J/ApJ/453/616ivo://CDS.VizieR/J/ApJ/453/616doi:10.26093/cds/vizier.14530616CDSSpinoglio L.Malkan M.A.Rush B.Carrasco L.Recillas-Cruz E.2013-03-05T06:34:51Z1999-03-02T10:15:57ZCDS support team

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

cds-question@unistra.frgalaxiesphotometryinfrared-photometryAperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.1995ApJ...453..616Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/453/616CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVII/157 : The extended 12um galaxy sample (Rush+ 1993)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/453/616https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/453/616http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/453/616https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/453/616https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/453/616http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/453/616GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/453/616/table1 (Near-IR photometry of the 12 micron galaxy sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/453/616/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/453/616/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/453/616/table1?GETtext/xml+votable180.050000true1.57582720.2005360.005555555555555556Cone search capability for table J/ApJ/453/616/table2 (Near-IR photometry of galaxies excluded from the 12 micron sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/453/616/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/453/616/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/453/616/table2?GETtext/xml+votable180.050000true0.79452421.9625350.0055555555555555566/203 226 231 286 538 627 664 700 709 909 932 941 2309 2564 4381 4423 4439 4446 4447 4695 5067 5116 5130 5200 5241 5306 5342 5572 5589 5596 5610 5634 5639 5751 5793 5796 5799 5966 5975 5995 5999 6034 6037 6261 6977 7030 7234 7386 7424 7550 7552 7602 7604 7743 7763 8225 8256 8331 8458 8482 8492 8506 8673 8729 8845 8922 8997 9133 9455 9882 9894 9895 10210 10213 10265 10364 10402 10453 10475 10628 10650 10761 10878 10905 10912 10927 10987 10990 10991 11000 11006 11010 11180 11206 11227 11246 11273 11362 11372 11392 11446 11457 11800 11832 11939 12004 12306 15333 16045 16453 16470 16531 16655 16690 16740 16755 16758 17061 17183 17252 17281 17486 17492 17509 17736 17747 17748 17754 17755 17927 18055 18206 18209 18212 18387 18402 18406 18427 18683 18714 18809 19070 19283 19619 19730 19883 20014 20023 20060 20061 20090 20118 20208 20226 20230 20315 21016 21198 22632 22638 22644 22654 22751 22792 22973 23160 23171 23233 23323 23339 24598 24735 24740 24824 24838 24948 24949 24957 24958 25136 25172 25312 25344 25460 25599 25635 25762 25772 25775 25946 25971 25979 26121 26148 26161 26175 26210 26223 26234 26264 26265 26292 26323 26472 26811 26932 27017 27096 27098 27191 27255 27285 27345 27365 27426 27514 27604 27712 27728 27767 27773 27814 27828 27862 27863 27909 27914 27937 28038 28141 28167 28172 28184 28213 28496 28517 28529 28612 31158 31365 31430 31503 32426 32930 32953 33034 33176 33228 33242 33455 33654 33681 34272 34294 34448 34495 34531 34695 34777 34913 35067 35193 35447 35576 35691 35924 35993 36134 36194 36241 36338 36377 36391 36450 36604 36691 36716 36785 36786 36789 36796 36831 36861 36896 38853 38887 38946 40410 40432 40437 40953 43748 43824 43978 43994 44507 44626 44660 44718 44741 44866 44896 45054 45112 45126 45462 45497 45558 46130 46438 46481 46811 46882 46987 47029 48292 48665 48744 490427.952274030004205e-20 1.0188844282367877e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/453/616?format=asciiOpticalInfrareddefaultJ/ApJ/453/616/table1Near-IR