J/AJ/152/88 Spectroscopy and photometry of HATS-11 and HATS-12 (Rabus+, 2016)
HATS-11b AND HATS-12b: two transiting hot Jupiters orbiting subsolar metallicity
stars selected for the K2 campaign 7.
Rabus M., Jordan A., Hartman J.D., Bakos G.A., Espinoza N., Brahm R.,
Penev K., Ciceri S., Zhou G., Bayliss D., Mancini L., Bhatti W.,
De Val-Borro M., Csbury Z., Sato B., Tan T.-G., Henning T., Schmidt B.,
Bento J., Suc V., Noyes R., Lazar J., Papp I., Sari P.
<Astron. J., 152, 88-88 (2016)>
=2016AJ....152...88R 2016AJ....152...88R (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Stars, double and multiple ; Photometry ;
Radial velocities
Keywords: planetary systems - stars: individual (HATS-11 - HATS-12) -
techniques: photometric - techniques: spectroscopic
Abstract:
We report the discovery of two transiting extrasolar planets from the
HATSouth survey. HATS-11, a V=14.1 G0-star shows a periodic 12.9mmag
dip in its light curve every 3.6192days and a radial velocity
variation consistent with a Keplerian orbit. HATS-11 has a mass of
1.000±0.060M☉, a radius of 1.444±0.057R☉ and an
effective temperature of 6060±150K, while its companion is a
0.85±0.12MJ, 1.510±0.078RJ planet in a circular orbit. HATS-12
shows a periodic 5.1mmag flux decrease every 3.1428days and Keplerian
radial velocities variations around a V=12.8 F-star. HATS-12 has a
mass of 1.489±0.071M☉, a radius of 2.21±0.21R☉, and an
effective temperature of 6408±75K. For HATS-12b, our measurements
indicate that this is a 2.38±0.11MJ, 1.35±0.17RJ planet in a
circular orbit. Both host stars show subsolar metallicities of
-0.390±0.060dex and -0.100±0.040dex, respectively, and are
(slightly) evolved stars. In fact, HATS-11 is among the most
metal-poor and, HATS-12, with a logg* of 3.923±0.065, is among the
most evolved stars hosting a hot-Jupiter planet. Importantly, HATS-11
and HATS-12 have been observed in long cadence by Kepler as part of K2
campaign 7 (EPIC216414930 and EPIC218131080 respectively).
Description:
The initial images of HATS-11 and HATS-12 were obtained with the
HATSouth wide-field telescope network consisting of 24 Takahashi E180
astrographs with an aperture of 18cm. The photons were detected with
Apogee 4k*4k U16M ALTA CCDs. Details on the time span and number of
images are shown in Table1. The numerical data of the light curves are
available in Table3.
The spectroscopic observations are summarized in Table2. The data for
the phased high-precision radial velocity and bisector span
measurements are presented in Table6.
Photometric follow-up observations are summarized in Table1. The data
are given in Table3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 68 2 Stars observed
table1.dat 70 18 Summary of photometric observations
table2.dat 73 10 Summary of spectroscopy observations
table3.dat 59 23050 Light curve data for HATS-11 and HATS-12
table6.dat 59 44 Relative radial velocities and bisector spans
for HATS-11 and HATS-12
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See also:
J/A+A/580/A63 : HATS-13b and HATS-14b light and RV curves (Mancini+, 2015)
J/AJ/150/33 : Photometry and spect. of HATS-9 and HATS-10 (Brahm+, 2015)
J/AJ/149/166 : Photometry and spectroscopy of HATS-6 (Hartman+, 2015)
J/AJ/148/29 : Spectroscopy and differential phot. of HATS-4 (Jordan+, 2014)
J/AJ/147/144 : Differential griz photometry of HATS-5 (Zhou+, 2014)
J/A+A/563/A143 : WASP-68b, WASP-73b, WASP-88b transits (Delrez+, 2014)
J/A+A/558/A55 : HATS-2b griz light curves (Mohler-Fischer+, 2013)
J/AJ/146/113 : Differential griz photometry of HATS-3 (Bayliss+, 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/ApJ/742/59 : HAT-P-32 and HAT-P-33 follow-up (Hartman+, 2011)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Object identifier: HATS-11 or HATS-12
9- 24 A16 --- 2MASS 2MASS identifier (1)
26- 27 I2 h RAh Hour of Right Ascension (J2000) (1)
29- 30 I2 min RAm Minute of Right Ascension (J2000) (1)
32- 36 F5.2 s RAs Second of Right Ascension (J2000) (1)
38 A1 --- DE- Sign of the Declination (J2000) (1)
39- 40 I2 deg DEd Degree of Declination (J2000) (1)
42- 43 I2 arcmin DEm Arcminute of Declination (J2000) (1)
45- 48 F4.1 arcsec DEs Arcsecond of Declination (J200) (1)
50- 58 F9.7 d Per Period (from Table5 in the paper)
60- 68 F9.7 d e_Per Error in Period (from Table5 of the paper)
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Note (1): From Table4 of the paper.
