J/AJ/155/203 HARPS-N RVs & activity indicators for Kepler-1655 (Haywood+, 2018)
An accurate mass determination for Kepler-1655b, a moderately irradiated world
with a significant volatile envelope.
Haywood R.D., Vanderburg A., Mortier A., Giles H.A.C., Lopez-Morales M.,
Lopez E.D., Malavolta L., Charbonneau D., Collier Cameron A.,
Coughlin J.L., Dressing C.D., Nava C., Latham D.W., Dumusque X., Lovis C.,
Molinari E., Pepe F., Sozzetti A., Udry S., Bouchy F., Johnson J.A.,
Mayor M., Micela G., Phillips D., Piotto G., Rice K., Sasselov D.,
Segransan D., Watson C., Affer L., Bonomo A.S., Buchhave L.A., Ciardi D.R.,
Fiorenzano A.F., Harutyunyan A.
<Astron. J., 155, 203-203 (2018)>
=2018AJ....155..203H 2018AJ....155..203H (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Radial velocities ; Spectroscopy ; Exoplanets
Keywords: stars: individual: Kepler-1655, KOI-280, KIC 4141376,
2MASS J19064546+3912428 - planets and satellites: detection -
planets and satellites: gaseous planets
Abstract:
We present the confirmation of a small, moderately irradiated
(F=155±7 F⊕) Neptune with a substantial gas envelope in
a P=11.8728787±0.0000085 day orbit about a quiet, Sun-like G0V star
Kepler-1655. Based on our analysis of the Kepler light curve, we
determined Kepler-1655b's radius to be 2.213±0.082 R⊕. We
acquired 95 high-resolution spectra with Telescopio Nazionale
Galileo/HARPS-N, enabling us to characterize the host star and determine
an accurate mass for Kepler-1655b of 5.0-2.8+3.1 M⊕ via
Gaussian-process regression. Our mass determination excludes an Earth-like
composition with 98% confidence. Kepler-1655b falls on the upper edge
of the evaporation valley, in the relatively sparsely occupied transition
region between rocky and gas-rich planets. It is therefore part of a
population of planets that we should actively seek to characterize further.
Description:
We observed Kepler-1655 with the HARPS-N instrument (Cosentino et al.
2012SPIE.8446E..1VC) on the Telescopio Nazionale Galileo (TNG) at La Palma,
Spain, over two seasons between 2015 June 7 and 2016 November 13. The
spectra were processed using the HARPS Data Reduction System (DRS;
Baranne et al. 1996A&AS..119..373B 1996A&AS..119..373B). The cross-correlation was performed
using a G2 spectral mask (Pepe et al. 2002Msngr.110....9P 2002Msngr.110....9P). The RV
measurements and the spectroscopic activity indicators are provided in
Table 4. The median, minimum, and maximum signal to noise ratio of the
HARPS spectra at the center of the spectral order number 50 are 51.8,
24.8, and 79.2, respectively.
Objects:
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RA (ICRS) DE Designation(s) (Period)
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19 06 45.46 +39 12 43.0 Kepler-1655 = KOI-280 (P=11.8728787)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 70 95 HARPS-N RV observations and spectroscopic
activity indicators, determined from the DRS
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See also:
J/A+A/552/A78 : Solar like stars radial velocities (Zechmeister+, 2013)
J/A+A/615/A175 : Solar system analogs with HARPS (Barbato+, 2018)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 14 F14.6 d BJD Barycentric Julian Date (UTC)
16- 24 F9.5 km/s RV [-40.64913/-40.62378] Radial velocity
26- 32 F7.5 km/s e_RV [0.00217/0.00819] 1σ uncertainty in RV
34- 40 F7.5 km/s FWHM [7.8364/7.89902] Full width at half maximum
42- 47 F6.3 --- Cont [29.016/29.389] Contrast of the cross-correlation
function (1)
49- 55 F7.5 km/s BIS [0.00964/0.04897] Line bisector of the
cross-correlation function (1)
57- 63 F7.4 [-] logRHK [-5.0566/-4.8835] Ca II activity indicator
logR'HK
65- 70 F6.4 [-] e_logRHK [0.0106/0.0775] 1σ uncertainty in logR(HK)
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Note (1): As defined in Queloz et al. 2001Msngr.105....1Q 2001Msngr.105....1Q.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 30-Nov-2018