Dusty Galaxies: PFS key-sciences withHerschel-ATLAS galaxies
PFS Science Workshop
9-10 December, 2010 @ NAOJ
Hideo Matsuhara (ISAS, JAXA)
Tomotsugu Goto (NAOJ/IfA), Toshi Takagi, (ISAS)
Steve Serjeant (Open Univ.),
Matt Malkan (UCLA)

List of my talk
• Background– Violent Epoch of the Universe– Importance of Far-IR• Overview of Herschel ATLAS• Key sciences– The obscured cosmic star-formation history (CSFH) andits environment-dependence– The link between black hole accretion and stellar massassembly– Discovery of Overwhelmingly Luminous IR Galaxies– Redshift determination of a large sample of strong
gravitational lenses• Proposed Survey & requirements– Survey Plan
– Instrument Requirements• Synergy with SPICA

The `Violent Epoch’Ueda et al. (2003)• Universe at z=1~2:
evolution of both galaxies
and AGN peaks• decelerating expansion toaccelerating expansion due to thedark energy• More Intense Starburst, themore deeply embedded in thedust• AGN are heaviliy obscured
at their youngest, Compton
thick age

Hopkins & Beacom (2006)

Advantage of AKARI :contiguous coveragein Mid-IR• 70cm, <6K telescope
launched in 2006
• All-Sky Survey– 9, 18, 65, 90, 140 160µm– ~1 million point-source
catalog now released• Pointing Deep Survey– NEP deep Field– ADF-SNEP-Deep

S-cam field

AKARI/IRC 2,3,4µm colour image

AKARI

SED diagnostics of AGN/
Starburst

Red AGN,no PAH

PAH

Broad, Continuous
wavelength coverage isessential!

6IR Luminosity Density
Evolution with AKARI• Strong
evolution
seen esp.
in ULIRGs

CSFH obscured by Dust:
Weakness of Spitzer & AKARI• Extrapolate the MIR luminosity to the total
IR (bolometric) luminosity– Relatively hot dust seen at MIR – so dusty
AGN can contribute– Self-absorption by dust is not negligible inMIR, hence spatial structure affects the SED• Far-IR & Submm wavelengths– trace relatively cold dust, good Star-formation
indicator– BUT, at far-IR, <1m telescope cannot go
beyond z~1

Herschel launched !!!
14 May 2009
 Deep FIR imaging : 3.5m aperture : confusion limit substantiallyimproved (and already reached there! )Credit: ESA

Herschel - ATLAS key project

Astrophysical Terahertz Large Area SurveyEales et al. (2010)• Total 550 deg2 OTKP on Herschel– 110, 170µm (PACS) 250, 350, 500µm (SPIRE)– 18” resolution @ 250 µm

10ATLAS Science Demonstration
Phase (SDP) data
released to public• a field roughly 4 x 4 degrees centred on 9hrs
5mins, +0deg 30mins (see marked out region).
• 6576 galaxies

SDSS Optical Identifications

Black : 250µm
Red: 500µm• Only 36% (23%) at 250(500) µm sample
are identified by SDSS

KEY SCIENCES

The Obscured CSFH & its
environmental dependence(1)• CSFH z<1 from H-ATLAS galaxies withPFS follow-up– Thorough wavelength coverage for the cold
dust emission  accurate total IR luminosity– Best possible direct measurement of dustshrouded star-formation rates by tracing thereprocessed emission from young massivestars.

• Extremely Large area survey (~100deg2)
at z=0.5-1 is sufficient to be free from theCosmic Variance

The Obscured CSFH & its
environmental dependence(2)• Environmental dependence– Star-forming galaxies avoid richer environments in thelocal Universe, but this relation is reversed at z~1(Elbaz et al. 2007)• ~60 (Abell class 1 orgreater) clusters
enable to test hisrelationship at z<1.

