J/AJ/165/164 Tull RVels, rotation periods and Inclinations (Bowler+, 2023)
Rotation Periods, Inclinations, and Obliquities of Cool Stars Hosting Directly
Imaged Substellar Companions; Spin-Orbit Misalignments Are Common.
Bowler B.P., Tran Q.H., Zhang Z., Morgan M., Ashok K.B., Blunt S.,
Bryan M.L., Evans A.E., Franson K., Huber D., Nagpal V., Wu Y.-L.,
Zhou Y.
<Astron. J., 165, 164 (2023)>
=2023AJ....165..164B 2023AJ....165..164B
ADC_Keywords: Stars, brown dwarf; Exoplanets; Spectra, optical;
Spectra, infrared; Radial velocities; Rotational velocities
Keywords: Brown dwarfs ; Extrasolar gaseous giant planets ; Planet
formation ; Stellar rotation
Abstract:
The orientation between a star's spin axis and a planet's orbital
plane provides valuable information about the system's formation and
dynamical history. For non-transiting planets at wide separations,
true stellar obliquities are challenging to measure, but lower limits
on spin-orbit orientations can be determined from the difference
between the inclination of the star's rotational axis and the
companion's orbital plane (Δi). We present results of a uniform
analysis of rotation periods, stellar inclinations, and obliquities of
cool stars (SpT≳F5) hosting directly imaged planets and brown dwarf
companions. As part of this effort, we have acquired new vsini* values
for 22 host stars with the high-resolution Tull spectrograph at the
Harlan J. Smith telescope. Altogether our sample contains 62 host
stars with rotation periods, most of which are newly measured using
light curves from the Transiting Exoplanet Survey Satellite. Among
these, 53 stars have inclinations determined from projected rotational
and equatorial velocities, and 21 stars predominantly hosting brown
dwarfs have constraints on Δi. Eleven of these (52-11+10% of
the sample) are likely misaligned, while the remaining 10 host stars
are consistent with spin- orbit alignment. As an ensemble, the minimum
obliquity distribution between 10 and 250au is more consistent with a
mixture of isotropic and aligned systems than either extreme scenario
alone-pointing to direct cloud collapse, formation within disks
bearing primordial alignments and misalignments, or architectures
processed by dynamical evolution. This contrasts with stars hosting
directly imaged planets, which show a preference for low obliquities.
These results reinforce an emerging distinction between the orbits of
long- period brown dwarfs and giant planets in terms of their stellar
obliquities and orbital eccentricities.
Description:
High-resolution optical spectra for 22 targets from our broader sample
were obtained with the Tull Coude Spectrograph at McDonald
Observatory's 2.7m Harlan J. Smith telescope between 2019 March and
2022 February. The 1.2" slit and E2 grating were used with the TS23
setup for all observations, which resulted in a resolving power of
R∼60000. Fifty-six echelle orders were simultaneously captured with
the TK3 Tektronix CCD from 3870-10500Å in (largely nonoverlapping)
segments ranging from 60-200Å.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 81 45 Tull Spectrograph radial velocities and projected
rotational velocities
table2.dat 134 63 Host star properties
table3.dat 129 55 Stellar inclinations and minimum obliquities
table4.dat 39 308 Adopted projected rotational velocities
refs2.dat 73 98 References used for table2
refs4.dat 71 89 References used for table4
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See also:
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Name Name
25- 28 I4 yr Obs.Y [2019/2022] Observation year, UT
30- 31 I2 "month" Obs.M Observation date, UT, month
33- 34 I2 d Obs.D Observation date, UT, day
36- 39 I4 s Texp [45/1200] Exposure time
41- 45 F5.1 m/s RVel [-27.7/35]? Radial Velocity
47- 49 F3.1 m/s e_RVel [0.2/4]? Uncertainty in RVel
51- 55 F5.1 km/s vsini [3.1/183] Projected rotational velocity
57- 60 F4.1 km/s e_vsini [0.2/35] Uncertainty in vsini
62- 70 A9 --- Std Standard or Model
72- 75 A4 --- SpT Spectral type
77- 81 I5 K Teff [3400/10800]? Effevtive temperature
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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- 27 A27 --- Name Name
29- 29 A1 --- f_Name Flag on Name (1)
31- 40 A10 --- SpT1 Host spectral type
42- 48 A7 --- SpT2 Companion spectral type
50- 54 A5 --- Disc Discovery Reference
56- 59 I4 au Sep [10/9708]? Separation
61- 71 A11 --- TESS TESS Sectors analyzed
73- 73 A1 --- f_TESS Flag on TESS (2)
75- 81 F7.4 d Prot [0.08/44] Rotational period, days
83- 88 F6.4 d e_Prot [0.0008/7] Uncertainty in Prot (3)
90- 91 A2 --- r_Prot Reference for Prot
93- 97 F5.3 Rsun Rstar [0.164/1.7] Host radius, solar units
99-103 F5.3 Rsun e_Rstar [0.005/0.2] Uncertainty in Rstar (4)
105-106 A2 --- r_Rstar Reference for Rstar
108-113 F6.3 km/s vsini [1.3/75]? Projected rotational velocity
115-119 F5.2 km/s e_vsini [0.05/11]? Uncertainty in vsini
121-127 F7.3 km/s veq [0.648/140] Equatorial rotational velocities
129-134 F6.2 km/s e_veq [0.11/30] Uncertainty in veq
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Note (1): c=GJ3305AB is a wide binary to the exoplanet host 51Eri. We
include the light curve analysis and inclination constraint in this
study for completeness, but do not count this system itself as a
substellar host.
