Optik und Feinmechanik (Germany))
Publication: Ground-based Instrumentation for Astronomy. Edited
by Alan F. M. Moorwood and Iye Masanori. Proceedings
of the SPIE, Volume 5492, pp. 381-388 (2004). (SPIE
Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550533
Bibliographic Code: 2004SPIE.5492..381A
Abstract
PEPSI is a high-resolution, fiber fed echelle spectrograph with
polarimetric capabilities for the LBT. In order to reach a maximum
resolution R=120.000 in polarimetric mode and 300.000 in integral light
mode with high efficiency in the spectral range 390-1050~nm, we designed
a white-pupil configuration with Maksutov collimators. Light is
dispersed by an R4 31.6 lines/mm monolithic echelle grating mosaic and
split into two arms through dichroics. The two arms, optimized for the
spectral range 390-550~nm and 550-1050~nm, respectively, consist of
Maksutov transfer collimators, VPH-grism cross dispersers, optimized
dioptric cameras and 7.5K x 7.5K 8~$,1'<(B CCDs. Fibers of different core
sizes coupled to different image-slicers allow a high throughput,
comparable to that of direct feed instruments. The optical configuration
with only spherical and cylindrical surfaces, except for one aspherical
surface in each camera, reduces costs and guarantees high optical
quality. PEPSI is under construction at AIP with first light expected in
2006.
Title: An overview of instrumentation for the Large
Binocular Telescope
Authors: Wagner, R. Mark
Affiliation: AA(Large Binocular Telescope Observatory/Univ. of
Arizona (USA))
Publication: Ground-based Instrumentation for Astronomy. Edited
by Alan F. M. Moorwood and Iye Masanori. Proceedings
of the SPIE, Volume 5492, pp. 108-120 (2004). (SPIE
Homepage)
Publication Date: 09/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.550645
Bibliographic Code: 2004SPIE.5492..108W
Abstract
An overview of instrumentation for the Large Binocular Telescope is
presented. Optical instrumentation includes the Large Binocular Camera
(LBC), a pair of wide-field (27'x 27') UB/VRI optimized mosaic CCD
imagers at the prime focus, and the Multi-Object Double Spectrograph
(MODS), a pair of dual-beam blue-red optimized long-slit spectrographs
mounted at the straight-through F/15 Gregorian focus incorporating
multiple slit masks for multi-object spectroscopy over a 6\arcmin\ field
and spectral resolutions of up to 8000. Infrared instrumentation
includes the LBT Near-IR Spectroscopic Utility with Camera and Integral
Field Unit for Extragalactic Research (LUCIFER), a modular near-infrared
(0.9-2.5 $,1'<(Bm) imager and spectrograph pair mounted at a bent interior
focal station and designed for seeing-limited (FOV: 4'x 4') imaging,
long-slit spectroscopy, and multi-object spectroscopy utilizing cooled
slit masks and diffraction limited (FOV: 0'.5 x 0'.5) imaging and
long-slit spectroscopy. Strategic instruments under development for the
remaining two combined focal stations include an interferometric
cryogenic beam combiner with near-infrared and thermal-infrared
instruments for Fizeau imaging and nulling interferometry (LBTI) and an
optical bench beam combiner with visible and near-infrared imagers
utilizing multi-conjugate adaptive optics for high angular resolution
and sensitivity (LINC/NIRVANA). In addition, a fiber-fed bench
spectrograph (PEPSI) capable of ultra high resolution spectroscopy and
spectropolarimetry (R = 40,000-300,000) will be available as a principal
investigator instrument. The availability of all these instruments
mounted simultaneously on the LBT permits unique science, flexible
scheduling, and improved operational support.
