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Home All issues Volume 505 / No 2 (October II 2009) A&A, 505 2 (2009) 497-508 Full HTML
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Table 1:

Observation of Milky Way and M 31 (re-scaled to 785 kpc).
Observable Milky Way Reference M 31 Reference
Global properties        
Type SbcI-II 1 SbI-II 1
K-band MK=-24.02 2 MK=-24.70 3
Total luminosity        
        LB ( $10^{10}~L_{B\odot}$) 1.8 4 3.3 5
        LV ( $10^{10}~L_{V\odot}$) 2.1 6 $2.6 \sim 2.7$ 1
        LK ( $10^{10}~L_{K\odot}$) 5.5 7 $6 \sim 12^a$ 8
Total colour (B-V) 0.84 4 0.81 9
Mass        
        Total (1010$M_{\odot}$) 40-55 10, 11 107-140 12
        Visible (1010$M_{\odot}$) 5.0 3 5.9-8.7 5
Rotational curve ( km s-1)        
        Flat velocity 220 1 226 13
Bulge        
        Stellar mass (1010$M_{\odot}$) 1-2 14 3.2 15
        Effective radius (kpc) 2.5 1 2.6 1
Disk        
Scalelength (kpc)        
        U     7.7 9
        B $4.0\sim5.0$ 7 6.6 9
        V $2.5\sim3.5$ 6, 16 6.0 9
        R 2.3 3 5.9 9
        I     5.7 17
        K $2.3\sim2.8$ 18 4.8 19
        L     6.08 8
Total SFR ($M_{\odot}$ yr-1) $\sim$1-5 20,21 0.35-1.0 1, 8, 21, 22
Infall rate ($M_{\odot}$ ${\rm yr}^{-1}$) $0.5\sim5$ 21, 23    
Total mass of        
        disk(1010$M_{\odot}$) 3.5b 24 $\sim$7 15, 25, 26
        star(1010$M_{\odot}$) 3.0c 16 $\sim$6 5
        gas(1010$M_{\odot}$) $\sim$0.7 27, 28 $\sim$0.6 29
        HI(1010$M_{\odot}$) 0.4 1 $\sim$0.5 1, 29, 30
        H2(1010$M_{\odot}$) 0.11 31 $\sim$0.02-0.04 29, 30, 31
Gas fraction $\sim$0.15-0.2 20, This paper $\sim$ 0.09 This paper
Abundance gradient        
        [O/H] (dex kpc-1) $-0.04 \sim -0.07$ 32, 33, 34 $-0.018 \sim -0.027$ 35, 36
Colour gradient        
        B-V (mag kpc-1)     0.016 9
Note: a: Assuming M/LK = 1.15 ( $M/L_K)_{\odot}$ and M 31 mass is taken to be $(7-14)\times 10^{10}~M_\odot$; b: derived based on the disk scalelength $r_{\rm d} = 2.3$ kpc and total disk surface density at the solar neighborhood $\Sigma_{\rm tot} = 50$ $M_{\odot}$ ${\rm pc}^{-2}$; c: derived based on the stellar disk scalelength $r_{\rm d} = 2.3$ kpc and stellar surface density at the solar neighborhood $\Sigma_{*}$ = 37 $M_{\odot}$ ${\rm pc}^{-2}$.
Reference: (1) van den Bergh (1999); (2) Drimmel & Spergel (2001); (3) Hammer et al. (2007); (4) van der Kruit (1986); (5) Tamm et al. (2007); (6) Sackett (1997); (7) Kent et al. (1991); (8) Barmby et al. (2006); (9) Walterbos & Kennicutt (1988); (10) Xue et al. (2008); (11) Sakamoto et al. (2003); (12) Tempel et al. (2007); (13) Carignan et al. (2006); (14) Dehnen & Binney (1998); (15) Geehan et al. (2006); (16) Zheng et al. (2001); (17) Worthey et al. (2005); (18) Freudenreich (1998); (19) Hiromoto et al. (1983); (20) Boissier & Prantzos (1999); (21) Fraternali (2009); (22) Williams (2003)a; (23) Blitz et al. (1999); (24) Holmberg & Flynn (2004); (25) Klypin et al. (2002); (26) Widrow et al. (2003); (27) Dame (1993); (28) Kulkarni & Heiles (1987); (29) Nieten et al. (2006); (30) Dame et al. (1993); (31) Koper et al. (1991); (32) Deharveng et al. (2000); (33) Daflon & Cunha (2004); (34) Rudolph et al. (2006); (35) Smartt et al. (2001); (36) Trundle et al. (2002).

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