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Object identifier: HATS-11 or HATS-12
9- 26 A18 --- Inst Instrument (1)
28 A1 --- f_Inst Flag on HS instrument (a) (2)
30- 33 A4 --- Field Field name (G579) for HATSouth unit
35- 51 A17 --- Date Date of observation
53- 56 I4 --- Nimg [46/4315] Number of images
58- 60 I3 s Cad [16/304] Cadence (3)
62- 63 A2 --- Flt Filter (Ks, Rc, R, g, r, or i)
65 A1 --- f_Flt [d] Flag "d" means Rc is standard Cousins R filter
67- 70 F4.1 mmag rms [0.7/11.5] Precision (4)
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Note (1): The instrument names are defined as below:
PEST = The 0.3m Perth Exoplanet Survey Telescope (PEST);
HS-1.2 = CCD 2 on HATSouth-1 unit located at Las Campanas
Observatory in Chile;
HS-3.1 = CCD 1 on HATSouth-3 unit located at the High Energy
Spectroscopic Survey (H.E.S.S.) site in Namibia;
HS-3.2 = CCD2 on HATSouth-3 unit;
HS-5.2 = CCD2 on HATSouth-5 unit located at Siding Spring
Observatory in Australia;
AAT+IRIS2 = InfraRed Imager and Spectrograph (IRIS2) on the 3.9m
Anglo Australian Telescope (AAT), at the Siding Spring
Observatory, Australia. The instrument uses a Hawaii
1-RG detector, has a field of view of 7.7'*7.7', pixel
scale of 0.4486''.
SWOPE 1 m = Swope 1m telescope;
LCOGT 1 m+SBIG = SBIG camera at Las Cumbres Observatory Global
Telescope (LCOGT) 1m network;
MPG 2.2 m+GROND = Gamma-Ray Burst Optical/Near-Infrared Detector (GROND)
at the Max Planck Gesellschaft (MPG) 2.2m telescope;
DK 1.54 m+DFOSC = Danish Faint Object Spectrograph and Camera (DFOSC) on
the DK 1.54m telescope;
LCOGT 1 m+Sinistro = Sinistro camera at Las Cumbres Observatory Global
Telescope (LCOGT) 1m network;
Note (2):
a=For HATSouth data, we list the HATSouth unit, CCD, and field name from
which the observations are taken. HS-1 and -2 are located at Las Campanas
Observatory in Chile, HS-3 and -4 are located at the High Energy
Spectroscopic Survey (H.E.S.S.) site in Namibia, and HS-5 and -6 are
located at Siding Spring Observatory in Australia. Each unit has 4 ccds.
Each field corresponds to one of 838 fixed pointings used to cover the
full 4π celestial sphere. All data from a given HATSouth field and CCD
number are reduced together, while detrending through External Parameter
Decorrelation (EPD) is done independently for each unique unit+CCD+field
combination.
Note (3): The median time between consecutive images rounded to the nearest
second. Due to factors such as weather, the day-night cycle, guiding, and
focus corrections, the cadence is only approximately uniform over short
timescales.
Note (4): The rms scatter of the residuals from our best-fit transit model for
each light curve at the cadence indicated in the table.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Object identifier: HATS-11 or HATS-12
9- 29 A21 --- Inst Instrument (1)
31- 47 A17 --- Date UT date(s) of observation
49- 50 I2 --- Nobs [1/12] Number of spectroscopic observations
52- 53 I2 --- Res [3/60] Resolution (Δλ/λ/1000)
55- 57 I3 --- S/N1 [11/257] First value of signal-to-noise ratio
range (2)
59- 61 I3 --- S/N2 [17/118]? Second value of signal-to-noise ratio
range (2)
63- 68 F6.2 km/s gamma [-58.8/-21.66]? γRV (3)
70- 73 I4 m/s Pre [13/4000]? Radial velocity precision (4)
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Note (1): The instruments are defined as below:
Subaru 8 m/HDS = I2-free observation with High Dispersion
Spectrograph (HDS) at the Subaru 8m telescope;
ANU 2.3 m/WiFeS = Australian National University (ANU) 2.3m telescope
using the Wide-Field Spectrograph (WiFES)
spectrograph;
MPG 2.2 m/FEROS = Fiber-fed Extended Range Optical Spectrograph
(FEROS) on the Max Planck Gesellschaft (MPG) 2.2m
telescope;
Subaru 8 m/HDS+I2 = I2 observation with High Dispersion Spectrograph
(HDS) at the Subaru 8m telescope;
Euler 1.2 m/Coralie = CORALIE spectrograph at the Euler 1.2m telescope;
du Pont 2.5 m/Echelle = duPont 2.5m telescope with echelle spectrograph.
