A multiwavelength view of galaxy evolution with AKARI

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

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

Outline • XTENDED PS program of resolved galaxies – Old friends: M 31, Arp 220, M 82, 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

M 31 • 90μm: blue • 140μm: green • 160μm: red

M 81 / M 82 Credit: Chynoweth et al. , NRAO/AUI/NSF, Digital Sky Survey

M 81 / M 82

M 81 / M 82 • 90μm: blue • 140μm: green • 160μm: red

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

IRAS F 10214+4724 • 60μm: blue • 90μm: green • 140μm: red Well, maybe ; )

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

Herschel Reference Survey • Volume-limited (15 -25 Mpc) and Ktot ≤ 12 (late-type) or Ktot ≤ 8. 7 (E, S 0, 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

SPIRE Mdust = 5. 5× 107 M SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

SPIRE Mdust = 7. 4× 107 M SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

SPIRE Mdust = 3. 4× 107 M SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

SPIRE Mdust = 6. 5× 107 M SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

SPIRE Mdust = 8. 5× 107 M SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

SPIRE Mdust = 8. 3× 107 M SEDs & SPIRE images courtesy of Matt Smith, Cardiff See Ciesla et al. in preparation

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 He. Vi. CS, but field sample lacks sensitive FIR data.

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

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

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

Herschel ATLAS • 550 deg 2 (1% of sky) at 110 -500μm to close to confusion limits at 250500μm • Largest open time key project on Herschel

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

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

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

AKARI Abell 2218 Hopwood et al. 2010 Ap. JL 716, L 45

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

Link between Herschel & AKARI populations in Abell 2218 • 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) Hopwood, Negrello, Serjeant 2012 MNRAS in preparation

Prospects for NEP field • Herschel: OT 2 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. 2 m telescope launch in 2019): ~20 k 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

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