SINGS: Panchromatic Data and Star Formation in Nearby Galaxies Daniela Calzetti (UMass, Amherst) Gas Accretion and Star Formation in Galaxies, Garching bei Munchen, Germany, Sept 10-14, 2007

SINGS (Spitzer Infrared Nearby Galaxies Survey) Cambridge University of Massachusetts Rob Kennicutt (PI) Daniela Calzetti (Deputy PI) STScI Claus Leitherer, Michael Regan, (Martin Meyer) Caltech/IPAC/SSC Lee Armus, Brent Buckalew, George Helou, Tom Jarrett, Kartik Sheth, Eric Murphy (Yale) Arizona Chad Engelbracht, (Karl Gordon), Moire Prescott, George Rieke, Marcia Rieke, JD Smith Arizona State Sangeeta Malhotra Bucknell Michele Thornley Hawaii Lisa Kewley MPIA Fabian Walter, Helene Roussel NASA Ames David Hollenbach Princeton Bruce Draine Wyoming Danny Dale Imperial College George Bendo

Introduction: Theory vs. Obs.  Star formation links the invisible (driven by gravity and the subject of theoretical modeling) and the visible (directly measurable) `Universe’  SF shapes its surroundings by:  depleting galaxies of gas  controlling the metal enrichment of the ISM and IGM  regulating the radiative and mechanical feedback into the ISM and IGM  shaping the stellar population mix in galaxies.  Need to:  Characterize the laws of SF  Derive unbiased SFR measurements. ACS-GOODS Giavalisco et al.

SFR Measurements Dale et al (  m) HH PP 8  m 24  m70  m160  m UV [OII] `calorimetric’ IR Derived virtually at all wavelengths, from the X-ray to the radio. Measure massive stars emission - requires IMF assumptions. Direct stellar light Dust-processed light

The `ground truth’ - 1  FIR, UV+FIR? (GALEX, Spitzer)  FIR is calorimetric measure (not a problem at low-z; IRAS, ISO, Spitzer, Herschel,…);  for extended sources (whole galaxies), contribution of evolved (non- star-forming) populations to both UV and FIR.  Optical lines (mainly H recombination lines)?  Dust extinction (blue lines)  Upper end IMF  Underlying stellar abs. (Balmer)  `Difficult to observe’ (IR lines) M51: UV, H , 24  m

The `ground truth’ - 2 Use P  (1.876  m) as `ground truth’, i.e., an `unbiased’ measure of instantaneous SFR (Boeker et al. 1999; Quillen & Yukita 2001) for investigating SINGS galaxies: Relatively insensitive to dust (A V =5 mag implies  P  < 2x) Sensitive to timescale ~ 10 Myr But … limited to central regions of galaxies Scale ~ pc M51 NGC normal galaxies (220 regions) 34 starbursts

UV, Dust, and Age Starbursts (Meurer et al. 1999, Goldader et al. 2002, C. et al. 1994,1995,1996,1997,2000)  26 A dusty stellar population may have similar UV characteristics of an old population  SFR > 0.3 – 1 M o /yr/kpc 2 SFR(UV corr,  ), SFR(UV+FIR) OK for starbursts at all redshifts (e.g., LBGs at z~3)

SFR-Extinction Starbursts A V = 3.1 E(B-V) = 14.4 Z  SFR 0.64 (Wang & Heckman, 1996; Heckman et al. 1998; Calzetti 2001 Hopkins et al. 2001, Sullivan et al. 2001, C. et al. 2007) SF regions in normal galaxies

UV, Dust, and SF Activity  26 (Buat et al. 2002, 2005, Bell 2002, Gordon et al. 2004, Xu et al. 2004, Seibert et al. 2005, C. et al. 2005) Blue= starbursts Red= normal SF  SFR << 0.3 – 1 M o /yr/kpc 2 Major boost from GALEX Deviations due to time-averaged SFH? (Xu et al. 2004) Johnson et al. (2007) find little correlation with D n (4000) < 1.7 Due to recent SFH? (< Myr, C. et al. 2005) displacement between UV and line or IR emission in M51.

FIR to SFR? Dale et al (  m)  m 24  m70  m160  m `calorimetric’ IR FIR - sensitive to heating from old, as well as young, stellar populations 8  m - mostly single photon heating (PAH emission) 24  m - both thermal and single photon heating 70  m and 160  m - mostly thermal, also from old stars

SFR[MidIR( )]  Spitzer has opened a `more sensitive’ window to the distant Universe:  A number of studieshas looked at the viability of monochromatic IR emission (mainly 8 and 24  m) as SFR indicator (Wu et al, 2005, Chary et al., Alonso-Herrero et al. 2006, etc.)  Appeal of PAH emission (restframe 7.7  m emission for z~2) for investigating star formation in high-z galaxy populations (e.g., First Look, GOODS, MIPS GTO, etc.; Daddi et al. 2005)  Monochromatic 24  m (restframe) emission also potentially useful for measuring high-z SFRs (see Dickinsons’ Spitzer Cy3 Legacy)  ISO provided ground for investigating monochromatic IR emission as SFR tracers, esp. UIB=AFE=(?)PAH (e.g., Madden 2000, Roussel et al. 2001, Boselli et al. 2004, Forster-Schreiber et al. 2004, Peeters et al. 2004, …). 8  m24  m F( )

