J/ApJ/919/100 Abundances of 6 stars in Praesepe cluster (Vejar+, 2021)
Detailed abundances of planet-hosting open clusters. The Praesepe (Beehive)
Cluster.
Vejar G., Schuler S.C., Stassun K.G.
<Astrophys. J., 919, 100 (2021)>
=2021ApJ...919..100V 2021ApJ...919..100V
ADC_Keywords: Abundances; Stars, G-type; Stars, F-type; Exoplanets;
Spectra, optical; Equivalent widths; Clusters, open
Keywords: Star-planet interactions ; Exoplanet systems ;
Extrasolar gaseous giant planets ; Optical observation ;
High resolution spectroscopy ; Open star clusters ;
Stellar abundances ; Planet formation
Abstract:
It is not yet fully understood how planet formation affects the
properties of host stars, in or out of a cluster; however, abundance
trends can help us understand this process. We present a detailed
chemical abundance analysis of six stars in Praesepe, a planet-hosting
open cluster. Pr0201 is known to host a close-in (period of 4.4days)
giant planet (mass of 0.54MJ), while the other five cluster members
in our sample (Pr0133, Pr0081, Pr0208, Pr0051, and Pr0076) have no
detected planets according to measurements of radial velocity. Using
high-resolution echelle spectra with high signal-to-noise ratio
obtained with Keck/HIRES and a novel approach to measurements of
equivalent width (XSpect-EW), we derived abundances of up to
20 elements spanning a range of condensation temperatures (TC). We
find a mean cluster metallicity of [Fe/H]=+0.21±0.02dex, in
agreement with most previous determinations. We find most of our
elements show an [X/Fe] scatter of ∼0.02-0.03dex and conclude that our
stellar sample is chemically homogeneous. The TC slope for the cluster
mean abundances is consistent with zero and none of the stars in our
sample exhibit individually a statistically significant TC slope.
Using a planet engulfment model, we find that the planet host, Pr0201,
shows no evidence of significant enrichment in its refractory elements
when compared to the cluster mean that would be consistent with a
planetary accretion scenario.
Description:
Three of the six stars (Pr0201, Pr0051, and Pr0076) were observed on
UT 2013 December 9 with the HIRES echelle spectrograph in the R=72000
mode on the 10m Keck I telescope. The spectra cover a wavelength range
of 4600-9000Å.
For the remaining three stars, Pr0133, Pr0208, and Pr0081, we obtained
raw data files from the Keck Observatory Archive (KOA). These spectra
were taken in UT 2003 January and February belonging to program ID
H39aH and H47aH; the data are fully described in
Boesgaard+ (2013ApJ...775...58B 2013ApJ...775...58B).
We also obtained an archive spectrum for Pr0076 from the same program
to verify that our analysis produces consistent results between these
different sets of spectra. In our final results we report the stellar
parameters and abundances for Pr0076 from both data sets and adopt the
results from data taken in 2013.
The archive spectra covered a smaller wavelength range (5650-8090Å)
than our new spectra and were obtained in the R=48000 mode.
