??????????????? ???FMOS???????????

1
??????????????????FMOS???????????

• ?? ??
• (??????? ???????)
• ?????????????????????
• ??19?5?28-30? ??????

2
Outline

• Gamma-Ray Bursts
• A brief introduction to GRBs
• GRB???????
• ????
• ????
• ????????
• ????????
• FastSound ??(???FMOS???????????)

3
GRB Light Curves
Fishman 94
Meegan 96
Short-hard
Long-soft
Duration two populations
4
Spatial Distribution
Isotropic, but not homogeneous indicating a
cosmological distribution
Euclidean expectation
Meegan 96
Event rate a few / day / all sky for the BATSE
sensitivity
5
Afterglows
GRB970508, first redshit (z0.835)
Metzger 97
GRB970228, first X-ray afterglow by BeppoSAX

• GRB970228, optical afterglow

6
Bright and Extremely Energetic
GRB 990123 Akerlof 99

• GRB 990123 (z1.6)
• Eiso,? 3x1054 erg 2Msunc2
• same GRB detectable out to z20
• Peak optical mag9 from z1.6
• E?,iso 1051-54 erg
• current record GRB 050904
• z6.3
• spectroscopic confirmation by Subaru (Kawai et
  al. 2006)

GRB050904 spectrum Kawai et al 06
7
The Big Picture of long GRBs
Internal shock external shock

• Ultra-relativistic fireball/outflow (G100-1000)
• ????????????????????????????????????????????
• Afterglow relativistic supernova remnants
• (most likely) jet-like explosions
• ????????????
• Isotropic-equivalent energy gt 1054 erg!
• Afterglow light curve break
• E1051 erg (jet corrected)
• Ejecta E/G10-5 Msun

8
Afterglow Theory Well Tested
Sari 98
Panaitescu Kumar 01

• Radiation by synchrotron of accelerated electons
• Power-law flux decay (?t-1 to t-2)
• Power-law spectral energy distribution
• Evidence of jet light curve break
• ?jet G(tbreak) 1

On-axis
Off-axis
Totani Panaitescu 02
9
long GRB SN Connection

• associated with very peculiar type Ic supernovae
  (hypernovae)
• Large explosion energy 1052 erg gtgt 1051 erg
• one of the brightest supernovae with 1 Msun 56Ni
  production (c.f. 0.075 Msun for SN 1987A)
• strong radio emission powered by 1049 erg
  relativistic electrons

GRB980425/SN1998bw
GRB 030329/SN 2003dh Hjorth et al. 03
Mazzali02
10
long GRBs jet from collapsing stars
11
Short-hard GRBs (SHBs) compact binary mergers?

• ?????(z0.2)?????????????????
• No supernova association

Gehrels 05
GRB050509B (z0.225)
Hjorth 05
12
GRB????????
13
GRBs as Star Formation Tracer

• GRB ?????????
• (long) GRB ??????????
• ??????? ltlt ???????????
• caveat selection effect?

Price et al.06
Hopkins Beacom 06
14
Different environment from SNe
core-collapse supernova hosts
Long GRB hosts
Fruchter 06
15
Different environment from SNe
Fruchter 06
supernova GRBs
(in pixels brighter than GRB/SNe location)
GRB?????????????? ?????
GRB??????????? ????????
Metallicity effect!?
16
GRB?????????
17
??????(1)

• Cosmic Microwave Background (CMB)
• z1100 (t40??) ???(??)????????????

2.7 K ?????? 10-5 ????
18
??????(2)

• ???????????(IGM)?????????
• The Gunn-Peterson Test
• IGM optical depth for Lya photons 2.1104
  (1z)3/2 xHI
• xHI lt10-5 for z0
• (xHI nHI / nH)

19
Reionization

• the Cosmic Dark Age
• from recombination (z1100) to reionization (z6?
  20?)
• reionization marks the beginning of galaxy
  formation and end of the dark age

20
??????CMB?????

• ?GP????
• zgt6 ???????????
• ???????????
• xHI gt 10-3 ????????
• CMB ?????
• zreion 10.92.7-2.3 (Page 06)
• z ????????????

21
GRB???????????(vs. quasars)

• Merits
• GRBs detectable at zgtgt6
• ????????????????
• ???????????????
• No proximity effect
• ??????????????????????????
• Damping wing ??????
• First constraint from GRB 050904
• damping wing analysis
• first quantitative upper bound on neutral
  fraction at zgt6
• nHI/nH lt 0.17 (68CL) or 0.60 (95CL) at z6.3

Totani 06
22
Constraints on Reionization
CMB polarization
nHI/nH
quasars
Fan 06
23
GRB???????????
24
Luminosity/distance indicators of GRBs
Liso-Epeak
Ejet-Epeak
Schaefer 06
Liso-variability
Liso- spectral lag
25
Applications

• star formation history
• By using GRBs without z
• Hubble diagram

Yonetoku 03
Schaefer 06
26
Constraint on Dark Energy?

• Pros Highest-z probe for dark energy
• Cons systematics
• ???????
• ?????????????????? luminosity indicator
  ???????????!
• circular argument / tautology
• ?????????????????
• ????????? L-indicator ???
• e.g., another distance measure (Cepheid etc.)
• e.g., low-z GRB sample
• ?????????????
• evolution?
• ??????

27
vs. Supernova Ia (1)
Schaefer 06
Astier 06, SNLS 1yr
28
vs. SN Ia (2)
29
FastSound???FMOS???????????
30
????????????????

• ????????????????????????????????
• ?????????????????
• ?????????????
• ODM/Ob5 ????DM?????????????? ? ????

31
?????????????

• z lt 0.3 ?????SDSS?????????
• ???? z ?????????????????????????????????

Tegmark et al. 06
Percival et al. 07
32
????????? FMOS

• Fiber-Multi-Object Spectrograph in NIR, 400
  fibers
• A Second Generation Common Use Instrument for the
  8.2m Subaru Telescope
• Collaboration with Japan (Kyoto)
  UK(Oxford, Durham, RAL) Australia(AAO)
• Installation underway at Subaru
• First Light
• ?????

33
FMOS ???

• ?????? ? ????????????(??30)???
• 400???????????????????
• ????????????
• ?????????????????????????????
• ????????????????????????????
• ????????????????????????
• ?????????50100??z1 ?????????????????????
• ?????????????
• P(k) ???????????????????????????
• ???
• FMOS???? ?????????
• FMOS?????????????? ????
• ??????????????? ????

34
????FMOS
35
backup slides
36
X-ray Emission Lines

• GRB991216, Chandra, Fe lines

GRB011121, XMM-Newton Reeves et al. (2002), but
see also Rutledge et al. and Borozdin et al.
37
thermal ?background from SNe/GRBs

• typical theoretical prediction
• F?n?/c50 cm2s-1(4psr)-1 (whole)
• F?n?/c0.5 cm2s-1(4psr)-1 (E?gt 20 MeV)
  a few events / yr in Super-K
• Super-K upper limit
• 1.2 cm2s-1 for E?gt19.3 MeV (Malek 03)
• GRBs?
• total energy of ?s may be 10 times higher
• event rate lt10-4 x supernovae
• neutrino spectrum ??

Malek 03
Totani 96