Abridged : The various IBIS/ISGRI catalogues contain a large population of hard X-ray sources whose nature is still unknown. Even if the $>20$ keV positional uncertainty provided by ISGRI is unprecedented, it is still too large to pinpoint the counterpart at other wavelengths, which is the only secure way of obtaining a source identification. We continue the work of trying to reveal the nature of these hard X-ray sources, starting with analysis of X-ray data collected via focusing X-ray telescopes, in order to obtain arcsec accurate X-ray positions. We can then identify counterparts at infrared and optical wavelengths and try to unveil the nature of the sources. We analysed data from observations of 13 \integral\ sources made with the \swift\ satellite. The X-ray images obtained by the X-Ray Telescope instrument allowed us to find possible counterparts to the IGR sources with a positional accuracy of a few arcsec. We then browsed the online catalogues to search for counterparts at other wavelengths. We also made use of the X-ray spectral parameters in trying to identify the nature of those objects. For the 13 objects, we found possible counterparts at X-ray energies and identified the IR/optical and/or UV counterparts as seen with \swift/UVOT. We also discuss the likelihood of association of the X-ray and \integral\ source in each case.
Deep Dive into Swift follow-up of 13 INTEGRAL sources.
Abridged : The various IBIS/ISGRI catalogues contain a large population of hard X-ray sources whose nature is still unknown. Even if the $>20$ keV positional uncertainty provided by ISGRI is unprecedented, it is still too large to pinpoint the counterpart at other wavelengths, which is the only secure way of obtaining a source identification. We continue the work of trying to reveal the nature of these hard X-ray sources, starting with analysis of X-ray data collected via focusing X-ray telescopes, in order to obtain arcsec accurate X-ray positions. We can then identify counterparts at infrared and optical wavelengths and try to unveil the nature of the sources. We analysed data from observations of 13 \integral\ sources made with the \swift\ satellite. The X-ray images obtained by the X-Ray Telescope instrument allowed us to find possible counterparts to the IGR sources with a positional accuracy of a few arcsec. We then browsed the online catalogues to search for counterparts at othe
arXiv:1003.3741v2 [astro-ph.HE] 8 Apr 2010
Astronomy & Astrophysics manuscript no. ms
c⃝ESO 2021
November 13, 2021
Swift follow-up observations of 13 INTEGRAL sources
J. Rodriguez1, J.A. Tomsick2, and A. Bodaghee2
1 Laboratoire AIM, CEA/IRFU - CNRS/INSU - Universit´e Paris Diderot, CEA DSM/IRFU/SAp, Centre de Saclay, F-91191 Gif-sur-
Yvette, France
e-mail: jrodriguez@cea.fr
2 Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA
ABSTRACT
The various IBIS/ISGRI catalogues contain a large population of hard X-ray sources whose nature is still unknown. Even if the > 20
keV positional uncertainty provided by ISGRI is unprecedented, it is still too large to pinpoint the counterpart at other wavelengths,
which is the only secure way of obtaining a source identification. We continue the work of trying to reveal the nature of these hard
X-ray sources, starting with analysis of X-ray data collected via focusing X-ray telescopes, in order to obtain arcsec accurate X-ray
positions. We can then identify counterparts at infrared and optical wavelengths and try to unveil the nature of the sources. We analysed
data from observations of 13 INTEGRAL sources made with the Swift satellite. The X-ray images obtained by the X-Ray Telescope
instrument allowed us to find possible counterparts to the IGR sources with a positional accuracy of a few arcsec. We then browsed
the online catalogues (e.g., NED, SIMBAD, 2MASS, 2MASX, USNO B1.0) to search for counterparts at other wavelengths. We also
made use of the X-ray spectral parameters in trying to identify the nature of those objects. For the 13 objects, we found possible
counterparts at X-ray energies and identified the IR/optical and/or UV counterparts as seen with Swift/UVOT. We also discuss the
likelihood of association of the X-ray and INTEGRAL source in each case. We confirm the previously proposed classification of
IGR J02524−0829 (Sey 2 AGN), J08023−6954 (RS CVn star), and J11457−1827 (Sey 1 AGN). For 7 of these sources we give the
first identification of their nature: IGR J02086−1742, J12060+3818, J12070+2535, J13042−1020, and J13412+3022 are AGN, and
J14488−5942 is a probable X-ray binary. For J03184−0014, although we question the association of the IGR and Swift sources, we
classify the latter as an AGN. We suggest that IGR J15283−4443 is a Galactic source, but we cannot classify the source further.
Finally, we question the association of IGR J11457−1827 and J23130+8608 with the X-ray sources we found, and go on to question
the genuineness of the former IGR source.
Key words. Astrometry — binaries:close — Galaxies: Seyfert — X-rays: binaries — X-rays: galaxies—
1. Introduction
The most recent version of the IBIS catalogue contains more
than 700 hard X-ray sources (Bird et al. 2010). While a certain
number were known as (hard) X-ray emitters prior to the launch
of INTEGRAL, about half of them have been detected for the
first time above 20 keV with IBIS/ISGRI (Lebrun et al. 2003).
In this paper we refer to these sources as ‘IGRs’1. Bodaghee
et al. (2007) has collected known parameters (e.g., the absorption
column density, NH, the pulse period for Galactic sources with
X-ray pulsations, the redshift for AGN, etc.) of all sources de-
tected by INTEGRAL during the first four years of activity. With
this they could study the parameter spaces occupied by different
families of sources and therefore deduce important aspects of the
physics of high-energy sources. However, many of these IGRs
have still not been identified, and therefore any attempt to study,
understand, and model populations of high-energy sources will
be incomplete. The determination of the nature of these object
is therefore extremely important if one wants to have the most
complete view of the content of our Galaxy and our Universe.
In this paper, we continue our work of identifying the un-
known IGRs that we started soon after the discovery of the first
IGRs. A first step is to provide an ∼arcsec position with soft
X-ray telescopes such as XMM-Newton (Rodriguez et al. 2003,
Send offprint requests to: J. Rodriguez
1 An up-to-date online catalogue of all IGRs can be found at
http://irfu.cea.fr/Sap/IGR-Sources/ note the new address for the site
2006; Bodaghee et al. 2006) Chandra (Tomsick et al. 2006,
2008, 2009), and also Swift (Rodriguez et al. 2008, 2009b,a).
We then search for counterparts at a position consistent with the
refined X-ray position of a given source. As in Rodriguez et al.
(2008) and Rodriguez et al. (2009b) (Papers 1 and 2 in the re-
mainder of this article), we report here the analysis of Swift ob-
servations (XRT imaging and spectral analysis and UVOT imag-
ing) of 13 IGRs that still lacked precise arcsec X-ray positions at
the time of the writing of the paper. We also present the identi-
fication of IR and optical counterparts obtained from online cat-
alogues such as SIMBAD, the United States Naval Observatory
(USNO), the 2 Micron All Sky Survey point source and ex
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