J/AJ/159/173 Photometry & RVs of 4 dwarfs hosting giant planets (Hartman+, 2020)
HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b: four warm giant planets transiting
K-dwarfs.
Hartman J.D., Jordan A., Bayliss D., Bakos G.A., Bento J., Bhatti W.,
Brahm R., Csubry Z., Espinoza N., Henning T., Mancini L., Penev K.,
Rabus M., Sarkis P., Suc V., de Val-Borro M., Zhou G., Crane J.D.,
Shectman S., Teske J.K., Wang S.X., Butler R.P., Lazar J., Papp I.,
Sari P., Anderson D.R., Hellier C., West R.G., Barkaoui K., Pozuelos F.J.,
Jehin E., Gillon M., Nielsen L., Lendl M., Udry S., Ricker G.R.,
Vanderspek R., Latham D.W., Seager S., Winn J.N., Christiansen J.,
Crossfield I.J.M., Henze C.E., Jenkins J.M., Smith J.C., Ting E.B.
<Astron. J., 159, 173 (2020)>
=2020AJ....159..173H 2020AJ....159..173H
ADC_Keywords: Stars, K-type; Exoplanets; Photometry, ugriz; Spectra, optical;
Radial velocities; Stars, ages; Stars, masses
Keywords: Exoplanets ; Extrasolar gas giants ; Hot Jupiters ; Transits
Abstract:
We report the discovery of four transiting giant planets around
K-dwarfs. The planets HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b have
masses of 0.369-0.021+0.031MJ, 0.243-0.030+0.022MJ,
0.353-0.027+0.038MJ, and 0.1254±0.0039MJ, respectively,
and radii of 1.117±0.014RJ, 0.800±0.015RJ,
0.765±0.013RJ, and 0.7224±0.0032RJ, respectively. The
planets orbit close to their host stars with orbital periods of
3.9228days, 3.1317days, 4.1480days, and 7.3279days, respectively. The
hosts are main-sequence K-dwarfs with masses of
0.674-0.012+0.016M☉, 0.7279±0.0066M☉,
0.7133±0.0075M☉, and 0.7311±0.0028, and with V-band
magnitudes of V=14.829±0.010, 14.35±0.11, 14.998±0.040 and
12.469±0.010. The super-Neptune HATS-72b (a.k.a. WASP-191b and
TOI294.01) was independently identified as a transiting planet
candidate by the HATSouth, WASP, and TESS surveys, and we present a
combined analysis of all of the data gathered by each of these
projects (and their follow-up programs). An exceptionally precise mass
is measured for HATS-72b thanks to high-precision radial velocity (RV)
measurements obtained with VLT/ESPRESSO, FEROS, HARPS, and
Magellan/PFS. We also incorporate TESS observations of the warm
Saturn-hosting systems HATS-47 (a.k.a. TOI1073.01), HATS-48A, and
HATS-49. HATS-47 was independently identified as a candidate by the
TESS team, while the other two systems were not previously identified
from the TESS data. The RV orbital variations are measured for these
systems using Magellan/PFS. HATS-48A has a resolved 5.4" neighbor in
Gaia DR2, which is a common-proper-motion binary star companion to
HATS-48A with a mass of 0.22M☉ and a current projected physical
separation of ∼1400au.
Description:
All four systems were observed by the NASA TESS mission as summarized
in Table1.
HATS-72 was observed by WASP-South over the period 2006-May to
2012-June, accumulating 24200 data points. WASP-South is an array of
eight cameras combining 200mm f/1.8lenses with 2kx2k CCDs and
observing with a broad, 400-700nm bandpass. It observed visible fields
with a typical cadence of 15minutes on each clear night. After
identification of a candidate 7.33day transit periodicity, HATS-72 was
placed on the WASP-South follow-up program in 2013-January. This led
to nine RVs being observed with the Euler/CORALIE spectrograph over
2013-2018, and the observation in 2018-July of a transit with
TRAPPIST-South, using an I+z filter.
