Dusty star-forming galaxies at high redshift (part 5) Flow of story 4.1.1 4.1.2 4.1.3 Millimetric Spectroscopic Redshifts Millimetric Photometric Redshifts Redshift Distributions of 24 μm selected DSFG populations 1
Millimetric Spectroscopic Redshifts millimetric spectroscopic redshifts mm-wavelength molecular gas emission lines DSFGs receiver bandwidth PdBI (Plateau de Bure Interferometer) WIDEX bandwidth correlator Millimetric Spectroscopic Redshifts millimetric spectroscopic redshifts multi-wavelength couterpart identification mm detect mm emission lines ALMA CO molecular gas CII cooling line submm DSFGs follow-up unlensed DSFGs 2
Millimetric Spectroscopic Redshifts lensed DSFGs Fig 16. lensed DSFGs mm (composite) Flow of story 4.1.1 4.1.2 4.1.3 Millimetric Spectroscopic Redshifts Millimetric Photometric Redshifts Redshift Distributions of 24 μm selected DSFG populations 3
Millimetric Photometric Redshifts millimetric photometric redshifts FIR/submm SED color DSFGs SED redshift rough intrinsic SED SED peak wavelength infrared luminosity redshift (?) Flow of story 4.1.1 Millimetric Spectroscopic Redshifts 4.1.2 4.1.3 Millimetric Photometric Redshifts Redshift Distributions of 24 μm selected DSFG populations 4
Redshift Distributions of 24 μm selected DSFG populations redshift distribution at 24 μm >300 mjy 24 μm galaxies z ~ 0.3 peak z ~ 0.9 2 peak z ~ 4.5 low-z or PAH emission redshift feature z ~ 2 DSFGs AGN-driven emission dominant (~55 %) DOGs luminosity 50 % 24 μm flux density Compton thick AGN Flow of story 4.1.4 4.1.5 Redshift Distributions of 850 μm-1.4 mm-selected DSFG populations Redshift Distributions of 250 μm-500 μm-selected DSFG populations 5
850/870 μm-selected DSFG population Fig 17. 850-870 μmselected galaxies redshift distribution 850/870 μm-selected DSFG population Chapman et al. 2005 radio counterparts radio counterparts <1 multi-slit spectroscopic targets 73 median z = 2.2 850 μm-selected galaxies 6
850/870 μm-selected DSFG population selection effect required sub-selection in radio 1.4 GHz continuum high-z galaxies <- radio positive K-correction very cold-dust SMGs <- higher S 850 /S 1.4 ratio dearth of sources between 1.2 < z < 1.9 LRIS redshift desert <- no bright emission lines lower redshifts -> OII, Hβ, OIII, Hα higher redshifts -> Lyα coverage = 3000~8000 Å -> 3000~10000 Å (desert z ~ 1.7) 850/870 μm-selected DSFG population high-z (z > 4) 850 μm-selected SMGs GN20 @ z = 4.055 (Daddi et al. 2009) LESS J033229.4-275619 @ z = 4.76 (Coppin et al. 2009) HDF 850.01 @ z = 5.17 (Walter et al. 2012) => Big Bang 1 Gyr SMGs LRIS spectroscopic desert DEIMOS -> z ~ 1.5 (Banerji et al. 2011) 7
850/870 μm-selected DSFG population Wardlow et al. 2011 optical/nir photometric analysis populations ECDFS LABOCA map noise 870 μm LABOCA-selected NIR samples missing source redshift bias radio detection completeness Lewis et al. 2005 (peak z ~ 2.5) 850/870 μm-selected DSFG population Wardlow et al. 2011 ALMA LABOCA-selected source multiplicity high resolution representative sample of 850/870 μm 850 μm samples median redshifts survey depth area limits brighter sources high-z (Pope et al. 2006, Koprowski et al. 2013) 8
1.1 μm-selected DSFG population Fig 18. 1.1 μm-selected DSFGs redshift distribution 1.1 μm-selected DSFG population 850 μm-selected SMGs completeness samples Chapman et al. 2009 median z = 2.7 850 μm Chanpman et al. (z = 2.2) Wardlow et al. (z = 2.5) Yun et al. 2012 optical/nir redshift distribution median z = 2.6 9
1.1 μm-selected DSFG population log-normal distribution fit f z = Smolcic et al. 2012 1 exp [ln 1+z ln(1+z μ)] 2 (1+z)σ 2π 2σ 2 submm multiplicity redshift (z = 3.1 ± 0.3) cosmic variance interferometric follow-up photometric redshift optical/nir photometric 1.4 μm-selected DSFG population Fig 18. 1.4 μm-selected DSFGs redshift distribution 10
1.4 μm-selected DSFG population Weiβ et al. 2013 samples gravitationally lensed galaxies SPT unlensed DSFGs detect depth z < 2 lensing bias phenomenological (Béthermin et al. 2012b) hybrid cosmological hydrodynamic (Hayward et al. 2013a) semi-analytic (Lacey et al. 2010, Benson et al. 2012) 1.4 μm-selected DSFG population SPT samples most spectroscopically complete DSFG samples DSFGs redshift size evolution lensing (Hezaveh & Holder et al. 2011) high-z compact 1.4 mm redshift distribution 11
Flow of story 4.1.4 4.1.5 Redshift Distributions of 850 μm-1.4 mm-selected DSFG populations Redshift Distributions of 250 μm-500 μm-selected DSFG populations Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Fig 19. 250-500 μmselected DSFGs redshift distribution 12
Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population 850 μm-1.1 mm BLAST H-ATLAS HerMES survey luminosity dynamic range survey detect 250-500 μm DSFGs 850 μm detect different redshift or SED characteristics selection wavelength (Bethermin et al. 2012b) 250 μm population 500 μm population redshift distribution Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population median redshift high redshift sample biases intrinsic SED variation, detection limits redshift distribution population selection 13
Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Negrello et al. 2007 250-500 μm-selected lensed populations phenomenological model S 350 > 100 mjy z ~ 2 peak Lagache et al. 2005 overall 350 μm populations z ~ 1 peak high-z model physical and Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Béthermin et al. 2011 very low redshifts 1 peak z ~ 2 2 peak Béthermin et al. 2012b star-forming galaxies stellar mass function IR main sequence empirical approach main sequence status template Magdis et al. 2012b 14
Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Amblard et al. 2010 H-ATLAS source SPIRE color millimetric redshift redshift redshift SED SPIRE color color-color redshift SPIRE source median z = 2.2 ± 0.6 Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Chapin et al. 2011 69 BLAST-detected ECDFS sources 0.5 < z < 3 flat z ~ 0.3 peak Casey et al. 2012a, b ~1600 HerMES SPIRE-selected galaxies ( ~800 optical ) median z = 1.1, peak z = 0.8 z ~ 5 spec/phot-z characterize 15
Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Chapin et al. 2011 Casey et al. 2012a, b z ~ 0.3 peak statistically consistent peak ECDFS cosmic variance Lagache et al. 2005 SED Negrello et al. 2007 Béthermin et al. 2012b statistically different Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Amblard Chapin Casey SPIRE galaxies SED shape different assumed temperature-luminosity relation peak 1.4 GHz 24 μm counterparts high-z galaxies optical redshift samples bias lower redshift 16
Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population Fig 19. 250-500 μmselected DSFGs redshift distribution Redshift Distributions of 250 μm-500 μm-selected DSFG populations 250-500 μm-selected DSFG population 450 μm redshift distribution SCUBA-2 (~7 ) Roseboom et al. 2013 -> median z = 1.4 Casey et al. 2013 -> median z = 1.95 survey depth 17
Flow of story 4.1 4.2 4.3 Acquiring Spectroscopic or Photometric Redshifts Infrared SED Fitting for DSFGs Estimating L IR, T dust and M dust from an SED Infrared SED Fitting for DSFGs FIR SED fitting dust emission infrared luminosity obscured star formation rate dust temperature and dust mass template libraries scaling relations direct data fitting, parametrized fits 18
Infrared SED Fitting for DSFGs FIR SED fitting photometric data model FIR emission dust distribution composition dust grain type orientation galaxy structure band parameter AGN heating emissivity and optical depth etc Infrared SED Fitting for DSFGs FIR SED fitting CO, CII emission line broadband submm flux densities 20-40 % contaminate SED fitting techniques direct comparison to models using Bayesian techniques modified black body functions stellar emission dust emission fit 19
Flow of story 4.2.1 Employing dust radiative transfer models and empirical templates 4.2.2 Direct modified blackbody SED modeling Employing dust radiative transfer models and empirical templates geometry luminosity dust infrared emission modeling accuracy applicability geometry distribution, optical depth high-z dusty starbursts SED fitting 20
Employing dust radiative transfer models and empirical templates Silva et al. 1998 UV FIR / stellar population synthesis models code age metalicity SFR gas fraction integrated spectra dust geometry chemical evolution dust grain size distribution relative gas trapped in MC versus diffuse ISM Employing dust radiative transfer models and empirical templates Chary & Elbaz 2001 Silva et al. 1998 z ~ 1 infrared-luminous galaxies SED population CIB mid-ir ISOCAM data 4 (Arp 220, NGC 6090, M82, M51) SED 20 μm Dale et al. 2001 21
Employing dust radiative transfer models and empirical templates Dale et al. 1998 dust emission curves dust mass distribution power-law SED @ FIR small, large, PAH grains 69 data normal galaxies S 60 /S 100 Dale & Helou 2002 Dale et al. 1998 >120 μm Employing dust radiative transfer models and empirical templates Dopita et al. 2005 UV FIR, radio SED STARBURST99 (Leitherer & Heckman 1995) model nebular line emission model dynamic evolution model of HII regions simplified synchrotron emissivity model stellar population synthesis model solar-metalicity starburst self-consistent SED FIR emission starburst ambient pressure 22