J/AJ/163/125 Light curve & radial velocity of 4 giants planets (Jordan+, 2022)
HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets
Around K and M Dwarfs.
Jordan A., Hartman J.D., Bayliss D., Bakos G.A., Brahm R., Bryant E.M.,
Csubry Z., Henning T., Hobson M., Mancini L., Penev K., Rabus M., Suc V.,
de Val-Borro M., Wallace J., Barkaoui K., Ciardi D.R., Collins K.A.,
Esparza-Borges E., Furlan E., Gan T., Benkhaldoun Z., Ghachoui M.,
Gillon M., Howell S., Jehin E., Fukui A., Kawauchi K., Livingston J.H.,
Luque R., Matson R., Matthews E.C., Osborn H.P., Murgas F., Narita N.,
Palle E., Parvianen H., Waalkes W.C.
<Astron. J., 163, 125 (2022)>
=2022AJ....163..125J 2022AJ....163..125J
ADC_Keywords: Stars, dwarfs; Exoplanets; Photometry, ugriz; Spectra, optical;
Radial velocities
Keywords: Exoplanets
Abstract:
The relative rarity of giant planets around low-mass stars compared
with solar-type stars is a key prediction from the core-accretion
planet formation theory. In this paper we report on the discovery of
four gas giant planets that transit low-mass late K and early M
dwarfs. The planets HATS-74Ab (TOI737b), HATS-75b (TOI552b), HATS-76b
(TOI555b), and HATS-77b (TOI730b) were all discovered from the
HATSouth photometric survey and follow-up using TESS and other
photometric facilities. We use the new ESPRESSO facility at the VLT to
confirm systems and measure their masses. We find that these planets
have masses of 1.46±0.14MJ, 0.491±0.039MJ,
2.629±0.089MJ, and 1.374-0.074+0.100MJ, respectively, and
radii of 1.032±0.021RJ, 0.884±0.013RJ,
1.079±0.031RJ, and 1.165±0.021RJ, respectively. The
planets all orbit close to their host stars with orbital periods
ranging from 1.7319days to 3.0876days. With further work, we aim to
test core-accretion theory by using these and further discoveries to
quantify the occurrence rate of giant planets around low-mass host
stars.
Description:
HATSouth uses a network of 24 telescopes, each 0.18m in aperture, and
4Kx4K front-side-illuminated CCD cameras. These are attached to a
total of 6 fully automated mounts, each with an associated enclosure,
which are in turn located at three sites around the Southern
Hemisphere. The three sites are Las Campanas Observatory (LCO) in
Chile, the site of the HESS gamma-ray observatory in Namibia, and
Siding Spring Observatory (SSO) in Australia.
The spectroscopic observations was carried out to confirm and
characterize the four transiting planet systems presented here. The
facilities used include: Echelle spectrograph on the du Pont 2.54m, 31
WiFeS on the ANU 2.3m, ARCES on the ARC 3.5m, FEROS on the MPG 2.2m,
ARCoIRIS on the Blanco 4m, and ESPRESSO on the VLT 8.2m. The du Pont,
WiFeS, ARCES, and FEROS observations were obtained only for HATS-74A,
while all four systems were observed with ARCoIRIS and ESPRESSO.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
objects.dat 184 4 *Astrometric and spectroscopic paramaters
table2.dat 65 160589 Light curve data
table5.dat 49 19 ESPRESSO relative radial velocities and
bisector spans
--------------------------------------------------------------------------------
Note on objects.dat: Constructed with data from table4 in the article
--------------------------------------------------------------------------------
See also:
II/346 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
J/A+A/415/1153 : [Fe/H] for 98 extra-solar planet-host stars (Santos+, 2004)
J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)
J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 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/551/A112 : Metallicity-giant planet correlation (Mortier+, 2013)
J/AJ/145/5 : Follow-up photometry of HATS-1 (Penev+, 2013)
J/ApJ/791/54 : Nearby M Dwarfs parameters (Gaidos+, 2014)
J/AJ/148/29 : Spectroscopy & diff photometry of HATS-4 (Jordan+, 2014)
J/AJ/147/20 : Spectroscopy of 447 nearby M dwarfs (Newton+, 2014)
