The Herschel Virgo Cluster Survey - III. A constraint on dust grain lifetime in early-type galaxies

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Table 1:

Dust mass loss rates and grain lifetimes, $t_{\rm g}$ .
NGC	$\dot{M}_{\rm d}/L_{\nu}(\rm K)$ $^{\dagger}$	$\dot{M}_{\rm d}/M$ $^{\ddagger}$	$\dot{M}_{\rm d}(\rm beam)$	$t_{\rm g}$ $^{\ast}$
	$\frac{M_{\odot}~{\rm yr}^{-1}}{\rm 10^{26}~W~Hz^{-1}}$	$\frac{M_{\odot}~{\rm yr}^{-1}}{10^{12}~M_{\odot}}$	$10^{-4}~M_{\odot}~{\rm yr}^{-1}$	$10^{6}\;\rm yr$
4371	3.80	0.00855	1.0	86
4442	3.48	0.00712	1.7	51
4473	3.57	0.00742	1.9	46
4474	3.71	0.00806	0.59	150
4551	2.61	0.00468	0.36	240
4564	4.28	0.00959	1.3	65

Notes. $^{(\ast)}$ For an assumed dust temperature of 30 K. $^{(\dagger)}$ The specific dust mass-loss rate per unit K-band luminosity. $^{(\ddagger)}$ The mass loss per $10^{12}~M_{\odot}$ of galaxy mass. A dust mass opacity coefficient suitable for amorphous silicate grains has been used.

Source LaTeX | All tables | In the text

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