J/A+A/558/A106 Chemical abundances for 83 transit hosts (Mortier+, 2013)
New and updated stellar parameters for 90 transit hosts.
The effect of the surface gravity.
Mortier A., Santos N.C., Sousa S.G., Fernandes J.M., Adibekyan V.Zh.,
Delgado Mena E., Montalto M., Israelian G.
<Astron. Astrophys. 558, A106 (2013)>
=2013A&A...558A.106M 2013A&A...558A.106M
ADC_Keywords: Stars, double and multiple ; Planets ; Abundances
Keywords: stars: fundamental parameters - stars: abundances -
planets and satellites: fundamental parameters -
techniques: spectroscopic
Abstract:
Precise stellar parameters are crucial in exoplanet research for
correctly determining of the planetary parameters. For stars hosting a
transiting planet, determining of the planetary mass and radius
depends on the stellar mass and radius, which in turn depend on the
atmospheric stellar parameters. Different methods can provide
different results, which leads to different planet characteristics.
In this paper, we use a uniform method to spectroscopically derive
stellar atmospheric parameters, chemical abundances, stellar masses,
and stellar radii for a sample of 90 transit hosts. Surface gravities
are also derived photometrically using the stellar density as derived
from the light curve. We study the effect of using these different
surface gravities on the determination of the chemical abundances and
the stellar mass and radius.
A spectroscopic analysis based on Kurucz models in LTE was performed
through the MOOG code to derive the atmospheric parameters and the
chemical abundances. The photometric surface gravity was determined
through isochrone fitting and the use of the stellar density, directly
determined from the light curve. Stellar masses and radii are
determined through calibration formulae.
Spectroscopic and photometric surface gravities differ, but this has
very little effect on the precise determination of the stellar mass in
our spectroscopic analysis. The stellar radius, and hence the
planetary radius, is most affected by the surface gravity
discrepancies. For the chemical abundances, the difference is, as
expected, only noticable for the abundances derived from analyzing of
lines of ionized species.
Description:
Table 5 contains chemical abundances for 83 stars in the sample,
calculated with the spectroscopic and photometric (suffix 2) logg.
99.99 is used if no value is available.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 125 90 Stellar parameters for the transit hosts
table5.dat 391 83 Chemical abundances of the transit hosts
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See also:
J/A+A/543/A45 : Planets around metal-poor stars (Mortier+, 2012)
J/A+A/551/A112 : Metallicity-giant planet correlation (Mortier+, 2013)
J/A+A/557/A70 : Evolved planet hosts - stellar parameters (Mortier+, 2013)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Star Star name
13- 16 I4 K Teff Effective temperature (spectroscopic)
18- 20 I3 K e_Teff Mean error on Teff
22- 25 F4.2 [cm/s2] logg Gravity (spectroscopic)
27- 30 F4.2 [cm/s2] e_logg Mean error on logg
35- 39 F5.2 [Sun] [Fe/H] Metallicity (spectroscopic)
41- 44 F4.2 [Sun] e_[Fe/H] Mean error on [Fe/H]
48- 51 F4.2 km/s Vt Microturbulence velocity ξ
53- 56 F4.2 km/s e_Vt Mean error on Vt
60- 63 F4.2 Msun M Mass (spectroscopic)
65- 68 F4.2 Msun e_M Mean error on M
70- 73 F4.2 Rsun R Star radius (spectroscopic)
75- 78 F4.2 Rsun e_R Mean error on R
80- 83 F4.2 Sun rho Stellar density ρ, relative to Sun
85- 88 F4.2 Sun e_rho Mean error on rho
