Transcript NEWFIRM: the NOAO Extremely Wide Field IR Imager

NEWFIRM: the NOAO
Extremely Wide Field IR
Imager
Presented by Ron Probst,
Project Scientist
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
NEWFIRM is …
An infrared camera with
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Wide field of view
Subarcsecond resolution
High sensitivity
Near infrared capability
( 28 x 28 arcmin)
( 0.4 arcsec/pixel )
( throughput, QE, 4-m aperture)
( 1-2.5 microns, 5<R<75)
…integrated into a system for
– Deep wide field surveys
– Rapid data turnaround
– Public data access
( efficient operation on telescope )
( pipeline reduction )
( NVO archive )
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
Widefield deep IR imaging in the large telescope era
• Study of growth of structure and complexity in the Universe
• 1-2.4 μm region physically rich, readily accessible
• 6-10 meter telescopes: Superb image quality over small fields
• NOAO 4-m’s well matched to deep wide survey needs
• Variety of exciting science programs
• Widely recognized need for US competitiveness
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
Major science themes
Cosmological properties of the Universe
Supernova search at z > 1
Evolution of large scale structure
Galaxy clustering evolution at z > 1
Formation and evolution of individual galaxies
Assembly and growth of galaxies at 1 < z < 3
Assembly and present structure of Galactic disk and halo
Formation of stars and stellar systems
Determination of the IMF in various environments
Mass, energy, and chemical exchange between stars and ISM
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NEWFIRM in
the suite of US
facilities
Deep widefield
imaging feeds high
spatial and/or
spectral resolution
instruments on
modern 4-10 m
telescopes, public
and private
NOAO Users Committee
meeting 23 Oct 2003
NEWFIRM
NOAO Users Committee
meeting 23 Oct 2003
NOAO Extremely Wide Field Infrared Imager
NEWFIRM in a global context
2005
2010
NEWFIRM
Magellan II
(rescoped)
CFHT
UKIDSS Surveys
UKIRT
VISTA
Surveys
Gemini N
IR instrument suite rampup
Gemini S
HST
SIRTF
SOFIA
Herschel
JWST
Next gen
instruments
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
Evolution of galaxies and galaxy clustering
at 1 < z < 3
Track assembly and spatial clustering of galaxies with a masssensitive probe  gravity driven phenomena
Compare with hierarchical formation theories
Abundance of rich clusters tests CDM variants
Need large area for sample size, linear dimension comparable to
power spectrum turnover length
Complementary observations: optical imaging survey (star
formation rate sensitive)
Followup observations: spectroscopic redshifts, high resolution
imaging (morphologies)
Added value: distant halo stars, high-z SN, QSOs, rare gal types
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
IMF, SFR, and YSOs in space and time
Quantify IMF and SFR in molecular clouds over large area, long time
Quantify range of lifetimes for disk accretion phase of YSOs
Input to definition of disk properties during planetary system formation
Need very large area, moderate depth, multiple epochs
Complementary observations: optical and X-ray surveys, optical proper
motions
Followup observations: NIR spectral classification, selected deep L-band
imaging, high resolution O/IR imaging and spectroscopy
Added value: evolution of angular momentum, structure of convective
stars; time domain science
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
Executing the science programs
• Survey mode: large scale, long term, project team
– Primary plus ancillary science; public archive for data mining
– Uniformity and rapid turnaround of data product
• General observer mode: short term, small group
– Specific science goal, hands-on observing/reduction
– Large data volumes compared to present instruments
• Science advisory committee: small external group
– Organization and execution of survey science
– Related scientific and technical issues
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
System elements: from photons to science
photons
KPNO
4-m telescope
CTIO
guider
NEWFIRM
instrument
ORION:
NOAO
USNO
NASA Ames
Raytheon
IR array
mosaic
S
W
MIP/NF
Tucson
La Serena
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
Array
controller
MIP/MONSOON
Tucson
La Serena
S
W
Data handling
system
Surveys
PI science
Special purpose
Science data
pipeline
Science
users
Science
archive
science
NOAO Users Committee
meeting 23 Oct 2003
Data Products:
3 teams +
U. Maryland
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
Optomechanical
Layout
NOAO Users Committee
meeting 23 Oct 2003
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
Orion Focal Plane Module
Clock and Biases
Output Current Mirrors
Light Baffles
Outputs 1-32
Outputs 33-64
Invar36 Pedestal
AlN
Motherboard
Alignment Locator
Detector SCA
Photo Courtesy RIO
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
System software components
• Observation control system: prep, setup, data taking
– Code re-use from working systems
– NOAO and other sources
• Data handling system: capture, verify, transport data
– SW technology from large physics experiments
– Initial deployment in place
• Pipeline to archive: high quality, uniform data reduction
– Toolkit and methods from SQIID, DeepWide, Las Campanas
– MOSAIC pipeline is pathfinder for NEWFIRM
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
Project status October 2003
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Finishing detailed hardware design
Initial hardware releases to La Serena, Tucson shops
Optics in fabrication at vendors
Filters received ( J H KS )
MONSOON first light with IR array August 2003
Negotiating detector foundry run
Software tasks proceeding as planned
 On schedule to first light 7/05
NEWFIRM
NOAO Extremely Wide Field Infrared Imager
NOAO Users Committee
meeting 23 Oct 2003
Back to the future
What does NEWFIRM bring to future efforts?
