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Table D.1

Comparison between stellar parameters and abundances derived in this work and those in the literature.

Star vsin i T eff log g log gC y log ϵ(C) log ϵ(N) log ϵ(O) [N/C] [N/O] Source
[km s-1] [K]
Cooler stars (DETAIL/SURFACE)
HD 93521 405 ± 15 30 000 ± 1000 3.60 ± 0.10 3.78 ± 0.10 0.166 ± 0.025 7.68 ± 0.12 8.10 ± 0.13 8.33 ± 0.21 0.42 ± 0.21 –0.23 ± 0.12 This work
400 ± 25 33 500 ± 1500 ... 3.80 ± 0.20 0.200 ± 0.050 ... ... ... ... ... Lennon et al. (1991)
435 ± 20 33 500 ± 1500 ... ... 0.180 ± 0.030 ... ... ... ... ... Howarth & Smith (2001)
390 ± 10 30 900 ± 700 3.67 ± 0.12 ... 0.178 ± 0.020 7.56 7.97 8.24 0.41 –0.27 Rauw et al. (2012)
HD 102415 357 ± 15 32 900 ± 1000 4.10 ± 0.10 4.19 ± 0.10 0.158 ± 0.025 <7.54 8.16 ± 0.13 8.22 ± 0.21 >0.62 –0.06 ± 0.12 This work
376 ± 10 31 000 ± 1500 3.50 ± 0.15 3.70 0.174 ± 0.068 ≤7.78 8.88 ≤8.48 ≥1.10 ≥0.40 Martins et al. (2015b)
HD 149757 (ζ Oph) 378 ± 15 31 500 ± 1000 3.87 ± 0.10 3.99 ± 0.10 0.135 ± 0.025 8.07 ± 0.12 7.85 ± 0.13 8.37 ± 0.21 –0.22 ± 0.21 –0.52 ± 0.12 This work
400 32 500 3.70 3.85 0.160 ... ... ... ... ... Puls et al. (1996)
399 ± 20 34 300 ± 1500 ... ... 0.200 ± 0.030 ... ... ... ... ... Howarth & Smith (2001)
400 32 500 ± 1500 3.50 ± 0.10 3.77 0.160 ± 0.030 ... ... ... ... ... Herrero et al. (2002)
400 32 000 ± 1000 3.65 ± 0.10 3.85 0.145 ± 0.022 ... ... ... ... ... Repolust et al. (2004)
340 ± 25 26 400 ± 700 3.80 ± 0.09 4.05 ± 0.07 ... ... ... ... ... ... Frémat et al. (2005)
400 32 100 ± 700 3.62 3.83 0.099 ... ... ... ... ... Mokiem et al. (2005)
... 33 500 ± 1700 ... 3.85 ± 0.10 0.145 ... ... ... ... ... Repolust et al. (2005) b
400 ± 20 34 000 ± 1000 3.70 ± 0.10 ... 0.110 ± 0.028 7.86 ± 0.30 8.34 ± 0.30 8.69 ± 0.30 0.48 –0.35 Villamariz & Herrero (2005)
400 32 000 ± 2000 3.60 ± 0.20 3.80 ... ... ... ... ... ... Marcolino et al. (2009)
400 ± 10 31 000 ± 1000 3.60 ± 0.15 ... ... ... ... ... ... ... Martins et al. (2015a)
HD 184915 (κ Aql) 252 ± 15 27 800 ± 1000 3.70 ± 0.10 3.77 ± 0.10 0.183 ± 0.025 <8.18 8.46 ± 0.13 8.62 ± 0.21 >0.28 –0.16 This work
270 26 800 3.56 ... 0.160 ± 0.011 ... ... ... ... ... Lyubimkov et al. (2004) a
229 ± 13 27 100 ± 500 3.49 ± 0.05 3.53 ± 0.06 ... ... ... ... ... ... Frémat et al. (2005)
249 ± 7 26 700 ± 750 3.59 ± 0.07 ... ... ... ... ... ... ... Huang & Gies (2008)
HD 198781 222 ± 15 29 100 ± 1000 3.90 ± 0.10 3.94 ± 0.10 0.230 ± 0.025 <8.09 8.62 ± 0.13 8.78 ± 0.21 >0.53 –0.16 ± 0.12 This work
224 24 400 3.50 ... 0.148 ± 0.011 ... ... ... ... ... Lyubimkov et al. (2004) a
Hotter stars (CMFGEN)
HD 13268 301 ± 15 32 500 ± 1500 3.42 ± 0.15 3.55 ± 0.15 0.206 ± 0.030 ≤7.50 8.61 ± 0.34 8.10 ± 0.21 ≥1.11 0.51 ± 0.40 This work
300 36 000 ± 2000 3.70 ± 0.30 ... ... ... ... ... ... ... Kendall et al. (1996)
