Broadband variability and correlation study of 3C 279 during flare of 2017-2018. (arXiv:2001.04493v1 [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 multiwavelength temporal and spectral analysis of flares of 3C 279 during
November 2017–July 2018 are presented in this work. Three bright gamma-ray
flares were observed simultaneously in X-ray and Optical/UV along with a
prolonged quiescent state. A “harder-when-brighter” trend is observed in both
gamma-rays and X-rays during the flaring period. The gamma-ray light curve for
all the flares are binned in one-day time bins and a day scale variability is
observed. Variability time constrains the size and location of the emission
region to 2.1$times$10$^{16}$ cm and 4.4$times$10$^{17}$ cm, respectively.
The fractional variability reveals that the source is more than 100% variable
in gamma-rays and it decreases towards the lower energy. A cross-correlation
study of the emission from different wavebands is done using the textit{DCF}
method, which shows a strong correlation between them without any time lags.
The zero time lag between different wavebands suggest their co-spatial origin.
This is the first time 3C 279 has shown a strong correlation between gamma-rays
and X-rays emission with zero time lag. A single zone emission model was
adopted to model the multiwavelength SEDs by using the publicly available code
GAMERA. The study reveals that a higher jet power in electrons is required to
explain the gamma-ray flux during the flaring state, as much as, ten times of
that required for the quiescent state. However, more jet power in magnetic
field has been observed during the quiescent state compared to the flaring
state.
A multiwavelength temporal and spectral analysis of flares of 3C 279 during
November 2017–July 2018 are presented in this work. Three bright gamma-ray
flares were observed simultaneously in X-ray and Optical/UV along with a
prolonged quiescent state. A “harder-when-brighter” trend is observed in both
gamma-rays and X-rays during the flaring period. The gamma-ray light curve for
all the flares are binned in one-day time bins and a day scale variability is
observed. Variability time constrains the size and location of the emission
region to 2.1$times$10$^{16}$ cm and 4.4$times$10$^{17}$ cm, respectively.
The fractional variability reveals that the source is more than 100% variable
in gamma-rays and it decreases towards the lower energy. A cross-correlation
study of the emission from different wavebands is done using the textit{DCF}
method, which shows a strong correlation between them without any time lags.
The zero time lag between different wavebands suggest their co-spatial origin.
This is the first time 3C 279 has shown a strong correlation between gamma-rays
and X-rays emission with zero time lag. A single zone emission model was
adopted to model the multiwavelength SEDs by using the publicly available code
GAMERA. The study reveals that a higher jet power in electrons is required to
explain the gamma-ray flux during the flaring state, as much as, ten times of
that required for the quiescent state. However, more jet power in magnetic
field has been observed during the quiescent state compared to the flaring
state.
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