J/ApJS/107/97 J/ApJS/107/97 Parameters of 2447 southern spirals D S Mathewson V L Ford Astrophys. J. Suppl. Ser. 107 97 1996 1996ApJS..107...97M Galaxies, photometry Morphology Redshifts Rotational velocities galaxies: distances and redshifts galaxies: kinematics and dynamics galaxies: photometry surveys I-band luminosities, rotational velocities, and redshifts of 1092 spiral galaxies have been measured by CCD photometry and Halpha spectroscopy using the 1m and 2.3m telescopes at Siding Spring Observatory, respectively. The results are tabulated. Luminosity profiles and Halpha rotation curves are given for the galaxies. When these results are combined with similar data for 1355 spiral galaxies published previously (Mathewson, Ford, & Buchhorn, hereafter Paper I, 1992ApJS...81..413M), it provides a large, uniform, and unique data set with which to measure, via the Tully-Fisher relation, the peculiar velocities of galaxies in the local universe to a distance of 11,000km/s (Mathewson & Ford, in Proc. Heron Island Workshop on Peculiar Velocities in the Universe). Taking advantage of the opportunity for publishing this data in machine-readable form, in the CD-ROM, we have also published similar data for the 1355 galaxies in Paper I.

Name Galaxy identification number Galaxy identification number; for galaxies south of -17.5 deg; it is the ESO-Uppsala Catalog (Cat. <VII/34>) number, and for galaxies north of -17.5 deg, it is either the UGC number (Cat. <VII/26>, the NGC (Cat. <VII/1>) or IC designation, or the MCG (Cat. <VII/62>) number. --- RAh Right ascension, 1950 h RAm Right ascension, 1950 min RAs Right ascension, 1950 s DE- Declination sign --- DEd Declination, 1950 deg DEm Declination, 1950 arcmin DEs Declination, 1950 arcsec GLon Galactic longitude deg GLat Galactic latitude deg SGL Supergalactic longitude deg SGB Supergalactic latitude deg Class Classification in the Hubble system --- Type Morphological type, +3 for Sb to +8 for Sd --- aESO Major axis diameter from various catalogs arcmin a Major axis diameter Major and minor axes diameters of the I = 23.5 mag/arcsec2 isophote. arcmin b Minor axis diameter arcmin i Inclination of optical disk Inclination of the optical disk computed from the average of axial ratios of the ellipses of surface brightness I = 22.5, 23.0, and 23.5 mag/arcsec2, following Bothun et al. (1985ApJS...57..423B). deg PA Position angle of the major axis Position angle of the major axis, which is an average of the position angles of the major axes of the ellipses of surface brightness I = 22.5, 23.0, and 23.5 mag/arcsec2 or the P.A. given in the ESO-Uppsala Catalog. deg D0 Face-on diameter Face-on diameter D(0) computed using the relation log D(0) = log(a) - 0.235 log(a/b) + 0.09 Aext where Aext = the absorption in our Galaxy, and the maximum value of a/b is 5 (cf. de Vaucouleurs, de Vaucouleurs, & Corwin 1976, Cat. <VII/112>). arcmin Aext Extinction in our Galaxy in I magnitudes The extinction in our Galaxy in I magnitudes. This has been calculated following Burstein & Heiles (1978ApJ...225...40B). The relation used is Aext=4.05x10^-4F(HI)-0.06. F(HI) is the integrated "zero-velocity" H I flux density in Jy km/s, measured with the 64 m Parkes radio telescope in the direction of each galaxy. The extinction in I is taken to be 42% of that in B. mag Aint Internal extinction in I magnitudes Internal extinction in a galaxy in I magnitudes. The corrections prescribed by Tully & Fouque, (1985ApJS...58...67T), were used to yield "face-on" magnitudes. The extinction in I is taken to be 42% of that in B. mag Kz K correction in I magnitudes K-correction in I magnitudes. The values were taken from Schneider et al. 1983ApJ...264..337S. mag It Total I magnitudes mag Itc Total I magnitudes corrected for extinction Total I magnitudes corrected for internal and external extinction and K dimming: Itc=It-Aext-Aint-Kz. mag ISB Integrated surface brightness Integrated surface brightness in I magnitudes/arcsec2: ISB=c_D(0)+5logD(0)+2.5log(pi) where Ic_D(0)=I_D(0)-Aext-Aint-Kz and I_D(0) are measured from the GASP output files. mag/arcsec2 Vopt Heliocentric systemic velocity, optical Heliocentric systemic velocity taken as the arithmetic mean of the maximum and minimum velocities of the optical rotation curve. km/s Vradio Heliocentric systemic velocity, radio Heliocentric systemic velocity taken as the arithmetic mean of the velocities where the H I profile falls to 50% of the mean of the highest channels in each half of the profile. km/s DVopt Diff. of max and min optical rotation Half the difference between the maximum and minimum values of the optical rotation curve, corrected for relativistic effects, i.e., divided by 1+z. km/s DV50 Diff. of H I profile at 50% intensity Half the widths of the H I profile between points where the intensity falls to 50% of the highest channels in each half of the profile and points corrected for relativistic effects. km/s e_DV50a First uncertainty in DV50 measurement Uncertainties in the measurement of DV50. These errors were calculated by perturbing the 50% level by the rms noise in the spectrum and measuring the amount by which the width changed. km/s e_DV50b Second uncertainty in DV50 measurement km/s DV20 Diff of H I profile at 20% intensity Same as DV50, but for the 20% level. km/s e_DV20a First uncertainty in DV20 measurement Same as e_DV20, but for the 20% level. Sometimes due to noise spikes, unrealistic error values were recorded. In this case, the the error fields may be blank. km/s e_DV20b Second uncertainty in DV20 measurement km/s Vrot Maximum rotation velocity of spiral galaxy Maximum velocity of rotation of the spiral galaxy, obtained by dividing DVopt by sin i. When there was only a radio measurement, DV50 was converted to DVopt using the algorithm DVopt = 1.03 DV50 - 11. km/s u_Vrot Vrot calculated by alternate method The colons after 20 of the Vrot entries indicate that the rotational velocities were derived from radio measurements by M. Haynes and R. Giovanelli, and converted to DVopt using the algorithm DVopt = 1.10 DV50 - 27. --- FHI H I flux density integral H I flux density integral corrected for beam effects. Jy.km/s rms rms noise mJy S/N Peak signal divided by rms noise --- Vcmb Heliocentric systemic velocity in CMB frame Heliocentric systemic velocity converted to the cosmic microwave background (CMB) frame of reference. If both Vopt and Vradio are given, Vopt is used, otherwise Vradio. There is no significant difference between the two values. km/s Vlg Heliocentric velocity in Local Group frame The same as Vcmb, except heliocentric velocities are converted to the frame of the Local Group. km/s CDS 1997Feb03AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 04-Nov-96 J_ApJS_107_97.xml