The molecular gas content of blue dwarf galaxies - A collapsing detached molecular system in He 2–10?

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Volume 496 / No 3 (March IV 2009)

A&A, 496 3 (2009) 677-682

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Table 1:

Main properties of the sample galaxies and CO line detections (K km s^-1) derived from the literature.
Name	D (Mpc)	12 + Log(O/H)	CO(1, 0)	CO(2, 1)	CO(3, 2)
He 2-10	9 $^{\rm K9}$	8.93 $^{\rm K9}$	10.0 (40 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Ba}$ , 4.85(55 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm K5}$	17.3 (21 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Ba}$ , 6.82 (27 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm K5}$	36.8 (14 $\hbox{$.\!\!^{\prime\prime}$ }$ 5) $^{\rm Ba}$ , 16.6 (22 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Me}$
IC 745	16.3¹, 15.4 $^{\rm Tu}$	8.9 $^{\rm Sa}$	1.12 (22 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Sa}$	1.02 (12 $\hbox{$.\!\!^{\prime\prime}$ }$ 5) $^{\rm Sa}$	-
NGC 4123	22.4 $^{\rm We}$ , 25.3 $^{\rm Tu}$	9.05 $^{\rm Ra}$	4.5 (35 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Go}$ , 17.8 (22 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Kr}$	32.7 (12 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Kr}$
NGC 4309	18.0 $^{\rm Fo}$		3.01 (55 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Le}$		-
NGC 4385	33.5 $^{\rm Tu}$	9.1 $^{\rm Ma}$	6.2 (35 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Go}$ , 6.8 (15 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm De}$ , 2.3 (44 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Tc}$		5.0 (14 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm De}$
NGC 4630	17.9 $^{\rm Tu}$ , 20 $^{\rm Al}$		4.45 (55 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Le}$ , 3.86 (24 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Al}$	4.84 (11 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Al}$
NGC 4701	20.5 $^{\rm Tu}$		4.85 (55 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Le}$ , 2.90 (21 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Bo}$	3.02 (11 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Bo}$
NGC 4713	17.9 $^{\rm Tu}$	8.84 $^{\rm Sk}$	3.61(55 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Le}$
NGC 5253	3.3 $^{\rm Fe}$	8.14 $^{\rm K9}$	0.72 (55 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Ty}$ , 1.3 (44 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Wi}$		3.39 (22 $\hbox {$^{\prime \prime }$ }$ ) $^{\rm Me}$

(1) Distance assuming H₀ = 70 km s^-1 Mpc^-1; (Al) Albrecht et al. (2004) - IRAM 30 m; (Ba) Baas et al. (1994) - SEST 15 m; (Bo) Boker et al. (2003) - IRAM 30 m; (De) Devereux et al. (1994) - NRO 45 m; (Fe) Ferrarese et al. (2000); (Fo) Fouque et al. (2001); (Go) Gondhalekar et al. (1998) - OSO 20 m; (K5) Kobulnicky et al. (1995) - NRAO 12 m; (K9) Kobulnicky et al. (1999); (Kr) Krugel et al. (1990) - IRAM 30 m; (Le) Leroy et al. (2005) - NRAO 12 m; (Ma) Mayya et al. (2004); (Me) Meier et al. (2001) - CSO 10.4 m; (Ra) Raimann et al. (2000); (Sa) Sage et al. (1992) - IRAM 30 m; (Sk) Skillman et al. (1996); (Tu) Tully (1988); (Tc) Tacconi et al. (1991) - SEST 15 m; (Ty) Taylor et al. (1998) - NRAO 12 m; (We) Weiner et al. (2001); (Wi) Wiklind & Henkel (1989) - SEST 15 m.

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