The colour of the Deep ROSAT X-ray sky fluctuations

• Main Authors: Ceballos, M. Teresa, Barcons, Xavier, Carrera, Francisco J, .
• Format: Journal Article
• Language: English
• Published: 05.11.1996
• Subjects: Physics - Astrophysics of Galaxies; Physics - Cosmology and Nongalactic Astrophysics; Physics - Earth and Planetary Astrophysics; Physics - High Energy Astrophysical Phenomena; Physics - Instrumentation and Methods for Astrophysics; Physics - Solar and Stellar Astrophysics
• DOI: 10.48550/arxiv.astro-ph/9611029

We have carried out a fluctuation analysis in four bands (R4, R5, R6 and R7 corresponding to 0.44-1.01 keV, 0.56-1.21 keV, 0.73-1.56 keV and to 1.05-2.04 keV respectively) of two very deep ROSAT PSPC observations in directions where the galactic H{\small I} column is minimal. This has enabled us to study the average spectrum of the sources contributing to 0.5-2 keV fluxes $\sim 10^{-15} \rm \ergpcmsqps$. The best fit spectral energy index for the average faint source spectrum, $\alpha=0.95^{+0.10}_{-0.15}$, is still steeper than the one measured for the extragalactic XRB at these energies $\alpha\sim 0.4-0.7$, but flatter than the typical AGN spectral index $\alpha\sim 1-1.5$. This result has allowed us to constrain the existence of a population of sources harder than the AGNs contributing to the source counts at these fluxes. We find that a population of X-ray sources with energy spectral index $\alpha\sim 0.4-0.6$ would contribute $(30\pm 20)$ per cent to the source counts at these fluxes if the rest of them are AGNs with energy spectral index $\alpha\sim 1.2$.