Title: LINC-NIRVANA: first attempt of an instrument for a
23-m-class telescope
Authors: Gassler, Wolfgang; Herbst, Thomas M.;
Ragazzoni, Roberto; Andersen, David R.;
Arcidiacono, Carmelo; Baumeister, Harald;
Beckmann, Udo; Bertram, Thomas;
Bizenberger, Peter; Bohnhardt, Hermann;
Diolaiti, Emiliano; Eckart, Andreas;
Farinato, Jacopo; Ligori, Sebastiano;
Rix, Hans-Walter; Rohloff, Ralf-Rainer;
Salinari, Piero; Soci, Roberto;
Straubmeier, Christian; Vernet-Viard, Elise;
Weigelt, Gerd; Weiss, Robert; Xu, Wenli
Affiliation: AA(Max-Planck-Institut fur Astronomie (Germany)),
AB(Max-Planck-Institut fur Astronomie (Germany)),
AC(Max-Planck-Institut fur Astronomie (Germany) and
Osservatorio Astrofisico di Arcetri (Italy)),
AD(Max-Planck-Institut fur Astronomie (Germany)),
AE(Osservatorio Astrofisico di Arcetri (Italy)),
AF(Max-Planck-Institut fur Astronomie (Germany)),
AG(Max-Planck-Institut fur Radioastronomie
(Germany)), AH(Univ. Koln (Germany)),
AI(Max-Planck-Institut fur Astronomie (Germany)),
AJ(Max-Planck-Institut fur Astronomie (Germany)),
AK(Osservatorio Astrofisico di Arcetri (Italy)),
AL(Univ. Koln (Germany)), AM(Osservatorio
Astrofisico di Arcetri (Italy)),
AN(Max-Planck-Institut fur Astronomie (Germany)),
AO(Max-Planck-Institut fur Astronomie (Germany)),
AP(Max-Planck-Institut fur Astronomie (Germany)),
AQ(Osservatorio Astrofisico di Arcetri (Italy)),
AR(Max-Planck-Institut fur Astronomie (Germany)),
AS(Univ. Koln (Germany)), AT(Osservatorio
Astrofisico di Arcetri (Italy)),
AU(Max-Planck-Institut fur Radioastronomie
(Germany)), AV(Max-Planck-Institut fur Astronomie
(Germany)), AW(Max-Planck-Institut fur Astronomie
(Germany))
Publication: Second Backaskog Workshop on Extremely Large
Telescopes. Edited by Ardeberg, Arne L.; Andersen,
Torben. Proceedings of the SPIE, Volume 5382, pp.
742-747 (2004). (SPIE Homepage)
Publication Date: 07/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.566389
Bibliographic Code: 2004SPIE.5382..742G
Abstract
LINC-NIRVANA is a Fizeau interferometer which will be built for the
Large Binocular Telescope (LBT). The LBT exists of two 8.4m mirrors on
one mounting with a distance of 22.8m between the outer edges of the two
mirrors. The interferometric technique used in LINC-NIRVANA provides
direct imaging with the resolution of a 23m telescope in one direction
and 8.4m in the other. The instrument uses multi-conjugated adaptive
optics (MCAO) to increase the sky coverage and achieve the diffraction
limit in J, H, K over a moderate Field of View (2 arcmin in diameter).
During the preliminary design phase the team faced several problems
similar to those for an instrument at a 23m telescope. We will give an
overview of the current design, explain problems related to 20m class
telescopes and present solutions.
