J/AJ/158/141 Differential photometry & RVs of HAT-P-69 & HAT-P-70 (Zhou+, 2019)
Two new HATNet hot Jupiters around A stars and the first glimpse at
the occurrence rate of hot Jupiters from TESS.
Zhou G., Huang C.X., Bakos G.A., Hartman J.D., Latham D.W., Quinn S.N.,
Collins K.A., Winn J.N., Wong I., Kovacs G., Csubry Z., Bhatti W., Penev K.,
Bieryla A., Esquerdo G.A., Berlind P., Calkins M.L., de Val-Borro M.,
Noyes R.W., Lazar J., Papp I., Sari P., Kovacs T., Buchhave L.A.,
Szklenar T., Beky B., Johnson M.C., Cochran W.D., Kniazev A.Y.,
Stassun K.G., Fulton B.J., Shporer A., Espinoza N., Bayliss D., Everett M.,
Howell S.B., Hellier C., Anderson D.R., Cameron A.C., West R.G.,
Brown D.J.A., Schanche N., Barkaoui K., Pozuelos F., Gillon M., Jehin E.,
Benkhaldoun Z., Daassou A., Ricker G., Vanderspek R., Seager S.,
Jenkins J.M., Lissauer J.J., Armstrong J.D., Collins K.I., Gan T., Hart R.,
Horne K., Kielkopf J.F., Nielsen L.D., Nishiumi T., Narita N., Palle E.,
Relles H.M., Sefako R., Tan T.G., Davies M., Goeke R.F., Guerrero N.,
Haworth K., Villanueva S.
<Astron. J., 158, 141 (2019)>
=2019AJ....158..141Z 2019AJ....158..141Z (SIMBAD/NED BibCode)
ADC_Keywords: Stars, A-type ; Photometry ; Optical ; Radial velocities ;
Stars, double and multiple ; Exoplanets ; Stars, distances ;
Effective temperatures ; Stars, masses ; Stars, diameters
Keywords: planetary systems -
stars: individual (HAT-P-69, HAT-P-70, TIC379929661, TIC399870368) -
techniques: photometric - techniques: spectroscopic
Abstract:
Wide-field surveys for transiting planets are well suited to searching
diverse stellar populations, enabling a better understanding of the link
between the properties of planets and their parent stars. We report
the discovery of HAT-P-69 b (TOI 625.01) and HAT-P-70 b (TOI 624.01),
two new hot Jupiters around A stars from the Hungarian-made Automated
Telescope Network (HATNet) survey that have also been observed by the
Transiting Exoplanet Survey Satellite. HAT-P-69 b has a mass of
3.58-0.58+0.58 MJup and a radius of 1.676-0.033+0.051 RJup
and resides in a prograde 4.79 day orbit. HAT-P-70 b has a radius of
1.87-0.10+0.15 RJup and a mass constraint of <6.78 (3σ) MJup
and resides in a retrograde 2.74 day orbit. We use the confirmation of
these planets around relatively massive stars as an opportunity to explore
the occurrence rate of hot Jupiters as a function of stellar mass. We
define a sample of 47126 main-sequence stars brighter than Tmag=10
that yields 31 giant planet candidates, including 18 confirmed planets,
3 candidates, and 10 false positives. We find a net hot Jupiter occurrence
rate of 0.41±0.10% within this sample, consistent with the rate measured
by Kepler for FGK stars. When divided into stellar mass bins, we find
the occurrence rate to be 0.71±0.31% for G stars, 0.43±0.15% for
F stars, and 0.26±0.11% for A stars. Thus, at this point, we cannot
discern any statistically significant trend in the occurrence of hot
Jupiters with stellar mass.
Description:
The HATNet survey (Bakos et al. 2004PASP..116..266B 2004PASP..116..266B) is one of the
longest-running wide-field photometric surveys for transiting planets.
It employs a network of small robotic telescopes at the Fred Lawrence
Whipple Observatory (FLWO) in Arizona and at Maunakea Observatory in
Hawaii. Each survey field is 8°x8°, and observations are obtained
with the Sloan r' filter.
HAT-P-69 and HAT-P-70 were both independently identified as planet
candidates by the WASP survey (Schanche et al. 2019MNRAS.483.5534S 2019MNRAS.483.5534S). The
northern facility (SuperWASP-North) and the southern facility (WASP-South)
both consist of arrays of eight 200 mm f/1.8 Canon telephoto lenses on
a common mount. Each camera is coupled with 2Kx2K detectors, yielding
a field of view of 7.8°x7.8° per camera (Pollacco et al.
