may 19-22, 2014bologna pg course infrared and submillimetre surveys, models for counts and...

May 19-22, 2014 Bologna pg course

Infrared and submillimetre surveys, models for counts

and backgroundMichael Rowan-

RobinsonImperial College

London1. Extragalactic infrared and submillimetre surveys2. Models for source-counts and background radiation, from submm to ultraviolet


Extragalactic infrared and submillimetre

surveysMichael Rowan-

RobinsonImperial College

London

Dole et al 2006

most of the starlight ever generated in the universe is emitted at infrared wavelengths, ~ 50% is absorbed by dust and reemitted at far infrared and submillimetre wavelengths


Pre-IRAS, IRAS

Pre-IRAS: 1969: Caltech 2 Micron Survey (Neugebauer and Leighton) – circumstellar dust shells, BN object1976: The AFGL Survey at 4.2, 11, 19.8 and 27.4 m

(Price and Walker) – cds, HII regionsIRAS:1984: IRAS all sky survey at 12, 20, 60, 100 m

- 30,000 infrared galaxies (measured redshifts of 12000 with S(60)>0.6 Jy - PSCz)

- ir cirrus- ULIRGS, HLIRGS- AGN dust tori- ir dipole, large scale structure


Infrared galaxy populations

with IRAS we were able to identify the main infrared galaxy populations

- quiescent galaxies (ir cirrus)- starburst galaxies (prototype M82)- extreme starbursts (prototype A220)- AGN dust tori

but the IRAS survey was not deep enough (z ~ 0.3) to study the cosmological evolution of these populations, though 60 m source-counts showed that evolution is present, at a comparable rate to that seen in radio-galaxies and quasars

an important insight was that as infrared luminosity increased, the proportion of interactions and mergers increased

new IRAS FSC galaxy redshift catalogue: Wang and R-R 2014


ISO surveysCAM Deep Surveys

Fadda et al, 2001, AA, astro-ph/011412 Franceschini et al, 2002, AA,

astro-ph/0108292Elbaz et al, 2002, AA 384, 848

ELAIS Survey at 6.7, 15, 90, 175 mOliver et al, 2000, MN 316, 749Serjeant et al, 2000, MN 316, 768Efstathiou et al, 2000, MN 319, 1169Serjeant et al, 2001, MN 322, 262Lari et al, 2001, MN 325, 1173Gruppioni et al, 2002, MN 341, L1Rowan-Robinson et al, 2004, MN 351,

1290ISO HDF-N and HDF-S surveys

Oliver et al, 2002, MN 332, 546Mann et al, 2002, MN 332, 549

FIRBACK 175 m surveyDole et al, 2001, AA 372, 264


ISO surveys * main result was very strong increase in star-formation rate in galaxies between z = 0 and 1 (factor ~10) (Rowan-Robinson et al 1997, Flores et al 1999), confirming the result from optical surveys (Lilley et al 1996, Madau et al 1996) and that the rate estimated from optical data without correction for extinction is severely underestimated.

• issue of consistency between estimates of star-formation rate from uv, H, radio, far infrared

sfr = 2.2 x 10-10 L60 = 2.5x10-8 LH = 4.5x10-10 L2800A


ISO counts at 15 m


Submillimetre surveysHubble Deep Field North

Hughes et al 1998

Hawaii surveysBarger et al 1998, 1999, Cowie et al

2002, Wang et al 2004

CUDSS surveyEales et al 1999, Webb et al 2003,Clements et al 2004, Ashby et al 2006

UK 8 mJy survey (200 sq arcmin)Scott et al 2001, Fox et al 2001,Ivison et al 2002, Almaini et al 2003

SHADES (0.5 sq deg)Mortier et al 2005, Coppin et al 2006, Ivison et al 2007, Aretxaga et al 2007

SCUBA Legacy Surveys (SASSy and CLS) – in progress


SHADES counts at 850 m

Coppins et al, 2007


Near-ir Surveys2MASS all-sky survey at J, H, K (to 15.8, 15.1, 14.3 mag.)

