2006A&A...449..109F


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.15CEST04:43:36

2006A&A...449..109F - Astronomy and Astrophysics, volume 449, 109-125 (2006/4-1)

Prospects for population synthesis in the H band: NeMo grids of stellar atmospheres compared to observations.

FREMAUX J., KUPKA F., BOISSON C., JOLY M. and TSYMBAL V.

Abstract (from CDS):

For applications in population synthesis, libraries of theoretical stellar spectra are often considered an alternative to template libraries of observed spectra, because they allow a complete sampling of stellar parameters. Most of the attention in published theoretical spectral libraries has been devoted to the visual wavelength range. The goal of the present work is to explore the near-infrared range where few observed fully calibrated spectra and no theoretical libraries are available. We make a detailed comparison of theoretical spectra in the range 1.57-1.67µm for spectral types from A to early M and for giant and dwarf stars, with observed stellar spectra at resolutions around 3000, which would be sufficient to disentangle the different groups of late-type stars. We selected the NeMo grids of stellar atmospheres to perform this comparison. We first demonstrate that observed spectral flux distributions can be matched very well with theoretical ones for almost the entire parameter range covered by the NeMo grids at moderate resolution in the visual range. In the infrared range, although the overall shape of the observed flux distributions still matches reasonably well, the individual spectral features are reproduced by the theoretical spectra only for stars earlier than mid F type. For later spectral types the differences increase, and theoretical spectra of K type stars have systematically weaker line features than those found in observations. These discrepancies are traced back to stem primarily from incomplete data on neutral atomic lines, although some of them are also related to molecules. Libraries of theoretical spectra for A to early M type stars can be successfully used in the visual regions for population synthesis, but their application in the infrared is restricted to early and intermediate type stars. Improving atomic data in the near infrared is a key element in making the construction of reliable libraries of stellar spectra feasible in the infrared.

Abstract Copyright:

Journal keyword(s): stars: atmospheres - infrared: stars - galaxies: stellar content

