J/AJ/152/182 iz follow-up photometry of HAT-P-65 and HAT-P-66 (Hartman+, 2016)
HAT-P-65b and HAT-P-66b: two transiting inflated hot Jupiters and observational
evidence for the reinflation of close-in giant planets.
Hartman J.D., Bakos G.A., Bhatti W., Penev K., Bieryla A., Latham D.W.,
Kovacs G., Torres G., Csubry Z., De Val-Borro M., Buchhave L., Kovacs T.,
Quinn S., Howard A.W., Isaacson H., Fulton B.J., Everett M.E., Esquerdo G.,
Beky B., Szklenar T., Falco E., Santerne A., Boisse I., Hebrard G.,
Burrows A., Lazar J., Papp I., Sari P.
<Astron. J., 152, 182-182 (2016)>
=2016AJ....152..182H 2016AJ....152..182H (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Stars, double and multiple ; Photometry ;
Radial velocities
Keywords: stars: individual: (HAT-P-65,GSC 1111-00383,HAT-P-66,GSC 3814-00307) -
techniques: photometric - techniques: spectroscopic
Abstract:
We present the discovery of the transiting exoplanets HAT-P-65b and
HAT-P-66b, with orbital periods of 2.6055 and 2.9721 days, masses of
0.527±0.083MJ and 0.783±0.057MJ, and inflated radii of
1.89±0.13RJ and 1.59-0.10+0.16RJ, respectively. They orbit
moderately bright (V=13.145±0.029 and V=12.993±0.052) stars of
mass 1.212±0.050M☉ and 1.255-0.054+0.107M☉. The
stars are at the main-sequence turnoff. While it is well known that
the radii of close-in giant planets are correlated with their
equilibrium temperatures, whether or not the radii of planets increase
in time as their hosts evolve and become more luminous is an open
question. Looking at the broader sample of well-characterized close-in
transiting giant planets, we find that there is a statistically
significant correlation between planetary radii and the fractional
ages of their host stars, with a false-alarm probability of only
0.0041%. We find that the correlation between the radii of planets and
the fractional ages of their hosts is fully explained by the known
correlation between planetary radii and their present-day equilibrium
temperatures; however, if the zero-age main-sequence equilibrium
temperature is used in place of the present-day equilibrium
temperature, then a correlation with age must also be included to
explain the planetary radii. This suggests that, after contracting
during the pre-main-sequence, close-in giant planets are reinflated
over time due to the increasing level of irradiation received from
their host stars. Prior theoretical work indicates that such a dynamic
response to irradiation requires a significant fraction of the
incident energy to be deposited deep within the planetary interiors.
Description:
Both HAT-P-65 and Both HAT-P-66 were selected as candidate transiting
planet systems based on Sloan r-band photometric time series
observations carried out with the HATNet telescope network.
HATNet consists of six 11cm aperture telephoto lenses, each coupled to
an APOGEE front-side-illuminated CCD camera, and each placed on a
fully automated telescope mount. Four of the instruments are located
at Fred Lawrence Whipple Observatory (FLWO) in Arizona, USA, while two
are located on the roof of the Submillimeter Array hangar building at
Mauna Kea Observatory (MKO) on the island of Hawaii, USA. Each
instrument observes a 10.6°*10.6° field of view. We conducted
follow-up photometric time series observations of each object using
KeplerCam on the 1.2m telescope at FLWO.