We required a solar spectrum to derive the solar abundances used to
determine the abundances of our target stars relative to the Sun. For
this purpose, we used the high-quality Keck/HIRES solar spectrum
(S/N∼800 near 6700Å) from Schuler+ (2015, J/ApJ/815/5) obtained in
2010 June in the R=50000 mode over the wavelength range 3750-8170Å.
See Section 2.2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 49 7 *Stellar parameters
table2.dat 118 191 Lines measured, equivalent widths, and abundances
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Note on table1.dat: Adopted solar parameters:
Teff=5777K, logg=4.44, and ξ=1.38km/s
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/AJ/124/1570 : JHKs photometry in Praesepe (Adams+, 2002)
J/A+A/489/403 : Line abundances for solar stars (Pace+, 2008)
J/A+A/508/L17 : Abundances in solar analogs (Ramirez+, 2009)
J/A+A/535/A30 : Abundance of 12 stars in open clusters (Carrera+, 2011)
J/ApJ/737/L32 : Abundances of 16 Cyg A and B (Schuler+, 2011)
J/A+A/583/A135 : XO-2N and XO-2S spectra (Biazzo+, 2015)
J/AJ/150/97 : RVs in M67. I. 1278 candidate members (Geller+, 2015)
J/MNRAS/446/3556 : O, Na, Ba & Eu abundances in open clusters (MacLean+, 2015)
J/ApJ/808/13 : XO-2S and XO-2N chemical composition (Ramirez+, 2015)
J/MNRAS/450/4301 : Line list for red giants in open clusters (Reddy+, 2015)
J/A+A/582/A17 : Keck+HIRES spectra of HD 80606 and HD 80607 (Saffe+, 2015)
J/ApJ/815/5 : Abundances of KOI stars with planets. I. (Schuler+, 2015)
J/ApJ/801/L10 : XO-2N and XO-2S equivalent widths (Teske+, 2015)
J/MNRAS/463/696 : M67 solar twins chemical compositions (Liu+, 2016)
J/ApJ/831/11 : KIC9777062 RVs & asteroseis. in NGC6811 (Sandquist+, 2016)
J/AJ/152/180 : Bolometric fluxes of EBs in Tycho-2 (Stassun+, 2016)
J/A+A/604/L4 : HAT-P-4 & TYC2569-744-1 abundances & spectra (Saffe+, 2017)
J/AJ/155/138 : WOCS.LXXVI. Vel. & abund. in NGC2506 (Anthony-Twarog+, 2018)
J/A+A/618/A93 : Gaia DR2 open clusters in Milky Way (Cantat-Gaudin+, 2018)
J/A+A/628/A54 : Fe, Mg, Ti in Galactic clusters (Kovalev+, 2019)
J/ApJ/878/99 : Abund. of dwarfs & giants in NGC752 with HIRES (Lum+, 2019)
J/MNRAS/487/2385 : Distances and ages of 150 open clusters (Monteiro+, 2019)
J/A+A/633/A38 : EW of 10 solar-type stars of Praesepe (D'Orazi+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Name Star name
8- 11 I4 --- m_Name [2003/2013]? Observation year for Pr0076
13- 16 I4 K Teff [5731/6168] Effective temperature
18- 19 I2 K e_Teff [24/72] Teff uncertainty
21- 24 F4.2 [cm/s2] logg [4.18/4.5] Log of surface gravity
26- 29 F4.2 [cm/s2] e_logg [0.07/0.13] logg uncertainty
31- 34 F4.2 [Sun] [Fe/H] [0.16/0.3] Metallicity
36- 39 F4.2 [Sun] e_[Fe/H] [0.03/0.07] [Fe/H] uncertainty
41- 44 F4.2 km/s Vt [1.3/1.8] Microturbulent velocity, ξ
46- 49 F4.2 km/s e_Vt [0.03/0.11] Vt uncertainty
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Ion Ion identifier
6- 13 F8.3 0.1nm lambda [4620.5/7775.4] Wavelength, vacuum in Å
15- 20 F6.3 eV ExPot [0/10.4] Excitation potential (1)
22- 27 F6.3 [-] loggf [-9.72/0.4] Log, statistical
weight*oscillator strength (1)
29- 34 F6.2 0.1pm EW-Solar [4/156]? Equivalent Width, Solar template (2)
36- 40 F5.3 [-] logN-Solar [3/8.93]? Abundance, Solar template (2)
42- 47 F6.2 0.1pm EW-Pr0201 [4.9/156.3]? Equivalent Width, Pr0201,
milli-Angstroms
49- 53 F5.3 [-] logN-Pr0201 [3/9.2]? Abundance, Pr0201
55- 60 F6.2 0.1pm EW-Pr0133 [11.5/164]? Equivalent Width, Pr0133,
milli-Angstroms
62- 66 F5.3 [-] logN-Pr0133 [2.9/9.2]? Abundance, Pr0133
68- 73 F6.2 0.1pm EW-Pr0208 [8.8/118]? Equivalent Width, Pr0208,
milli-Angstroms
75- 79 F5.3 [-] logN-Pr0208 [3/9.1]? Abundance, Pr0208
81- 86 F6.2 0.1pm EW-Pr0081 [10.2/172]? Equivalent Width, Pr0081,
milli-Angstroms
88- 92 F5.3 [-] logN-Pr0081 [3/9.1]? Abundance, Pr0081
94- 99 F6.2 0.1pm EW-Pr0051 [7.6/165]? Equivalent Width, Pr0051,
milli-Angstroms
101- 105 F5.3 [-] logN-Pr0051 [3/9.1]? Abundance, Pr0051
107- 112 F6.2 0.1pm EW-Pr0076 [8.4/175]? Equivalent Width, Pr0076,
milli-Angstroms
114- 118 F5.3 [-] logN-Pr0076 [3/9.2]? Abundance, Pr0076
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Note (1): Atomic excitation energies and transition probabilities
taken from Mack+ (2014ApJ...787...98M 2014ApJ...787...98M).
Note (2): Keck/HIRES solar spectrum from Schuler+ (2015, J/ApJ/815/5)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-Jan-2023