TY - JOUR
T1 - A newly discovered double-double candidate microquasar in NGC 300
AU - Urquhart, R.
AU - Soria, R.
AU - Pakull, M. W.
AU - Miller-Jones, J. C.A.
AU - Anderson, G. E.
AU - Plotkin, R. M.
AU - Motch, C.
AU - Maccarone, T. J.
AU - McLeod, A. F.
AU - Scaringi, S.
N1 - Funding Information:
We thank William Blair, Jifeng Liu, Vlad Tudor, and Sam Mc-Sweeney for useful discussions. We also thank the anonymous referee whose constructive feedback helped to improve this paper. RU acknowledges that this research is supported by an Australian Government Research Training Program (RTP) Scholarship. RS acknowledges support from a Curtin University Senior Research Fellowship; he is also grateful for support, discussions, and hospitality at the Strasbourg Observatory during part of this work. JCAM-J is the recipient of an Australian Research Council Fu- ture Fellowship (FT140101082). GEA is the recipient of an Australian Research Council Discovery Early Career Researcher Award (project number DE180100346) funded by the Australian Government. RMP acknowledges support from Curtin University through the Peter Curran Memorial Fellowship. The International Centre for Radio Astronomy Research is a joint venture between Curtin University and the University of Western Australia, funded by the state government of Western Australia and the joint venture partners. The scientific results reported in this article are based on data obtained from the Chandra Data Archive. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO. Based on observations made with the NASA/ESA HST, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 10915. IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https: //www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The ATCA is part of the Australia Telescope National Facility that is funded by the Australian Government for operation as a National Facility managed by CSIRO. This research has made use of NASA’s Astrophysics Data System.
Funding Information:
We thank William Blair, Jifeng Liu, Vlad Tudor, and Sam Mc-Sweeney for useful discussions. We also thank the anonymous referee whose constructive feedback helped to improve this paper. RU acknowledges that this research is supported by an Australian Government Research Training Program (RTP) Scholarship. RS acknowledges support from a Curtin University Senior Research Fellowship; he is also grateful for support, discussions, and hospitality at the Strasbourg Observatory during part of this work. JCAM-J is the recipient of an Australian Research Council Future Fellowship (FT140101082). GEA is the recipient of an Australian Research Council Discovery Early Career Researcher Award (project number DE180100346) funded by the Australian Government. RMP acknowledges support from Curtin University through the Peter Curran Memorial Fellowship. The International Centre for Radio Astronomy Research is a joint venture between Curtin University and the University of Western Australia, funded by the state government of Western Australia and the joint venture partners. The scientific results reported in this article are based on data obtained from the Chandra Data Archive. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO. Based on observations made with the NASA/ESA HST, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 10915. IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https: //www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The ATCA is part of the Australia Telescope National Facility that is funded by the Australian Government for operation as a National Facility managed by CSIRO. This research has made use of NASA's Astrophysics Data System.
Publisher Copyright:
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2019/1/11
Y1 - 2019/1/11
N2 - We present the discovery of a powerful candidate microquasar in NGC 300, associated with the S 10 optical nebula (previously classified as a supernova remnant). Chandra images show four discrete X-ray knots aligned in the plane of the sky over a length of ≈150 pc. The X-ray emission from the knots is well fitted with a thermal plasma model at a temperature of ≈0.6 keV and a combined 0.3-8 keV luminosity of ≈1037 erg s−1. The X-ray core, if present at all, does not stand out above the thermal emission of the knots: this suggests that the accreting compact object is either currently in a dim state or occulted from our view. We interpret the emission from the knots as the result of shocks from the interaction of a jet with the interstellar medium (possibly over different epochs of enhanced activity). Cooler shock-heated gas is likely the origin also of the optical bubble and lobes near the X-ray structure, detected in images from the Hubble Space Telescope and the Very Large Telescope. In the radio bands, we observed the region with the Australia Telescope Compact Array, and discovered an elongated radio nebula (about 170 × 55 pc in size) with its major axis aligned with the chain of Chandra sources. The radio nebula has an integrated 5.5 GHz radio luminosity of ≈1034 erg s−1 for a distance of 1.88 Mpc. The morphology, size, and luminosity of the extended X-ray, optical, and radio structure suggest that NGC 300-S 10 belongs to the same class of powerful (Pjet > 1039 erg s−1) microquasars as SS 433, Ho II X-1, and NGC 7793-S 26.
AB - We present the discovery of a powerful candidate microquasar in NGC 300, associated with the S 10 optical nebula (previously classified as a supernova remnant). Chandra images show four discrete X-ray knots aligned in the plane of the sky over a length of ≈150 pc. The X-ray emission from the knots is well fitted with a thermal plasma model at a temperature of ≈0.6 keV and a combined 0.3-8 keV luminosity of ≈1037 erg s−1. The X-ray core, if present at all, does not stand out above the thermal emission of the knots: this suggests that the accreting compact object is either currently in a dim state or occulted from our view. We interpret the emission from the knots as the result of shocks from the interaction of a jet with the interstellar medium (possibly over different epochs of enhanced activity). Cooler shock-heated gas is likely the origin also of the optical bubble and lobes near the X-ray structure, detected in images from the Hubble Space Telescope and the Very Large Telescope. In the radio bands, we observed the region with the Australia Telescope Compact Array, and discovered an elongated radio nebula (about 170 × 55 pc in size) with its major axis aligned with the chain of Chandra sources. The radio nebula has an integrated 5.5 GHz radio luminosity of ≈1034 erg s−1 for a distance of 1.88 Mpc. The morphology, size, and luminosity of the extended X-ray, optical, and radio structure suggest that NGC 300-S 10 belongs to the same class of powerful (Pjet > 1039 erg s−1) microquasars as SS 433, Ho II X-1, and NGC 7793-S 26.
KW - Accretion
KW - Accretion discs
KW - Stars: Black holes
KW - X-rays: Binaries
UR - http://www.scopus.com/inward/record.url?scp=85066924070&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty2771
DO - 10.1093/mnras/sty2771
M3 - Article
AN - SCOPUS:85066924070
VL - 482
SP - 2389
EP - 2406
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -