J/A+A/677/A12 TOI-1416 radial velocities (Deeg+, 2023)
TOI-1416: A system with a super-Earth planet with a 1.07 d period.
Deeg H.J., Georgieva I.Y., Nowak G., Persson C.M., Cale B.L., Murgas F.,
Palle E., Godoy-Rivera D., Dai F., Ciardi D.R., Akana Murphy J.M.,
Beck P.G., Burke C.J., Cabrera J., Carleo I., Cochran W.D., Collins K.A.,
Csizmadia Sz., El Mufti M., Fridlund M., Fukui A., Gandolfi D., Garcia R.A.,
Guenther E.W., Guerra P., Grziwa S., Isaacson H., Isogai K., Jenkins J.M.,
Kabath P., Korth J., Lam K.W.F., Latham D.W., Luque R., Lund M.B.,
Livingston J.H., Mathis S., Mathur S., Narita N., Orell-Miquel J.,
Osborne H.L.M., Parviainen H., Plavchan P.P., Redfield S., Rodriguez D.R.,
Schwarz R.P., Seager S., Smith A.M.S., Van Eylen V., Van Zandt J.,
Winn J.N., Ziegler C.
<Astron. Astrophys. 677, A12 (2023)>
=2023A&A...677A..12D 2023A&A...677A..12D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, G-type ; Exoplanets ;
Radial velocities ; Optical
Keywords: planets and satellites: individual: TOI-1416 b -
planets and satellites: detection -
planets and satellites: terrestrial planets - planetary systems -
planets and satellites: composition - techniques: radial velocities
Abstract:
TOI-1416 (BD+42 2504, HIP 70705) is a V=10 late G- or early K-type
dwarf star. TESS detected transits in its Sectors 16, 23, and 50 with
a depth of about 455ppm and a period of 1.07 days. Radial velocities
(RVs) confirm the presence of the transiting planet TOI-1416 b, which
has a mass of 3.48±0.47M⊕ and a radius of
1.62±0.08R⊕, implying a slightly sub-Earth density of
4.50+0.90-0.83g/cm3. The RV data also further indicate a
tentative planet, c, with a period of 27.4 or 29.5 days, whose nature
cannot be verified due to strong suspicions of contamination by a
signal related to the Moon's synodic period of 29.53 days. The nearly
ultra-short-period planet TOI-1416 b is a typical representative of a
short-period and hot (Teq≃1570K) super-Earth-like planet. A planet
model of an interior of molten magma containing a significant fraction
of dissolved water provides a plausible explanation for its
composition, and its atmosphere could be suitable for transmission
spectroscopy with JWST. The position of TOI-1416 b within the
radius-period distribution corroborates the idea that planets with
periods of less than one day do not form any special group. It instead
implies that ultra-short-period planets belong to a continuous
distribution of super-Earth-like planets with periods ranging from the
shortest known ones up to ≃30 days; their period-radius distribution
is delimited against larger radii by the Neptune Desert and by the
period-radius valley that separates super-Earths from sub-Neptune
planets. In the abundance of small, short-periodic planets, a notable
plateau has emerged between periods of 0.6-1.4 days, which is
compatible with the low-eccentricity formation channel. For the
Neptune Desert, its lower limits required a revision due to the
increasing population of short-period planets; for periods shorter
then 2 days, we establish a radius of 1.6R⊕ and a mass of
0.028Mjup (corresponding to 8.9M⊕) as the desert's lower
limits. We also provide corresponding limits to the Neptune Desert
against the planets' insolation and effective temperatures.
Description:
The Radial Velocities of TOI-1416 from the five contributing
instruments are provided, which led to the confirmation of TOI-1416 b
as an exoplanet. For data from the HARPS-N instrument, a separate file
provides also absolute radial velocities and several activity
indicators, from both the SERVAL (as defined by Zechmeister et al.,
2018A&A...609A..12Z 2018A&A...609A..12Z) and the DRS (Cosentino et al.,
2014SPIE.9147E..8CC) pipelines.