J/AJ/150/33 : Photometry & spectroscopy of HATS-9 and HATS-10 (Brahm+, 2015)
J/ApJ/800/85 : Teff, radii and luminosities of cool dwarfs (Newton+, 2015)
J/AJ/153/71 : Kepler follow-up obs. program. I. Imaging (Furlan+, 2017)
J/AJ/153/136 : Planets & host stars 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/158/109 : Occurrence rates of planets orbiting FGK stars (Hsu+, 2019)
J/other/Sci/365.1441 : GJ 512 radial velocity and light curves (Morales+, 2019)
J/AJ/159/267 : Observations & radial velocity of HATS-71b (Bakos+, 2020)
Byte-by-byte Description of file: objects.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Star identifier
9- 24 A16 --- 2MASS 2MASS star identifier
26- 34 I9 --- TIC TIC identifier
36- 41 F6.2 --- TOI TOI identifier
43- 61 I19 --- Gaia Gaia DR2 identifier
63- 64 I2 h RAh [4/11] Hour of right ascension (J2000)
66- 67 I2 min RAm Minute of right ascension (J2000)
69- 75 F7.4 s RAs Second of right ascension (J2000)
77 A1 --- DE- [-] Sign of declination (J2000)
78- 79 I2 deg DEd [19/32] Degree of declination (J2000)
81- 82 I2 arcmin DEm Arcminute of declination (J2000)
84- 90 F7.4 arcsec DEs Arcsecond of declination (J2000)
92- 98 F7.3 mas/yr pmRA [-38.9/12.9] Proper motion in right ascension
100-104 F5.3 mas/yr e_pmRA [0.03/0.2] Error in pmRA
106-112 F7.3 mas/yr pmDE [-38.7/39.7] Proper motion in declination
114-118 F5.3 mas/yr e_pmDE [0.04/0.1] Error in pmDE
120-124 F5.3 mas plx [2.26/5.1] Parallax
126-130 F5.3 mas e_plx [0.02/0.06] Error on plx
132-135 I4 K Teff [3775/4082] Effective temperature
137-139 I3 K e_Teff [54/120] Error on Teff
141-146 F6.3 [-] Fe/H [-0.12/0.3] Log metallicity
148-152 F5.3 [-] e_Fe/H [0.08/0.2] Error on Fe/H
154-160 F7.1 m/s RVel [-7758/39998] Radial velocity
162-165 F4.1 m/s e_RVel [5/43] Error on RVel
167-175 F9.6 d Prot [4.74/35.1]? Period of rotation
177-184 F8.6 d e_Prot [0.00004/0.002]? Error on Prot
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Star identifier
9- 21 F13.5 d BJD [2455216/2459221] Barycentric Julian Date, TDB system
w/leap second corrections
23- 30 F8.5 mag mag [-0.34/19.4] Out-of-transit subtracted magnitude (1)
32- 38 F7.5 mag e_mag [0.001/0.3] Uncertainty in mag
40- 47 F8.5 mag omag [-0.34/27.5]? Raw magnitude in Filt (2)
49- 50 A2 --- Filt Filter used in the observation
52- 65 A14 --- Inst Instrument (3)
--------------------------------------------------------------------------------
Note (1): 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. 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 7. 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 (2): 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.
Note (3): Instruments as follows:
CTIO09m = CTIO 0.9m
HS = HATSouth network
HS/focus = HATSouth network + focus
LCO/MuSCAT3 = MuSCAT3 imager at LCO 2m telescope at Haleakala Observatory
LCOGT0.4m = 0.4m network telescopes from Las Cumbres Observatory
LCOGT1m = 1m telescopes from the Las Cumbres Observatory
MtStuart = Mt. Stuart 0.3m telescope near Dunedin, New Zealand
MuSCAT2 = MuSCAT2 imager on the 1.5m Telescopio Carlos Sanchez (TCS)
at Teide Observatory
TESS = TESS Follow-up Program
TESS/Sec4 = TESS Sector 4
TESS/Sec5 = TESS Sector 5
TESS/Sec9 = TESS Sector 9
TRAPPIST-South = TRAPPIST-South
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Star identifier
9- 18 F10.5 d BJD [8756/8849] Barycentric Julian Date, BJD-2450000
20- 26 F7.2 m/s RVel [-566/362]? Radial velocity (1)
28- 32 F5.2 m/s e_RVel [8/27]? The 1σ uncertainty in RVel (2)
34- 38 F5.1 m/s BIS [-20.4/109]? Bisector span of the cross-correlation
function profile
40- 43 F4.1 m/s e_BIS [16/54]? The 1σ uncertainty in BS
45- 49 F5.3 --- Phase [0.03/1] Orbital phase
--------------------------------------------------------------------------------
Note (1): The zero-point of these velocities is arbitrary. An overall offset
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.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 21-Apr-2022