2005ApJ...626..465R


Query : 2005ApJ...626..465R

2005ApJ...626..465R - Astrophys. J., 626, 465-485 (2005/June-2)

The effective temperature scale of FGK stars. II. Teff:Color:[Fe/H] calibrations.

RAMIREZ I. and MELENDEZ J.

Abstract (from CDS):

We present up-to-date metallicity-dependent temperature versus color calibrations for main-sequence and giant stars based on temperatures derived with the infrared flux method (IRFM). Seventeen colors in the photometric systems UBV, uvby, Vilnius, Geneva, RI(Cousins), DDO, Hipparcos-Tycho, and Two Micron All Sky Survey (2MASS) have been calibrated. The spectral types covered by the calibrations range from F0 to K5 (7000K≳Teff≳4000K) with some relations extending below 4000 K or up to 8000 K. Most of the calibrations are valid in the metallicity range -3.5≳[Fe/H]≳0.4, although some of them extend to as low as [Fe/H]~-4.0. All fits to the data have been performed with more than 100 stars; standard deviations range from 30 to 120 K. Fits were carefully performed and corrected to eliminate the small systematic errors introduced by the calibration formulae. Tables of colors as a function of Teffand [Fe/H] are provided. This work is largely based on the study by A. Alonso and collaborators; thus, our relations do not significantly differ from theirs except for the very metal-poor hot stars. From the calibrations, the temperatures of 44 dwarf and giant stars with direct temperatures available are obtained. The comparison with direct temperatures confirms our finding in Paper I that the zero point of the IRFM temperature scale is in agreement, to the 10 K level, with the absolute temperature scale (that based on stellar angular diameters) within the ranges of atmospheric parameters covered by those 44 stars. The colors of the Sun are derived from the present IRFM Teffscale and they compare well with those of five solar analogs. It is shown that if the IRFM Teffscale accurately reproduces the temperatures of very metal-poor stars, systematic errors of the order of 200 K, introduced by the assumption of (V-K) being completely metallicity independent when studying very metal-poor dwarf stars, are no longer acceptable. Comparisons with other Teffscales, both empirical and theoretical, are also shown to be in reasonable agreement with our results, although it seems that both Kurucz and MARCS synthetic colors fail to predict the detailed metallicity dependence, given that for [Fe/H]=-2.0, differences as high as approximately ±200 K are found.

Abstract Copyright:

Journal keyword(s): Stars: Abundances - Stars: Atmospheres - Stars: Fundamental Parameters

