The new Wolf-Rayet binary system WR62a | Astronomy & Astrophysics (A&A)

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Table 2

Observed heliocentric radial velocities of WR62a.

HJD	Phase	N iv	N v	N v	C iv	He ii	He ii	He ii	He ii	Mean Abs [n]^a
2 450 000+		4057.66 Å	4603.73 Å	4944.56 Å	5811.98 Å	4685.68 Å	5411.52 Å	4199.87 Å	4541.59 Å
		[km s^-1]	[km s^-1]	[km s^-1]	[km s^-1]	[km s^-1]	[km s^-1]	[km s^-1]	[km s^-1]	[km s^-1]

2386.72	0.98	–213	49			113	55			−43 ± 27 (5)
4188.89	0.05	–65		–41	59	254	235			−113 ± 22 (8)
4189.82	0.15	53	220	106	155	278	306	308	387	−204 ± 32 (10)
4191.84	0.37	–8	213	96	185	134	223	297	397	−175 ± 29 (10)
4192.85	0.48	–161	9	–8	–16	–61	86	162	261	−83 ± 22 (9)
4193.65	0.57	–275	–119	–199	–155	–162	–62	42	–30	19 ± 59 (9)
4193.87	0.59	–228	–143	–280	–135	–250	–192	–72		18 ± 52 (9)
4575.84	0.36	87	187	102	182	133	259	374	359	−157 ± 36 (10)
4576.82	0.47	–122	48	–32	–19	–53	79	90		−85 ± 28 (6)
4577.73	0.57	–285	–116	–193	–178	–199	–119		–14	19 ± 38 (9)
4578.80	0.69	–403	–254	–346	–257	–282	–284
4579.59	0.77	–379	–255	–276	–257	–191	–234	–246	–215	31 ± 37 (9)
4579.85	0.80		–257		–290	–173	–250	–262	–230	36 ± 35 (9)
4914.83	0.43	–8	173	101		49	130		307	−75 ± 26 (5)
4915.82	0.54	–134	–14	–161		–89	–25	114	139	25 ± 18 (3)
4916.78	0.65	–255				–251	–208	–181	–86	98 ± 14 (4)
4917.74	0.75	–406	–216	–343		–183	–282		–212	91 ± 23 (5)
4941.57	0.36	91	254	150		218	278	375	362	−151 ± 24 (7)
4942.71	0.48	–163	19	–97		–12	–21	166		−77 ± 28 (8)
5031.64	0.21	81	273	155		301	302	326	429	−204 ± 21 (8)
5036.59	0.75	–372		–288	–212	–168	–227	–249	–205	102 ± 24 (7)
5038.58	0.97	–204	–41	–167	–185	131	33	–32	109	−97 ± 36 (3)
5039.61	0.08	–31	123	–1		263	218	228	244	−168 ± 33 (7)
5057.52	0.04		170	–118		352	314			−137 ± 40 (7)
5059.52	0.25		287	175		356				−183 ± 28 (6)
5060.49	0.36		191	60		187	237			−151 ± 17 (7)
5296.79	0.20	153				267			373	−195 ± 33 (6)
5299.66	0.51					–113				31 ± 1 (4)

FWHM [Å]		18.5	10.4	19.7	33.9	24.7	22.4	17.3	18.7
EW [Å]		–4.6	–1.6	–1.5	–2.2	–26.1	–3.8	–1.2	–1.6

Notes.The mean FWHM and mean EW of each emission line measured from the separated spectra are indicated in the last two rows, respectively.

^(a)

The errors are the standard deviation of the mean, and the (n) values indicate the number of absorption lines measured.

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