Chemical depletion in the Large Magellanic Cloud: RV Tauri stars and the photospheric feedback from their dusty discs

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This article has an erratum: [https://doi.org/10.1051/0004-6361/200912982e]

Table 1:

List of stellar parameters for our sample sources.
Name	Other name	$\alpha$ (J2000)	$\delta$ (J2000)	$T_{\rm eff}$	$\log g$	[Fe/H]	$E(B-V)_{\rm tot}$	$L_{\rm IR}/L_*$	L_*	P
		(h m s)	( $^\circ$ ' '')	(K)	(cgs)			(%)	$L_\odot$	(days)
MACHO 79.5501.13	J051418.1-691235	05 14 18.1	-69 12 34.9	5750	0.5	-2.0	$0.14 \pm 0.01$	$60 \pm 3$	$5000 \pm 500$	48.5
	HV 915
MACHO 81.8520.15	J053254.5-693513	05 32 54.5	-69 35 13.2	6250	1.0	-1.5	$0.27 \pm 0.03$	$0 \pm 1$	$4200 \pm 500$	42.1
MACHO 81.9728.14	J054000.5-694214	05 40 00.5	-69 42 14.6	5750	1.5	-1.0	$0.05 \pm 0.02$	$53 \pm 3$	$4200 \pm 500$	47.1
MACHO 82.8405.15	J053150.9-691146	05 31 51.0	-69 11 46.4	6000	0.5	-2.5	$0.05 \pm 0.01$	$84 \pm 3$	$4000 \pm 500$	46.5

Note: The name, equatorial coordinates $\alpha$ and $\delta$ (J2000), effective temperature $T_{\rm eff}$ , surface gravity $\log g$ and metallicity [Fe/H] of our sample stars. Also given are the total reddening $E(B-V)_{\rm tot}$ , the energy ratio $L_{\rm IR}/L_*$ , the calculated luminosity (computed by integrating the dereddened photosphere), assuming a distance of d = 50 kpc, and the period P as given in (Alcock et al. 1998).

Source LaTeX | All tables | In the text

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