J/MNRAS/442/3565ivo://CDS.VizieR/J/MNRAS/442/3565doi:10.26093/cds/vizier.74423565CDSChavez R.Terlevich R.Terlevich E.Bresolin F.Melnick J.Plionis M.,Basilakos S.2024-08-09T20:15:34Z2015-06-23T07:21:43ZCDS support team

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

cds-question@unistra.frgalaxiesspectroscopyh-ii-regionsline-intensitiesThe validity of the emission-line luminosity versus ionized gas velocity dispersion (L-{sigma}) correlation for HII galaxies (HIIGx) and its potential as an accurate distance estimator are assessed. For a sample of 128 local (0.02<~z<~0.2) compact HIIGx with high equivalent widths of their Balmer emission lines, we obtained the ionized gas velocity dispersion from high signal-to-noise ratio (S/N) high-dispersion spectroscopy (Subaru High Dispersion Spectrograph (HDS) and European Southern Observatory (ESO) Very Large Telescope Ultraviolet and Visual Echelle Spectrograph (VLT-UVES)) and integrated H{beta} fluxes from low-dispersion wide aperture spectrophotometry. We find that the L(H{beta})-{sigma} relation is strong and stable against restrictions in the sample (mostly based on the emission-line profiles). The `Gaussianity' of the profile is important for reducing the root-mean-square (rms) uncertainty of the distance indicator, but at the expense of substantially reducing the sample. By fitting other physical parameters into the correlation, we are able to decrease the scatter significantly without reducing the sample. The size of the star-forming region is an important second parameter, while adding the emission-line equivalent width or the continuum colour and metallicity produces the solution with the smallest rms scatter={delta}logL(H{beta})=0.233. The derived coefficients in the best L(H{beta})-{sigma} relation are very close to what is expected from virialized ionizing clusters, while the derived sum of the stellar and ionized gas masses is similar to the dynamical mass estimated using the Hubble Space Telescope} (HST}) corrected Petrosian radius. These results are compatible with gravity being the main mechanism causing the broadening of the emission lines in these very young and massive clusters. The derived masses range from about 2x10^6^M_{sun}_ to 10^9^M_{sun}_ and their 'corrected' Petrosian radius ranges from a few tens to a few hundred pc.2014MNRAS.442.3565Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/442/3565CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/442/3565https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/442/3565http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/442/3565https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/442/3565https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/442/3565http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/442/3565GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/442/3565/galaxies (Results of our high-resolution spectroscopy on HII galaxies: FWHM (table5) and fluxes (table3) of H{beta} and [OIII] lines, line intensities (table4), and derived values (table6))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/442/3565/galaxies?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/442/3565/galaxies?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/442/3565/galaxies?GETtext/xml+votable180.050000true1.737580.857190.0055555555555555566/4109 4164 4184 4258 4276 4298 4330 4441 4464 4503 4516 4576 4685 4716 4738 4758 4773 4815 4871 4913 5018 5100 5173-5174 5223 5246 5252 5290 5637 5646 5669 5731 5825 6215 6402 7185 7208 7252 7259 7304 7315 7328 7354 7381 7483 7524 8914 9481 10441 17242 17249 17516 17571 17601 17748 18025 18091 18177 18388 18785 18845 18880 18953 19028 19036 19122 19323 19327 19389 19754 19756 20002-20003 21877-21878 22719 23187 24696 25851 25938 26142 26390 26551 26555 26963 26971 27053 27057 27068 27071 27227 27243 27260 27291 27303 27333 27396 27409 27431 27446 27463 27467 27499 27512 27518 27581 27604 27770 28290 28363 31725 34243 36716 36766 36779 36785 36801 38850 39628 43829 47701 49011 49016 49095 49101https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/442/3565?format=asciiOpticaldefaultJ/MNRAS/442/3565/table1Journal of observationsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDatesObservation datestime.epochcharTelTelescope: ESO-VLT, NOAJ-Subaru, OAGH-2.12m or OAN-2instr.telcharInstInstrument: B&C, HDS or UVES-Redmeta.notecharDetDetectormeta.id;meta.maincharn_Det[a] a: 2x4 binningmeta.notecharSlit[2/13.1] Slit widtharcsecspect.line.widthfloatJ/MNRAS/442/3565/galaxiesResults of our high-resolution spectroscopy on HII galaxies: FWHM (table5) and fluxes (table3) of H{beta} and [OIII] lines, line intensities (table4), and derived values (table6)Sam[1/4] Sample flag (2)meta.idintSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[1/128] Sequential numbermeta.recordintNameGalaxy Name (JHHMMSS+DDMMSS)meta.id;meta.maincharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainzh[0.009/0.2] Heliocentric