The spectroscopic observations carried out to confirm and characterize
the four transiting planet systems presented here are summarized in
Table3. The facilities are: WiFeS on the Australian National
university (ANU) 2.3m, Planet Finder Spectrograph (PFS) on the
Magellan 6.5m, Fiber-fed Extended Range Optical Spectrograph (FEROS)
on the Max Planck Society (MPG) 2.2m, High Accuracy Radial velocity
Planet Searcher (HARPS) on the European Southern Observatory (ESO)
3.6m, Coralie on the Euler 1.2m, and Echelle SPectrograph for Rocky
Exoplanets and Stable Spectroscopic Observations (ESPRESSO) on the
Very Large Telescope (VLT) 8.2m.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 73 34 Summary of Photometric Observations
table2.dat 66 115324 Light curve data for HATS-47, HATS-48A, HATS-49,
and HATS-72
table3.dat 83 20 Summary of Spectroscopy Observations
table5.dat 60 65 Relative radial velocities and bisector spans for
HATS-47, HATS-48A, HATS-49 and HATS-72
table6.dat 173 4 *Adopted derived stellar parameters for HATS-47,
HATS-48A, HATS-49, and HATS-72
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Note on table6.dat: The listed parameters are those determined through
the joint differential evolution Markov Chain analysis described in
Section 3.1. For all four systems, the RV observations are consistent
with a circular orbit, and we assume a fixed circular orbit in
generating the parameters listed here. Systematic errors in the
bolometric correction tables or stellar evolution models are not
included, and may dominate the error budget for some of these
parameters.
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
J/ApJ/724/866 : Follow-up observations of HAT-P-15 (Kovacs+, 2010)
J/ApJ/742/59 : HAT-P-32 and HAT-P-33 follow-up (Hartman+, 2011)
J/ApJ/750/84 : Follow-up photometry and velocity of Qatar 2 (Bryan+, 2012)
J/A+A/546/A14 : Limb-darkening for CoRoT, Kepler, Spitzer (Claret+, 2012)
J/AJ/146/113 : Differential griz photometry of HATS-3 (Bayliss+, 2013)
J/A+A/552/A16 : Limb-darkening for CoRoT, Kepler, Spitzer.II. (Claret+,2013)
J/A+A/552/A82 : WASP-64b and WASP-72b light curves (Gillon+, 2013)
J/AJ/145/5 : Follow-up photometry of HATS-1 (Penev+, 2013)
J/A+A/551/A80 : WASP-80 photometric and radial velocity data (Triaud+, 2013)
J/MNRAS/440/1470 : Ji light curves of WTS-2 (Birkby+, 2014)
J/AJ/148/29 : Spectro. & differential photometry of HATS-4 (Jordan+, 2014)
J/AJ/149/166 : Photometry and spectroscopy of HATS-6 (Hartman+, 2015)
J/AJ/152/108 : i filter photom. HATS-25 through HATS-30 (Espinoza+, 2016)
J/ApJ/831/64 : Mass-metallicity relation giant planets (Thorngren+, 2016)
J/AJ/153/136 : Planets & their host with Gaia parallaxes (Stassun+, 2017)
J/A+A/618/A20 : Limb-darkening for TESS, Kepler, Corot, MOST (Claret, 2018)
J/AJ/156/259 : Robo-AO detected close binaries in Gaia DR2 (Ziegler+, 2018)
J/AJ/157/55 : RVs and light curves for HATS-60-HATS-69 (Hartman+, 2019)
J/AJ/159/19 : SOAR TESS survey. I. (Ziegler+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Object identifier
10- 25 A16 --- Inst Instrument and field used (1)
27- 30 I4 yr start.Y [2006/2019] Year of the beginning of the
observation
32- 34 A3 "month" start.M Month of the beginning of the observation
36- 37 I2 d start.D ? Day of the beginning of the observation
39- 42 I4 yr end.Y [2011/2019]? Year of the end of the observation,
only if different from the beginning year
44- 46 A3 "month" end.M ? Month of the end of the observation, only if
different from the beginning month
48- 52 I5 --- Nphot [30/24431] Number of images, excluding any
outliers or other data not included in the
modeling
54- 57 I4 s Cad [21/1798] The median time between consecutive
images rounded to the nearest second (2)
59- 67 A9 --- Filt Filter used
69- 73 F5.2 mmag rms [0.66/21.8] The rms of the residuals from the
best-fit model (3)
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Note (1): For HATSouth data, we list the HATSouth unit, CCD, and field
name from which the observations are taken. HS-1 and -2 are located
at Las Campanas Observatory in Chile, HS-3 and -4 are located at the
H.E.S.S. site in Namibia, and HS-5 and -6 are located at Siding
Spring Observatory in Australia. Each unit has four CCDs. Each field
corresponds to one of 838 fixed pointings used to cover the full 4π
celestial sphere. All data from a given HATSouth field and CCD number
are reduced together, while detrending through External Parameter
Decorrelation (EPD) is done independently for each unique
unit+CCD+field combination.
