can we search for the first stars using grbs? susumu inoue (kyoto u.) - signature of pop iii stars -...
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Pop 3 (~Myr ) → Pop 2 (~Gyr) transition: beginning of life? wikipedia articleTRANSCRIPT
Can We Search for the First Stars Using GRBs?
Susumu Inoue (Kyoto U.)
- signature of Pop III stars- Pop III -> II transition
“A long-standing problem has been put to rest.”K. Omukai, apparently distinguished professor
“A long-standing theoretical problem has been put to rest.”
To solve a scientific problem,experimental (observational) tests are necessary!
first star epoch
Yoshida, Omukai & Hernquist 08
z~100-10Pop 3=metal/dust-free, H2+HD-cooling
assume: no metal/dust, B field, CR, turbulence, DM heating
(1st generation) massive, high UV1st HII region -> IGM reionization1st SN -> 1st metal/dust (+CR+B)
(2nd generation)
Pop 3.1
Pop 3.2not-so-massive?
Pop 2=metal/dust-cooling1st sun -> 1st planet, life, human!
1st BH -> 1st QSO
need to be tested observationally!
when and how?need observations
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Pop 3 (~Myr ) → Pop 2 (~Gyr)transition: beginning of life?
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wikipedia article
Pop 3 → Pop 2 transition
Omukai+ 05 model
[Z/H]<-6: Mfrag~103M Pop 3-3<[Z/H]<-5: Mfrag~0.1-100M Pop 2
[Z/H]crit=-5+-1
H2
H2+HDdust
T minimum -> fragmentationcollapsing zero/low-metal. protostellar clouds
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What is a “first star”?
first Pop 3 stars are (probably) characterized by:- very high to high redshift z~60-5?- very low metals/dust Z/Z~<10-5?- very massive M/M>few x100?
- luminous UV -> large HII region?- weak wind -> clean environment?? - GRB progenitors?
Mamma,che cosa è unaprima stella?
Allora,tesorina…
uncertain but probablelet’s assume for now
upper limits on Pop 3 stars
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slide from T. Nagao
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THE very first GRB Naoz & Bromberg 07
peak energy ~few keV (XRF)long duration ~1000s
z~60-30?
1054 erg/s
1053
1052
Swiftdetectability
expected GRB rate
high-z GRB afterglows c.f. SI, Omukai & Ciardi
2007 MNRAS 380, 1715
GRBs are:very brightvery broadband (<GHz-GeV<)
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161412108 log ν [Hz]
z=1
t=1 day
5
30
tiνt=8hr, 5σ σeνσitivitieσ
10
ALMA
VLA
EVLA
SKA
Spitzer
60
SPICA
Subaru
BUT transient
very high z
c.f. SI, Omukai & Ciardi 2007 MNRAS 380, 1715
JWST, SPICA
z~60-20 (Ly break >3-7 m)
z>~20 space instruments
: Ly break spectroscopy in mid IR
crude, quick z indicatorsalso useful
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15.515.014.514.013.513.0
log ν [Hz]
z=1
t=1 day
5
30
R=100, tiνt=3 hr, S/N=10 σeνσitivity
Ly a
10
60
Subaru
TMT+AO
JWST 20
Compton attenuation in IGM
concordance universeCompton thick at z>~56
z
tT
E>~keV indep. of ionizationE>~MeV Klein-Nishina decline
attenuated spectrum
log E [MeV]
log νFν
star formation with first dust Schneider+ 06
PISN Z=0 SNII
absorption by first dust
Schneider+ 06
(optical depth at fragmentation)
or even marginal Pop 3 ([Z/H]~<10-5) observable?
If such dust-cooling cores exist near a GRB:
also depends on first dust properties other metal lines?
effects of Pop 3 -> Pop 2 transition
very low metals/dust
column density of first protostellar cores
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log(Z/Z)
log
N H,f
rag
Yoshida+ 08
at low metallicity, highly Compton-thick tT>>1
Does all the core material accrete onto the star? May be not.
column densityat fragmentationvs metallicity
If not, is the remaining material swept out by the HII region? How far?Can dust and/or molecules survive destruction in such material?
By the end of the progenitor’s life:
GRBs in Compton thick environments
tT=0, 0.1, 0.3,1,10,30,100central point source in spherefollowing Sunyaev & Titarchuk 80
Compton downscattering
log(E/mec2)
log(
νfν)
- spectral softening- duration lengthening- variability smearing
c.f. Compton-thick AGNs
possible Pop3 signature?
Pop 3 HII regions
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Whalen+ 04
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- large r~<100 pc- low density n~0.1 cm-3
Can be probed throughafterglow evolution?
- flat profile
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Pop 3 HII regions
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Kitayama+ 04
Mstar=200M
Mhalo=106MMhalo=107M
depends on halo environment
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dust distribution in GRB environment
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rdest
GRB
dust
foreground star forming cores
GRB
star forming cores triggered byphotodiss. region driven shock
caveats:dust-cooled fragments -> not GRB progenitors?
Tsuribe & Omukai 06
effect of progenitor evolution: UV, HII region, wind …destruction by GRB UV+X
Questions to Pop 3 theorists
Q1. How much core material is remaining in the vicinityof the star (e.g. ~< pc) at the end of its life?
Q2. How much dust (or molecules) are remainingin such material?
If significant, Compton attenuation of prompt emission?
Summary and Outlook
GRBs are likely observable out to very high z (~60)
In any case, density profile can be probed throughafterglow evolution?
If significant, very low (critical) metallicity observable?
first dust from first supernovae
Maiolino+ 04Todini & Ferrara+ 01also Nozawa+ 03, 06, 07
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Schneider+ 06
SiO2
Mg2SiO4
AC
ACPISN
Z=0 SNII
less formation time, smaller grains→ more efficient coolant flatter extinction curve (matches QSO obs.?)
⇔ today’s dust from AGB
QSO z=6
but destruction by reverse shock?
PISN
Schneider+ 04