Multi-frequency variability study of Ton 599 during high activity of 2017. (arXiv:1811.11256v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Prince_R/0/1/0/all/0/1">Raj Prince</a>
In this work, I have presented a multi-frequency variability and correlation
study of the blazar Ton 599, which was observed first time in flaring state at
the end of 2017. Data from textit{Fermi}-LAT, Swift-XRT/UVOT, Steward
Observatory, and OVRO (15 GHz) is used, and it is found that the source is more
variable in $gamma$-ray and optical/UV than X-ray and radio. Large variations
in the degree of polarization (DoP) and position angle (PA) is noticed during
the flaring period. Maximum flux during $gamma$-ray flare is found to be
12.63$times$10$^{-7}$ at MJD 58057.5 from the 1-day bin light curve (LC),
which is the maximum flux ever achieved by this source. It is further found
that all the peaks of flare are very symmetric, which suggests the cooling time
of electrons is much smaller than light crossing time. Using 1-day as a fast
variability time, the size of the $gamma$-ray emission region is estimated as
1.88$times$10$^{16}$ cm. Two 42 GeV of photons are detected during the flare
which puts a constraint on the location of the emission region, and it is found
that the $gamma$-ray emitting blob is located at the outer edge or outside the
broad line region (BLR). A trend of increasing fractional variability towards
higher energies is also seen. Strong correlations were seen between
$gamma$-ray, optical/UV, X-ray, and radio (15 GHz) emission. A small time lag
between $gamma$-ray and optical/UV suggest their emission to be co-spatial
while lag of 27 days between $gamma$-ray and OVRO (15 GHz) suggest two
different emission zone separated by a distance of $sim$ 5 pc.
In this work, I have presented a multi-frequency variability and correlation
study of the blazar Ton 599, which was observed first time in flaring state at
the end of 2017. Data from textit{Fermi}-LAT, Swift-XRT/UVOT, Steward
Observatory, and OVRO (15 GHz) is used, and it is found that the source is more
variable in $gamma$-ray and optical/UV than X-ray and radio. Large variations
in the degree of polarization (DoP) and position angle (PA) is noticed during
the flaring period. Maximum flux during $gamma$-ray flare is found to be
12.63$times$10$^{-7}$ at MJD 58057.5 from the 1-day bin light curve (LC),
which is the maximum flux ever achieved by this source. It is further found
that all the peaks of flare are very symmetric, which suggests the cooling time
of electrons is much smaller than light crossing time. Using 1-day as a fast
variability time, the size of the $gamma$-ray emission region is estimated as
1.88$times$10$^{16}$ cm. Two 42 GeV of photons are detected during the flare
which puts a constraint on the location of the emission region, and it is found
that the $gamma$-ray emitting blob is located at the outer edge or outside the
broad line region (BLR). A trend of increasing fractional variability towards
higher energies is also seen. Strong correlations were seen between
$gamma$-ray, optical/UV, X-ray, and radio (15 GHz) emission. A small time lag
between $gamma$-ray and optical/UV suggest their emission to be co-spatial
while lag of 27 days between $gamma$-ray and OVRO (15 GHz) suggest two
different emission zone separated by a distance of $sim$ 5 pc.
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