2008A&A...485..823B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.16CEST16:43:26

2008A&A...485..823B - Astronomy and Astrophysics, volume 485, 823-835 (2008/7-3)

Probing Atlas model atmospheres at high spectral resolution. Stellar synthesis and reference template validation.

BERTONE E., BUZZONI A., CHAVEZ M. and RODRIGUEZ-MERINO L.H.

Abstract (from CDS):

The fast improvement of spectroscopic observations makes mandatory a strong effort on the theoretical side to better reproduce the spectral energy distribution (SED) of stars at high spectral resolution. In this regard, relying on the Kurucz Atlas/Synthe original codes we computed the Bluered library, consisting of 832 synthetic SED of stars, that cover a large parameter space at very high spectral resolution (R=500000) along the 3500-7000Å wavelength range. Bluered synthetic spectra have been used to assess in finer detail the intrinsic reliability and the performance limits of the Atlas theoretical framework. The continuum-normalized spectra of the Sun, Arcturus, and Vega, plus a selected list of 45 bright stars with high-quality SEDs from the Prugniel & Soubiran E lodie catalog, form our sample designed to probe the global properties of synthetic spectra across the entire range of H-R parameters.Atlas models display a better fitting performance with increasing stellar temperature. High-resolution spectra of Vega, the Sun, and Arcturus have been reproduced at R=100000, respectively, within a 0.7%, 4.5%, and 8.8% relative scatter in residual flux. In all the three cases, the residual flux distribution shows a significant asymmetry (skewness parameter γ=-2.21, -0.98, -0.67, respectively), which neatly confirms an overall ``excess'' of theoretical line blanketing. For the Sun, this apparent discrepancy is alleviated, but not recovered, by a systematic decrease (-40%) of the line oscillator strengths, log (gf), especially referring to iron transitions. Definitely, a straight ``astrophysical'' determination of log(gf) for each individual atomic transition has to be devised to overcome the problem. By neglecting overblanketing effects in theoretical models when fitting high-resolution continuum-normalized spectra of real stars, we lead to a systematically warmer effective temperature (between +80 and +300K for the solar fit) and a slightly poorer metal content.

Abstract Copyright:

Journal keyword(s): Sun: atmosphere - stars: atmospheres - stars: individual: Arcturus - stars: individual: Vega - fundamental parameters - stars: line: profiles

