Multi-Messenger GRB
Astrophysics
Center for Cosmology and AstroParticleCenter for Cosmology and AstroParticlePhysics (CCAPP) FellowPhysics (CCAPP) Fellow
The Ohio State University (OSU)The Ohio State University (OSU)[email protected]@nasa.gov
The Inaugural CCAPP Symposium 2009The Inaugural CCAPP Symposium 2009The Ohio State UniversityThe Ohio State University
Department of PhysicsDepartment of PhysicsOctober 12, 2009October 12, 2009
Michael StamatikosMichael Stamatikos
GSFC
Overview
I. GRB Electromagnetic Emission
II. GRB Satellite Missions
III. Neutrino Astronomy
IV. Summary & Future Outlook
A. PromptB. Afterglow
A. Swift (BAT, XRT & UVOT)B. Fermi (LAT & GBM)C. Correlative observations of GRBs
A. Fireball phenomenology & GRB NeutrinosB. Discrete Neutrino fluxC. IceCube/ANTARES/NESTOR/KM3NET
A. Decade of science synergy
• Millisecond temporal variability implies compact objects R ≤ 2ct.
• Compactness problem resolved via ~100 ≤ Bulk ≤ ~1000, ensuring transparent optical depth to observed -ray photons, i.e.≤ 1.
Gamma-Ray Bursts (GRBs): Prompt Emission• GRBs are unique, varying from burst to burst and class to class (short, long, X-ray rich, non-triggered).
• Super-Eddington luminosities imply relativistic expansion.
T90 (seconds)
Nu
mb
er
of
Bu
rsts
“Long” GRBs ~1301 s
“Short” GRBs ~0.02 s
T90 (seconds) ≡ Time required to accumulate from 5% to 95% of total counts in 50-350 keV band50-350 keV band.
“Short” GRBs
are “hard”
“Long” GRBs
are “soft”
Durations span 6 orders of magnitude!
Num
ber
of B
urst
sN
umbe
r of
Bur
sts
BATSE GRBs
AMANDA-II IceCube
ANTARES /NESTOR KM3NET
b
b
d
dn
for
for
energyBreak
indices Spectral,
densitynumber Spectral
b
oE
d
dn
Kouveliotou et al., ApJ 413: 101 (1993)
Briggs et al., ApJ 459: 40 (1996)
GRBs: Multi-Wavelength EM Afterglows
Spectroscopically observed Doppler redshifts from optical transient (OT) afterglows.
Isotropic Emission: ~ 1 GRB/Day → RGRBiso ~ 0.5 GRB/(Gpc3·yr).
Beamed (Jet) Emission: Corrections → RGRBiso·(4/Ωb) sr and
Eiso· (Ωb/4) sr. Where: b ≡ Beaming solid angle (sr).
Isotropic EmissionIsotropic Emission
Beamed EmissionBeamed Emission
22Bulkc/v1
1
Bulk1
fraction Beamingcos1
jet
jetbf
Boeing Delta II expendable launch vehicle ignition blasted NASA's Swift spacecraft from Complex 17A, Cape Canaveral Air
Force Station, FL on Nov. 20 at 12:16:00.611 p.m. EST in 2004.
“Swifts fly expertly on their first try. Regardless of their
introduction to flight, all young are adept at it soon after they
take their initial leap.”
– National Geographic Society
The Swift MIDEX Mission
BAT
UVOT
XRT
The Swift MIDEX Mission• Burst Alert Telescope (BAT) 15-150 keV
– Coded array of 32,768 CdZnTe detectors.– Sensitivity~ 10-8 ergs/cm2/sec– Detects ~100 GRBs per year – Energy resolution ~7 keV– PSF = 17’, 1-4 arcmin positions
• X-Ray Telescope (XRT) 0.2-10 keV– Arcsec positions 23.6”x 23.6” FOV– Sensitivity ~2x10-14 ergs/cm2/s– 1 mcrab in 104 sec– CCD spectroscopy
• (UVOT) UV/Optical Telescope – Sub-arcsec imaging, 17”x17” FOV– Grism spectroscopy– 24th mag sensitivity (1000 sec)– 170 nm - 600 nm, 6 colors– Sensitivity~ B=24 in white light in 1000 s
GRB Triggers BAT
T < 10 secR < ~4 arcmin BAT Error Circle
XRT Image < 90 sUVOT Image
T< 300 secT< 300 sec
Autonomous re-pointing, = 50 < ~75 s, Orbit of 600 km x 21 inclination.
Temporal Decay of Afterglows: XRT & UVOT GRB 050525A
Fluxes decrease Fluxes decrease by orders of by orders of magnitude in magnitude in first hours!first hours!
