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Cosmological Transient Objects
Poonam Chandra
Royal Military College of Canada
Raman Research Institute14th December 2010
Cosmological Transient Objects
Supernovae and
Gamma Ray Bursts
Supernovae and Gamma Ray Bursts
• Supernova energy 1029 more than an atmospheric nuclear bomb explosion.
• At the time of explosion, the supernova can shine brighter than the host galaxy consisting of billions of stars.
• In one month, a supernova can emit as much energy as Sun would emit in its entire life span of billions of years.
• GRBs: biggest source of gamma-rays in universe and 100 times more energetic than supernovae.
Outline (Gamma Ray Bursts)
• Challenges• How to meet the challenge: multiwaveband
modeling• Importance of radio observations• Our radio campaign and some results• Future of gamma ray burst science
Gamma Ray Bursts
• A big challenge when discovered in 1960s.• Gamma-ray signals for just a fraction of
seconds to at most few minutes.• Non-terrestrial origin • BATSE: isotropic
Meszaros and Rees 1997
Major breakthrough
• BeppoSAX: first detection of X-ray counterpart of GRB 970228.
• Optical detection after 20 hours.
GRB 970508: a watershed event
• X-ray BeppoSAX• Optical , z=0.835 => Cosmological• Scintillation: fireball model• Radio, late time- energetics
• GRB 980425/SN1998bw- massive star origin
Crisis: GRB 990123
• Assuming isotropy, the -g ray energies spanned three orders of magnitude: 3×1051 to 3×1054 erg
• Central engine energy requirements??
The GRB Energy Crisis circa 1999
Astrophysics at the Extremes, Dec. 15-17, 2009, Hebrew University
10
Stan Woosley says “I’m a very troubled theorist.”
erg 102M 542sun c
Piran, Science, 08 Feb 2002
ApJ 519, L7, 1999
Jet Signatures
11
radio
opticalX-ray
jtFl
ux D
ensi
ty
time
-1t
-2t
-1/3t
Harrison et al. 1999
tjet
The GRB Energy Crisis Resolved
Frail et al (2001)
That was then…• The GRB energy crisis was resolved• GRB outflows are highly beamed (θ ~ 1-10
degrees)• Geometry measured from jet break signature in
light curves• Beaming-corrected radiated energies are
narrowly distributed around a “standard” value of ~1051 erg
• A host of other measurements (X-ray afterglows, broadband modeling, calorimetry) support this energy scale
• This energy scale is consistent with models of GRB central engines
13
This is now… POST-SWIFT1. The mystery of the missing jets in the Swift era.2. The emerging population of hyper-energetic
events.3. The established class of sub-energetic gamma-
ray bursts.
Multiwaveband modeling• Long lived afterglow with powerlaw decays• Spectrum broadly consistent with the synchrotron.
• Measure Fm, nm, na, nc and obtain Ek (Kinetic energy), n (density), ee, eb (micro parameters), theta (jet break), p (electron spectral index).
Radio Observations
• Late time follow up- accurate calorimetry• Scintillation- constraint on size• VLBI- fireball expansion• Density structure- wind-type versus constant
Multiwaveband modeling
Radio afterglow statistics: 1997-2010
•1/3rd of all GRBs seen as radio afterglows since 1997-2010.•93 out of 244•46 out of 149 (post Swift)•No strong redshift dependence.•z<2 47/88• z>2 21/43 Chandra et al. 2011
Radio afterglow statistics: post-Swift
•1/3rd of all GRBs seen as radio afterglows since 1997-2010.•93 out of 244•46 out of 149 (post Swift)•No strong redshift dependence.•z<2 47/88• z>2 21/43 Chandra et al. 2011
Canonical radio afterglow light curve
GRB 070125 (Chandra et al. 2008)
• One of the brightest Swift burst with isotropic energy of 1.1x1054 erg.
• Followed extensively in X-ray, optical, mm and radio bands.
• In radio bands, observed for more than a year.
GRB 070125: Scintillation (Chandra et al. 2008)
Jet break in GRB 070125Chandra et al. 2008
• Chromatic jet break…
• Optical band, day 3• X-ray band, day 10• Explanation—
– Inverse-Compton Mechanism
Inverse-Compton in X-rays
Inverse Compton Scattering
• Possible explanation for the delay in jet breaks or chromatic jet breaks in various GRBs.
• Does not affect radio and optical bands but dominates in X-ray bands.
• More effective in high-density environments. Radio data is crucial.
GRB 070125: Highlights (Chandra et al. 2008)
• Diffractive scintillation- constrain the fireball size
• Chromatic jet break- Inverse Compton• Collimated g-energy 2.5x1052 erg.• Kinetic energy 1.7x1051 erg.