Note (2): Due to factors such as weather, the day-night cycle,
guiding, and focus corrections, the cadence is only approximately
uniform over short timescales.
Note (3): In the case of HATSouth and TESS observations, the transit
may appear artificially shallower due to overfiltering and/or blending
from unresolved neighbors. As a result, the S/N of the transit may be
less than what would be calculated from Rp/R* and the rms
estimates given here.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Object identifier
10- 22 F13.5 d BJD [2453862/2458683] Barycentric Julian Date (1)
24- 31 F8.5 mag mag [-6.86/14.5] Observed magnitude in Filter
33- 39 F7.5 mag e_mag [0.0007/4] The 1σ uncertainty in mag
41- 48 F8.5 mag Omag [-0.11/16]? Original magnitude (2)
50- 51 A2 --- Filt Filter used (I+, T, i, r and un)
53- 66 A14 --- Inst Instrument used (3)
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Note (1): Barycentric Julian Dates in this paper are reported on the
Barycentric Dynamical Time (TDB) system.
Note (2): The out-of-transit level has been subtracted. For observations made
with the HATSouth instruments these magnitudes have been corrected
for trends using the EPD and TFA procedures applied prior to fitting
the transit model. This procedure may lead to an artificial dilution
in the transit depths. For several of these systems neighboring stars
are blended into the TESS observations as well. The blend factors
for the HATSouth and TESS light curves are listed in Table 6. For
observations made with follow-up instruments (anything other than
"HS", "TESS" and "WASP" 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. For the Swope 1m observations of HATS-47, these
observations have been further detrended against a set of 20
light curves for other stars observed in the field.
Note (3): See text for details and Table1 for the summary of the
photometric observations.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Object identifier
10- 31 A22 --- Inst Instrument used
33- 36 I4 yr start.Y [2013/2019] Year of the beginning of the
observation
38- 40 A3 "month" start.M Month of the beginning of the observation
42- 43 I2 d start.D ? Day of he beginning of the observation
45- 48 I4 yr end.Y ? Year of the end of the observation, only if
different from the year of beginning
50- 52 A3 "month" end.M ? Month of the end of the observation, only if
different from the month of beginning
54- 55 I2 d end.D ? Day of the end of the observation, only if
different from the day of beginning
57- 58 I2 --- Nspec [1/12] Number of spectra
60- 62 I3 --- R [3/140] Resolution/1000
64- 65 I2 --- S/Nmin [9/52]? Minimum S/N per resolution element near
5180Å
67- 68 I2 --- S/Nmax [31/68]? Maximum S/N per resolution element near
5180Å, if different from minimum
70- 76 F7.3 km/s gRV [-23/68]? Zero-point RV from the best-fit orbit
(γRV) (1)
78- 83 F6.1 m/s pRV [10.5/4000]? Scatter in the RV residuals from the
best-fit orbit (2)
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Note (1): For high-precision RV observations included in the orbit
determination, this is the zero-point RV from the best-fit orbit. For
other instruments, it is the mean value. We only provide this quantity
when applicable.