– http://www.ipac.caltech.edu/2mass/UKIDDS survey of 7500 sq deg in JHK (K=18.3)

-http://www.ukidss.org/

FIR SurveysSPITZER surveys (GTO - various, FLS - 4 sq deg, SWIRE - 49 sq deg, GOODS - 0.1 sq deg, AEGIS - 1 sq deg, COSMOS - 1 sq deg) at 3.6, 4.5, 5.6, 8, 24, 70, 160 m

- http://ssc.spitzer.caltech.edu/

AKARI all-sky survey in 6 bands at 9-180 m- http://www.akari.org.uk


Layered SPITZER Surveys• Wide–shallow FLS GTO-shallow SWIRE

– greatest volume 4 8.5 49 sq deg

– rare luminous objects– large-scale structure

• Confusion-limited GTO-deep GOODS-IRAC– maximum information 2.5 sq deg 300 sq arcmin

on faintest resolved sources

• Ultra-deep GTO-ultra GOODS-24 m– confusion distribution 150 300 sq arcmin


SPITZER SWIRE survey

49 sq deg in 6 areas, at 3.6, 4.5, 5.8, 8, 24, 70, 160 m


differential counts at 24 m

• 24 m differential counts (Shupe et al, 2007, Papovich et al 2004)


AKARI• Japanese mission, 68 cm cooled telescope, first all-sky far infrared survey since IRAS, 90 and 140 m, sensitivity comparable to IRAS FSS, better spatial resolution, but worse confirmation rate


HERSCHEL3.6 m passively cooled telecope operating at 50-500 m

layered extragalactic surveys were carried out by SPIRE and PACS teams in guaranteed time


HERSCHEL surveys• SPIRE-HerMES survey of ~100 sq deg at 250, 350, 500 m• H-ATLAS survey of 550 sq deg at 100, 160, 250, 350, 500 m• PACS-PEP survey of GOODS-S at 70, 100, 160 m

• HerMES counts - Oliver et al 2010• H-ATLAS counts – Clements et al 2010• PEP counts – Berta et al 2010• counts and luminosity functions at 70, 100, 160 – Magnelli et al

2013• evolution and luminosity functions to z ~ 4 at 70-500 m –

Gruppioni et al 2013

Hermes source-counts

Oliver et al. A&A 518, L21 counts + P(D) account for large fraction of infrared background



PACS 100 and 160 m countsMagnelli et al 2013


FIR luminosity density as function of z


star-formation history to z = 6

Thompson et al 2006

Reddy et al 2007


Templates, z distribns, in PEP survey

Gruppioni et al 2013

100

160


FIR luminosity function from z = 0-4


a schematic evolutionary scenario


PLANCKPLANCK carried out a shallow all-sky extragalactic point-source survey, which detected several thousand galaxies, a few high-z very luminous submm galaxies


AKARIAKARI carried out an all-sky point-source survey, at 9, 18, 65, 90, 140, 160 m.

AKARI-FIS All-sky Bright Source Catalogue, v 1.0, contains 427,071 sources at 65, 90, 140, 160 m (Yamamura et al 2010)

AKARI-IRC All-sky Bright Source Catalogue, v 1.0, contains 844,649 sources at 9 m, 194,551 sources at 18 m (Ishihara et al 2010)

also carried out deep surveys at the ecliptic poles (eg Goto et al 2010, 2011)


WISEWISE, launched 2009, carried out all-sky survey at 3.4, 4.6, 12 and 22 m, 5 sensitivities 0.08, 0.11, 1 and 6 mJy.(Wright et al 2010)

Source Catalog (2013) lists 563 million objects


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


Far infrared and submillimetre source-count models

Franceschini et al, 2001, AA 378, 1Rowan-Robinson et al, 2001, Elbaz et al, 2002, AA 384, 848Lagache et al, 2004, ApJS 154, 112Gruppioni et al, 2005, ApJ 318, 9(review Lagache, Puget, Dole, 2005, ARAA 43, 727)Rowan-Robinson, 2009,Valiante et al, 2009,Le Borgne et al, 2009,Franceschini et al, 2010,Gruppioni et al, 2010,Lacey et al, 2010,Marsden et al 2011,Rahmati & van der Werf, 2011Niemi et al, 2012,Bethermin et al, 2012,


MODELS FOR COUNTS AND BACKGROUND FROM OPTICAL TO SUBMM

(Rowan-Robinson 2001, ApJ, 549, 745,2009 MN)

* 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


PARAMETERIZED MODEL FOR STAR FORMATION HISTORY* assumed star formation history:

sfr = *(t)/ *(to) = exp Q1 - t/to . (t/to) P

meaning of parameters: t0/Q =sf (cf Bruzual,Charlot 1993) peak sfr when t/to = 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[log10(1+L/L*)/]2

(Saunders et al 1990)* assume luminosity evolution with L*(t)/L*(to) = *(t)/ *(to)

* for each P,Q, parameters L*(to) and are solved for from PSCz data (15000 IRAS galaxies with known z, S(60)≥ 0.6 Jy)


parameterized star-formation history

sfr = *(t)/ *(to) =

exp Q1 - t/to . (t/to) P

meaning of parameters: t0/Q =sf

peak sfr when t/to = P/Q, or t = P sf


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 12-25-60-100-850 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 chi2) values of P,Q:

