radtrans07

Radiative transfer models for extragalactic infrared sources: 

Radiative transfer models for extragalactic infrared sources radiative transfer models for ir sources cirrus models for local quiescent galaxies models for starburst, UKIRGs, HLIRGs applications to Spitzer galaxies, submm galaxies IRS spectra and their interpretation

ingredients for models for seds of infrared sources: 

ingredients for models for seds of infrared sources model for interstellar grains [ Mathis et al 1977, Draine and Lee 1984, Rowan-Robinson 1992, Desert et al 1990, Siebenmorgen and Krugel 1992, Dwek 1998] assumed density distribution for dust [r ~r-b, HII region physics (Yorke 1977, Efstathiou et al 2000)] dust geometry [ spherically symmetric, axisymmetric (Efstathiou and RR 1990, 1991, 1995, Pier and Krolik 1992, Granato et al 1994, 1997, Silva et al 1998), clumpy [Rowan-Robinson 1995, Hoenig et al 2006] radiative transfer code [Rowan-Robinson 1980, Efstathiou and RR 1990, Pier and Krolik 1992, Krugel and Siebenmorgen 1994, Granato et al 1997, Silva et al 1998, Popescu et al 2000, Hoenig et al 2006]

Radiative transfer models for infrared sources: 

Radiative transfer models for infrared sources spherically symmetric dust clouds - first accurate code 1980 (R-R, ApJS 234, 111) - circumstellar dust shells 1981-3 starbursts and ULIRGs (RRE, 1993, MN 263, 675; ERRS, 2000) cirrus galaxies (ERR, 2003) axially symmetric dust clouds - first accurate code 1990 (Efstathiou and R-R, MN 245, 275) - protostars 1991 - AGN dust tori 1995

the radiative transfer equation: 

the radiative transfer equation The intensity of radiation In(r,q) satisfies the equation dIn/ds = - n(r) Cn,ext In + n(r) Cn,abs Bn [T(r)] + n(r) |4p Cn,sc (q’) In (q’) dw/4p where Cn,abs = pa2 Qn,abs , Cn,sc = pa2 Qn,sc z(q’) Cn,ext = Cn,abs + |4p Cn,sc (q’) dw/4p

interstellar dust grains: 

interstellar dust grains size 50 A - 0.1 mm (and larger ?) composition: amorphous C graphite amorphous silicates crystalline silicates SiC PAHs Brownlee particle

discovery of PAHs: 

discovery of PAHs Leger and Puget, 1984, AA 137, L5

IRAS - cirrus: 

IRAS - cirrus south celestial pole

Cirrus models for local galaxies: 

Cirrus models for local galaxies assume optically thin ism, extinction AV (<1, 0.4-0.9) BC starburst models, age t*, exponential decay time t characterise galaxies by single mean intensity, y = bolometric intensity/solar neighbourhood intensity (~2-5) for local galaxies, t* = 0.25 Gyr, t = 5-11 Gyr (Efstathiou and Rowan-Robinson 2003, MN 343, 322)

IRAS - star forming regions: 

IRAS - star forming regions constellation Orion LMC

IRAS - ultraluminous infrared galaxies: 

IRAS - ultraluminous infrared galaxies Arp 220 Soifer et al, 1984, ApJ 283, L1: the remarkable infrared galaxy Arp 220

Slide11: 

Eftstathiou, R-R, Seibenmorgen, 2000, MN 313, 734 embedded phase, t < 107 yrs expanding neutral shell, t = 107-108 years at 108 yrs, indistinguishable from cirrus Models for starburst galaxies

Slide13: 

galaxy sed model fits from GRASIL (Silva et al 1998)

seds of ultraluminous infrared galaxies : 

seds of ultraluminous infrared galaxies L:ISO R:SPITZER

IRAS - AGN dust tori: 

IRAS - AGN dust tori Miley et al, 1984, ApJ 278, L79: A 25 mm component in 3C390.3

Infrared templates: 

Infrared templates (Rowan-Robinson 2001)

Hyperluminous infrared galaxies: 

Hyperluminous infrared galaxies Rowan-Robinson, 2000, MN 316, 885 starburst dominated IRAS F10214, z=2.3 galaxy Teplitz et al 2006

dust torus dominated: 

dust torus dominated

SPITZER-IRS: IRAS F00183-7111, hyperluminous infrared galaxy: 

SPITZER-IRS: IRAS F00183-7111, hyperluminous infrared galaxy IRS spectrum of the hyperluminous ir galaxy F00183-7111 = IRAS P00182-7112 (Spoon et al 2004) z = 0.327 (narrow line object), lg Lsb = 13.25

Ltor v. Lsb: 

Ltor v. Lsb

Lsb v. Mgas: 

Lsb v. Mgas broken lines show time-scale to convert gas mass into stars ULIRGs and HLIRGs have bursts on shorter time-scale, or need truncated IMF

cirrus models for SCUBA galaxies: 

cirrus models for SCUBA galaxies Efstathiou and R-R (2003) found that cirrus models, with slightly higher AV and y ( ~ 2-3 times higher than local quiescent galaxies) can also fit high-z galaxies from SCUBA blank-field surveys restrict analysis to SCUBA sources: (a) which have been confirmed by submm interferometry, or (b) sources from 8 mJy survey which have radio associations 70% of sources (16/23) successfully modeled by cirrus model. Note: models fit radio data also. assume t* = 0.25 Gyr, t = 6 Gyr

SCUBA galaxies: 

SCUBA galaxies

z<0.12 galaxies with cirrus seds: 

z<0.12 galaxies with cirrus seds Rowan-Robinson et al, 2005, AJ 129, 1183 sources with good ISO-ELAIS and SPITZER-SWIRE data templates

z=0.1-0.9 galaxies: 

z=0.1-0.9 galaxies fitted with cirrus or A220 template A220 model: AV = 200, t* = 26 Myr (Efstathiou and RR 2001)

seds of z=0.1-2.2 galaxies/quasars: 

fitted with cirrus, A220 starburst and AGN dust torus templates seds of z=0.1-2.2 galaxies/quasars

SPITZER-IRS spectra of ELAIS sources: 

SPITZER-IRS spectra of ELAIS sources IRS spectra for 70 ELAIS-N1 and -N2 sources with S15> 1mJy validate the template fits most are ULIRGs, with z =1-3 Filled circles: optical, ISO, SWIRE ( and MAMBO) data Solid curves: model seds Red curve: calibrated IRS data (Hernan-Caballero et al 2006)

seds of submillimetre galaxies: 

seds of submillimetre galaxies SHADES SXDS Clements et al 2007

what powers ultraluminous infrared galaxies ?: 

what powers ultraluminous infrared galaxies ? Genzel et al, 1998, ApJ 498, 579

what powers ultraluminous infrared galaxies ?: 

what powers ultraluminous infrared galaxies ? Spoon et al, 2007, astro-ph/0611918