J/A+A/659/A183ivo://CDS.VizieR/J/A+A/659/A183doi:10.26093/cds/vizier.36590183CDSKerutt J.Wisotzki L.Verhamme A.Schmidt K.B.Leclercq F.Herenz E.C.,Urrutia T.Garel T.Hashimoto T.Maseda M.Matthee J.Kusakabe H.,Schaye J.Richard J.Guiderdoni B.Mauerhofer V.Nanayakkara T.,Vitte E.2025-01-23T20:00:55Z2022-03-25T10:06:32ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiescatalogsultraviolet-astronomyspectroscopyThe hydrogen Lyman{alpha} line is often the only measurable feature in optical spectra of high-redshift galaxies. Its shape and strength are influenced by radiative transfer processes and the properties of the underlying stellar population. High equivalent widths of several hundred {AA} are especially hard to explain by models and could point towards unusual stellar populations, for example with low metallicities, young stellar ages, and a top-heavy initial mass function. Other aspects influencing equivalent widths are the morphology of the galaxy and its gas properties. The aim of this study is to better understand the connection between the Lyman{alpha} rest-frame equivalent width (EW0) and spectral properties as well as ultraviolet (UV) continuum morphology by obtaining reliable EW0 histograms for a statistical sample of galaxies and by assessing the fraction of objects with large equivalent widths. We used integral field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data from the Hubble Space Telescope (HST) to measure EW0 . We analysed the emission lines of 1920 Lyman{alpha} emitters (LAEs) detected in the full MUSE-Wide (one hour exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum counterparts in archival HST data. We fitted the UV continuum photometric images using the Galfit software to gain morphological information on the rest-UV emission and fitted the spectra obtained from MUSE to determine the double peak fraction, asymmetry, full-width at half maximum, and flux of the Lyman{alpha} line. The two surveys show different histograms of Lyman{alpha} EW0 . In MUSE-Wide, 20% of objects have EW0>240{AA}, while this fraction is only 11% in MUSE-Deep and ~=16% for the full sample. This includes objects without HST continuum counterparts (one-third of our sample), for which we give lower limits for EW0. The object with the highest securely measured EW0 has EW0=589+/-193{AA} (the highest lower limit being EW0=4464{AA}). We investigate the connection between EW0 and Lyman{alpha} spectral or UV continuum morphological properties. The survey depth has to be taken into account when studying EW0 distributions. We find that in general, high EW0 objects can have a wide range of spectral and UV morphological properties, which might reflect that the underlying causes for high EW0 values are equally varied.2022A&A...659A.183Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/659/A183CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/608/A2 : MUSE Hubble Ultra Deep Field Survey. II. (Inami+, 2017)J/A+A/621/A107 : MUSE-Wide Lyman alpha luminosity function 3<z<6 (Herenz+ 2019)J/A+A/624/A141 : MUSE-Wide Survey DR1 catalog (Urrutia+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/659/A183https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/659/A183http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/659/A183https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/659/A183https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/659/A183http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/659/A183GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/659/A183/tableb1 (Catalog)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/659/A183/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/659/A183/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/659/A183/tableb1?GETtext/xml+votable180.050000true53.13779-27.795530.0055555555555555566/27258 35935https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/659/A183?format=asciiUVdefaultJ/A+A/659/A183/tableb1CatalogSimbadNameSimbad column added by the CDSmeta.idcharnullableI17ID? Source identifier in Inami et al., 2017, Cat. J/A+A/608/A2, [IBB2017] NNNN in Simbad (2)meta.idintnullableRAJ2000Right Ascension (J2000) of UV continuumdegpos.eq.ra;meta.mainDEJ2000Declination (J2000) of UV continuumdegpos.eq.dec;meta.mainzRedshift of the source based on Lyasrc.redshiftfloate_zUncertainty on the redshiftstat.error;src.redshiftdoubleConf[0/3] Confidence level from QtClassify as in Urrutia et al., 2019A&A...624A.141U (3)meta.codeintEW0Rest-frame equivalent width of Ly alpha0.1nmspect.line.eqWidthfloate_EW0Uncertainty on EW00.1nmstat.errorfloatMUVEstimated absolute UV magnitude (AB) at 1500 Angstrommagphys.magAbsfloate_MUVUncertainty on MUVmagstat.errorfloatlogLLyalog Ly alpha luminosity given in erg/slog(1e-07W)phys.luminosity;em.UVfloate_logLLyaUncertainty on logLLyalog(1e-07W)stat.errorfloatPeaksepPeak separation of LAEs with a two-component Ly alpha linekm/sphys.veloc;arith.difffloate_PeaksepUncertainty on Peaksepkm/sstat.errordoubleFWHMFull-width at half maximum of the Ly alpha (red component) emission linekm/sspect.line.widthfloate_FWHMUncertainty on FWHMkm/sstat.error;phys.angSizedoubleAsymAsymmetry parameter of the asymmetric Gaussian fit to the main red peakstat.fit.param;meta.main;stat.maxfloate_AsymUncertainty of Asymstat.errorfloatReEffective radius in (physical) kpc measured with Galfitkpcphys.size.radiusfloate_Reuncertainty on Rekpcstat.errorfloataxisratioMorphological parameter of the UV continuum counterpart, obtained using Galfitmeta.id.assoc;src.morph.param;spect.continuumfloate_axisratioUncertainty of axisratiostat.errorfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDUnique MUSE-Wide object ID (1)meta.id;meta.mainlong