J/AJ/164/104 NEID and HIRES radial velocity of TOI-1478 (Rice+, 2022)
A Tendency Toward Alignment in Single-star Warm-Jupiter Systems.
Rice M., Wang S., Wang X.-Y., Stefansson G., Isaacson H., Howard A.W.,
Logsdon S.E., Schweiker H., Dai F., Brinkman C., Giacalone S., Holcomb R.
<Astron. J., 164, 104 (2022)>
=2022AJ....164..104R 2022AJ....164..104R
ADC_Keywords: Exoplanets; Stars, high-velocity; Spectra, optical; Stars, ages;
Radial velocities; Effective temperatures
Keywords: Planetary alignment ; Exoplanet dynamics ; Exoplanet evolution ;
Star-planet interactions ; Exoplanets ; Planetary theory ;
Exoplanet systems ; Exoplanet astronomy ; Planetary dynamics ;
Hot Jupiters ; Protoplanetary disks
Abstract:
The distribution of spin-orbit angles for systems with
wide-separation, tidally detached exoplanets offers a unique
constraint on the prevalence of dynamically violent planetary
evolution histories. Tidally detached planets provide a relatively
unbiased view of the primordial stellar obliquity distribution, as
they cannot tidally realign within the system lifetime. We present the
third result from our Stellar Obliquities in Long-period Exoplanet
Systems (SOLES) survey: a measurement of the Rossiter-McLaughlin
effect across two transits of the tidally detached warm Jupiter
TOI-1478b with the WIYN/NEID and Keck/HIRES spectrographs, revealing a
sky-projected spin-orbit angle λ=6.2-5.5+5.9deg. Combining
this new measurement with the full set of archival obliquity
measurements, including two previous constraints from the SOLES
survey, we demonstrate that, in single-star systems, tidally detached
warm Jupiters are preferentially more aligned than closer-orbiting hot
Jupiters. This finding has two key implications: (1) planets in
single-star systems tend to form within aligned protoplanetary disks,
and (2) warm Jupiters form more quiescently than hot Jupiters, which,
in single-star systems, are likely perturbed into a misaligned state
through planet-planet interactions in the post-disk-dispersal phase.
We also find that lower-mass Saturns span a wide range of spin-orbit
angles, suggesting a prevalence of planet-planet scattering and/or
secular mechanisms in these systems.
Description:
We obtained 20 radial velocity measurements of TOI-1478 with the
high-resolution mode of the NEID spectrograph (R∼110000) from
03:18-09:49 UT on 2022 February 5. Exposure times were fixed at 1000s.
We obtained 39 radial velocity measurements of TOI-1478 with the High
Resolution Echelle Spectrometer (HIRES) spectrograph from 06:00-13:00
UT on 2022 February 15. The median exposure time was 592s, with 100k
exposure meter counts per spectrum.(R=60000)
To calibrate our observations and extract precise stellar parameters,
we also obtained a 21minute iodine-free HIRES template exposure of
TOI-1478 using the B3 decker (14.0x0.574", R=72000) on UT 2022
February 21.
Objects:
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RA (2000) DE Designation(s)
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08 25 44.11 -13 33 35.4 TOI-1478 = TOI-1478
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 26 20 NEID radial velocities for the TOI-1478 system
table2.dat 38 39 HIRES radial velocities for the TOI-1478 system
table4.dat 142 91 Parameters for the population of warm Jupiters,
hot Jupiters, and Saturns studied in this work
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See also:
B/simbad : Simbad objects catalogue (M.Wenger 2000)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005)
J/A+A/517/L1 : Radial velocities of WASP-8b planet (Queloz+, 2010)
J/ApJ/757/18 : Radial velocities 16 hot Jupiter host stars (Albrecht+, 2012)
J/A+A/571/A37 : KOI-1257 photometric and velocimetric data (Santerne+, 2014)
J/A+A/579/A136 : HAT-P-36 and WASP-11/HAT-P-10 light curves (Mancini+, 2015)
J/ApJ/808/16 : The Cannon; new approach to determine abundances (Ness+, 2015)
J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016)
J/AJ/155/225 : M dwarf stars rotational broadening measures (Kesseli+, 2018)
J/ApJ/898/119 : Keck HIRES spectra analyzed with The Cannon (Rice+, 2020)
J/AJ/160/214 : 130 Stellar ages & planet orbital properties (Safsten+, 2020)
J/ApJ/911/138 : Low-mass pre-main-sequence stars Taurus-Auriga (Nofi+, 2021)
J/AJ/161/194 : LCs & RVs 5 exoplanets discovered by TESS (Rodriguez+, 2021)
J/AJ/164/26 : Hot Jupiters isochrone analyse & stellar model (Hamer+, 2022)
J/AJ/163/247 : HIRES, PEPSI & TRES radial velocity V1298Tau (Johnson+, 2022)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 14 F14.6 d BJD [2459615/2459616] Barycentric Julian Date at TDB
16- 22 F7.1 m/s RVel [20783/20806] Radial Velocity
24- 26 F3.1 m/s e_RVel [3/6] Uncertainty in RVel
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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- 14 F14.6 d BJD [2459625/2459627] Barycentric Julian Date at TDB
16- 21 F6.2 m/s RVel [-15.6/10.2] Radial Velocity
23- 26 F4.2 m/s e_RVel [1/2] Uncertainty in RVel
28- 32 F5.3 --- SHK [0.14/0.16] S-index
34- 38 F5.3 --- e_SHK [0.001] Uncertainty in SHK
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Type Population type; Warm Jupiter, hot Jupiter or
Saturn
15- 23 A9 --- Name System identifier
25- 25 A1 --- Planet Planet observed
27- 27 A1 --- l_Mass [<] Limit flag on Mass
29- 34 F6.3 Mjup Mass [0.21/12.9] Planet mass
36- 40 F5.3 Mjup E_Mass [0.03/4]? Upper uncertainty on Mass
42- 46 F5.3 Mjup e_Mass [0.01/2]? Lower (or symmetric) uncertainty on Mass
48- 53 F6.3 --- a/Rad* [2.27/24.2] Ratio, semi-major axis/stellar radius
55- 58 F4.2 --- E_a/Rad* [0.1/2]? Upper uncertainty on a/Rad*
60- 64 F5.3 --- e_a/Rad* [0.07/4]? Lower (or symmetric) uncertainty on
a/Rad*
66- 66 A1 --- l_e [<] Limit flag on e
68- 73 F6.4 --- e [0/0.68]? Orbital eccentricity of planet
75- 80 F6.4 --- E_e [0.003/0.3]? Upper uncertainty on e
82- 87 F6.4 --- e_e [0.001/0.2]? Lower (or symmetric) uncertainty on e
89- 89 A1 --- l_Age [] Limit flag on Age
91- 96 F6.3 Gyr Age [0.01/12]? System Age, Gyr
98-102 F5.2 Gyr E_Age [0.03/10]? Upper uncertainty on Age
104-108 F5.3 Gyr e_Age [0.002/7]? Lower (or symmetric) uncertainty on Age
110-113 I4 K Teff [4145/9600] Stellar effective temperature
115-117 I3 K E_Teff [50/630]? Upper uncertainty on Teff
119-121 I3 K e_Teff [21/820] Lower (or symmetric) uncertainty on Teff
123-129 F7.2 deg lambda [-155/165] sky-projected spin-orbit angle
131-135 F5.2 deg E_lambda [0.2/41]? Upper uncertainty on lambda
137-142 F6.2 deg e_lambda [0.08/45] Lower (or symmetric) uncertainty on
lambda
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 18-Nov-2022