cosmology with grbs - european southern … · cosmology with grbs [email protected]...
TRANSCRIPT
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Cosmology with Cosmology with [email protected]@merate.mi.astro.it
--
OsservatorioOsservatorio
didi
BreraBrera
Giancarlo Giancarlo GhirlandaGhirlanda
In coll. withIn coll. with
Gabriele Gabriele GhiselliniGhisellini
DavideDavide
LazzatiLazzati
Claudio Claudio FirmaniFirmani
Vladimir AvilaVladimir Avila--ReeseReese
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Prompt emission Prompt emission Afterglow emission Afterglow emission
• energiesenergies
> 10 > 10 keVkeV
• 1 1 ms to ms to 1 1 ks ks
•• high high varibility varibility
• energiesenergies
X,X,
OptOpt, IR, Radio, IR, Radio
•• days to months days to months
•• smooth powerlawsmooth powerlaw(s) (s)
GRBs are fast transient high energy sources @ cosmological distances
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The standard The standard picturepicture
Γ
= 102 - 104 Γ
= 10 ↓
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GRB 970228
Gamma ray position accuracy 2 deg!!Need arcmin accuracy to
1.
Identify the counterpart
2.
Follow the afterglow and measure the redshift
X ray afterglow indetification
OT spectrum
42 redshift
s /3000 GRBsGRBsGRBs
are are cosmological cosmological
Optical transient
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42 GRBs with redshift
Assuming isotropyAssuming isotropy
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GRB typical Fluence (i.e. time int. flux) is 10-8 – 10-4 erg/cm2
Huge isotropic Huge isotropic equivalent energyequivalent energy!!!!
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Jet opening angleRelativistc beaming:
emitting surface ∝
1/Γ
Γ
↓
, Surf.↑
Jet Break ϑ ∼
1/Γ
Log(t)
Log(F)
Jet Jet effecteffect
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GRB Jet GRB Jet measuremeasure
“Jet break”
Jet break time tbreak
Jet opening angle ϑ
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““TrueTrue”” energeticsenergetics
Frail et
al. 2
001
Isotropic equivalent energyIsotropic equivalent energy
Etrue
= Eiso (1 –
cos ϑ)
Bloo
m e
t al. 20
03
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GRB Peak Energy
Characteristic energy of most emitted photons
Prompt emission spectrumPrompt emission spectrum
GRB Spectrum
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Isotropic energy [erg]
EEpp(1+z)=E(1+z)=Eisoiso0.40.4
28 GRB +2 XRF28 GRB +2 XRFAmat
i et
al. 2
002,
Amat
i et
al. 2
002,
Ghirlan
daGh
irland
aet
al. 2
004
et a
l. 2
004
11--cos(cos(θθ))??031203
ttjet,djet,d
((ηηγγ
n)n)
uniform n, 1<n<10 if unknown uniform n, 1<n<10 if unknown
1 1 keVkeV
––
10 10 MeVMeV
ηηγγ=0.2=0.2
3/83/8 1/81/8θθ==0.160.16
(1+z)(1+z) EE
γ,γ,iso,52iso,521/81/83/83/8
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Ghirland
aGh
irland
a , , Gh
isellin
iGh
isellin
i & & La
zzat
iLa
zzat
i 200
420
04χχrr
22=1.27=1.27
EE peak
peak=k
E=k
E γγ0.
706
0.70
6
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EEpeakpeak
––
EEtruetrue
correlationcorrelation
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Ghirland
aGh
irland
a , , Gh
isellin
iGh
isellin
i & & La
zzat
iLa
zzat
i 200
420
04ELT –
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Similar to Supernovae Similar to Supernovae IaIa
““StretchingStretching””: : the slower the slower
the brighterthe brighter
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Ghirland
aGh
irland
a , , Gh
isellin
iGh
isellin
i , , L
azza
tiLa
zzat
i & & Fi
rman
iFi
rman
i 200
420
04
Luminos
ity
dist
ance
Luminos
ity
dist
ance
E=10E=105151
ergerg
redshiftredshift
ELT –
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Luminos
ity
dist
ance
Luminos
ity
dist
ance
Luminos
ity
dist
ance
Luminos
ity
dist
ance
E=10E=105151
ergerg
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χχrr22==2.92.9
χχrr22==1.321.32
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1.5 -1.5
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0.2 -
0.1
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Ghirland
aGh
irland
a , , Gh
isellin
iGh
isellin
i , , L
azza
tiLa
zzat
i & & Fi
rman
iFi
rman
i 200
420
04
Consistent with Consistent with WMAP: WMAP:
ΩΩMM=0.3, =0.3, ΩΩΛΛ
=0.7=0.7
1515156156
GRB+SNGRB+SN
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Firm
ani
Firm
ani , , G
hise
llini
Ghisellin
i , , G
hirlan
daGh
irland
a&
Avila
& Avila-- R
eese
, 20
04Re
ese,
200
4Flat UniverseFlat Universe: : ΩΩtottot=1=1
P=wP=w00
ρρcc22
transition z: transition z: a = 0a = 0
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Firm