Simbad objects: 58

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Number of rows : 58
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3766 0
2 * eps And PM* 00 38 33.3474310042 +29 18 42.311618884 5.72 5.25 4.38 3.70 3.19 G7IIIFe-3CH1 267 0
3 * del And SB* 00 39 19.6751809 +30 51 39.678320 6.04 4.56 3.28 2.36 1.70 K3III-IIIbCN0.5 321 0
4 * alf Cas PM* 00 40 30.4410679 +56 32 14.392170 4.52 3.40 2.23 1.45 0.85 K0-IIIa 328 0
5 NGC 288 GlC 00 52 45.24 -26 34 57.4   10 8.13     ~ 999 0
6 NGC 362 GlC 01 03 14.26 -70 50 55.6     6.58     ~ 1023 0
7 * bet And PM* 01 09 43.92388 +35 37 14.0075 5.58 3.62 2.05 0.81 -0.19 M0+IIIa 543 0
8 * ups Per PM* 01 37 59.5569926 +48 37 41.569533 6.29 4.85 3.57 2.61 1.96 K3-IIICN0.5 226 0
9 * nu. Psc * 01 41 25.8939097 +05 29 15.406225 7.36 5.81 4.44 3.38 2.67 K3III 232 0
10 HD 10307 SB* 01 41 47.1268541099 +42 36 48.221567818 5.69 5.58 4.96 4.43 4.10 G1V 486 0
11 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1187 1
12 * gam01 And SB* 02 03 53.95229 +42 19 47.0223 4.22 3.30 2.10 1.16 0.47 K2+IIb 336 0
13 * alf Ari PM* 02 07 10.40570 +23 27 44.7032 4.29 3.17 2.01 1.15 0.54 K2-IIIbCa-1 615 1
14 HD 16160 PM* 02 36 04.9013368983 +06 53 12.383654295   6.81   5.2   K3V 515 0
15 * alf Cet LP? 03 02 16.77307 +04 05 23.0596 6.10 4.17 2.53 1.18 0.02 M1.5IIIa 450 0
16 NGC 1261 GlC 03 12 16.21 -55 12 58.4     8.63     ~ 479 0
17 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1825 1
18 * omi02 Eri Er* 04 15 16.3196189945 -07 39 10.330779018 5.69 5.25 4.43 3.74 3.29 K0V 782 0
19 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1224 1
20 HD 47309 PM* 06 40 49.0410428928 +51 58 41.970261576       7.2   G0 57 0
21 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1829 0
22 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1080 1
23 * g Gem SB* 07 46 07.4484186384 +18 30 35.993172960 8.09 6.33 4.87 3.72 2.89 K4III 170 0
24 HD 71148 PM* 08 27 36.7846606556 +45 39 10.754559179   6.94   5.9   G1V 184 0
25 NGC 2682 OpC 08 51 23 +11 48.8           ~ 2218 0
26 * zet Hya PM* 08 55 23.6261352 +05 56 44.035380 4.92 4.10 3.10 2.39 1.90 G8.5III 234 0
27 * alf Lyn PM* 09 21 03.3002104870 +34 23 33.213441656 6.63 4.69 3.14 1.91 1.01 K6III 203 0
28 HD 88230 Er* 10 11 22.1399492383 +49 27 15.251007087 9.23 7.94 6.61 5.36 4.56 K6VeFe-1 447 0
29 * 46 LMi PM* 10 53 18.7048735 +34 12 53.537492 5.79 4.87 3.83 3.00 2.46 K0+III-IV 230 0
30 * 47 UMa PM* 10 59 27.9727514012 +40 25 48.920572724   5.66   4.7   G1-VFe-0.5 751 1
31 * e Leo * 11 30 18.8933524920 -03 00 12.598924644 8.14 6.31 4.77     K3+IIIFe-0.5 132 0
32 * chi UMa PM* 11 46 03.0140741 +47 46 45.862653 6.06 4.90 3.72 2.84 2.24 K0.5IIIb: 210 0
33 * eps Vir PM* 13 02 10.5978496 +10 57 32.941443 4.45 3.71 2.79 2.16 1.71 G8III-IIIb 538 0
34 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2392 0
35 * eta Boo SB* 13 54 41.07892 +18 23 51.7946 3.440 3.250 2.680 2.24 1.95 G0IV 682 1
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 2244 0
37 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 976 1
38 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1220 0
39 HD 131977 BY* 14 57 28.0007918772 -21 24 55.727265310 7.89 6.83 5.72 4.74 4.19 K4V 466 0
40 * del Boo PM* 15 15 30.1629518 +33 18 53.392558 5.12 4.44 3.49 2.76 2.25 G8IIIFe-1 368 0
41 HD 140283 Pe* 15 43 03.0971190219 -10 56 00.595693188 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 899 0
42 * 18 Sco PM* 16 15 37.2702755653 -08 22 09.982125430   6.15 5.50     G2Va 550 0
43 * eta Her PM* 16 42 53.7650947 +38 55 20.112868 5.03 4.42 3.50 2.83 2.35 G7IIIFe-1 277 0
44 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 2016 0
45 * gam Dra * 17 56 36.36988 +51 29 20.0242 5.630 3.760 2.230 1.08 0.23 K5III 540 0
46 * 109 Her ** 18 23 41.8897062084 +21 46 11.109609046 6.18 5.02 3.84 2.99 2.39 K2IIIab 172 0
47 * kap Cyg PM* 19 17 06.1686516 +53 22 06.453375 5.47 4.73 3.76 3.13 2.66 G9III 201 0
48 M 71 GlC 19 53 46.49 +18 46 45.1           ~ 1081 0
49 * gam Sge PM* 19 58 45.4286265 +19 29 31.728079 6.97 5.04 3.47 2.27 1.35 M0-III 253 0
50 * eta Cep PM* 20 45 17.3755540 +61 50 19.616737 4.960 4.320 3.410 2.76 2.27 K0IV 432 0
51 * eps Cyg ** 20 46 12.6823609 +33 58 12.924926 4.370 3.520 2.480 1.73 1.19 K0III 494 0
52 HD 209458 V* 22 03 10.7727465312 +18 53 03.549393384   8.21 7.63     F9V 1061 1
53 * eps Ind PM* 22 03 21.6536261624 -56 47 09.522795714   5.75 4.69     K5V 514 0
54 * zet Cep EB* 22 10 51.2769159 +58 12 04.545587 6.62 4.90 3.35 2.27 1.49 K1.5Ib 271 0
55 * 11 Lac PM* 22 40 30.8588068 +44 16 34.704241 7.15 5.79 4.46 3.54 2.86 K2.5III 133 0
56 * bet Peg LP* 23 03 46.45746 +28 04 58.0336 6.05 4.09 2.42 0.92 -0.40 M2.5II-III 585 0
57 * 70 Peg SB* 23 29 09.2992398120 +12 45 37.979571348 6.24 5.50 4.56 3.82 3.37 G8IIIa 146 0
58 * lam And RS* 23 37 33.8427800830 +46 27 29.344721109 5.54 4.84 3.82 3.04 2.47 G8IVk 655 0

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2022.11.26-09:49:47

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