The faint "heartbeats" of IGR J17091-3624: an exceptional black-hole candidate

TL;DR

This study analyzes 180 days of RXTE data on IGR J17091-3624, revealing complex variability patterns similar to GRS 1915+105 but at much lower luminosities, challenging existing models of black hole variability.

Contribution

First detailed characterization of IGR J17091-3624's variability patterns, comparing them with GRS 1915+105 and discussing implications for black hole models.

Findings

IGR J17091-3624 exhibits multiple variability classes similar to GRS 1915+105.

The source's luminosity during variability is 10-50 times lower than GRS 1915+105.

The 'heartbeats' occur with periods from a few seconds to ~100 seconds.

Abstract

We report on the first 180 days of RXTE observations of the outburst of the black hole candidate IGR J17091-3624. This source exhibits a broad variety of complex light curve patterns including periods of strong flares alternating with quiet intervals. Similar patterns in the X-ray light curves have been seen in the (up to now) unique black hole system GRS 1915+105. In the context of the variability classes defined by Belloni et al. (2000) for GRS 1915+105, we find that IGR J17091-3624 shows the \nu, \rho, \alpha, \lambda, \beta and \mu classes as well as quiet periods which resemble the \chi class, all occurring at 2-60 keV count rate levels which can be 10-50 times lower than observed in GRS 1915+105. The so-called \rho class "heartbeats" occur as fast as every few seconds and as slow as ~100 seconds, tracing a loop in the hardness-intensity diagram which resembles that previously seen in GRS 1915+105. However, while GRS 1915+105 traverses this loop clockwise, IGR J17091-3624 does so in the opposite sense. We briefly discuss our findings in the context of the models proposed for GRS 1915+105 and find that either all models requiring near Eddington luminosities for GRS 1915+105-like variability fail, or IGR J17091-3624 lies at a distance well in excess of 20 kpc or, it harbors one of the least massive black holes known (< 3 M_sun).