An Overview of Current Gamma-Ray Burst Experiments AGILE Fermi - - PowerPoint PPT Presentation

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An Overview of Current Gamma-Ray Burst Experiments AGILE Fermi - - PowerPoint PPT Presentation

Oct 21, 2022 168 likes •445 views

An Overview of Current Gamma-Ray Burst Experiments AGILE Fermi INTEGRAL RHESSI MESSENGER Swift Suzaku Odyssey Wind Kevin Hurley UC Berkeley Space Sciences Laboratory khurley@ssl.berkeley.edu A Golden Age of GRB Experiments? 9

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SLIDE 1

An Overview of Current Gamma-Ray Burst Experiments

Kevin Hurley UC Berkeley Space Sciences Laboratory khurley@ssl.berkeley.edu

AGILE Fermi INTEGRAL RHESSI MESSENGER Swift Suzaku Odyssey Wind

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A Golden Age of GRB Experiments? 9 missions (13 experiments) are now operating in space which have the capability to detect the prompt emission of GRBs They cover 8 decades in energy (3 keV – 300 GeV) They have up to arcminute localization capability Some of them can localize GRBs almost in real time They are detecting over 400 bursts per year

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The Missions and Experiments

  • 1. AGILE (Super-AGILE, Mini-Calorimeter, and Gamma-Ray Imaging Detector)
  • 2. Fermi (Gamma Burst Monitor1 and Large Area Telescope)
  • 3. INTEGRAL (Imager on Board the INTEGRAL Satellite - IBIS,

SPI Anticoincidence System1)

  • 4. RHESSI (Ge spectrometer)
  • 5. Mars Odyssey (High Energy Neutron Spectrometer)
  • 6. MESSENGER (Gamma-Ray and Neutron Spectrometer)
  • 7. Suzaku (Hard X-Ray Detector Wide Area Monitor1)
  • 8. Swift2 (Burst Alert Telescope1)
  • 9. Wind (Konus1)

1 Dedicated GRB experiment (5)

  • 10. IKAROS (GRB Polarimeter) May 22 launch

2 Dedicated GRB mission (1)

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SLIDE 4

Overview: Energy Ranges

1 keV 10 keV 100 keV 1 MeV 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV AGILE Fermi INTEGRAL Mars Odyssey MESSENGER RHESSI Suzaku Swift Wind

3 keV 300 GeV

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SLIDE 5

Overview: Independent Precise Localization Capabilities

6 10 10 140 Number of bursts/year 90ºx90º (.20 sky) Real- time 10΄ Fermi/LAT 107ºx68º (.18 sky) Hours 3΄ AGILE/SuperAGILE 8.3ºx8º (.0016 sky) Real- time 1.5΄ INTEGRAL/IBIS 100ºx60º (.15 sky) Real- time 3΄ Swift/BAT Field of view Speed Initial localization accuracy Mission/Experiment

These are the bursts for which almost all X-ray, optical, and radio counterpart searches take place today

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SLIDE 6

Mars (Odyssey)

Swift  

INTEGRAL 0.5 light-s WIND 6 light-s

  • LEO Spacecraft

24 light-ms

Mercury (MESSENGER)

AGILE Suzaku Fermi

RHESSI

. . . . . . . 600 l-s 1000 l-s

The 9 spacecraft together form the interplanetary network (IPN)

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SLIDE 7

Overview: Other localization capabilities

250 250 325 Number of bursts/year Whole sky Day Ecliptic latitude band 10º wide Wind/Konus Whole unocculted sky Real-time 3º and above Fermi/GBM Whole sky Hours and more 3΄ and above IPN Field of view Speed Localization accuracy Mission/Experiment

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SLIDE 8

Overlap between Swift, Fermi, and IPN Bursts

IPN 325/yr Fermi 250/yr Swift 140/yr 79 53 31 6

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Overview: Sensitivities

  • Sensitivity is a function of GRB duration, spectrum, peak flux, and

fluence, and the instrument energy range, and time resolution, among

  • ther things
  • Using only the GRB fluence, in various energy ranges between ~15

and ~1000 keV: – Swift BAT 1.2 x 10-8 erg cm-2 – Fermi – GBM 4.0 x 10-8 erg cm-2 – INTEGRAL – IBIS 5.7 x 10-8 erg cm-2 – AGILE – SuperAGILE 1.0 x 10-7 erg cm-2 – IPN 5.0 x 10-7 erg cm-2

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Overview: Redshifts Sampled by Various Missions

2 4 6 8 REDSHIFT, z AGILE INTEGRAL Fermi IPN Swift

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SLIDE 11

Swift (Repetita Juvant)

BAT XRT Spacecraft UVOT

BAT UVOT XRT

  • Burst Alert Telescope (BAT)

– 3΄ positions for GRBs in real- time – 15-150 keV

  • X-Ray Telescope (XRT)

