dc.contributor.author | Smith, Daniel | |
dc.contributor.author | Simpson, C. | |
dc.contributor.author | Swinbank, A.M. | |
dc.contributor.author | Rawlings, S. | |
dc.contributor.author | Jarvis, M.J. | |
dc.date.accessioned | 2010-10-27T08:19:53Z | |
dc.date.available | 2010-10-27T08:19:53Z | |
dc.date.issued | 2010 | |
dc.identifier.citation | Smith , D , Simpson , C , Swinbank , A M , Rawlings , S & Jarvis , M J 2010 , ' When galaxies collide : understanding the broad absorption-line radio galaxy 4C +72.26 ' , Monthly Notices of the Royal Astronomical Society , vol. 404 , no. 3 , pp. 1089-1099 . https://doi.org/10.1111/j.1365-2966.2010.16279.x | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | dspace: 2299/4925 | |
dc.identifier.other | ORCID: /0000-0001-9708-253X/work/69424367 | |
dc.identifier.uri | http://hdl.handle.net/2299/4925 | |
dc.description | Original article can be found at: http://www3.interscience.wiley.com/ Copyright Royal Astronomical Society | |
dc.description.abstract | We present a range of new observations of the 'broad absorption-line radio galaxy' 4C +72.26 (z≈ 3.5) , including sensitive rest-frame ultraviolet integral field spectroscopy using the Gemini/GMOS-N instrument and Subaru/CISCO K-band imaging and spectroscopy. We show that 4C +72.26 is a system of two vigorously star-forming galaxies superimposed along the line of sight separated by ∼1300 ± 200 km s−1 in velocity, with each demonstrating spectroscopically resolved absorption lines. The most active star-forming galaxy also hosts the accreting supermassive black hole which powers the extended radio source. We conclude that the star formation is unlikely to have been induced by a shock caused by the passage of the radio jet, and instead propose that a collision is a more probable trigger for the star formation. Despite the massive starburst, the ultraviolet-mid-infrared spectral energy distribution suggests that the pre-existing stellar population comprises ∼1012 M⊙ of stellar mass, with the current burst only contributing a further ∼2 per cent, suggesting that 4C +72.26 has already assembled most of its final stellar mass. | en |
dc.format.extent | 11 | |
dc.format.extent | 956463 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.subject | galaxies: haloes | |
dc.subject | galaxies: high-redshift | |
dc.subject | galaxies: individual: 4C+72 | |
dc.subject | 26 | |
dc.subject | quasars: emission lines | |
dc.subject | galaxies: starburst | |
dc.subject | K-Z RELATION | |
dc.subject | STAR-FORMATION HISTORY | |
dc.subject | COSMIC MICROSCOPE | |
dc.subject | EARLY UNIVERSE | |
dc.subject | 4C 41.17 | |
dc.subject | QUASARS | |
dc.subject | SPECTROSCOPY | |
dc.subject | SAMPLE | |
dc.subject | DUST | |
dc.subject | STELLAR | |
dc.title | When galaxies collide : understanding the broad absorption-line radio galaxy 4C +72.26 | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.contributor.institution | School of Physics, Engineering & Computer Science | |
dc.contributor.institution | Department of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | 10.1111/j.1365-2966.2010.16279.x | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |