two years of blazar monitoring with the ovro 40m telescope at 15ghz in support of the fermi gst
DESCRIPTION
Two years of blazar monitoring with the OVRO 40m telescope at 15GHz in support of the Fermi GST. Vasiliki Pavlidou (Caltech) on behalf of the OVRO 40m team. The team:. The plan:. Science Observational Program Preliminary Results. Science. - PowerPoint PPT PresentationTRANSCRIPT
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Two years of blazar monitoring with the OVRO 40m telescope at 15GHz
in support of the Fermi GST
Vasiliki Pavlidou (Caltech)on behalf of the OVRO 40m team
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The team:
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The plan:
• Science
• Observational Program
• Preliminary Results
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Science
Blazars (~aligned AGN)
beamed & boosted
fast variability
high apparent luminosity
superluminal motions
high-energy emission
Jets: how are they launched, accelerated, collimated, confined?
What is the jet composition?
How are particles accelerated to relativistic energies?
What are the details of the emission mechanism, and where in the jet is the observed emission coming from?
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McKinney 2006
Blandford & Znajek 1977
Marscher et al. 2008
Blandford & Payne 1982
Dermer, Schlickeiser & Mastichiadis 1991
Lind et al. 1989
Blandford & Levinson 1995
Sikora, Begelman & Rees 1994
Science: theory
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Science: phenomenology
Blazars (~aligned AGN)
beamed & boosted
fast variability
high apparent luminosity
superluminal motions
high-energy emission
What is the correlation between variability, luminosity, beaming?How is emission at different wavelengths correlated?Timelags between flares at different frequencies?
Dependence of variability on spectral properties?
Cosmic evolution of blazar properties?
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Phenomenology: strategy
•Sensitive dependence of observed properties on
•Physical processes: everything goes?(different for different blazars or even for different flares of single blazar?)
•Most impressive behavior need not be typical behavior
Need:
• Large sample
• Statistically well-defined sample
• Regular monitoring
multiwavelength
GeV: Fermi Radio (15 GHz): OVRO 40m
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The OVRO 40m program: sample and strategy
• Sample: all CGRaBS sources at >200
(additional sources monitored, not used in population studies,
e.g.:non-CGRaBS LAT AGN within accessible sky
VERITAS monitoring…)
• Strategy: twice-a-week flux observations at 15GHz
selected based on radio spectral index, radio flux, and X-ray flux
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The OVRO 40m program: data filters and calibration
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• Data: available to Fermi collaboration
• released to public at ~ time of Fermi public data release
• regularly updated thereafter
http://www.astro.caltech.edu/GLAST/
The OVRO 40m program: data policy
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OVRO 40m program: First Results
• Richards et al. (2009): description of program, lightcurves, statistics of variability for individual objects
• Max-Moerbeck et al. (2009): population studies of radio variability
• (also: Fuhrmann et al. 2009: F-GAMMA program description)
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Results: Lightcurves
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Results: Lightcurves
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Results: Variability Amplitude
• One blazar: quantify using intrinsic modulation index flux rms in units of mean m=/<S>
• Obtain through likelihood analysisaccounting for:– uncertainties in individual observations– number of observations
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bimodality!
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Results: Variability Amplitude
• Population Studies
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• Population studies– Is the distribution of modulation indices the
same at high and low redshifts?
Results: Variability Amplitude
High z (>1.1)
Low z (<1.1)
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Results: Time Domain
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Results: Correlation with gamma-ray emission
• Need longer lightcurves!
Fermi LAT data
OVRO data
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Summary• Regular multiwavelength monitoring of large and uniform
samples critical for blazar science
• OVRO 40m telescope is monitoring ~1200 CGRaBS blazars @15 GHz ~twice a week
• Fermi is continuously monitoring the GeV sky
• First results tantalizing, coming soon at a preprint server near you
• The future is bright, tune (and/or join) in!
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Variability Amplitude - population studies
High z / Low z(FSRQs only)
FSRQs vs BLLs
2 random equally-sized subsamples