Swift and XMM-Newton monitoring of the ISP blazar ON 231 in outburst state. (arXiv:1906.01964v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kalita_N/0/1/0/all/0/1">Nibedita Kalita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sawangwit_U/0/1/0/all/0/1">Utane Sawangwit</a>
We present a detailed temporal and spectral study of the intermediate type
blazar, ON 231 with observations taken by Swift and XMM-Newton satellites
during an outburst phase in June 2008. The source shows multiple X-ray flares
in that period when the flux amplitude varies in the range of 27-38%. The X-ray
spectra are well fitted with a broken power-law model indicating the presence
of both synchrotron and inverse Compton components. We find that the source
shows strong and variable emission in the soft energy bands (below 3-4 keV),
where the hard band emission is weak and stable. All the soft X-ray bands show
correlated variability with zero lag, while a soft lag of -600 s between the
0.3-0.5 and 4-10 keV bands is observed with DCF analysis. A time-resolved
spectral study of the flares gives a positive relation between the total fluxes
and the break energies of the two emission components.
We present a detailed temporal and spectral study of the intermediate type
blazar, ON 231 with observations taken by Swift and XMM-Newton satellites
during an outburst phase in June 2008. The source shows multiple X-ray flares
in that period when the flux amplitude varies in the range of 27-38%. The X-ray
spectra are well fitted with a broken power-law model indicating the presence
of both synchrotron and inverse Compton components. We find that the source
shows strong and variable emission in the soft energy bands (below 3-4 keV),
where the hard band emission is weak and stable. All the soft X-ray bands show
correlated variability with zero lag, while a soft lag of -600 s between the
0.3-0.5 and 4-10 keV bands is observed with DCF analysis. A time-resolved
spectral study of the flares gives a positive relation between the total fluxes
and the break energies of the two emission components.
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