P Probing High z Universe with GRB bi Hi h U i ith GRB GRB - PowerPoint PPT Presentation

P Probing High ‐ z Universe with GRB bi Hi h U i ith GRB ● GRB Afterglows as Cosmic Lighthouses  detect highest ‐ z GRBs AG at their brightest phase ● GRB as the tracer of high ‐ z star ‐ formation What are the GRB precursors? p Are GRBs unbiased or biased tracers of SF? How they probe the formation of very massive stars? y p y ● GRB as cosmological standard candle ● GRB as cosmological standard candle

Outline Outline 1. GRB Hosts and High ‐ z Galaxies 2. Massive ‐ star formation at high ‐ redshift Does IMF change? Does IMF change? 3. Probing Star ‐ Formation at z=7 ‐ 20, “That is your WISH, isn’t it?”

GRB Hosts: SFR/Stellar Mass / GRB hosts GRB hosts × galaxies Savaglio et al 2008 Savaglio et al. 2008 GRB @ z=0 ‐ 6.3 also, e.g., Jakobsson et al. 2005

GRB Hosts: UV Luminosity UV Luminosity Distribution of GRB (w/opt. AG) Hosts y ( / p ) (7 hosts detected/15 at z> 2) GRB ~ General Gal General Gal Population Chen et al. 2009

GRB Hosts: Morphology p gy Morphology of GRB hosts Morphology of GRB hosts GRBs ~exp profile , large irregularity Majority at z = 1 ‐ 2 Re M B Wainwright et al. 2007 Conselice et al 2005 Conselice et al. 2005 Similar Size ‐ Luminosity Relation Large concentration at high ‐ z? with the general sample?

GRB Hosts: Metallicity Metallicity distribution: scattered ~general Metallicity distribution: scattered, ~general C ll Collapser threshold th h ld Z~0.3Z sun Erb et al. GRB GRB GRBs ALS Savaglio et al. 2008 Fynbo et al. 2006 also see Chen et al. 2009

GRB Hosts (long burst, w/OA) ● SFR, M*, UV Luminosity Distribution ● SFR M* UV L i it Di t ib ti … ~ Random Galaxy Population e.g., Chen et al. 2009, Savaglio et al. 2008, Wainwright et al. 2007 ● Morphology ● Morphology … similar with the general? larger concentration? e.g., Wainwright et al. 2007 / Concelice et al. 2005 e g Wainwright et al 2007 / Concelice et al 2005 ● ISM Metallicity … <0.3 Z sun (Collapser model threshold) <0 3 Z (Collapser model threshold) but ~ Unbiased Population at z>2 e g Fynbo et al 2006 Price et al 2007 e.g., Fynbo et al.2006, Price et al. 2007

Dust in GRB Line of Sight g Prochaska et al. 2007 Peyley et al. 2009 ey ey et a 009 GRB (z=3 03) Av=3 2 GRB (z=3.03) Av=3.2

GRB as a tracer of high ‐ z star ‐ formation g Unbiased Tracers? GRB rate vs UV SFR Unbiased Tracers? GRB rate vs. UV SFR Cosmic SF History GRB GRB rate GRB rate, Normalized to SFR LBGs at z=1 ‐ 4 Kistler et al. 2008 But see Jakobsson et al. 2005

● GRB Hosts seems ● GRB Hosts seems distributed over the general population ..But this is reasonable if GRBs are certain ‐ type, but frequent population of massive stars. f t l ti f i t ● GRB seems to be Unbiased Tracers ● GRB seems to be Unbiased Tracers of Star Formation?   Massive star formation at High Redshift

Some Evidence of Flat/Top ‐ Heavy IMF / p y In Local and High ‐ z Universe NGC3603

Stella Mass Function in NGC3603 Stella Mass Function in NGC3603 VLT+NACO Harayama et al. 2007 ‐ Stellar mass segregation is observed ‐ yet the IMF for the entire cluster is still flat ‐ yet, the IMF for the entire cluster is still flat x= ‐ 0.74 ( > ‐ 1.35, Salpeter)

