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Wide-field Surveys with Subaru

Wide-field Surveys with Subaru. Toru Yamada. - A Review of Subaru Wide-Field and Deep Surveys + some prospects for HSC/ WFMOS era - Introduction to the two very wide-field deep survey with Subaru SCDXT, SSA22-NB surveys. MOIRCS 4’x7’.

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Wide-field Surveys with Subaru

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  1. Wide-field Surveys with Subaru Toru Yamada

  2. - A Review of Subaru Wide-Field and Deep Surveys + some prospects for HSC/ WFMOS era - Introduction to the two very wide-field deep survey with Subaru SCDXT, SSA22-NB surveys

  3. MOIRCS 4’x7’

  4. Distribution of Distant Red Galaxies (J-K>2.3) near HDF 7 arcmin Subru MOIRCS Kajisawa et al. 2006

  5. Previous wide-field observations with Suprime Cam These are not all the surveys by Subaru

  6. c.f., comoving volume sampled by Suprime Cam NB filters

  7. Previous wide-field observations with Subaru

  8. SDF (deepest) - Unveiling the Re-Ionization Era Subaru Deep Field NB980 34’ (north, difficult to observe from ALMA) Kodaira et al. 2003, Taniguchi et al. 2004, Kashikawa et al. 2005 Iye et al. 2006 (for the z=6.96 object), Ota et al. 2007 submitted

  9. SDF The deepest search for the highest-redshift objects SXDS Tracing Structure Formation and Galaxy Formation/Evolution

  10. Iye et al. 2006

  11. Witnessing the Re-ionization of the Universe? Kashikawa et al. 2006 Haiman 2002

  12. Observing Cosmic Reionization by (the clustering of) Lyα Emitters average neutral fraction SDF z=6.6 McQuinn et al. 2007

  13. There are also studies about continuum selected objects • Lyman Break Galaxies at z=3-7 • luminosity function and star-formation history • clustering •  Ouchi et al., Yoshida et al., Shimasaku et al., • Iwata et al. (GOODS) • z~2 (BzK) galaxies • Motohara et al., Kong et al. • (EIS) Yoshida et al. 2006

  14. Previous wide-field observations with Subaru These are not all the surveys by Subaru * TY (at least partially) involved or leading

  15. UKIDSS UDS K<23 (Vega) Panoramic Deep Image: Subaru/XMM Deep Survey Galaxy evolution can be studied in fairly large volume. 1.3° NIR (UKIDSS UDS), MIR-FIR (SWIRE), radio (VLA), sub-mm (SHADES), etc.

  16. SDF The deepest search for the highest-redshift objects SXDS Tracing Structure Formation and Galaxy Formation/Evolution

  17. MDH~1012Mo Large-scale clustering Small scale clustering Distribution of Galaxies in SXDS (1) B-drop LBGs (i<27) mass Ouchi et al. 2005

  18. ＳＤＳＳ Red galaxies z=0 SDSS Morphological E/S0 (Nakamura et al.) Passive Evolution zf=3 and 5 Distribution of Galaxies in SXDS (2) Yamada et al. 2005

  19. Connecting Different Type of Galaxies at different epoch by their clustering properties

  20. UKIDSS-UDS + SXDS: K-band LF evolution up to z~2 Cirasuolo et al. 2007 K_AB<22.5 22000 sources (0.6 deg^2) Number density evolution of red and blue bright objects

  21. COSMOS – Subaru provides the ground-base multi-band data Massey et al. 2006 Taniguchi et al. 2007 COSMOS-21 (Taniguchi+) Broad-Band Intermediate-Band Narrow-band

  22. Narrow-band Surveys at SDF, SXDS, COSMOS, SSA22….

  23. z=3 simulation at larger scale (Benson et al. 2001) 141 h-1 Mpc N-body + semi-analytic treatment B&W :CDMColord: Galaxies

  24. Large-Scale Structure of Lyman Alpha Emitters (1) z=4.9 z=4.79 z=4.86 Shimasaku et al. 2003, 2004

  25. Large-Scale Structure of Lyman Alpha Emitters (2) z=5.7 z=5.7±0.05 Clump ‘A’ Δv~ 180 km/s M~1x1013Msun Ouchi et al. 2005, ApJ, 620, L1

  26. HDR LAB2 LAB1 Large-Scale Structure of Lyman Alpha Emitters (3) z=3.1 Subaru Narrow-Band Observation of the SSA22 Proto-cluster (z=3.1) region Lyα Emitters (LA) • 2 x 10-17erg/s/cm2 • EWobs> 160 Å • 283 objects Lyα Absorbers Hayashino et al. 2004 LAE average local density Steidel et al. 2000

  27. Some Prospects for HSC / WFMOS era Hyper Suprime Cam: ~2 deg2 [8 x FoV of Scam] (Miyazaki-san’s talk) • Precision Cosmology favors 1000-10000 deg2 surveys • (other many talks in this WS…) • Broad-Band Imaging (photo-z) + • Spectroscopy (z~1, z~3) • Galaxy Deep Surveys • deepest ~ 10 deg2 • wide and deep ~ 100 deg2 especially for NB survey • Broad-Band, Narrow-Band, maybe Intermediate Band • Deep Opt & IR Spectroscopy for the selected objects

