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Information about sings2mw

Published on August 29, 2007

Author: Mahugani


SINGS: THE SIRTF NEARBY GALAXIES SURVEY:  SINGS: THE SIRTF NEARBY GALAXIES SURVEY Robert Kennicutt (U. Arizona) SINGS PROJECT OVERVIEW:  SINGS PROJECT OVERVIEW Science Core Characterize star formation in 75 nearby galaxies Trace processing of energy from young stars through the dusty ISM Legacy Core Observations designed to maximize long-term scientific return, archival value of survey Primary data products SED, spectral libraries of galaxies and IR-emitting components OUTLINE:  OUTLINE SIRTF Legacy Overview SIRTF scientific capabilities Legacy science program SINGS scientific context scientific objectives observing program and strategy data products and archive Space Infrared Telescope Facility:  Infrared Great Observatory Background Limited Performance 3 -- 180 m 85 cm f/12 Beryllium Telescope, T andlt; 5.5K 6.5 m Diffraction Limit New Generation Detector Arrays Instrumental Capabilities Imaging/Photometry, 3-180 m Spectroscopy, 5-40 m Spectrophotometry, 50-100 m Planetary Tracking, 1 arcsec/sec andgt;75% of observing time for the General Scientific Community 2.5 yr Lifetime/5 yr Goal Launch in July 2002 (Delta 7920H) Solar Orbit Cornerstone of NASA’s Origins Program Space Infrared Telescope Facility Slide5:  SIRTF Telescope Installation Solar Orbit:A Better Choice:  Solar Orbit: A Better Choice 0.6 AU 0.5 AU 0.4 AU 0.3 AU 0.2 AU Earth Observatory position on February 3, 2007 'Loops' and 'kinks' in trajectory occur on 1-year centers. 50% More Mass Than HEO Better Thermal Environment No Earth-Moon Avoidance No Need for Propulsion No Earth Radiation Belt Simple Deep Space Tracking Less Complex Fault Protection Simple Observation Planning DSN andamp; HGA Comm Sun SIRTF Family Portrait:  SIRTF Family Portrait MIPS IRAC IRS SIRTF Measurements - Imaging:  SIRTF Measurements - Imaging SIRTF Measurements - Spectroscopy:  SIRTF Measurements - Spectroscopy SIRTF Performance Expectations:  SIRTF Performance Expectations SIRTF Legacy Science:  SIRTF Legacy Science Requirements Large, coherent scientific investigations - not realizable as series of smaller GO Programs Programs whose data are of general and lasting importance to the broad community and also stimulate SIRTF follow-on Data are non-proprietary, enabling timely and effective opportunities for SIRTF follow-on and archival research Scope Six teams selected in November, 2000, with a total of 3160 hours of observing time (~50% of the first year of SIRTF) Limited amount of time on NOAO facilities was allocated in the same process All teams planning to deliver value-added products (data bases, catalogs, atlases, non-SIRTF data) for distribution to community via SSC The Legacy Science Program:  The Legacy Science Program Mark Dickinson (STScI) andamp; 38 Co-Investigators @ 13 institutions 'GOODS: Great Observatories Origins Deep Survey' 647 hours (IRAC, MIPS) Carol Lonsdale (IPAC/Caltech) andamp; 19 Co-Is @ 9 institutions 'SWIRE: SIRTF Wide-area Infrared Extragalactic Survey' 851 hours (IRAC, MIPS) Robert Kennicutt (U. Arizona) andamp; 14 Co-Is @ 7 institutions 'SINGS: SIRTF Nearby Galaxies Survey' 512 hours (IRAC, MIPS, IRS) Ed Churchwell (U. Wisconsin) andamp; 13 Co-Is @ 6 institutions 'The SIRTF Galactic Plane Survey (GLIMPSE)' 400 hours (IRAC) Neal Evans (U. Texas) andamp; 10 Co-Is @ 8 institutions 'From Molecular Cores to Planets (Cores to Disks)' 400 hours (IRAC, MIPS, IRS) Michael Meyer (U. Arizona) andamp; 18 Co-Is @ 12 institutions 'The Formation and Evolution of Planetary Systems (FEPS)' 350 hours (IRAC, MIPS, IRS) Slide13:  Planned SIRTF Surveys:   [ ] limiting flux model dependent due to predicted confusion *- MIPS Real Deep Survey will cover only 0.02 square degree **- Locations of Surveys as follows: WIDE = NOAO Deep Field; DEEP = HDF-N, Groth Strip, CXO-S, SSA 13, Lockman Hole, XMM Deep; GOODS = HDF-N, CXO-S;REAL