2006PASP..118.1407P 2006PASP..118.1407P). HAT-P-69 was observed by both WASP-South and
SuperWASP-North, producing 25200 photometric points spanning from 2009
January 14 to 2012 April 23. HAT-P-70 was observed by SuperWASP-North,
producing 19200 observations spanning 2008 October 13 to 2011 February 4.
A number of transit observations were obtained with the FLWO 1.2 m
telescope and KeplerCam, a 4Kx4K CCD camera operated with 2x2 binning,
giving a plate scale of 0.672"/pixel. Photometry was extracted as per
Bakos et al. (2010, J/ApJ/710/1724). Follow-up photometry was also obtained
using the Las Cumbres Observatory (LCO; Brown et al. 2013PASP..125.1031B 2013PASP..125.1031B)
network. These observations included transits obtained via the 0.8 m LCO
telescope located at the Byrne Observatory at Sedgwick, California, using
the SBIG STX-16803 4Kx4K camera with a field of view of 16'x16'. Additional
photometric follow-up was obtained using the TRAPPIST (TRAnsiting Planets
and PlanetesImals Small Telescope) North facility (Jehin et al.
2011Msngr.145....2J 2011Msngr.145....2J; Gillon et al. 2013, J/A+A/552/A82; Barkaoui et al.
2019, J/AJ/157/43) at Oukaimeden Observatory in Morocco. TRAPPIST-North is
a 0.6 m robotic photometer employing a 2Kx2K CCD with a field of view
of 19.8'x19.8' at a plate scale of 0.6" per pixel.
The Tillinghast Reflector Echelle Spectrograph (TRES; Furesz 2008,
PhD thesis Univ. Szeged) on the 1.5 m telescope at FLWO, Arizona, was used
to obtain dozens of spectra for each system. TRES is a fiber-fed echelle
spectrograph with a spectral resolution of R=44000 over the wavelength
region of 3850-9100 Å. The observing strategy and data reduction process
are described by Buchhave et al. (2012, J/other/Nat/486.375). For HAT-P-69,
relative radial velocities were obtained using a multiorder analysis
(Quinn et al. 2012, J/ApJ/745/80) of the TRES spectra. For HAT-P-70, we
modeled the stellar line profiles derived from a least-squares
deconvolution (LSD; Donati et al. 1997MNRAS.291..658D 1997MNRAS.291..658D) to derive the
absolute radial velocities of each spectrum.
Objects:
-------------------------------------------------------
RA (ICRS) DE Designation(s)
-------------------------------------------------------
08 42 01.36 +03 42 38.0 HAT-P-69 = TYC 215-1594-1
04 58 12.56 +09 59 52.8 HAT-P-70 = HD 287325
-------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 68 53163 Differential photometry of HAT-P-69
table3.dat 68 30857 Differential photometry of HAT-P-70
table5.dat 32 53 Relative radial velocities of HAT-P-69
table6.dat 32 54 Relative radial velocities of HAT-P-70
table9.dat 173 18 Confirmed planets with Tmag<10
table10.dat 173 3 Planet candidates
table11.dat 173 10 Candidates determined to be false positives
table12.dat 173 5 Confirmed planets around evolved stars with
Tmag<10 not included in occurrence rate
calculation
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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/745/80 : HAT-P-25 differential photometry (Quinn+, 2012)
J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012)
J/A+A/552/A82 : WASP-64b and WASP-72b light curves (Gillon+, 2013)
J/ApJ/809/77 : Transiting Exoplanet Survey Satellite (TESS)
(Sullivan+, 2015)
J/AJ/156/102 : The TESS Input Catalog and Candidate Target List
(Stassun+, 2018)
J/AJ/157/31 : Differential photometry + radial velocities of HATS-70
(Zhou+, 2019)
J/AJ/157/43 : WASP-161b, WASP-163b and WASP-170b (Barkaoui+, 2019)
J/AJ/157/55 : RVs and light curves for HATS-60-HATS-69 (Hartman+, 2019)
Byte-by-byte Description of file: table2.dat table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 F18.10 d BJD Barycentric Julian Date
20- 27 F8.5 mag Rawmag [-0.04633/11.97588] Raw magnitude in Filter (1)
29- 36 F8.5 mag EPDmag [9.00787/10.04926]? External Parameter
Decorrelation magnitude in Filter (1)
38- 45 F8.5 mag TFAmag [9.65422/10.03226]? Trend Filtering Algorithm
magnitude in Filter (1)
47- 53 F7.5 mag e_mag [0.00082/0.18312]? Magnitude uncertainty
55- 63 A9 --- Inst Instrument (2)
65- 68 A4 --- Filter Filter used (3)
--------------------------------------------------------------------------------
Note (1): The detrending and potential blending may cause the HATNet transit
to be shallower than the true transit in the EPD and TFA light curves. This is
accounted for in the global modeling by the inclusion of a dilution factor.
