J/AJ/150/33 Photometry and spectroscopy of HATS-9 and HATS-10 (Brahm+, 2015)
HATS9-b and HATS10-b: two compact hot jupiters in field 7 of the K2 mission.
Brahm R., Jordan A., Hartman J.D., Bakos G.A., Bayliss D., Penev K.,
Zhou G., Ciceri S., Rabus M., Espinoza N., Mancini L., de Val-borro M.,
Bhatti W., Sato B., Tan T.G., Csubry Z., Buchhave L., Henning T.,
Schmidt B., Suc V., Noyes R.W., Papp I., Lazar J., Sari P.
<Astron. J., 150, 33 (2015)>
=2015AJ....150...33B 2015AJ....150...33B
ADC_Keywords: Planets ; Stars, double and multiple ; Stars, dwarfs ;
Stars, G-type ; Photometry ; Radial velocities
Keywords: planetary systems -
stars: individual: (HATS-9,GSC 6305-02502,HATS-10,GSC 6311-00085) -
techniques: photometric - techniques: spectroscopic
Abstract:
We report the discovery of two transiting extrasolar planets by the
HATSouth survey. HATS-9b orbits an old (10.8±1.5Gyr) V=13.3 G dwarf
star with a period p≈1.9153days. The host star has a mass of
1.03M☉, radius of 1.503R☉, and effective temperature
5366±70K. The planetary companion has a mass of 0.837MJ and radius
of 1.065RJ, yielding a mean density of 0.85g/cm-3. HATS-10b orbits
a V=13.1 G dwarf star with a period p≈3.3128days. The host star has a
mass of 1.1M☉, radius of 1.11R☉, and effective temperature
5880±120K. The planetary companion has a mass of 0.53MJ and radius
of 0.97RJ, yielding a mean density of 0.7g/cm3. Both planets are
compact in comparison with planets receiving similar irradiation from
their host stars and lie in the nominal coordinates of Field 7 of K2,
but only HATS-9b falls on working silicon. Future characterization of
HATS-9b with the exquisite photometric precision of the Kepler
telescope may provide measurements of its reflected light signature.
Description:
In this work we present the discovery of HATS-9b and HATS-10b, two hot
Jupiters discovered by the HATSouth survey that are located in the
nominal coordinates of Field 7 of the K2 mission.
HATS-9 and HATS-10 were identified as transiting planetary host
candidates after obtaining ∼10000 images of the same field (G579) with
three stations (HATSouth-1, HATSouth-3, and HATSouth-5) on the three
HATSouth observing sites (HS-1 is located at Las Cumbres Observatory
in Chile, HS-3 is located at the High Energy Spectroscopic Survey
(H.E.S.S.) site in Namibia, and HS-5 is located at Siding Spring
Observatory in Australia). HATS-9 was observed on 2010 Mar-2011 Aug
with HS-1, on 2010 Mar-2011 Aug with HS-3, and on 2010 Sep-2011 Aug
with HS-5. HATS-10 was observed on 2009 Sep-2011 Aug with HS-1, on
2010 Mar-2011 Aug with HS-3, and on 2011 Mar-2011 Aug with HS-5. The
HATSouth observations consist of four-minute Sloan r-band exposures
obtained with 24 Takahashi E180 astrographs (18cm aperture) coupled to
Apogee 4K*4K U16M ALTA CCDs.
Two partial transits of HATS-9 were detected using the 0.3m Perth
Exoplanet Survey Telescope (PEST) on 2013 May 31 and the spectral
camera on the 2m Faulkes Telescope South (FTS) on 2013 Apr 11, part of
Las Cumbres Observatory Global Telescope (LCOGT). Two partial transits
of HATS-10 were observed with FTS on 2013 Apr 05 and the Cerro Tololo
Inter-American Observatory (CTIO) 0.9m telescope on 2012 Aug 29.
Another two full transits were measured with PEST on 2013 Jun 27 and
the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) instrument
on the MPG 2.2m telescope at the ESO Observatory in La Silla on 2013
Jun 14. Results of these observations are presented in Table 4.
