J/AJ/151/89 Spectroscopy and photometry of HATS-17 (Brahm+, 2016)
HATS-17b: a transiting compact warm Jupiter in a 16.3 day circular orbit.
Brahm R., Jordan A., Bakos G.A., Penev K., Espinoza N., Rabus M.,
Hartman J.D., Bayliss D., Ciceri S., Zhou G., Mancini L., Tan T.G.,
De Val-Borro M., Bhatti W., Csubry Z., Bento J., Henning T., Schmidt B.,
Rojas F., Suc V., Lazar J., Papp I., Sari P.
<Astron. J., 151, 89 (2016)>
=2016AJ....151...89B 2016AJ....151...89B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, G-type ; Planets ;
Radial velocities ; Photometry
Keywords: planetary systems - stars: individual (HATS-17) -
techniques: photometric - techniques: spectroscopic
Abstract:
We report the discovery of HATS-17b, the first transiting warm Jupiter
of the HATSouth network. HATS-17b transits its bright (V=12.4) G-type
(M*=1.131±0.030M☉, R*=1.090-0.046+0.070)
metal-rich ([Fe/H]=+0.3dex) host star in a circular orbit with a
period of P=16.2546days. HATS-17b has a very compact radius of
0.777±0.056RJ given its Jupiter-like mass of 1.338±0.065MJ. Up
to 50% of the mass of HATS-17b may be composed of heavy elements in
order to explain its high density with current models of planetary
structure. HATS-17b is the longest period transiting planet discovered
to date by a ground-based photometric survey, and is one of the
brightest transiting warm Jupiter systems known. The brightness of
HATS-17 will allow detailed follow-up observations to characterize the
orbital geometry of the system and the atmosphere of the planet.
Description:
The star HATS-17 was observed by HATSouth instruments between UT 2011
April 26 and UT 2012 July 31 using the HS-2 (on 2011 Apr-2012 Jul with
r filter), HS-4 (on 2011 Jul-2012 Jul with r filter), and HS-6 (on
2011 May-2012 Jul with r filter) units at Las Campanas Observatory
(LCO) in Chile, the High Energy Spectroscopic Survey (H.E.S.S.) site
in Namibia, and Siding Spring Observatory (SSO) in Australia,
respectively.
The first photometric follow-up light curve of this system was
obtained with the 0.3m Perth Exoplanet Survey Telescope (PEST) located
near Perth on 2015 Apr 26 with a RC filter.
Another two partial transits were then acquired with the Las Cumbres
Observatory Global Telescope (LCOGT) 1m telescope network,
specifically with the telescope at Cerro Tololo Inter-American
Observatory (CTIO) on 2015 May 13 with i filter, and with the Swope 1m
coupled with the e2v camera at Las Campanas Observatory (LCO) on 2015
May 29 with i filter.
Finally, two partial transits of the same event were measured with
high photometric precision (∼1mmag). The observations were performed
with the same two telescopes that registered the previous partial
transits (Swope 1m/e2v (LCO) on 2015 Jul 17 with i filter, and LCOGT
1 m/sinistro (CTIO) on 2015 Jul 17 with i filter).
Several high resolution spectra were acquired with three spectrographs
installed in the ESO La Silla observatory. We obtained 11 spectra
using HARPS at the ESO 3.6m telescope, 8 spectra using CORALIE, at the
Euler 1.2m telescope and 2 spectra with FEROS at the MPG 2.2m
telescope.
Table2 provides the light curve data. Radial velocity and bisector
span values are presented in Table3 with their corresponding
uncertainties.