Follow-up light curves have been treated with EPD simultaneous to the transit
fitting. Pre-EPD magnitudes are presented for the follow-up light curves.
There are no EPDmag or TFAmag values for WASP, KeplerCam, LCO, and TRAPPIST
observations.
Note (2): Instrument as follows:
HATNet = The HATNet survey (Bakos et al. 2004PASP..116..266B 2004PASP..116..266B);
WASP = The WASP survey (Schanche et al. 2019MNRAS.483.5534S 2019MNRAS.483.5534S);
KeplerCam = The FLWO 1.2m telescope with KeplerCam;
LCO = The 0.8m Las Cumbres Observatory at the Byrne Observatory;
TRAPPIST = The TRAPPIST (TRAnsiting Planets and PlanetesImals Small
Telescope) North 0.6 m telescope.
Note (3): Filter as follows:
GC = Green continuum filter centered at 5260 Å with width of 65 Å;
RC = Red continuum filter centered at 7128 Å with width of 58 Å;
WASP = WASP broadband.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 F14.6 d BJD Barycentric Julian Date (UTC)
16- 21 F6.3 km/s RV [0.062/36.999] Relative radial velocity (1)
23- 27 F5.3 km/s e_RV [0.098/3.309] Uncertainty in RV (1)
29- 32 A4 --- Inst Instrument (TRES)
--------------------------------------------------------------------------------
Note (1): In Table 5: relative radial velocities from a multiorder cross
correlation. In Table 6: Absolute velocities derived from the least-squares
deconvolution profiles. Internal errors excluding the component of
astrophysical/instrumental jitter considered in Section 3. Velocities exclude
those taken in transit.
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Byte-by-byte Description of file: table9.dat table1[012].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I9 --- TIC [1129033/455135327] TESS Input Catalog identifier
11- 16 F6.2 --- TOI [102.01/630.01] TESS Object of Interest identifier
18- 25 A8 --- OName Alternative name of star (only in Tables 9 and 12)
27- 29 A3 --- Status Status (1)
31- 34 F4.1 d Per [0.9/10.3] Period
36- 40 I5 ppm Depth [859/20670] Transit depth
42- 46 F5.2 mag Gmag [8.23/10.59] Gaia G-band magnitude
48- 52 F5.2 mag BPmag [8.43/11.23] Gaia BP magnitude
54- 57 F4.2 mag RPmag [7.77/9.95] Gaia RP magnitude
59- 61 I3 pc Dist [44/640] Distance
63- 66 I4 K Teff [4216/8400] Effective temperature (2)
68- 71 F4.2 Msun M* [0.5/2.2] Stellar mass (2)
73- 76 F4.2 Rsun R* [0.81/3.28] Stellar radius (2)
78-105 A28 --- Ref Reference (only in Tables 9 and 12)
107-125 A19 --- Bibcode Bibcode of the reference (only in Tables 9 and 12)
127-140 A14 --- Com Comment on reference (only in Table 9)
142-173 A32 --- Fup Follow-up status (only in Table 10)
--------------------------------------------------------------------------------
Note (1): Status as follows:
P = Confirmed planet;
PC = Active planet candidate;
NEB = Nearby eclipsing binary;
BEB = Blended eclipsing binary;
SB1 = Single-lined spectroscopic binary;
NPC = Transit caused by nearby source that may still be planetary in origin.
Note (2): Parameters Teff, M*, and R* from isochrone interpolation of the
Gaia color-magnitude values. These can deviate from literature values but are
consistent with the remainder of the analysis of the field star population.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 28-Oct-2019