Simbad objects: 48

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Number of rows : 48

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * 85 Peg SB* 00 02 10.3411392575 +27 04 54.476788744 6.47 6.42 5.75 5.16 4.73 G5VbFe-2 523 0
2 HD 400 PM* 00 08 40.9385088178 +36 37 37.648934145       5.9   F8IV 152 0
3 * 9 Cet BY* 00 22 51.7883318927 -12 12 33.972374893 7.29 7.05 6.39     G2.5V 451 0
4 HD 3567 PM* 00 38 31.9476246205 -08 18 33.395481958 9.54 9.70 9.23     F7/8wF3 190 0
5 * mu. Cas SB* 01 08 16.39470 +54 55 13.2264 5.93 5.86 5.17 4.55 4.13 G5Vb 545 1
6 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1092 1
7 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
8 HD 25329 PM* 04 03 14.9983565018 +35 16 23.806254921 9.75 9.37 8.50 7.75 7.23 K1VbFe-2 347 0
9 HD 26297 Pe* 04 09 03.4179730777 -15 53 27.057216777   8.55 7.47 7.09   G5/6IVw 140 0
10 * lam Aur PM* 05 19 08.4754630747 +40 05 56.589643877 5.46 5.33 4.71 4.18 3.86 G1.5IV-VFe-1 488 0
11 * chi01 Ori RS* 05 54 22.9829893 +20 16 34.222038 5.08 5.00 4.40 3.90 3.59 G0V 800 0
12 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1758 0
13 HD 64606 SB* 07 54 34.1796660767 -01 24 44.207014054 8.32 8.165 7.433 7.007 6.569 K0V 231 0
14 HD 76932 PM* 08 58 43.9328634171 -16 07 57.805389219 6.47 6.39 5.86     G2VFe-1.8CH-1 366 0
15 HD 87141 * 10 04 36.3228504340 +53 53 30.173493630   6.191 5.708     F5V 112 0
16 HD 94028 PM* 10 51 28.1254469804 +20 16 38.965521484 8.51 8.69 8.22 7.82 7.54 F8 329 0
17 * bet Vir PM* 11 50 41.7182390 +01 45 52.991019 4.26 4.15 3.60 3.13 2.85 F9V 856 0
18 * omi Vir PM* 12 05 12.5404884 +08 43 58.749788 5.75 5.11 4.12 3.38 2.89 G8IIICN0.5CH1Ba1 266 0
19 * bet CVn ** 12 33 44.5448195 +41 21 26.924857 4.91 4.86 4.25 3.73 3.42 G0V 541 0
20 * eps Vir PM* 13 02 10.5978496 +10 57 32.941443 4.45 3.71 2.79 2.16 1.71 G8III-IIIb 515 0
21 * bet Com PM* 13 11 52.3937856 +27 52 41.453553 4.92 4.84 4.25 3.77 3.47 F9.5V 847 0
22 HD 114762 SB* 13 12 19.7467346230 +17 31 01.611425890 7.78         F9VgF8mF4+M6?V 509 1
23 * e Vir PM* 13 16 46.5161591991 +09 25 26.967205938   5.81   4.8   G0V 502 1
24 HD 122956 PM* 14 05 13.0245301143 -14 51 25.455585497   8.18 7.25 6.88   G6IV/VwF6 142 0
25 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2133 0
26 * iot Vir PM* 14 16 00.8695049 -06 00 01.963348 4.64 4.60 4.08     F7III 334 0
27 * lam Ser PM* 15 46 26.6144291449 +07 21 11.041647444 5.13 5.03 4.42 3.92 3.60 G0-V 534 0
28 HD 150177 PM* 16 39 39.1297665715 -09 33 16.513863824   6.794 6.332     F6V 136 0
29 HD 157089 PM* 17 21 07.0567914512 +01 26 34.981760941 7.60 7.59 7.01 6.46 6.14 F8VgF8mF6 233 0
30 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2505 0
31 * 110 Her PM* 18 45 39.7257041 +20 32 46.717099 4.66 4.65 4.19 3.80 3.54 F5.5IV-V 378 0
32 HD 175305 Pe* 18 47 06.4424234462 +74 43 31.448124921 8.07 7.93 7.18 6.52 6.03 G5III 192 0
33 HD 174912 PM* 18 51 25.1794717878 +38 37 35.652070012       6.8   F8 106 0
34 * 16 Cyg A ** 19 41 48.9539315338 +50 31 30.218780803 6.79 6.59 5.95 5.50 5.17 G1.5Vb 675 1
35 * 16 Cyg B PM* 19 41 51.9731830550 +50 31 03.086127222 7.07 6.86 6.20 5.76 5.42 G3V 793 1
36 * omi Aql PM* 19 51 01.6437560393 +10 24 56.595177367   5.66   4.8   F8V 423 0
37 HD 189558 PM* 20 01 00.2452564415 -12 15 20.355884232   8.27 7.72     F8/G2V 170 1
38 HD 194598 PM* 20 26 11.9185966774 +09 27 00.429262518 8.62 8.82 8.34 7.90 7.56 F8 284 0
39 * eps Cyg ** 20 46 12.6823609 +33 58 12.924926 4.370 3.520 2.480 1.73 1.19 K0III 480 0
40 HD 201891 PM* 21 11 59.0322335571 +17 43 39.888647667 7.74 7.88 7.37 6.91 6.59 G5V_Fe-2.5 367 0
41 HD 204543 * 21 29 28.2127594590 -03 30 55.356028557   9.17 8.30 7.99   F6/8(V) 124 0
42 * 15 Peg PM* 21 52 29.9167067804 +28 47 36.751682373 5.82 5.95 5.53     F2V 225 0
43 HD 208906 PM* 21 58 40.8319509283 +29 48 45.457435407 7.35 7.47 6.96 6.53 6.22 G0VmF2 160 0
44 * ksi Peg PM* 22 46 41.5811758 +12 10 22.385447 4.66 4.69 4.20 3.73 3.42 F6V 354 1
45 HD 216143 Pe* 22 50 31.0884300128 -06 54 49.557528724   8.78 7.81 7.44   G2/3(IV)(we) 128 0
46 * sig Peg PM* 22 52 24.0744875405 +09 50 08.386917893   5.64   4.9   F6V 256 0
47 * 51 Peg Ro* 22 57 27.9804167474 +20 46 07.782240714 6.39 6.16 5.46 4.97 4.61 G2IV 1071 1
48 * iot Psc PM* 23 39 57.0413764 +05 37 34.647529 4.640 4.620 4.120 3.68 3.37 F7V 579 0

    Equat.    Gal    SGal    Ecl

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2020.07.16-16:43:26

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