HAT-P-65 was observed on 2009 Sep-Dec with a r-band filter using the
HAT-6/G342 (located at FLWO) and the HAT-8/G342 (located on the roof
of the Smithsonian Astrophysical Observatory Submillimeter Array
hangar building at Mauna Kea Observatory in Hawaii), and on 2011 Jun
10 (i filter), 2011 Jun 26 (i filter), 2011 Jul 14 (i filter), 2011
Sep 20 (i filter), 2013 Sep 16 (z filter), 2013 Sep 29 (i filter), and
2013 Oct 04 (i filter) using the FLWO 1.2m/KeplerCam. HAT-P-66 was
observed on 2011 Feb-2012 Mar using the HAT-10/G101 (located at FLWO)
with a r-band filter, using the HAT-6/G101 (located at FLWO) with a
r-band filter, and using the HAT-7/G101 (located at FLWO) with a
r-band filter, on 2011 Feb-2012 Apr using the HAT-5/G101 (located at
FLWO) with a r-band filter, on 2011 May-2012 Jun using the HAT-8/G101
(located on the roof of the Smithsonian Astrophysical Observatory
Submillimeter Array hangar building at Mauna Kea Observatory in
Hawaii) with a r-band filter, on 2011 Oct-2012 Jan using the
HAT-9/G101 (located at FLWO) with a r-band filter, and on 2015 Apr 29
(i filter), 2015 Nov 26 (z filter), 2015 Dec 08 (i filter) using the
FLWO 1.2m/KeplerCam.
Spectroscopic observations of both HAT-P-65 and HAT-P-66 were carried
out using the Tillinghast Reflector Echelle Spectrograph (TRES) on the
1.5m Tillinghast Reflector at FLWO (on 2010 Oct 27 for HAT-P-65, and
2014 Nov-2015 Jun for HAT-P-66), and the HIgh-Resolution Echelle
Spectrometer (HIRES) on the Keck I 10m at Mauna Kea Observatory (MKO)
on the island of Hawaii, USA (on 2010 Dec 14 and 2010 Dec-2013 Aug for
HAT-P-65, and on 2016 Feb 3 and 2015 Dec-2016 Jan for HAT-P-66). For
HAT-P-65 we also obtained observations on 2010 Aug 21-22 and 2011 Oct
8 using the Fibre-fed Echelle Spectrograph (FIES) on the 2.5m Nordic
Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos
on the Spanish island of La Palma. For HAT-P-66 spectroscopic
observations were also collected on 2015 Mar-2016 Jan using the SOPHIE
spectrograph on the 1.93m telescope at the Observatoire de
Haute-Provence (OHP) in France.
The light curve measurements are available in Table2. The individual
radial velocity and bisector span measurements are made available in
Table4.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stars.dat 58 2 Stars observed
table2.dat 58 21756 Light-curve data for HAT-P-65 and HAT-P-66
table4.dat 60 43 Relative radial velocities and bisector spans
for HAT-P-65 and HAT-P-66
table7.dat 167 223 *Adopted parameters for transiting planet systems
discovered by HAT, KELT, TrES, and WASP
refs.dat 76 167 References
--------------------------------------------------------------------------------
Note on table7.dat: Hungarian Automated Telescope (HAT), Kilodegree Extremely
Little Telescope (KELT), Tillinghast reflector Echelle Spectrograph (TrES), and
Wide Angle Search for Planets (WASP).
