Two-zone emission modeling of PKS 1510-089 during the high state of 2015. (arXiv:1908.04803v1 [astro-ph.HE])

Two-zone emission modeling of PKS 1510-089 during the high state of 2015. (arXiv:1908.04803v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Prince_R/0/1/0/all/0/1">Raj Prince</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_N/0/1/0/all/0/1">Nayantara Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nalewajko_K/0/1/0/all/0/1">Krzysztof Nalewajko</a>

PKS 1510-089 is one of the most variable blazars in the third Fermi-LAT
source catalog. During 2015, this source has shown four flares identified as
flare A, B, C, and D in between three quiescent states Q1, Q2, and Q3. The
multi-wavelength data from Fermi-LAT, Swift-XRT/UVOT, OVRO, and SMA observatory
are used in our work to model these states. Different flux doubling times have
been observed in different energy bands which indicate there could be multiple
emission zones. The flux doubling time from the gamma-ray and X-ray light
curves are found to be 10.6 hr, 2.5 days, and the average flux doubling time in
the optical/UV band is 1 day. It is possible that the gamma-ray and optical/UV
emission are produced in the same region whereas X-ray emission is coming from
a different region along the jet axis. We have also estimated the discrete
correlations functions (DCFs) among the light curves of different energy bands
to infer about their emission regions. However, our DCF analysis does not show
significant correlation in different energy bands though it shows peaks in some
cases at small time lags. We perform a two-zone multi-wavelength time-dependent
SED modeling with one emission zone located near the outer edge of the broad
line region (BLR) and another further away in the dusty/molecular torus (DT/MT)
region to study this high state.

PKS 1510-089 is one of the most variable blazars in the third Fermi-LAT
source catalog. During 2015, this source has shown four flares identified as
flare A, B, C, and D in between three quiescent states Q1, Q2, and Q3. The
multi-wavelength data from Fermi-LAT, Swift-XRT/UVOT, OVRO, and SMA observatory
are used in our work to model these states. Different flux doubling times have
been observed in different energy bands which indicate there could be multiple
emission zones. The flux doubling time from the gamma-ray and X-ray light
curves are found to be 10.6 hr, 2.5 days, and the average flux doubling time in
the optical/UV band is 1 day. It is possible that the gamma-ray and optical/UV
emission are produced in the same region whereas X-ray emission is coming from
a different region along the jet axis. We have also estimated the discrete
correlations functions (DCFs) among the light curves of different energy bands
to infer about their emission regions. However, our DCF analysis does not show
significant correlation in different energy bands though it shows peaks in some
cases at small time lags. We perform a two-zone multi-wavelength time-dependent
SED modeling with one emission zone located near the outer edge of the broad
line region (BLR) and another further away in the dusty/molecular torus (DT/MT)
region to study this high state.

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