J/AJ/113/22 J/AJ/113/22 Tully-Fisher Relation. I. R Giovanelli M P Haynes T Herter N P Vogt G Wegner J J Salzer L N Da Costa W Freudling Astron. J. 113 22 1997 1997AJ....113...22G Clusters, galaxy Morphology Photometry Radial velocities Observational parameters which can be used for redshift-independent distance determination using the Tully-Fisher (TF) technique are given for 782 spiral galaxies in the fields of 24 clusters or groups. I band photometry for the full sample was either obtained by us or compiled from published literature. Rotational velocities are derived either from 21 cm spectra or optical emission line long-slit spectra, and converted to a homogeneous scale. In addition to presenting the data, a discussion of the various sources of error on TF parameters is introduced, and the criteria for the assignment of membership to each cluster are given.

Cluster Cluster name --- Name1 First identification name If the galaxy is listed in the UGC catalog, the UGC number is listed first; if not, the first listing corresponds to the author's internal coding number. --- Name2 Second identification name The second name is added with the following priority scheme: NGC or IC number; CGCG number in the form "field-number"; for southern galaxies, if and NGC or IC number is not available the ESO/Uppsala catalog name is given. --- RAh Right ascension, 1950.0 h RAm Right ascension, 1950.0 min RAs Right ascension, 1950.0 s DE- Sign of declination --- DEd Declination, 1950.0 deg DEm Declination, 1950.0 arcmin DEs Declination, 1950.0 arcsec T Hubble morphological type Morphological type code in the RC3 scheme, where 1 corresponds to Sa, 3 to Sb, 5 to Sc, etc. If the code is followed by a B, the galaxy disk has an identifiable bar. --- Vcmb Radial velocity in the Cosmic Microwave Background (CMB) reference frame km/s Theta Angular distance from center of cluster deg Mem Membership code c - galaxy is considered a bona fide cluster member g - galaxy is sufficiently removed from the cluster center that cluster membership cannot be safely assigned; the galaxy is, however, in the periphery of the cluster, at roughly the same redshift and it is a nearby supercluster member f - foreground galaxy b - background galaxy --- W Measured velocity width km/s W1 Velocity width, corrected except for inclination km/s Wcor Velocity width, converted to edge-on km/s Inc Adopted inclination of plane of disk deg log(Wcor) Log10 of Wcor --- e_log(Wcor) Estimated uncertainty in log(Wcor) The uncertainty takes into account both measurement errors and uncertainties arising from the corrections. The value (11), for example is equivalent to +/- 0.011. 10-3 Imag Measured and extrapolated I band mag. Measure I band magnitude, extrapolated to infinity assuming that the surface brightness profile of the disk is well described by an exponential function; this value is sometimes adopted as an average of two or more measurements, as footnoted. mag Icor Corrected apparent magnitude Apparent magnitude, to which k-term, galactic, and internal extinction corrections were applied. mag Mcor Corrected absolute magnitude Absolute magnitude, computed assuming that the galaxy is at the distance indicated either by the cluster redshift, if the galaxy is a member, or by the galaxy redshift if not. mag e_Mcor Uncertainty of Mcor The uncertainty on the magnitude is the sum in quadrature of the measurement errors and the estimate of the uncertainty in the corrections applied to the measured parameter. The error estimate does not include the uncertainty on the value of the distance. 0.01mag u_Mcor Uncertainty flag on Mcor --- Ref1 Reference code for photometry A letter code identifies the source for the photometry: a - Authors' photometric observations b - Bernstein et al. 1994AJ....107..1962B, restricted to Coma h - Han & Mould 1992ApJ...396..453H m - Mathewson, Ford, & Buchhorn 1992ApJS...81. 413M p - Pierce & Tully 1988ApJ...330..579P, restricted to Ursa Major s - Bureau et al. 1996ApJ...463...60B, restricted to Fornax x - Combination of different sources as noted --- Ref2 Reference code for velocity width A numerical code identifies the source of velocity width: 0 - Author's 21 cm measurements 1 - Author's optical spectroscopy 2 - Averages of several measurements, see notes 3 - 21 cm observations of Gavazzi 1987ApJ...320...96G and Scodeggio & Gavazzi 1993ApJ...409..110S 4 - 21 cm observations of Bothun et al. 1985ApJS...57..423B, and Aaronson et al. 1989ApJ...338..654A, cross-identified with the compilation of Bottinelli et al. 1990A&AS...82..391B 5 - 21 cm measurements of Mathewson, Ford, & Buchhorn 1992ApJS...81. 413M 6 - Optical spectroscopy of Mathewson, Ford, & Buchhorn 1992ApJS...81. 413M 7 - 21 cm measurements of Pierce & Tully 1988ApJ...330..579P 8 - 21 cm observations of Fontanelli 1984A&A...138...85F; Lewis 1985ApJS...59. 161L; and Schneider et al. 1991ApJS...72.2455S 9 - 21 cm observations of Bureau et al. 1996ApJ...463...60B --- Note Indicates notes in printed paper If an asterisk appears in this column a note for this galaxy is given in the printed paper. --- table2.texAASTeX version of table2 Patricia Bauer CDS 1997Feb11AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 06-Nov-1996 J_AJ_113_22.xml