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WISH Canada

WISH Canada . - Canadian Science Interests -. Marcin Sawicki with contributions from Michael Balogh Pauline Barmby Scott Chapman Jon Willis Howard Yee. Canadian context. CCAT. ~150 PhD-level astronomers. JWST. ALMA. TMT. CFHT. Gemini (x2). JCMT. ngCFHT.

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WISH Canada

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

  2. Canadian context CCAT ~150 PhD-level astronomers JWST ALMA TMT CFHT Gemini (x2) JCMT ngCFHT

  3. JWST: complement to WISH JWST: high-z galaxy hunter NIRCAM NIRSPEC NIRISS but small FOV => v. faint, more numerous sources TFI/NIRISS: built by ComDev Ottawa for CSA, delivered to GSFC (summer 2013) for testing & integration

  4. WISH Flip-type Wide-field Filter Exchange System Current concept from the WISH study team

  5. Toru’s WISH:

  6. 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

  7. Ferrarese Scott Willott Doyon Abraham Davidge Webb Yee Kavelaars McConnachie Sawicki Willis Ellison Chapman Barmby Parker Pritchet Balogh WISH Canada WISH Canada Ferrarese Scott Willott Doyon Abraham Davidge Webb Yee Kavelaars McConnachie Sawicki Willis Ellison Chapman Barmby Parker Pritchet Balogh

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

  9. WISH for Galactic star clusters Pauline Barmby • metal-rich bulge globulars • young massive clusters • mass loss on the AGB and RGB Omega Cen: 30 arcmin Spitzer IRAC/MIPS (Boyer)

  10. WISH for nearby galaxies Pauline Barmby • 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

  11. These scientific goals require: large samples and high redshift Why do we want to find high-z galaxy clusters? Howard Yee 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

  12. Finding high-z clusters: Howard Yee 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.

  13. 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 The SBS (Stellar Bump Sequence) Method: Howard Yee 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)

  14. VLT FORS2 spectroscopy (2 masks, 3.75hrs integration each); 56 high-confidence redshifts, 12 (members) with 1.62<z<1.64 SpARCS 163435+402151` zphot= 1.25 Howard Yee IRAC 3.6 z-band

  15. A multi-wavelength view of distant, massive galaxy clusters Jon Willis • 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

  16. Jon Willis High stellar mass Low gas mass Collapsing structures? 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).

  17. Galaxy Evolution at 1<z<3 Michael Balogh • 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)

  18. WISH and the 1<z<3 Universe Michael Balogh • 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

  19. WISH and environment Michael Balogh • 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.

  20. WISH and the z~4-5 Universe Marcin Sawicki Muzzin et al. (2013) Ilbert et al. (2013) • Quiescentgalaxies 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

  21. classic BzK Daddi et al 2004 Marcin Sawicki BzK @ z=2 WISH @ z=5

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

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

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

  25. WISH and CCAT Scott Chapman • The integrated star formation: • Rises at z>3 • Peaks at z~1-3 • Declines at z<1 Log Density of Star Formation log(Redshift) Hopkins et al. 2007

  26. WISH and CCAT Scott Chapman • 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

  27. WISH and CCAT Scott Chapman • CCAT will survey • >100 deg2 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 WISH 4000A

  28. 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

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