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– 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
• SIRTF Legacy Overview – SIRTF scientific capabilities
– Legacy science program
• SINGS– scientific context
– scientific objectives
– observing program and strategy
– data products and archive
• 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
Space Infrared Telescope Facility
SIRTF Telescope Installation
Solar Orbit:A Better Choice
0.6 AU 0.5 AU 0.4 AU 0.3 AU 0.2 AUEarth
Observatory positionon February 3, 2007
“Loops” and “kinks”in trajectory occuron 1-year centers.
50% More Mass Than HEOBetter Thermal EnvironmentNo Earth-Moon Avoidance
No Need for PropulsionNo Earth Radiation Belt
Simple Deep Space TrackingLess Complex Fault ProtectionSimple Observation Planning
DSN & HGA Comm
Sun
SIRTF Family Portrait
MIPSIRAC
IRS
8
SIRTF Measurements - Imaging
3.6 , m
MIPS
IRAC
Numberof
Pixels
Fieldof
View
4.5 5.8 8.0
256x256 256x256 256x256 256x256
5’x5’ 5’x5’ 5’x5’ 5’x5’ 1’x1.2’
IRS
15
33x45
24
5’x5’
128x128
70
5’x5’
32x32
160
0.5’x5’
2x20
9
SIRTF Measurements - Spectroscopy
0
10
100
1000
4 10 40 160100
Wavelength, microns
Re
so
lvin
g P
ow
er
IRS Hi
IRS Lo
MIPS SED
MIPSIRSIRAC
10
SIRTF Performance Expectations
100
10
1
10-1
10-2
10-3
10-4
4.5 10 25 45 70 160
(m)
LIM
ITIN
G F
LUX
F (
mJy
)
ALL FLUX LIMITS 1 – 1 HR (HIGH LATITUDE CONFUSION INCLUDED)
*
SIRTF IMAGING
SIRTF SPECTROSCOPY (R = 50)
SIRTF SED MODE
109 yr, 5MJ
DISK AROUND BETA PICTORIS x 10 -3
ULTRALUMINOUS GALAXY, Z = 7
L GALAXY, Z = 5
- MWW (2/20/98)
BROWN DWARF AT 10 pc
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
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)
[ ] 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
Type**
m m m m m m m
SWIRE(Legacy)
70 7.3 18.9
9.7 18
27.5 16.5
32.515.9
450 2750 [17500]
WIDE(GTO)
9 8.418.7
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]
AreaDeg^2
5- limiting flux, Jy(5- limiting magnitude)
Planned SIRTF Surveys
Anchor Points in the Local Universe (SINGS)
Simulated galaxy spectrum (z=1)
The Local Universe
The Distant Universe
SINGS TeamArizona
Rob Kennicutt (PI), George Bendo, Chad Engelbracht, Karl Gordon, Aigen Li, George Rieke, Marcia Rieke, JD Smith
Caltech/IPAC/SSCLee Armus, George Helou, Tom Jarrett, Helene Roussel
STScIDaniela Calzetti, Claus Leitherer, Michael Regan, Sangeeta Malhotra
BucknellMichele Thornley
Harvard/CfALisa Kewley
NASA Ames David Hollenbach
NRAOFabian Walter
Princeton Bruce Draine
WyomingDanny Dale
Ferguson et al 1998, ApJ, 506, L19 ISOCAM 15m
NGC 6946 H vs IR
Barger et al. 2000, AJ, 119, 2092
IR-submm selected
UV-visible selected
•bolometric pixel-resolved maps of 75 galaxies•spatially-resolved SED maps: 0.15 - 200 m•high-resolution spectra of 150 IR-emitting regions•matched H, HI, CO, dust, radio continuum maps
Physics of Galaxy Evolution
• Robust treatment of dust extinction & heating
• Test, reconcile UV, H, 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
SINGS will bridge gapbetween 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
Ha SurveysKISS, UCM
SINGG/HIPASSHaGS
STARFORMMOSAIC Clusters
11 Mpc
SIRTF Surveys
GOODSSWIRE
MIPS GTO
Submm Surveys
SCUBAALMA
Spectroscopic Surveys
Keck, MagellanVLT, MMT
Subaru
UV Surveys
GALEX
SDSS
SINGS+
GTO Surveys
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
SIRTF CapabilitiesFiducial distance = 3.5 Mpc (e.g., M81 group)
• resolution– angular resolution = /4 (m)
– linear resolution = 40-700 pc (3.5 - 160 m)• sensitivities (all 10)
– MIPS: 105 Mo cloud in 10 sec – IRAC: 104 Mo cloud in 10 sec – IRS: [NeII]12.8m from Orion in 30 sec– IRS: H2 S(0) -> S(1) from 5x105 Mo cloud (100K)
