requirements on array detectors from the owl instrument concept studies sandro d’odorico european...
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Requirements on array detectors from the
OWL Instrument Concept Studies
Sandro D’OdoricoEuropean Southern Observatory
SDW 2005TAORMINA
SDW _ 20.6.2005_S.D’Odorico/ 2
OWL INSTRUMENT CONCEPT STUDIES
Framework, Scope, Status
8 Instrument Studies were launched in 2004 by ESO in the framework of the 100m OWL Concept Study,
The present set of instruments cover the spectral range from the blue to sub-mm with different scientific field of views and image quality requirements
The scope of the studies is:
• to support the OWL science cases
• to verify with actual instrument concepts interfaces and operation scheme of the telescope design
• to check feasibility of instrument concepts and identify needs and required R&D for the different subsystems
The Instrument Concept Study final Reports are due in September-October 2005. This
advanced overview of the detectors requirements is based on the work in
progress.
Thanks to the P.I.s!
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OWL Instrument Concept Studies (status June2005)
Instrument Wave range (m)
Capability Primary Science Goals (current guess)
Institutes External Responsible
Responsible at ESO
CODEX 0.4-0.7 High velocity accuracy, visual spectrograph
To measure the dynamics of the Universe
ESO, INAF-Ts, Geneve Obs, IoA
Cambridge
= L. Pasquini
T-OWL 2.5-20 Thermal, Mid Infrared Imager and possibly
Spectrograph
Search, study of planets, high redshift H galaxies
MPIfA, Heidelberg, Leiden Obs., ESO
R. Lenzen H.U. Kaeufl
QUANTEYE 0.4-1 Study will review /explore aspects of quantum
astrophysics with OWL
Astrophysical phenomena varying at sub-second time scale, others
tbd
Padova Univ., Lund University
C.Barbieri and D. Dravins
R. Fosbury
SCOWL 250-450-850 tbc
Imaging at sub-millimeter wavelengths
Surveys of dusty regions, of extr. fields for star-forming galaxies
ATC I. Egan R. Siebenmorgen
MOMFIS 0.8-2.5 Near IR spectroscopy with multi-object,multi field
units
Masses of high z galaxies, regions of star formation, GC stars
CRAL, LAM, OPM J.G. Cuby M. Casali
Large Field IR camera
0.8-2.5 NIR Imaging Camera on a field of 1x1 / 2x2 arcmin
Faint stellar and galaxy population INAF- ArcetriHeidelberg MPIfA
R. Ragazzoni E. Marchetti
EPICS 1-5 tbc
NIR Camera-Spectrograph at diffraction
limit(+coronograph)
Imaging and spectroscopy of earth-like planets
ESO + ext. experts = N.Hubin
Hyper-telescope Camera
1-2.5 Speckle interferometry with a partially filled
OWL aperture
Planetary disks, exo-planets LISE lab at OHP V. Borkowski G. Monnet
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Cosmic Dynamics EXperimentConcept Study carried out by ESO, Cambridge,
Geneve and INAF Oss. Trieste
Main GoalA direct measurement of the
cosmic acceleration
Obtained by comparing high resolution spectra of the Ly forest and metal systems in the direction of bright QSOs
over a large time interval (10 years or more)
Portion of the Ly forest at z=3
Simulation of the difference between 2 epochs
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Cosmic Dynamics EXperiment
Concept Study carried out by ESO, Cambridge, Geneve and INAF Trieste
RequirementsSpectral range: 400-650 nmResolution 100000-150000
Stability 1cm/s with long term absolute calibration
ConceptThe light is sent to 5 separate echelle
spectrographs a la HARPS (in vacuum, at very stable T)
Detector estateThe spectra are spread out over 60 2K x 4K CCD (15 pixel). Within a factor
of 2, depending on telescope size and resolution. r.o.n 1-2 e-,d.c. 1e/pix/h
Echelle mosaic 22 x 170 cm
Camera
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Earth-like Planet Imaging Camera Spectrograph
Concept study by ESO and a number of scientists and engineers from different institutes in F, I, D,NL and SUI
EPICS starting point are the current studies for the Planet Finder at the VLT
The instrument aims at the detection and characterization of earth-like planets
The AO system for this instrument is expected to be a combination of the standard system offered by the telescope + an EXAO internal to the instrument
The observing modes being presently considered are Differential Imaging, Polarimetry and Integral Field Spectroscopy in the visual and Y,J bands
SDW 2005 _ 20.6.2005_S.D’Odorico/ 5b
Earth-like Planet Imaging Camera Spectrograph
Concept study by ESO and a number of scientists and engineers from different institutes in F, I, D,NL and SUI
Mode Field (arcsec)
Pixel R Total Array Estate
Differential Imaging 4 x 4 0.5 mas 2( 8K x 8K) IR
Polarimetry 2 x 2 0.5 mas 8K x 4K , fast read-out
IFS red 1 x 1 0. 35 mas 10 8K x 8K CCD
J band 2 x 2 0.5 mas 10-50 8K x 8K NIR
Wawefront Sensor for EXAO
= 3K x 3K, ~1KHz (SH)
Preliminary detector requirements from EPICS
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QUANTEYE
Concept Study carried out by Dept.of Astronomy, Univ. Padova and Observatory, Univ. Lund (P.I.s C.
