The baryonic Tully-Fisher relation and its implication for dark matter halos

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Volume 505 / No 2 (October II 2009)

A&A, 505 2 (2009) 577-587

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Table 2:

Derived parameters for the profile width sub-sample.
ID	$\alpha_{2000}$	$\delta_{2000}$	$V_{\rm sys}$	D	M_V	(V-I)	$M_{\rm HI}$	W₂₀	W₅₀	W₂₀ $_{\rm {,~turb}}$	W₅₀ $_{\rm {,~turb}}$	i
	(h m s)	( $\circ~~~ \hbox{$^\prime$ }~~~ \hbox{$^{\prime\prime}$ }$ )	km s^-1	Mpc	mag		10⁷ $M_{\odot}$	km s^-1	km s^-1	km s^-1	km s^-1	$^\circ$
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)
D572-5	11 48 16.4	+18 38 33	994	14.6	-14.56	0.52	8.55	77	62	68	55	50^a
D575-1	12 51 46.1	+21 44 07	600	10.0	-14.22	0.70	3.76	38	24	30	18	53
D575-5	12 55 41.4	+19 12 34	437	7.7	-13.21	0.44	4.27	28	19	16	10	50
D640-13	10 56 13.9	+12 00 41	958	13.4	-14.36	0.55	4.53	38	25	30	18	48^a
D646-7	12 58 40.4	+14 13 03	233	2.1^b	-12.52	0.84	0.37	35	23	26	16	55^a

^a Optical I-band inclination from Pildis et al. (1997).
^b Distance as given in Karachentsev et al. (2003).
Notes: (1) galaxy identifier; (2, 3) central position taken from NED; (4) systemic velocity derived from the central velocity of the W₅₀ profile; (5) distance in Mpc. If no reference is given, the distance is based on $V_{\rm sys}$ (Col. 4) and a Hubble flow using $H_0=75\rm {~{km}~{s}^{-1}~Mpc^{-1}}$ , including a correction for Virgocentric infall (Mould et al. 2000); (6) absolute V-band magnitude as given in Pildis et al. (1997), corrected to our distance estimates; (7) V-I color from Pildis et al. (1997); (8) total H I mass (in units of $10^7~M_{\odot}$ ); (9) uncorrected width of the H I profile at the 20 percent level of the maximum intensity. The values listed here for W₂₀ are derived using the Hanning smoothed data; (10) as Col. 9, but for the W₅₀ profile; (11) width of the W₂₀ profile, corrected for the finite velocity resolution, and turbulent motion of the H I gas; (12) as Col. 11, but for the W₅₀ profile; (13) adopted inclination angle. The velocity widths in Cols. (9)-(12) are not corrected for inclination effects.

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