ISTITUTO NAZIONALE DI ASTROFISICA
24 Giugno 2017 [12:32]
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Evento Id: 223
Oratore:
none
Istituto:
INAF
Dove: Mount Graham - LBT
Data & Ora: 14-05-2010 14:00 (durata: 1 day)
Titolo: 2nd semester Italian time at LBT
-----
Abstract:
LBT Italian Coordination Facility
Centro Italiano di Coordinamento alle Osservazioni LBT
Announcement of opportunity at the Large Binocular Telescope
Italian time
Semester 2010B is now open for proposals
Applications for observing time for the periods:
Oct 6 - Oct 10, 2010
Nov 30 – Dec 4, 2010
are solicited and should be submitted by
Tuesday 14th May, 2009, 14:00 CEST
The Large Binocular Telescope is a binocular facility composed of two 8.4mtelescopes
rigidly mounted, located atop the Mount Graham, Arizona, USA at an
elevation of 3221 m, as part of the Mount Graham International Observatory
(MGIO).
LBT is an international joint project among Italy, Germany and the United
States of America, of which Italy has 25% of the total observing time.
It is currently equipped with a wide field prime focus camera (LBC, Large
Binocular Camera) offering imaging from the ultraviolet to the near-IR wavelengths
(1 micron) at the two telescopes, in single and binocular mode, and a near-IR
imaging and spectrograph camera (LUCIFER) currently available only on the left side
mirror, offering imaging, long-slit and multi-object (MOS) spectroscopy in the near-
IR wavelength range. It can be operated in binocular mode, observing the same field
with the two telescopes and in single telescope mode. The dates available to the
Italian community in the SECOND semester of 2010 are listed above.
Further information can be found at http://lbt.inaf.it and in the links therein.
Who can apply:
The PI of a proposal must be a researcher affiliated to an Italian astronomical
institute or university. Researchers affiliated to other institutions are allowed in the
CoI list up to the 50% of the total number of applicants.
Application forms and proposal submission.
Proposal submission is handled by the TNG system. Forms can be downloaded at
http://lbt.inaf.it/observing.html and proposals must be submitted at
http://www.tng.iac.es/lbt/submit.html within Friday 14th May, 2010, 14:00 CEST.
Offered Instruments and modes:
LBC (Binocular)
LBC is a twin optical imager composed of two identical large field cameras, with a
FoV of ~25' x ~25', mounted at the prime foci of the two telescopes. LBC is a fully
binocular instrument that observes simultaneously the same field with the two
cameras. The camera on the left side (SX) is optimized for the UV/blue wavelength
range and offers imaging in the Bessel filters (U,B,V) and in the SDSS-like filters
(Uspec,g,r). The camera on the right side (DX) is optimized for the red/near-IR
range and offers imaging in the filters V,R,I (Bessel), r,i,z (SDSS), 1μm broad-band
Y and the narrow band F972N20, centered at 972 nm.
Details on the instrument can be found at http://lbc.oa-roma.inaf.it .
LUCIFER
LUCIFER (LBT NIR spectroscopic Utility with Camera and Integral-Field Unit for
Extragalactic Research) is composed of two near-IR spectrographs and imagers
mounted at the Nasmyth foci, of which only the one at the SX telescope is available
for use in this semester (LUCIFER1). It offers imaging, long-slit and multi-object
(MOS) spectroscopy in the wavelength range 1- 2.5 μm over a field-of-view ~4’ x 4’.
All modes currently work in seeing-limited mode. Details on the instrument can be
found at http://www.astro.rub.de/LuciferHome and
http://abell.as.arizona.edu/~lbtsci/Instruments/LUCIFER/lucifer.html
Evaluation of the exposure times
The LBC Exposure Time Calculator is available at:
http://lbc.oa-roma.inaf.it/cgi-bin/ETC.pl.
The LUCIFER is available at:
http://www.lsw.uni-heidelberg.de/lucifer-cgi/calculator/calculator.py
For both instruments, applicants must compute and specify in the proposal only the
net exposure time requested (including special calibrations, see below), with no
correction for overheads.
