J/A+A/579/A102ivo://CDS.VizieR/J/A+A/579/A102doi:10.26093/cds/vizier.35790102CDSBoselli A.Fossati M.Gavazzi G.Ciesla L.Buat V.Boissier S.,Hughes T.2018-01-31T06:09:53Z2015-07-07T09:44:22ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsvisible-astronomyh-alpha-photometryline-intensitiesgalaxy-classification-systemsspectroscopyWe present new H{alpha}+[NII] imaging data of late-type galaxies in the Herschel Reference Sample aimed at studying the star formation properties of a K-band-selected, volume-limited sample of nearby galaxies. The H{alpha}+[NII] data are corrected for [NII] contamination and dust attenuation using different recipes based on the Balmer decrement and the 24um luminosities. We show that the H{alpha} luminosities derived with different corrections give consistent results only whenever the the uncertainty on the estimate of the Balmer decrement is [C(H{beta})]<=0.1. We use these data to derive the star formation rate of the late-type galaxies of the sample, and compare these estimates to those determined using independent monochromatic tracers (FUV, radio continuum) or the output of spectral energy distribution (SED) fitting codes. This comparison suggests that the 24um based dust extinction correction for the H{alpha} data might be non universal, and that it should be used with caution in all objects with a low star formation activity, where dust heating can be dominated by the old stellar population. Furthermore, because of the sudden truncation of the star formation activity of cluster galaxies occurring after their interaction with the surrounding environment, the stationarity conditions required to transform monochromatic fluxes into star formation rates might not always be satisfied in tracers other than the H{alpha} luminosity. In a similar way, the parametrisation of the star formation history generally used in SED fitting codes might not be adequate for these recently interacting systems. We then use the derived star formation rates to study the SFR luminosity distribution and the typical scaling relations of the late-type galaxies of the HRS. We observe a systematic decrease of the specific star formation rate with increasing stellar mass, stellar mass surface density, and metallicity. We also observe an increase of the asymmetry and smoothness parameters measured in the H{alpha}-band with increasing SSFR, probably induced by an increase of the contribution of giant HII regions to the H{alpha} luminosity function in star-forming low-luminosity galaxies.2015A&A...579A.102Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/579/A102CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/PASP/122/261 : Herschel Reference Survey Sample (Boselli+, 2010)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/579/A102https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/579/A102http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/579/A102https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/579/A102https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/579/A102http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/579/A102GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/579/A102/HRS (Herschel Reference Survey: basic properties (table1), H{alpha}+NII luxes (table3), CAS parameters (table4), 20cm data (table5), star formation rates (table6), and emission-line fluxes (table7))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/579/A102/HRS?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/579/A102/HRS?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/579/A102/HRS?GETtext/xml+votable180.050000true154.4152522.80997220.0055555555555555565/6928 6941 6965 6984-6985 6/4439 5124-5125 5152 5164 5172 5181-5183 5190 5196 5198 5200 5241 5244 5247 5332 5336 5342 5440 5629 5966-5967 5975-5978 5981-5982 5999 6001 6011 6037 6082 6087 6103 8235 8320 8330 8359 10454 10475 10592 10632 10672 10684 10845 10990 11010 11074 11435 11789 25575 25581 25599 25775 25788 25790 25966 25980 25997 26055 26065 26068 26072 26088 26090-26091 26119 26125 26128 26139 26148 26157 26161 26166 26174-26175 26210 26214 26217 26222-26223 26260 26265 26271 26285 26294 26301-26303 26307-26309 26311 26313 26316-26318 26320 26323 26330-26331 26336 26338 26340 26343-26344 26346-26347 26349 26351 26361-26363 26365 26377 26388 26432 26472 26528 26530 26537 26542 27079 27130 27603 27606 27653-27654 27716 27718-27719 27724-27725 27727-27728 27730-27731 27734-27736 27738-27739 27741 27743 27750 27757-27758 27761 27763 27772-27773 27814 27823 27841 27853 27855 27857 27889 27907-27909 27913-27918 27922 27926 27931 27934 27944-27945 27947-27949 27955 28032-28033 28035 28037-28039 28041 28054 28056 28123 28126 28141-28142 28162 28170 28191 28201 28208 28213 28220-28221 28234 28258 28264 28294 28299-28300 28304 28348 28404 28416 28491 28508 28529 28538 28643 286519.932213363424795e-25 9.932213363424795e-25https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/579/A102?format=asciiOpticaldefaultJ/A+A/579/A102/table2H{alpha} observational parameters of the 138 target galaxiesTexp[180/1200] ON-band exposure time per posestime.duration;obs.exposurefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHRS[1/323] HRS galaxy namemeta.id;meta.mainintFilter[6570/6607] ON-band filter wavelength0.1nmmeta.code;instr.filterintTelTelescope