Reconnaissance spectroscopy was performed for HATS-9 with ARCES on the
APO 3.5m on 2012 Aug 25 (R=Δλ/λ=31.5), and for
HATS-10 using the echelle spectrograph mounted on the du Pont 2.5m
telescope at LCO on 2013 Aug 21 (R=Δλ/λ=40). Once
both candidates were identified as single-lined late-type dwarfs,
spectra from high-precision instruments were required to measure
radial velocity variations with high precision. HATS-9 and HATS-10
were observed several times with Coralie on the 1.2m Euler telescope
(HATS-9 on 2012 Nov 6-10 with R=Δλ/λ=60, and
HATS-10 on 2012 Aug-2013 Aug with R=Δλ/λ=60),
Fiber-fed Extended Range Optical Spectrograph (FEROS) on the 2.2m MPG
telescope (HATS-9 on 2012 Aug-2013 May with
R=Δλ/λ=48, and HATS-10 on 2013 Mar-Jul with
R=Δλ/λ=48), and HDS on the 8m Subaru telescope
(HATS-9 on 2012 Sep 19-22 with R=Δλ/λ=60, and
HATS-10 on 2012 Sep 19-22 with R=Δλ/λ=60). Phased
high-precision radial velocity and bisector span measurements are
listed in Table 3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars 17 2 Stars observed
table3.dat 59 54 Relative radial velocities and bisector spans
for HATS-9 and HATS-10
table4.dat 63 20560 Light curve data for HATS-9 and HATS-10
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See also:
J/AJ/149/166 : Photometry and spectroscopy of HATS-6 (Hartman+, 2015)
J/AJ/149/149 : Photometry and spectroscopy of HAT-P-54 (Bakos+, 2015)
J/AJ/144/19 : Follow-up photometry for HAT-P-34--HAT-P-37 (Bakos+, 2012)
J/AJ/148/29 : Spectroscopy and photometry of HATS-4 (Jordan+, 2014)
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/AJ/146/113 : Differential griz photometry of HATS-3 (Bayliss+, 2013)
J/A+A/558/A55 : HATS-2b griz light curves (Mohler-Fischer+, 2013)
J/AJ/145/5 : Follow-up photometry of HATS-1 (Penev+, 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/AJ/141/166 : HATNet variability survey of K and M dwarfs (Hartman+, 2011)
J/ApJ/742/59 : HAT-P-32 and HAT-P-33 follow-up (Hartman+, 2011)
J/ApJ/726/52 : HAT-P-18 and HAT-P-19 follow-up (Hartman+, 2011)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
Byte-by-byte Description of file: stars
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Object name
9- 17 F9.7 d Per Period (from Table 6 in the paper)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Object name (HATS-9 or HATS-10)
9- 17 F9.5 d BJD Barycentric Julian Date (BJD-2456000)
19 A1 --- f_BJD 'c' indicates Coralie observation acquired in
2013 August and contaminated with moonlight
21- 27 F7.2 m/s RV [-141.84/177]? Relative radial velocity (1)
29- 33 F5.2 m/s e_RV [7.39/64]? 1σ uncertainty in RV (2)
35- 40 F6.1 m/s BS [-126/462]? Bisector span
42- 45 F4.1 m/s e_BS [8.8/38.3]? 1σ uncertainty in BS
47- 51 F5.3 --- Phase [0/1] Phase
53- 59 A7 --- Inst Instrument (Coralie, FEROS, or Subaru) (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 are
considered in Section 3.3.
Note (3): Here are some details about the three instruments:
Coralie = CORALIE spectrograph (mounted on the Euler 1.2m telescope);
FEROS = Fiber-fed Extended Range Optical Spectrograph
(mounted on the ESO/MPG 2.2m telescope);
Subaru = Subaru 8m telescope (with High Dispersion Spectrograph).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Object Name (HATS-9 or HATS-10)
9- 21 F13.5 d BJD UTC Barycentric Julian date (BJD-2400000) (1)
23- 30 F8.5 mag Dmag [-0.03354/0.03015] Δm observed in filter (2)
32- 38 F7.5 mag e_Dmag [0.00042/0.04129] Uncertainty in mag
40- 47 F8.5 mag omag [-0.00668/14.3135]? Raw, observed magnitude (3)
49- 50 A2 --- Flt Filter used in the observation (Rc, g, r, i, z)
52- 63 A12 --- Inst Instrument used in the observation (CTIO09,
ESO22/GROND, FTS/Spectral, HS or PEST) (4)
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Note (1): Barycentric Julian Date is 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 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; Kovacs
et al., 2005MNRAS.356..557K 2005MNRAS.356..557K) procedures applied prior to fitting the
transit model. This procedure may lead to an artificial dilution in the
transit depths. For HATS-9b our fit is consistent with no dilution, for
HATS-10b the HATSouth transit depth is 93% that of the true depth. 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 fit simultaneously with the transit.
Note (3): Raw magnitude values without correction for the quadratic trend in
time. These are only reported for the follow-up observations.
Note (4): Instruments we used are:
HS = HATSouth at Las Campanas;
FTS/Spectral = Spectral camera on the 2m Faulkes Telescope South;
PEST = 0.3m Perth Exoplanet Survey Telescope;
CTIO09 = 0.9m telescope at Cerro Tololo Inter-American Observatory;
ESO22/GROND = Gamma-Ray Burst Optical/Near-Infrared Detector on MPG/ESO 2.2m.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 30-Jul-2015