Large L/M d Large L/M dyn of a Cluster (F) in M82 of a Cluster (F) in M82 Salpeter (Kroupa) IMF  L/M  L/M dyn 7 ‐ 12 L sun /M sun ~ 7 ‐ 12 L /M (for 60Myr age) Observed 42 ± 10 L Observed 42 ± 10 L sun /M sun /M M82 Bastian et al. 2007

Change of M dyn /L along the time: Cl Cluster Ellipticals Fundamental Plane at z=0.1 ‐ 0.8 t Elli ti l F d t l Pl t 0 1 0 8 Fundamental Plane Evolution Changes in M/L I Is more consistent i t t with flat (x=0.3) IMF Van Dokkum 2008 Δ (U V) ~ A Δ (U ‐ V) ~ Age, Not depending as much on IMF slope as on age

Cosmic SF History and IMF Cosmic SF History and IMF Inconsistent Normalization of l f Cosmic SFR and Stellar Mass History Uncertainties: ‐ High ‐ z Mass Function ‐ IMF Star Formation Rate ‐ Field ‐ to ‐ Field Variance Integration Stellar Mass Density Stellar Mass Density Hopkins and Beacom 2006

MOIRCS Deep Survey (MODS) J, H, Ks, (NB119) Wide K~22.5 (Vega) Deep K~23 6 (Vega) K~23.6 (Vega) BVIzJHK IRAC ch1 ‐ 4 GOODS ‐ N P.I. Takashi Ichikawa

Cosmic SF Rate Density and Stellar ‐ Mass Density Our Results Our Results Kajisawa et al. 2009 MOIRCS Deep Survey

Cosmic SF Rate Density and Stellar ‐ Mass Density Change of IMF needed Change of IMF needed More contribution by 1.5 ‐ 4M sun stars at high ‐ z ity s Densi ar Mas Stella Fardal et al. 2006 Redshift

Large Equivalent Width of Ly α Emitters Ly α Equivalent Width Ly α Equivalent Width ~ Ly α Line Luminosity / Adjacent Continuum Luminosity per wavelength / Adj C i L i i l h Top heavy IMF x=0.5 T h IMF 0 5 ~ Number of Ionizing Photon / Non ‐ Ionizing Photon ~240 Å (for Photo Ionization) S l Salpeter IMF x=2.35 t IMF 2 35 Constant Continuous SF, 1/20 Z solar M l =1 M M l =1 M sun , M u =120 M sun M =120 M Shimasaku+06 Shimasaku+06 Malhotra et sl. 2002; Charlot and Fall 1993 Z=5.7 LAE

SSA22 z=3.1 LAE Sample SSA22 z 3.1 LAE Sample General Fields SSA22 SXDS SDF 1391 LAEs 589 LAEs Bl Black points: LAEs k i t LAE Green lines: contour of average number density of LAEs Gray Region: masked region to avoid some bright stars

Large Equivalent Width of Ly α Emitters Large Equivalent Width of Ly α Emitters Nakamura 2010 Shaded area: lower limit

Large Equivalent Width of Ly α Emitters Large Equivalent Width of Ly α Emitters Including the toal Ly α and UV Ly α and UV Ly α Ly α UV Nakamura 2010

Very Blue UV Slop of z=7 Galaxies e y ue U S op o Ga a es ~ λ β λ β F F λ （ UV wavelength ） （ UV wavelength ） Bluer in Bluer in ◆ higher ‐ z galaxies ◆ f i t ◆ fainter galaxies l i β β How to make β ~ ‐ 3 Very Metal Poor Hot Stars y Large Escape Fraction Bouwens et al. 2010 M(UV)

High ‐ z Type ‐ IIn Super Novae g yp p Cooke et al. 2009 k l More than a few Type ‐ IIn SNe detected at z~2 Epoch 1 Epoch 2 Cooke et al. (2009) argues that The current rate is still consistent with Salpeter like IMF though small statistics Salpeter ‐ like IMF, though small statistics Observed Subtracted