DEEP = Groth Strip; FIRST LOOK = North Ecliptic Pole *** - GOODS Survey may go somewhat deeper in IRAC bands over ~ 0.02 sq degrees Area Deg^2 5-s limiting flux, mJy (5-s limiting magnitude) Planned SIRTF Surveys Slide15:  Slide16:  Anchor Points in the Local Universe (SINGS):  Anchor Points in the Local Universe (SINGS) Simulated galaxy spectrum (z=1) The Local Universe The Distant Universe SINGS Team:  SINGS Team Arizona Rob Kennicutt (PI), George Bendo, Chad Engelbracht, Karl Gordon, Aigen Li, George Rieke, Marcia Rieke, JD Smith Caltech/IPAC/SSC Lee Armus, George Helou, Tom Jarrett, Helene Roussel STScI Daniela Calzetti, Claus Leitherer, Michael Regan, Sangeeta Malhotra Bucknell Michele Thornley Harvard/CfA Lisa Kewley NASA Ames David Hollenbach NRAO Fabian Walter Princeton Bruce Draine Wyoming Danny Dale Slide19:  Ferguson et al 1998, ApJ, 506, L19 ISOCAM 15mm NGC 6946 Ha vs IR Slide20:  Slide21:  Slide22:  Barger et al. 2000, AJ, 119, 2092 IR-submm selected UV-visible selected Slide23:  bolometric pixel-resolved maps of 75 galaxies spatially-resolved SED maps: 0.15 - 200 mm high-resolution spectra of 150 IR-emitting regions matched Ha, HI, CO, dust, radio continuum maps Physics of Galaxy Evolution:  Physics of Galaxy Evolution Robust treatment of dust extinction andamp; heating Test, reconcile UV, Ha, FIR-based SFR scales Quantify physical relationships between SFR and ISM properties (SF law) over full range of environments Physical characteristics, demographics of obscured vs UV-bright SF components along Hubble sequence ISM energy balance, FIR/radio correlation Slide25:  SINGS will bridge gap between UV-Ha based diagnostics of disk star formation and IR-based studies of dense starburst regions. normal disks IR-selected starbursts 105 range! Kennicutt 1998, ApJ, 498, 541 Slide26:  Ha Surveys KISS, UCM SINGG/HIPASS HaGS STARFORM MOSAIC Clusters 11 Mpc SIRTF Surveys GOODS SWIRE MIPS GTO Submm Surveys SCUBA ALMA Spectroscopic Surveys Keck, Magellan VLT, MMT Subaru UV Surveys GALEX SDSS SINGS + GTO Surveys Slide27:  Physics of the Star-Forming ISM:  Physics of the Star-Forming ISM dust physics (PAH features, IR SEDs) observe full range of Z/Zo and ISRF full spatial coverage from IRAC, MIPS maps in-depth coverage with IRS low-res maps ionized gas (fine-structure lines) hardness indices (Ne+ -andgt; Ne++++) ionization rates ([NeII]) IMF, AGN vs starburst diagnostics cold gas (H2, [SiII], [FeII]) physics of PDR, SF region interfaces continuity of physical properties vs density, AV, dynamical environment visible --andgt; infrared diagnostics of SF regions SIRTF Capabilities:  SIRTF Capabilities Fiducial distance = 3.5 Mpc (e.g., M81 group) resolution angular resolution = l/4 (mm) linear resolution = 40-700 pc (3.5 - 160 mm) sensitivities (all 10s) MIPS: 105 Mo cloud in 10 sec IRAC: 104 Mo cloud in 10 sec IRS: [NeII]12.8mm from Orion in 30 sec IRS: H2 S(0) -andgt; S(1) from 5x105 Mo cloud (100K) in 500 sec SINGS Mapping Schemes:  SINGS Mapping Schemes IRAC and MIPS fields SED Scans Targeted Spectroscopy Sample Design and Selection:  Sample Design and Selection Physically-Based Galaxy Sample full parameter space of type (SFR, gas fraction), mass (luminosity, Z/Zo), LIR/LB representative range of other properties (inclination, bar, spiral structure, nuclear type, environment) preference to well-studied objects within parameter space cells Physically-Based Spectroscopic Sample parameter space: abundance, luminosity, AV, radiation field strength, shape mix of optically, IR-selected targets Slide32:  SINGS Sample: Parameter Space Slide33:  SINGS Mapping Schemes:  SINGS Mapping Schemes IRAC and MIPS fields SED Scans Targeted Spectroscopy Slide35:  Slide36:  SINGS Mapping Schemes:  SINGS Mapping Schemes IRAC and MIPS fields SED Scans Targeted Spectroscopy Slide38:  Observations: Summary:  Observations: Summary Imaging IRAC + MIPS (3.5 - 160 mm) full wavelength + spatial coverage (R andlt; R25) Low-Resolution