cosmology with grbs - european southern … · cosmology with grbs [email protected]...
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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
ELT –
Florence 2004
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
ELT –
Florence 2004
The standard The standard picturepicture
Γ
= 102 - 104 Γ
= 10 ↓
ELT –
Florence 2004
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
ELT –
Florence 2004
42 GRBs with redshift
Assuming isotropyAssuming isotropy
ELT –
Florence 2004
GRB typical Fluence (i.e. time int. flux) is 10-8 – 10-4 erg/cm2
Huge isotropic Huge isotropic equivalent energyequivalent energy!!!!
Jet opening angleRelativistc beaming:
emitting surface ∝
1/Γ
Γ
↓
, Surf.↑
Jet Break ϑ ∼
1/Γ
Log(t)
Log(F)
Jet Jet effecteffect
ELT –
Florence 2004
GRB Jet GRB Jet measuremeasure
“Jet break”
Jet break time tbreak
Jet opening angle ϑ
ELT –
Florence 2004
““TrueTrue”” energeticsenergetics
Frail et
al. 2
001
Isotropic equivalent energyIsotropic equivalent energy
Etrue
= Eiso (1 –
cos ϑ)
Bloo
m e
t al. 20
03
ELT –
Florence 2004
GRB Peak Energy
Characteristic energy of most emitted photons
Prompt emission spectrumPrompt emission spectrum
GRB Spectrum
ELT –
Florence 2004
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
ELT –
Florence 2004
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
ELT –
Florence 2004
EEpeakpeak
––
EEtruetrue
correlationcorrelation
Ghirland
aGh
irland
a , , Gh
isellin
iGh
isellin
i & & La
zzat
iLa
zzat
i 200
420
04ELT –
Florence 2004
Similar to Supernovae Similar to Supernovae IaIa
““StretchingStretching””: : the slower the slower
the brighterthe brighter
ELT –
Florence 2004
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 –
Florence 2004redshiftredshift
Luminos
ity
dist
ance
Luminos
ity
dist
ance
Luminos
ity
dist
ance
Luminos
ity
dist
ance
E=10E=105151
ergerg
χχrr22==2.92.9
χχrr22==1.321.32
ELT –
Florence 2004
1.5 -1.5
ELT –
Florence 2004
0.2 -
0.1
ELT –
Florence 2004
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
ELT –
Florence 2004
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
ELT –
Florence 2004
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
ELT –
Florence 2004
FirmaniFirmani, , GhiselliniGhisellini, , GhirlandaGhirlanda,& Avila,& Avila--Reese, 2004Reese, 2004Sw
iftSw
iftELT –
Florence 2004
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
ELT –
Florence 2004
Simulation for 150 Simulation for 150 ““Swift burstsSwift bursts””
150
ELT –
Florence 2004
ttbreakbreak=0.3d=0.3d
……
the the latest latest GRB GRB ……
ELT –
Florence 2004
`
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
ELT –
Florence 2004
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
ELT –
Florence 2004
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
ELT –
Florence 2004
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..
ELT –
Florence 2004
041006041006
windwind
Ghirland
aGh
irland
a , , Gh
isellin
iGh
isellin
i , , L
azza
tiLa
zzat
i & & Fi
rman
iFi
rman
i 200
420
04
Spheres or jets?Spheres or jets?
“Jet break”
The fireball decelerates1/Γ
opens up
EEisoiso --
EE““truetrue””
EE““truetrue””
= = EEisoiso
(1(1--coscosθθjetjet))
θθjetjet
ttbreakbreak
measures measures θθjetjet
Structured jets?Structured jets?
θviewview
θjetjet
E(θ)=const
E(θ)=E0
θ-2
smoothsmooth bumpybumpy
Firm
aniet
al. 2
004
LL--1.5+1.5+--0.050.05
Universal Universal EEpeakpeak??Pr
eece
et a
l.~200 ~200 keVkeV, , observerobserver
frameframe
BATSEBATSE
HETE IIHETE II
0 0
2
2
ΩΩΛΛ
ΩΩ MM
z=1z=1dL
The cosmic whirlThe cosmic whirl
ttbreakbreak
θθ