Note (2): S/N per resolution element near 5180Å.
Note (3): For the CORALIE and FEROS observations of HATS-11, and for the FEROS
observations of HATS-12, this is the zero-point radial velocity (RV) from
the best-fit orbit. For the WiFeS and du Pont Echelle, it is the mean of
the observations. We do not provide this quantity for HDS for which only
relative RVs are measured, or for the lower resolution WiFeS observations,
which were only used to measure stellar atmospheric parameters.
Note (4): For high-precision radial velocity observations included in the orbit
determination, this is the scatter in the radial velocity 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 do not provide this
quantity for low-resolution observations from the ANU 2.3m/WiFeS or for
I2-free observations made with HDS, as radial velocities are not measured
from these data.
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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 identifier: HATS-11 or HATS-12
9- 21 F13.5 d BJD Barycentric Julian Date (1)
23- 30 F8.5 mag Dmag [-0.055/0.041] Observed differential magnitude in
Flt (2)
32- 38 F7.5 mag e_Dmag [0.0005/0.02] 1σ uncertainty in Dmag
40- 47 F8.5 mag omag [-0.025/14.4]? Original/raw magnitude in Flt (3)
49 A1 --- Flt Filter used (K, R, g, r, or i)
51- 59 A9 --- Inst Instrument used (AAT/IRIS2, DK154, GROND, HS,
LCOGT1m, PEST, or Swope) (4)
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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 HATSouth instruments (identified by "HS" in the Inst column) these
magnitudes have been corrected for trends using the EPD and TFA procedures
applied prior to fitting the transit model. This procedure may lead to an
artificial dilution in the transit depths. For HATS-11 the transit depth is
72% and 84% that of the true depth for the G579.1 and G579.2 observations,
respectively. For HATS-12 it is 100% and 78% that of the true depth for the
G579.4 and G580.1 observations, respectively. 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): The instruments are defined as below:
HS = HATSouth;
PEST = Perth Exoplanet Survey Telescope;
Swope = Swope 1m telescope;
GROND = Gamma-Ray Burst Optical/Near-Infrared Detector;
DK154 = DK 1.54m telescope;
LCOGT1m = Las Cumbres Observatory Global Telescope (LCOGT) 1m network;
AAT/IRIS2 = InfraRed Imager and Spectrograph (IRIS2) on the 3.9m Anglo
Australian Telescope (AAT).
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Object identifier: HATS-11 or HATS-12
9- 17 F9.5 d BJD [161/733] Barycentric Julian Date (BJD-2456000)
19- 25 F7.2 m/s RV [-375/282]? Radial velocity (1)
27- 32 F6.2 m/s e_RV [11/144]? 1σ error in RV (2)
34- 39 F6.1 m/s BS [-171/247] Bisector span (1)
41- 45 F5.1 m/s e_BS [9/288] 1σ error in BS (3)
47- 51 F5.3 --- Phase [0/1] Phase
53- 59 A7 --- Inst Instrument (Coralie, FEROS, or HDS) (4)
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Note (1): Note that for the HDS iodine-free template exposures we do not measure
the RV but do measure the BS. Such template exposures can be distinguished
by the missing RV value. The HDS observation of HATS-12 without a BS
measurement has too low S/N in the I2-free blue spectral region to pass our
quality threshold for calculating accurate BS values. The zero-point of the
RVs 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
considered in Section 3.3.
Note (3): For FEROS and Coralie, we take the BS uncertainty to be twice the RV
uncertainty. For HDS, the BS uncertainty is taken to be the standard error
on the mean of the BS values calculated for each of the Echelle orders.
Note (4): The instruments are defined as below:
HDS = High Dispersion Spectrograph;
FEROS = Fiber-fed Extended Range Optical Spectrograph;
Coralie = Coralie spectrograph.
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History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 26-Oct-2016