Note (2): TESS sectors for L 34-26: 3; 4; 6; 7; 10-13; 27; 30; 33; 34; 36-39.
Note (3): Total period uncertainty including periodogram measurement
uncertainty and a term to account for potential differential rotation.
We adopt a Solar absolute shear of 0.072rad/d for all stars except
51Eri, for which we use 0.7rad/d based on trends from Reinhold &
Gizon, 2015, J/A+A/583/A65. See Section 4.2 for details.
Note (4): Stellar radius estimates from Stassun+, 2019, IV/38 have
been inflated by 7% based on a comparison in that study between the
original estimates and those from asteroseismology.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Name Name
25- 28 F4.1 deg i [3.7/90] Inclination with Maximum a
posteriori probability
30- 30 A1 --- f_i Flag on i (1)
32- 35 F4.1 deg medi [3.8/85.9] Median stellar inclination
37- 40 F4.1 deg E_medi [0.7/25.9] Upper uncertainty on medi
42- 45 F4.1 deg e_medi [0.9/21.2] Lower uncertainty on medi
47- 50 F4.1 deg b_i [1.1/78.1] Lower bound on i, 94.5%
Confidence Interval
52- 55 F4.1 deg B_i [6.6/90] Upper bound on i, 94.5%
Confidence Interval
57- 62 F6.2 deg medio [5.5/151]? med io
64- 68 F5.2 deg E_medio [0.16/23.1]? Upper uncertainty on medio
70- 74 F5.2 deg e_medio [0.16/19.8]? Lower uncertainty on medio
76- 76 A1 --- f_medio Flag on med-io (2)
78- 79 A2 --- r_medio Reference for med-io (3)
81- 85 F5.1 deg di [0/121]? Inclination difference with
Maximum a posteriori probability
87- 90 F4.1 deg meddi [9.2/97.3]? Median inclination difference
92- 95 F4.1 deg E_meddi [4.1/44.3]? Upper uncertainty on meddi
97-100 F4.1 deg e_meddi [9/82.7]? Lower uncertainty on meddi
102-105 F4.1 deg b_di [0/52.6]? Lower bound on di, 94.5%
Confidence Interval
107-111 F5.1 deg B_di [24/141]? Upper bound on di, 94.5%
Confidence Interval
113-117 F5.3 --- Prob [0.561/1]? Prob, di>10deg
119-129 A11 --- Mis? Misaligned? (4)
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Note (1): d = The stellar inclination of κAnd is taken from the
solar-metallicity model fits to oblateness measurements in Jones+,
2016ApJ...822L...3J 2016ApJ...822L...3J. The slightly asymmetric reported uncertainties
are averaged to 4deg for these purposes.
Note (2): c = Our normal approximation to reported io
Note (3): References as follows:
1 = Bowler+, 2020, J/AJ/159/63
2 = Bryan+, 2020AJ....159..181B 2020AJ....159..181B
3 = Dupuy+, 2022MNRAS.509.4411D 2022MNRAS.509.4411D
4 = Palma-Bifani+, 2022arXiv221101474P 2022arXiv221101474P
5 = Feng+, 2022, J/ApJS/262/21
6 = Stolker+, 2021AJ....162..286S 2021AJ....162..286S
7 = Pearce+, 2019, J/AJ/157/71
8 = Wang+, (in prep.)
9 = Maire+, 2020, J/A+A/639/A47
10 = Franson+, 2022AJ....163...50F 2022AJ....163...50F
11 = Brandt+, 2019AJ....158..140B 2019AJ....158..140B
12 = Wang+, 2020AJ....159..263W 2020AJ....159..263W
13 = Bryan+, 2016ApJ...827..100B 2016ApJ...827..100B
14 = Dupuy+, 2023MNRAS.519.1688D 2023MNRAS.519.1688D
Note (4): Systems are classified as misaligned ("Yes") if the
probability that di* values are greater than 10deg is ≥ 95% and the
MAP value of the di* posteriors is greater than 10deg. If
P(di>10deg)≥80% and the di MAP value is>10deg then the system is
classified as being "Likely" misaligned. If neither is satisfied, the
system is consistent with spin-orbit alignment ("No Evidence").
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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- 23 A23 --- Name Name
25- 30 F6.3 km/s vsini [0.1/95] Projected rotational velocity
32- 36 F5.2 km/s e_vsini [0.04/13]? Uncertainty in vsini
38- 39 I2 --- r_vsini [1/89] Reference for vsini
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Byte-by-byte Description of file: refs2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref [1/98] Reference code
4- 26 A23 --- Author Main author
28- 46 A19 --- BIB BIBcode
48- 63 A16 --- Cat. Catalog in VizieR
65- 73 A9 --- Note Additional note
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Byte-by-byte Description of file: refs4.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Ref [1/89] Reference code
5- 23 A19 --- BIB BIBcode
25- 40 A16 --- Cat. Catalog in VizieR
42- 71 A30 --- Note Additional Note
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 05-Sep-2023