320 35 000 3.30 3.50 0.200 ... ... ... ... ... Puls et al. (1996)
320 35 000 ± 1500 3.30 ± 0.10 3.42 ≥0.200 ... ... ... ... ... Herrero et al. (1992)
300 33 000 ± 1000 3.25 ± 0.10 3.48 0.200 ± 0.019 ... ... ... ... ... Repolust et al. (2004)
... 33 000 ± 1650 ... 3.48 ± 0.10 0.200 ... ... ... ... ... Repolust et al. (2005) b
310 ± 10 32 000 ± 1500 3.50 ± 0.15 3.63 0.167 ± 0.069 ≤7.70 8.70 8.49 ≥1.00 0.21 Martins et al. (2015b)
HD 14434 408 ± 15 40 000 ± 1500 3.89 ± 0.15 4.03 ± 0.15 0.103 ± 0.030 7.96 ± 0.27 8.81 ± 0.34 ≤8.10 0.85 ± 0.43 ≥0.71 This work
380 43 000 ± 2000 3.80 ± 0.20 ... ... ... ... ... ... ... Kendall et al. (1996)
HD 14442 285 ± 15 39 200 ± 1500 3.69 ± 0.15 3.78 ± 0.15 0.097 ± 0.030 7.10 ± 0.27 8.61 ± 0.34 ≤8.10 1.51 ± 0.43 ≥0.51 This work
260 43 000 ± 2000 3.60 ± 0.20 ... ... ... ... ... ... ... Kendall et al. (1996)
HD 15137 267 ± 15 29 500 ± 1500 3.18 ± 0.15 3.31 ± 0.15 0.112 ± 0.030 7.63 ± 0.27 8.27 ± 0.34 ≤8.30 0.64 ± 0.43 ≥–0.03 This work
234 ± 10 29 700 ± 700 3.50 ± 0.10 ... ... ... ... ... ... ... McSwain et al. (2007)
258 ± 20 29 700 ± 1700 3.50 ± 0.25 ... ... ... ... ... ... ... McSwain et al. (2010)
HD 46056 350 ± 15 34 500 ± 1500 3.90 ± 0.15 4.00 ± 0.15 0.088 ± 0.030 8.34 ± 0.27 7.78 ± 0.34 8.32 ± 0.21 –0.56 ± 0.43 –0.54 ± 0.40 This work
330 ± 10 34 500 ± 1000 3.75 ± 0.15 ... ... 8.28 ± 0.07 7.78 ± 0.14 8.45 ± 0.28 –0.50 –0.67 Martins et al. (2015a)
HD 46485 315 ± 15 37 000 ± 1500 4.00 ± 0.15 4.08 ± 0.15 0.076 ± 0.030 8.46 ± 0.27 7.95 ± 0.34 8.72 ± 0.21 –0.51 ± 0.43 –0.77 ± 0.40 This work
300 ± 10 36 000 ± 1000 3.75 ± 0.15 ... ... 8.43 7.95 ± 0.10 8.64 –0.48 –0.69 Martins et al. (2015a)
HD 66811 (ζ Pup) 225 ± 15 41 000 ± 1500 3.55 ± 0.15 3.62 ± 0.15 0.148 ± 0.030 ≤7.00 8.94 ± 0.34 8.20 ± 0.21 ≥1.94 0.74 This work
220 42 000 3.50 3.60 0.107 ... ... ... ... ... Puls et al. (1996)
220 39 000 ± 1500 3.55 ± 0.10 3.59 ± 0.09 0.167 ± 0.021 ... ... ... ... ... Repolust et al. (2004)
... 39 000 ± 1950 ... 3.59 ± 0.10 0.145 ... ... ... ... ... Repolust et al. (2005) b
210 40 000 ± 1000 ... 3.64 ± 0.10 0.140 6.60 ± 0.25 9.10 ± 0.17 8.13 ± 0.30 2.50 0.97 Bouret et al. (2012)
210 ± 10 40 000 ± 1000 3.64 ± 0.15 ... ... 6.60 ± 0.22 9.10 ± 0.17 8.13 ± 0.29 2.50 0.97 Martins et al. (2015a)
HD 69106 306 ± 15 29 500 ± 1500 3.45 ± 0.15 3.58 ± 0.15 0.091 ± 0.030 7.88 ± 0.27 7.74 ± 0.34 8.47 ± 0.21 –0.14 ± 0.43 –0.73 ± 0.40 This work
320 ± 10 29 000 ± 1000 3.40 ± 0.15 ... ... 7.60 ≤8.00 8.40 ≤0.40 ≤–0.40 Martins et al. (2015a)
HD 117490 361 ± 15 30 000 ± 1500 3.55 ± 0.15 3.70 ± 0.15 0.141 ± 0.030 ≤7.39 8.50 ± 0.34 8.15 ± 0.21 ≥1.11 0.35 ± 0.40 This work
375 ± 10 30 500 ± 1500 3.50 ± 0.15 3.66 0.138 ≤7.48 8.88 8.40 ≥1.40 0.48 Martins et al. (2015b)
HD 150574 233 ± 15 31 500 ± 1500 3.32 ± 0.15 3.41 ± 0.15 0.172 ± 0.030 7.48 ± 0.27 ≥9.08 ≥8.93 ≥1.60 ... This work