  28. What’re the Desirable “Deep” Survey Strategies for HSC ? “Deepest (= highest-z) Survey” Strategy • Primary Goals: • Obtain “Comprehensive” View of the Re-ionization Era • Synergy with • ALMA (NAOJ) • Thirty-Meter Telescope (Subaru/NAOJ ?) • James-Webb Space Telescope • ground-base deepest NIR (VISTA/WFCAM/Subaru??) • space NIR Very Wide Field Imager

  29. What’re the Desirable “Deep” Survey Strategies for HSC ? y HSC i-drop z~6 galaxies z-drop z~7 galaxies HSC+NIR optical-drop z > 8 Ouchi 2005

  30. Re-Ionization Era and Earliest Galaxies Important Questions (reionization) ●　When and How Cosmic Re-ionization Occurred ? LAE luminosity-dependent number-density evolution evolution of luminosity-dependent clustering ●　What are the source of ionization ? UV-selected objects (LBG) luminosity function, color But the knowledge of escape fraction below Lyman Limit is essential ●　How reionization affects galaxy formation?

  31. Re-Ionization Era and Earliest Galaxies Important Questions (galaxy formation) ●　How galaxy formation proceeds at z=5-10? ALMA .. Dust emission (for brightest objects 100M/yr)) High-J CO? (z~6 maybe detectable z~10 difficult) IR-bright objects near UV-selected sources? TMT/JWST .. redshift identification (relatively rare bright objects AB~25-26) stellar contents metal lines: metallicity, excitation, kinematics AGN signatures ●　Search for galaxies at z=7-10 (z-drop, y-drop) JWST: wide-field NIR imaging survey? ground-based IR camera : brightest galaxies

  32. Thirty Meter Telescope (Caltech / UC / Canada)

  33. Previous wide-field observations with Subaru Suprime Cam These are not all the surveys by Subaru * TY involved

  34. Two Subaru Very Wide Field Deep Surveys • SCDXT: Suprime Cam/ UKIDSS Deep eXtragalactic Survey (DXS) • Ten Square DegreesSurvey • - search for clusters and proto-clusters at z=1-2 • (working report) • - A Proto-cluster at z=3.1 and Galaxy Formation • Subaru (Suprime Cam, FOCAS, MOIRCS) / Spitzer / • / VLT (VIMOS) / JCMT-SCUBA / XMM / UKIDSS / Chandra

  35. Suprime-Cam/UKIDSS DXS 10 aq.deg. Survey I’~26 UKIDSS DXS J~22 K~21 SWIRE IRAC/MIPS

  36. SCDXT: Field of View Lockman Field and ELAIS N1 Lockman Hole ELAIS N1 2300000 sources down to I’~26 (AB: 25.5 – 26.0 @ ~90% completeness)

  37. I’-band – IRAC [3.6][4.5] Two-Color Diagram [3.6] < 20.5 sample Redshifted Coma-elliptical passive mdels Z=2.0 Z=1.0 24um>0.45mJy Model grid: Bruzual and Charlot z=0-3, Age 0-Tuniv, E(B-V)=0

  38. Cluster Finding Distribution of galaxies is converted to the density map by smoothing with various kernels. (e.g., Gaussian FWHM=45”) Peak finding with the criteria matched with the smoothed scale. Optical/NIR MOS spectroscopic follow-up Being proposed MOIRCS / FMOS ELAIS N1 1.0 < z < 1.2 1.2 < z < 1.4 Lockman hole 1.4 < z < 1.8 1.4 < z < 1.8 1.2 < z < 1.4 1.0 < z < 1.2

  39. HDR LAB2 LAB1 A Proto-clusrter around SSA22 field az=3.1 (Steidel et al. 1998) 25”=190kpc Steidel et al. 2000 LAE average local density Hayashino et al. 2004 Matsuda et al. 2004 Subaru Scam NB 7h LAB2 LAB1

  40. New Very Wide-Field Lyα Emitters Survey at ‘SSA22’ area • 2 x 10-17erg/s/cm2 • EWobs> 120 Å Lyα Emitters w/ Hayashino, Matsuda, Nakamura, et al.

  41. Estimation of the Large-Scale Over-density Control fields SDF, SXDS, (GOODS-N) Vs.CDM linear theory Millenium Simulation Over-density distribution of SF galaxies Vs. False LAE in Millenium Simulation

  42. Lyα Emission Equivalent Width and IMF Constant continuous SF history １／２０solar metallicity Model A Salpeter IMF x=2.35 Model B Top heavy IMF x=0.5 Ml=1 Msun Mu=120 Msun ~240Å EW0 > 240 Å POPIII ? If constant continuous SFH Malhotra et sl. 2002; Charlot and Fall 1993

  43. Summary Previous Subaru Wide-Area Surveys ★ The deepest search for the highest-redshift objects ~ 0.25 deg2 (1 Scam FoV) SDF, others.. ★ Tracing Structure Formation and Galaxy Formation/Evolution ~ 1 deg2 (4 Scam FoV) SXDS, COSMOS, others.. ★　~ 10 deg2 limited band/depth coverage Future Prospects w/HSC Precision Cosmology favors 1000 deg2 surveys Galaxy Deep Surveys deepest ~ 10 deg2 wide and deep ~ 100 deg2 especially for NB survey

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