Following the discovery of IGR J17177-3656 (Frankowski et al. 2011, ATel #3223) on 2011-03-15, we requested a Swift ToO, which was executed on 2011-03-16 from 18:39:24 to 20:41:01 UT with a total exposure of ~3.9 ks. 2266 photons have been extracted from the source region between 0.2 and 10 keV, corresponding to a net count rate of ~0.59 cts/s. Using the online Swift tool we find an enhanced position of RA = 259.428 (17h17m43s), Dec = -36.934 deg (-36:56:03s) (J2000), with a 90% confidence level error of 2.1 arcsec, consistent with the position measurements made by IBIS/ISGRI and JEM-X (ATel #3223)

Beckmann, V.

Bozzo, E.

Caballero, I.

Cadolle Bel, M.

Capitanio, F.

Chen, Y.P.

Del Santo, M.

Drave, S.P.

Ferrigno, C.

Frankowski, a.

Hadasch, D.

Hartog, P.R.

Jonker, P.

Kretschmar, P.

Kreykenbohm, I.

Kuiper, L.

Kuulkers, E.

Li, J.

Migliari, S.

Natalucci, L.

Pottschmidt, K.

Puehlhofer, G.

Rea, N.

Rodriguez, J.

Sanchez-Fernandez, C.

Sguera, V.

Torres, D.F.

Wang, J.M.

Watanabe, K.

Wijnands, R.

Zhang, S.

Zhang, S.N.

English

Frankowski, A.

