CCAT06 Chapman

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