GRB 090423
• Highest redshift GRB at z=8.2• Highest redshift object of any kind known in
our Universe.• Must have exploded just 630 million years
after the Big Bang.
GRB 090423
• X-ray observtions: 73 s after detection• Optical observations: 109 s after detection• No optical transient.• Detection in J band onwards.• Photo-z=8.06+/-0.25• Spectral-z=8.23+/-0.08
Radio observations of GRB 090423(Chandra et al. 2010)
Detections - VLA: 8.5 GHz on Apr 25-
Jun 27.– 74 +/- 22 uJy at Δt~8 d– 2-hr integrations every 2
days– Data sets averaged (in UV
plane) to improve detection sensitivity
– Undetectable after Δt~65 d
PdBI: 95 GHz on Apr 23-24
– Castro-Tirado et al. report a secure source detection of 200 uJy (no error bar given)
Non-Detections - WSRT: 4.9 GHz
on May 22-23CARMA: 95
GHz on Apr. 25
IRAM 30-m: 250 GHz on Apr 25
29
Multiwaveband modeling:(Chandra et al. 2010)
Broadband modeling
31
• High energy burst exploded in constant density medium.
• No jet break occurred until day 50.
Reverse shock emission in GRB 090423
• Reverse shock emission at day 9 (time dilated)• After 1+z correction, reverse shock on day 1• Seen is 250 GHz data also at around 10 hours
(1+z corrected).• Implications for high Lorentz factor
Previous high redshift GRB 050904 z=6.26
Afterglow Properties –
– GRB 050904 (z=6.26). Both are hyper-energetic (>1051 erg) but they exploded in very different environments. (in situ n=600 cm-3 for GRB 050904)
– Large energy predicted for Pop III. Not unique.
– Low, constant density predicted for Pop III. Not unique.
– No predictions for θj, εB, εe & p
– Reverse shock detection in both GRBs
Canonical radio afterglow light curve
• Swift had expected to find many RS
• At most, 1:25 optical AG have RS
• Favored explanation– Ejecta are magnetized (i.e. σ>1). – Do not need to be fully Poynting-flux
dominated – Suppresses RS emission
• Does not explain why prompt radio emission is seen more frequently.
• About 1:4 radio AG may be RS• Possible Explanation: The RS
spectral peak is shifted out of the optical band to lower frequencies
36
Kul
karn
i et
al.
(199
9)
Reverse shock in radio GRBs Chandra et al. 2010b
A seismic shift in radio afterglow studies
• The VLA got a makeover!• More bandwidth, better receivers, frequency
coverage• 20-fold increase in sensitivity• Capabilities started in 2010
• GRBs at higher frequencies where ISS is reduced• Measure polarization and rotation measures• Absorption lines possible (CO; see Inoue et al.
2007)
Future of GRB Physics
• Expanded Very Large Array (EVLA)• 20 times more sensitive than the VLA.
Future: The EVLA- accurate calorimetry
EVLA, 3-s, z=8.5 1 hr
EVLA, 3-s, z=2.5 1 hr
Future: Atacama Large Millimeter Array (ALMA)
Accurate determination of kinetic energy
Future: ALMA Debate between wind versus ISM solved
Future: ALMAReverse Shock at high redshifts
mm emission from RS is bright, redshift-independent (no extinction or scintillation) (Inoue et al. 2007). ALMA will be ideal.
Conclusions
• Multiwaveband modeling required to understand the GRB afterglow Physics.
• New class of hyperenergetic GRBs such as GRB 070125.• Star formation taking place even at 630 million years after
the big bang.• New explanation for the delay in jet breaks in Swift bursts• Radio and mm is crucial as they are unique in estimating
the accurate energy, density and type of medium.• Future lies with the EVLA and the ALMA.
Supernovae• Chandra, Dwarkadas, et at. 2009, ApJ 699, 388
– X-rays from the explosion site: 15 years of light curves of SN 1993J.• Nymark, Chandra, Fransson 2009, A &A 494, 179
– Modeling the X-ray emission of SN 1993J.• Patat, Chandra, et al. 2007, Science 317, 924
– Detection of circumstellar material in a normal Type Ia supernova.• Chandra, Ray, et al. 2005, ApJ 629, 933
– Chandra’s tryst with SN 1995N.• Chandra, Ray, Bhatnagar 2004, ApJ 612, 974
– The late time radio emission from SN 1993J at meter wavelengths.• Chandra, Ray, Bhatnagar 2004, ApJL 604, 97
– Synchrotron aging and radio spectrum of SN 1993J.
Collaborators for GRB work
• Dale Frail• Shri Kulkarni• Brad Cenko• Derek Fox• Edo Berger• Fiona Harrison• Mansi Kasliwal
THANKS