Objects:
--------------------------------------------------------------------
RA (ICRS) DE Designation(s) (Period)
--------------------------------------------------------------------
12 48 45.55 -47 36 49.3 HATS-17 = GSC 08249-00170 (P=16.254611)
--------------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 61 10397 Differential photometry of HATS-17
table3.dat 49 21 Relative radial velocities and bisector span
measurements of HATS-17
--------------------------------------------------------------------------------
See also:
J/ApJ/813/111 : Differential photometry of the K dwarf HATS-7 (Bakos+, 2015)
J/AJ/150/49 : Photometry and spectroscopy of HATS-8 (Bayliss+, 2015)
J/AJ/149/166 : Photometry and spectroscopy of HATS-6 (Hartman+, 2015)
J/AJ/148/29 : Spectroscopy and photometry of HATS-4 (Jordan+, 2014)
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/724/866 : Follow-up observations of HAT-P-15 (Kovacs+, 2010)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.5 d BJD UTC Barycentric Julian date (BJD-2400000) (G1)
14- 21 F8.5 mag Dmag [-0.03/0.021] Observed differential magnitude
in Flt (1)
25- 31 F7.5 mag e_Dmag [0.0006/0.009] Uncertainty in Dmag
34- 41 F8.5 mag omag [-0.006/12.5]? Raw, observed magnitude (2)
43- 44 A2 --- Flt Filter used in the observation (Rc, r, or i)
46- 61 A16 --- Inst Instrument used in observation (HS=HATSouth,
PEST, LCOGT1m/sinistro, or Swope/E2V) (3)
--------------------------------------------------------------------------------
Note (1): The out-of-transit level has been subtracted. For the HATSouth light
curve (rows with "HS" in the Instrument column), these magnitudes have been
detrended using the External Parameter Decorrelation (EPD; Bakos et al.
2010, cat. J/ApJ/710/1724 ) and the Trend Filtering Algorithm (TFA; Kovacs
et al. 2005MNRAS.356..557K 2005MNRAS.356..557K) procedures prior to fitting a transit model
to the light curve. Primarily as a result of this detrending, but also due
to blending from neighbors, the apparent HATSouth transit depth is somewhat
shallower than that of the true depth in the Sloan r filter (the apparent
depth is 79% that of the true depth). For the follow-up light curves (rows
with an Instrument other than "HS") these magnitudes have been detrended
with the EPD procedure, carried out simultaneously with the transit fit
(the transit shape is preserved in this process).
Note (2): Raw magnitude values without correction for the quadratic trend in
time. These are only reported for the follow-up observations.
Note (3): Instrument used in the observation are defined as below:
HS = HATSouth;
PEST = 0.3m Perth Exoplanet Survey Telescope;
LCOGT1m/sinistro = Las Cumbres Observatory Global Telescope (LCOGT) 1.0m
telescope network at Cerro Tololo Inter-American
Observatory (CTIO) in Chile using the Sinistro imaging
camera;
Swope/E2V = 1.0m Swope telescope at Las Campanas Observatory (LCO)
with the E2V imaging camera.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.5 d BJD UTC Barycentric Julian date (BJD-2456000) (G1)
12- 18 F7.2 m/s RV [-128.2/101] Relative Radial Velocity (1)
20- 24 F5.2 m/s e_RV [4/18] Uncertainty in RV (2)
26- 30 F5.1 m/s BS [-88/38] Bisector Span
32- 35 F4.1 m/s e_BS [10/40] Uncertainty in BS
37- 41 F5.3 --- Phase [0/1] Orbital Phase
43- 49 A7 --- Inst Instrument used in the observation (Coralie,
FEROS, or HARPS) (3)
--------------------------------------------------------------------------------
Note (1): The zero-point of these velocities is arbitrary. An overall offset,
γrel, fitted separately to the data from three instruments has been
subtracted.
Note (2): Internal errors excluding the component of astrophysical/instrumental
jitter considered in Section 3 of this article.
Note (3): Instrument used in the observation are defined as below:
HARPS = HARPS spectrograph (ESO 3.6m telescope at La Silla);
Coralie = CORALIE/Euler 1.2m telescope;
FEROS = FEROS/MPG 2.2m telescope at the ESO Observatory in La Silla.
--------------------------------------------------------------------------------
Global Notes:
Note (G1): Barycentric Julian Date is computed directly from the UTC time
without correction for leap seconds.
History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 26-Jul-2016