J/AJ/161/64 Radial velocity and gri light curve of HAT-P-68 (Lindor+, 2021)
HAT-P-68b: a transiting hot Jupiter around a K5 dwarf star*.
Lindor B.M., Hartman J.D., Bakos G.A., Bhatti W., Csubry Z., Penev K.,
Bieryla A., Latham D.W., Torres G., Buchhave L.A., de Val-Borro M.,
Howard A.W., Isaacson H., Fulton B.J., Boisse I., Santerne A., Hebrard G.,
Kovacs T., Huang C.X., Dembicky J., Falco E., Everett M.E., Horch E.P.,
Lazar J., Papp I., Sari P.
<Astron. J., 161, 64 (2021)>
=2021AJ....161...64L 2021AJ....161...64L
ADC_Keywords: Exoplanets; Stars, dwarfs; Stars, K-type; Spectra, optical;
Photometry, ugriz; Radial velocities
Keywords: Exoplanet detection methods ; Exoplanets ; Transit photometry ;
Exoplanet systems ; Extrasolar gas giants ; Hot Jupiters ;
High resolution spectroscopy ; Spectroscopy
Abstract:
We report the discovery by the ground-based Hungarian-made Automated
Telescope Network (HATNet) survey of the transiting exoplanet
HAT-P-68b, which has a mass of 0.724±0.043MJ, and radius of
1.072±0.012RJ. The planet is in a circular P=2.2984day orbit
around a moderately bright V=13.937±0.030magnitude K-dwarf star of
mass 0.673-0.014+0.020M☉, and radius 0.6726±0.0069R☉.
The planetary nature of this system is confirmed through follow-up
transit photometry obtained with the Fred L. Whipple Observatory
(FLWO) 1.2m telescope, high-precision radial velocities measured using
Keck I/High Resolution Echelle Spectrometer (HIRES), FLWO
1.5m/Tillinghast Reflector Echelle Spectrograph (TRES), and
Observatoire de Haute-Provence (OHP) 1.9m/Sophie, and
high-spatial-resolution speckle imaging from WIYN 3.5m/DSSI. HAT-P-68
is at an ecliptic latitude of +3° and outside the field of view of
both the NASA Transiting Exoplanet Survey Satellite primary mission
and the K2 mission. The large transit depth of 0.036mag (r band) makes
HAT-P-68b a promising target for atmospheric characterization via
transmission spectroscopy.
Description:
We have used a number of observations to aid our understanding of
HAT-P-68, and to confirm the existence of an extrasolar planet in the
system. These observations include discovery light curves obtained by
the HATNet survey, ground-based follow-up transit light curves,
high-resolution spectra and associated RVs, high-spatial resolution
imaging, and catalog broadband photometry and astrometry. See Tables 1
and 3 for brief summaries of all the spectroscopic and photometric
observations collected for HAT-P-68.
Objects:
---------------------------------------------------------------
RA (2000) DE Designation(s) (Period)
---------------------------------------------------------------
07 53 55.98 +23 56 17.6 HAT-P-68 = HAT-P-68 (P=2.29840551d)
---------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 66 4 Summary of spectroscopic observations
table2.dat 50 14 Relative radial velocities and bisector spans of
HAT-P-68
table3.dat 57 7 Summary of photometric observations
table4.dat 58 9456 Differential photometry of HAT-P-68
--------------------------------------------------------------------------------
See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/A+A/428/1001 : Non-linear limb-darkening law LTE models. III. (Claret, 2004)
J/A+A/505/853 : HD16760 radial velocity curve (Bouchy+, 2009)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
J/AJ/141/166 : HATNet variability survey of K and M dwarfs (Hartman+, 2011)
J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)
J/ApJ/757/112 : Stellar diameters. II. K and M-stars (Boyajian+, 2012)
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/A+A/558/A86 : HAT-P-42b and HAT-P-43b ri light curves (Boisse+, 2013)
J/A+A/552/A16 : Limb-darkening for CoRoT, Kepler, Spitzer. II. (Claret+,2013)
J/AJ/147/84 : Photometry and spectroscopy of HAT-P-49 (Bieryla+, 2014)
J/A+A/563/A40 : WASP-43b g'r'i'z'JHK light curves (Chen+, 2014)
J/A+A/562/A126 : Light curves of WASP-80 transit events (Mancini+, 2014)
J/AJ/150/168 : Spectro. & photometry for HAT-P-50--HAT-P-53 (Hartman+, 2015)
J/AJ/152/182 : iz follow-up photo. of HAT-P-65 & HAT-P-66 (Hartman+, 2016)
J/AJ/153/136 : Planets & their host stars with Gaia plxs (Stassun+, 2017)
J/A+A/618/A20 : Limb-darkening for TESS, Kepler, Corot, MOST (Claret, 2018)
J/MNRAS/474/876 : WASP-80b wavelength-binned light curves (Kirk+, 2018)
J/AJ/156/18 : APOGEE DR14:Binary comp. evolved stars (Price-Whelan+, 2018)
J/A+A/612/A99 : Gaia-ESO Survey in 7 open star cluster fields (Randich+,2018)