Spectral Scans radial strip scans (S15 andgt; 1 MJy/sr; R andlt; 0.55 R25) IRS scans (14-40 mm) + MIPS SED scans (52-99 mm) Targeted Spectroscopy 75 nuclei + 75 extra-nuclear regions physically-based sample (Z/Zo, Lbol, Gn, T*, AV , F8/15) IRS low-resolution scans (5-14 mm, R = 60-120) IRS high-resolution mini-maps (10-37 mm, R = 600) Ancillary Data:  Ancillary Data visible/IR imaging (BVRIJHK, Ha) visible spectra (3600-7000 A) spectral scans nuclear spectra, extranuclear targets HST Pa-a, H-band maps (central arcmin2) CO, HI maps (BIMA SONG, VLA, WSRT) radio continuum maps (VLA, WSRT) UV imaging (GALEX) (1500 A, 2500 A) Archival Science (examples):  Archival Science (examples) stellar mass distributions, spiral structure optical depth of disks dust and gas in E/S0 galaxies cold dust in halos, extended disks the AGN/starburst connection interstellar shocks applications and synergies modeling of high-z galaxies modeling of ULIRGs Galactic star formation: the big picture The SINGS Legacy: Products:  The SINGS Legacy: Products Full-coverage IRAC + MIPS imaging Pixel-resolved SED library of galaxies (3.6 - 160 mm ---andgt; 0.1 - 160 mm) Spectral library of galaxy centers and extra-nuclear IR-emitting regions (5 - 37 mm) Multi-wavelength data (BVRIJHK, Ha, UV, CO) Data analysis tools matched-beam SED, spectrum extraction spectral data cube generators Web-based access, browse, downloading Slide43:  Legacy Design:  Legacy Design Unbiased, physically-based samples Homogeneous data sets, uniform wavelength coverage, sensitivity limits, spatial sampling Comprehensive data, maximize archival value, discovery potential Integrated multi-wavelength observations Complement GTO observations SIRTF Instrumentation Summary:  SIRTF Instrumentation Summary Sensitivity numbers are indicative of SIRTF performance. Detailed times estimates should be based on tools available on SSC website: Slide46:  normal galaxies starburst galaxies gas density star formation rate Slide47:  NGC 2841 NGC 3184 NGC 4449 Sb Sc Irr Slide48:  Extended Star Formation in Disks - global trends Kennicutt 1998, ARAA, 36, 189 Bendo et al. 2002, in prep Slide49:  Circumnuclear Star Formation - trends with type Ho et al. 1997, ApJ, 487, 595 Slide50:  Slide51:  Bell et al. 2002, ApJ, 565, 994 Testbed: LMC Slide52:  Bell 2002, ApJL, in prep Ha Imaging Surveys:  Ha Imaging Surveys Survey Ngal Selection PI GOLD Mine 277 magnitude Coma/Virgo G. Gavazzi MOSAIC ~1100 Ha Abell clusters R. Kennicutt S. Sakai HaGS 450 mag/volume field (andlt;40 Mpc) P. James SINGG 500 HI field (andlt;40 Mpc) G. Meurer STARFORM 150 volume field (andlt;25 Mpc) S. Hameed 11 Mpc 432 volume field (andlt;11 Mpc) R. Kennicutt KIG ~270 magnitude field L. Montenegro Palomar/LCO 83 obj prism BCDs (andlt;50 Mpc) A. Gil de Paz SINGS 75 multi-param andlt;30 Mpc R. Kennicutt Ha Surveys: Objectives:  Ha Surveys: Objectives Complete inventories of local SF galaxies robust determination of rSF at z = 0 (SINGG) completeness of objective prism surveys (e.g., UCM) completeness of optically, HI-selected surveys serendipidous detection of star-forming galaxies Environmental effects on disk SF Dwarf galaxy evolution role of bursts, quiescent evolution, duty cycle Metrics of disk star formation, evolution Aperture, inclination effects on total SFRs Integration with GALEX, SIRTF UV vs Ha SFRs optically visible vs enshrouded SF Physics of Galaxy Evolution:  Physics of Galaxy Evolution Bolometric pixel-resolved maps of 75 galaxies Spatially-resolved SED maps: 0.15 - 200 mm Matched Ha, HI, CO, dust, radio continuum maps Robust treatment of dust extinction andamp; heating Test, reconcile UV, Ha, FIR-based SFR scales Quantify physical relationships between SFR and ISM properties (SF law) over full range of environments Physical characteristics, demographics of obscured vs UV-bright SF components along Hubble sequence ISM energy balance, FIR/radio correlation

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