redshift from SDSS-DR7src.redshiftdoublee_zhrms uncertainty on zstat.errorfloatW(Hb)[0.57/3.62]? H{beta} FWHM0.1nmspect.line.widthfloatnullablee_W(Hb)[0.03/0.23]? rms uncertainty on W(Hb)0.1nmstat.errorfloatnullableW(5007)[0.63/3.24]? [OIII]{lambda}5007 FWHM0.1nmspect.line.widthfloatnullablee_W(5007)[0/0.22]? rms uncertainty on W(5007)0.1nmstat.errorfloatnullableF(Hb)SDSS DR7 H{beta} flux (10^-16^erg/cm^2^/s)1e-19W.m**-2phot.flux;em.line.Hbetafloate_F(Hb)rms uncertainty on F(Hb)1e-19W.m**-2stat.errorfloatF(Hb)gGaussian (peak) fit H{beta} flux1e-19W.m**-2phot.flux;em.line.Hbetafloate_F(Hb)grms uncertainty on F(Hb)g1e-19W.m**-2stat.errorfloatF(Hb)iIntegral H{beta} flux1e-19W.m**-2phot.flux;em.line.Hbetafloate_F(Hb)irms uncertainty on F(Hb)i1e-19W.m**-2stat.errorfloatF(4959)? Gaussian fit (peak) flux of [OIII]{lambda}4959 line1e-19W.m**-2phot.flux;em.line.OIII;meta.modelledfloatnullablee_F(4959)? rms uncertainty on F(4959)1e-19W.m**-2stat.errorfloatnullableF(5007)? Gaussian fit (peak) flux of [OIII]{lambda}5007 line1e-19W.m**-2phot.flux;em.line.OIII;meta.modelledfloatnullablee_F(5007)? rms uncertainty on F([OIII]2)1e-19W.m**-2stat.errorfloatnullableEW(Hb)H{beta} equivalent width ({AA})0.1nmspect.line.eqWidth;em.line.Hbetafloate_EW(Hb)rms uncertainty on EW(Hb)0.1nmstat.errorfloatInst[1/3] Origin of the fluxes and EWs (1)meta.ref;pos.frameintI3726? [OII]{lambda}3726/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_I3726? rms uncertainty on I3726%stat.errorfloatnullableI3729? [OII]{lambda}3729/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_I3729? rms uncertainty on I3729%stat.errorfloatnullableI4363? [OIII]{lambda}4363/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_I4363? rms uncertainty on I4363%stat.errorfloatnullableI4959? [OIII]{lambda}4959/H{beta} intensity ratio%spect.line.intensity;arith.ratiointnullablee_I4959? rms uncertainty on I4959%stat.errorfloatnullableI5007? [OIII]{lambda}5007/H{beta} intensity ratio%spect.line.intensity;arith.ratiointnullablee_I5007? rms uncertainty on I5007%stat.errorfloatnullableHg? H{gamma}/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_Hg? rms uncertainty on H{gamma}%stat.errorfloatnullableHa? H{alpha}/H{beta} intensity ratio%spect.line.intensity;arith.ratiointnullablee_Ha? rms uncertainty on H{alpha}%stat.errorfloatnullableI6548? [NII]{lambda}6548/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_I6548? rms uncertainty on I6548%stat.errorfloatnullableI6584? [NII]{lambda}6584/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_I6584? rms uncertainty on I6584%stat.errorfloatnullableI6716? [SII]{lambda}6716/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_I6716? rms uncertainty on I6716%stat.errorfloatnullableI6731? [SII]{lambda}6731/H{beta} intensity ratio%spect.line.intensity;arith.ratiofloatnullablee_I6731? rms uncertainty on I6731%stat.errorfloatnullablez[0.009/0.2] Our heliocentric redshift, corrected from bulk flow effectssrc.redshiftdoublee_zrms uncertainty on zstat.error;src.redshiftfloatAV[0/1.9] Absorption in V bandmagphot.mag;em.opt.Vfloate_AV[0/0.8] rms uncertainty on AVmagstat.errorfloatQ[0/33] Ratio between the equivalent widths of H{beta} in absorption and in emission.%phot.flux;arith.ratiofloatcHb[0/0.18] Balmer decrementphot.flux;arith.ratiofloate_cHb[0/0.08] rms uncertainty on cHbstat.errorfloatlogsHb[1.1/1.9]? H{beta} velocity dispersionlog(km.s**-1)phys.veloc.dispersion;spect.linefloatnullablee_logsHb[0.04/0.06]? rms uncertainty on logsigHblog(km.s**-1)stat.errorfloatnullablelogsO[1.1/1.9]? [OIII] velocity dispersionlog(km.s**-1)phys.veloc.dispersion;spect.linefloatnullablee_logsO[0/0.04]? rms uncertainty on logsig[OIII]log(km.s**-1)stat.errorfloatnullablelogLHb[39.5/42.5] Corrected H{beta} luminositylog(1e-07W)phys.luminosity;em.line.Hbetafloate_logLHb[0.03/0.33] rms uncertainty on logL(H{beta})log(1e-07W)stat.errorfloatAb(O)[7.6/8.4]? Total oxygen abundance Ab(O)=12+log(O/H)phys.abundfloatnullablee_Ab(O)[0.05/0.4]? rms uncertainty on Ab(O)stat.errorfloatnullablelogRu[2/3.4]? Seeing-corrected Petrosian radiuslog(pc)phys.size.radiusfloatnullablee_logRu? rms uncertainty on logRulog(pc)stat.errorfloatnullablelogMdyn[6.9/9.3]? Dynamical masslog(solMass)phys.massfloatnullablee_logMdyn[0.04/0.17]? rms uncertainty on logMdynlog(solMass)stat.errorfloatnullablelogMcl[6.3/9.4]? Photometric mass of the ionizing clusterslog(solMass)phys.massfloatnullablee_logMcl[0.03/0.33]? rms uncertainty on logMcllog(solMass)stat.errorfloatnullablelogMion[5.1/8.1]? Photometric mass of ionized gaslog(solMass)phys.massfloatnullablee_logMion[0.05/0.2]? rms uncertainty on logMionlog(solMass)stat.errorfloatnullablelogSFR[-1.3/1.7] Star formation ratelog(solMass.yr**-1)phys.SFRfloate_logSFR[0.03/0.33] rms uncertainty on logSFRlog(solMass.yr**-1)stat.error;phys.SFRfloatSloanDisplay the SDSS data for this galaxymeta.ref.urlchar