# High Energy Gamma-Ray Emission From PKS 1441+25

## TL;DR

This paper reports gamma-ray observations of quasar PKS 1441+25, highlighting a rapid flare, spectral hardening, and modeling of emission mechanisms, revealing insights into jet physics and particle acceleration.

## Contribution

First detailed gamma-ray spectral analysis of PKS 1441+25 during a flare, including spectral cutoff detection and leptonic modeling with MCMC methods.

## Key findings

- Detected a gamma-ray flare with flux doubling in ~1.44 days.
- Observed spectral hardening with photon index as low as 1.54.
- Modeled emission with leptonic processes indicating increased Lorentz factor or magnetic field during flares.

## Abstract

We present the $\gamma$-ray observations of the flat-spectrum radio quasar PKS 1441+25 (z=0.939), using the {\it Fermi} large Area Telescope data accumulated during January - December 2015. A $\gamma$-ray flare was observed in January 24, when the flux increased up to $(2.22\pm0.38)\times10^{-6}\;{\rm photon\:cm^{-2}\:s^{-1}}$ with the flux-doubling time scale being as short as $\sim1.44$ days. The spectral analysis shows that from April 13 to April 28, 2015 the MeV-to-GeV photon index has hardened and changes in the range of $\Gamma=(1.73-1.79)$ for most of the time. The hardest photon index of $\Gamma=1.54\pm0.16$ has been observed on MJD 57131.46 with $11.8\sigma$ which is not common for flat-spectrum radio quasars. For the same period the \gray spectrum shows a possible deviation from a simple power-law shape, indicating a spectral cutoff at $E_{\rm cut}=17.7\pm8.9$ GeV. The spectral energy distributions during quiescent and flaring states are modeled using one-zone leptonic models that include the synchrotron, synchrotron self Compton and external inverse Compton processes; the model parameters are estimated using the Markov Chain Monte Carlo method. The emission in the flaring states can be modeled assuming that either the bulk Lorentz factor or the magnetic field has increased. The modeling shows that there is a hint of hardening of the low-energy index ($\sim1.98$) of the underlying non-thermal distribution of electrons responsible for the emission in April 2015. Such hardening agrees with the $\gamma$-ray data, which pointed out a significant $\gamma$-ray photon index hardening on April 13 to 28, 2015.