J/AJ/127/3273 Nearby galaxies HI observations (Vogt+, 2004)
M/L, Hα rotation curves, and H I measurements for 329 nearby cluster and
field spirals. I. Data.
Vogt N.P., Haynes M.P., Herter T., Giovanelli R.
<Astron. J., 127, 3273-3299 (2004)>
=2004AJ....127.3273V 2004AJ....127.3273V
ADC_Keywords: Galaxies, nearby ; H I data ; Morphology ; Radial velocities
Keywords: galaxies: clusters: general - galaxies: evolution -
galaxies: kinematics and dynamics
Abstract:
A survey of 329 nearby galaxies (redshift z<0.045) has been conducted
to study the distribution of mass and light within spiral galaxies
over a range of environments. The 18 observed clusters and groups
span a range of richness, density, and X-ray temperature and are
supplemented by a set of 30 isolated field galaxies. Optical
spectroscopy taken with the 200inch (5m) Hale Telescope provides
separately resolved Hα and [NII] major-axis rotation curves for
the complete set of galaxies, which are analyzed to yield velocity
widths and profile shapes, extents, and gradients. HI line profiles
provide an independent velocity width measurement and a measure of HI
gas mass and distribution. I-band images are used to deconvolve
profiles into disk and bulge components, to determine global
luminosities and ellipticities, and to check morphological
classification. These data are combined to form a unified data set
ideal for the study of the effects of environment upon galaxy
evolution.
Description:
Moderate-resolution long-slit optical spectra were obtained for 329
spiral galaxies with the Hale 200inch telescope using the Double
Spectrograph at the Cassegrain focus (f/15.7) on 51 nights spread
throughout 12 observing runs from 1990 April to 1994 June.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 83 329 Galaxy Parameters I
table3.dat 89 329 Galaxy Parameters II
table4.dat 94 329 Galaxy Parameters III
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Source identification (G1)
17- 18 I2 h RAh Hour of Right Ascension (B1950)
20- 21 I2 min RAm Minute of Right Ascension (B1950)
23- 26 F4.1 s RAs Second of Right Ascension (B1950) (1)
28 A1 --- DE- Sign of the Declination (B1950)
29- 30 I2 deg DEd Degree of Declination (B1950)
32- 33 I2 arcmin DEm Arcminute of Declination (B1950)
35- 36 I2 arcsec DEs Arcsecond of Declination (B1950) (1)
38- 40 A3 --- TType RC3 (Cat. VII/155) morphological type code (2)
42- 46 I5 km/s RV Galaxy radial velocity in CMB reference frame (3)
48- 53 A6 --- Clust Associated cluster (4)
55- 56 A2 --- MCode Membership code (5)
58- 61 F4.2 deg Dist ? Angular distance from cluster center (6)
63- 67 F5.2 --- RSep ? Radial separation from cluster center expressed
in σ (6)
69- 73 F5.3 arcsec Size Angular size, in arcseconds, of 1h-1kpc
75- 78 I4 --- Qual Quality and shape code (7)
80- 82 I3 deg PA Position angle (8)
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Note (1): Positions typically have 15" accuracy.
Note (2): The RC3 (Cat. VII/155) morphological type code (followed by a
"B" when the galaxy disk has an identifiable bar) is defined as follows:
1 = Sa
2 = Sb
5 = Sc
Note (3): This value is obtained from high quality (QHI=1) HI measurements
where available, and otherwise taken from the optical spectra.
Note (4): "Field" for field sources.
Note (5): The membership code is defined as follows:
c = the galaxy is considered a bona fide cluster member
g = the 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 galaxies
b = background galaxies
A, B, C, D = the Cancer group has been recognized to be an assembly of
clumps (Bothun et al. 1983ApJ...268...47B 1983ApJ...268...47B) We use the criteria
given in that reference to assign membership to each of the clumps.
The case of A2634 (RV∼9200km/s) and A2666 (RV∼8100km/s) is also
complicated. Scodeggio et al. (1995ApJ...444...41S 1995ApJ...444...41S) have produced
a detailed study of the region, and within the redshift range
spanned by the two clusters they also distinguished several other
groups. In particular, one of the groups is at a systemic velocity
near 7000km/s, near in redshift to, but distinct from A2666.
g7 = code for the members of the 7000km/s group projected on the
foreground of A2634.
X = field sources
Note (6): As the Cancer group consists of several subclumps, distances have
been measured from the center of the main clump A
(see Bothum et al 1983ApJ...268...47B 1983ApJ...268...47B).
Note (7): A four-digit quality and shape code (1 for high quality), defined
as follows:
Qopt = the quality of the optical spectra,
Qsh = the shape of the rotation curve,
QHI = the quality of the 21cm line spectra,
Qim = the quality of the I-band photometry.
