J/A+A/654/A135ivo://CDS.VizieR/J/A+A/654/A135doi:10.26093/cds/vizier.36540135CDSDiaz-Garcia S.Lisenfeld U.Perez I.Zurita A.Verley S.Combes F.,Espada D.Leon S.Martinez-Badenes V.Sabater J.Verdes-Montenegro L.2022-01-19T13:06:49Z2021-10-22T10:11:01ZCDS support team

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

cds-question@unistra.frgalaxiesphotometryradio-galaxiesinfrared-photometrymillimeter-astronomysubmillimeter-astronomyultraviolet-photometryWhile some galactic bars show recent massive star formation (SF) along them, some others present a lack of it. Whether bars with low level of SF are a consequence of low star formation efficiency, low gas inflow rate, or dynamical effects, remains a matter of debate. In order to study the physical conditions that enable or prevent SF, we perform a multi-wavelength analysis of 12 strongly barred galaxies with total stellar masses log10(M*/M_{sun}_){in}[10.2,11], chosen to host different degrees of SF along the bar major axis without any prior condition on gas content. We observe the CO(1-0) and CO(2-1) emission within bars with the IRAM-30m telescope (beam sizes of 1.7-3.9kpc and 0.9-2.0kpc, respectively; 7-8 pointings per galaxy on average). We estimate molecular gas masses (Mmol) from the CO(1-0) and CO(2-1) emissions. SF rates (SFR) are calculated from GALEX near-ultraviolet (UV) and WISE 12um images within the beam-pointings, covering the full bar extent (SFRs are also derived from far-UV and 22um). Results. We detect molecular gas along the bars of all probed galaxies. Molecular gas and SFR surface densities span the ranges log10({Sigma}_mol_/[M_{sun}_/pc^2^]){in}[0.4,2.4] and log10({Sigma}_SFR_/[M_{sun}_/pc/kpc^2^]){in}[-3.25,-0.75], respectively. The star formation efficiency (SFE=SFR/Mmol) in bars varies between galaxies by up to an order of magnitude (SFE{in}[0.1,1.8]Gyr^-1^). On average, SFEs are roughly constant along bars. SFEs are not significantly different from the mean value in spiral galaxies reported in the literature (~0.43Gyr^-1^), regardless of whether we estimate Mmol from CO(1-0) or CO(2-1). Interestingly, the higher the total stellar mass of the host galaxy, the lower the SFE within their bars. In particular, the two galaxies in our sample with lowest SFE and {Sigma}_SFR_ (NGC 4548 and NGC 5850, SFE<=0.25Gyr^-1^, {Sigma}_SFR_<=10^-2.25^M_{sun}_/yr/kpc^2^, M*<=10^10.7^M_{sun}_) are also the ones hosting massive bulges and signs of past interactions with nearby companions. We present a statistical analysis of the SFE in bars for a sample of 12 galaxies. The SFE in strong bars is not systematically inhibited (either in the central, mid- or end-parts of the bar). Both environmental and internal quenching are likely responsible for the lowest SFEs reported in this work.2021A&A...654A.135Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/654/A135CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/654/A135https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/654/A135http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/654/A135https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/654/A135https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/654/A135http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/654/A135GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/654/A135/galaxies (Equatorial coordinates (J2000) of central pointing for each galaxy)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/654/A135/galaxies?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/654/A135/galaxies?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/654/A135/galaxies?GETtext/xml+votable180.050000true165.7962527.972220.0055555555555555566/5200 8196 8256 10650 12122 15955 17281 26148 27653 27728 27942 28045https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/654/A135?format=asciiUVInfraredMillimeterRadiodefaultJ/A+A/654/A135/galaxiesEquatorial coordinates (J2000) of central pointing for each galaxyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyGalaxy identificationmeta.id;meta.maincharRAJ2000Right ascension of centre of the IRAM-30m central pointing (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of centre of the IRAM-30m central pointing (J2000)degpos.eq.dec;meta.mainSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/654/A135/listspList of individual spectraspShow the spectrummeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyGalaxy namemeta.id;meta.maincharoRAOffset in Right ascension (1)arcsecpos.eq.ra;arith.diffintoDEOffset in DEclination (1)arcsecpos.eq.dec;arith.diffintLineLine (CO(1-0) or CO(2-1))meta.id;spect.linecharFileNameName of the spectrum file in subdirectory spmeta.id;meta.filechar