Gamma-Ray Bursts: Things that REALLY Go Bang in the Night Andy Fruchter STScI.
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Transcript of Gamma-Ray Bursts: Things that REALLY Go Bang in the Night Andy Fruchter STScI.
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Gamma-Ray Bursts: Things that REALLY Go Bang in the Night
Andy Fruchter
STScI
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Primary Topics
• An Historical Introduction• The Beppo-Sax Era and Beyond• HST Images• The Astrophysics of the Bursts • The Nature of the Hosts
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The Electromagnetic Spectrum
Gamma-rays observed in Gamma-Ray Bursts have about 10 to 100 times the energy of the X-rays
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What is Redshift?
• Ever since the big bang the universe has expanded with time
• As the universe expands, so do the photons in it --- their wavelengths get longer, and thus they become redder
• Astronomers use “z” to characterize this effect -- with the relative size of the universe equal to 1/(1+z)
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The Sky at Different Wavelengths
Radio
Infra-red
Gamma-Ray
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The Vela Satellites:Protecting the Nation from Illicit GRBs
Designed to detect nuclear tests (in violation of the test ban treaty), the Vela satellites discovered GRBs
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Demonstrating the Cosmic Origin of Gamma Ray Bursts
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Compton Gamma-Ray Observatory
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Taken from http://www.batse.msfc.nasa.gov/data/grb/skymap
BATSE GRB Sky Distribution
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Beppo-Sax Localization
BeppoSAX X-ray images of GRB 990123
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GRB 970228
STIS: 4 September 1997 NICMOS: 24 February 1998
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GRB 970508
2 June 1997 5 July 1998
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OT GRB970508
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OT Spectrum of GRB 970508
Metzger et al. 1997
z=0.83
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Chicken or Egg?(or Red Herring?)
GRB 980425 Error Circles SN 1998bw
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What is a Hypernova?
• “Royal Ahold, the international food retailer, opened its first hypermarket in the Czech capital of Prague. 'Hypernova'… is open every day - including Sunday - from 9 to 9.”
• Sales to date are well above expectations.
• My thought, exactly.
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Daddy, where do stars go when they die?
White Dwarf Neutron Star?
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43+= oαα
cθΓ1
To Beam or Not To BeamTwo primary mechanisms predict a change in the behavior of the light curve when 1/Γ~ θc
1. Mésáros and Rees: Edge Effect =>
2. Rhoads; Sari and Piran: Physical Expansion =>
300Γ+≈+= θτθθ ct
csc
p−=α
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GRB 990123
• The brightest SAX burst yet
• Detected in optical during gamma-ray burst, with
peak
• Keck and NOT spectroscopy find metal absorption
lines => z=1.6
• Resulting ergs
• OT faded by a factor of 4 million in two weeks
54102E ×=γ
9mV =
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GRB 990123: The First Ten Minutes
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ROTSE-1
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GRB 990123 Going…......going….…....gone
+16 days +59 days +380 days
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Are Gamma Ray Bursts “Searchlights”?
• The extreme energy needed to produce a GRB could be reduced dramatically if the bursts are collimated “searchlights”.
• Two predictions for collimated GRBs:– There should be “orphan afterglows”, and
– Afterglows of collimated GRBs should fade more rapidly at late times.
• There are now a number observations of rapid late time fading.
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Beaming Statistics
Frail et al. 2001
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What GRB 990123 Lacks:A SN of Its Own
• Not its fault: at z=1.6, NICMOS or ACS would have been required to detect the SN component
• Numerous bursts show a late-time red excess 0.5 to 1.0 mags fainter than SN1998bw -- only one convincing case of a missing SN (Price et al. 2002) -- and limit is only 1.5 mags > 1998BW.
• At least one burst (GRB 020410; Levan et al. 2003) has been discovered by the late-time excess
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What 990123 Lacked:
Hjorth et al. 2003 (Nature, submitted)
GRB 03032/SN2003dh
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A Galaxy on (nearly) Every Burst
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GRB 000301c
6 March 2000 3 April 2000
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HST/STIS UV Spectrum of GRB 000301c
Smette et al. (2000)
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•Star•z<1•1<z<2•2<z•z undetermined•GRB
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Neon Signs
Bloom et al. 1998
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GRB 990510
Convolved to FWHM = 0.”3 Native Resolution
~1 Year After Burst
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Vreeswijk et al. 2000
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Gamma Ray Bursts and the Deaths of Massive Stars
Afterglow data suggests that …• GRBS occur in galaxies with active star
formation,• often in regions with a lot of gas, which is where
new stars form and where the most massive stars spend their entire brief lives.
• And may often (always?) have underlying SNeHowever, GRBs are so rare that only a tiny fraction
of massive star deaths could produce them.
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Effects of Gamma Ray Bursts on their Environments
Gamma ray bursts are not nice neighbors.The high energy photons they produce can
evaporate interstellar dust grains up 100 light years away, and ionize interstellar gas out to may light years.
The ionized gas will fluoresce as it gradually recombines, and might be used to look for GRB remnants in nearby galaxies.
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What if a GRB happened nearby?
• It could be spectacular: GRB 990123 reached 9th magnitude at a redshift z=1.6.
• A GRB in our Galaxy would ionize atmospheric gasses, creating NOx compounds which destroy ozone (Thorsett 1995).
• Volcanic eruptions, industrial emissions, etc can have similar effects.
• Once in 100 million years, a GRB might be close enough to be more dangerous than Mt. Pinatubo.
• An asteroid will probably get us first.
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The Shape of Things to Come
• SWIFT, a NASA MidEx mission, is approved and should fly in September. Yield: 300 good positions per year?
• These will open the way for systematic study of afterglows, including the still-mysterious short bursts.
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Tomorrow’s QuestionsUpcoming space missions, better coordinated
followup, and ongoing theoretical work all promise continued rapid progress in GRBs.
Specific questions:• Do the short GRBs have afterglows? Host galaxies?
Are they caused by the death of massive stars, merging neutron stars or ….?
• Do all long GRBs have associated supernovae?And, ultimately….• Is every GRB the birth of a new black hole?
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Conclusions
• In all cases evidence is found that the GRB lies in a host galaxies.
• The optical transients display power-law decays for a substantial fraction of the time (in log time), and some display possible evidence of beaming or SNe, but no one model explains all variaitions form power-law decay
• The hosts are blue, have strong [OII] emission, and a steep luminosity function -- all indicating a high star-formation rate.
• GRBs may provide a unique probe of a high-redshift star-forming galaxies.
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GRB 990712
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Loveday, Tresse and Maddox (1999)
M*
α
Hi [OII]
Med [OII]Low [OII]
⎟⎟⎠
⎞⎜⎜⎝
⎛−⎟⎟
⎠
⎞⎜⎜⎝
⎛=
∗ *
exp)(L
L
L
LL
α
φ
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A Galaxy without an (optical) Afterglow
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The SED of GRB 980329
Fruchter (1998)
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Through Every Cloud a GRB May Shine
From Galama and Wijers, 2000
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Light Curve of GRB 990510
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GRB 980405
SN1998bw
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Luminosity Functions by Play Dough
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Luminosity Functions by Play Dough
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12.055.1 ±−=α
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The Evidence Gets Beta
Chary, Becklin and Armus (2002)
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(nearly) Every GRB Is Above Average
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Berger et al. 2002
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Through Every Cloud a GRB May Shine
From Galama and Wijers, 2000
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From Fruchter, Krolik and Rhoads (2001)