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NEWFIRM: the N OAO E xtremely W ide F ield IR I m ager

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)

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NEWFIRM: the N OAO E xtremely W ide F ield IR I m ager

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  1. NEWFIRM: the NOAO Extremely Wide Field IR Imager Presented by Ron Probst, Project Scientist

  2. NEWFIRM is … Aninfrared camerawith • 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 asystemfor • Deep wide field surveys ( efficient operation on telescope ) • Rapid data turnaround ( pipeline reduction ) • Public data access ( NVO archive )

  3. 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

  4. 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

  5. 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

  6. NEWFIRM in a global context

  7. 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 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

  8. 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

  9. 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

  10. System elements: from photons to science photons 4-m telescope KPNO CTIO guider NEWFIRM instrument S W MIP/NF Tucson La Serena ORION: NOAO USNO NASA Ames Raytheon IR array mosaic

  11. Array controller S W MIP/MONSOON Tucson La Serena Data handling system Data Products: 3 teams + U. Maryland Surveys PI science Special purpose Science data pipeline Science users Science archive science

  12. OptomechanicalLayout

  13. Orion Focal Plane Module Clock and Biases Output Current Mirrors Light Baffles Outputs 1-32 Outputs 33-64 AlN Motherboard Invar36 Pedestal Alignment Locator Detector SCA Photo Courtesy RIO

  14. 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

  15. 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

  16. 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

  17. The SOAR Adaptive Optics System Presented by Andrei Tokovinin, Project Scientist

  18. SOAR Adaptive Optics A. Tokovinin

  19. 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?

  20. Resolution is important! • Resolution: 2-3 times • mlim [sky]: gain 0.5-1 mag (rival 8-m) • mlim [confusion]: gain 1-2 mag (half-way to HST) 0.3” 0.7”

  21. Rayleigh UV Laser Guide Star at 10km Solution:Ground-layercompensation Partial compensation of high layers Good compensation of low layers Deformabe mirror 1’ 2’ 3’ seeing

  22. 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

  23. Prediction for SOAR AO [arcseconds] 21 nights January 2003

  24. 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

  25. History of LMC clusters (K.Olsen) Ground-based, 1” SOAR AO, 0.3” Reaches turn-off HST, 0.1” Photometric error from crowding

  26. Science instruments for SOAR AO 1st light SOAR instruments or dedicated? • 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? …not a good solution!

  27. SOAR AO on SOAR

  28. AO module on ISB AO module ISB CCD Imager Electronics

  29. Laser • Solid-state Nd:YAG laser DS20-355 (Photonics) • =355 nm, 8 W @ 10 kHz • Cost $138K or cheaper • Resource ~10000h (~5yr) Safety: aircraft and satellite-safe, no visual hazards Tip-tilt: 2-3 NGS to V=18, complete sky coverage

  30. Control System Block Diagram

  31. CoDR: April 2003 • PDR: March 2004 • Lab closed-loop: 2004 • On the sky: 2005 Planning and cost Affordable SOAR partners (MSU+UNC) apply for AODP funding to build “set-and-forget” Rayleigh laser guide star for SOAR

  32. 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)

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