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dc.contributor.authorHardcastle, M.J.
dc.contributor.authorWorrall, D.M.
dc.contributor.authorBirkinshaw, M.
dc.contributor.authorLaing, R.A.
dc.contributor.authorBridle, A.H.
dc.date.accessioned2007-08-11T20:22:23Z
dc.date.available2007-08-11T20:22:23Z
dc.date.issued2002-07
dc.identifier.citationHardcastle , M J , Worrall , D M , Birkinshaw , M , Laing , R A & Bridle , A H 2002 , ' A Chandra observation of the X-ray environment and jet of 3C 31 ' , Monthly Notices of the Royal Astronomical Society , vol. 334 , no. 1 , pp. 182-192 .
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 138572
dc.identifier.otherPURE UUID: d856f9c4-9902-43c3-89ac-8561ca189548
dc.identifier.otherdspace: 2299/374
dc.identifier.otherScopus: 0001087748
dc.identifier.urihttp://hdl.handle.net/2299/374
dc.description.abstractWe have used a deep Chandra observation of the central regions of the twin-jet FRI radio galaxy 3C 31 to resolve the thermal X-ray emission in the central few kiloparsecs of the host galaxy, NGC 383, where the jets are thought to be decelerating rapidly. This allows us to make high-precision measurements of the density, temperature and pressure distributions in this region, and to show that the X-ray emitting gas in the centre of the galaxy has a cooling time of only 5 × 107 years. In a companion paper these measurements are used to place constraints on models of the jet dynamics. A previously unknown one-sided X-ray jet in 3C 31, extending up to 8 arcsec from the nucleus, is detected and resolved. Its structure and steep X-ray spectrum are similar to those of X-ray jets known in other FRI sources, and we attribute the radiation to synchrotron emission from a high-energy population of electrons. In situ particle acceleration is required in the region of the jet where bulk deceleration is taking place. We also present X-ray spectra and luminosities of the galaxies in the Arp 331 chain of which NGC 383 is a member. The spectrum and spatial properties of the nearby bright X- ray source 1E 0104+3153 are used to argue that the soft X-ray emission is mostly due to a foreground group of galaxies rather than to the background broad absorption-line quasar.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectAstronomy
dc.titleA Chandra observation of the X-ray environment and jet of 3C 31en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionSPECS Deans Group
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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