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Table 2

Observed heliocentric radial velocities of WR 68a.

HJD Phase N iv N iii He ii He ii C iv Mean abs.
2 450 000+ 4057.76 Å 4640.64 Å 4685.68 Å 5411.52 Å 5811.98 Å Hδ-Hγ-Hβ
[km s-1] [km s-1] [km s-1] [km s-1] [km s-1] [km s-1]

4189.83 0.99 238 ± 2 173 ± 2 58 ± 1 46 ± 5 471 ± 3 113 ± 3
4189.85 0.99 239 ± 1 203 ± 2 41 ± 2 30 ± 1 491 ± 4 158 ± 3
4191.86 0.38 54 ± 2 85 ± 2 190 ± 1 274 ± 2 68 ± 5 290 ± 6
4192.89 0.58 450 ± 1 268 ± 4 162 ± 7 441 ± 3 110 ± 6
4193.67 0.72 425 ± 1 550 ± 2 309 ± 3 301 ± 3 702 ± 3 10 ± 9
4193.90 0.77 483 ± 2 542 ± 1 297 ± 1 327 ± 4 742 ± 3 15 ± 9
4575.90 0.94 297 ± 1 281 ± 2 64 ± 1 113 ± 3 571 ± 3 36 ± 3
4576.86 0.12 45 ± 2 17 ± 1 256 ± 1 243 ± 1 213 ± 3 209 ± 13
4577.75 0.29 150 ± 2 38 ± 2 272 ± 1 340 ± 1 32 ± 5 283 ± 17
4578.66 0.47 299 ± 3 6 ± 1 103 ± 1 230 ± 2 268 ± 7
4578.89 0.51 188 ± 4 365 ± 3 157 ± 2 70 ± 6 249 ± 2 161 ± 5
4579.61 0.65 365 ± 4 545 ± 2 303 ± 1 239 ± 1 587 ± 2 32 ± 10
4579.88 0.70 478 ± 5 592 ± 1 342 ± 1 306 ± 2 693 ± 3 2 ± 14
4633.69 0.01 213 ± 3 160 ± 3 66 ± 3 121 ± 3 411 ± 7 113 ± 21
4914.87 0.87 415 ± 3 177 ± 3 270 ± 2
4915.85 0.06 18 ± 1 202 ± 1 231 ± 3
4915.88 0.06 28 ± 1 214 ± 1 194 ± 4
4916.81 0.24 8 ± 3 314 ± 1 308 ± 1
4916.84 0.24 33 ± 4 329 ± 2 326 ± 1
4917.80 0.43 66 ± 2 114 ± 3 120 ± 1 157 ± 1 304 ± 13
4917.83 0.43 49 ± 2 123 ± 1 111 ± 2 148 ± 1 283 ± 12
5035.65 0.00 256 ± 2 128 ± 2 93 ± 1 66 ± 2 103 ± 5
5038.62 0.57 228 ± 5 392 ± 1 230 ± 4 225 ± 5 399 ± 2 76 ± 9
5039.64 0.77 444 ± 1 531 ± 1 283 ± 1 338 ± 3 28 ± 20
5059.56 0.58 440 ± 3 194 ± 3 131 ± 3
5060.53 0.77 304 ± 2 296 ± 2
5060.56 0.77 317 ± 1 234 ± 1
5296.85 0.03 90 ± 2 135 ± 2
5297.81 0.22 317 ± 1 367 ± 1
5410.52 0.81 557 ± 2 239 ± 1
5411.55 0.00 158 ± 2 128 ± 4
5413.50 0.38 197 ± 1 258 ± 1
5416.51 0.95 156 ± 2 30 ± 2
5657.88 0.19 73 ± 2 309 ± 3 268 ± 4
5662.74 0.12 284 ± 2 216 ± 1
6425.80 0.28 2 ± 3 322 ± 1 353 ± 3

FWHMa [Å] 14.6 30.0 22.5 21.6 34.5
EWa [Å] 4.6 8.5 31.4 5.3 5.6

Notes. Radial velocities errors listed in table are provided by the fxcor task of IRAF. The errors are calculated from the asymmetric noise of the cross-correlation function and of the fitted height of the peak.

(a)

The mean FWHM and EW of each emission line were measured in the disentangled spectra.

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