Deep and Monitoring Observations of the Black Hole Candidates 1E 1740.7-2942 and GRS 1758-258

Details Deep and Monitoring Observations of the Black Hole Candidates 1E 1740.7-2942 and GRS 1758-258 Deep and Monitoring Observations of the Black Hole Candidates 1E 1740.7-2942 and GRS 1758-258

Jun 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998ucsd.reptq....h&link_type=abstract

Technical Report, NASA/CR-1998-208052; NAS 1.26:208052

Astronomy and Astrophysics

Astronomy

Black Holes (Astronomy), Monitors, Variability, Power Spectra, Energy Spectra, X Ray Timing Explorer, X Ray Sources, Time Measurement, Targets, Stability, Quasars, Luminosity, Actuators

Scientific paper

The purpose of this effort was to obtain detailed information on the long term variability of the power spectra and energy spectra of the two Black Hole Candidates (BHCs) and so-called "micro-quasars", 1E 1740.7-2942 and GRS 1758-258. Observations with the pointed instruments on the Rossi X-ray Timing Explorer (RXTE) were carried out on a weekly basis for an entire year, in order to observe the extent to which these sources changed on long timescales. The observations also served as a trigger for longer observations carried out under a sister proposal "Target of Opportunity Observations of the Black Hole Candidates 1E 1740.7-2942 and GRS 1758-258". The work done at UCSD by W. Heindl consisted first of monitoring the data from the High Energy X-ray Timing Experiment (HEXTE) to determine when the sources were bright enough to trigger our Target of Opportunity observations. He was then responsible for the reduction and interpretation of the HEXTE data and for contributing to the publication of results of this work. Historically, these objects have been highly variable on long timescales. Observations between 1988 and 1995 found that they tend to spend periods of several months in high and low flux states which differ in luminosity by more than an order of magnitude. In more than 2 years of RXTE observations to date, we have found variability only on the level of tens of percent. Both sources have remained near their historical maximum luminosities during this time. This is a significant change from previous behavior, and indicates that their accretion rates have stabilized in recent years. In addition, their observed spectra have been quite stable.

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