UvA-DARE

Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rays

NARCIS 

International Migration, Integration and Social Cohesion online publications

UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl)UvA-DARE (Digital Academic Repository)Swift/XRT follow-up observation on IGR J17177-3656 at soft X-raysZhang, S.; Chen, Y.P.; Li, J.; Wang, J.M.; Zhang, S.N.; Torres, D.F.; Hadasch, D.; Rea, N.;Sanchez-Fernandez, C.; Kuulkers, E.; Cadolle Bel, M.; Kretschmar, P.; Ferrigno, C.; Bozzo,E.; Caballero, I.; Rodriguez, J.; Beckmann, V.; Jonker, P.; Kuiper, L.; Pottschmidt, K.; Migliari,S.; Capitanio, F.; Natalucci, L.; Del Santo, M.; Watanabe, K.; Wijnands, R. ; Drave, S.P.;Hartog, P.R.; Kreykenbohm, I.; Puehlhofer, G.; Sguera, V.; Frankowski, A.Publication date2011Document VersionFinal published versionPublished inThe astronomer's telegramLicenseUnspecifiedLink to publicationCitation for published version (APA):Zhang, S., Chen, Y. P., Li, J., Wang, J. M., Zhang, S. N., Torres, D. F., Hadasch, D., Rea, N.,Sanchez-Fernandez, C., Kuulkers, E., Cadolle Bel, M., Kretschmar, P., Ferrigno, C., Bozzo,E., Caballero, I., Rodriguez, J., Beckmann, V., Jonker, P., Kuiper, L., ... Frankowski, A.(2011). Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rays. Theastronomer's telegram. https://www.astronomerstelegram.org/?read=3226General rightsIt is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s)and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an opencontent license (like Creative Commons).Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, pleaselet the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the materialinaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letterto: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. Youwill be contacted as soon as possible.Download date:09 Mar 2023ATel #3226: Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rayshttps://www.astronomerstelegram.org/?read=3226[14-10-2022 15:17:28]OutsideGCNIAUCs ATel on TwitterPatreonPost | Search | PoliciesCredential | Feeds | Email14 Oct 2022; 13:17 UTThis space for free for your conference.[ Previous | Next | ADS  ]Swift/XRT follow-up observation on IGR J17177-3656 atsoft X-raysATel #3226; S. Zhang, Y. P. Chen, J. Li, J. M. Wang, S. N. Zhang (IHEP, China), D. F.Torres, D. Hadasch, N. Rea (IEEC-CSIC, Spain), C. Sanchez-Fernandez, E.Kuulkers, M. Cadolle Bel, P. Kretschmar (ESA/ESAC, Spain), C. Ferrigno, E. Bozzo(ISDC, Switzerland), I. Caballero, J. Rodriguez(CEA-AIM, France), V. Beckmann(APC, France), P. Jonker, L. Kuiper (SRON, The Netherlands), K. Pottschmidt(Cresst/UMBC/GSFC, USA), S. Migliari (Univ. of Barcelona, Spain), F. Capitanio, L.Natalucci, M. Del Santo (INAF/IASF-Roma, Italy), K. Watanabe (Florida Gulf CoastUniv., USA), R. Wijnands (Univ. of Amsterdam, The Netherlands), S. P. Drave(Univ. of Southampton, UK), P. R. Hartog (Stanford Univ. HEPL-KIPAC, USA), I.Kreykenbohm (ECAP, Germany), G. Puehlhofer (IAAT, Germany), V. Sguera(INAF/IASF-Bo, Italy), A. Frankowski (CAMK Warsaw, Poland & ISDC, Switzerland)on 18 Mar 2011; 14:08 UTCredential Certification: Shu Zhang (szhang@mail.ihep.ac.cn)Subjects: X-ray, TransientReferred to by ATel #: 3236, 3241, 3275TweetFollowing the discovery of IGR J17177-3656 (Frankowski et al. 2011, ATel #3223) on2011-03-15, we requested a Swift ToO, which was executed on 2011-03-16 from18:39:24 to 20:41:01 UT with a total exposure of ~3.9 ks.2266 photons have been extracted from the source region between 0.2 and 10 keV,corresponding to a net count rate of ~0.59 cts/s. Using the online Swift tool we find anenhanced position of RA = 259.428 (17h17m43s), Dec = -36.934 deg (-36:56:03s)(J2000), with a 90% confidence level error of 2.1 arcsec, consistent with the positionmeasurements made by IBIS/ISGRI and JEM-X (ATel #3223). The angular separation ofthe proposed optical counterpart by Malizia et al. (ATel #3224) from the XRT position is2 arcmin, and the association is therefore ruled out.The XRT spectrum can be reasonably well fitted (reduced chi2=1.37 for 68 dof) with anabsorbed power-law model. The spectral parameters we derive in the 0.2-9 keV energyband are: N_H = 3.7+/-0.5 e22 atoms/cm2 and photon index = 1.45+/-0.20. The 1-10keV unabsorbed flux is 1.0e-10 erg/cm2/s. Splitting this observation into two parts showsRelated3275 VVV near-infraredobservations of the IGRJ17177-3656 field3247 Correction to ATel #3246: Aradio counterpart to IGRJ17177-3656 discovered bythe ATCA3246 Radio emission from IGRJ17091-3624 observed withthe ATCA3241 On the infrared counterpart toIGR J17177-36563236 A Chandra observation of IGRJ17177-36563226 Swift/XRT follow-upobservation on IGR J17177-3656 at soft X-rays3224 POSSIBLE COUNTERPARTOF THE NEW INTEGRALTRANSIENT SOURCE IGRJ17177-36563223 INTEGRAL discovery of a newhard X-ray transient: IGRJ17177-3656ATel #3226: Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rayshttps://www.astronomerstelegram.org/?read=3226[14-10-2022 15:17:28]consistent spectral parameters within 1 sigma errors, indicative of a lack of significantvariability on time scales of two hours.A combined Swift/XRT and INTEGRAL/IBIS/ISGRI (latter obtained the previous day, seeATel #3223) spectral fit with an absorbed power-law model yielded: N_H = (3.9 +0.5-0.4) e22 atoms/cm2 and photon index = 1.5+/-0.2, with a reduced chi2 of 1.30 for 76dof. The 1-200 keV unabsorbed flux is 7.8e-10 erg/cm2/s. We notice that the absorptionis larger than the Galactic column density (1.3e22 atoms/cm2 as estimated at the sourceposition by using the tool available at the HEASARC website, Kalberla et al. 2005), andhence indicates additional absorption intrinsic to the source.We performed a search through the VizieR database and there is only one match withinthe 2.1 arcsec 90% confidence level: 2MASS J17174269-3656039. This star has J, Hand K magnitudes of 15.2, 13.9 and 12.9, respectively, and is located at about 1.3arcsec from the Swift position. The 2MASS source is also present in the NOMAD andGLIMPSE catalogs, with very similar magnitudes. Although this is the only source in theSwift error circle it is by no means certain that this is the counterpart; uncertainties in theN_H make the determined intrinsic near-infra-red colours inaccurate.There is also a radio source from the 1.4 GHz NRAO VLA Sky Survey (catalog version:2004) with a position consistent with our Swift determined one: NVSS J171743-365606.Its nominal position is about 7 arcsec away from our Swift position, with an error radiusof 12 arcsec, and it is extended with a width of about 100 arcsec (beam width of thesurvey is 45 arcsec). Its measured flux density is 24 +/- 5 mJy.[ Telegram Index ]R. E. Rutledge, Editor-in-ChiefDerek Fox, Editor

UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl)UvA-DARE (Digital Academic Repository)Swift/XRT follow-up observation on IGR J17177-3656 at soft X-raysZhang, S.; Chen, Y.P.; Li, J.; Wang, J.M.; Zhang, S.N.; Torres, D.F.; Hadasch, D.; Rea, N.;Sanchez-Fernandez, C.; Kuulkers, E.; Cadolle Bel, M.; Kretschmar, P.; Ferrigno, C.; Bozzo,E.; Caballero, I.; Rodriguez, J.; Beckmann, V.; Jonker, P.; Kuiper, L.; Pottschmidt, K.; Migliari,S.; Capitanio, F.; Natalucci, L.; Del Santo, M.; Watanabe, K.; Wijnands, R. ; Drave, S.P.;Hartog, P.R.; Kreykenbohm, I.; Puehlhofer, G.; Sguera, V.; Frankowski, a.Publication date2011Document VersionFinal published versionPublished inThe astronomer's telegramLicenseUnspecifiedLink to publicationCitation for published version (APA):Zhang, S., Chen, Y. P., Li, J., Wang, J. M., Zhang, S. N., Torres, D. F., Hadasch, D., Rea, N.,Sanchez-Fernandez, C., Kuulkers, E., Cadolle Bel, M., Kretschmar, P., Ferrigno, C., Bozzo,E., Caballero, I., Rodriguez, J., Beckmann, V., Jonker, P., Kuiper, L., ... Frankowski, A.(2011). Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rays. Theastronomer's telegram. https://www.astronomerstelegram.org/?read=3226General rightsIt is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s)and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an opencontent license (like Creative Commons).Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, pleaselet the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the materialinaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letterto: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. Youwill be contacted as soon as possible.Download date:11 Nov 2022ATel #3226: Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rayshttps://www.astronomerstelegram.org/?read=3226[14-10-2022 15:17:28]OutsideGCNIAUCs ATel on TwitterPatreonPost | Search | PoliciesCredential | Feeds | Email14 Oct 2022; 13:17 UTThis space for free for your conference.[ Previous | Next | ADS  ]Swift/XRT follow-up observation on IGR J17177-3656 atsoft X-raysATel #3226; S. Zhang, Y. P. Chen, J. Li, J. M. Wang, S. N. Zhang (IHEP, China), D. F.Torres, D. Hadasch, N. Rea (IEEC-CSIC, Spain), C. Sanchez-Fernandez, E.Kuulkers, M. Cadolle Bel, P. Kretschmar (ESA/ESAC, Spain), C. Ferrigno, E. Bozzo(ISDC, Switzerland), I. Caballero, J. Rodriguez(CEA-AIM, France), V. Beckmann(APC, France), P. Jonker, L. Kuiper (SRON, The Netherlands), K. Pottschmidt(Cresst/UMBC/GSFC, USA), S. Migliari (Univ. of Barcelona, Spain), F. Capitanio, L.Natalucci, M. Del Santo (INAF/IASF-Roma, Italy), K. Watanabe (Florida Gulf CoastUniv., USA), R. Wijnands (Univ. of Amsterdam, The Netherlands), S. P. Drave(Univ. of Southampton, UK), P. R. Hartog (Stanford Univ. HEPL-KIPAC, USA), I.Kreykenbohm (ECAP, Germany), G. Puehlhofer (IAAT, Germany), V. Sguera(INAF/IASF-Bo, Italy), A. Frankowski (CAMK Warsaw, Poland & ISDC, Switzerland)on 18 Mar 2011; 14:08 UTCredential Certification: Shu Zhang (szhang@mail.ihep.ac.cn)Subjects: X-ray, TransientReferred to by ATel #: 3236, 3241, 3275TweetFollowing the discovery of IGR J17177-3656 (Frankowski et al. 2011, ATel #3223) on2011-03-15, we requested a Swift ToO, which was executed on 2011-03-16 from18:39:24 to 20:41:01 UT with a total exposure of ~3.9 ks.2266 photons have been extracted from the source region between 0.2 and 10 keV,corresponding to a net count rate of ~0.59 cts/s. Using the