0.001 0.01 0.1 1 10 Redshift
N
umbe
r < z > = 2.3
~400 Swift GRBs 95% with XRT @ T < 200 ks ~60% with optical (UVOT + ground) ~10% Short GRBs
• Afterglow Curves, Breaks, Flares, etc.• SGRB Redshift within elliptical galaxy• SGRB with extended soft emission• Over 133 Swift GRBs have redshifts.• GRB 090423 z ~ 8.0! (GCN 9215), i.e.
~85 Gpc or ~ 13 Gyr look back time.
Gehrels et al., New Journal of Physics 9:37 (2007)
XRTUVOT
Over ¾ of all GRB x-ray afterglows and Over ¾ of all GRB x-ray afterglows and redshift are based upon Swift bursts!redshift are based upon Swift bursts!
Fermi (LAT & GBM)
• Large Area Telescope (LAT)
- < 20 MeV to > 300 GeV
- Field of View (FOV) ~ 2.5 sr• GLAST Burst Monitor (GBM)
- 8 keV – 30 MeV• 12 Sodium Iodide (NaI)
Scintillation Detectors– Energy Range:
• 8 keV – 1 MeV– Wide FOV (~8 sr)– Onboard Burst Trigger
• 2 Bismuth Germanate (BGO) Scintillation detectors– Energy Range:
• 0.15 – 30 MeV– Provides important overlap
with LAT energy range.
Large Area Telescope (LAT)
GLAST Burst Monitor (GBM)
LAT FoV
GBM FoV
Correlative Observations: Mutual Science Benefit!
Y. Kaneko et al 2006, ApJS 166, 298
BATSE Epeak Distribution
• BAT increases GBM’s ~20-100 keV effective area by a factor of ~ 3.• Most GRBs have Epeak above BAT energy range. BAT-GBM GRBs↑ Epeaks.• BAT localization precision ~2-3 orders of magnitude better, ↑ follow-up (z).• Test validity of Epeak-Eiso redshift relationships (~35% Swift GRBs have z).• Broad-band spectral/temporal evolution ~ 6 energy decades (keV-GeV) for BAT-
GBM, and ~11 energy decades for UVOT/XRT/BAT/GBM/LAT!! Has been realized in GRB 090510: LAT/GBM (GCN 9334/9336) and BAT/XRT/UVOT (GCN 9331).
Comparison of Effective Areas
2 BGO (0.15 to 30 MeV)
LAT (20 MeV to >300 GeV)
12 NaI (8 keV to 1 MeV)
Stamatikos arXiv:0904.2755
Left plate: Swift-BAT light curve for GRB 080810 with T0 = 13:10:12.3 UTC. Blue line indicates Swift slew-time. Red and green lines indicate 1st and 2nd joint fit interval, respectively. Center plate: Joint Swift-BAT/Fermi-GBM energy spectral fit for 1st interval, with fit parameters of α ~ 0.94 (+0.13, -0.15) and Epeak ~ 674 (+493, -237) keV (χ2/dof~1.33). Right plate: Joint fit for 2nd interval, resulting in fit parameters of α ~ 1.15 (+0.09, -0.10) and Epeak
~ 406 (+189, -106) keV (χ2/dof~1.15). Both intervals were best fit via a Comptonized model. Although consistent within their error bars, the 2nd (brighter) interval provides a better Epeak constraint .
BAT-GBM Joint Spectral Fit of GRB 080810
BAT-GBM Inter-calibration has ~50 common GRBs. Joint analysis is in preparation.
The Fireball Phenomenology: GRB- Connection
Self-Compton Scattering
Magnetic FieldMagnetic Field ElectronElectron
---
-ray-raySynchrotron Radiation
ElectronElectron -ray-rayLow-Energy Low-Energy
PhotonPhoton
Prompt -ray emission of GRB is due to non-thermal processes such as electron synchrotron radiation or self-Compton scattering.
ee-- pp++
E 1051 – 1054 ergs
Internal Shocks
Prompt GRB Emission
External Shocks
Afterglow
Radio
Optical X-ray
-ray
Optical Afterglow Radio Afterglow
Multi-wavelength Afterglows Span EM Spectrum
eThp
cm enpEE If
Photomeson interactions involving relativistically ( 300) shock-accelerated protons (Ep 1016 eV) and synchrotron gamma-ray photons (E 250 keV) in the fireball wind yield high-energy muonic neutrinos (E 1014 – 1015 eV).
R < 108 cm
R 1014 cmT 3 x 103 seconds
R 1018 cm T 3 x 1016 seconds
energy. thresholdΔ E &energy mass ofcenter pγ E Th
Δ
pγcm
C
ount
s/se
c
Time (seconds)Time (seconds)
Spatial & temporal coincidence with
prompt GRB emission
• Shock variability is a unique “finger-print” reflected in the complexity of the GRB time profile.
• Implies compact object.
