J/ApJS/250/29 Search for nearby Earth analogs. III. RV sets (Feng+, 2020)
Search for nearby Earth analogs.
III. Detection of 10 new planets, 3 planet candidates, and confirmation of
3 planets around 11 nearby M dwarfs.
Feng F., Shectman S.A., Clement M.S., Vogt S.S., Tuomi M., Teske J.K.,
Burt J., Crane J.D., Holden B., Wang S.X., Thompson I.B., Diaz M.R.,
Butler R.P.
<Astrophys. J. Suppl. Ser., 250, 29 (2020)>
=2020ApJS..250...29F 2020ApJS..250...29F
ADC_Keywords: Stars, M-type; Radial velocities; Spectra, optical
Keywords: Exoplanet astronomy ; Radial velocity ; Exoplanet detection methods ;
M dwarf stars ; Astrostatistics ; High resolution spectroscopy
Abstract:
Earth-sized planets in the habitable zones of M dwarfs are good
candidates for the study of habitability and detection of
biosignatures. To search for these planets, we analyze all available
radial velocity data and apply four signal detection criteria to
select the optimal candidates. We find 10 strong candidates satisfying
these criteria and three weak candidates showing inconsistency over
time due to data samplings. We also confirm three previous planet
candidates and improve their orbital solutions through combined
analyses of updated data sets. Among the strong planet candidates,
HIP38594b is a temperate super-Earth with a mass of 8.2±1.7M⊕
and an orbital period of 60.7±0.1 days, orbiting around an
early-type M dwarf. Early-type M dwarfs are less active and thus are
better hosts for habitable planets than mid-type and late-type M
dwarfs. Moreover, we report the detection of five two-planet systems,
including two systems made up of a warm or cold Neptune and a cold
Jupiter, consistent with a positive correlation between these two
types of planets. We also detect three temperate Neptunes, four cold
Neptunes, and four cold Jupiters, contributing to a rarely explored
planet population. Due to their proximity to the Sun, these planets on
wide orbits are appropriate targets for direct imaging by future
facilities such as the Habitable Exoplanet Observatory and the
Extremely Large Telescope.
Description:
We select M dwarfs with RV data sets from the Automated Planet Finder
(APF), the High Accuracy Radial velocity Planet Searcher (HARPS), the
High Resolution Echelle Spectrometer mounted on a Keck telescope
(HIRES/Keck), the Planet Finder Spectrograph (PFS), and the
Spectrographe pour l'Observation des Phenomenes des Interieurs
stellaires et des Exoplanetes (SOPHIE). Based on comprehensive
analyses, we identify eleven stars that probably host planets.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 78 11 Stellar parameters and radial velocity (RV) data sets
table2.dat 69 901 RV data sets
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
J/ApJ/646/505 : Catalog of nearby exoplanets (Butler+, 2006)
J/A+A/523/A48 : Gaia photometry (Jordi+, 2010)
J/ApJ/812/3 : MEarth mid-to-late M dwarfs kinematics (West+, 2015)
J/A+A/600/A13 : HARPS M dwarf magnetic activity (Astudillo-Defru+, 2017)
J/AJ/153/208 : LCES HIRES/Keck RV Exoplanet Survey (Butler+, 2017)
J/AJ/156/276 : Exoplanet atmospheric data with MIRI (Danielski+, 2018)
J/AJ/155/39 : Variability data of TIC stars with KELT (Oelkers+, 2018)
J/other/Nat/563.365 : Barnard's star radial velocity curve (Ribas+, 2018)
J/A+A/616/A7 : Gaia DR2 RV standard stars cat. (Soubiran+, 2018)
J/AJ/157/52 : RV obs. in super-Earth systems (Bryan+, 2019)
J/MNRAS/484/L8 : Systematic errors for HIRES/Keck RVs (Tal-Or+, 2019)
J/A+A/627/A49 : Teegarden's Star RV & Hα (Zechmeister+, 2019)
J/A+A/636/A74 : HARPS radial velocity database (Trifonov+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Main name of the star
11- 24 A14 --- OName Other name
26- 31 A6 --- SpT SIMBAD spectral type
33- 36 F4.2 Msun Mass [0.15/0.63] Stellar mass from TESS Input Catalog
(TIC; Stassun+, 2019, IV/38)
38- 41 F4.2 Msun e_Mass [0.02/0.08] Mass uncertainty
43- 48 F6.2 mas Plx [35.13/223.63] Gaia DR2 parallax
50- 53 F4.2 mas e_Plx [0.03/0.11] Parallax uncertainty
55- 58 F4.1 mag Vmag [8.9/12.5] V magnitude (1)
60- 62 I3 --- APF [0/149] Number of RVs from APF
64- 65 I2 --- H1 [0/84] Number of RVs from "HARPSpre" (before the
fiber change for HARPS in 2015)
67- 68 I2 --- H2 [0/48] Number of RVs from "HARPSpost" (after the
fiber change for HARPS in 2015)
70- 72 I3 --- Keck [0/147] Number of RVs from Keck
74- 75 I2 --- PFS [0/55] Number of RVs from PSF
77- 78 I2 --- Soph [0/12] Number of RVs from SOPHIE
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Note (1): The V magnitude is derived from the G magnitude from Gaia DR2 (I/345)
according to Jordi+ (2010, J/A+A/523/A48)
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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- 9 A9 --- Name Star name
11- 23 F13.5 d BJD Barycentric Julian Date
25- 44 F20.15 m/s RV [-106.5/97.6] Barycenter corrected radial velocity
46- 62 F17.14 m/s e_RV [0.8/7.2] Uncertainty in RV
64- 69 A6 --- Inst Instrument (1)
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Note (1): Instruments used as follows:
APF = Levy spectrometer mounted on the 2.4m Automated Planet Finder
(279 occurrences);
KECK = HIRES/KECK (383 occurrences);
PFS = Carnegie Planet Finder Spectrograph (227 occurrences);
SOPHIE = SOPHIE data released by Soubiran+ (2018, J/A+A/616/A7)
with correction of zero point drift (Courcol+ 2015A&A...581A..38C 2015A&A...581A..38C)
(12 occurrences).
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History:
From electronic version of the journal
References:
Feng et al. Paper I. 2019ApJS..242...25F 2019ApJS..242...25F
Feng et al. Paper II. 2020ApJS..246...11F 2020ApJS..246...11F Cat. J/ApJS/246/11
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Nov-2020