WISH Canada

Marcin Sawicki

with contributions fromMichael Balogh Pauline Barmby Scott Chapman Jon WillisHoward Yee

- Canadian Science Interests -

CFHTGemini (x2)JCMT

CCAT

ngCFHTTMT

JWST

ALMA

Canadian context~150 PhD-level

astronomers

TFI/NIRISS: built by ComDev Ottawa for CSA,delivered to GSFC (summer 2013) for testing & integration

JWST: complement to WISHJWST: high-z galaxy hunter

NIRCAMNIRSPECNIRISSbut small FOV => v. faint, more numerous sources

WISH Flip-type Wide-field Filter Exchange System

Current concept from

the WISH study team

Toru’s WISH:

Canadians WISH for+ luminous First Light sources (of

course!)+ Dark Energy (CFHTLS heritage)

...but also... + galaxy evolution out to z~5+ galaxy clusters out to z~2+ stellar populations in nearby galaxies+ Solar System objects

Willis

Kavelaars

AbrahamDavidge

Ellison

McConnachie

Pritchet

ScottWillottFerrarese

Yee

Sawicki

Barmby Chapman

Doyon

BaloghParker

WISH CanadaWISH Canada

Webb

Willis

Kavelaars

AbrahamDavidge

Ellison

McConnachie

Pritchet

ScottWillottFerrarese

Yee

Sawicki

Barmby Chapman

Doyon

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Parker

WISH CanadaWISH Canada

Solar system objects(see JJ Kavelaars’s talk on Tuesday)

WISH for Galactic star clusters

• metal-rich bulge globulars• young massive clusters• mass loss on the AGB and RGB

Omega Cen: 30 arcmin Spitzer IRAC/MIPS (Boyer)

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WISH for nearby galaxies

• Individual mass-losing stars• Integrated stellar mass profiles• Extinction law • Rare, short-lived evolutionary phases (eg TP-AGB)

M33: 2MASS J-band (Jarrett) with WISH FOV

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Why do we want to find high-z galaxy clusters?

1. Growth of structures: the measurement of cosmological parameters. - independent of the geometric methods such as SNe distance, CMB, BAO - One of the very few ways to test GR at very large scale.2. Galaxy evolution, cluster formation: effects of environment, large scale structure

These scientific goals require: large samples and high redshift

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Finding high-z clusters:

Cluster survey methods:

1. Optical/IR2. Sunyeav-Zeldovich effect3. X-ray

cost:10$-$$

10$$ (rich clusters)10$$$

10$$$) (limited to z<~0.8)(4. Weak gravitational lensing

For finding relatively low-mass clusters at high-z, multi-band opt/IR imaging proves to be the most efficient.

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The SBS (Stellar Bump Sequence) Method:

Muzzin, Wilson, Demarco, Lidman, Nantais, Hoekstra, Yee & Rettura, 2013, ApJ, 767; arXiv:1301.5905)

The 1.6um peak (produced by the minimum in H-- opacity in spectra of cool stars was first tested as a feature useful for photo-z by Sawicki (2002, AJ)

The [3.6μm-4.5μm] colorforms an increasingly red (observed) color sequence from the 1.6μm feature between z~0.8 and 1.7

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z-bandz-band

zphot = 1.25zphot = 1.25

IRAC 3.6IRAC 3.6

SpARCS 163435+402151`SpARCS 163435+402151`

VLT FORS2 spectroscopy (2 masks, 3.75hrs integration each); 56 high-confidence redshifts, 12 (members) with 1.62<z<1.64

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A multi-wavelength view of distant, massive galaxy clusters• Current surveys of massive galaxy clusters extend to z=2

• Driven by optical-IR, X-ray or SZ observations over ~100 deg2

• Surface density is of order 2 deg-2 (e.g. 1014 Msolar at z>0.8)

• WISH wide and deep surveys will generate competitive samples

• However, exploiting overlap with X-ray and SZ surveys enable key science:

• z > 1.5 represents a key period where such structures are collapsing and attaining virial equilibrium

• optical-IR searches + photo-z will detect clusters - but a lot of filaments, LSS and projections as well

• X-ray plus SZ turns this into an opportunity: we can identify virial and non-virial structures and follow the impact of virialisation on baryons

• Important baryon physics: BCG growth, central activity and satellite quenching are imprinted upon the galaxy stellar populations and hot gas

Jon

Willis

Jon

Willis

Science highlights: a zphot=1.9

X-ray (white), SZ (cyan), photo-z selected galaxies

(green)

Distant (z>0.8) clusters on the X-ray vs IRAC luminosity plane: X-ray selected (blue squares), IRAC selected + X-

ray detected (black squares), IRAC selected + X-ray faint (red upper limits).

