Temporal properties of GX 301-2 over a year-long observation with SuperAGILE

TL;DR

This study provides a comprehensive year-long analysis of GX 301-2's X-ray emission, revealing orbital modulation, spectral hardness variations, and pulse profile changes, enhancing understanding of its accretion processes and timing behavior.

Contribution

First long-term, continuous hard X-ray monitoring of GX 301-2 with SuperAGILE, detailing spectral, timing, and pulse profile variations over an entire orbital cycle.

Findings

Orbital modulation of spectral hardness peaks at pre-periastron and phase 0.25.

Secular trend of the 680 s pulse period is consistent with previous data.

Pulsed fraction is strongly anti-correlated with source intensity.

Abstract

We present the long-term monitoring of the High Mass X-ray Binary GX 301-2 performed with the SuperAGILE instrument on-board the AGILE mission. The source was monitored in the 20-60 keV energy band during the first year of the mission from 2007 July 17 to 2008 August 31, covering about one whole orbital period and three more pre-periastron passages for a total net observation time of about 3.7 Ms. The SuperAGILE dataset represents one of the most continuous and complete monitoring at hard X-ray energies of the 41.5 day long binary period available to date. The source behavior was characterized at all orbital phases in terms of hard X-ray flux, spectral hardness, spin period history, pulsed fraction and pulse shape profile. We also complemented the SuperAGILE observations with the soft X-ray data of the RossiXTE/ASM. Our analysis shows a clear orbital modulation of the spectral hardness, with peaks in correspondence with the pre-periastron flare and near phase 0.25. The hardness peaks we found could be related with the wind-plus-stream accretion model proposed in order to explain the orbital light curve modulation of GX 301-2. Timing analysis of the pulsar spin period shows that the secular trend of the about 680 s pulse period is consistent with the previous observations, although there is evidence of a slight decrease in the spin-down rate. The analysis of the hard X-ray pulsed emission also showed a variable pulse shape profile as a function of the orbital phase, with substructures detected near the passage at the periastron, and a clear modulation of the pulsed fraction, which appears in turn strongly anti-correlated with the source intensity.