J/AJ/157/55 RVs and light curves for HATS-60-HATS-69 (Hartman+, 2019)
HATS-60b-HATS-69b: 10 transiting planets from HATSouth.
Hartman J.D., Bakos G.A., Bayliss D., Bento J., Bhatti W., Brahm R.,
Csubry Z., Espinoza N., Henning T., Jordan A., Mancini L., Penev K.,
Rabus M., Sarkis P., Suc V., de Val-Borro M., Zhou G., Addison B.,
Arriagada P., Butler R.P., Crane J., Durkan S., Shectman S., Tan T.G.,
Thompson I., Tinney C.G., Wright D.J., Lazar J., Papp I., Sari P.
<Astron. J., 157, 55 (2019)>
=2019AJ....157...55H 2019AJ....157...55H (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs ; Stars, double and multiple ; Radial velocities ;
Photometry ; Optical ; Exoplanets
Keywords: stars: individual - techniques: photometric -
techniques: spectroscopic
Abstract:
We report the discovery of 10 transiting extrasolar planets by the
HATSouth survey. The planets range in mass from the super-Neptune HATS-62b,
with Mp<0.179 MJ, to the super-Jupiter HATS-66b, with Mp=5.33 MJ,
and in size from the Saturn HATS-69b, with Rp=0.94 RJ, to the inflated
Jupiter HATS-67b, with Rp=1.69 RJ. The planets have orbital periods
between 1.6092 days (HATS-67b) and 7.8180 days (HATS-61b). The hosts
are dwarf stars with masses ranging from 0.89 M☉ (HATS-69) to
1.56 M☉ (HATS-64) and have apparent magnitudes between
V=12.276±0.020 mag (HATS-68) and V=14.095±0.030 mag (HATS-66). The
super-Neptune HATS-62b is the least massive planet discovered to date
with a radius larger than Jupiter. Based largely on the Gaia DR2 distances
and broadband photometry, we identify three systems (HATS-62, HATS-64,
and HATS-65) as having possible unresolved binary star companions. We
discuss in detail our methods for incorporating the Gaia DR2 observations
into our modeling of the system parameters and into our blend analysis
procedures.
Description:
Spectroscopic observations were carried out to confirm and characterize
each of the transiting planet systems. The facilities used include FEROS
on the MPG 2.2 m (all 10 targets, 138 observations total; Kaufer & Pasquini
1998SPIE.3355..844K 1998SPIE.3355..844K), Coralie on the Euler 1.2 m (5 targets, 28 observations
total; Queloz et al. 2001Msngr.105....1Q 2001Msngr.105....1Q), HARPS on the ESO 3.6 m
(4 targets, 27 observations total; Mayor et al. 2003Msngr.114...20M 2003Msngr.114...20M), WiFeS
on the ANU 2.3 m (5 targets, 18 observations total; Dopita et al.
2007Ap&SS.310..255D 2007Ap&SS.310..255D), PFS on the Magellan 6.5 m (1 target, 10 observations;
Crane et al. 2010SPIE.7735E..53C 2010SPIE.7735E..53C), UVES on the VLT UT2 8 m (3 targets,
3 observations; Dekker et al. 2000SPIE.4008..534D 2000SPIE.4008..534D), and CYCLOPS on the
AAT 3.9 m (1 target, 3 observations; Horton et al. 2012SPIE.8446E..3AH).
Follow-up higher-precision ground-based photometric transits
observations were obtained for all 10 systems. The facilities used for
this purpose include the Chilean-Hungarian Automated Telescope (CHAT) 0.7 m
telescope at Las Campanas Observatory, Chile (six transits of four targets;
A. Jordan et al. 2018 in preparation); 1 m telescopes from the Las Cumbres
Observatory (LCO) network, including units at McDonald Observatory (MCD)
in Texas, at Cerro Telolo Inter-American Observatory (CTIO) in Chile,
at Siding Spring Observatory (SSO) in Australia, and at the South African
Astronomical Observatory (SAAO) in South Africa (21 transits of six targets
altogether; Brown et al. 2013PASP..125.1031B 2013PASP..125.1031B); the 2 m Faulkes Telescope
South (FTS) operated at SSO by LCO (one transit of one target); the SMARTS
CTIO 0.9 m telescope (two transits of one target; Subasavage et al.
