CCAT06 Chapman

Information about CCAT06 Chapman

Published on August 29, 2007

Author: CoolDude26

Source: authorstream.com

Content

CCAT - Sept13/06, CardiffPopulation of Far-IR background galaxies& z-machine style emission line surveys:  CCAT - Sept13/06, Cardiff Population of Far-IR background galaxies andamp; z-machine style emission line surveys Scott C. Chapman (IoA Cambridge) Galaxy Evolution:Where are we, where do we go?:  Galaxy Evolution: Where are we, where do we go? 1) Currently only scratching the surface of luminous/massive galaxies (Spitzer and Herschel are/will help considerably) -still unsure if we have census of all z~2 luminous galaxies 2) To really understand galaxy formation and evolution (andlt;M* galaxies), we need larger facilities. -finding the hyper-luminous peaks in different bands not enough. Counts and Models:  Counts and Models Old models (Dole+, Chary/Elbaz, Chapman/Lewis, etc.) easily fit data Spitzer forced refinements to models (eg., Lagache+04) -strength of aromatics/PAHs, range of SEDs for a given luminosity -epoch dependent density and luminosity evolution 24um N(z) Spitzer and submm galaxies:  N(z) Spitzer and submm galaxies 15um/24um hump at z~1 from 6-9um/11-14um aromatics also z~2 hump in 24um from 6-9um aromatics? (Chapman,Lewis,Helou 2003, 2005 model predictions) K-corrections mean that 15/24/850 probe CIB in well-defined, and distinct z ranges: z=0.7 (15um), z=1.1 (24um), z=2.3 (850um) Components of FIRB (SCUBA2 and CCAT):  Submm is almost all high-z galaxies (80% zandlt;4) MidIR and FarIR is 80% zandlt;1.7 SMM best (only?) way to probe the high-z components of FIRB Components of FIRB (SCUBA2 and CCAT) Dole et al. 2005 850 350 SCUBA contribution to mm/FIRB:  SCUBA contribution to mm/FIRB andgt;0.5mJy SCUBA population produces 80-100% of 850um background CCAT territory! Median redshift of bright SMGs is z~2.3 Fit dust SEDs to radio/850um at known z 850um population produces bulk of the andgt;400um FIRB andgt;5mJy fitted SMG SEDs andgt;5mJy Arp220 SED Corrected for andlt;5mJy sources The Star Formation History of the Universe :  The Star Formation History of the Universe SMGs are the main site of massive star formation at zandgt;2 UV galaxies evolve differently from SCUBA galaxies Balance between obscured and unobscured SF has shifted drastically in last 80% THub (Chapman et al. 2004) X-ray andamp; extended-radio =andgt; SCUBA galaxies not dominated by AGN interpret far-IR luminosities in terms of star formation (30% AGN) UV-selected SCUBA L* ? Spitzer -- SPICA/BLISS, ALMA, LMT, CCAT25 Confusion:  Confusion Currently impossible to probe high-z galaxies in FarIR! Nowhere near probing IR morphologies Submm/FIR Continuum: CCAT deep surveys…:  Submm/FIR Continuum: CCAT deep surveys… 850 850 200 160 350 600 Bivariate LF (Chapman+03) to model Td distribution. Molecular/Fine Structure emission lines :  Molecular gas defines sites of star formation IRAM-PdBI Needs precise redshifts (500Mhz band) 30 SMGs observed, 18 detected in CO (Neri et al. 2003, Greve et al. 2005, Tacconi et al. 2005) CO(3-2) Molecular/Fine Structure emission lines Longest baselines: Hi-Res CO studies:  Longest baselines: Hi-Res CO studies (Tacconi et al. 2005) Fine Structure Lines: COLD, 3.5m aperture:  Fine Structure Lines: COLD, 3.5m aperture ULIRG Cii CCAT/z-spec Simulation of all galaxies in 1’ beam: :  Simulation of all galaxies in 1’ beam: -Bivariate LF : emission line templates matched to Arp220 or M82 based on dust temperature. -14 brightest galaxies contribute the bulk of the detectable lines. -CCAT targeted low-res spectroscopy could survey large numbers of obscured galaxies for redshifts, line strengths and ratios. The End:  The End

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