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See also:
J/AJ/150/197 : Photometry and spectroscopy of HAT-P-57 (Hartman+, 2015)
J/AJ/149/149 : Photometry and spectroscopy of HAT-P-54 (Bakos+, 2015)
J/AJ/147/128 : HAT-P-44, HAT-P-45, and HAT-P-46 follow-up (Hartman+, 2014)
J/AJ/147/84 : Photometry and spectroscopy of HAT-P-49 (Bieryla+, 2014)
J/A+A/558/A86 : HAT-P-42b and HAT-P-43b ri light curves (Boisse+, 2013)
J/AJ/144/139 : HAT-P-39, HAT-P-40, and HAT-P-41 follow-up (Hartman+, 2012)
J/AJ/144/19 : Follow-up photometry for HAT-P-34-HAT-P-37 (Bakos+, 2012)
J/ApJ/742/59 : HAT-P-32 and HAT-P-33 follow-up (Hartman+, 2011)
J/ApJ/742/116 : Photometry of 4 massive transiting exoplanets (Bakos+, 2011)
J/ApJ/734/109 : Follow-up photometry of HAT-P-27 (Beky+, 2011)
J/ApJ/733/116 : HAT-P-28 and HAT-P-29 photometry (Buchhave+, 2011)
J/ApJ/728/138 : Follow-up photometry of HAT-P-26 (Hartman+, 2011)
J/ApJ/726/52 : HAT-P-18 and HAT-P-19 follow-up (Hartman+, 2011)
J/ApJ/720/1118 : i-band photometry of HAT-P-16 (Buchhave+, 2010)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
J/ApJ/706/785 : HAT-P-12 light curve (Hartman+, 2009)
J/ApJ/696/1950 : Sloan iz light curves of HAT-P-10 (Bakos+, 2009)
J/A+A/508/1011 : Planetary transit of TrES-1 and TrES-2 (Rabus+, 2009)
J/ApJ/707/446 : HAT-P-13 photometry follow-up (Bakos+, 2009)
J/ApJ/704/1107 : Transiting planet in HATNet field 205 (Latham+, 2009)
Byte-by-byte Description of file: stars.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Star name
10- 11 I2 h RAh Hour of Right Ascension (J2000)
13- 14 I2 min RAm Minute of Right Ascension (J2000)
16- 20 F5.2 s RAs Second of Right Ascension (J2000)
22 A1 --- DE- Sign of the Declination
23- 24 I2 deg DEd Degree of Declination (J2000)
26- 27 I2 arcmin DEm Arcminute of Declination (J2000)
29- 32 F4.1 arcsec DEs Arcsecond of Declination (J2000)
34- 39 F6.3 mag Vmag V-band magnitude
41- 45 F5.3 mag e_Vmag Error in Vmag
47- 48 A2 --- SpT Spectral type
50- 58 F9.7 d Per Period
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Object identifier (either HAT-P-65 or HAT-P-66)
10- 20 F11.5 d BJD Barycentric Julian Date (BJD-2400000) (1)
22- 29 F8.5 mag mag [-0.09/0.06] Out-of-transit magnitude in Filter (2)
31- 37 F7.5 mag e_mag [0.001/0.066] Uncertainty in mag (σMag)
39- 46 F8.5 mag omag [10.8/12.4]? Original magnitude in Filter (3)
48 A1 --- Flt [riz] Filter used in the observation
50- 58 A9 --- Inst Instrument (HATNet for detection, or KeplerCam for
follow-up) (4)
--------------------------------------------------------------------------------
Note (1): 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 HATNet instruments (identified by "HATNet" in the "Instrument"
column) these magnitudes have been corrected for trends using the external
parameter decorrelation (EPD; see Bakos et al., Cat. J/ApJ/710/1724) and
Trend Filtering Algorithm (TFA; see Kovacs et al. 2005MNRAS.356..557K 2005MNRAS.356..557K)
procedures applied in signal-reconstruction mode. For observations made
with follow-up instruments (anything other than "HATNet" in the
"Instrument" column), the magnitudes have been corrected for a quadratic
trend in time, for variations correlated with three Point-Spread Function
(PSF) shape parameters, and with a linear basis of template light curves
representing other systematic trends, which are fit simultaneously with the
transit.
Note (3): Raw magnitude values without correction for the quadratic trend in
time, or for trends correlated with the shape of the Point-Spread Function
(PSF). These are only reported for the follow-up observations.
Note (4): The two instruments are defined as below:
HATNet = Hungarian Automated Telescope Network;
KeplerCam = KeplerCam on the 1.2m telescope at Fred Lawrence Whipple
Observatory (FLWO).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Object identifier (HAT-P-65 or HAT-P-66)
10- 19 F10.5 d BJD Barycentric Julian Date (BJD-2450000)
21 A1 --- f_BJD [c] Flag for excluded observation (c) (1)
23- 29 F7.2 m/s RV [-132.3/191]? Radial velocity (2)
31- 35 F5.2 m/s e_RV [2.9/75.3]? Uncertainty in RV (σRV) (3)
37- 42 F6.1 m/s BS [-204/61.3]? Bisector span
44- 47 F4.1 m/s e_BS [2.2/84.6]? Uncertainty in BS (σBS)
49- 53 F5.3 --- Phase [0/1] Phase
55- 60 A6 --- Inst Instrument (HIRES, Sophie, or TRES) (4)
--------------------------------------------------------------------------------
Note (1): These observations were excluded from the analysis because they were
obtained during transit and the radial velocities may be affected by the
Rossiter-McLaughlin effect.