2010SPIE.7737E..1CS); the 0.3 m Perth Exoplanet Survey Telescope in
Australia (PEST; five transits of four targets); the Danish 1.54 m
telescope at La Silla Observatory in Chile (one transit of one target;
Andersen et al. 1995Msngr..79...12A 1995Msngr..79...12A); and the Swope 1 m telescope at
Las Campanas Observatory in Chile (one transit of one target).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 35 10 Generalized Lomb-Scargle (GLS) search for
periodic signals in HATSouth light curves
table3.dat 57 10 Box-fitting least-squares (BLS) search for
additional transit signals in HATSouth light
curves
table5.dat 60 190 Relative radial velocities and bisector spans
for HATS-60-HATS-69
table6.dat 74 153037 Light curve data for HATS-60-HATS-69
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See also:
J/A+A/580/A63 : HATS-13b and HATS-14b light and RV curves (Mancini+, 2015)
J/AJ/155/79 : RV & light curves data for 4 G-type dwarf stars
(Henning+, 2018)
J/AJ/155/112 : Radial velocities & light curves for HATS-43-HATS-46
(Brahm+, 2018)
J/AJ/156/216 : Differential photometry & RVs of HATS-59 (Sarkis+, 2018)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- ID System identifier (HATS-60-HATS-69)
9- 19 F11.8 d Per(GLS) [0.0127448/28.54] Peak period
21- 25 F5.2 [-] logFAP [-3.7/-0.02] Log10 of false-alarm probability
27- 30 F4.2 mmag Amp [0.32/1.1] Semi-amplitude
32- 35 F4.2 mmag E_Amp [0.43/1.6] Semi-amplitude 95% upper limit
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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- 7 A7 --- ID System identifier (HATS-60-HATS-69)
9- 19 F11.8 d Per(BLS) [0.11051/88.8988] Peak period
21- 24 F4.2 mmag Depth [0.74/5.5] Transit depth
26- 33 F8.5 d Dur [0.00309/10.3] Transit duration
35- 37 F3.1 --- S/N [5.3/7.5] Signal-to-noise ratio
39- 47 F9.7 d Per [1.60917/7.81796] Orbital period (from
Tables 16-18 of this paper)
49- 57 F9.7 d e_Per [1.6e-06/3.2e-05] Uncertainty in Per (from
Tables 16-18 of this paper)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- ID System identifier (HATS-60-HATS-69)
9- 18 F10.5 d BJD [6056.30075/8041.87936] Barycentric Julian Date
(BJD-2450000)
20- 26 F7.2 m/s RV [-730.32/764.58]? Radial velocity, arbitrary
zeropoint (1)
28- 33 F6.2 m/s e_RV [7.9/107.5]? Uncertainty in RV (2)
35- 40 F6.1 m/s BS [-727/854]? Spectral line bisector span
42- 46 F5.1 m/s e_BS [11/215.4]? Uncertainty in BS
48- 52 F5.3 --- Phase [0.073/0.997] Phase
54- 60 A7 --- Inst Instrument (3)
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Note (1): The zero-point of these velocities is arbitrary. An overall offset
γrel fitted independently to the velocities from each instrument has
been subtracted.
Note (2): Internal errors excluding the component of astrophysical jitter
considered in Section 3.2.
Note (3): Instrument as follows:
CYCLOPS = CYCLOPS on the AAT 3.9m;
Coralie = Coralie on the Euler 1.2m;
FEROS = FEROS on the MPG 2.2m;
HARPS = HARPS on the ESO 3.6m;
PFS = PFS on the Magellan 6.5m.
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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- 7 A7 --- ID System identifier (HATS-60-HATS-69)
9- 19 F11.5 d BJD [55091.47377/58079.77631] Barycentric Julian Date
(BJD-2400000; UTC) (1)
21- 28 F8.5 mag mag [-0.06916/0.0491] Out-of-transit subtracted
magnitude (2)
30- 36 F7.5 mag e_mag [0.0004/0.03592] Uncertainty in mag
38- 45 F8.5 mag omag [-0.0152/14.3424]? Raw magnitude in Filt (3)
47- 48 A2 --- Filt [R Rc griz] Filter used in the observation
50- 74 A25 --- Inst Instrument used in the observation
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Note (1): Barycentric Julian Date is computed directly from the UTC time
without correction for leap seconds.
Note (2): The out-of-transit level has been subtracted. For observations made
with the HATSouth instruments (identified by "HS" in the "Inst" column) these
magnitudes have been corrected for trends using the external parameter
decorrelation (EPD) and trend filtering algorithm (TFA) procedures applied
prior to fitting the transit model. This procedure may lead to an artificial
dilution in the transit depths. The blend factors for the HATSouth light
curves are listed in Table 14. For observations made with follow-up
instruments (anything other than "HS" in the "Inst" column), the magnitudes
have been corrected for a quadratic trend in time, and for variations
correlated with up to three PSF shape parameters, fit simultaneously with the
transit.
Note (3): Raw magnitude values without correction for the quadratic trend in
time, or for trends correlated with the seeing. These are only reported for
the follow-up observations.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 16-May-2019