| INTEGRALPlanckGaiaPOLARCHEOPSEuclidATHENA |
| HEAVENSFACTCTALOFTSPICAJEM-EUSOXIPEeXTPTheseus |
| XRISMMAGBOUNDSMARTNet |
| ISDCCDCI |
| Data Centre for Astrophysics Astronomy Department of the University of Geneva |
AX J1910.7+0917 and three newly discovered INTEGRAL sources
| We investigated the nature of the still poorly known X-ray source AX J1910.7+0917 and searched for closeby previously undetected objects, making use of the high sensitivity of the IBIS/ISGRI telescope and the improvements in the data analysis software. We analyzed all publicly available data from INTEGRAL, XMM-Newton, Chandra and ASCA and we discussed the different possibilities for the nature of AX J1910.7+0917. In the IBIS/ISGRI field-of-view around AX J1910.7+0917, we discovered three new sources: IGR J19173+0747, IGR J19294+1327 and IGR J19149+1036. For two of them we report the results of follow-up observations carried out with Swift/XRT. |
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ABSTRACT
Aims. We take advantage of the high sensitivity of the IBIS/ISGRI telescope and the improvements in the data analysis software to investigate the nature of the still poorly known X-ray source AX J1910.7+0917, and search for closeby previously undetected objects.
Methods. We analyze all publicly available INTEGRAL data of AX J1910.7+0917, together with a number of archival observations that were carried out in the direction of the source with Chandra, XMM-Newton, and ASCA. In the IBIS/ISGRI field-of-view around AX J1910.7+0917, we discovered three new sources: IGR J19173+0747, IGR J19294+1327 and IGR J19149+1036; the latter is positionally coincident with the Einstein source 2E 1912.5+1031. For the first two sources, we also report the results of follow-up observations carried out with Swift /XRT.
Results. AX J1910.7+0917 features a clear variability in the X-rays. Its spectrum can be well described with an absorbed (NH∼6×1022 cm−2) power-law (Γ≃1.5) model plus an iron line at 6.4 keV. We also obtained a refined position and report on possible infrared counterparts.
Conclusions. The present data do not allow for a unique classification of the sources. Based on the property of its X-ray emission and the analysis of a likely infrared counterpart, we investigate different possibilities for the nature of AX J1910.7+0917.
Methods. We analyze all publicly available INTEGRAL data of AX J1910.7+0917, together with a number of archival observations that were carried out in the direction of the source with Chandra, XMM-Newton, and ASCA. In the IBIS/ISGRI field-of-view around AX J1910.7+0917, we discovered three new sources: IGR J19173+0747, IGR J19294+1327 and IGR J19149+1036; the latter is positionally coincident with the Einstein source 2E 1912.5+1031. For the first two sources, we also report the results of follow-up observations carried out with Swift /XRT.
Results. AX J1910.7+0917 features a clear variability in the X-rays. Its spectrum can be well described with an absorbed (NH∼6×1022 cm−2) power-law (Γ≃1.5) model plus an iron line at 6.4 keV. We also obtained a refined position and report on possible infrared counterparts.
Conclusions. The present data do not allow for a unique classification of the sources. Based on the property of its X-ray emission and the analysis of a likely infrared counterpart, we investigate different possibilities for the nature of AX J1910.7+0917.
Newly discovered INTEGRAL source IGRJ19173+0747 observed with Swift/XRT.Only one soft X-ray source is found in Swift/XRT (left) within the ISGRI error circle. A positionally coincident ROSAT source is also shown. The 2MASS infrared image (J band, on the right) is shown together with the Swift/XRT error circle and the position of the IR and optical counterpart. Credits: ISDC/E.Bozzo |
IBIS/ISGRI mosaic around AX J1910.7+0917Significance map obtained in the 17-80 keV range. The dashed grids denote galactic coordinates. Together with AX J1910.7+0917, the three newly discovered sources are shown: IGR J19173+0747 , IGR J19294+1327, IGR J19149+1036. Credits: ISDC/R.Walter |
XMM-Newton Epic-pn spectrum of AX J1910.7+0917The data are shown together with the best-fit model (an absorbed power-law) and the residuals from the fit. The residuals clearly show an iron line at ∼6.4 keV. Credits: ISDC/E.Bozzo |
| by Lucia Pavan on 2011-01-11 | >> INTEGRAL science results | >> All science results |
