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SINGS: THE SIRTF NEARBY GALAXIES SURVEY

SINGS: THE SIRTF NEARBY GALAXIES SURVEY. Robert Kennicutt (U. Arizona). http://ircamera.as.arizona.edu/legacy. 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

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SINGS: THE SIRTF NEARBY GALAXIES SURVEY

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  1. SINGS: THE SIRTF NEARBY GALAXIES SURVEY Robert Kennicutt (U. Arizona) http://ircamera.as.arizona.edu/legacy

  2. 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

  3. OUTLINE • SIRTF Legacy Overview • SIRTF scientific capabilities • Legacy science program • SINGS • scientific context • scientific objectives • observing program and strategy • data products and archive

  4. Space Infrared Telescope Facility • Infrared Great Observatory • Background Limited Performance 3 -- 180 m • 85 cm f/12 Beryllium Telescope, T < 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 • >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

  5. SIRTF Telescope Installation

  6. Solar Orbit:A Better Choice Earth Sun 0.4 AU 0.3 AU 0.2 AU 0.6 AU 0.5 AU 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 & HGA Comm “Loops” and “kinks” in trajectory occur on 1-year centers. Observatory position on February 3, 2007

  7. SIRTF Family Portrait IRS MIPS IRAC

  8. SIRTF Measurements - Imaging

  9. SIRTF Measurements - Spectroscopy

  10. SIRTF Performance Expectations

  11. 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

  12. The Legacy Science Program • Mark Dickinson (STScI) & 38 Co-Investigators @ 13 institutions “GOODS: Great Observatories Origins Deep Survey” 647 hours (IRAC, MIPS) • Carol Lonsdale (IPAC/Caltech) & 19 Co-Is @ 9 institutions “SWIRE: SIRTF Wide-area Infrared Extragalactic Survey” 851 hours (IRAC, MIPS) • Robert Kennicutt (U. Arizona) & 14 Co-Is @ 7 institutions “SINGS: SIRTF Nearby Galaxies Survey” 512 hours (IRAC, MIPS, IRS) • Ed Churchwell (U. Wisconsin) & 13 Co-Is @ 6 institutions “The SIRTF Galactic Plane Survey(GLIMPSE)” 400 hours (IRAC) • Neal Evans (U. Texas) & 10 Co-Is @ 8 institutions “From Molecular Cores to Planets (Cores to Disks)” 400 hours (IRAC, MIPS, IRS) • Michael Meyer (U. Arizona) & 18 Co-Is @ 12 institutions “The Formation and Evolution of Planetary Systems (FEPS)” 350 hours (IRAC, MIPS, IRS)

  13. Type** 3.6mm 4.5mm 5.8mm 8mm 24mm 70mm 160mm SWIRE (Legacy) 70 7.3 18.9 9.7 18 27.5 16.5 32.5 15.9 450 2750 [17500] WIDE(GTO) 9 8.4 18.7 11 17.8 33 16.3 38 15.5 600 3600 [33000] DEEP(GTO) 2 [2.5] 20.1 3.6 19.0 11.4 17.4 15.3 16.5 150 1000 [30000] REAL DEEP (GTO) 0.2 [2.5] 20.1 [2.5] 19.4 2.5 19.1 3.4 18.1 [60]* [700]* FIRST LOOK (SSC) 5 23 17.6 24 17.0 70 15.5 58 15.0 1100 3800 [33000] GOODS*** (Legacy) ~0.1 [0.55] 21.7 [0.55] 21 [1.1] 20 [1.2] 19.2 [22] Planned SIRTF Surveys Area Deg^2 5-s limiting flux, mJy (5-s limiting magnitude)  [ ] 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

  14. Anchor Points in the Local Universe (SINGS) The Distant Universe The Local Universe Simulated galaxy spectrum (z=1)

  15. 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 SINGS Team

  16. NGC 6946 Havs IR Ferguson et al 1998, ApJ, 506, L19 ISOCAM 15mm

  17. IR-submm selected UV-visible selected Barger et al. 2000, AJ, 119, 2092

  18. 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

  19. Physics of Galaxy Evolution • Robust treatment of dust extinction & 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

  20. IR-selected starbursts SINGS will bridge gap between UV-Ha based diagnostics of disk star formation and IR-based studies of dense starburst regions. normal disks 105 range! Kennicutt 1998, ApJ, 498, 541

  21. Spectroscopic Surveys Keck, Magellan VLT, MMT Subaru Ha Surveys KISS, UCM SINGG/HIPASS HaGS STARFORM MOSAIC Clusters 11 Mpc SIRTF Surveys GOODS SWIRE MIPS GTO SINGS + GTO Surveys UV Surveys GALEX Submm Surveys SCUBA ALMA SDSS

  22. 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+ -> 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 --> infrared diagnostics of SF regions

  23. 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) -> S(1) from 5x105 Mo cloud (100K) in 500 sec

  24. SINGS Mapping Schemes Targeted Spectroscopy IRAC and MIPS fields SED Scans

  25. 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

  26. SINGS Sample: Parameter Space

  27. SINGS Mapping Schemes Targeted Spectroscopy IRAC and MIPS fields SED Scans

  28. SINGS Mapping Schemes Targeted Spectroscopy IRAC and MIPS fields SED Scans

  29. Observations: Summary • Imaging • IRAC + MIPS (3.5 - 160 mm) • full wavelength + spatial coverage (R < R25) • Low-Resolution Spectral Scans • radial strip scans (S15 > 1 MJy/sr; R < 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)

  30. 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)

  31. 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

  32. The SINGS Legacy: Products • Full-coverage IRAC + MIPS imaging • Pixel-resolved SED library of galaxies (3.6 - 160 mm ---> 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

  33. 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

  34. SIRTF Instrumentation Summary Sensitivity numbers are indicative of SIRTF performance. Detailed times estimates should be based on tools available on SSC website: http://sirtf.caltech.edu.

  35. starburst galaxies star formation rate normal galaxies gas density

  36. NGC 2841 NGC 3184 NGC 4449 Sb Sc Irr

  37. Extended Star Formation in Disks - global trends Kennicutt 1998, ARAA, 36, 189 Bendo et al. 2002, in prep

  38. Circumnuclear Star Formation - trends with type Ho et al. 1997, ApJ, 487, 595

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