Note (2): For high-precision RV observations included in the orbit
determination, this is the scatter in the RV residuals from the
best-fit orbit (which may include astrophysical jitter). For other
instruments, this is either an estimate of the precision (not
including jitter) or the measured standard deviation. We only provide
this quantity when applicable.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Object identifier
10- 19 F10.5 d BJD [7023/86387] Barycentric Julian Date BJD-2450000
21- 26 F6.2 m/s RVel [-93.65/78.44]? Radial velocity (1)
28- 32 F5.2 m/s e_RVel [0.6/35]? The 1σ uncertainty in RVel (2)
34- 39 F6.1 m/s BS [-379.5/698.2]? Spectral line bisector span
41- 45 F5.1 m/s e_BS [10/286]? Uncertainty in BS
47- 51 F5.3 m/s Phase [0.014/0.951] Orbital phase
53- 60 A8 --- Inst Instrument used (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
allowed to vary in the fit.
Note (3): See text for details and Table3 for the summary of the
spectroscopic observations.
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Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Object identifier
10- 15 F6.4 Msun M [0.67/0.74] Object mass
17- 23 F7.4 Msun e_M [0.002/0.02] Minimum error on M
25- 29 F5.3 Msun E_M [0.016]? Maximum error on M, if different from
minimum error
31- 36 F6.4 Rsun R [0.65/0.73] Radii
38- 43 F6.4 Rsun e_R [0.002/0.006] Error on R
45- 50 F6.4 [cm/s2] logg [4.58/4.64] Surface gravity
52- 57 F6.4 [cm/s2] e_logg [0.002/0.02] Error on logg
59- 63 F5.3 g/cm3 rho [2.74/3.36] Density (ρ)
65- 69 F5.3 g/cm3 e_rho [0.02/0.1] Minimum error on rho
71- 75 F5.3 g/cm3 E_rho [0.13]? Maximum error on rho, if different from
minimum error
77- 82 F6.4 Lsun L [0.15/0.22] Luminosity
84- 89 F6.4 Lsun e_L [0.002/0.005] Error on L
91- 96 F6.1 K Teff [4405/4657] Effective temperature
98-101 F4.1 K e_Teff [8.9/19] Minimum error on Teff
103-104 I2 K E_Teff [23]? Maximum error on Teff, if different from
minimum error
106-111 F6.3 [-] [Fe/H] [-0.12/0.21] Metallicity
113-117 F5.3 [-] e_[Fe/H] [0.01/0.06] Error on [Fe/H]
119-123 F5.2 Gyr Age [8.1/12.2] Age
125-128 F4.2 Gyr e_Age [0.45/4.3] Minimum error on Age
130-133 F4.2 Gyr E_Age [0.24/2.9] Maximum error on Age
135-140 F6.4 mag AV [0.02/0.12] V band extinction
142-147 F6.4 mag e_AV [0.008/0.04] Error on AV
149-154 F6.2 pc Dist [127.6/324.6] Distance
156-159 F4.2 pc e_Dist [0.52/2.2] Error on Dist
161 A1 --- l_Mcomp Limit flag on Mcomp
163-166 F4.2 Msun Mcomp [0.22/0.36] Companion mass (1)
168-173 F6.4 d Per [3.13/7.33] Period as found in the abstract
(added by CDS)
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Note (1): For HATS-47, HATS-49, and HATS-72, we list the 95%
confidence upper limit on the mass of any unresolved stellar companion
based on modeling the system as a blend between a transiting planet
system and an unresolved wide stellar binary companion (Section 3.2).
For HATS-48A, we list the estimated mass for the 5.4" neighbor in
Gaia DR2 that we determined to be a common-proper-motion and
common-parallax companion to HATS-48A (Section 2.4).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 30-Jun-2020