J/A+A/641/A118ivo://CDS.VizieR/J/A+A/641/A118doi:10.26093/cds/vizier.36410118CDSFeltre A.Maseda M.V.Bacon R.Pradeep J.Leclercq F.Kusakabe H.,Wisotzki L.Hashimoto T.Schmidt K.B.Blaizot J.Brinchmann J.,Boogaard L.Cantalupo S.Carton D.Inami H.Kollatschny W.Marino R.A.,Matthee J.Nanayakkara T.Richard J.Schaye J.Tresse L.Urrutia T.,Verhamme A.Weilbacher P.M.2020-12-07T11:09:53Z2020-09-18T08:50:23ZCDS support team

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

cds-question@unistra.frgalaxiesspectroscopyultraviolet-astronomyWe investigate the ultraviolet (UV) spectral properties of faint Lyman{alpha} emitters (LAEs) in the redshift range 2.9<=z<=4.6 and provide material to prepare future observations of the faint Universe. We use data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median M_UV_ of -18 and down to M_UV_ of -16), low stellar mass (median value of 10^8.4^ and down to 10^7^ solar masses) LAEs at redshift z>3. We compute various averaged spectra of LAEs sub-sampled on the basis of their observational (e.g., Ly{alpha} strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We search for UV spectral features other than Ly{alpha}, such as higher-ionization nebular emission lines and absorption features. We successfully observe the OIII]{lambda}1666 and [CIII]{lambda}1907+CIII]{lambda}1909 collisionally excited emission lines and the HeII{lambda}1640 recombination feature, as well as the resonant CIV{lambda}1548,1551 doublet either in emission or P-Cygni. We compare the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Ly{alpha} equivalent widths, fainter UV magnitudes, bluer UV spectral slopes and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z>2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass and faint LAEs. We publicly release the stacked spectra as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope.2020A&A...641A.118Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/641/A118CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/608/A2 : MUSE Hubble Ultra Deep Field Survey. II (Inami+, 2017)J/A+A/608/A8 : MUSE Hubble Ultra Deep Field Survey. VIII (Leclercq+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/641/A118https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/641/A118http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/641/A118https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/641/A118https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/641/A118http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/641/A118GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVdefaultJ/A+A/641/A118/table1Details of the MUSE HUDF LAE subsamples and emission-line EWs measured from the stacked spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNo[00/20] Reference number of the stacked spectrameta.numberintSubsamplesBinning criterion of the LAE subsamplemeta.noteNLAENumber of LAEs in each subsamplemeta.numberintl_EWHeIILimit flag on EWHeIImeta.code.errorcharEWHeII? HeII{lambda}1640 equivalent width (1)0.1nmspect.line.eqWidthfloatnullablee_EWHeII? HeII{lambda}1640 equivalent width error0.1nmstat.errorfloatnullablel_EWOIII]Limit flag on EWOIII]meta.code.errorcharEWOIII]? OIII]{lambda}1666 equivalent width (1)0.1nmspect.line.eqWidthfloatnullablee_EWOIII]? OIII]{lambda}1666 equivalent width error0.1nmstat.errorfloatnullablel_EW[SiIII]? Limit flag on EW[SiIII]meta.code.error;spect.line.eqWidthcharEW[SiIII]? [SiIII]{lambda}1883 equivalent width (1)0.1nmspect.line.eqWidthfloatnullablee_EW[SiIII]? [SiIII]{lambda}1883 equivalent width error0.1nmstat.error;spect.line.eqWidthfloatnullablel_EW[CIII]07Limit flag on EW[CIII]07meta.code.error;spect.line.eqWidthcharEW[CIII]07? [CIII]{lambda}1907 equivalent width (1)0.1nmspect.line.eqWidthfloatnullablee_EW[CIII]07? [CIII]{lambda}1907 equivalent width error0.1nmstat.error;spect.line.eqWidthfloatnullablel_EW[CIII]09Limit flag on EW[CIII]09meta.code.error;spect.line.eqWidthcharEW[CIII]09? [CIII]{lambda}1909 equivalent width (1)0.1nmspect.line.eqWidthfloatnullablee_EW[CIII]09? [CIII]{lambda}1909 equivalent width error0.1nmstat.error;spect.line.eqWidthfloatnullablespShow the spectrummeta.ref.urlcharFileNameName of the file with the stacked spectra of the subsample, in subdirectory spmeta.id;meta.filechar