High stellar massLow gas mass

Collapsing structures?

Jon

Willis

Jon

Willis

Galaxy Evolution at 1<z<3

• Current surveys barely “resolve” the peak in galaxy formation efficiency at 1<z<3

• Evolution of galaxies with M<1010 is largely unconstrained.

Environment:• At low redshift, the influence of

environment is most apparent in low-mass galaxies. It is largely unknown what happens at z>1, where dynamical times are much shorter, galaxies are more gas-rich, etc.

Morphology and Black Holes:• AGN activity peaks at 1<z<3. Is this

associated with bulge growth?

Muzzin et al. (2013)

Behroozi et al. (2013)

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WISH and the 1<z<3 Universe

•WISH will allow stellar mass measurements of quiescent galaxies with M>109, and star-forming galaxies with M>108.–Requires deep optical imaging as well. HSC and LSST

deep fields would match well.–Morphologies of somewhat brighter galaxies will

enable tracking the mass growth of bulges and disks.• Identification and characterization of low-mass

galaxies will provide great targets for follow-up with TMT, ALMA

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WISH and environment• eROSITA will find a few hundred clusters at 1<z<1.5, and a

handful at higher redshift. Targeting these would be very valuable.• Other methods for identifying high-z protoclusters (e.g.

using massive radio galaxies) will provide a handful of targets.• Photometric selection may be possible, though lack of a

prominent red sequence may be a hindrance.• These ideas should be developed more: low-mass

galaxies in protocluster environments would be very interesting.

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WISH and the z~4-5 Universe

Muzzin et al. (2013)

Ilbert et al. (2013)Quiescent galaxies at z~5:• Universe only 1.2Gyr old at z=5• z=5 quiescent galaxies are fossils of z=10+ SF’ing galaxies• observable to M~10 M with WISH (W5=26AB) • ~1-100/sq deg/mag ?? Need ~100 sq deg

10sun

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classic BzKDaddi et al 2004

BzK @ z=2WISH @ z=5

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E(B-V)=0

E(B-V)=0.3

E(B-V)=0.6

1Gyr0.2Gyr

“BzK” at z=4~5:

0.7Gyr

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Note: W0=28AB means we need W5=26AB

WISH and the z~4-5 Universe

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For high-z quiescents, shallower but wider W5 would be better:100 deg to W5=26 AB

For high-z quiescents, shallower but wider W5 would be better:100 deg to W5=26 ABFor z=4-5 quiescents, red filters (W5, W4) are essential. They can be 2 mags shallower than bluer filters.

For z=4-5 quiescents, red filters (W5, W4) are essential. They can be 2 mags shallower than bluer filters.

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12/01/13

WISH and CCAT

(Scott Chapman, on behalf of CCAT team)

High Redshift Galaxy Evolution with CCATSc

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WISH and CCAT• The integrated star

formation:

– Rises at z>3– Peaks at z~1-3– Declines at z<1

Hopkins et al. 2007

Log

Den

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of S

tar F

orm

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log(Redshift)

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WISH and CCAT

• The majority of dust appears to form at 3<z<6• We currently have

few constraints on how it forms• We need CCAT to

measure it

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WISH and CCAT

• CCAT will survey >100 deg2 at 350, 450, 850um • Designed for large

surveys and large statistical samples

ALMA = Keck/TMTCCAT = WISH/LSST/DES/SDSS

• WISH will sample around 4000A at z~5, => measure stellar masses etc. of these objects

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4000A

WISH

In summary•Strong interest in Canada spanning a

range of science

•WISH highly complementary to other Canadian projects (JWST, TMT, ngCFHT, CCAT)

•Capability and interest in Canada to work on the Filter Exchange Unit (ComDev, UdeM)

•Canadian Space Agency does not have a regular proposal framework, so we are working on them to secure support for WISH-Canada