J/AJ/157/55 : RVs and light curves for HATS-60-HATS-69 (Hartman+, 2019)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Tel Telescope used (1)
7- 17 A11 --- Inst Instrument used (2)
19- 22 I4 --- ObsYb [2012/2013] Year of beginning of observation
24- 26 A3 --- ObsMb Month of beginning of observation
28- 31 I4 --- ObsYe [2013/2015] Year of end of observation
33- 35 A3 --- ObsMe Month of end of observation
37 I1 --- Nspec [3/6] Number of spectra
39- 43 I5 --- R [18000/55000] Resolution
45- 48 F4.1 --- S/Nmin [10/81] Minimum S/N (3)
50- 54 F5.1 --- S/Nmax [17/115] Maximum S/N (3)
56- 60 I5 m/s ZP [-8890/-7960]? Zero point (4)
62- 66 F5.1 m/s RVprec [12.5/430] RV precision (5)
--------------------------------------------------------------------------------
Note (1): Telescopes as follows:
APO = Apache Point Observatory in New Mexico
FLWO = Fred L. Whipple Observatory, Arizona
OHP = Observatoire de Haute-Provence, France
KeckI = W. M. Keck Observatory, Hawaii
Note (2): Instruments as follows:
1.5m/TRES = Tillinghast Reflector Echelle Spectrograph
1.9m/Sophie = 1.,9m Sophie
10m/HIRES = High Resolution Echelle Spectrometer
3.5m/ARCES = Astrophysical Research Consortium Echelle Spectrometer
Note (3): Signal-to-noise ratio (S/N) per resolution element near 5180Å.
Note (4): For Sophie RV observations this is the zero-point RV from
the best-fit orbit. For ARCES and TRES it is the mean value of the
low-precision reconnaissance RV. Higher-precision RVs were measured
from the TRES observations and used in the orbit fitting as well,
however these are relative RV measurements that were not adjusted to
an absolute standard.
Note (5): 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.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.5 d BJD [6255/7356] Barycentric Julian Date; BJD-2450000
12- 18 F7.2 m/s RVel [-153/156]? Radial velocity (1)
20- 24 F5.2 m/s e_RVel [2.4/57]? The 1σ uncertainty in RVel (2)
26- 32 F7.1 m/s BIS [-19.7/25886]? Bisector span
34- 37 F4.1 m/s e_BIS [20.3/85]? The 1σ uncertainty in BS
39- 43 F5.3 --- Phase [0.27/0.94] Orbital phase
45- 50 A6 --- Inst Instrument
--------------------------------------------------------------------------------
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/instrumental
jitter considered in Section 3.1.1.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Inst Instrument used (1)
7- 20 A14 --- Field Field name
22- 25 I4 --- ObsYb [2011/2016] Year of observation beginning
27- 29 A3 --- ObsMb Month of observation beginning
31- 32 I2 --- ObsDb ? Day of observation beginning
34- 37 I4 --- ObsYe [2012]? Year of observation end
39- 41 A3 --- ObsMe Month of observation end
43- 46 I4 --- Nphot [18/5867] Number of images
48- 50 I3 s Cad [114/216] Cadence (2)
52 A1 --- Filt Filter used
54- 57 F4.1 mmag Prec [1.3/25.6] rms of residuals from best-fit model
--------------------------------------------------------------------------------
Note (1): Instruments as follows:
FLWO = Fred L. Whipple Observatory, Arizona
HAT-5 = Hungarian Automated Telescope at Fred L. Whipple Observatory, Arizona
HAT-8 = Hungarian Automated Telescope at Maunakea Observatory, Hawaii
Note (2): The median time between consecutive images rounded to the
nearest second. Due to factors such as weather, the day-night cycle,
and guiding and focus corrections, the cadence is only approximately
uniform over short timescales.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Object name
10- 20 F11.5 d BJD [55873/57481]?=0.00000 Barycentric Julian Date,
TDB system w/leap second corrections; BJD-2400000
22- 29 F8.5 mag mag [-0.1/0.2] Out-of-transit subtracted magnitude (1)
31- 37 F7.5 mag e_mag [0/0.1] Uncertainty in mag
39- 46 F8.5 mag omag [0/12.5]? Raw magnitude in Filt (2)
48- 48 A1 --- Filt Filter used in the observation
50- 58 A9 --- Inst Instrument
--------------------------------------------------------------------------------
Note (1): The out-of-transit level has been subtracted.For the HATNet light
curve, these magnitudes have been detrended using the EPD and TFA
procedures prior to fitting a transit model to the light curve. For the
follow-up light curves derived for instruments other than HATNet, these
magnitudes have been detrended with the EPD and TFA procedure, carried
out simultaneously with the transit fit.
Note (2): Raw magnitude values without application of the EPD and TFA
procedure. This is only reported for the follow-up light curves.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 29-Mar-2021