2010A&A...519A.105S


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.14CEST13:58:36

2010A&A...519A.105S - Astronomy and Astrophysics, volume 519, A105-105 (2010/9-1)

A physically-motivated photometric calibration of M dwarf metallicity.

SCHLAUFMAN K.C. and LAUGHLIN G.

Abstract (from CDS):

The location of M dwarfs in the (V-Ks)-MKs color-magnitude diagram (CMD) has been shown to correlate with metallicity. We demonstrate that previous empirical photometric calibrations of M dwarf metallicity exploiting this correlation systematically underestimate or overestimate metallicity at the extremes of their range. We improve upon previous calibrations in three ways. First, we use both a volume-limited and kinematically-matched sample of F and G dwarfs from the Geneva-Copehnagen Survey (GCS) to infer the mean metallicity of M dwarfs in the Solar Neighborhood. Second, we use theoretical models of M dwarf interiors and atmospheres to determine the effect of metallicity on M dwarfs in the (V-Ks)-MKs CMD. Third, though we use the GCS to infer the mean metallicity of M dwarfs in the Solar Neighborhood, our final calibration is based purely on high-resolution spectroscopy of FGK primaries with M dwarf companions as well as the trigonometric parallaxes and apparent V- and Ks-band magnitudes of those M dwarf companions. As a result, our photometric calibration explains an order of magnitude more of the variance in the calibration sample than previous photometric calibrations. We use our calibration to non-parametrically quantify the significance of the observation that M dwarfs that host exoplanets are preferentially in a region of the (V-Ks)-MKs plane populated by metal-rich M dwarfs. We find that the probability p that planet-hosting M dwarfs are distributed across the (V-Ks)-MKs CMD in the same way as field M dwarfs is p=0.06±0.008. Interestingly, the subsample of M dwarfs that host Neptune and sub-Neptune mass planets may also be preferentially located in the region of the (V-Ks)-MKs plane populated by high-metallicity M dwarfs. The probability of this occurrence by chance is p=0.40±0.02, and this observation hints that low-mass planets may be more likely to be found around metal-rich M dwarfs. The confirmation of this hint would be in contrast to the result obtained for FGK stars, where it appears that metal-rich and metal-poor stars hosts Neptune-mass planets with approximately equal probability. An increased rate of low-mass planet occurrence around metal-rich M dwarfs would be a natural consequence of the core-accretion model of planet formation.

Abstract Copyright:

Journal keyword(s): planets and satellites: formation - stars: abundances - stars: low-mass - stars: statistics

Simbad objects: 32

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Number of rows : 32

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 HD 6660B PM* 01 07 38.5333790402 +22 57 20.722795290   15.6 13.60 14.21   M3.5Ve 35 0
2 G 272-127 PM* 01 57 11.0549604018 -10 14 53.303154135   11.39 10.56 10.758 9.41 M0.0Ve 25 1
3 NGC 752 OpC 01 57 41 +37 47.1           ~ 538 0
4 V* BX Cet BY* 02 36 15.2666844128 +06 52 17.924295081   13.28   11.405   M3.5V 154 1
5 * tet Per B PM* 02 44 10.2671029181 +49 13 54.003171390   10.8 9.87 9.6   M1.5V 49 1
6 HD 18143C PM* 02 55 35.7790759279 +26 52 20.464563691   15.45   13.493   M4.0V 48 1
7 * omi02 Eri C Er* 04 15 21.5389590304 -07 39 20.718136574   12.85 11.17     M4.5V 189 0
8 HD 285968 PM* 04 42 55.7753203198 +18 57 29.394344631 12.668 11.49 9.951 8.931 7.702 M2.5V 251 2
9 Wolf 1539 PM* 04 52 05.7323109095 +06 28 35.589503596 14.791 13.568 12.018 10.854 9.334 M2V 122 1
10 HD 233153 PM* 05 41 30.7305969608 +53 29 23.290085020   11.31   9.343   M1.0V 151 0
11 HD 38529B PM* 05 46 19.3765701218 +01 12 47.263218467   13.9   13.010   M2.5V 17 1
12 G 106-36 PM* 06 17 10.6528247532 +05 07 02.359413607   14.91 13.32 12.852   M3.5V 46 1
13 HD 46375B PM* 06 33 12.0900929259 +05 27 53.170881462     11.8 11.683   M2.0V 13 0
14 HD 50281B ** 06 52 18.0414038629 -05 11 24.039080436   11.47 10.05 9.870   M2.5V 104 0
15 * 18 Pup B ** 08 10 34.2940211397 -13 48 51.131341156   13.29 11.815 11.422   M2.5V 46 0
16 L 675-81 PM* 08 40 59.2055621000 -23 27 22.598649814   13.2 11.975 11.637 9.37 M3.5V 106 1
17 * rho01 Cnc B PM* 08 52 40.8627482955 +28 18 58.824842873   14.80   12.814   M4.5V 117 1
18 Ross 905 PM* 11 42 11.0933874353 +26 42 23.658083337   12.06 10.613 10.272 8.24 M3V 498 1
19 V* V645 Cen Er* 14 29 42.9451234609 -62 40 46.170818907 14.21 12.95 11.13 9.45 7.41 M5.5Ve 966 0
20 BD-07 4003 BY* 15 19 26.8271336166 -07 43 20.190958776 13.403 11.76 10.560 9.461 8.911 M3V 538 2
21 LP 804-27 PM* 16 12 41.7802216507 -18 52 31.811210360 14.015 12.88 11.372 10.289 9.37 M3V 51 1
22 BD+25 3173 PM* 16 58 08.8497933735 +25 44 38.971120252 12.342 11.139 9.655 8.685 7.602 M2V 169 1
23 G 139-21 PM* 17 15 18.9337265994 +04 57 50.064695682   16.40   14.394   M4.5V 239 1
24 CD-46 11540 PM* 17 28 39.9455601300 -46 53 42.693246243 12.177 10.973 9.407 8.337 7.006 M3V 205 1
25 IC 4756 OpC 18 38 31.2 +05 29 24           ~ 199 0
26 * omi Aql B PM* 19 51 00.6800315390 +10 24 39.851890982     13.7 12.72   M4 28 1
27 G 125-55 PM* 20 03 26.5808933057 +29 51 59.527225990       14.09 11.24 M4.5V 67 0
28 G 143-35 PM* 20 11 13.2595959381 +16 11 07.989062567   15.55 13.932 13.774   M4.0V 50 1
29 L 1288-4 ** 20 40 44.5176 +19 54 03.126   13.42   11.46   M2.5V 49 1
30 HD 204961 PM* 21 33 33.9749932664 -49 00 32.403471949 11.359 10.176 8.672 7.665 6.479 M2/3V 209 1
31 BD-05 5715 PM* 22 09 40.3443754647 -04 38 26.651267098 13.006 11.868 10.366 9.279 7.877 M3.5V 222 1
32 BD-15 6290 BY* 22 53 16.7323107416 -14 15 49.303409936 12.928 11.749 10.192 9.013 7.462 M3.5V 859 1

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2020.08.14-13:58:36

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