Note (2): The zero point of these velocities is arbitrary. An overall offset
γrel fitted independently to the velocities from each instrument
has been subtracted. Radial velocities are not measured for the I2-free
HIRES template spectra, but spectral line bisector spans are measured for
these spectra.
Note (3): Internal errors excluding the component of astrophysical jitter
considered in Section 3.3.
Note (4): The instrument codes are defined as follows:
TRES = Tillinghast Reflector Echelle Spectrograph (on the 1.5m
Tillinghast Reflector at Fred Lawrence Whipple Observatory in
Arizona, USA);
HIRES = HIgh-Resolution Echelle Spectrometer (on the Keck I 10m at Mauna
Kea Observatory on the island of Hawaii, USA);
Sophie = SOPHIE spectrograph on the 1.93m telescope at the Observatoire de
Haute-Provence in France.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Planet name
11- 16 F6.3 d Per [0.7/16.3]? Period
18- 23 F6.3 Mjup Mp [0/61]? Planet mass (in Jupiter mass)
25- 29 F5.3 Mjup e_Mp [0/0.9]? Uncertainty in Mp (or negative error)
31- 35 F5.3 Mjup E_Mp [0.012/1.85]? Positive error in Mp
37- 41 F5.3 Rjup Rp [0.1/2.1]? Planet radius (in Jupiter radius)
43- 47 F5.3 Rjup e_Rp [0/0.4]? Uncertainty (or negative error) in Rp
49- 53 F5.3 Rjup E_Rp [0.017/0.48]? Positive error in Mp
55- 58 I4 K Teq [670/2516]? Planet equilibrium temperature
60- 62 I3 K e_Teq [5/140]? Uncertainty (or negative error) in Teq
64- 66 I3 K E_Teq [13/230]? Positive error in Teq
68- 71 I4 K Teff [3770/7500]? Effective temperature of the star
73- 75 I3 K e_Teff [27/250]? Uncertainty (or negative error) in Teff
77- 79 I3 K E_Teff [38/200]? Positive error in Teff
81- 85 F5.3 g/cm3 rho [0.1/4.4]? Stellar density ρ*
87- 91 F5.3 g/cm3 e_rho [0/0.9]? Uncertainty (or negative error) in rho
93- 97 F5.3 g/cm3 E_rho [0/0.92]? Positive error in rho
99-103 F5.2 [Sun] [Fe/H] [-0.6/0.45]? Metallicity
105-108 F4.2 [Sun] e_[Fe/H] [0.03/0.25]? Uncertainty (or negative error) in
[Fe/H]
110-113 F4.2 [Sun] E_[Fe/H] [0.04/0.11]? Positive error in [Fe/H]
115-119 F5.3 Msun Mass [0.5/1.7]? Stellar mass
121-126 F6.3 Msun e_Mass [0.01/60]? Uncertainty (or negative error) in
Mass
128-132 F5.3 Msun E_Mass [0.02/0.13]? Positive error in Mass
134-138 F5.2 Gyr Age [0/18.5]? Age
140-143 F4.2 Gyr e_Age [0/6.4]? Uncertainty (or negative error) in Age
145-148 F4.2 Gyr E_Age [0.02/6.35]? Positive error in Age
150-154 F5.2 Gyr Ttot [2.35/19.95]? Total lifetime
156-167 A12 --- Ref Reference; in refs.dat file
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Ref [1/167] Reference identifier
5- 23 A19 --- BibCode Bibliographic code
25- 54 A30 --- Aut Author's name
56- 76 A21 --- Com Comments
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History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 09-May-2017