C. S. Stalin Indian Institute of Astrophysics › ~tifrjet › presentations ›...
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Variability of blazars: Optical and GeV
C. S. Stalin
Indian Institute of Astrophysics
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Abdo et al. 2011, ApJ, 736, 131 Jorstad et al. 2013, ApJ, 773, 147
Compton dominance < 1; gamma-ray emission due to synchrotron self Compton mechanism
Compton dominance > 1; gamma-ray emission due to EC processes
Blazars
Leptonic / hadronic / hybrid models
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If leptonic models are correct, how do they reflect in variability ?
In leptonic scenario, low (optical) and high (gamma) energy emission are from the same population of electrons and thus both these variations are correlated
➢Correlation between optical and GeV bands are studied for about a dozen sources
➢Close correlations noticed
Bonning et al. 2012 (12 sources) Chatterjee et al. 2012 (6 sources)
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E W. Bonning et al. 2012
3C 454.3
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3C 279 (z = 0.536): A major flare in April 2014
➢First FSRQ detected in VHE (E > 100 GeV; MAGIC in 2008)
➢Underwent a major flare during 25 March – 13 April 2014
➢Brightest gamma-ray flare ever observed in this source
➢Two other flares observed; June 2015 and December 2013
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Flaring state
Paliya et al. 2015, ApJ, 803, 15
April 2014 flare
Second flare: June 2015: SEDs are explained by Leptonic Scenario
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Flares of 2013 December and 2014 April
Paliya et al. 2016, ApJ, in press
2014 Flare Leptonic, 2013 Flare NOT leptonic; a source can behave differently at different times
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How Variability can test these models?
➢Leptonic Scenario: optical and GeV variations are correlated
➢Hadronic scenario: Optical and GeV variations are not correlated
We have less than half – a – dozen studies that focus on this
This could be due to lack of good simultaneous data
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Case 1: FSRQ PKS 0208-512
Correlation during Flares 1 and 3
No correlation during Flare 2
R. Chatterjee et al. 2013
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Case 2: FSRQ 2142-75
Correlation during Flare A, but no correlation during Flare B
M. S. Dutka et al. 2013
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Case 3: NLSy1 1H 0323+342
Paliya et al. 2014, ApJ, 789, 143
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Case 4: FSRQ 3C 279
D. Bhattacharya et al. (2016, to be submitted)
In different band different physical processes may be operating?
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A systematic search for correlated/uncorrelated opical – GeV variations in blazars
Sample: All blazars from 3FGL (Ackermann et al. 2015) : Cross-correlated with CRTS (optical V – band) Only those sources that have good V-band data considered ( 1218 sources)
FSRQ (LSP) --> 343FSRQs (ISP) --> 39FSRQs (HSP) --> 3BL Lacs (LSP) --> 216BL Lacs (ISP) --> 269BL Lacs (HSP) -> 348
Analyzed 7 years of Fermi – LAT data (Analysis in progress)Optical -> CRTSLooked for correlated optical/GeV variations
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Case 1
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Case 2
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Case 3
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Conclusions
➢Optial – GeV variability patterns of blazars clearly tell that the variability behavior shown by them is complex
➢ correlated optical – GeV flux variations
➢ optical flares with no GeV counterparts
➢ GeV flares with no optical counterparts
Blazars do not show similar variability characteristics at all times
Leptonic/Hadronic?
One zone/multi-zone ?
Hybrid models?
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Optical – GeV connection: Towards the answer
➢GeV: Fermi is there
➢Optical: need more planned monitoring (flux + polarization)
➢X-ray : this too is needed (would be nice to try with ASTRSAT when a blazar flares)
➢More understanding needed driven by good quality observations
Observations
Theory
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How ASTROSAT can help us?
ASTROSAT + ground based optical/IR observations (flux and polarization) can give a better data set for broad band modeling of blazars. This in conjunction with improved models will help us in constraining the emission processes in blazars.
For BL Lacs, ASTROSAT X-ray bands lie in the falling part of the first peak as well as in the valley
For FSRQs, ASTROSAT X-ray bands lie in the rising part of the second peak
Careful sample selection + observation of few targets (BL Lacs + FSRQs)
Future: X-ray polarization will help (leptonic v/s hadronic)
Now: