Fornax dSph - Data Tables
Mateo 1998 (Annual Review of Astronomy and Astrophysics)
Table 1: Distance and Heliocentric Velocity
l b E(B-V) (m-M)_0 Distance Ref V_h,opt V_h,radio Ref Notes
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
237.1 -65.7 0.03 ±0.01 20.70 ±0.12 138 ±8 56 53 ±3 --- 4,57,142 C
Columns 1 and 2: Galactic longitude and latitude.
Column 3: Foreground reddening.
Column 4: True distance modulus.
Column 5: Distance. (kpc)
Column 6: Distance/reddening references.
Column 7: Heliocentric velocity based on optical measurements. (km/s)
Column 8: Heliocentric velocity based on radio measurements. (km/s)
Column 9: Velocity references.
Column 10: Notes.
Notes:
C. No HI detected. (see Table 4 for limits)
Ref:
[4] Huchtmeier & Richter (1986);
[56] Beauchamp et al (1995);
[57] Mateo et al (1991b);
[142] Knapp et al (1978);
Table 2: Integrated Photometric Properties and Structural Parameters
V_T (B-V)_T Other Colors Sigma_0 r R PA e r_e Ref Notes
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
7.6 ±0.3 0.63 ±0.05 0.08 [1];0.45 [2];1.02 [3] 23.4 ±0.3 13.8 ±0.8 71 ±4 48 ±6 0.31 ±0.03 10.2 5,20-22,24,50
Column 1: Integrated apparent V-band magnitude.
Column 2: Integrated (B-V) color.
Column 3: Other integrated colors. [1] = (U-B), [2] = (V-R), [3] = (V-I)
Column 4: V-band central surface brightness. (mag/arcsec^2)
Column 5: Core radius. (arcmin)
Column 6: Tidal radius. (arcmin)
Column 7: Major-axis position angle (°), with N = 0° and E = 90°.
Column 8: The ellipticity of the outer parts of the galaxy, defined as e=(1 - b/a), where b=minor axis and a=major axis.
Column 9: The exponential scale length of the surface-brightness distribution, typically along the major axis.(arcmin)
Column 10: References.
Ref:
[5] Caldwell et al (1992);
[20] Irwin & Hatzidimitriou (1995);
[21] Hodge & Smith (1974);
[22] de Vaucouleurs & Ables (1968);
[24] Poulain & Nieto (1994);
[50] Demers et al (1994b);
Table 3: Derived Photometric and Kinematic Properties
M_V M_B L_V R_c rho_0 I_0 M_tot (M/L)_0,V (M/L)_tot,V M_HI/M_tot M_HI/L_B
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
-13.2 -12.6 15.5 460 0.086 0.018 68 4.8 4.4 <0.001 <0.001
Column 1: Integrated V-band absolute magnitude.
Column 2: Integrated B-band absolute magnitude.
Column 3: Visual luminosity in units of 10^6 L_0.
Column 4: `Core' radius in parsecs, corresponding to the observed core radius, r_c, when available, or 1.25 times r_e
if r_c is not measured but the exponential scale length is measured (compare with Bender et al 1991; the average of
r_c/r_e for the 18 galaxies in Table 3 with both radii is 1.27 ±0.12), or a/3 if neither r_c nor r_e is available,
where a is the observed Holmberg semi-major axis as defined in Table 3.
Column 5: The central mass density in M_0/pc^3, here approximated as rho_0 = 166 sigma_0^2/R_c, where sigma_0 is the
central velocity dispersion in km/s, and R_c is in pc; this is computed only for systems that are pressure supported
(see Mateo et al 1991b for details). For rotating Local Group dwarfs, the central mass density is dominated by the
visible material and has been approximated as 2.5 I_0, where I_0 is defined in the explanation of column 6 (see Note F).
Column 6: The central luminosity density in L_o/pc^3, taken as I_0 = S_0/2 r_c, where S_0 is the central surface
brightness expressed in units of L_0/pc^2, and r_c is in pc (see Mateo et al 1991b for details).
Column 7: The total mass; if a central velocity dispersion is known and exceeds the rotational velocity, then M_tot =
167 beta R_c sigma_0^2, where beta is a scaling factor for King profiles taken to be 8.0 here, appropriate for
low-concentration King models. If v_rot > sigma_0, then M_tot = R_rot v_rot^2/G, where v_rot is the rotational
velocity -- corrected for the galaxy inclination -- at the projected distance R_{rot} from the galaxy center.
Column 8: The central V-band mass-to-light ratio, defined as rho_0/I_0, in solar units.
Column 9: The integrated V-band mass-to-light ratio defined as M_tot/L_V, in solar units.
Column 10: The ratio of integrated H I mass to the total mass, M_tot from column 7.
Column 11: The ratio of the integrated H I mass and the blue luminosity, in solar B-band units;
Table 4: Integrated and Derived Properties of the ISM
S(HI) M(HI) Ref f60 f100 M_d(FIR) Dust Ref
(1) (2) (3) (4) (5) (6) (7) (8)
<1.05 <0.005 1,20 <17 <86 0.0 --- 12
Column 1: Integrated 21-cm flux.(Jy km/s)
Column 2: Total HI mass in 10^6 solar units: M_HI = 2.36 times 10^11 F(HI) d^2, where d is the galaxy distance in Mpc, and
F(HI) in Jy km/s.
Column 3: HI References.
Columns 4 and 5: The IRAS 60 microns and 100 microns integrated fluxes. (mJy)
Column 6: The total mass of cool dust in solar units.
Column 7: A flag indicating whether there are optical indicators of dust in the galaxy either through detection of
internal reddening or direct observation of opaque dust clouds.
Column 8: Far-IR and dust references.
Ref:
[1] Huchtmeier & Richter (1986)
[12] Knapp et al (1985)
[20] Knapp et al (1978)
Table 5: Heavy Element Abundances
[Fe/H] sigma_[Fe/H] Ref 12+log(O/H) [N/O] Ref Notes
(1) (2) (3) (4) (5) (6) (7)
-1.3 ±0.2 0.6 ±0.1 24,50 7.98 ±0.4 --- 6,72 F,H
Column 1: The mean iron abundance for the old and intermediate-age stellar populations where
[Fe/H] = log(Z/Z_O).
Column 2: The intrinsic dispersion in [Fe/H]. If the reference gave a full metallicity range
instead of a dispersion, I assumed sigma = 0.5 Delta[Fe/H]. This reasonably approximates
the scaling between these quantities for the few galaxies that have independent estimates of
both sigma_[Fe/H] and Delta[Fe/H].
Column 3: References for the stellar abundances.
Column 4: The oxygen abundance defined as 12 + log(O/H), where (O/H) is the number ratio of
oxygen to hydrogen atoms.
Column 5: The nitrogen to oxygen ratio defined as [N/O] = log(N/O), where (N/O) is the number
ratio of nitrogen to oxygen atoms.
Column 6: References for the oxygen and nitrogen abundances.
Column 7: Notes.
Notes:
F. The oxygen abundance was derived, at least in part, from one or more planetary nebula.
H. The 5 globular clusters are more metal poor on average than the field stars.
Ref:
[6] Richer & McCall (1995);
[72] Maran et al (1984);
Table 6: Internal Kinematic Properties
sigma_* v_rot,* Ref
(1) (2) (3)
10.5 ±1.5 <2.0 24,25
Column 1: The stellar central velocity dispersion. (km/s)
Column 2: The rotation velocity from stellar velocity measurements.(km/s)
Column 3: Optical kinematic references.
Ref:
[24] Mateo et al (1991b);
[25] Paltaglou & Freeman (1987);
Table 7: Summary of the Content
N_RR N_Ceph N_Mira N_AC Refs N_OBA N_WR N_HII N_Dust N_AGB N_PN N_GC Refs Notes
(1) (2) (3) (4) (5) (6) (7) (8) (9 ) (10) (11) (12) (13) (14)
400+ 1 30 1 52,70,75,136 --- --- --- --- 82 1 5 10,32,106,115,116,143 F,G
Columns 1-4: The census of known populations of variable stars: RR Lyr stars, Cepheids, Mira (long-period) variables,
and Anomalous Cepheids.
Column 5: References for variable stars.
Columns 6-9: The census of tracers of young populations: OB associations, Wolf-Rayet stars, H II regions, and discrete
dust clouds.
Columns 10-12: The census of known intermediate-age and old-age population tracers: asymptotic giant branch stars,
planetary nebulae, and globular clusters.
Column 13: References for the intermediate-age and old-age tracers.
Column 14: Notes
Notes:
F. Approximately 21 RR Lyr stars may be associated with Fornax cluster 1 (Smith et al 1996).
G. The Cepheid is most likely a W Vir or Pop II Cepheid (Light et al 1986).
Ref:
[5] Armandroff et al (1993)
[10] Aaronson et al (1983)
[32] Hodge (1988)
[52] Nemec et al (1988)
[70] Demers & Irwin (1987)
[75] Light et al (1986)
[106] Richer & Westerlund (1983)
[115] Maran et al (1984)
[116] Danzinger et al (1978)
[136] Mateo et al (1998a)
[143] Azzopardi (1994)