J/AJ/158/181 Radial velocities and S-index values for HR 5183 (Blunt+, 2019)
Radial velocity discovery of an eccentric Jovian world orbiting at 18 au.
Blunt S., Endl M., Weiss L.M., Cochran W.D., Howard A.W., MacQueen P.J.,
Fulton B.J., Henry G.W., Johnson M.C., Kosiarek M.R., Lawson K.D.,
Macintosh B., Mills S.M., Nielsen E.L., Petigura E.A., Schneider G.,
Vanderburg A., Wisniewski J.P., Wittenmyer R.A., Brugamyer E., Caldwell C.,
Cochran A.L., Hatzes A.P., Hirsch L.A., Isaacson H., Robertson P., Roy A.,
Shen Z.
<Astron. J., 158, 181 (2019)>
=2019AJ....158..181B 2019AJ....158..181B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Radial velocities ; Exoplanets
Keywords: planets and satellites: detection -
planets and satellites: fundamental parameters -
stars: individual (HR 5183)
Abstract:
Based on two decades of radial velocity (RV) observations using Keck/High
Resolution Echelle Spectrometer (HIRES) and McDonald/Tull, and more recent
observations using the Automated Planet Finder, we found that the nearby
star HR 5183 (HD 120066) hosts a 3 MJ minimum mass planet with an orbital
period of 74-22+43 yr. The orbit is highly eccentric (e∼0.84),
shuttling the planet from within the orbit of Jupiter to beyond the orbit
of Neptune. Our careful survey design enabled high cadence observations
before, during, and after the planet's periastron passage, yielding precise
orbital parameter constraints. We searched for stellar or planetary
companions that could have excited the planet's eccentricity, but found no
candidates, potentially implying that the perturber was ejected from
the system. We did identify a bound stellar companion more than 15000 au
from the primary, but reasoned that it is currently too widely separated
to have an appreciable effect on HR 5183 b. Because HR 5183 b's wide orbit
takes it more than 30 au (1") from its star, we also explored the potential
of complimentary studies with direct imaging or stellar astrometry. We
found that a Gaia detection is very likely, and that imaging at 10 µm
is a promising avenue. This discovery highlights the value of long-baseline
RV surveys for discovering and characterizing long-period, eccentric Jovian
planets. This population may offer important insights into the dynamical
evolution of planetary systems containing multiple massive planets.
Description:
Doppler monitoring of HR 5183 began in 1997 at Keck/HIRES and in 1999 at
McDonald/Tull. HR 5183 was also monitored on the Automated Planet Finder
(APF) with high cadence since its commissioning in 2013. The APF is an
automated 2.4 meter telescope at Lick Observatory on Mt. Hamilton,
California.
Between 1997 and 2019, 78 high-resolution (R=60000) spectra of HR 5183 with
the HIRES spectrograph (Vogt et al. 1994SPIE.2198..362V 1994SPIE.2198..362V; Cumming et al.
2008PASP..120..531C 2008PASP..120..531C; Howard et al. 2010, J/other/Sci/330.653) were
obtained. Between 1999 and 2019, 175 high-resolution (R=60000) spectra with
the Tull Coude Spectrograph (Tull et al. 1995PASP..107..251T 1995PASP..107..251T) on the 2.7 m
Harlan J. Smith telescope were collected, as part of the McDonald
Observatory planet search (Cochran et al. 1997ApJ...483..457C 1997ApJ...483..457C; Hatzes et al.
2000ApJ...544L.145H 2000ApJ...544L.145H). Finally, between 2013 and 2019, 104 spectra of HR 5183
with the APF (Radovan et al. 2014SPIE.9145E..2BR; Vogt et al.
2014PASP..126..359V 2014PASP..126..359V) were obtained.
Objects:
-------------------------------------------------
RA (ICRS) DE Designation(s)
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13 46 57.12 +06 21 01.3 HR 5183 = HD 120066
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 42 357 Radial velocities and S-index values
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See also:
J/other/Sci/330.653 : Detected planets in the Eta-Earth Survey (Howard+, 2010)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 F10.4 d BJD [10463.1705/18675.7767] Time of observation,
BJD-2440000
12- 17 F6.2 m/s RV [-67.93/61.01] Radial velocity
19- 22 F4.2 m/s e_RV [1.07/9.03] Uncertainty in RV
24- 28 A5 --- Inst Instrument flag
30- 30 A1 --- f_Inst [a] Flag indicating pre-upgrade HIRES measurement
32- 36 F5.3 --- SHK [0.114/0.17]? Ca II H&K line emission indicator
(1)
38- 42 F5.3 --- e_SHK [0.002/0.03]? Uncertainty in SHK (1)
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Note (1): Note that the SHK values for each instrument do not have the same
zero-point. Pre- and post-upgrade HIRES S-values should be treated
independently.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 17-Dec-2019