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  Current Research Highlight :: February 2004 all highlights

RXTE 3-20 keV all sky survey,
Statistical properties of local AGNs

Researchers at the Max-Planck Institute for Astrophysics have performed a new all-sky X-ray survey using the RXTE observatory. The results of this survey in particular improve our knowledge of the properties of the local AGN population.



Fig. 1: Rossi X-ray Timing Explorer observatory



Fig. 2: Image of the X-ray (3-20 keV) sky obtained with the RXTE/PCA slew survey.





Fig. 3: Distribution of X-ray volume emissivity between AGNs of various luminosities and absorption columns.



Fig. 4: Intrinsic absorption distribution of low and high luminosity AGNs.

At energies higher than 2-5 keV the X-ray illumination of Earth is dominated by tens of millions of extragalactic sources that make up the Cosmic X-ray Background (CXB). The main contributors to the CXB are active galactic nuclei (AGNs). AGNs fill almost the entire volume of the Universe, approximately tracing the matter density distribution. Deep surveys such as those performed recently with the CHANDRA and XMM-Newton observatories can efficiently probe the distant Universe (out to a redshift ~4), but tell us very little about our local environment because such surveys cover only a tiny fraction of the sky. In order to study the local population of extragalactic sources all-sky surveys are needed. The last such survey at energies above >2 keV was carried out more than 20 years ago by the HEAO 1 observatory. With the help of the RXTE observatory researchers at the Max-Planck Institute for Astrophysics have now performed a new all-sky X-ray survey.

The RXTE observatory (Fig.1) was launched at the end of 1995 and has been successfully operating in orbit since then. Its main instruments PCA and HEXTE are collimated spectrometers designed to observe X-ray point sources while the observatory is oriented toward them. We took advantage of the excellent calibration, moderate field of view (1 deg radius) and high effective area (~6400 sq. cm) of the PCA instrument to construct a map of the whole sky in the 3-20 keV band (Fig. 2) from the data accumulated during reorientations (slews) of the observatory from one target to another.

During the period 1996-2003 slew observations covered almost the whole sky with a total exposure of ~20 million sec. For most of the sky a flux limit of 0.9 mCrab (2-10 keV) or better has been achieved, which is better than and comparable to that of the HEAO1/A2 and HEAO1/A1 surveys, respectively. In addition, approximately 20% of the sky have been covered with a much higher sensitivity of 0.3 mCrab. Furthemore, our survey extends into the energy range 10-20 keV, surpassing by an order of magnitude the sensitivity of the previous hard X-ray survey done with the HEAO 1/A4 experiment.

As a result of the analysis of the all-sky map, a total of 294 X-ray sources have been detected and localized to better than 1 deg. 236 of them can be confidently associated with a single known astrophysical object, including 63 sources located within the Milky Way, LMC or SMC, 64 clusters of galaxies and 100 AGNs. 35 of the detected sources remain unidentified, and because their observed X-ray spectra are hard we believe that many of them are AGNs, including highly obscured ones undetectable by soft X-ray telescopes.

Using the sample of detected sources, we have constructed the best-to-date X-ray luminosity function of local (at redshift below 0.1) AGNs. It turns out that relatively weak AGNs with a large degree of circumnuclear obscuration, which were largely missed by previous all-sky surveys, dominate in the X-ray output of the local Universe (Fig.3). In addition to that our analysis has revealed that the ratio of obscured objects to unobscured ones strongly changes with the AGN luminosity, from 2:1 for low-luminosity AGNs (L_X < 10^43.5 erg/s) to less than 1:5 for high-luminosity ones. This behavior is illustrated in Fig. 4.

Mikhail Revnivtsev, Sergey Sazonov, Marat Gilfanov

References:
Revnivtsev M., Sazonov S., Jahoda K., Gilfanov M. 2004, A&A submitted
Sazonov S., Revnivtsev M. 2004, A&A submitted


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