J/A+A/691/A59ivo://CDS.VizieR/J/A+A/691/A59doi:10.26093/cds/vizier.36910059CDSLlerena M.Amorin R.Pentericci L.Arrabal Haro P.Backhaus B.E.,Bagley M.B.Calabro A.Cleri N.J.Davis K.Dickinson M.,Finkelstein S.L.Gawiser E.Grogin N.A.Hathi N.P.Hirschmann M.,Kartaltepe J.S.Koekemoer A.M.McGrath E.J.Mobasher B.Napolitano L.,Papovich C.Pirzkal N.Trump J.R.Wilkins S.M.Yung L.Y.A.2025-02-26T20:01:52Z2024-10-29T07:46:48ZCDS support team

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

cds-question@unistra.frgalaxiesredshiftedinfrared-photometryline-intensitiesExtreme emission line galaxies (EELGs) are typically characterized by high equivalent widths (EWs) which are driven by elevated specific star formation rates (sSFR) in low-mass galaxies with subsolar metallicities and little dust. Such extreme systems are rare in the local universe, but the number density of EELGs increases with redshift. Such starburst galaxies are currently presumed to be the main drivers of hydrogen reionization over 5.5<z<15, which serves to motivate many of the searches for high-z EELGs. We aim to characterize the physical properties of a sample of ~730 EELGs at 4<z<9 photometrically selected from the CEERS survey using JWST/NIRCam. We validate our method and demonstrate the main physical properties of a subset of EELGs using NIRSpec spectra. We create synthetic NIRCam observations of EELGs using empirical templates based on ~2000 local metal-poor starbursts to select EELGs based on color-color criteria. We study their properties based on SED fitting and flux excess from emission lines in the photometric filters. Our sample has a mean stellar mass of 107.84Msun with high sSFRs with a mean value of 10^-7.03^yr^-1^. We consider a delayed-{tau} model for the star formation history and find our sample of EELGs are young with a mean value of the time after the onset of star formation of 45Myr. We find that they have similar line ratios to local metal-poor starbursts with high log([OIII]/H{beta})>~0.4-1 which indicates that star formation may be the dominant source of ionization. Based on the photometric fluxes, we find an increase of EW([OIII]+H{beta}) with sSFR and {SIGMA}_SFR_, and a decrease with age and stellar mass. The sample of EELGs can reach {SIGMA}_SFR_>10M_{sun}_/yr/kpc^2^ which indicate they are strong candidates of LyC leakers. Another indirect indicator is the high values of O32>5 that can be reached for some galaxies in the sample.2024A&A...691A..59Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/691/A59CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/691/A59https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/691/A59http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/691/A59https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/691/A59https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/691/A59http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/691/A59GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/691/A59/table2 (Photometry information for the EELGs candidates ordered by increasing CEERS ID number)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/691/A59/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/691/A59/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/691/A59/table2?GETtext/xml+votable180.050000true214.9247688952.964053060.0055555555555555566/11425https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/691/A59?format=asciiInfrareddefaultJ/A+A/691/A59/table2Photometry information for the EELGs candidates ordered by increasing CEERS ID numbere_F356WFlux in F356W filter uncertaintynJystat.errorintF410MFlux in F410M filternJyphot.flux.density;em.IRinte_F410MFlux in F410M filter uncertaintynJystat.errorintFluxO3HbPhotometric flux of [OIII]+Hbeta in 10^-18^ergs/cm^2^/s unit1e-21W.m**-2phot.flux;em.line.Hbetafloate_FluxO3HbPhotometric flux uncertainty of [OIII]+Hbeta in 10^-18^ergs/cm^2^/s unit1e-21W.m**-2stat.errorfloatFluxHa? Photometric flux of Halpha in 10^-18^ergs/cm^2^/s unit1e-21W.m**-2phot.flux;em.line.Halphafloatnullablee_FluxHa? Photometric flux uncertainty of Halpha in 10^-18^ergs/cm^2^/s unit1e-21W.m**-2stat.errorfloatnullableEWO3HbPhotometric rest-frame equivalent width of [OIII]+Hbeta in Angstroem unit0.1nmspect.line.eqWidthinte_EWO3HbPhotometric rest-frame equivalent width uncertainty of [OIII]+Hbeta in Angstroem unit0.1nmstat.errorintEWHa? Photometric rest-frame equivalent width of Halpha in Angstroem unit0.1nmspect.line.eqWidthintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDCEERS IDmeta.id;meta.mainintRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainzphotPhotometric redshiftsrc.redshiftdoubleFlag[0/1] Quality flag (1)meta.code.errorintF277W? Flux in F277W filternJyphot.mag;em.IR.Kintnullablee_F277WFlux in F277W filter uncertaintynJystat.errorintF356WFlux in F356W filternJyphot.flux.density;em.IR.3-4uminte_EWHa? Photometric rest-frame equivalent width uncertainty of Halpha in Angstroem unit0.1nmstat.errorintnullableJ/A+A/691/A59/table3SED parameters for the EELGs candidates ordered by increasing CEERS ID numbere_AgeAge uncertaintyMyrstat.error;time.ageintlogUIonization parameterphys.ionizParamfloate_logUIonization parameter uncertaintystat.error;pos.cartesian.xfloatZ*Stellar metallicityphys.abund.Zfloate_Z*Stellar metallicity uncertaintystat.error;src.redshiftfloatAvAbsolute attenuationmagphys.absorptionfloate_AvAbsolute attenuation uncertaintymagstat.errorfloatreff? Physical size in F200W filterkpcem.UV.100-200nmfloatnullablee_reff? Physical size in F200W filter uncertaintykpcstat.errorfloatnullableSigmaSFR? Star formation rate surface densitysolMass.yr**-1.kpc**-2phys.SFRfloatnullablee_SigmaSFR? Star formation rate surface density uncertaintysolMass.yr**-1.kpc**-2stat.errorfloatnullablee_logM*Stellar mass uncertaintylog(solMass)stat.errorfloatSFRStar formation ratesolMass/yrphys.SFRfloate_SFRStar formation rate uncertaintysolMass/yrstat.error;phys.SFRfloatAgeAgeMyrtime.ageintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDCEERS IDmeta.id;meta.mainintlogM*Stellar masslog(solMass)phys.massfloat