Unidentified emission features in the R Coronae Borealis star V854 Centauri

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Table 1

Log of VLT/X-shooter observations.

Target	d	Phase	Obs. date	m_v	m_v	S∕N
	(kpc)			(max)	(obs)
V854 Cen	2.4	Max	2012-05-04	7.1¹	7.2	90
		Min	2012-06-14		13.3	70
		Min	2012-06-18		12.8	130
		Rise	2012-07-05		9.9	170
		Rise	2012-07-05		9.9	150
		Rise	2012-07-05		9.9	170
		Max	2013-07-15		7.2	85
ASAS-RCB-12	17.5	Min	2013-07-15	<11.7²	14.0	30
R CrB	1.3	Min	2013-07-15	5.7³	13.7	35
RT Nor	9.9	Min	2013-07-15	10.6³	15.2	20
RZ Nor	10.5	Min	2013-07-15	10.6³	16.2	15
S Aps	7.1	Min	2013-07-15	9.6³	14.3	10
V CrA	6.6	Min	2013-07-15	9.4³	17.5	10

Notes. During the rise of V854 Cen, three different position angles were used. The magnitudes were measured from the acquisition images, except for V854 Cen during maximum light, for which they are saturated. For these, values from the AAVSO were used. The distance of V854 Cen is based on the (V − I) − M_V relation for RCBs in the LMC by Tisserand et al. (2009). For the others, a typical value of M_v = −5 (Clayton 2012) is assumed. The signal-to-noise ratio was measured in the continuum around 6200 Å.

References. (1) Samus’ et al. (2003); (2) Tisserand et al. (2013); (3) Ducati (2002).

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