The mass of the Andromeda galaxy

被引:103
作者
Evans, NW
Wilkinson, MI
机构
[1] Univ Oxford, Dept Phys, Oxford OX1 3NP, England
[2] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
关键词
celestial mechanics; stellar dynamics; galaxies : individual : M31 galaxies : kinematics and dynamics; Local Group;
D O I
10.1046/j.1365-8711.2000.03645.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
This paper argues that the Milky Way galaxy is probably the largest member of the Local Group. The evidence comes from estimates of the total mass of the Andromeda galaxy (M31) derived from the three-dimensional positions and radial velocities of its satellite galaxies, as well as the projected positions and radial velocities of its distant globular clusters and planetary nebulae. The available data set comprises 10 satellite galaxies, 17 distant globular clusters and nine halo planetary nebulae with radial velocities. We find that the halo of Andromeda has a mass of similar to 12.3(-6)(+18) x 10(11) M., together with a scalelength of similar to 90 kpc and a predominantly isotropic velocity distribution. For comparison, our earlier estimate for the Milky Way halo is similar to 19(-17)(+36) x 10(11) M.. Although the error bars are admittedly large, this suggests that the total mass of M31 is probably less than that of the Milky Way. We verify the robustness of our results to changes in the modelling assumptions and to errors caused by the small size and incompleteness of the data set. Our surprising claim can be checked in several ways in the near future. The numbers of satellite galaxies, planetary nebulae and globular clusters with radial velocities can be increased by ground-based spectroscopy, while the proper motions of the companion galaxies and the unresolved cores of the globular clusters can be measured using the astrometric satellites Space Interferometry Mission (SIM) and Global Astrometric Interferometer for Astrophysics (GAIA). Using 100 globular clusters at projected radii 20 less than or similar to R less than or similar to 50 kpc with both radial velocities and proper motions, it will be possible to estimate the mass within 50 kpc to an accuracy of similar to 20 per cent. Measuring the proper motions of the companion galaxies with SIM and GAIA will reduce the uncertainty in the total mass caused by the small size of the data set to similar to 22 per cent.
引用
收藏
页码:929 / 942
页数:14
相关论文
共 70 条
[1]  
Aceves H, 1999, ASTRON ASTROPHYS, V345, P439
[2]  
ARMANDROFF TE, 1999, P IAU S, V192, P203
[3]  
Arnaboldi M, 2000, ASTR SOC P, V197, P103
[4]  
Ashman K. M., 1998, GLOBULAR CLUSTER SYS
[5]   METHODS FOR DETERMINING THE MASSES OF SPHERICAL SYSTEMS .1. TEST PARTICLES AROUND A POINT MASS [J].
BAHCALL, JN ;
TREMAINE, S .
ASTROPHYSICAL JOURNAL, 1981, 244 (03) :805-819
[6]   M31 globular clusters: Colors and metallicities [J].
Barmby, P ;
Huchra, JP ;
Brodie, JP ;
Forbes, DA ;
Schroder, LL .
ASTRONOMICAL JOURNAL, 2000, 119 (02) :727-747
[7]  
Binney J., 2008, Galactic Dynamics
[8]   THE DISTRIBUTION AND KINEMATICS OF NEUTRAL GAS IN M31 [J].
BRAUN, R .
ASTROPHYSICAL JOURNAL, 1991, 372 (01) :54-66
[9]  
Bridges T, 1999, ASTR SOC P, V182, P415
[10]   Internal kinematics of the Andromeda II dwarf spheroidal galaxy [J].
Côte, P ;
Mateo, M ;
Olszewski, EW ;
Cook, KH .
ASTROPHYSICAL JOURNAL, 1999, 526 (01) :147-151