online Swift tool we find anenhanced position of RA = 259.428 (17h17m43s), Dec = -36.934 deg (-36:56:03s)(J2000), with a 90% confidence level error of 2.1 arcsec, consistent with the positionmeasurements made by IBIS/ISGRI and JEM-X (ATel #3223). The angular separation ofthe proposed optical counterpart by Malizia et al. (ATel #3224) from the XRT position is2 arcmin, and the association is therefore ruled out.The XRT spectrum can be reasonably well fitted (reduced chi2=1.37 for 68 dof) with anabsorbed power-law model. The spectral parameters we derive in the 0.2-9 keV energyband are: N_H = 3.7+/-0.5 e22 atoms/cm2 and photon index = 1.45+/-0.20. The 1-10keV unabsorbed flux is 1.0e-10 erg/cm2/s. Splitting this observation into two parts showsRelated3275 VVV near-infraredobservations of the IGRJ17177-3656 field3247 Correction to ATel #3246: Aradio counterpart to IGRJ17177-3656 discovered bythe ATCA3246 Radio emission from IGRJ17091-3624 observed withthe ATCA3241 On the infrared counterpart toIGR J17177-36563236 A Chandra observation of IGRJ17177-36563226 Swift/XRT follow-upobservation on IGR J17177-3656 at soft X-rays3224 POSSIBLE COUNTERPARTOF THE NEW INTEGRALTRANSIENT SOURCE IGRJ17177-36563223 INTEGRAL discovery of a newhard X-ray transient: IGRJ17177-3656ATel #3226: Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rayshttps://www.astronomerstelegram.org/?read=3226[14-10-2022 15:17:28]consistent spectral parameters within 1 sigma errors, indicative of a lack of significantvariability on time scales of two hours.A combined Swift/XRT and INTEGRAL/IBIS/ISGRI (latter obtained the previous day, seeATel #3223) spectral fit with an absorbed power-law model yielded: N_H = (3.9 +0.5-0.4) e22 atoms/cm2 and photon index = 1.5+/-0.2, with a reduced chi2 of 1.30 for 76dof. The 1-200 keV unabsorbed flux is 7.8e-10 erg/cm2/s. We notice that the absorptionis larger than the Galactic column density (1.3e22 atoms/cm2 as estimated at the sourceposition by using the tool available at the HEASARC website, Kalberla et al. 2005), andhence indicates additional absorption intrinsic to the source.We performed a search through the VizieR database and there is only one match withinthe 2.1 arcsec 90% confidence level: 2MASS J17174269-3656039. This star has J, Hand K magnitudes of 15.2, 13.9 and 12.9, respectively, and is located at about 1.3arcsec from the Swift position. The 2MASS source is also present in the NOMAD andGLIMPSE catalogs, with very similar magnitudes. Although this is the only source in theSwift error circle it is by no means certain that this is the counterpart; uncertainties in theN_H make the determined intrinsic near-infra-red colours inaccurate.There is also a radio source from the 1.4 GHz NRAO VLA Sky Survey (catalog version:2004) with a position consistent with our Swift determined one: NVSS J171743-365606.Its nominal position is about 7 arcsec away from our Swift position, with an error radiusof 12 arcsec, and it is extended with a width of about 100 arcsec (beam width of thesurvey is 45 arcsec). Its measured flux density is 24 +/- 5 mJy.[ Telegram Index ]R. E. Rutledge, Editor-in-ChiefDerek Fox, Editor

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Swift/XRT follow-up observation on IGR J17177-3656 at soft X-rays

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International Migration, Integration and Social Cohesion online publications