A large high-energy gamma-ray flare from the blazar 3C 273

TL;DR

This paper reports a significant high-energy gamma-ray flare from the blazar 3C 273, observed by CGRO, showing energy-dependent variability and spectral hardening during the flare, suggesting different emission mechanisms at play.

Contribution

It provides the first detailed analysis of a large gamma-ray flare from 3C 273, highlighting energy-dependent variability and spectral changes with implications for emission mechanisms.

Findings

EGRET observed a significant >100 MeV flare from 3C 273.

COMPTEL did not observe variability below ~30 MeV during the flare.

Spectral hardening occurred during the flaring period, indicating different emission processes.

Abstract

The Compton Gamma-Ray Observatory (CGRO) experiments EGRET and COMPTEL observed the Virgo sky region continuously for 7 weeks between December 10, 1996 and January 28, 1997. The prominent quasar 3C~273 was found to be the brightest source in gamma-rays and was significantly detected by EGRET and COMPTEL. The EGRET experiment observed a time-variable flux at energies above 100 MeV, which reached in a 2-week flaring period (December 30, 1996 to January 14, 1997) its highest flux level observed during the CGRO-era. COMPTEL, however, does not observe obvious time variability at energies below ~30 MeV contemporaneous to EGRET. In particular, no flare was observed, indicating that this outburst is solely a high-energy (>100 MeV) phenomenon. The energy spectrum between 3 MeV and 10 GeV is well represented by a simple power-law model. Below 3 MeV a spectral turnover is indicated. Performing spectral analysis for different time periods, we found evidence for a spectral hardening during the flaring period, which is consistent with the flare occurring mainly at the higher energies and with its absence at COMPTEL energies of a few MeV. This may be interpreted as an indication that the emission in the EGRET energy range is dominated by a different radiation mechanism than the MeV emission. We argue that the most likely mechanism for the high-energy flare is inverse-Compton scattering of reprocessed accretion-disk radiation.