GRB Prompt Emission GRB Prompt Emission (Temporal) Light Curve(Temporal) Light Curve
Prompt GRB Photon Energy Spectrum –
Characterized by the “Band Function”
Spectral Fit Parameters
A, b, P
Fireball Phenomenology: GRBs & ’s• Fireball Phenomenology + Relativistic Hadronic Acceleration Neutrinos.
• “Smoking gun” signature of hadronic acceleration cosmic rays
• Assuming GRBs were CR accelerators Diffuse flux prediction.
• AMANDA 1 PeV Diffuse Flux Upper Limits:
(eV)(eV) ArrivalArrival Astrophysical Astrophysical
Mechanism/CommentsMechanism/Comments
107 Before Progenitor Collapse/Merger
109 – 1010 Before Baryonic (n, p) Longitudinal decoupling
1012 - ≤ 1014 Before “Precursor” (pp/p)
1014 – 1015 During Prompt (Photomeson/internal shocks)
1017-1018 After Afterglow (Photomeson/External shocks)TeV-PeV muon neutrinos spatio-temporal coincidence
Razzaque, Meszaros & Waxman PRD 69 023001 (2004)Razzaque, Meszaros & Waxman PRD 69 023001 (2004)
Stamatikos, M. et al., AIP Conference Proceedings 727, 146-149 (2004) Stamatikos, M. et al., AIP Conference Proceedings 727, 146-149 (2004)
Waxman, E. Physical Review Letters 75, 386-389 (1995)Waxman, E. Physical Review Letters 75, 386-389 (1995) Stamatikos et al. astro-ph/0510336Stamatikos et al. astro-ph/0510336
Waxman & Bahcall, Phys. Rev. D 59 023002Waxman & Bahcall, Phys. Rev. D 59 023002
Achterberg et al., ApJ 674: 357 (2008)Achterberg et al., ApJ 674: 357 (2008)Achterberg et al., ApJ 664: 397 (2007)Achterberg et al., ApJ 664: 397 (2007)
“Background free” search
• Fluctuations enhance neutrino production, e.g. GRB 941017.
• EM variance neutrino variance.
• Diffuse flux methodology All GRBs described by same energy spectrum• Based upon average values for observables contradicts observations.
Halzen & Hooper ApJ 527, L93-L96 (1999)Halzen & Hooper ApJ 527, L93-L96 (1999)
Alverez-Muniz, Halzen & Hooper Phys. Rev. D 62, (2000)Alverez-Muniz, Halzen & Hooper Phys. Rev. D 62, (2000)
Guetta et al., Astroparticle Physics 20 (2004) 429-455Guetta et al., Astroparticle Physics 20 (2004) 429-455
Few GRBs Few GRBs produce produce
detectable detectable signalsignal
5 orders of magnitude5 orders of magnitude
• GRB030329 Case study.
Motivation for Discrete Approach
• Distributions:
1. Span orders of magnitude,
2. Differ from burst to burst
3. Class to class, and are
4. Effected by selection effects.
Stamatikos et al. astro-ph/0510336Stamatikos et al. astro-ph/0510336
Parameterization of Muon Neutrino Spectrum
b
bb
b
bb
b
b
A
21
1
1
2
ionNormalizat10ln8 90
T
fFA
e
effeciencyProton 1
20,2
45.2
52,
zt
L.f
bMeVv,
FactorBoost LorentzBulk 1276~ 61
max,
12v,52, ztL MeV
energybreak NeutrinoGeV
1
107
,
25.2
2
5
b
MeV
b
z
energybreak n SynchrotroGeV1
102v,
45.2
21
52,2
12
18
tL
z Beb
MeV 100
MeV 1
s10
10
sergs10
max,
,
22v,
5.25.2
5252,
MeV
bb
MeV
vtt
LL
Neutrino spectrum is expected Neutrino spectrum is expected to trace the photon spectrum.to trace the photon spectrum.
Guetta et al., Astroparticle Physics 20, 429-455 (2004)
1 p
Stamatikos et al. astro-ph/0510336Stamatikos et al. astro-ph/0510336
Neutrino Flux Models
Model 1: Discrete Isotropic Model 2: Discrete Jet Model 3: Average Isotropic
ConclusionsConclusions
Expect ~1-3 BAT-GBM GRBs/month (~3217/year).
Can constrain/determine Epeak for all coincident bursts, use redshift to determine burst luminosity and test empirical redshift relations.
Facilitate multi-messenger searches, e.g. neutrino astronomy via IceCube/ANTARES/NESTOR and KM3NET. (See Stamatikos et al 2009, Astro2010 Decadal Whitepaper.)
Science Synergy: Swift-Fermi affords spectral & temporal evolution analysis over an unprecedented 11 energy decades (UVOTLAT)!