Aug 8th, 2007MAGPOP Summer School Models for source counts and background spectrum, from submm to ultraviolet ingredients for counts model at submm to uv wavelengths star-formation history, luminosity functions assumed seds, parameter estimation predicted counts and background intensity

Aug 8th, 2007MAGPOP Summer School MODELS FOR COUNTS AND BACKGROUND FROM OPTICAL TO SUBMM (Rowan-Robinson 2001, ApJ, 549, 745, 2007, in prep) * parameterized approach to star formation history * fitted to infrared and submm counts and background * 60  m luminosity function derived from PSCz data * ir and submm seds based on mixture of four components (cirrus, M82-starbust, AGN dust torus, Arp220), proportions depending on luminosity

Aug 8th, 2007MAGPOP Summer School OTHER RECENT WORK Franceschini et al, 2001, AA 378, 1 Gispert et al, 2000, astro-ph/ Xu et al, 2001, ApJ 562, 179 Takeuchi et al, 2001, PASJ, astro-ph/ Pearson et al, 2001, MN 325, 1511 Elbaz et al, 2002, AA 384, 848 Lagache et al, 2004, ApJS 154, 112 Gruppioni et al, 2005, ApJ 318, 9 Lagache, Puget, Dole, 2005, ARAA 43, 727

Aug 8th, 2007MAGPOP Summer School PARAMETERIZED MODEL FOR STAR FORMATION HISTORY * assumed star formation history: sfr =  * (t)/  * (t o ) = exp Q{1 - t/t o }. (t/t o ) P meaning of parameters: t 0 /Q =  sf (cf Bruzual,Charlot 1993) peak sfr when t/t o = P/Q, or t = P  sf (essentially the Bruzual and Charlot models with an additional parameter to tune the epoch of peak star formation rate) * assume 60 µm luminosity function of the form  (L) = C * (L/ L * ) 1-  exp{-0.5[log 10 (1+L/L * )/  ] 2 } (Saunders et al 1990) * assume luminosity evolution with L * (t)/L * (t o ) =  * (t)/  *( t o ) * for each P,Q, parameters L * (t o ) and  are solved for from PSCz data (15000 IRAS galaxies with known z, S(60)≥ 0.6 Jy)

Aug 8th, 2007MAGPOP Summer School parameterized star-formation history sfr =  * (t)/  * (t o ) = exp Q{1 - t/t o }. (t/t o ) P meaning of parameters: t 0 /Q =  sf peak sfr when t/t o = P/Q, or t = P  sf

Aug 8th, 2007MAGPOP Summer School assumed seds, fit to counts, predictions assumed spectral energy distribution, to convert luminosity function to other wavelengths, is mixture of cirrus, M82-starburst, AGN dust torus, Arp220-starburst components (radiative transfer models from Efstathiou et al 2000, Rowan-Robinson 1995), with proportion varying with 60 µm luminosity, to match colour-colour and colour-luminosity diagrams * fit to observed counts at 60, 850 µm, and background intensity at 140, 350, 750 µm to find best (least chi 2 ) values of P,Q: Ω o  PQ best-fitting models then used to predict counts and background spectrum at  m

Aug 8th, 2007MAGPOP Summer School Infrared templates

Aug 8th, 2007MAGPOP Summer School colour-colour, colour-luminosity (Rowan- Robinson 2001)

Aug 8th, 2007MAGPOP Summer School Luminosity function at 850  m

Aug 8th, 2007MAGPOP Summer School Luminosity function at 60  m

Aug 8th, 2007MAGPOP Summer School Luminosity function at 12  m

Aug 8th, 2007MAGPOP Summer School Luminosity function at 0.44  m

Aug 8th, 2007MAGPOP Summer School Counts at 15 and 850  m

Aug 8th, 2007MAGPOP Summer School Counts at 90 and 175  m

Aug 8th, 2007MAGPOP Summer School Counts at 0.44 and 1.6  m (King and RR 2002: improved fits using some density evolution)

Aug 8th, 2007MAGPOP Summer School Redshift distributions

Aug 8th, 2007MAGPOP Summer School Star- formation history (Rowan-Robinson 2003b)

Aug 8th, 2007MAGPOP Summer School differential counts at 24  m 24  m differential counts (Shupe et al, 2007, Papovich et al 2004)

Aug 8th, 2007MAGPOP Summer School new model for 24  m counts 24  m differential counts (Shupe et al, 2007, Papovich et al 2004) new model for ir counts (developed from RR 2001 models): independent evolution for each component, evolution has to flatten off at z < 0.5 M82 cirrus dust tori

Aug 8th, 2007MAGPOP Summer School SHADES counts at 850  m Coppins et al, 2007, astro-ph/

Aug 8th, 2007MAGPOP Summer School differential counts at  m new SWIRE 70, 160 and SHADES 850  m differential counts (Afonso-Luis et al, 2007, in prep, Coppins et al 2007)

Aug 8th, 2007MAGPOP Summer School contribution of different fir luminosity ranges to star-formation rate blue: lg L firr /L o < 11 orange: 11 < lg L firr /L o < 12 red: 12 < lg L firr /L o green: total LeFloch et al, 2005, ApJ Reddy et al 2007

Aug 8th, 2007MAGPOP Summer School star-formation history to z = 6 Thompson et al 2006 Reddy et al 2007

Aug 8th, 2007MAGPOP Summer School Frank Low: 1968: the far infrared background

Aug 8th, 2007MAGPOP Summer School the far ir and submm background Hauser and Dwek, 2001, ARAA 39, 249

Aug 8th, 2007MAGPOP Summer School the interpretation of the extragalactic background the integrated extragalactic background spectrum is a weighted integral of the star-formation history I = c | o to  (t) L Z (t) dt weighting is by K-correction L Z /L so submm weighted to higher redshift than far and mid ir submm background can give strong limit on high z sfr

Aug 8th, 2007MAGPOP Summer School Models for infrared background Rowan-Robinson 2001

Aug 8th, 2007MAGPOP Summer School far ir and submm background from stacking analyses

Aug 8th, 2007MAGPOP Summer School Models for infrared background Rowan-Robinson 2007 now have good bg data at 24, 70, 160  m models, modified to fit 24  m counts, now also give better fit to background spectrum

Aug 8th, 2007MAGPOP Summer School History of the universe

Aug 8th, 2007MAGPOP Summer School the future Darwin TPF ALMA Herschel