WISH Canada Marcin Sawicki with contributions from Michael Balogh Pauline Barmby Scott Chapman Jon Willis Howard Yee - Canadian Science Interests -

CFHT Gemini (x2) JCMT CCAT ngCFHT TMT 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 WISH JWST: high-z galaxy hunter NIRCAM NIRSPEC NIRISS but 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 Abraham Davidge Ellison McConnachie Pritchet Scott Willott Ferrarese Yee Sawicki Barmby Chapman Doyon Balogh Parker WISH Canada Webb Willis Kavelaars Abraham Davidge Ellison McConnachie Pritchet Scott Willott Ferrarese Yee Sawicki Barmby Chapman Doyon Balogh Webb Parker WISH 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) Pauline Barmby

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 Pauline Barmby

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 Howard Yee

Finding high-z clusters: Cluster survey methods: 1. Optical/IR 2. Sunyeav-Zeldovich effect 3. 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. Howard Yee

The SBS (Stellar Bump Sequence) Method: Muzzin, Wilson, Demarco, Lidman, Nantais, Hoekstra, Yee & Rettura, 2013, ApJ, 767; arXiv: ) 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] color forms an increasingly red (observed) color sequence from the 1.6μm feature between z~0.8 and 1.7 Howard Yee

z-band z phot = 1.25 IRAC 3.6 SpARCS ` VLT FORS2 spectroscopy (2 masks, 3.75hrs integration each); 56 high-confidence redshifts, 12 (members) with 1.62<z<1.64 Howard Yee

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 deg 2 Surface density is of order 2 deg -2 (e.g M solar 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

Science highlights: a z phot =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 mass Low gas mass Collapsing structures? 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<10 10 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) Michael Balogh

WISH and the 1<z<3 Universe WISH will allow stellar mass measurements of quiescent galaxies with M>10 9, and star-forming galaxies with M>10 8. – 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 Michael Balogh

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. Michael Balogh

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 10 sun Marcin Sawicki

classic BzK Daddi et al 2004 z=2 z=5 Marcin Sawicki

E(B-V)=0 E(B-V)=0.3 E(B-V)=0.6 1Gyr 0.2Gyr “BzK” at z=4~5: 0.7Gyr Marcin Sawicki Note: W0=28AB means we need W5=26AB WISH and the z~4-5 Universe

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

12/01/13 WISH and CCAT (Scott Chapman, on behalf of CCAT team) High Redshift Galaxy Evolution with CCAT Scott Chapman

25 WISH and CCAT The integrated star formation: – Rises at z>3 – Peaks at z~1-3 – Declines at z<1 Hopkins et al Log Density of Star Formation log(Redshift) Scott Chapman

26 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 Scott Chapman

27 WISH and CCAT CCAT will survey >100 deg 2 at 350, 450, 850um Designed for large surveys and large statistical samples ALMA = Keck/TMT CCAT = WISH/LSST/DES/SDSS WISH will sample around 4000A at z~5, => measure stellar masses etc. of these objects Scott Chapman 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