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DC Field | Value | Language |
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dc.contributor.author | Sharma, Mahavir | - |
dc.contributor.author | Nath, Biman B. | - |
dc.contributor.author | Chand, Hum | - |
dc.date.accessioned | 2013-05-06T09:30:52Z | - |
dc.date.available | 2013-05-06T09:30:52Z | - |
dc.date.issued | 2013-04-01 | - |
dc.identifier.citation | Monthly Notices of the Royal Astronomical Society : Letters, 2013, 431, L93-L97 | en |
dc.identifier.issn | 1745-3933 (online) | - |
dc.identifier.uri | http://hdl.handle.net/2289/5573 | - |
dc.description | Restricted Access. An open-access version is available at arXiv.org (one of the alternative locations) | en |
dc.description.abstract | We report a correlation between velocity offset (β = v/c) of strong Mg ii absorption systems and the bolometric luminosity (Lbol) of quasars in SDSS-DR7. We find that β shows a power-law increase with Lbol, with a slope ∼1/4. We find that such a relation of β with Lbol is expected for outflows driven by scattering of black hole radiation by dust grains, and which are launched from the innermost dust survival radius. Our results indicate that a significant fraction of the strong Mg ii absorbers, in the range of β = 0–0.4, may be associated with the quasars themselves. | en |
dc.language.iso | en | en |
dc.publisher | Oxford University Press for the RAS | en |
dc.relation.uri | http://adsabs.harvard.edu/abs/2013MNRAS.431L..93S | en |
dc.relation.uri | http://arxiv.org/abs/1212.3755 | en |
dc.relation.uri | http://dx.doi.org/10.1093/mnrasl/slt015 | en |
dc.rights | 2013 The authors & the Royal Astronomical Society. | en |
dc.subject | ISM | en |
dc.subject | jets and outflows galaxies | en |
dc.subject | active quasars | en |
dc.subject | absorption lines | en |
dc.subject | quasars - General | en |
dc.title | Signature of outflows in strong Mg II absorbers in quasar sightlines | en |
dc.type | Article | en |
Appears in Collections: | Research Papers (A&A) |
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2013_MNRASL_431_L93.pdf Restricted Access | Restricted Access | 303.98 kB | Adobe PDF | View/Open Request a copy |
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