Title: Layer-Oriented on paper, laboratory, and soon on the
sky
Authors: Farinato, Jacopo; Ragazzoni, Roberto;
Arcidiacono, Carmelo; Paolo, Bagnara;
Baruffolo, Andrea; Baumeister, Harald;
Bisson, Raffaella; Bohnhardt, Hermann;
Brindisi, Angela; Brynnel, Joar;
Cecconi, Massimo; Coyne, Julien;
Delabre, Bernhard; Diolaiti, Emiliano;
Donaldson, Rob; Fedrigo, Enrico;
Franza, Francis; Gassler, Wolfgang;
Ghedina, Adriano; Herbst, Thomas M.;
Hubin, Norbert N.; Kellner, Stephan;
Kolb, Johann; Lizon, Jean-Louis;
Lombini, Matteo; Marchetti, Enrico;
Meneghini, Gianluigi; Mohr, Lars;
Reiss, Roland; Rohloff, Ralf-Rainer;
Soci, Roberto; Vernet, Elise; Weiss, Robert;
Xompero, Marco; Xu, Wenli
Affiliation: AA(INAF-Osservatorio Astrofisico di Arcetri (Italy)
and Max-Planck-Institut fur Astronomie (Germany)),
AB(INAF-Osservatorio Astrofisico di Arcetri (Italy)
and Max-Planck-Institut fur Astronomie (Germany)),
AC(Univ. degli Studi di Firenze (Italy)),
AD(INAF-Osservatorio Astronomico di Padova (Italy)),
AE(INAF-Osservatorio Astronomico di Padova (Italy)),
AF(Max-Planck-Institut fur Astronomie (Germany)),
AG(NIDEK Technologies Srl (Italy)),
AH(Max-Planck-Institut fur Astronomie (Germany)),
AI(INAF-Osservatorio Astrofisico di Arcetri
(Italy)), AJ(European Southern Observatory
(Germany)), AK(Ctr. Galileo Galilei (Spain)),
AL(INAF-Osservatorio Astrofisico di Arcetri
(Italy)), AM(European Southern Observatory
(Germany)), AN(INAF-Osservatorio Astronomico di
Arcetri (Italy) and Univ. degli Studi di Padova
(Italy)), AO(European Southern Observatory
(Germany)), AP(European Southern Observatory
(Germany)), AQ(European Southern Observatory
(Germany)), AR(Max-Planck-Institut fur Astronomie
(Germany)), AS(Ctr. Galileo Galilei (Spain)),
AT(Max-Planck-Institut fur Astronomie (Germany)),
AU(European Southern Observatory (Germany)),
AV(Max-Planck-Institut fur Astronomie (Germany)),
AW(European Southern Observatory (Germany)),
AX(European Southern Observatory (Germany)),
AY(INAF-Osservatorio Astrofisico di Arcetri (Italy)
and Univ. degli Studi di Bologna (Italy)),
AZ(European Southern Observatory (Germany)),
BA(NIDEK Technologies Srl (Italy)),
BB(Max-Planck-Institut fur Astronomie (Germany)),
BC(European Southern Observatory (Germany)),
BD(Max-Planck-Institut fur Astronomie (Germany)),
BE(Max-Planck-Institut fur Astronomie (Germany)),
BF(INAF-Osservatorio Astrofisico di Arcetri
(Italy)), BG(Max-Planck-Institut fur Astronomie
(Germany)), BH(INAF-Osservatorio Astrofisico di
Arcetri (Italy) and Univ. degli Studi di Padova
(Italy)), BI(Max-Planck-Institut fur Astronomie
(Germany))
Publication: Second Backaskog Workshop on Extremely Large
Telescopes. Edited by Ardeberg, Arne L.; Andersen,
Torben. Proceedings of the SPIE, Volume 5382, pp.
578-587 (2004). (SPIE Homepage)
Publication Date: 07/2004
Origin: SPIE
Abstract Copyright: (c) 2004: SPIE--The International Society for
Optical Engineering. Downloading of the abstract is
permitted for personal use only.
DOI: 10.1117/12.566345
Bibliographic Code: 2004SPIE.5382..578F
Abstract
Layer Oriented represented in the last few years a new and promising
aproach to solve the problems related to the limited field of view
achieved by classical Adaptive Optics systems. It is basically a
different approach to multi conjugate adaptive optics, in which pupil
plane wavefront sensors (like the pyramid one) are conjugated to the
same altitudes as the deformable mirrors. Each wavefront sensor is
independently driving its conjugated deformable mirror thus simplifying
strongly the complexity of the wavefront computers used to reconstruct
the deformations and drive the mirror themselves, fact that can become
very important in the case of extremely large telescopes where the
complexity is a serious issue. The fact of using pupil plane wavefront
sensors allow for optical co-addition of the light at the level of the
detector thus increasing the SNR of the system and permitting the usage
of faint stars, improving the efficiency of the wavefront sensor.