Massive Star Formation at High Redshift Massive Star Formation at High Redshift Evidence suggesting enhanced massive ‐ star formation is being observed formation is being observed. More direct constraints needed ‐ Colors of Very High ‐ z Galaxies Colors of Very High z Galaxies POPII/III stars toward z=20 ‐ GRB / Type ‐ IIn SNe, GRB / T II SN tracers of massive stars at intermediate and high redshift

P Probing the Very Early Universe: bi th V E l U i That is our WISH That is our WISH

WISH WISH Wide-field Imaging Surveyor for High-Redshift Wide field Imaging Surveyor for High Redshift 超広視野初期宇宙探査衛星 超広視野初期宇宙探査衛星 WISH W WISH W WISH Working Group WISH Working Group ki ki G G http://www.wishmission.org/en/index.html M31 Phot: R.Gendler

WISH WG under JAXA/ISAS Science Committee R&D On ‐ Going Toru Yamada, Chihiro Tkokku (Tohoku University) d h h k kk ( h k ) Ikuru Iwata, S.Tsuneta, T.Morokuma, T.Kodama, Y.Komiyama (NAOJ) k d ( ) H.Matsuhara, T.Wada, Y.Oyabu (JAXA/ISAS) K.Ohta, K.Yabe (Kyoto University) h b ( i i ) M.Doi, N.Yasuda (University of Tokyo) N K N.Kawai (TiTEC) i (TiTEC) A.Inoue (Osaka Sangyo University) YIk d (Ph Y.Ikeda (Photocoding) di ) T.Iwamura (M.R.J) CG of a 1 st –gen galaxy, by Toru Yamada

Cosmic Microwave Background (CMB) Universe: Neutral WISH First ‐ Generation Galaxies Galaxies Ultimate Frontier of Galaxies Universe: Ionized Subaru Subaru VLT ………… Hubble Space Telescope Hubble Space Telescope

WISH Science Goals WISH Science Goals [1] Discovery of the First Generation Objects ( galaxies SMBH and GRB) ( galaxies, SMBH, and GRB) and Study Galaxy Form ation at EoR. [2] Study of the expansion history of the universe and properties of dark energy by using type-I a p p gy y g yp supernovae lum inosity at rest-fram e NI R( i-band) w avelength [3] Extensive study of galaxy form ation and evolution utilizing the unique w ide-area NI R observations

WISH Specifications Quick Summary WISH Specifications Quick Summary Primary Mirror Diameter 1.5m 1 5m P i Mi Di t Wavelength Coverage 1 ‐ 5 μ m μ g g Image Quality achieving diffraction limit to the FoV edge at 1 ‐ 5 μ m at 1 ‐ 5 μ m Spatial Sampling 0.15”/18 μ m (optimized at 1.5 μ m ) Limiting Magnitude ~28 AB/10 ‐ 20h ~20nJy (3sigma) Camera Field of View ~ １０００ acmin 2 Orbit SE ‐ L2 Orbit S Launcher Japanese HIIA (fit to the Dual Launch)

WISH Optical Layout and the Focal Plane Layout Three Mirror system, Very FLAT FP Diffraction limit ff l at 1 ‐ 5 μ m Current Plan Current Plan For the FP Layout

WISH 5 Years Survey Plan y S Surveys A Area D Depth h N Note Ultra Deep Ultra Deep 100 deg2 100 deg2 ~28AB 28AB Z~10 ‐ 17 Z 10 17 Multi ‐ band ~10 deg2 ~28 Z~8 ‐ 10 Ultra wide ~1000 deg2 ~25 QSO,WL Extreme ~1 deg2 ~29 ‐ 30 Faint End WISH is the survey dedicated mission Survey speed 2X of JWST w/ φ 0 2” aperture photometry Survey speed 2X of JWST w/ φ =0.2” aperture photometry ½X Point Sources