Calibrations and Pre-imaging
All applicants must describe the calibration needs of their proposal in Sect. 14.
Standard calibrations are typically taken at the beginning and at the end of night, or
in daytime. These include bias/dark, flats and photometric standards for imaging,
and darks, flat-field and arcs for spectroscopic modes. Due to feasibility limitations,
the availability of standards and flat in the same night of the science data is not
guaranteed.
The standard calibrations described above are not accounted for in the total
requested time.
Any other specific need, requiring observations during night-time (like e.g. (spectro)-
photometric standards taken between consecutive observations, IR telluric standard
etc) must be described in Sect. 14 and accounted for in the requested time.
Photometric standards with LBC or LUCIFER need 15 min. each to be executed, while
telluric spectroscopic standards require 30min each.
Pre-imaging is not required for MOS observations with LUCIFER. Masks can be
prepared using the LUCIFER dedicated tool (LMS) using a pre-existing image (in any
wavelength) with accurate WCS astrometry. Thanks to the low distortion in LUCIFER,
the resulting masks are accurate for all slit widths equal or larger than 1”.
If the target coordinates are not known with the required accuracy, and a LUCIFER
or LBC image is needed to locate the objects, the corresponding observing time must
be explicitly requested in the proposal.
Targets and observing runs
Each proposal is split into one or more “runs”, following the ESO definition. In
practice, a “run” is the smallest part of an observing program which delivers selfcontained
results. Each “run” is defined by one target and one observing mode of a
specific instruments only (different filters or grisms on one target are allowed within
one “run”). Each “run” may be evaluated independently and given different priorities
by the TAC.
Target of Opportunity (ToO)
ToOs will be available in this semester, in two categories.
Soft-ToO are intended for targets whose coordinates are not known at the moment
of submitting a proposal, but which will be available at the beginning of the Italian
observing run. Relevant observations will be executed in one of the nights of the
italian run, following the scientific rank provided by the TAC.
Hard-ToO are intended for targets whose coordinates are not known at the moment
of submitting a proposal and that must be observed as promptly as possible.
If approved by TAC, the Hard-ToO observations will be given the highest prioirity and
executed as soon as possible.
In the proposal, the applicants must clearly describe the maximum time lag after the
triggering event during which the observations are useful. A maximum number of
two hard-ToOs for a total for 4 observing hours are available in this period.
ToOs of both categories cannot be requested for LUCIFER1 MOS observations.
Time-constrained or time-critical observations cannot be requested, even for targets
of known coordinates.
Proposal Evaluation:
The proposals will be evaluated by the INAF Time Allocation Committee, the same
appointed for the TNG and REM proposals.
Collaborative programs aiming at using also observing time from other LBT partners
are encouraged, although each application will be independently evaluated by the
competent TAC.
A schedule of observing periods allocated to the other LBT partners can be found at
http://lbt.inaf.it/observing.html
Observing modes:
The observations will be conducted in service mode. Programs will be executed by
their scientific ranking, as established by the TAC, regardless of the requested
instrument(s), and respecting the observational constraints requested by the
applicants.
Standard calibrations will be provided by the service observers. Special calibration
should be described in the proposal and included in the total time request.
Data Flow:
All the scientific data from LBC and LUCIFER will be stored at the IA2 italian archive
(http://wwwas.oats.inaf.it/IA2/) in raw form, and are accessible to the P.I. within
few days from the observations.
Imaging data from LBC and LUCIFER will be reduced at the LBC Survey Center (LSC)
at OAR and made available to the P.I. at http://deep01.oa-roma.inaf.it/. The LSC
staff will also provide user support for those willing to reduce data with their own
software.
A similar support for the data reduction of LUCIFER spectroscopic data is under
development at IASF-Mi and a preliminary version of such support will likely be
available for these runs.
For further information, send an e-mail to lbt_info at inaf.it. 
-----
Tipo di Evento: Scadenza Proposal
Link: link
Presentazioni Disponibili:
Non fornita


 
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