240 ± 10 31 000 ± 1500 3.40 ± 0.15 3.49 0.187 ± 0.040 ≤7.70 ≥9.00 8.78 ≥1.30 ≥0.22 Martins et al. (2015b)
HD 191423 420 ± 15 30 600 ± 1500 3.33 ± 0.15 3.57 ± 0.15 0.134 ± 0.030 ≤7.24 8.33 ± 0.34 ≤8.33 ≥1.09 ≥0.00 This work
450 34 000 ± 1500 3.40 ± 0.10 3.68 0.200 ... ... ... ... ... Herrero et al. (1992)
450 34 000 3.40 3.70 0.200 ... ... ... ... ... Puls et al. (1996)
435 34 300 ... ... 0.190 ± 0.030 ... ... ... ... ... Howarth & Smith (2001)
450 35 000 ± 1000 3.40 ± 0.10 ... 0.120 ± 0.030 7.57 ± 0.24 8.36 ± 0.17 8.23 ± 0.48 0.79 0.13 Villamariz et al. (2002) c
400 32 500 ± 1000 3.35 ± 0.10 3.60 0.167 ± 0.021 ... ... ... ... ... Repolust et al. (2004)
... 32 000 ± 1600 ... 3.56 ± 0.10 0.167 ... ... ... ... ... Repolust et al. (2005) b
410 30 600 ± 1000 3.50 ± 0.10 3.67 ... ... 8.73 ± 0.20 ... ... ... Mahy et al. (2015)
445 ± 10 31 500 ± 1500 3.50 ± 0.15 3.72 0.200 ± 0.051 ... ≥8.70 ... ... ... Martins et al. (2015b)
HD 192281 (V819 Cyg) 276 ± 15 39 000 ± 1500 3.64 ± 0.15 3.73 ± 0.15 0.103 ± 0.030 8.00 ± 0.27 8.76 ± 0.34 8.05 ± 0.21 0.76 ± 0.43 0.71 ± 0.40 This work
245 ± 10 39 000 ± 1000 3.65 ± 0.15 ... ... 8.11 8.92 8.15 ± 0.09 0.81 0.77 Martins et al. (2015a)
HD 203064 (68 Cyg) 298 ± 15 35 000 ± 1500 3.73 ± 0.15 3.82 ± 0.15 0.076 ± 0.030 7.92 ± 0.27 8.23 ± 0.34 8.46 ± 0.21 0.31 ± 0.43 –0.23 ± 0.40 This work
315 37 500 3.50 3.65 0.123 ... ... ... ... ... Puls et al. (1996)
315 37 500 ± 1000 3.50 ± 0.10 3.62 0.120 ± 0.030 ... ... ... ... ... Herrero et al. (1992)
300 34 500 ± 1000 3.50 ± 0.10 3.60 0.091 ± 0.017 ... ... ... ... ... Repolust et al. (2004)
... 34 500 ± 1700 ... 3.60 ± 0.10 0.167 ... ... ... ... ... Repolust et al. (2005) b
300 ± 10 34 000 ± 1000 3.60 ± 0.15 ... ... 8.20 ± 0.11 8.20 ± 0.19 ... 0.00 ... Martins et al. (2015a)
HD 210839 (λCep) 214 ± 15 36 000 ± 1500 3.50 ± 0.15 3.56 ± 0.15 0.113 ± 0.030 7.83 ± 0.27 8.74 ± 0.34 8.13 ± 0.21 0.91 ± 0.43 0.61 ± 0.40 This work
100 38 000 3.60 3.65 0.091 ... ... ... ... ... Puls et al. (1996)
250 37 000 ± 1500 3.55 ± 0.10 ... 0.250 ± 0.030 ... ... ... ... ... Herrero et al. (2000)
200 36 000 ± 1500 3.55 ± 0.10 3.58 ± 0.09 0.091 ± 0.017 ... ... ... ... ... Repolust et al. (2004)
210 36 000 ± 1000 ... 3.54 ± 0.10 0.107 8.22 ± 0.21 8.70 ± 0.15 8.48 ± 0.14 0.48 0.22 Bouret et al. (2012)
210 ± 10 36 000 ± 1000 3.50 ± 0.15 ... ... 7.78 ± 0.15 8.78 8.40 ± 0.35 1.00 0.38 Martins et al. (2015a)
HD 228841 305 ± 15 34 000 ± 1500 3.50 ± 0.15 3.62 ± 0.15 0.112 ± 0.030 7.48 ± 0.27 8.74 ± 0.34 8.67 ± 0.21 1.26 ± 0.43 0.07 ± 0.40 This work
317 34 500 ± 1000 3.50 ± 0.10 3.62 ... ... 8.73 ± 0.22 ... ... ... Mahy et al. (2015)

Notes.

(a)

The value of y corresponding to ξ derived from He i lines is chosen.

(b)

Only values from the infrared analysis are indicated.

(c)

Values not corrected for Galactic chemical gradient.

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