sizeminstr.telfloatCCDUsed CCDmeta.id;instrcharSize[0.28/0.35] Pixel sizearcsecphys.angSize;instr.pixelfloatYear[2006/2012] Year of the observationsyrtime.epochintNexp[1/5] Number of exposuresmeta.numberintAirM[1/1.8] Air massobs.airMassfloatPhot[0/1] Photometric quality of the sky, i=good (1)meta.codeintZp[-15.8/-14.6]? Zero point of the observationmW.m**-2stat.fit;arith.zpfloatnullablen[0.09/1.8] Normalisation factor between the ON- and the OFF-band (r-Gunn) filterinstr.paramfloatJ/A+A/579/A102/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference codemeta.notecharBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notecharJ/A+A/579/A102/HRSHerschel Reference Survey: basic properties (table1), H{alpha}+NII luxes (table3), CAS parameters (table4), 20cm data (table5), star formation rates (table6), and emission-line fluxes (table7)Dist[15/172] Distance (1)Mpcpos.distance;pos.heliocentricfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHRS[1/323] HRS name <[BEC2010] HRS NNN> in Simbadmeta.id;meta.mainintprimaryCGCG? CGCG (Cat. VII/190) namemeta.idintnullableVCC? VCC (Cat. J/AJ/90/1681) namemeta.idintnullableUGC? UGC (Cat. VII/26) namemeta.idintnullableNGC? NGC (Cat. VII/118) namemeta.idintnullablem_NGC[A] Multiplicity index on NGCmeta.code.multipcharIC? IC (Cat. VII/118) namemeta.idintnullableRAJ2000Right Ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainMTypeMorphological typesrc.morph.typecharlogM*[8.4/11.6]? Stellar mass (2)log(solMass)phys.massfloatnullablen_logM*[a] Method used to derive logM* (2)meta.notecharD24.5g[0.5/13] g-band diameter (3)arcminphys.angSizefloatIncl[0/90] Inclination (4)degsrc.orbital.inclinationfloatVel[-273/12000] Recessional velocity (5)km/sphys.veloc;pos.heliocentricintMembCluster or cloud membership (6)meta.id.parentcharHa[0/1] H{alpha} data available ? 1=yes, 0=nometa.noteintSimbadSimbad column added by the CDSmeta.ref.urlcharObsNumber of H{alpha}+NII observations (table2)meta.ref.urlintnullableEW[-2/78]? H{alpha}+[NII] equivalent width0.1nmspect.line.eqWidth;em.line.Halphaintnullablee_EW[0/36]? error on the EWHa+[NII]0.1nmstat.error;spect.line.eqWidthintnullablelogF[-13.81/-10.85]? H{alpha}+[NII] fluxlog(mW.m**-2)phot.fluxfloatnullableu_logFUncertainty flag on logF(Ha+[NII])meta.code.errorchare_logF[0.02/1]? Error on logF(Hal+[NII])log(mW.m**-2)stat.errorfloatnullablef_logF[:] Uncertainty flag on e_logF(Ha+[NII])meta.codecharn_logF[cmv] Notes on H{alpha}+[NII] fluxes (7)meta.notecharRefReference, in refs.dat filemeta.ref;pos.frame;meta.filecharRef2Alternative reference, in refs.dat filemeta.bibcharre(r)[3/136]? r band effective radius r_e_(r)arcsecphys.angSize;srcfloatnullablere(Ha)[2.6/144]? H{alpha}+[NII] effective radiusarcsecphys.angSize;srcfloatnullablere(EW)[5/211]? H{alpha}+[NII] equivalent width effective radiusarcsecphys.angSize;srcfloatnullableCr[1.9/5.2] r band concentration indexphys.size;arith.ratiofloatnullableAr[-0.1/0.4] r band asymmetrysrc.morph.paramfloatnullableSr[-0.1/1.2] r band clumpinessstat.fit.paramfloatnullableCH[0.2/5.6]? H{alpha}+[NII] concentration indexphys.size;arith.ratiofloatnullableAH[-0.17/1]? H{alpha}+[NII] asymmetrysrc.morph.paramfloatnullableSH[-1.1/2.21]? H{alpha}+[NII] clumpinessstat.fit.paramfloatnullablef_S20[0/2] code for detections (1) and undetections (0) of 20cm datameta.codeintS20[0.2/266000] Radio flux density at 20cm or upper limitmJyphot.flux.density;em.radio.750-1500MHzdoubleq_S20[1/2]? 20cm data quality: 1=high, 2=uncertainmeta.code.qualintnullabler_S20[1/6] Reference (8)meta.ref;pos.frameintlogL20[18/25] Radio luminosity at 20cm or upper limitlog(W.Hz**-1)phys.luminosity;em.radio.750-1500MHzfloatSFR1? Star formation rate determined using H{alpha} data corrected for attenuation using the Balmer decrementsolMass/yrphys.SFR;spect.linefloatnullableSFR2? Star formation rate determined using H{alpha} data corrected for attenuation using the 24um emissionsolMass/yrphys.SFR;spect.linefloatnullableSFR3? Star formation rate determined using FUV emission corrected for attenuation using the 24um emissionsolMass/yrphys.SFRfloatnullableSFR4? Star formation rate determined using the radio 20cm emissionsolMass/yrphys.SFRfloatnullableSFRm[0.01/9.3]? Star formation rate determined by averaging the previous 4 estimatessolMass/yrphys.SFRfloatnullableSFR6? Star formation rate determined using SED fitting with 1 exponentially declining SFRsolMass/yrphys.SFRfloatnullableSFR7? Star formation rate determined using SED fitting with 2 exponentially declining SFRsolMass/yrphys.SFRfloatnullableSFR8? Star formation rate determined using SED fitting with a delaied SFRsolMass/yrphys.SFRfloatnullableF3727? [OII]3727 flux normalised to H{alpha}phot.flux;arith.ratiofloatnullableFHb? H{beta} flux normalised to H{alpha}phot.flux;arith.ratiofloatnullableF5007? [OIII]5007 flux normalised to H{alpha}phot.flux;arith.ratiofloatnullableF6584? [NII]6584 flux normalised to H{alpha}phot.flux;arith.ratiofloatnullableF6716? [SII]6716 flux normalised to H{alpha}phot.flux;arith.ratiofloatnullableF6731? [SII]6731 flux normalised to H{alpha}phot.flux;arith.ratiofloatnullableS/Na? Signal-to-noise at H{alpha}stat.snrfloatnullableS/Nb? Signal-to-noise at H{beta}stat.snrfloatnullableC(Hb)? Balmer decrementmeta.notefloatnullablee_C(Hb)? Error on the Balmer decrementstat.errorfloatnullable