Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/4438
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dc.contributor.authorNath, Biman B.-
dc.contributor.authorEichler, D.-
dc.date.accessioned2012-05-07T08:35:55Z-
dc.date.available2012-05-07T08:35:55Z-
dc.date.issued1993-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 1993, Vol.261, pL25en
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/4438-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractWe discuss the possibility of detecting protogalaxies in the ultraviolet, assuming that galaxy formation occurred at z ~ 5-6. We show that the diffuse gas in collapsing galaxy-sized objects with temperatures ~10^6+0.5 K, and with modest metallicities, should produce many emission lines from highly ionized iron atoms. We compare the expected luminosity from models of galaxy formation with the sensitivity of the Hubble Space Telescope (HST).en
dc.language.isoenen
dc.publisherRoyal Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/1993MNRAS.261L..25Nen
dc.relation.urihttp://arxiv.org/abs/astro-ph/9301012en
dc.rights1993 Royal Astronomical Societyen
dc.titlePossible forest of emission lines from protogalaxiesen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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