Fermi Observations of the Very Hard Gamma-ray Blazar PG 1553+113

TL;DR

This study presents the first detailed GeV gamma-ray analysis of blazar PG 1553+113 using Fermi data, revealing its spectral properties, broadband SED, and an upper limit on its redshift based on EBL absorption modeling.

Contribution

It provides the first detailed GeV gamma-ray spectral analysis of PG 1553+113 and constrains its redshift using EBL absorption models.

Findings

PG 1553+113 is a steady, hard-spectrum gamma-ray source.

A simple synchrotron self-Compton model fits its broadband SED.

An upper limit on the redshift of PG 1553+113 is derived from EBL absorption.

Abstract

We report the observations of PG 1553+113 during the first ~200 days of Fermi Gamma-ray Space Telescope science operations, from 4 August 2008 to 22 February 2009 (MJD 54682.7-54884.2). This is the first detailed study of PG 1553+113 in the GeV gamma-ray regime and it allows us to fill a gap of three decades in energy in its spectral energy distribution. We find PG 1553+113 to be a steady source with a hard spectrum that is best fit by a simple power-law in the Fermi energy band. We combine the Fermi data with archival radio, optical, X-ray and very high energy (VHE) gamma-ray data to model its broadband spectral energy distribution and find that a simple, one-zone synchrotron self-Compton model provides a reasonable fit. PG 1553+113 has the softest VHE spectrum of all sources detected in that regime and, out of those with significant detections across the Fermi energy bandpass so far, the hardest spectrum in that energy regime. Thus, it has the largest spectral break of any gamma-ray source studied to date, which could be due to the absorption of the intrinsic gamma-ray spectrum by the extragalactic background light (EBL). Assuming this to be the case, we selected a model with a low level of EBL and used it to absorb the power-law spectrum from PG 1553+113 measured with Fermi (200 MeV - 157 GeV) to find the redshift which gave the best fit to the measured VHE data (90 GeV - 1.1 TeV) for this parameterisation of the EBL. We show that this redshift can be considered an upper limit on the distance to PG 1553+113.