Ωo P Q

0.3 0.7 3.0 9.0

• best-fitting models then used to predict counts and background spectrum at 0.1 - 1250 m


Infrared

templates


colour-colour, colour-luminosity

(Rowan-Robinson 2001)


Luminosity

function at 850

m


Luminosity

function at 60 m


Luminosity

function at 12 m


Redshift distributions850 m

175 m

60 m 0.44 m


Star-formatio

n history

(Rowan-Robinson 2003b)

far ir and submm source-counts

• new model for ir counts (developed from RR 2001 models): independent evolution for each component, evolution has to flatten off at z < 0.5, allow max. z cutoff (RR, 2009)

M82

cirrusAGN dust tori


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counts at 70-1100 m, ir background

new SWIRE 70, 160,SHADES 850,COSMOS,AZTEC1100 m differentialcounts (Afonso-Luis et

al,2009, Coppins et al

2009,Austermann et al2008,2009) models RR 2009

May 19-22, 2014


Bethermin et al (2012) counts modelDependence of key parameters on redshift

Evolution of

adopted templateswith

redshift


Bethermin et al (2012) counts model


the interpretation of the extragalactic

background

the integrated extragalactic background spectrum is a weighted integral of the star-formation history

I = c ∫oto (t) LZ (t) dt

weighting is by K-correction LZ /L

so submm weighted to higher redshift than far and mid ir

submm background can give strong limit on high z sfr


Models for

infrared backgrou

ndRowan-Robinson 2001


Models for

infrared backgrou

ndRowan-Robinson 2009

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


Evolution of galaxies- the infrared view

• submillimetre galaxies, window to high redshift ?

• lensing as a route to high redshift

• star formation history

• heavy element formation, evolution of gas and dust

• far ir and submm counts and background

• when was the first infrared light from galaxies ?


submillimetre galaxies• first z > 2 IRAS galaxy (F10214+4723) turned out to be bright at 850 m (R-R et al 1991, 1993)

• negative K-correction at submm wavelengths makes these a window to high redshift (Franceschini et al 1994) • however, observed z-distribution of submm galaxies peaks at z~2-3 (Chapman et al 2005)

• source-count models seem to need z cutoff at ~4 to explain 850 and 1100 m counts (R-R 2009)


gravitational lensing• Blain (1996) emphasized lensing could be a big factor in explaining luminosities of submillimetre galaxies

• significant fraction of IRAS hyperluminous infrared galaxies are lensed (R-R and Wang 2010 estimate lensed percentage 10-30%)

• Negrello et al (2010) show 5 lensed galaxies from the Herschel-Atlas survey, predict more than 100 will be found

• need to see more systematic use of lenses to survey high-z universe. So far not finding large numbers of z > 4 infrared galaxies.

Herschel-ATLAS: lensed galaxies

N

E80’’

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Significant fraction (50%?) of bright (>100mJy) 500 m sources are lenses(Negrello et al 2010)

z=2.958 lensed Hermes galaxy

N

E80’’

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Spectrum using CSO ZSPEC, Scott et al 2011May 19-22, 2014


Star formation history• Madau (1996) used Lilley et al survey and HDF to estimate sfr(z)

• R-R et al (1997) used ISO data to derive much higher sf rates to z=1 (uv-opt need dust correction)

• need to correct far ir for heating by evolved stars (Bell 2003, R-R 2003). With this correction, far ir luminosity is a good estimator for obscured star formation rate

compilation based on uv, H, far ir (Hopkins 2007)

May 19-22, 2014

Variation of average AV with z Observed points are

from study of photometric redshifts in HDF. Curves are closed box galaxy models with constant yield, instantaneous recycling, star-formation history consistent with observed history, and in which all heavy elements are assumed to be in dust.(Rowan-Robinson 2003)

<AV>0.30.20.10

z=0 1 2 3 4 5

similar result from SWIRE(R-R et al 2008)

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When was the first (rest-frame) infrared

light ?• Reionization appears to have taken place between z =11 and z = 6. First stars at z~30 ? First galaxies at z~10? First quasars at z~10? (and which came first?)

• How long did it take to get AV>1 (and hence most starlight being reprocessed in the infrared) in star-forming clouds ? If supernovae make enough dust, need 106 years, if need AGB stars, then need 109 years. [1 Gyr from z=10 would be z=4]

• can learn a lot from dwarf galaxies, with metallicity extending down to 1/30th solar. Halo of our Galaxy has stars with very low metallicity, which could be from z>10 era.

may 19-22, 2014bologna pg course infrared and submillimetre surveys, models for counts and...

Documents

wang et

serjeant et

webb et

cowie et

clements et

surveydole et

mmoliver et

madau et