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Design solutions for large instruments
Detector and acquisition system development
Observing tools supporting high degree of automation
Understanding of pipeline processing and its limits
Archiving and cataloging tools and methods
• US community experience with large scale survey science
The SOAR Adaptive Optics
System
Presented by Andrei Tokovinin,
Project Scientist
SOAR Adaptive Optics
A. Tokovinin
Telescope system in Chile
We need:
Resolution ~0.3”
Field 3’-5’
Full sky coverage
Imaging+spectroscopy
Can it be done?
Can we afford it?
Resolution is important!
0.3”
0.7”
 Resolution: 2-3 times
 mlim [sky]: gain 0.5-1 mag (rival 8-m)
 mlim [confusion]: gain 1-2 mag (half-way to HST)
Rayleigh UV Laser
Guide Star at 10km
Solution:
Ground-layer
compensation
Partial compensation
of high layers
Good compensation
of low layers
Deformabe mirror
1’
2’
3’
seeing
Seeing at Cerro Pachon
• Median seeing: 0.67”
(Gemini campaign)
• Turbulence profiles:
May-Sept. 2002 at Tololo,
January 2003 at Pachon
Free-atm. + ground layer:
~1”
Free atmosphere only:
~0.2”
A good night: January 15, 2003
Prediction for SOAR AO
25% 50% 75%
β,”
0.94
1.11
1.33
0.5μm
0.38
0.53
0.71
0.7μm
0.22
0.31
0.49
1μm
0.17
0.22
0.30
[arcseconds]
21 nights
January 2003
Sample science with SOAR AO
 Photometry of distant supernovae
 Dynamics and kinematics of galaxies
(with IFU)
 Clusters in Galaxy, LMC (CMD)
 Morphology of lensed galaxies
 Resolved nearby galaxies (CMD, star formation,
distance scale, post-AGB)
 Planetary and symbiotic nebulae
Imaging+spectroscopy at high angular resolution
History of LMC clusters (K.Olsen)
Ground-based, 1”
SOAR AO, 0.3”
Reaches turn-off
HST, 0.1”
Photometric error
from crowding
Science instruments for SOAR AO
1st light SOAR instruments
• Adaptive secondary
($2M)
• WFS at each
instrument (not planned)
• Pixel scale?
…not a good solution!
or
dedicated?
• CCD imager: 2Kx2K,
0.08” pixels
• SOAR-Brazil IFU
(+ Fabry-Perot?)
• Port for a “visitor”
AO instrument
SOAR AO
on SOAR
ISB
AO module
on ISB
AO module
CCD
Imager
Electronics
 Solid-state Nd:YAG laser
DS20-355 (Photonics)
 =355 nm, 8 W @ 10 kHz
 Cost $138K or cheaper
 Resource ~10000h (~5yr)
Laser
Safety: aircraft and satellite-safe, no visual hazards
Tip-tilt: 2-3 NGS to V=18, complete sky coverage
Control System Block Diagram
CoDR: April 2003
PDR: March 2004
 Lab closed-loop: 2004
 On the sky: 2005
Planning
and cost
Manpower
MY
16.5
K$
589
Capital
K$
540
Total
K$
1.13
Affordable
SOAR partners (MSU+UNC) apply for AODP funding
to build “set-and-forget” Rayleigh laser guide star for SOAR
A road into the future…
 Build reliable and productive AO system
to enhance SOAR science
and
 Demonstrate AO technology scalable to ELTs
 Build AO expertise for TMT and other
projects
 Synergy with Gemini-S (MCAO, NICI)