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J/ApJS/173/572      GALEX/Spitzer photometry in NGC 7331     (Thilker+, 2007)

Ultraviolet and infrared diagnostics of star formation and dust in NGC 7331. Thilker D.A., Boissier S., Bianchi L., Calzetti D., Boselli A., Dale D.A., Seibert M., Braun R., Burgarella D., Gil De Paz A., Helou G., Walter F., Kennicutt R.C.JR, Madore B.F., Martin D.C., Barlow T.A., Forster K., Friedman P.G., Morrissey P., Neff S.G., Schiminovich D., Small T., Wyder T.K., Donas J., Heckman T.M., Lee Y.-W., Milliard B., Rich R.M., Szalay A.S., Welsh B.Y., Yi S.K. <Astrophys. J. Suppl. Ser., 173, 572-596 (2007)> =2007ApJS..173..572T
ADC_Keywords: Galaxies, photometry ; Ultraviolet ; Photometry, infrared Keywords: galaxies: evolution - galaxies: individual (NGC 7331) - infrared: galaxies - ultraviolet: galaxies Abstract: We present images of NGC 7331 obtained with GALEX and Spitzer, tracing UV and IR signatures of star formation. NGC 7331's morphology at 8-850um is dominated by a central dust ring. This structure is a vigorous site of star formation (hosting one-third of the present activity) but remains inconspicuous in our GALEX UV imagery. Radial profile analysis and photometry for discrete UV- and UV+IR-selected substructures indicate a decline in UV extinction with increasing galactocentric distance, although highly attenuated star-forming regions can be found throughout the disk. UV-optical surface brightness profiles suggest a recent birthrate parameter (b8) that is highest in the outer part of the disk, even though the local star formation intensity peaks in the ring. Bolometric luminosity and UV attenuation are correlated in substructures on 0.4kpc scales, with a relationship similar to that established for starburst galaxies. Description: The data set assembled for this study, although focused on Spitzer and GALEX observations, spans the radio, millimeter, submillimeter, far-IR (FIR), mid-IR (MIR), near-IR (NIR), visible, and UV bands. Spitzer images of NGC 7331 were obtained with both the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24, 70, and 160um) instruments as part of the SINGS Legacy project. GALEX obtained far-UV (FUV; 1350-1750Å) and near-UV (NUV; 1750-2750Å) direct imaging observations of NGC 7331 for a total duration of 3322s, spanning five visits during 2003 August. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 67 144 Photometry of UV+IR and UV-selected substructures in NGC 7331
See also: J/ApJ/586/794 : Multiwavelength luminosities of galaxies (Bell, 2003) J/A+AS/131/317 : NGC 7331 HII regions catalogue (Petit 1998) J/A+A/285/404 : Star formation in compact groups of galaxies (Moles+ 1994) J/A+A/288/713 : Star formation in galaxies (Firmani+ 1994) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 A8 --- [TBB2007] Name of the substructure (1) 10- 11 I2 h RAh Hour of Right Ascension (J2000) 13- 14 I2 min RAm Minute of Right Ascension (J2000) 16- 19 F4.1 s RAs Second of Right Ascension (J2000) 21 A1 --- DE- Sign of the Declination (J2000) 22- 23 I2 deg DEd Degree of Declination (J2000) 25- 26 I2 arcmin DEm Arcminute of Declination (J2000) 28- 29 I2 arcsec DEs Arcsecond of Declination (J2000) 31- 34 F4.2 kpc2 Area Area of the substructure (1kpc=15arcsec) 36- 37 I2 kpc Dist Distance from galaxy center (1kpc=15arcsec) 39- 43 F5.2 [10-7W] LFUV FUV (153nm) luminosity, log scale (2) 45- 49 F5.2 [10-7W] LNUV NUV (231nm) luminosity, log scale (2) 51- 55 F5.2 [10-7W] L8um 8um luminosity, log scale (2) 57- 61 F5.2 [10-7W] L24um 24um luminosity, log scale (2) 63- 67 F5.2 [10-7W] LIR Total IR (3-1100um) luminosity, log scale (2)
Note (1): [TBB2007] UV+IR-NN or [TBB2007] UV-NN in Simbad. Note (2): The maximum 1σ uncertainty in reported luminosity values for sources included in this table is 0.09dex.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 28-May-2009
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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