90- 91 I2 --- Ref [1/40] Reference of spectroscopic parameters (2)
95- 98 F4.2 [cm/s2] logg2 ? log.gLC, gravity (photometric)
100-103 F4.2 [cm/s2] e_logg2 ? Mean error on logg2
107-110 F4.2 Msun M2 ? Mass MLC (photometric)
112-115 F4.2 Msun e_M2 ? Mean error on M2
117-120 F4.2 Rsun R2 ? Star radius RLC (photometric)
122-125 F4.2 Rsun e_R2 ? Mean error on R2
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Note (2): References as follows:
1 = Southworth 2011MNRAS.417.2166S 2011MNRAS.417.2166S
2 = Southworth 2012MNRAS.426.1291S 2012MNRAS.426.1291S
3 = Southworth 2010MNRAS.408.1689S 2010MNRAS.408.1689S
4 = Howard et al. 2012ApJ...749..134H 2012ApJ...749..134H
5 = Bakos et al. 2011ApJ...742..116B 2011ApJ...742..116B
6 = Hartman et al. 2011ApJ...728..138H 2011ApJ...728..138H
7 = Beky et al. 2011ApJ...734..109B 2011ApJ...734..109B
8 = Johnson et al. 2011ApJ...735...24J 2011ApJ...735...24J
9 = Bakos et al. 2012AJ....144...19B 2012AJ....144...19B
10 = Todorov et al. 2012ApJ...746..111T 2012ApJ...746..111T
11 = Henry et al. 2011, 1109.2549
12 = Howell et al. 2012ApJ...746..123H 2012ApJ...746..123H
13 = West et al. 2009A&A...502..395W 2009A&A...502..395W
14 = West et al. 2009AJ....137.4834W 2009AJ....137.4834W
15 = Lister et al. 2009ApJ...703..752L 2009ApJ...703..752L
16 = Hebb et al. 2010ApJ...708..224H 2010ApJ...708..224H
17 = Maxted et al. 2010AJ....140.2007M 2010AJ....140.2007M
18 = Triaud et al. 2011A&A...531A..24T 2011A&A...531A..24T
19 = Street et al. 2010ApJ...720..337S 2010ApJ...720..337S
20 = Enoch et al. 2011MNRAS.410.1631E 2011MNRAS.410.1631E
21 = Smalley et al. 2010A&A...520A..56S 2010A&A...520A..56S
22 = West R.G., Anderson D.R., Gillon M., et al. 2013, submitted
23 = Hellier et al. 2010ApJ...723L..60H 2010ApJ...723L..60H
24 = Anderson et al. 2011A&A...531A..60A 2011A&A...531A..60A
25 = Maxted et al. 2010PASP..122.1465M 2010PASP..122.1465M
26 = Smalley et al. 2011A&A...526A.130S 2011A&A...526A.130S
27 = Enoch et al. 2011AJ....142...86E 2011AJ....142...86E
28 = Smith et al. 2012AJ....143...81S 2012AJ....143...81S
29 = Barros et al. 2011A&A...525A..54B 2011A&A...525A..54B
30 = Maxted et al. 2011PASP..123..547M 2011PASP..123..547M
31 = Lendl et al. 2012A&A...544A..72L 2012A&A...544A..72L
32 = Anderson et al. 2012MNRAS.422.1988A 2012MNRAS.422.1988A
33 = Hellier et al. 2012MNRAS.426..739H 2012MNRAS.426..739H
34 = Gillon et al. 2011A&A...533A..88G 2011A&A...533A..88G
35 = Faedi et al. 2013A&A...551A..73F 2013A&A...551A..73F
36 = Gillon et al. 2009A&A...501..785G 2009A&A...501..785G
37 = Smith et al. 2013A&A...552A.120S 2013A&A...552A.120S
38 = Maxted et al. 2013PASP..125...48M 2013PASP..125...48M
39 = Smalley et al. 2012A&A...547A..61S 2012A&A...547A..61S
40 = Queloz et al. 2010A&A...517L...1Q 2010A&A...517L...1Q
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Star Star name
17- 21 F5.2 [Sun] [AlI/H] ?=99.99 AlI abundance
23- 27 F5.2 [Sun] e_[AlI/H] ?=99.99 Error on AlI abundance
29- 33 F5.2 [Sun] [CaI/H] ?=99.99 CaI abundance
35- 39 F5.2 [Sun] e_[CaI/H] ?=99.99 Error on CaI abundance
41- 45 F5.2 [Sun] [CoI/H] ?=99.99 CoI abundance
47- 51 F5.2 [Sun] e_[CoI/H] ?=99.99 Error on CoI abundance
53- 57 F5.2 [Sun] [CrI/H] ?=99.99 CrI abundance
59- 63 F5.2 [Sun] e_[CrI/H] ?=99.99 Error on CrI abundance
65- 69 F5.2 [Sun] [CrII/H] ?=99.99 CrII abundance
71- 75 F5.2 [Sun] e_[CrII/H] ?=99.99 Error on CrII abundance
77- 81 F5.2 [Sun] [MgI/H] ?=99.99 MgI abundance
83- 87 F5.2 [Sun] e_[MgI/H] ?=99.99 Error on MgI abundance
89- 93 F5.2 [Sun] [MnI/H] ?=99.99 MnI abundance
