A serendipitous survey for variability amongst the massive stellar population of Westerlund 1

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Table 4:

Summary of spectroscopic data for supergiants of spectral type B2 and earlier.
ID	Spectral	RA, Dec (J2000)	R	I	1.5 m	NTT	NTT	VLT	VLT	Notes
	type				(2001)	(2002)	(2003)	(2004)	(2008/9)
W2a	B2Ia	16 46 59.7 -45 50 51.1	14.23	11.73	$\bullet$	#6		R+z		A, cand. binary, H $\alpha$ var.
W6a	B0.5Iab	16 47 04.0 -45 50 21.0	15.80	13.16	$\bullet$		#7	R+z	$\bullet$	P, cand. binary, H $\alpha$ var.
W8b	B1.5Ia	16 47 06.0 -45 50 25.0	-	-				R+z	$\bullet$	pulsator
W10	B0.5+OB	16 47 03.3 -45 50 34.7	-	-	$\bullet$			R+z		A, binary
W11	B2 Ia	16 47 02.2 -45 50 47.0	14.52	11.91		#6+#7		R+z		A
W15	O9Ib	16 47 07.0 -45 50 28.0	16.38	13.75	$\bullet$			R	$\bullet$	A
W19	B1Ia	16 47 04.9 -45 50 59.1	15.21	12.37		#6+#7		R+z		A, H $\alpha$ var.
W21	B0.5Ia	16 47 02.0 -45 51 11.0	15.56	12.74				R+z	$\bullet$	A, pulsator
W23a	B2Ia+OB	16 47 03.0 -45 51 08.0	14.91	12.07		#6+#7		R+z	$\bullet$	A, binary, H $\alpha$ var., pulsator
W24	O9Iab	16 47 03.0 -45 51 11.0	15.96	13.24		#6+#7		z	$\bullet$	cand. pulsator
W28	B2Ia	16 47 04.7 -45 50 38.4	14.26	11.64		#6+#7		R+z		A, H $\alpha$ var.
W29	O9Ib	16 47 04.4 -45 50 39.8	16.02	13.38	$\bullet$			R+z
W30a	O+O	16 47 05.0 -45 50 39.0	15.80	13.20		#6+#7		R+z	$\bullet$	binary, H $\alpha$ var.
W35	O9Iab	16 47 04.2 -45 50 53.5	16.00	13.31	$\bullet$			R+z
W41	O9Iab	16 47 02.7 -45 50 56.9	15.39	12.78	$\bullet$			R+z
W43a	B1Ia	16 46 03.5 -45 50 57.3	15.22	12.26	$\bullet$	#6+#7		R+z	$\bullet$	A,binary, H $\alpha$ var.
W55	B0Ia	16 46 59.0 -45 51 29.0	15.25	12.67	$\bullet$				$\bullet$	A
W60	B0Iab	16 47 05.0 -45 51 51.0	15.96	13.28		#6+#7		R+z	$\bullet$	A
W61a	B0.5Ia	16 47 02.3 -45 51 41.6	14.62	12.01		#6+#7		R+z		A, H $\alpha$ var.
W61b	O9.5Iab	16 47 02.6 -45 51 41.6	16.00	13.31		#6+#7		z
W74	O9.5Iab	16 47 07.0 -45 50 10.0	-	-				R+z	$\bullet$	A
W78	B1Ia	16 47 02.0 -45 49 56.0	14.54	12.04				R+z	$\bullet$	A, pulsator
W238	B1Iab	16 47 05.0 -45 52 27.0	14.98	12.45	$\bullet$			R+z	$\bullet$	A

Notes. Note that W2a was also observed in 2005 March and W61a in 2005 May+July (VLT FLAMES+Medusa). Spectral classifications are from Negueruela et al. (2010). The final column indicates whether a given star is identified as a Periodic or Aperiodic photometric variable, (candidate) binary, H $\alpha$ variable and/or (candidate) photospheric pulsator (Sect. 3).

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