J/A+A/640/A73 pi Men radial velocity curves (De Rosa+, 2020)
A significant mutual inclination between the planets within the π Mensae
system.
De Rosa R.J., Dawson R., Nielsen E.L.
<Astron. Astrophys. 640, A73 (2020)>
=2020A&A...640A..73D 2020A&A...640A..73D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Radial velocities
Keywords: astrometry -
planets and satellites: dynamical evolution and stability -
stars individual: pi Mensae
Abstract:
Measuring the geometry of multi-planet extrasolar systems can provide
insight into their dynamical history and the processes of planetary
formation. These types of measurements are challenging for systems
that are detected through indirect techniques such as radial velocity
and transit, having only been measured for a handful of systems to
date.
We aim to place constraints on the orbital geometry of the outer
planet in the π Mensae system, a G0V star at a distance of 18.3pc that
is host to a wide-orbit super-Jovian (Msini=10.02±0.15MJup) with a
5.7-year period and an inner transiting super-Earth
(M=4.82±0.85M⊕) with a 6.3-d period.
The reflex motion induced by the outer planet on the Mensae star
causes a significant motion of the photocenter of the system on the
sky plane over the course of the 5.7-year orbital period of the
planet. We combined astrometric measurements from the Hipparcos and
Gaia satellites with a precisely determined spectroscopic orbit in an
attempt to measure this reflex motion, and in turn we constrained the
inclination of the orbital plane of the outer planet.
We measure an inclination of ib=49.9+5.3-4.5deg for the orbital
plane of π Mensae b, leading to a direct measurement of its mass of
13:01+1.03-0.95M{Jup}. We find a significant mutual inclination
between the orbital planes of the two planets, with a 95% credible
interval for imut of between 34.5° and 140.6° after
accounting for the unknown position angle of the orbit of π Mensae
c, strongly excluding a co-planar scenario for the two planets within
this system. All orbits are stable in the present-day configuration,
and secular oscillations of planet c's eccentricity are quenched by
general relativistic precession. Planet c may have undergone high
eccentricity tidal migration triggered by Kozai-Lidov cycles, but
dynamical histories involving disk migration or in situ formation are
not ruled out. Nonetheless, this system provides the first piece of
direct evidence that giant planets with large mutual inclinations have
a role to play in the origins and evolution of some super-Earth
systems.
Description:
We tabulate the measurements used in our joint astrometric and radial
velocity analysis of the orbit of the outer giant planet within the pi
Mensae system. The radial velocities were obtained from the literature
and public archives. The astrometric measurements by the Hipparcos
satellite were from the DVD containing the intermediate astrometric
data for all stars observed by Hipparcos (van Leeuwen 2007). The
predicted timings and orientations of the Gaia observations were
obtained from the gost utility (https://gaia.esac.esa.int/gost/) on 7
January 2020.
The tables contain radial velocities of the pi Mensae star,
astrometric measurements of the photocenter made by Hipparcos, and
predicted timings and orientations of the Gaia observations used to
construct the Gaia DR2 catalogue.
Objects:
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RA (2000) DE Designation(s)
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05 37 09.89 -80 28 08.8 pi Men = HD 39091
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table5.dat 33 359 Radial velocities of pi Mensae
table6.dat 40 137 Hipparcos astrometric measurements of pi Mensae
table7.dat 42 26 Predicted Gaia scan timings and orientations
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See also:
J/A+A/619/L10 : pi Men radial velocity curves (Gandolfi+, 2018)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.4 d BJD Barycentric Julian date (BJD-2450000)
11- 18 F8.5 km/s RV Radial velocity
20- 26 F7.5 km/s e_RV Radial velocity error
28- 33 A6 --- Inst Instrument used to measure radial velocity
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 6 F6.3 yr Year Year (Year-1991.25)
8- 13 F6.3 --- parf Parallax factor
15- 21 F7.4 --- cosp Cosine of the scan angle
23- 29 F7.4 --- sinp Sine of the scan angle
31- 35 F5.2 mas res Abscissa residuals
37- 40 F4.2 mas e_res Abscissa residual uncertainty
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 F6.3 yr Year Year (Year-1991.25)
8- 15 F8.2 d MJD Modified Julian date
17- 24 F8.5 --- parf Parallax factor
26- 33 F8.5 --- sint Sine of the scan position angle
35- 42 F8.5 --- cost Cosine of the scan position angle
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Acknowledgements:
Robert De Rosa, rderosa(at)eso.org
(End) Patricia Vannier [CDS] 04-Aug-2020