Note (8): The position angle is measured eastwards from north along which
the optical spectrum was observed.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Source identification (G1)
17- 20 F4.1 arcsec Rel Turnover (elbow) point
22- 25 F4.1 arcsec Rf Rotation curve maximum radial extent
27- 31 F5.2 kpc DelHa Differential extent of Hα or [NII]
emission (in h-1kpc, see Table 2)
33- 36 F4.2 kpc RatHa Ratio of the Hα or [NII] emission
differential extent (in h-1kpc, see Table 2)
38- 41 F4.2 --- Sin Measured inner slope (1)
43- 46 F4.2 --- e_Sin Estimated uncertainty in Sin
48- 52 F5.2 --- Sout Measured outer slope (1)
54- 57 F4.2 --- e_Sout Estimated uncertainty in Sout
59- 61 I3 --- Gin ? Measured inner gradient (1)
63- 65 I3 --- Gout ? Measured outer gradient (1)
67- 69 I3 km/s OW0 Measured velocity width
71- 73 I3 km/s OW1 Velocity width corrected for the shape of the
rotation curve and cosmological stretch
75- 77 I3 km/s OW2 ? Corrected velocity width converted to
edge-on viewing
79- 80 I2 km/s e_OW2 Estimated uncertainty in OW2 (2)
82- 84 I3 km/s OW3 ? Corrected velocity width converted to
edge-on viewing measured at 2*Rd
86- 88 I3 km/s e_OW3 Estimated uncertainty in OW3 (2)
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Note (1): As a percentage of the measured optical velocity half-width of
the rotation curves.
Note (2): Taking into account both measurement errors and uncertainties
arising from the corrections.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Source identification (G1)
17- 19 I3 km/s RW0 ? Measured 21cm line profile velocity
width (1)
21- 23 I3 km/s RW1 ? Corrected 21cm line profile velocity
width (2)
25- 27 I3 km/s RW2 ? Converted to edge on viewing 21cm line
profile velocity width
29- 30 I2 km/s e_RW2 ? Estimated uncertainty in RW2
32- 36 F5.2 [10+10solMass] MHIo ? Log of the observed HI mass
38- 42 F5.2 [10+10solMass] MHIp ? Log of the predicted HI mass
44- 45 I2 deg Inc ? Adopted inclination (3)
47- 51 F5.2 mag Imag ? Apparent Mould I band magnitude (4)
53- 58 F6.2 mag IMag ? Absolute Mould I band magnitude (5)
60- 63 F4.2 mag e_IMag ? Estimated uncertainty in IMag (6)
65- 66 I2 % D/T ? Disk percentage of total luminosity
68- 72 F5.2 arcsec Rd ? Exponential disk scale length corrected
to face-on value
74- 77 F4.1 arcsec R23.5 ? Radius at which the surface brightness
profile reaches 23.5mag/arcsec2
79- 82 F4.2 Sun M/Lm ? Measured mass-to-light ratio in solar
units
84- 87 F4.2 Sun M/Lc ? Corrected mass-to-light ratio in solar
units (7)
89- 92 F4.2 --- Dark ? Ratio of dark to light matter within
Rf
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Note (1): Measured at a level of 50% of the profile horns.
Note (2): Corrected for instrumental and data processing broadening, signal
to noise effects, interstellar medium turbulence, and cosmological stretch.
Note (3): Of the plane of the disk to the line of sight
(90° corresponding to edge-on perspective).
Note (4): The apparent I band magnitude, to which k-term, galactic and
internal extinction corrections were applied, measured in Mould I.
Note (5): The absolute I band magnitude, computed assuming that the
galaxy is at the distance indicated either by the cluster redshift, if
the galaxy is a true cluster member, or by the galaxy redshift if it
is not. The calculation assumes H0=100h.km/s/Mpc, so the value
listed is strictly MI+5log(h).
Note (6): 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 (7): Corrected for inclination and extinction effects.
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Global Notes:
Note (G1): The first listing is an internal coding number, which is
equal to the UGC number if the galaxy is listed in the UGC catalog
(Nilson 1973, Cat. VII/26).
A second galaxy name is added with the following priority scheme:
if the galaxy has an NGC or IC number, that coding is entered
preferentially; if the galaxy is listed in the CGCG (Zwicky, Herzog,
& Wild 1968, Cat. VII/49), that coding is listed with second
priority, in the form: field number - ordinal number within the field.
If entries in those three catalogs are not available, a second name is
not entered.
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History:
From electronic version of the journal
References:
Vogt et al., Paper II 2004AJ....127.3300V 2004AJ....127.3300V
Vogt et al., Paper III 2004AJ....127.3325V 2004AJ....127.3325V
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 10-May-2005