95- 99 F5.2 [Sun] e_[MnI/H] ?=99.99 Error on MnI abundance
101-105 F5.2 [Sun] [NaI/H] ?=99.99 NaI abundance
107-111 F5.2 [Sun] e_[NaI/H] ?=99.99 Error on NaI abundance
113-117 F5.2 [Sun] [NiI/H] ?=99.99 NiI abundance
119-123 F5.2 [Sun] e_[NiI/H] ?=99.99 Error on NiI abundance
125-129 F5.2 [Sun] [ScI/H] ?=99.99 ScI abundance
131-135 F5.2 [Sun] e_[ScI/H] ?=99.99 Error on ScI abundance
137-141 F5.2 [Sun] [ScII/H] ?=99.99 ScII abundance
143-147 F5.2 [Sun] e_[ScII/H] ?=99.99 Error on ScII abundance
149-153 F5.2 [Sun] [SiI/H] ?=99.99 SiI abundance
155-159 F5.2 [Sun] e_[SiI/H] ?=99.99 Error on SiI abundance
161-165 F5.2 [Sun] [TiI/H] ?=99.99 TiI abundance
167-171 F5.2 [Sun] e_[TiI/H] ?=99.99 Error on TiI abundance
173-177 F5.2 [Sun] [TiII/H] ?=99.99 TiII abundance
179-183 F5.2 [Sun] e_[TiII/H] ?=99.99 Error on TiII abundance
185-189 F5.2 [Sun] [VI/H] ?=99.99 VI abundance
191-195 F5.2 [Sun] e_[VI/H] ?=99.99 Error on VI abundance
197-201 F5.2 [Sun] [AlI/H]2 ?=99.99 AlI abundance with loggLC (1)
203-207 F5.2 [Sun] e_[AlI/H]2 ?=99.99 Error on AlI abundance with loggLC
209-213 F5.2 [Sun] [CaI/H]2 ?=99.99 CaI abundance with loggLC (1)
215-219 F5.2 [Sun] e_[CaI/H]2 ?=99.99 Error on CaI abundance with loggLC
221-225 F5.2 [Sun] [CoI/H]2 ?=99.99 CoI abundance with loggLC (1)
227-231 F5.2 [Sun] e_[CoI/H]2 ?=99.99 Error on CoI abundance with loggLC
233-237 F5.2 [Sun] [CrI/H]2 ?=99.99 CrI abundance with loggLC (1)
239-243 F5.2 [Sun] e_[CrI/H]2 ?=99.99 Error on CrI abundance with loggLC
245-249 F5.2 [Sun] [CrII/H]2 ?=99.99 CrII abundance with loggLC (1)
251-255 F5.2 [Sun] e_[CrII/H]2 ?=99.99 Error on CrII abundance with loggLC
257-261 F5.2 [Sun] [MgI/H]2 ?=99.99 MgI abundance with loggLC (1)
263-267 F5.2 [Sun] e_[MgI/H]2 ?=99.99 Error on MgI abundance with loggLC
269-273 F5.2 [Sun] [MnI/H]2 ?=99.99 MnI abundance with loggLC (1)
275-279 F5.2 [Sun] e_[MnI/H]2 ?=99.99 Error on MnI abundance with loggLC
281-285 F5.2 [Sun] [NaI/H]2 ?=99.99 NaI abundance with loggLC (1)
287-291 F5.2 [Sun] e_[NaI/H]2 ?=99.99 Error on NaI abundance with loggLC
293-297 F5.2 [Sun] [NiI/H]2 ?=99.99 NiI abundance with loggLC (1)
299-303 F5.2 [Sun] e_[NiI/H]2 ?=99.99 Error on NiI abundance with loggLC
305-309 F5.2 [Sun] [ScI/H]2 ?=99.99 ScI abundance with loggLC (1)
311-315 F5.2 [Sun] e_[ScI/H]2 ?=99.99 Error on ScI abundance with loggLC
317-321 F5.2 [Sun] [ScII/H]2 ?=99.99 ScII abundance with loggLC (1)
323-327 F5.2 [Sun] e_[ScII/H]2 ?=99.99 Error on ScII abundance with loggLC
329-333 F5.2 [Sun] [SiI/H]2 ?=99.99 SiI abundance with loggLC (1)
335-339 F5.2 [Sun] e_[SiI/H]2 ?=99.99 Error on SiI abundance with loggLC
341-345 F5.2 [Sun] [TiI/H]2 ?=99.99 TiI abundance with loggLC (1)
347-351 F5.2 [Sun] e_[TiI/H]2 ?=99.99 Error on TiI abundance with loggLC
353-357 F5.2 [Sun] [TiII/H]2 ?=99.99 TiII abundance with loggLC (1)
359-363 F5.2 [Sun] e_[TiII/H]2 ?=99.99 Error on TiII abundance with loggLC
365-369 F5.2 [Sun] [VI/H]2 ?=99.99 VI abundance with loggLC (1)
371-375 F5.2 [Sun] e_[VI/H]2 ?=99.99 Error on VI abundance with loggLC
377-381 F5.2 [-] A(Li) ?=99.99 Lithium abundance (logN(Li)/N(H)+12)
383-387 F5.2 [-] e_A(Li) ?=99.99 Error on lithium abundance
389-391 A3 --- l_A(Li) [yes ] Lithium upper limit?
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Note (1): computed with the value of log(g) derived from the photometry
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Acknowledgements:
Annelies Mortier, amortier(at)astro.up.pt
(End) Annelies Mortier [CAUP-Porto, Portugal] Patricia Vannier [CDS] 18-Sep-2013