Performance of Large Area X-ray Proportional Counters in a Balloon Experiment

TL;DR

This paper reports on a balloon experiment testing the performance of Large Area X-ray Proportional Counters (LAXPCs), designed for the ASTROSAT satellite, focusing on their calibration, background rates, and observations of Cygnus X-1 in the 3-80 keV range.

Contribution

It presents the design, calibration, and testing of prototype LAXPC detectors in a balloon experiment, demonstrating their capabilities for X-ray timing and spectral studies.

Findings

LAXPC detectors operated successfully at high altitude.

Background counting rates were characterized across energy bands.

Cyg X-1 was observed with measurable intensity variations.

Abstract

ASTROSAT is India's first satellite fully devoted to astronomical observations covering a wide spectral band from optical to hard X-rays by a complement of 4 co-aligned instruments and a Scanning Sky X-ray Monitor. One of the instruments is Large Area X-ray Proportional Counter with 3 identical detectors. In order to assess the performance of this instrument, a balloon experiment with two prototype Large Area X-ray Proportional Counters (LAXPC) was carried out on 2008 April 14. The design of these LAXPCs was similar to those on the ASTROSAT except that their field of view (FOV) was 3$^{\circ}$ $\times$ 3$^{\circ}$ versus FOV of 1$^{\circ}$ $\times$ 1$^{\circ}$ for the LAXPCs on the ASTROSAT. The LAXPCs are aimed at the timing and spectral studies of X-ray sources in 3-80 keV region. In the balloon experiment, the LAXPC, associated electronics and support systems were mounted on an oriented platform which could be pre-programmed to track any source in the sky. A brief description of the LAXPC design, laboratory tests, calibration and the detector characteristics is presented here. The details of the experiment and background counting rates of the 2 LAXPCs at the float altitude of about 41 km are presented in different energy bands. The bright black hole X-ray binary Cygnus X-1 (Cyg X-1) was observed in the experiment for $\sim$ 3 hours. Details of Cyg X-1 observations, count rates measured from it in different energy intervals and the intensity variations of Cyg X-1 detected during the observations are presented and briefly discussed.