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

P bi Hi h U i ith GRB Probing High‐z Universe with 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 also, e.g., Jakobsson et al. 2005

GRB @ z=0‐6.3

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

Morphology of GRB hosts

p gy

Morphology of GRB hosts ~exp profile , large irregularity

GRBs

Majority at z = 1‐2

Re

Wainwright et al. 2007 Conselice et al 2005

MB

Conselice et al. 2005

Similar Size‐Luminosity Relation with the general sample? Large concentration at high‐z?

GRB Hosts: Metallicity

Metallicity distribution: scattered ~general Metallicity distribution: scattered, ~general

C ll th h ld Collapser threshold Z~0.3Zsun Erb et al. GRB

GRBs ALS

GRB

Fynbo et al. 2006 Savaglio et al. 2008

also see Chen et al. 2009

GRB Hosts (long burst, w/OA)

• SFR M* UV L

i it Di t ib ti

• SFR, M*, UV Luminosity Distribution

… ~ 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 (Collapser model threshold) … <0.3 Zsun (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 GRB (z=3 03) Av=3 2

Peyley et al. 2009

GRB (z=3.03) Av=3.2

ey ey et a 009

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 rate GRB GRB rate, Normalized to SFR at z=1‐4 LBGs 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 f t l ti f i t frequent population of massive stars.

• GRB seems to be Unbiased Tracers
• GRB seems to be Unbiased Tracers
• f 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/Md

• f a Cluster (F) in M82

Large L/Mdyn of a Cluster (F) in M82

Salpeter (Kroupa) IMF  L/M ~ 7‐12 L /M  L/Mdyn 7‐12 Lsun/Msun (for 60Myr age) Observed 42±10 L /M Observed 42±10 Lsun/Msun

Bastian et al. 2007 M82

Change of Mdyn/L along the time: Cl t Elli ti l F d t l Pl t 0 1 0 8 Cluster Ellipticals Fundamental Plane at z=0.1‐0.8 Fundamental Plane Evolution Changes in M/L I i t t Is more consistent with flat (x=0.3) IMF

Van Dokkum 2008

Δ(U V) ~ A Δ(U‐V) ~ Age, Not depending as much

• n IMF slope as on age

Cosmic SF History and IMF Cosmic SF History and IMF

l f Inconsistent Normalization of Cosmic SFR and Stellar Mass History

Uncertainties: ‐ High‐z Mass Function ‐ IMF ‐ Field‐to‐Field Variance Star Formation Rate 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) GOODS‐N BVIzJHK IRAC ch1‐4 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

ity

Change of IMF needed More contribution by 1.5‐4Msun stars at high‐z

s Densi ar Mas Stella Fardal et al. 2006 Redshift

Large Equivalent Width of Lyα Emitters Lyα Equivalent Width

T h IMF 0 5

Lyα Equivalent Width

~ Lyα Line Luminosity / Adj C i L i i l h

~240Å Top heavy IMF x=0.5

/ Adjacent Continuum Luminosity per wavelength ~ Number of Ionizing Photon / Non‐Ionizing Photon

S l t IMF 2 35

(for Photo Ionization)

Salpeter IMF x=2.35

Shimasaku+06

Constant Continuous SF, 1/20 Zsolar Ml=1 M M =120 M

Shimasaku+06 Z=5.7 LAE

Malhotra et sl. 2002; Charlot and Fall 1993 Ml=1 Msun , Mu=120 Msun

SSA22 z=3.1 LAE Sample

SSA22 General Fields

SXDS

SSA22 z 3.1 LAE Sample

SDF Bl k i t LAE

1391LAEs 589LAEs

Black points: LAEs Green lines: contour of average number density of LAEs Gray Region: masked region to avoid some bright stars

Large Equivalent Width of Lyα Emitters Large Equivalent Width of Lyα Emitters

Nakamura 2010

Shaded area: lower limit

Large Equivalent Width of Lyα Emitters Large Equivalent Width of Lyα Emitters

Including the toal Lyα and UV

Lyα

Lyα and UV

Lyα UV

Nakamura 2010

Very Blue UV Slop of z=7 Galaxies

F ~ λβ

（UV wavelength）

e y ue U S op o Ga a es

Fλ λβ

（UV wavelength） Bluer in Bluer in ◆ higher‐z galaxies ◆ f i t l i ◆ fainter galaxies

β

How to make β ~ ‐3

Very Metal Poor Hot Stars

β

y Large Escape Fraction

Bouwens et al. 2010

M(UV)

High‐z Type‐IIn Super Novae g yp p

k l

More than a few Type‐IIn SNe detected at z~2

Cooke et al. 2009

Epoch 1 Epoch 2

Cooke et al. (2009) argues that The current rate is still consistent with Salpeter like IMF though small statistics

Observed Subtracted

Salpeter‐like IMF, though small statistics

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 / T II SN ‐ GRB / Type‐IIn SNe, tracers of massive stars at intermediate and high redshift

P bi th V E l U i Probing the Very Early Universe:

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 ki G WISH W ki G WISH Working Group WISH Working Group

http://www.wishmission.org/en/index.html

M31 Phot: R.Gendler

WISH WG under JAXA/ISAS Science Committee

d h h k kk ( h k )

R&D On‐Going

Toru Yamada, Chihiro Tkokku (Tohoku University) Ikuru Iwata, S.Tsuneta, k d ( ) T.Morokuma, T.Kodama, Y.Komiyama (NAOJ) H.Matsuhara, T.Wada, Y.Oyabu (JAXA/ISAS) h b ( i i ) K.Ohta, K.Yabe (Kyoto University) M.Doi, N.Yasuda (University of Tokyo) N K i (TiTEC) N.Kawai (TiTEC) A.Inoue (Osaka Sangyo University) YIk d (Ph di ) Y.Ikeda (Photocoding) T.Iwamura (M.R.J)

CG of a 1st –gen galaxy, by Toru Yamada

Cosmic Microwave Background (CMB) Universe: Neutral

WISH

First‐Generation Galaxies Galaxies

Ultimate Frontier

• f Galaxies

Subaru

Universe: Ionized

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

P i Mi Di t

1 5m

WISH Specifications Quick Summary

Primary Mirror Diameter 1.5m Wavelength Coverage 1‐5μm g g

μ

Image Quality achieving diffraction limit to the FoV edge

at 1‐5 μm at 1‐5 μm

Spatial Sampling 0.15”/18μm (optimized at 1.5μm ) Limiting Magnitude ~28 AB/10‐20h ~20nJy (3sigma) Camera Field of View ~１０００acmin2 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 ff l Diffraction limit at 1‐5μm Current Plan Current Plan For the FP Layout

WISH 5 Years Survey Plan y

S A D h N Surveys Area Depth Note Ultra Deep

100 deg2 ~28AB Z~10‐17

Ultra Deep

100 deg2 28AB 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

E pected N mbers Expected Numbers

Number / 1 deg2

Expected Numbers

No Evol.

No Evolution from z=7 extrapolation Semi‐analytic Kobayashi, M.

By Iwata, Yabe for WISH team

y For WISH