A wide-field H I mosaic of Messier 31 - II. The disk warp, rotation, and the dark matter halo

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Table 3:

Andromeda mass estimated at large galactocentric radii.
Reference	R	Mass	$V_{\rm c}$	Objects
	[kpc]	[10¹⁰ $M_\odot$ ]	km s^-1
Evans & Wilkinson (2000)	32	$\rm 39^{+2}_{-10}$	$\rm 230^{+5}_{-32}$	17 Globular Clusters^a
This paper	37	$\rm 49^{+12}_{-14}$	$\rm 240^{+38}_{-38}$	21-cm data
Evans & Wilkinson (2000)	41	$\rm 48^{+34}_{-23}$	$\rm 225^{+69}_{-63}$	17 Globular Clusters^b
Lee et al. (2008)	55	$\rm 55^{+4}_{-3}$	$\rm 208^{+7}_{-6}$	504 Globular Clusters
Galleti et al. (2006)	60	$\rm 44^{+26}_{-4}$	$\rm 178^{+48}_{-8}$	349 Globular Clusters^c
Côté et al. (2000)	100	$\rm 79^{+5}_{-5}$	$\rm 185^{+6}_{-6}$	12 Satellites^d
Ibata et al. (2004)	125	$\rm 75^{+25}_{-13}$	$\rm 161^{+25}_{-15}$	Stellar Stream
Fardal et al. (2006)	125	$\rm 74^{+12}_{-12}$	$\rm 160^{+13}_{-14}$	Stellar Stream
Courteau & van den Bergh (1999)	268	$\rm 137^{+18}_{-18}$	$\rm 149^{+9}_{-10}$	7 Satellites
Evans & Wilkinson (2000)	560	$\rm 125^{+180}_{-60}$	$\rm 98^{+55}_{-27}$	11 Satellites^e
Evans et al. (2000)	560	$\rm 99^{+146}_{-63}$	$\rm 87^{+51}_{-34}$	16 Satellites^f

Notes. ^(a) Best mass estimate using GCs; the lower mass extreme is the value inferred using 9 PNe, the upper mass extreme is from data on 11 Satellites. ^(b) Uncertanties derived from ``Error analysis'' section of original paper. ^(c) Uncertanties include uncertanties on the isotropy degree of the velocity distribution and the mass estimate using only the 14 most distant GCs. ^(d) Mass estimate assuming isotropic orbits; the mass range is larger, 79 ⁺¹⁷⁴_-46, if models with only radial or circular orbits are included. ^(e) Uncertanties derived from ``Error analysis'' section of original paper. ^(f) Mass estimate assuming Osipkov-Merrit distribution function; the given mass range includes also the mass estimated assuming a constant orbital anisotropy.

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