MIR fraction

MIR galaxies prefer cluster outskirts, but avoid cluster centre

AKARI

log (density)
Koyamaet al. (2008)

Angular correlation function
on large scales• Large-scale
structure of thestar-forming
galaxies up to~1000Mpc
scale at z~1• Monte Carlosimulation topredict theangularcorrelation
function

Eales et al, 2010;
van Kampen et al. 2005)

The Link between Black HoleAccretion and Stellar MassAssembly• Indication of AGN feedback (energy input)
to host galaxies regulating star-formation– Close relationship between Black Hole growthand stellar mass assembly– AGN contribution to bolometric luminosity
increases for higher luminosity starbursts• Measure star-formation rates in the QSO
host galaxies– ~60,000 AGN candidates in ATLAS NGP field– Pioneering work (Serjeant et al. 2010) byusing the stacking analysis of SDP Herschelimages

CSFH of Quasar HostGalaxies(Serjeant et al. 2010)-22>IAB>-24-26>IAB>-28-28>IAB• Very strong
evolution
rate at highluminosities

Gravitational Lensing

Bright SDP sources are lensamplified !!

ID 81 blind z=3.04
determination with Z-Specby using 12CO ladder
Followed by PdB & GBT

Z-Spec/ CSO, Mauna Kea

Submm Bright source Survey is
Quite Efficient Way for Selecting
Gravitational Lenses• Once ATLAS
Completed,~3000 strongly
lensed sources
are predictedSubaru/PFS
Baseline Survey Plan
• Main sample– ATLAS-NGP field （150deg2, 22,000 galaxies withrAB < 22.4 mag (~1/3 of all Hershel galaxies)– z=0.3-0.5? (Dye et al. 2010)– ~20 nights assuming 5 FoV (1.5deg2) can beobserved per night– So far GAMA survey is rAB < 19.8 mag  GAMAfield may be inclluded• Secondary Sample– Fainter sample (rAB < 24 mag) of entire ATLAS(NGP & GAMA) fields– z~1? Probably 70,000 galaxies @ ~300deg2

Subaru/PFS
Instrument Requirements• Field-of-View– To survey the entire main sample field in reasonable
observing time, 1.5 deg2 or larger is preferable• Number of fibers– > 500 fibres per deg2 (surface density of ATLASsources)• Throughput– the sensitivity is key issue– The degraded throughput (10%) of PFS leads to lose
the advantage over Keck/DEIMOS (~40%, >200 slits) in
the survey speed• Wavelength coverage– Baseline (3900-10800A) is sufficient for z=0.3-0.5
sample– Longer extension (upto 1.3 µm) is preferable to observe[O III] @z=1

SYNERGY WITH SPICASPICA Mission Overview
 Specifications
 Telescope: 3m-class, 6 K
 Superb spatial resolution withexcellent sensitivity

 Core wavelength: 5-210 µm
 Orbit: Sun-Earth L2 Halo
 Mission Life

3 years (nominal)
 5 years (goal) Weight: 3.7 t
 Launch: FY2018 (proposed)with H-IIA-204 (5S fairing) launch schedule under discussion

 Heritage
IRAS, ISO, AKARI, HerschelWith Cooled telescope Mission！

Background will be 1 million times smaller than the warm
(passively cooled ) telescope !!
28

Diagnostics of Violent Epoch withmuch better mid & far-IR spectralline sensitivity !!

29

Synergy with SPICA• Very deep & fast imaging survey at20-210µm– More than 100deg2 @ 100µm is possible• Very deep mid- far-IR study of dustobscured galaxies– Complementary to optical diagnostics withPFS• Aimed Launch of SPICA : FY2018– Close to the commission of PFS• SPICA is a Japanese-led Mission– Strategic plan with Subaru/HSC & PFS !!

SPiCA-Science Work Shop-

2010.12.16(木)~17(金)@国立天文台 三鷹 大セミナー室(すばる棟)
問合せ：spica̲ws@ir.isas.jaxa.jp
詳しくはSPICAWebページをご覧下さい。
http://www.ir.isas.jaxa.jp/SPICA/SPICA̲HP/index.html

BACKUP SLIDESThe NEP Survey - footprints
NEP-Wide
CFHT/Mega-prime cam
NEP-DeepSubaru/Suprime-cam
1 deg

2007.12.1
4

Panoramic Views of Galaxy Formationand Evolution