Furthermore if coupled to the Pyramid wavefront sensor (because of its
high sensitivity), this technique is actually peforming a very efficient
usage of the light leading to the expectation that, even by using only
natural guide stars, a good sky coverage can be achieved, above all in
the case of giant telescopes. These are the main reasons for which in
the last two years several projects decided to make MCAO systems based
on the Layer Oriented technique. This is the case of MAD (an MCAO
demonstrator that ESO is building with one wavefront sensing channel
based on the Layer Oriented concept) and NIRVANA (an instrument for
LBT). Few months ago we built and successfully tested a first prototype
of a layer oriented wavefront sensor and experiments and demonstrations
on the sky are foreseen even before the effective first light of the
above mentioned instruments. The current situation of all these projects
is presented, including the extensive laboratory testing and the
on-going experiments on the sky.
Title: Supernova 2004cv in MCG +03-41-120
Authors: Schwarz, G.; Karam, A.; Wagner, R. M.;
Rohrbach, J. G.; Starrfield, S.
Publication: IAU Circ., 8364, 2 (2004). Edited by Green, D. W.
E. (IAUC Homepage)
Publication Date: 07/2004
Origin: CBAT
Objects: 2004cv
Bibliographic Code: 2004IAUC.8364....2S
Abstract
IAUC 8364 available at Central Bureau for Astronomical Telegrams.
Title: The Development Process of the LUCIFER Control
Software
Authors: Jütte, M.; Polsterer, K.; Lehmitz, M.
Publication: Astronomical Data Analysis Software and Systems
(ADASS) XIII, Proceedings of the conference held
12-15 October, 2003 in Strasbourg, France. Edited by
Francois Ochsenbein, Mark G. Allen and Daniel Egret.
ASP Conference Proceedings, Vol. 314. San Francisco:
Astronomical Society of the Pacific, 2004., p.712
Publication Date: 07/2004
Origin: AUTHOR
Bibliographic Code: 2004ASPC..314..712J
Abstract
We present the design and development process of the control software
for the LBT NIR spectroscopic Utility with Camera and Integral-Field
Unit for Extragalactic Research (LUCIFER) which is one of the
first-light instruments for the LBT on Mt. Graham, Arizona. The LBT will
be equipped with two identical LUCIFER instruments for both mirrors. We
give an overview of the software architecture and the current state of
the software package and describe the development process by using a
virtual LUCIFER instrument.
Title: An Overview of the Large Binocular Telescope Control
System
Authors: Axelrod, T. A.; de La Peña, M. D.
Publication: Astronomical Data Analysis Software and Systems
(ADASS) XIII, Proceedings of the conference held
12-15 October, 2003 in Strasbourg, France. Edited by
Francois Ochsenbein, Mark G. Allen and Daniel Egret.
ASP Conference Proceedings, Vol. 314. San Francisco:
Astronomical Society of the Pacific, 2004., p.704
Publication Date: 07/2004
Origin: AUTHOR
Bibliographic Code: 2004ASPC..314..704A
Abstract
The Large Binocular Telescope (LBT) consists of two 8.4-meter mirrors on
a common mount. This configuration provides the light gathering power
equivalent to an 11.8-meter telescope and the resolving power of an
22.8-meter telescope. Due to the binocular nature of the telescope,
there are unique requirements imposed on the telescope control system
(TCS) to ensure the health and safety of the telescope, while also
enabling observations in both independent and interferometric mode.
This paper presents an overview of the design of the TCS, from the
graphical user interface (GUI) and the plotting and analysis
capabilities at the highest interaction level to the low-level
interfaces for the software.
Title: The science case of the PEPSI high-resolution
echelle spectrograph and polarimeter for the LBT
Authors: Strassmeier, K. G.; Pallavicini, R.;
Rice, J. B.; Andersen, M. I.
Affiliation: AA(Astrophysical Institute Potsdam (AIP), An der
Sternwarte 16, 14482 Potsdam, Germany; Universität
Potsdam, Am Neuen Palais 10, 14469 Potsdam,
Germany), AB(INAF - Osservatorio Astronomico di
Palermo, Piazza del Parlamento 1, 90134 Palermo,
Italy), AC(Department of Physics, Brandon
University, Brandon, Manitoba R7A 6A9, Canada;
Astrophysical Institute Potsdam (AIP), An der
Sternwarte 16, 14482 Potsdam, Germany),
AD(Astrophysical Institute Potsdam