Objects:
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RA (2000) DE Designation(s)
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14 27 41.766 +41 57 12.32 TOI-1416 = HIP 70705 = BD+42 2504
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
allrv.dat 35 205 Radial velocities of all instruments
hn.dat 235 96 RVs and activity indicators from HARPS-N
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Byte-by-byte Description of file: allrv.dat
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Bytes Format Units Label Explanations
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1- 13 F13.5 d BJD Exposure mid-time (in BJD_TDB)
16- 21 F6.2 m/s RV Barycentric corrected radial velocities (1)
23- 27 F5.2 m/s e_RV Error of RV
29- 35 A7 --- Inst Instrument performing the observation (2)
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Note (1): RV are relative radial velocities that were zeroed for each
instrument individually; small instrument-dependent offsets from a mean of
zero remain however. The mean RVs (in m/s) for each instrument are:
CA: 0.491, HN: 0.507, apf: 1.127, hires_j: -1.067, iSHELL: 0.278
Note (2): Instruments are as follows:
CA = CARMENES spectrograph at the 3.5 m telescope at Calar Alto
Observatory, Almeria, Spain
HN = HARPS-N spectrograph at the 3.58 m Telescopio Nazionale Galileo (TNG)
at the Roque de los Muchachos Observatory in La Palma, Spain
apf = Automatic Planet 69 Finder (APF) at Lick Observatory, USA
hires_j = High Resolution Echelle Spectrometer (HIRES) at the 10m Keck
Observatory, USA
iSHELL = iSHELL instrument at the NASA InfraRed Telescope Facility (IRTF) on
Mauna Kea, Hawaii, USA
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Byte-by-byte Description of file: hn.dat
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Bytes Format Units Label Explanations
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1- 13 F13.5 d BJD Exposure mid-time (in BJD_TDB)
15- 24 F10.6 m/s rvsSRV Barycentric corrected relative RV (1)
26- 33 F8.6 m/s e_rvsSRV Error of rvsSRV
35- 45 F11.6 m/s rvsDRS Barycentric corrected absolute RV (1)
47- 54 F8.6 m/s e_rvsDRS Error of rvsDRS
56- 64 F9.6 m/s ccf-bisDRS Bisector Inverse Slope (BIS) from CCFs
66- 73 F8.6 m/s e_ccf-bisDRS Error of ccfbisDRS
75- 82 F8.6 km/s ccf-fwhmDRS Full Width at Half Maximum of CCF
84- 92 F9.6 % ccf-ctrDRS CCF contrast
94-101 F8.6 --- smwDRS Mont-Wilson S-index
103-110 F8.6 --- e_smwDRS Error of smwDRS
112-118 F7.4 --- logrhkDRS Log(RHK) index
120-125 F6.4 --- e_logrhkDRS Error of logrhkDRS
127-136 F10.6 m/s crxSRV Chromatic RV index (CRX) (2)
138-146 F9.6 m/s e_crxSRV Error of crxSRV (2)
148-157 F10.6 m2/s2 dlwSRV Differential line width (dLW)
159-166 F8.6 m2/s2 e_dlwSRV Error of dlwSRV
168-175 F8.6 --- HalphaSRV H-alpha index
177-184 F8.6 --- e_HalphaSRV Error of HalphaSRV
186-193 F8.6 --- NAD1SRV Sodium Na∼D1 index
195-202 F8.6 --- e_NAD1SRV Error of NAD1SRV
204-211 F8.6 --- NAD2SRV Sodium Na∼D2 index
213-220 F8.6 --- e_NAD2SRV Error of NAD2SRV
222-226 F5.1 --- snr550nmDRS S/N at spectral order 46 (∼550nm)
228-235 F8.3 s ExpTime exposure time
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Note (1): Suffix DRS in labels refers to values obtained with the DRS
pipeline and SRV refers to the SERVAL pipeline
Note (2): The complete unit is m/s per neper (natural logarithmic ratio of
two wavelengths); see Zechmeister et al. (2018A&A...609A..12Z 2018A&A...609A..12Z)
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Acknowledgements:
Hans J. Deeg, hdeeg(at)iac.es,
Instituto de Astrofisica de Canarias, Spain
(End) Patricia Vannier [CDS] 14-Jul-2023