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J/ApJ/453/616   JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)

Multiwavelength energy distributions and bolometric luminosities of the 12 micron galaxy sample Spinoglio L., Malkan M.A., Rush B., Carrasco L., Recillas-Cruz E. <Astrophys. J. 453, 616 (1995)> =1995ApJ...453..616S
ADC_Keywords: Galaxies, photometry ; Photometry, infrared Keywords: galaxies: active - galaxies: nuclei - galaxies: photometry - galaxies: Seyfert - galaxies: starburst - infrared: galaxies Abstract: Aperture 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. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1 79 408 Near-IR photometry of the 12 micron galaxy sample table2 79 19 Near-IR photometry of galaxies excluded from the 12 micron sample table3.dat 77 514 Derived NIR parameters for the 12 micron galaxy sample
See also: VII/157 : The extended 12um galaxy sample (Rush+ 1993) Byte-by-byte Description of file: table1 table2
Bytes Format Units Label Explanations
1- 12 A12 --- Name Name of galaxy 14- 15 I2 h RAh *? Right ascension (B1950.0), from IRAS FSC 17- 18 I2 min RAm *? Right ascension (B1950.0), from IRAS FSC 20- 23 F4.1 s RAs *? Right ascension (B1950.0), from IRAS FSC 25 A1 --- DE- Declination sign 26- 27 I2 deg DEd *? Declination (B1950.0), from IRAS FSC 29- 30 I2 arcmin DEm *? Declination (B1950.0), from IRAS FSC 32- 33 I2 arcsec DEs *? Declination (B1950.0), from IRAS FSC 35- 40 F6.1 mJy FnuJ ? J-band flux density 41 A1 --- u_FnuJ FnuJ uncertainty flag 42- 47 F6.1 mJy FnuH H-band flux density 48 A1 --- u_FnuH FnuH uncertainty flag 49- 54 F6.1 mJy FnuK ? K-band flux density 55 A1 --- u_FnuK FnuK uncertainty flag 56- 61 F6.1 mJy FnuL ? L-band flux density 62 A1 --- u_FnuL FnuL uncertainty flag 63- 65 I3 arcsec Diam Diameter of observing aperture 67- 73 A7 --- Date Site (ESO or SPM [San Pedro Martir]) and date 75 I1 --- Type [0-4] Object Type: 1, 2 = Seyfert1,2; 3 = IR-luminous; 4 = Liner; 0 = normal 77- 79 A3 --- Flag *Flags explaining why object was observed
Note on RAh, RAm, RAs, DEd, DEm, DEs: Positions from IRAS FSC II/156. Blank when the galaxy is not in IRAS FSC. Note on Flag: a: originally in the 12-Micron Sample, based on its flux in the FSC-2, but later excluded because the ADDSCAN flux is below the sample limit (see Appendix A of Rush, Malkan, and Spinoglio 1993 VII/157, hereafter RMS93) b: in Spinoglio & Malkan (1989ApJ...342...83S) c: unidentified object excluded from the 12-Micron Sample in RMS93 VII/157 (see Table 12 of RMS93).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Name of galaxy 14- 20 F7.5 --- z Redshift (corrected as described in RMS93) 22- 25 F4.2 [mJy] log(FJmag) []? Computed total flux in the J band 27- 30 F4.2 [mJy] log(FHmag) []? Computed total flux in the H band 32- 35 F4.2 [mJy] log(FKmag) []? Computed total flux in the K band 37- 40 F4.2 mag J-H []? J-H color, smallest available aperture 42- 45 F4.2 mag H-K []? H-K color, smallest available aperture 47- 50 F4.2 mag K-L []? K-L color, smallest available aperture 52- 53 I2 arcsec Apert []? Aperture for colors (for [H-K] if different for each) 55- 59 F5.2 [10-7W] log(LNIR) []? Luminosity integrated over 1.2-3.4um 61- 65 F5.2 [10-7W] log(LFIR) Luminosity integrated over IRAS wavebands 67- 71 F5.2 [10-7W] log(LTOT) []? Bolometric luminosity 73 I1 --- Type [0-4] Object Type: 1, 2 = Seyfert1,2; 3 = IR-luminous; 4 = Liner; 0 = normal 75- 77 A3 --- Flag *Flags pertaining to apertures and colors
Note on Flag: a A Seyfert galaxy for which the authors only have whole-galaxy (extrapolated) colors and thus no aperture is given b An object for which no aperture was given with the reference, but where the authors can assume that these are whole-galaxy fluxes because it is very point-like J The [J-H] is from a larger aperture than the [H-K] color (10 objects) L The [K-L] is from a larger aperture than the [H-K] color (7 objects)
Origin: AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 04-Nov-95
(End) [CDS] 29-Jan-1996
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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