ani
Firm
ani , , G
hise
llini
Ghisellin
i , , G
hirlan
daGh
irland
a&
Avila
& Avila-- R
eese
, 20
04Re
ese,
200
4Flat UniverseFlat Universe: : ΩΩtottot=1,=1,
ΩΩMM
=0.27=0.27
P=(wP=(w00
+w+w’’z)z)ρρcc22
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FirmaniFirmani, , GhiselliniGhisellini, , GhirlandaGhirlanda,& Avila,& Avila--Reese, 2004Reese, 2004Sw
iftSw
iftELT –
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In the Swift era:In the Swift era:FluencesFluences
not strongly dependent on znot strongly dependent on z
Early afterglow very well monitoredEarly afterglow very well monitored
Hope for small errors even at highHope for small errors even at high--zzXRFXRF
XRFXRF
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Simulation for 150 Simulation for 150 ““Swift burstsSwift bursts””
150
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ttbreakbreak=0.3d=0.3d
……
the the latest latest GRB GRB ……
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`
Updated Correlation Updated Correlation
Updated cosmological constraintsUpdated cosmological constraints
www.merate.mi.astro.it/~ghirla/deep/blink.htmlwww.merate.mi.astro.it/~ghirla/deep/blink.html
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High High redshift GRBs redshift GRBs and and ttbreakbreak
Z=10Z=10
Z=1Z=1
ttbreakbreak
=11 =11 daysdays
FF∝∝tt--1 1 forfor t<t<ttbreakbreak
FF∝∝tt--2 2 forfor t>t>ttbreakbreak
@ z=1@ z=1
ttbreakbreak = 2 = 2 days days
H H ≈≈
19 @ 1 day 19 @ 1 day
Typical Typical AfterglowAfterglow
ttbreakbreak
=2 =2 daysdays
VLTVLT
ELTELT
ELT ELT is mandatory to is mandatory to measure measure the jet break the jet break time of high z time of high z GRBsGRBs
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Cosmology with Cosmology with high z high z GRBsGRBs
15 15 GRBs GRBs ((present samplepresent sample) ) 0.1 < z < 3.20.1 < z < 3.2
++
10 10 GRBs GRBs
9 < z < 109 < z < 10
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ConclusionsConclusions
••
GRBsGRBs
areare
amongamong
the the most powerful sources most powerful sources of the of the universe universe and through the GGL04 and through the GGL04 correlation correlation can can be used be used as cosmological rulersas cosmological rulers..
••
GRBsGRBs
((detectable detectable out out to to z=17)z=17)
representrepresent
thethe
link link betweenbetween
SN Ia and CMBSN Ia and CMB
primary anysotropiesprimary anysotropies, and , and allows to allows to study study the the Universe geometry Universe geometry and and dynamicsdynamics..
••
RequirementsRequirements: : accurate accurate measure measure of of ttbreakbreak
+ + inclusion inclusion of of very very high high redshiftredshift
GRBsGRBs. At z > 6. At z > 6--7 7 need for Extramely need for Extramely Large TelescopesLarge Telescopes. .
••
ELTELT
high res. high res. Imaging Imaging can can also contribute also contribute in in understanding understanding the GRB the GRB progenitorprogenitor
nature, nature, emissionemission
processprocess
nature, GRB nature, GRB dynamicsdynamics
••
ELTELT
high res. high res. Spectroscopy Spectroscopy can can contribute contribute in in understanding understanding the GRB the GRB environsenvirons, , galaxygalaxy
populationpopulation..
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041006041006
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windwind
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Ghirland
aGh
irland
a , , Gh
isellin
iGh
isellin
i , , L
azza
tiLa
zzat
i & & Fi
rman
iFi
rman
i 200
420
04
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Spheres or jets?Spheres or jets?
“Jet break”
The fireball decelerates1/Γ
opens up
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EEisoiso --
EE““truetrue””
EE““truetrue””
= = EEisoiso
(1(1--coscosθθjetjet))
θθjetjet
ttbreakbreak
measures measures θθjetjet
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Structured jets?Structured jets?
θviewview
θjetjet
E(θ)=const
E(θ)=E0
θ-2
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smoothsmooth bumpybumpy
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Firm
aniet
al. 2
004
LL--1.5+1.5+--0.050.05
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Universal Universal EEpeakpeak??Pr
eece
et a
l.~200 ~200 keVkeV, , observerobserver
frameframe
BATSEBATSE
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HETE IIHETE II
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0 0
2
2
ΩΩΛΛ
ΩΩ MM
z=1z=1dL
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The cosmic whirlThe cosmic whirl
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ttbreakbreak
θθ