photometry of the 12 micron galaxy samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of galaxymeta.id;meta.maincharRAB1950? Right ascension (B1950.0), from IRAS FSCpos.eq.ra;meta.mainnullableDEB1950? Declination (B1950.0), from IRAS FSCpos.eq.dec;meta.mainnullableFnuJ? J-band flux densitymJyphot.flux.density;em.IR.Jfloatnullableu_FnuJFnuJ uncertainty flagmeta.code.errorcharFnuHH-band flux densitymJyphot.flux.density;em.IR.Hfloatu_FnuHFnuH uncertainty flagmeta.code.errorcharFnuK? K-band flux densitymJyphot.mag;em.IR.Kfloatnullableu_FnuKFnuK uncertainty flagmeta.code.errorcharFnuL? L-band flux densitymJyphot.flux.density;em.IR.3-4umfloatnullableu_FnuLFnuL uncertainty flagmeta.code.errorcharDiamDiameter of observing aperturearcsecphys.angSizeintDateSite (ESO or SPM [San Pedro Martir]) and datemeta.id;instr.obstycharType[0-4] Object Type: 1, 2 = Seyfert1,2; 3 = IR-luminous; 4 = Liner; 0 = normalsrc.classintFlagFlags explaining why object was observedmeta.code.errorchar_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data)pos.eq.ranullableindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data)pos.eq.decnullableindexedJ/ApJ/453/616/table2Near-IR photometry of galaxies excluded from the 12 micron sampleu_FnuJFnuJ uncertainty flagmeta.code.errorcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of galaxymeta.id;meta.maincharRAB1950? Right ascension (B1950.0), from IRAS FSCpos.eq.ra;meta.mainnullableDEB1950? Declination (B1950.0), from IRAS FSCpos.eq.dec;meta.mainnullableFnuJ? J-band flux densitymJyphot.flux.density;em.IR.JfloatnullableFnuHH-band flux densitymJyphot.flux.density;em.IR.Hfloatu_FnuHFnuH uncertainty flagmeta.code.errorcharFnuK? K-band flux densitymJyphot.mag;em.IR.Kfloatnullableu_FnuKFnuK uncertainty flagmeta.code.errorcharFnuL? L-band flux densitymJyphot.flux.density;em.IR.3-4umfloatnullableu_FnuLFnuL uncertainty flagmeta.code.errorcharDiamDiameter of observing aperturearcsecphys.angSizeintDateSite (ESO or SPM [San Pedro Martir]) and datemeta.id;instr.obstycharType[0-4] Object Type: 1, 2 = Seyfert1,2; 3 = IR-luminous; 4 = Liner; 0 = normalsrc.classintFlagFlags explaining why object was observedmeta.code.errorchar_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data)pos.eq.ranullableindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data)pos.eq.decnullableindexedJ/ApJ/453/616/table3Derived NIR parameters for the 12 micron galaxy samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of galaxymeta.id;meta.maincharzRedshift (corrected as described in RMS93)src.redshiftdoublelog(FJmag)[]? Computed total flux in the J bandlog(mJy)phot.flux.density;em.IR.Jfloatnullablelog(FHmag)[]? Computed total flux in the H bandlog(mJy)phot.flux.density;em.IR.Hfloatnullablelog(FKmag)[]? Computed total flux in the K bandlog(mJy)phot.mag;em.IR.KfloatnullableJ-H[]? J-H color, smallest available aperturemagphot.color;em.IR.J;em.IR.HfloatnullableH-K[]? H-K color, smallest available aperturemagphot.color;em.IR.H;em.IR.KfloatnullableK-L[]? K-L color, smallest available aperturemagphot.color;em.IR.K;em.IR.3-4umfloatnullableApert[]? Aperture for colors (for [H-K] if different for each)arcsecinstr.fovintnullablelog(LNIR)[]? Luminosity integrated over 1.2-3.4umlog(1e-07W)phys.luminosity;em.IRfloatnullablelog(LFIR)Luminosity integrated over IRAS wavebandslog(1e-07W)phys.luminosity;em.IRfloatlog(LTOT)[]? Bolometric luminositylog(1e-07W)phys.luminosityfloatnullableType[0-4] Object Type: 1, 2 = Seyfert1,2; 3 = IR-luminous; 4 = Liner; 0 = normalsrc.classintFlagFlags pertaining to apertures and colorsmeta.code.errorchar