J/ApJ/757/18 Radial velocities for 16 hot Jupiter host stars (Albrecht+, 2012)
Obliquities of hot Jupiter host stars: evidence for tidal interactions and
primordial misalignments.
Albrecht S., Winn J.N., Johnson J.A., Howard A.W., Marcy G.W., Butler R.P.,
Arriagada P., Crane J.D., Shectman S.A., Thompson I.B., Hirano T.,
Bakos G., Hartman J.D.
<Astrophys. J., 757, 18 (2012)>
=2012ApJ...757...18A 2012ApJ...757...18A
ADC_Keywords: Radial velocities ; Stars, double and multiple ; Planets
Keywords: planetary systems; planets and satellites: formation;
planet-star interactions; stars: rotation; techniques: spectroscopic
Abstract:
We provide evidence that the obliquities of stars with close-in giant
planets were initially nearly random, and that the low obliquities
that are often observed are a consequence of star-planet tidal
interactions. The evidence is based on 14 new measurements of the
Rossiter-McLaughlin effect (for the systems HAT-P-6, HAT-P-7,
HAT-P-16, HAT-P-24, HAT-P-32, HAT-P-34, WASP-12, WASP-16, WASP-18,
WASP-19, WASP-26, WASP-31, Gl 436, and Kepler-8), as well as a
critical review of previous observations. The low-obliquity
(well-aligned) systems are those for which the expected tidal
timescale is short, and likewise the high-obliquity (misaligned and
retrograde) systems are those for which the expected timescale is
long. At face value, this finding indicates that the origin of hot
Jupiters involves dynamical interactions like planet-planet
interactions or the Kozai effect that tilt their orbits rather than
inspiraling due to interaction with a protoplanetary disk. We discuss
the status of this hypothesis and the observations that are needed for
a more definitive conclusion.
Description:
14 new observations presented in this paper were conducted with the
Keck I telescope and its High Resolution Spectrograph (HIRES, for
northern objects, and with the Magellan II (Clay) 6.5m telescope and
the Planet Finder Spectrograph (PFS) for southern objects. Table 1 is
a log of the observations (spanning from 2010 Apr 24/25 for Gl 436 to
2012 Mar 12/13 for WASP-31).
To derive the relative radial velocities (RVs) we compared the spectra
observed through the iodine cell with the stellar template spectrum
multiplied by an iodine template spectrum. The velocity shift of the
stellar template and the parameters of the point-spread function (PSF)
of the spectrograph are free parameters in this comparison. The
velocity shift of the template that gives the best fit to an observed
spectrum represents the measured relative RV for that observation. In
particular, we used codes based on those of Butler et al.
(1996PASP..108..500B 1996PASP..108..500B).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 44 16 Observation log
table2.dat 46 718 Relative radial velocity measurements
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See also:
J/A+A/563/A22 : Radial velocities of 3 new hot Jupiters (Moutou+, 2014)
J/A+A/557/A30 : Transits of HAT-P-16 and WASP-21 (Ciceri+, 2013)
J/A+A/553/A49 : WASP-19b secondary eclipses (Abe+, 2013)
J/A+A/552/A2 : WASP-19b light curves (Lendl+, 2013)
J/A+A/551/A108 : Multi-site obs. of WASP-12 b transit (Maciejewski+, 2013)
J/MNRAS/436/2 : Light curves of WASP-19 transit events (Mancini+, 2013)
J/MNRAS/434/1300 : WASP-15 and WASP-16 light curves (Southworth+, 2013)
J/MNRAS/428/3164 : Spectroscopy of WASP planet host stars (Doyle+, 2013)
J/A+A/539/A102 : HD 209458 and HD 189733 theoretical spectra (Hayek+, 2012)
J/ApJ/755/9 : Spitzer/IRAC light curves of GJ 436 system (Stevenson+, 2012)
J/ApJ/745/77 : Photochemical model for planet WASP-12b (Kopparapu+, 2012)
J/MNRAS/426/739 : RVs for seven transiting hot Jupiters (Hellier+, 2012)
J/MNRAS/423/1503 : RV curves of WASP-16, 25 and 31 (Brown+, 2012)
J/AJ/144/19 : Follow-up phot. for HAT-P-34 through HAT-P-37 (Bakos+, 2012)
J/AJ/141/179 : Transits of TrES-4b, HAT-P-3b and WASP-12b (Chan+, 2011)
J/A+A/534/A16 : WASP-22 & WASP-26 photometry and velocities (Anderson+, 2011)
J/A+A/531/A60 : WASP-31b photometry and radial velocities (Anderson+, 2011)
J/A+A/528/A65 : WASP-12b transits (Maciejewski+, 2011)
J/A+A/527/L11 : HAT-P-6 radial velocity curve (Hebrard+, 2011)
J/ApJS/197/8 : Kepler's cand. multiple transiting planets (Lissauer+, 2011)
J/ApJ/742/59 : HAT-P-32 and HAT-P-33 follow-up (Hartman+, 2011)
J/ApJ/727/125 : Two secondary eclipses of WASP-12b with Spitzer (Campo+, 2011)
J/PASP/123/412 : Exoplanet Orbit Database (Wright+, 2011)
J/ApJ/725/2017 : Sloan i-band light curve of HAT-P-24 (Kipping+, 2010)
J/ApJ/720/1118 : i-band photometry of HAT-P-16 (Buchhave+, 2010)
J/ApJ/720/872 : A spectropolarimetric analysis of WASP-12 (Fossati+, 2010)
J/A+A/524/A25 : Radial Velocities on 6 exoplanet host stars (Triaud+, 2010)
J/A+A/520/A56 : WASP-26b RV and photometric data (Smalley+, 2010)
J/A+A/513/L3 : H-band thermal emission of WASP-19b (Anderson+, 2010)
J/ApJ/707/167 : Transiting planetary system WASP-18 (Southworth+, 2009)
J/ApJ/703/L99 : Outlandish orbit of HAT-P-7b (Winn+, 2009)
http://www.astro.keele.ac.uk/jkt/tepcat/ : Cat. of transiting planet properties
http://www.physics.mcmaster.ca/~rheller/ : 75 planets with published
measurements of the Rossiter-McLaughlin effect
http://exoplanets.org/ : Exoplanet orbit database
http://exoplanet.eu/ : The extrasolar planets encyclopaedia
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 System name
11- 21 A11 "YYYY/MMM/DD" Date First observation date
22 A1 --- --- [-]
23- 24 I2 --- Day ? Day of the second observation date
26- 44 A19 --- Source Instrument for the observation or
reference for the reanalysis (1)
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Note (1): HAT-P-2 and HD 209458 added by CDS to match sources in table 2.
See sections 4.15 and 4.17 for further details about these stars
measurements.
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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 System name
11- 23 F13.5 d BJD Barycentric Julian Date
25- 32 F8.2 m/s RVel [-1660.3/1209.9] Radial velocity
33 A1 --- f_RVel [*] Flag on RVel (1)
35- 40 F6.2 m/s e_RVel [-40.9/23.1] Internally estimated uncertainty
in RVel (2)
42- 46 A5 --- Inst Spectrograph used in observation (3)
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Note (1):
* = RVel not used for the final results in the paper.
Note (2): Without any jitter term. See Section 3.6.
Note (3): Instrument as follows:
HIRES = Keck I 10m telescope and High Resolution Spectrograph.
PFS = Magellan II (Clay) 6.5m telescope and Planet Finder Spectrograph.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 20-May-2014