Barbieri and D.Dravins)
Ultra-fast photometer for Quantum Astronomy
Main mode: to study the single photon arrival time statistics at the largely unexplored 10-3 -10 -9 second resolution. Large advantage from telescope size when studying photon correlation.
Wavelength range 400-700 nm, target on axis + reference in the 3 arcmin field, 2D resolution not required,
Single photon counting detectors with required ns resolution , high efficiency, low dark current
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QUANTEYE
Concept Study carried out by Univ. Padova and Univ. Lund (P.I.s C. Barbieri and D.Dravins)
1 arcsec in OWL focalplane ~ 3mm. Present concept: to sample collimated beam in 100 subpupils
Possible Detectors: 2 disperse arrays of 10 x 10 Si Single Photon Avalanche Diode (SPAD-A)
Antireflection Coating on SPADs
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
400 450 500 550 600 650 700 750 800
Wavelength [nm]
Det
ectio
n E
ffic
ienc
y
Multilayer 78 nm SiO2 50 nm Si3N4
120 nm SiO2
No coating
AR coatings on SPAD-courtesy of S.Cova
OWL focus f/6f/1
f/1
… …
f/1 SPAD
M = 1/6 M = 1/10
SPADA Test Chip-PoliMi
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Large-Field NIR Camera
Concept Study carried out by INAF-Arcetri and MPIfA Heidelberg (P.I. R. Ragazzoni)
•J,H,K; central field (30-60 arcsec diameter sampled at ~diffraction limit); outer field 3-6 arcmin. Choice dictated by AO performance, science case, cost and complexity.
•MCAO using 2-3 DM for the central part, GLAO for the outer part
Detector Requirements
Central field of 30” sampled at 1mas (Nyquist at K) 15 x15 (2K x 2K)Hg Cd Te arrays (or 8 x 8 (4K x 4K), 12m pixels)
Outer field (e.g. 3’ x 3’) with a 10mas sampling 9 x 9 (2K x 2K)Hg Cd Te arrays
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Multi–Object Multi–Field Imager Spectrograph
Concept Study carried out by LAS Marseille, GEPI, Obs. Meudon, Obs. Lyon (P.I. J.G. Cuby)
Multi-IFU (30) system to pick up targets over the 3’ (6’) scientific field
“local” AO using mini DM in the light path of each IFU
Spectroscopy J or H or K in one shot at R= 4000
Spatial sampling 50 mas, N pixels per IFU 30 x30
18 Hg Cd Te (2K x 2K) arrays / band
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T – OWL (Thermal IR Camera - Spectrograph for OWL)
Concept Study carried out by MPIfA Heidelberg and Leiden Observatory (P.I. R. Lenzen)
Wavelength Range: 3- 27 m
Imaging Pixel Scale: 3.5 mas@ 3-5 m,
7.0 mas @ 7-14 and 16-25 m
FOV 15x15 arcsec
4 (2k x 2k) InSb (0.9 – 5.4 m)
4 (1k x1k) Si-As (2-28 m)*
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SCOWL (SCUBA at OWL)
Concept Study carried out by ATC (P.I. I. Egan)
Imager in the 350 and 450 m bands (850 m desiderable)
FOV 2 x 2 arcmin, Surveyer for ALMA targets Resolution <2 arcsec
4 SCUBA 2 TES Detectors (20480 pix)
Transition Edge Sensors hybridized to a Superconducting Quantum Interference Design (SQUID) time-division multiplexer
Ceramic PCB 40x32 sub-array
NiobiumFlex Cable
Woven Cables to Room Temperature
SQUIDSeriesArray
Amplifiers
Ceramic PCB 40x32 sub-array
NiobiumFlex Cable
Woven Cables to Room Temperature
SQUIDSeriesArray
Amplifiers
subarray
Readout PCBs
subarray
Readout PCBs