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A high signal-to-noise ratio composite quasar spectrum

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dc.contributor.authorFrancis, Paul
dc.contributor.authorHewett, Paul C.
dc.contributor.authorFoltz, Craig B.
dc.contributor.authorChaffee, Frederic H.
dc.contributor.authorWeymann, Ray J.
dc.contributor.authorMorris, Simon L.
dc.date.accessioned2018-09-11T04:07:11Z
dc.date.available2018-09-11T04:07:11Z
dc.date.issued1991
dc.description.abstractA very high signal-to-noise ratio (S/N of about 400) composite spectrum of the rest-frame ultraviolet and optical region of high luminosity quasars is presented. The spectrum is derived from 718 individual spectra obtained as part of the Large Bright Quasar Survey. The moderate resolution, 4A or less, and high signal-to-noise ratio allow numerous weak emission features to be identified. Of particular note is the large equivalent-width of the Fe II emission in the rest-frame ultraviolet and the blue continuum slope of the composite. The primary aim of this paper is to provide a reference spectrum for use in line identifications, and a series of large-scale representations of the composite spectrum are shown. A measure of the standard deviation of the individual quasar spectra from the composite spectrum is also presented.en_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0004-637Xen_AU
dc.identifier.urihttp://hdl.handle.net/1885/147324
dc.publisherAmerican Astronomical Societyen_AU
dc.rightshttp://www.sherpa.ac.uk/romeo/issn/0004-637X/..."Publisher's version/PDF may be used on any website or authors' institutional repository" from SHERPA/RoMEO site (as at 11/09/18).en_AU
dc.sourceThe Astrophysical Journalen_AU
dc.titleA high signal-to-noise ratio composite quasar spectrumen_AU
dc.typeJournal articleen_AU
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.lastpage470en_AU
local.bibliographicCitation.startpage465en_AU
local.contributor.affiliationFrancis, P., Mount Stromlo Observatory, Research School of Astronomy and Astrophysics, The Australian National Universityen_AU
local.contributor.authoruidu9710753en_AU
local.description.notesThe author was affiliated with Institute of Astronomy, Madingley Road, Cambridge, England when the paper was published.en_AU
local.identifier.citationvolume373en_AU
local.identifier.doi10.1086/170066en_AU
local.publisher.urlhttps://aas.org/en_AU
local.type.statusPublished Versionen_AU

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