Transcript Slide 1

Requirements on array detectors from the
OWL Instrument Concept Studies
Sandro D’Odorico
European Southern Observatory
SDW 2005
TAORMINA
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
the spectral
range from
The
Instrument
Conceptcover
Study
final Reports
the blue to sub-mm with different scientific field of
views
are
duequality
in September-October
2005. This
and
image
requirements
advanced overview of the detectors
The scope of the studies is:
requirements is based on the work in
• to support the OWL science cases
progress.
• to verify with actual instrument concepts interfaces and
operation scheme
of the telescope
Thanks
to the design
P.I.s!
• to check feasibility of instrument concepts and identify
needs and required R&D for the different subsystems
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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
250-450850 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- Arcetri
Heidelberg 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
Hypertelescope
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 EXperiment
Concept Study carried out by ESO, Cambridge,
Geneve and INAF Oss. Trieste
Portion of the Ly  forest at z=3 
Main Goal
A 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)
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
Requirements
Spectral range: 400-650 nm
Resolution 100000-150000
Stability 1cm/s with long term
absolute calibration
Concept
The light is sent to 5 separate echelle
spectrographs a la HARPS (in
vacuum, at very stable T)
Detector estate
The 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
Camera
Echelle mosaic
22 x 170 cm
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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
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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
Preliminary detector requirements from EPICS
Mode
Field
(arcsec)
Pixel
R
Total Array
Estate
Differential Imaging
4x4
0.5 mas
2( 8K x 8K) IR
Polarimetry
2x2
0.5 mas
8K x 4K , fast
read-out
IFS red
1x1
0. 35 mas
10
8K x 8K CCD
2x2
0.5 mas
10-50
8K x 8K NIR
J band
Wawefront Sensor for
EXAO
=
3K x 3K, ~1KHz
(SH)
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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
f/1
0.7
0.6
f/1
0.4
…
M = 1/6
0.5
…
Detection Efficiency
OWL focus
f/1
f/6
SPAD
Multilayer 78 nm SiO2 50 nm Si3N4
120 nm SiO2
No coating
0.3
0.2
M = 1/10
0.1
0
400
450
500
550
600
650
700
750
800
Wavelength [nm]
SPADA Test Chip-PoliMi
AR coatings on SPAD-courtesy of S.Cova
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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), 12m 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
Ceramic PCB
Resolution <2 arcsec
40x32 sub-array
Niobium
Flex Cable
subarray
SQUID
Series
Array
Amplifiers
Readout
PCBs
Woven Cables to Room Temperature
4 SCUBA 2 TES Detectors (20480 pix)
Transition Edge Sensors hybridized to a Superconducting Quantum
Interference Design (SQUID) time-division multiplexer
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