TABLE OF PHOTOMETRIC AND SPECTROSCOPIC PARAMETERS for 304 CF GALAXIES |
Field Name | Description |
UGC | The galaxy UGC number. The last two entries refer to CGCG reference number |
N | n, the total number of spectroscopic observations per galaxy; |
EPS | eps, the ellipticity of the best-fitting isophote on the disk-dominated part of the galaxy profile (see C96); |
INCL | incl, inclination computed with an intrinsic flattening, q0 = 0.18; |
vhel | vhel, the heliocentric redshift in km/sec. Defined as the center of symmetry of the rotation curve as measured with Model 2 (cf C97); |
vlg | vlg, the radial velocity corrected for motion with respect to the Local Group; vlg = vhel + 300 sin(l)cos(b); <-- fix! |
vcmb | vcmb, the radial velocity in the frame of the Cosmic Microwave Background. The correction uses the motion of the Sun with respect to the CMB frame determined by the COBE dipole anisotropy (Kogut \etal 1993); |
dv15q | dv15q, the velocity width measured from the flux-weighted rotation profile at 15\% of the total area; |
eta15 | eta15 = log(dv15q) - 2.5; |
dv20q | dv20q, same as $W_{15}$ but measured at 20\% of the total area; |
eta20 | eta20 = log(dv20q) - 2.5; |
vmax | vmax, maximum velocity of RC model 2 (as in C97); |
evmax | evmax = log(vmax) - 2.5; |
vdisk | vdisk (equivalent to v2.2), velocity measured from Model 2 at 2.15 disk scalelengths (peak velocity for pure disk); |
evdisk | evdisk = log(vdisk) - 2.5; |
viso | viso, "Isophotal" velocity measured from Model 2 at the isophotal level of 23 mag/arcsec^-2; |
eviso | eviso = log(eviso) - 2.5; |
vopt | vopt, the velocity from Model 2 measured at r_opt = 3.2h (optical radius as defined by Persic & Salucci); |
evopt | evopt = log(vopt) - 2.5; |
Whist | Whist, the velocity difference between the 10th and 90th (interpolated) percentile points in the ranked distribution of velocities; |
ewhist | ewhist = log(Whist) - 2.5; |
ls_m | ls_m, the mean logslope dlogv/dlogr from Model 2 using bootstrap least- square fits between r_disk (=2.15h) and the last fitted velocity point; |
ls_r | ls_r, the logslope measured from the observed RC between r_disk and the last measured velocity point; |
ls23 | ls23, the logslope measured from the observed RC between r_disk and 3 exponential disk scale lengths; |
n_23 | n_23, the number of points used to bootstrap ls_23; |
sd23 | sd23, the 1 sigma deviation for the 100 random realizations in ls_23; |
ls24 | ls24, the logslope measured from the observed RC between r_disk and 4 exponential disk scale lengths; |
n_24 | n_24, the number of points used to bootstrap ls_24; |
sd24 | sd24, the 1 sigma deviation for the 100 random realizations in ls_24 |
r23kpc | r23kpc, the corrected radius at the 23 r mag arcsec^{-2} isophote in kpc. Isophotal radii are corrected for both Galactic extinction effects and cosmological stretch (as in C96). The transformation to kpc assumes a distance from the vlg redshift and a Hubble constant of 70 km/sec/Mpc; |
r24kpc | r24kpc. Analogous to r23kpc; |
r25kpc | r25kpc. Analogous to r23kpc and r24kpc; |
rmaxkpc | rmaxkpc, the maximum radius in kpc from the last measured detection on either side of the RC; |
rmax | rmax, same as rmaxkpc but expressed in arcsec; |
h_sec | h["], the corrected scalelength in arcsec. Values from Broeils & Courteau '96 (1D B/D) were adopted when available. All scalelengths are corrected for cosmological stretch. Galactic extinction is irrelevant; |
hkpc | hkpc, the corrected disk scalelength in kpc; |
rmax_ropt | rmax/ropt, the maximum RC radius divided by the optical radius measured at 3.2 disk scalelength; |
rmax_h | rmax/h, the maximum RC radius divided by the disk scalelength; |
rp_h | rp/h, radius where the rotation curve peaks (often last point of RC) divided by the disk scalelength; |
rmag23 | rmag23, the corrected apparent magnitude at the 23 mag arcsec^{-2} level. Isophotal and total magnitudes are corrected for Galactic reddening (abcor) and internal extinction (extcor) (see C96); |
rmag24 | rmag24, the corrected apparent magnitude at the 24 mag arcsec^{-2} level; |
rmag25 | rmag25, the corrected apparent magnitude at the 25 mag arcsec^{-2} level; |
abcorr | abcorr, correction for r-band Galactic extinction (C96); |
extcorr | extcorr, correction for r-band internal extinction (C96); |
rmag | rmag (m_r^c), the corrected r-band total extrapolated apparent magnitude; |
rm2_2 | rm2_2, corrected apparent magnitude measured inside r_disk; |
absm23 | absm23, absolute magnitude of fully corrected rmag23. Absolute magnitudes are computed using LG redshifts and H0=70; |
absm25 | absm25, absolute magnitude of fully corrected rmag25; |
absm2_2 | absm2_2, absolute magnitude of fully corrected rm2_2; |
absmr | absmr, absolute magnitude of fully corrected rmag. absmr = rmag - 5log D[Mpc] + 25; |
absBRC3 | absBRC3, absolute magnitude of B-band magnitude from fully corrected RC3 raw magnitudes. The correction for Galactic extinction follows a Burstein-Heiles prescription with $A_B = 0.xx$ and our internal correction uses B_Tcorr = B_T - 1.45*loga/b - loga/b_70 Use $A_B = 1.45$ following Cardiff paper Burstein, Willick, \& Courteau 1996; |
B_r | B-r color term (51 - 50). The mean value is 0.74 +/- 0.23; |
L_B | L_B, absolute B-band luminosity in solar units /1E10. Assumes $M_B\odot$ = 5.41; |
L_B_star | L_B*, absolute B-band luminosity divided by Schecter's L* in the B-band. I use M*B = -19.5 + 5.*alog10H0/100. from Stromlo-APM survey. For H0=70, M*B=-20.27 and L*=1.88E+10 in solar units; |
D_T | D/T, the ratio if fitted disk light to total measured light for the whole galaxy; |
D_M2_2 | D/M2_2, the ratio if fitted disk light to measured light inside r_disk; |
CSB | CSB, central surface brightness from disk fits; |
DIST | DIST, the distance of the galaxy in Mpc, computed as D = vlg/H0 (Inferred TF distances are discarded since peculiar motions are more uncertain than distance errors); |
FACT | FACT, conversion factor to change arcseconds into kpc; |
Gamma | Gamma, the exponent term in Model 2 (see function summary below); |
Rt_Ropt | Rt/Ropt, the turnaround radius in Model 2 divided by the optical radius; |
F | F, the Freeman Type (I or II); |
QHF | QHF, 0/1 if the galaxy is away from/included in the Quiet Hubble flow; |
The rotation curve parameterization (Model 2) has the form: vr = v_0 + v_c * 1+x^b / 1 + x^g^1/g, where x = r_t/r-r_0 where: a1 = v_0 velocity center a2 = r_0 position center a3 = v_c asymptotic velocity (positive if curve has + slope negative if curve has - slope) a4 = r_t turnover radius between solid-body and flat part a5 = Gamma sharpness of turnover a6 = Beta flat curve drop-off index------------------------------------------------------------------------------