1. A multi-wavelength view of galaxy evolution with AKARI Stephen Serjeant 29 th February 2012

2. A multi-wavelength view of galaxy evolution with AKARI Stephen Serjeant 29 th February 2012

3. Outline XTENDED PS program of resolved galaxies –Old friends: M31, Arp 220, M82, NGC 253 etc –The Herschel Reference Survey –The JCMT Nearby Galaxies Survey Bright galaxies in the Herschel ATLAS key project –Nearby galaxies (see also Chris Pearson’s talk) –Bright submm galaxies (see also Chris Sedgwick’s talk) and strong gravitational lenses The link between Herschel and AKARI ultra-deep populations The prospects for Herschel data in the NEP-Deep field

4. 90μm: blue 140μm: green 160μm: red M31

5. Credit: Chynoweth et al., NRAO/AUI/NSF, Digital Sky Survey M81 / M82

7. 90μm: blue 140μm: green 160μm: red

8. Image: CFH NGC 253 90μm: blue 140μm: green 160μm: red

9. IRAS F10214+4724 60μm: blue 90μm: green 140μm: red Well, maybe ;)

10. Arp 220 AKARI photometry shown in red Aperture effect? Or saturation? Assume AKARI flux calibration correct in the following SEDs

11. Herschel Reference Survey Volume-limited (15-25 Mpc) and K tot ≤ 12 (late-type) or K tot ≤ 8.7 (E, S0, Sa) Goals: e.g. census of cold dust along Hubble sequence; relation between dust emission and star formation; galaxy extinction; dust in ellipticals Over 1/3 of the sample lack sensitive far-IR data (e.g. Spitzer, Herschel PACS) The following are preliminary photometry from the AKARI all-sky survey diffuse maps; photometric errors probably underestimated

12. M dust = 5.5×10 7 M  SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation SPIRE

13. M dust = 7.4×10 7 M  SPIRE SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

14. M dust = 3.4×10 7 M  SPIRE SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

15. M dust = 6.5×10 7 M  SPIRE SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

16. M dust = 8.5×10 7 M  SPIRE SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

17. M dust = 8.3×10 7 M  SPIRE SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

18. JCMT Nearby Galaxies Survey Legacy Survey on the JCMT Observations: sub-kpc resolved CO (J=3-2) and continuum (450μm and 850μm) in 155 nearby galaxies Sample: –SINGS (heterogenous selection) –HI-selected field galaxies –HI-selected Virgo cluster galaxies. Goals: physical properties of dust; gas:dust ratio; effects of morphology and environment SINGS has Spitzer & Herschel FIR data; Virgo sample has Herschel PACS from HeViCS, but field sample lacks sensitive FIR data.

19. NGC 1156 140μm (Wide-L) 2’x2’ shown AKARI resolution can benefit photometry in higher cirrus regions

20. LIRG/ULIRG SMG QSO LBG Spiral o Irregular Peculiar / Wolf-Rayet JCMT Nearby Galaxies Survey: FIR vs CO Extends nearly linear L FIR vs. L CO(3-2) relation to ~5 orders of magnitude lower L FIR in homogeneously-selected local sample Iono et al. 2009 & JCMT NGLS field sample N B the few heterogeneously-selected local galaxies in the Iono sample are not plotted

21. JCMT Nearby Galaxies Survey: FIR vs CO L FIR /L CO  SFR/M CO  Molecular gas depletion time ~3 Gyr Iono et al. 2009 & JCMT NGLS field sample LIRG/ULIRG SMG QSO LBG Spiral o Irregular Peculiar / Wolf-Rayet N B the few heterogenously-selected local galaxies in the Iono sample are not plotted

22. Herschel ATLAS 550 deg 2 (1% of sky) at 110-500μm to close to confusion limits at 250- 500μm Largest open time key project on Herschel

23. Herschel ATLAS UGC 4754 (Baes et al. 2010): radiative transfer models under-predict far- IR by ~×2 Suggests presence of highly obscured star formation that does not contribute significantly to global extinction See also Chris Pearson’s talk for AKARI detections of H-ATLAS local galaxies

24. Herschel ATLAS Bright Herschel population also a rich source of strong lenses – not every optical ID is physically associated with the far-IR See Negrello et al. 2010 Science Arises due to steep intrinsic high-z galaxy submm source counts

25. Herschel ATLAS Bright Herschel population also a rich source of strong lenses – not every optical ID is physically associated with the far-IR See Negrello et al. 2010 Science Arises due to steep intrinsic high-z galaxy submm source counts HST SNAPs; Negrello et al. in prep

27. AKARI Abell 2218 Hopwood et al. 2010 ApJL 716, L45

28. Hopwood, Negrello, Serjeant 2012 MNRAS in preparation Stack 15μm positions in Herschel maps Link between Herschel & AKARI populations in Abell 2218

29. Hopwood, Negrello, Serjeant 2012 MNRAS in preparation Stack 15μm positions in Herschel maps Results: the 15μm population contributes 41%, 33%, 27% of the CIRB at 250μm, 350μm, 500μm (uncertainties dominated by ~5σ CIRB measurements) Link between Herschel & AKARI populations in Abell 2218

30. Prospects for NEP field Herschel: OT2 award (see Chris Pearson’s talk) SCUBA-2: scheduled to observe NEP in UH time and remains a deep field in re-scoped JCMT Cosmology Legacy Survey LOFAR: NEP in tier 2 of extragalactic wedding cake (50 hours per pointing) Euclid (1.2m telescope launch in 2019): ~20k deg 2 shallow survey & ~40 deg 2 of deep surveys (vis,Y,J,H to 26-26.5 mag 5σ) plus 1.1-2μm low-resolution spectra; Ecliptic Poles are the only deep fields guaranteed to be observed given orbit visibility constraints

31. Conclusions Preliminary photometry in Herschel reference survey: dust masses for the HRS field sample Preliminary photometry in JCMT Nearby Galaxies Legacy Survey: L FIR vs. L CO(3-2) relation extended in homogeneously-selected sample to ~5 orders of magnitude lower L FIR ; molecular gas depletion timescale ~3Gyr AKARI 15μm ultra-deep population contributes ~1/3 of submm background in Herschel SPIRE bands