newfirm: the n oao e xtremely w ide f ield ir i m ager
DESCRIPTION
NEWFIRM: the N OAO E xtremely W ide F ield IR I m ager. Presented by Ron Probst, Project Scientist. NEWFIRM is …. An infrared camera with Wide field of view ( 28 x 28 arcmin) Subarcsecond resolution ( 0.4 arcsec/pixel ) High sensitivity ( throughput, QE, 4-m aperture) - PowerPoint PPT PresentationTRANSCRIPT
NEWFIRM: the NOAO Extremely Wide Field IR
Imager
Presented by Ron Probst, Project Scientist
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRM is …
An infrared camera with– Wide field of view ( 28 x 28 arcmin)
– Subarcsecond resolution ( 0.4 arcsec/pixel )
– High sensitivity ( throughput, QE, 4-m aperture)
– Near infrared capability ( 1-2.5 microns, 5<R<75)
…integrated into a system for– Deep wide field surveys ( efficient operation on telescope )
– Rapid data turnaround ( pipeline reduction )
– Public data access ( NVO archive )
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO 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
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
Major science themes
Cosmological properties of the UniverseSupernova search at z > 1
Evolution of large scale structure Galaxy clustering evolution at z > 1
Formation and evolution of individual galaxiesAssembly and growth of galaxies at 1 < z < 3Assembly and present structure of Galactic disk and halo
Formation of stars and stellar systems Determination of the IMF in various environmentsMass, energy, and chemical exchange between stars and
ISM
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
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
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRM in a global context
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO 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 mass-sensitive probe gravity driven phenomena
Compare with hierarchical formation theoriesAbundance 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
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO 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 timeQuantify range of lifetimes for disk accretion phase of YSOsInput 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 motionsFollowup observations: NIR spectral classification, selected deep L-band imaging,
high resolution O/IR imaging and spectroscopyAdded value: evolution of angular momentum, structure of convective stars; time
domain science
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO 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
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
System elements: from photons to science
photons
4-m telescope
guider
NEWFIRMinstrument
IR arraymosaic
KPNO CTIO
MIP/NFTucsonLa SerenaORION:
NOAOUSNONASA AmesRaytheon
SW
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
Arraycontroller
Data handlingsystem
Science datapipeline
Scienceusers
MIP/MONSOONTucsonLa Serena
Sciencearchive
science
Data Products:3 teams +U. MarylandSurveys
PI scienceSpecial purpose
SW
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
OptomechanicalLayout
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
Invar36 Pedestal AlN Motherboard
Detector SCA
Alignment Locator
Output Current Mirrors
Light Baffles
Photo Courtesy RIO
Clock and Biases
Outputs 1-32
Outputs 33-64
Orion Focal Plane Module
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO 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
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
Project status October 2003
• 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
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
NEWFIRMNOAO Extremely Wide Field Infrared Imager
NOAO Users Committee meeting 23 Oct 2003
Back to the future
What does NEWFIRM bring to future efforts?
• 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 SOAR Adaptive Optics
A. Tokovinin
Telescope system in Chile
Telescope system in Chile
Resolution ~0.3”Field 3’-5’Full sky coverageImaging+spectroscopy
We need:
Can it be done?Can we afford it?
Can it be done?Can we afford it?
Resolution is important!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)
Solution:Ground-layercompensatio
n
Solution:Ground-layercompensatio
n
Deformabe mirror
Rayleigh UV LaserGuide Star at 10km
Partial compensation of high layers
Good compensation of low layers
1’ 2’ 3’ seeing
Seeing at Cerro Pachon
Seeing at Cerro Pachon
A good night: January 15, 2003
• 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”
Prediction for SOAR AOPrediction 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 nightsJanuary 2003
Sample science with SOAR AOSample 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 resolutionImaging+spectroscopy at high angular resolution
History of LMC clusters (K.Olsen)History of LMC clusters (K.Olsen)
Ground-based, 1”
SOAR AO, 0.3”
HST, 0.1”
Reaches turn-off
Photometric errorfrom crowding
Photometric errorfrom crowding
Science instruments for SOAR AOScience instruments for SOAR AO
• CCD imager: 2Kx2K, 0.08” pixels
• SOAR-Brazil IFU
(+ Fabry-Perot?)• Port for a “visitor”
AO instrument
• Adaptive secondary ($2M)
• WFS at each instrument (not planned)
• Pixel scale?
dedicated?1st light SOAR instruments or
…not a good solution!
SOAR AO on SOAR
SOAR AO on SOAR
Electronics
ISBAO module
CCDImager
AO module on ISB
AO module on ISB
LaserLaser Solid-state Nd:YAG laser DS20-355 (Photonics)
=355 nm, 8 W @ 10 kHz Cost $138K or cheaper Resource ~10000h (~5yr)
Tip-tilt: 2-3 NGS to V=18, complete sky coverageTip-tilt: 2-3 NGS to V=18, complete sky coverage
Safety: aircraft and satellite-safe, no visual hazardsSafety: aircraft and satellite-safe, no visual hazards
Control System Block Diagram
Planning and cost
Planning and cost
CoDR: April 2003 PDR: March 2004 Lab closed-loop: 2004 On the sky: 2005
Manpower Capital Total
MY K$ K$ K$
16.5 589 540 1.13
SOAR partners (MSU+UNC) apply for AODP fundingto build “set-and-forget” Rayleigh laser guide star for SOAR
SOAR partners (MSU+UNC) apply for AODP fundingto build “set-and-forget” Rayleigh laser guide star for SOAR
Affordable
A road into the future…
A road into the future…
Build reliable and productive AO system to enhance SOAR scienceand Demonstrate AO technology scalable to ELTs Build AO expertise for TMT and other projects Synergy with Gemini-S (MCAO, NICI)