SFR(24) Red: High Metallicity SF regions Green: Medium Metallicity SF regions Blue: Low Metallicity SF regions Black filled symbols: Low Met Starbursts and LIRGs Can we understand (and interpret) the slopes, and the spread, of the data? C. et al Slope is `super-linear’ (1.23) 2.Slight dependence on metallicity (Walter et al. 2007) 3.Spread is significant (0.4 dex FWHM) SFR(M o yr -1 ) = 1.27 x [L 24 (erg s -1 )] 0.885

Models L(IR) = 0 F S ( ) [1- 10 (-0.4 A( )) ] d L(8), L(24) Draine & Li 2006; assume mass fraction of low-mass PAH depends on metallicity F S ( ) ~ F S (mass/age,SFR,Z) Starburst99; Leitherer et al attenuation law/geometry=> A( ) Calzetti et al. 1994, Meurer et al. 1999; Calzetti 2001; implicit foreground. L(IR) H , P  (intr.) H , P  (obs) SFR - Extinction

SFR(24) in Models 4 Myr burst (or 100 Myr constant) SF, solar metallicity 1/10 Z Myr: o Larger-than-unity slope (in log-log scale) is effect of increasing `dust temperature’ o Non-linear behavior at decreasing luminosities is due to increasing ISM transparency o Spread due to range of HII regions ages (~2-8 Myr) o Some dependence on metallicity (Walter et al. 2007) L(IR) ~ L(P  ) for E(B-V) > 1 mag How do we get a super-linear slope? Draine & Li 2006

24  m Morphology vs IR/UV L(IR)/L(UV) F (70)/F (160) Dale et al Spirals D/Irr S/nuc

SFR(8) C. et al.2007 Red: High Metallicity SF regions Green: Medium Metallicity SF regions Blue: Low Metallicity SF regions Black symbols: Low Met Starbursts and LIRGs 1.Slope is `sub-linear’ 2.Strong dependence on metallicity 3.Dependence on region measured 4. Same spread as SFR(24) for high metallicity data.

SFR(8) in Models 4 Myr burst (or 100 Myr constant) SF, solar metallicity 1/10 Z Myr: o Lower-than-unity slope and region-size dependence unaccounted for by models; measured L(8) may be `contaminated’ by diffuse emission heated by underlying (non-star- forming) populations; or may be destroyed/fragmented by high intensity radiation. o L(8  m) is strongly dependent on metallicity; lower metallicity may lower number of low-mass PAH Draine & Li 2006

F(8  m) vs. metallicity Draine et al. 2007

A new `ground truth’ a L(H  )+b L(24  m) Kennicutt et al C. et al L(H  ) = unobscured SF L(24  m) = dust-obscured SF best fit slope ~ 1 Not necessarily `practical’ for high-z studies How can we compensate for increasing medium’s transparency at low IR emission end? SFR (M o yr -1 ) = 5.3 x [L H , obs L 24  m (erg s -1 )]

Dust Masses and Xco Draine et al. 2007

The Large Millimeter Telescope/ Grande Telescopio Millimetrico  A Mexico/USA collaboration  Single-dish 50 m antenna; 2.5 m secondary  8’ non-aberrated FOV; 6” resolution at 1 mm  ~1-4 mm science: cold dust emission, CO, HCN, etc.  Sensitivity is such that dwarf galaxies and interarm regions in spirals will be observable (or tight upper limits will be placed):  Will remove major limitations in current studies of the laws of star formation  Will be instrumental in understanding dependencies of the H 2 /CO ratio (X-factor) Expected first light ~ mid/end 2008

Conclusions  SFR(UV,  ) and SFR(UV+FIR) measure intrinsic SFRs in starbursts (  SFR > 0.3 – 1 M o /yr/kpc 2 );  In normal SF galaxies, the UV probes timescales up to ~ 100 Myr. Affected by both dust extinction and dust-age degeneracy. Conversion to SFR not immediate without `second parameter’ dependence.  SFR(FIR) probes star-forming as well as non-star-forming stellar populations, thus also potentially problematic (at the ~2-3x factor level) in normal SF galaxies. It is a `calorimetric’ measure (potentially limiting at high z).  SFR(8) and SFR(24) are more closely associated with H  than with UV (C. et al. 2005).  In the absence of AGNs, L(24) and L(24)+aL(H  provide more robust SFR indicators than L(8) (possibly also better than UV in normal SF galaxies)  Use of the 8  m emission requires extreme caution: very sensitive to both metallicity (30x) and presence of diffuse emission (PAH heated by the general stellar population; ~2x)  Although derived for HII regions/starbursts, preliminary studies indicate that calibrations should be applicable to general SF galaxy population (within 20%)