– Arcsecond positions for GRB afterglows – .2 – 10 keV

  • UV/Optical Telescope (UVOT)

– Sub-arcsecond imaging for GRB afterglows – 22.3 mag sensitivity (1000 sec) – Finding chart for other

  • bservers
  • Autonomous re-pointing in ~ 1

minute

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SLIDE 12

Swift

  • The Swift Burst Alert Telescope detects about as many GRBs which

are outside its field of view as inside it (140/year); positions can’t be

  • btained for them onboard
  • These can often be localized by the Interplanetary Network
  • The spacecraft can then repoint to observe the afterglows of these

bursts and obtain arcsecond positions for them

  • It can do the same for GRBs which are localized by Fermi, AGILE,

and INTEGRAL, provided that the error box fits within the 24΄ FoV of the XRT

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Fermi

  • Large Area Telescope (LAT)

– 20 MeV – 300 GeV – 90ºx90º FoV – 10΄ localization in real-time

  • Gamma Burst Monitor (GBM)

– NSSTC/MPE – 8 keV – 40 MeV – All the unocculted sky – 3º localization in real-time

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SLIDE 14

Fermi

  • Nominally points 45º from orbital plane zenith, in survey mode
  • Autonomous repointing to GRB positions within ~5 minutes

– Positions determined by the LAT, or – Positions determined by the GBM, outside the LAT FoV

  • High energy GRB emission is often delayed
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SLIDE 15

How They Work Together – Energy Spectra GRB 100423A

10 100 1000 10000 ENERGY, KEV 0.0001 0.001 0.01 0.1 1 10 PHOTONS/CM

2 S KEV

BAT

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SLIDE 16

How They Work Together – Energy Spectra GRB 100423A

10 100 1000 10000 ENERGY, KEV 0.0001 0.001 0.01 0.1 1 10 PHOTONS/CM

2 S KEV

BAT Konus

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SLIDE 17

How They Work Together – Energy Spectra GRB 100423A

10 100 1000 10000 ENERGY, KEV 0.0001 0.001 0.01 0.1 1 10 PHOTONS/CM

2 S KEV

BAT Konus Suzaku

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SLIDE 18

How They Work Together – Follow-up Observations

  • Swift slews to BAT burst positions and follows up with X-ray and
  • ptical observations using the XRT and UVOT
  • It also slews to the positions of bursts observed and localized by

AGILE, Fermi, INTEGRAL, and the IPN, and obtains arcsecond positions for them from their fading X-ray counterparts

  • This leads to ground-based observations, and measurements of

redshifts

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How They Work Together - Localizations

  • IPN localizations can be used to refine AGILE, Fermi, and
  • ccasionally INTEGRAL and Swift GRB positions
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SLIDE 20

47 IPN/Fermi GBM localizations (there are more)

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How They Work Together - Localizations

  • IPN localizations can be used to refine AGILE, Fermi, and
  • ccasionally INTEGRAL and Swift GRB positions
  • Refined Fermi GBM/IPN localizations can be searched more

efficiently by the Fermi LAT for evidence of high energy emission because their areas are smaller by orders of magnitude

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SLIDE 22

AGILE Suzaku INTEGRAL Konus RHESSI IPN Swift Fermi Energy spectra Localization data Follow-up

  • bservations
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SLIDE 23

GRB Science

  • Redshifts, host galaxies, IGM,

source mechanisms

  • Broadband energy spectra
  • VHE γ radiation, Lorentz

invariance, jet Γ factor, EBL

  • Gravitational radiation, ν, GRB/SN

connection, ground-based VHE searches, your birthday burst

  • Swift GRBs, or bursts followed up

by Swift

  • Swift/Konus, Swift/Suzaku,

Swift/RHESSI, Fermi GRBs

  • Fermi LAT, AGILE GRID GRBs
  • IPN, Swift, Fermi GRBs

If you’re interested in: You should look at:

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SLIDE 24

A New Approach: Polarimetry

  • Polarization of GRB prompt emission has been reported in several

cases

  • The evidence for it is either controversial, or statistically at the limit
  • None of the experiments was a dedicated polarimeter
  • The GRB Polarimeter aboard IKAROS may resolve this issue
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SLIDE 25

GRB Polarimeter aboard IKAROS

  • IKAROS is a solar-sail spacecraft

to Venus built by JAXA

  • Launch was May 22
  • The mission has a dedicated

Compton-scatter GRB polarimeter built by T. Murakami and collaborators

  • Over the 6 month mission lifetime,

definitive polarization measurements of several GRBs are expected

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SLIDE 26

Golden Ages Don’t Last Forever

2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014

YEAR

Konus-Wind Mars Odyssey RHESSI INTEGRAL MESSENGER Swift Suzaku AGILE Fermi