in 500 sec
SINGS Mapping Schemes
IRAC and MIPS fields SED Scans Targeted Spectroscopy
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
SINGS Sample: Parameter Space
SINGS Mapping Schemes
IRAC and MIPS fields SED Scans Targeted Spectroscopy
SINGS Mapping Schemes
IRAC and MIPS fields SED Scans Targeted Spectroscopy
Observations: Summary
• Imaging– IRAC + MIPS (3.5 - 160m)– full wavelength + spatial coverage (R < R25)
• Low-Resolution Spectral Scans– radial strip scans (15 > 1 MJy/sr; R < 0.55 R25)– IRS scans (14-40 m) + MIPS SED scans (52-99 m)
• Targeted Spectroscopy– 75 nuclei + 75 extra-nuclear regions– physically-based sample (Z/Zo, Lbol, G, T*, AV , F8/15) – IRS low-resolution scans (5-14 m, R = 60-120) – IRS high-resolution mini-maps (10-37 m, R = 600)
Ancillary Data
• visible/IR imaging (BVRIJHK, H)
• visible spectra (3600-7000 A)
– spectral scans
– nuclear spectra, extranuclear targets
• HST Pa-, 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)
• 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
• Full-coverage IRAC + MIPS imaging• Pixel-resolved SED library of galaxies
(3.6 - 160 m ---> 0.1 - 160 m)
• Spectral library of galaxy centers and extra-nuclear IR-emitting regions (5 - 37 m)
• Multi-wavelength data (BVRIJHK, Ha, UV, CO)
• Data analysis tools– matched-beam SED, spectrum extraction– spectral data cube generators
• Web-based access, browse, downloading
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
Pixel Size Sensitivity (Jy) (m) Array Type F.O.V. (arcsec) (5 in 500 sec, incl. confusion)
IRAC: InfraRed Array Camera
3.6 InSb 4.9 5.1' x 5.1' 1.2 3
4.5 InSb 4.3 5.1' x 5.1' 1.2 4
5.8 Si:As (IBC) 4.0 5.1' x 5.1' 1.2 10
8.0 Si:As (IBC) 2.7 5.1' x 5.1' 1.2 15
MIPS: Multiband Imaging Photometer for SIRTF
24 Si:As (IBC) 4 5.1' x 5.1' 2.4 370
70 Ge:Ga 3.5 2.7' x 2.7' / 5.1' x 5.1' 4.9 / 9.4 1400
52 - 99 Ge:Ga 14 - 24 18.75" x 4' 9.4 6500
160 Ge:Ga (stressed) 4 0.5' x 5.1' 15 22.5 mJy
IRS: Infrared Spectrograph
5.3 - 14.5 Si:As (IBC) 60 - 120 3.6" x 55" 1.8 550 Jy
15 (peakup imaging) Si:As (IBC) 3 1' x 1.2' 1.8 100 Jy
10 - 19.5 Si:As (IBC) 600 4.8" x 11.8" 2.4 3x10-18 W/m2
14 - 40 Si:Sb (IBC) 60 - 120 9.7" x 151" 4.8 1.5 mJy
19 - 37 Si:Sb (IBC) 600 9.7" x 22.4" 4.8 3x10-18 W/m2
Sensitivity numbers are indicative of SIRTF performance. Detailed times estimates should be based on tools available on SSC website: http://sirtf.caltech.edu.
normal galaxies
starburst galaxies
gas density
sta
r fo
rmati
on
rate
NGC 2841 NGC 3184 NGC 4449 Sb Sc Irr
Extended Star Formation in Disks - global trends
Kennicutt 1998, ARAA, 36, 189 Bendo et al. 2002, in prep
Circumnuclear Star Formation
- trends with type
Ho et al. 1997, ApJ, 487, 595
Bell et al. 2002, ApJ, 565, 994
Testbed:
LMC
Bell 2002, ApJL, in prep
H Imaging Surveys
Survey Ngal Selection PI
GOLD Mine 277 magnitude Coma/Virgo G. Gavazzi
MOSAIC ~1100 H Abell clusters R. Kennicutt S. Sakai
HGS 450 mag/volume field (<40 Mpc) P. James
SINGG 500 HI field (<40 Mpc) G. Meurer
STARFORM 150 volume field (<25 Mpc) S. Hameed
11 Mpc 432 volume field (<11 Mpc) R. Kennicutt
KIG ~270 magnitude field L. Montenegro
Palomar/LCO 83 obj prism BCDs (<50 Mpc) A. Gil de Paz
SINGS 75 multi-param <30 Mpc R. Kennicutt
H Surveys: Objectives• Complete inventories of local SF galaxies
– robust determination of SF 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
Bolometric pixel-resolved maps of 75 galaxiesSpatially-resolved SED maps: 0.15 - 200 m
Matched H, HI, CO, dust, radio continuum maps
• Robust treatment of dust extinction & heating• Test, reconcile UV, H, 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