Simbad objects: 54

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Number of rows : 54

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 * bet Cas dS* 00 09 10.68518 +59 08 59.2120 2.73 2.61 2.27 1.97 1.77 F2III 498 0
2 HD 2506 * 00 29 14.2626441789 +59 28 10.124664234   8.98 8.03     G4III 25 0
3 * del And SB* 00 39 19.6751809 +30 51 39.678320 6.04 4.56 3.28 2.36 1.70 K3III-IIIbCN0.5 313 0
4 HD 10307 SB* 01 41 47.1431421954 +42 36 48.443521767 5.69 5.58 4.96 4.43 4.10 G1V 468 0
5 HD 15866 PM* 02 33 54.2272497529 +31 34 50.085485116   8.63 8.01     G0III 34 0
6 * 59 Ari PM* 03 19 55.7955610419 +27 04 16.066156518   6.774 5.918     G7IV 59 0
7 HD 21110 *iN 03 25 23.9193709303 +31 43 51.948641201 10.49 8.80 7.29     K4III-IV 38 1
8 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1704 1
9 HD 23524 ** 03 48 23.00324 +52 02 16.2701   9.66 9.03 8.96   G5V 73 0
10 HD 25894 PM* 04 07 09.8560058741 +27 30 33.414830417   9.26 8.54     G2III 25 0
11 HD 26015 ** 04 07 41.98340 +15 09 46.0260           F3V 143 0
12 * h Tau dS* 04 19 57.7045549280 +14 02 06.739482030   5.856 5.568 5.407 5.250 F0IV 206 0
13 * 59 Eri * 04 48 32.5337354995 -16 19 46.148858822   6.278 5.755     F8V 66 0
14 HD 283916 * 04 52 53.0107750269 +27 18 51.196178615   10.42 8.99     K5 13 0
15 HD 33278 * 05 08 55.1129173134 -02 31 16.992129261   9.70 8.61     K0III 14 0
16 HD 33506 * 05 10 44.3594959118 +00 04 09.281262668   10.01 8.81     F0V 8 0
17 HD 36395 PM* 05 31 27.3958475290 -03 40 38.021551815 10.626 9.443 7.968 6.996 5.913 M1.5Ve 428 0
18 HD 38858 PM* 05 48 34.9401453172 -04 05 40.719529406 6.71 6.61 5.97     G2V 253 1
19 HD 39715 PM* 05 54 28.5764090262 +02 08 32.042623455   9.86   8.1   K3V 75 0
20 V* V350 CMa gD* 06 42 46.0439873451 -22 26 54.933639357   6.56 6.23     F2V 56 0
21 * ups02 Cnc PM* 08 33 00.1040838196 +24 05 05.260865502   7.373 6.340     G9III 139 0
22 HD 79210 Fl* 09 14 22.7754519714 +52 41 11.792840757   9.388   6.8   K7V 252 0
23 * zet Leo V* 10 16 41.4159679 +23 25 02.322080 3.89 3.72 3.41 3.09 2.91 F0IIIa 216 0
24 HD 88815 PM* 10 18 01.0889610624 +73 04 24.678690312   6.840 6.525     F2V 26 0
25 HD 93800 PM* 10 49 31.6947561192 -06 46 10.498094370   10.00 9.10     K1III 23 0
26 * ksi UMa B SB* 11 18 10.8360115405 +31 31 44.821690914   5.41 4.77 4.4   G2V 328 1
27 * ksi UMa A SB* 11 18 10.901164 +31 31 44.97910   4.79 4.25     F8.5:V 302 1
28 * 61 UMa PM* 11 41 03.0159358291 +34 12 05.882438337 6.31 6.08 5.34 4.73 4.38 G8V 567 0
29 HD 106116 PM* 12 12 28.8425973802 -03 05 04.108792898   8.15 7.50     G5V 151 0
30 * 5 CVn * 12 24 01.4946052553 +51 33 44.115130783   5.643 4.761     G7IIIBa0.3 137 0
31 HD 112164 PM* 12 54 58.5416895952 -44 09 06.912346816 6.78 6.53 5.89     F9Vp 111 0
32 * 37 Com RS* 13 00 16.4672517487 +30 47 06.064425348   6.02 4.88     G9IIICH-2CN-1 150 0
33 V* EL CVn Al* 13 23 57.0189467152 +43 35 55.439213684   9.58 9.42     A1V 34 1
34 * eta Boo SB* 13 54 41.07892 +18 23 51.7946 3.440 3.250 2.680 2.24 1.95 G0IV 657 1
35 HD 124320 * 14 11 57.3191502956 +38 49 52.375555839   8.98 8.84     A2V 21 0
36 * 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 2136 0
37 HD 131977 BY* 14 57 28.0008928545 -21 24 55.726897561 7.89 6.83 5.72 4.74 4.19 K4V 449 0
38 * 12 Oph BY* 16 36 21.4492997704 -02 19 28.512485729 7.00 6.55 5.77 5.13 4.74 K1V 450 0
39 HD 149890 PM* 16 36 26.0008402790 +30 56 30.056695569   7.66   6.8   F8V 52 0
40 HD 151541 PM* 16 42 38.5768818637 +68 06 07.792148115   8.32   7.1   K1 111 0
41 BD+27 2725 PM* 16 57 36.4165057403 +26 54 20.332587149   10.44   9.1   K0 17 0
42 HD 154733 PM* 17 06 18.0470502343 +22 05 02.953283634   6.871 5.565     K3III 98 0
43 BD+37 2879 PM* 17 23 57.3321361749 +37 16 48.711591818   9.69   8.3   K0 18 0
44 * sig Ara * 17 35 39.5895684 -46 30 20.461748 4.47 4.56 4.59 4.60 4.65 A0V 60 0
45 * mu.01 Her ** 17 46 27.5266778 +27 43 14.437984 4.56 4.17 3.42 2.89 2.51 G5IV 650 0
46 * ksi Her LP* 17 57 45.8857114 +29 14 52.367509 5.34 4.64 3.70 3.01 2.55 G8.5III 224 0
47 * lam Lyr V* 19 00 00.8253423216 +32 08 43.841834157   6.401 4.930     K2.5III:Ba0.5 108 0
48 * tau Dra PM* 19 15 32.9788792685 +73 21 19.872611829 7.15 5.70 4.45 3.55 2.97 K2+IIIbCN1 114 0
49 * sig Dra PM* 19 32 21.5902990 +69 39 40.234737 5.860 5.460 4.680 4.04 3.63 K0V 582 0
50 * omi Aql PM* 19 51 01.6437560393 +10 24 56.595177367   5.66   4.8   F8V 423 0
51 HD 190785 V* 20 05 24.2522303038 +34 59 04.327865502   8.25 8.16     A4V 14 0
52 * eps Cyg ** 20 46 12.6823609 +33 58 12.924926 4.370 3.520 2.480 1.73 1.19 K0III 480 0
53 HD 201902 * 21 13 19.7658588787 -28 27 37.563999370   9.83 9.51     F0V 3 0
54 HD 221741 * 23 34 19.4310901999 +61 26 14.525117741   9.05 8.93     A3V 13 0

    Equat.    Gal    SGal    Ecl

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2020.08.15-04:43:36

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