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J/AJ/113/22         Tully-Fisher Relation. I. (Giovanelli+ 1997)

The I Band Tully-Fisher Relation for Cluster Galaxies: Data Presentation Giovanelli R., Haynes M.P., Herter T., Vogt N.P., Wegner G., Salzer J.J., Da Costa L.N., Freudling W. <Astron. J. 113, 22 (1997)> =1997AJ....113...22G (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Photometry ; Morphology ; Radial velocities Abstract: 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. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2 128 782 Galaxy parameters, by cluster table2.tex 140 1328 AASTeX version of table2
Byte-by-byte Description of file: table2
Bytes Format Units Label Explanations
1- 16 A16 --- Cluster Cluster name 18- 23 A6 --- Name1 *First identification name 25- 32 A8 --- Name2 *Second identification name 35- 36 I2 h RAh Right ascension, 1950.0 37- 38 I2 min RAm Right ascension, 1950.0 39- 42 F4.1 s RAs Right ascension, 1950.0 44 A1 --- DE- Sign of declination 45- 46 I2 deg DEd Declination, 1950.0 47- 48 I2 arcmin DEm Declination, 1950.0 49- 50 I2 arcsec DEs Declination, 1950.0 52- 54 A3 --- T *Hubble morphological type 56- 60 I5 km/s Vcmb Radial velocity in the Cosmic Microwave Background (CMB) reference frame 62- 65 F4.1 deg Theta Angular distance from center of cluster 68- 69 A2 --- Mem *Membership code 71- 73 I3 km/s W ? Measured velocity width 75- 77 I3 km/s W1 ? Velocity width, corrected except for inclination 79- 81 I3 km/s Wcor ? Velocity width, converted to edge-on 83- 85 I3 deg Inc Adopted inclination of plane of disk 88- 92 F5.3 --- log(Wcor) ? Log10 of Wcor 94- 96 I3 10-3 e_log(Wcor) *? Estimated uncertainty in log(Wcor) 99-103 F5.2 mag Imag *Measured and extrapolated I band mag. 105-109 F5.2 mag Icor *Corrected apparent magnitude 112-117 F6.2 mag Mcor *? Corrected absolute magnitude 119-120 I2 0.01mag e_Mcor *? Uncertainty of Mcor 122 A1 --- u_Mcor Uncertainty flag on Mcor 124 A1 --- Ref1 *Reference code for photometry 126 A1 --- Ref2 *Reference code for velocity width 128 A1 --- Note *[*] Indicates notes in printed paper
Note to Name1: 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. Note to Name2: 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. Note to T: 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. Note to Mem: 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 Note to e_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. Note to Imag: 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. Note to Icor: Apparent magnitude, to which k-term, galactic, and internal extinction corrections were applied. Note to Mcor: 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. Note to e_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. Note to Ref1: 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 Note to Ref2: A numerical cote idmn4ifies 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 to Note: If an asterisk appears in this column a note for this galaxy is given in the printed paper. Origin: AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 06-Nov-1996
(End) Patricia Bauer [CDS] 11-Feb-1997
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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