J/AJ/152/161 Photometry for HATS-31 through HATS-35 (de Val-Borro+, 2016)
HATS-31b through HATS-35b: five transiting hot Jupiters discovered by the
HATSouth survey.
de Val-Borro M., Bakos G.A., Brahm R., Hartman J.D., Espinoza N., Penev K.,
Ciceri S., Jordan A., Bhatti W., Csubry Z., Bayliss D., Bento J., Zhou G.,
Rabus M., Mancini L., Henning T., Schmidt B., Tan T.G., Tinney C.G.,
Wright D.J., Kedziora-Chudczer L., Bailey J., Suc V., Durkan S., Lazar J.,
Papp I., Sari P.
<Astron. J., 152, 161-161 (2016)>
=2016AJ....152..161D 2016AJ....152..161D (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Stars, double and multiple ; Photometry ;
Radial velocities
Keywords: planetary systems - stars: individual - techniques: photometric -
techniques: spectroscopic
Abstract:
We report the discovery of five new transiting hot-Jupiter planets
discovered by the HATSouth survey, HATS-31b through HATS-35b. These
planets orbit moderately bright stars with V magnitudes within the
range of 11.9-14.4mag while the planets span a range of masses of
0.88-1.22MJ and have somewhat inflated radii between 1.23 and
1.64RJ. These planets can be classified as typical hot Jupiters,
with HATS-31b and HATS-35b being moderately inflated gas giant planets
with radii of 1.64±0.22RJ and 1.464-0.044+0.069RJ,
respectively, that can be used to constrain inflation mechanisms. All
five systems present a higher Bayesian evidence for a
fixed-circular-orbit model than for an eccentric orbit. The orbital
periods range from 1.8209993±0.0000016 day for HATS-35b) to
3.377960±0.000012 day for HATS-31b. Additionally, HATS-35b orbits a
relatively young F star with an age of 2.13±0.51Gyr. We discuss the
analysis to derive the properties of these systems and compare them in
the context of the sample of well-characterized transiting hot
Jupiters known to date.
Description:
The HATSouth survey is a global network of homogeneous, completely
automated wide-field telescopes located at three sites in the Southern
Hemisphere: HS-1 and -2 are located at Las Campanas Observatory (LCO)
in Chile, HS-3 and -4 are located at the High Energy Stereoscopic
Survey (H.E.S.S.) site in Namibia, and HS-5 and -6 are located at
Siding Spring Observatory (SSO) in Australia. Observations are
performed using a Sloan-r filter with four-minute exposures. The
HATSouth network was commissioned in 2009 and since then has proved to
be a robust system for the monitoring of time-variable phenomena. Each
HATSouth unit consists of four Takahashi E180 astrographs with an
aperture of 18cm and an f/2.8 focal ratio on a common mount, equipped
with Apogee 4096*4096 U16M ALTA cameras.
HATS-31 was observed with the HS-1.4/G565 on 2012 Dec-2013 Jun, with
the HS-3.4/G565 on 2012 Dec-2013 Jul, and with the HS-5.4/G565 on 2012
Dec-2013 Jul. HATS-32 was observed with the HS-2.3/G586 on 2010
Aug-2011 Nov, with the HS-4.3/G586 on 2010 Aug-2011 Nov, and with the
HS-6.3/G586 on 2010 Aug-2011 Nov. HATS-33 was observed with the
HS-1.4/G747 on 2013 Mar-2013 Oct, with the HS-2.4/G747 on 2013
Sep-2013 Oct, with the HS-3.4/G747 on 2013 Apr-2013 Nov, with the
HS-4.4/G747 on 2013 Sep-2013 Nov, with the HS-5.4/G747 on 2013
Mar-2013 Nov, and with the HS-6.4/G747 on 2013 Sep-2013 Nov. HATS-34
was observed with the HS-2.4/G754 on 2012 Sep-2012 Dec, with the
HS-4.4/G754 on 2012 Sep-2013 Jan, and with the HS-6.4/G754 on 2012
Sep-2012 Dec. HATS-35 was observed with the HS-2.4/G778 on 2011
May-2012 Nov, with the HS-4.4/G778 on 2011 Jul-2012 Nov, with the
HS-6.4/G778 on 2011 Apr-2012 Oct.
The egress of HATS-31b was observed on 2015 February 28 and 2015 April
02 with the Las Cumbres Observatory Global Telescope (LCOGT) 1m+Cerro
Tololo Inter-American Observatory (CTIO) telescope network and the
Swope 1m telescopes, respectively. Additionally, an almost full
transit of HATS-31b was observed with LCOGT 1m+South African
Astronomical Observatory/Santa Barbara Instrument Group (LCOGT
1 m+SAAO/SBIG) on 2015 March 6. Another three partial transits of
HATS-32b were observed with the Perth Exoplanet Survey Telescope
(PEST) 0.3m, DK 1.54m, and the Swope 1m telescopes on 2014 Jul 09,
2014 Nov 04, and 2015 May 28, respectively. The egress of HATS-33 was
measured with the 1m LCOGT at CTIO on 2015 May 20. Both ingress and
egress of HATS-34b were observed by the PEST 0.3m on 2014 Oct 26 and
by the Danish Faint Object Spectrograph and Camera (DFOSC) on the DK
1.54m telescope on 2014 Nov 03. HATS-34b was also observed using
Anglo-Australian Telescope 3.9m/InfraRed Imaging Spectrograph 2 (AAT
3.9m/IRIS2) on 2015 Sep 25 but This light curve covers a predicted
secondary eclipse event, it is not included in the analysis carried
out to determine the system parameters for HATS-34 (however, it is
included in the analysis carried out to exclude blend scenarios).
Finally, five partial transit events of HATS-35b were obtained between
2015 June 12 and 2015 July 24 using the LCOGT network at CTIO on 2015
Jun 12, 2015 Jul 15 and 2015 Jul 24, at SAAO on 2015 Jul 14, and at
SSO on 2015 Jul 18.
Reconnaissance spectroscopy was carried out using the Wide Field
Spectrograph (WiFeS) on the Australian National University (ANU) 2.3m
telescope at SSO on 2014 Dec 30-31 and 2015 Jan 1 for HATS-31, on 2014
Jun 3-5 and 2014 Jun 4 for HATS-32, on 2014 Dec-2015 Mar and 2015 Mar
4 for HATS-33, on 2014 Oct 4 and 2014 Oct 4-10 for HATS-34, and on
2014 Oct 5 and 2014 Oct 11 for HATS-35. Medium-resolution WiFeS
observations spectral resolution was R=λ/Δλ=7000.
We obtained 11 spectra using CYCLOPS2+University College London
Echelle Spectrograph (CYCLOPS2+UCLES;
Δλ/λ/1000=70) at the 3.9m AAT on 2015 May 7-13 for
HATS-33, 11 spectra using the High-Accuracy Radial velocity Planetary
Searcher (HARPS; Δλ/λ/1000=115) on the European
Southern Observatory (ESO) 3.6m telescope (6 spectra on 2015 Feb 14-19
for HATS-31; 3 spectra on 2015 Apr 6-8 for HATS-33; 2 spectra on 2015
Apr 7-8 for HATS-35), 10 spectra using CORALIE
(Δλ/λ/1000=60) on the Euler 1.2m telescope (5
spectra on 2015 Mar-Jun for HATS-33; 5 spectra on 2014 Nov-2015 Jun
for HATS-35), and 32 spectra with Fiber-fed Extended Range Optical
Spectrograph (FEROS; Δλ/λ/1000=48) at the Max
Planck Gesellschaft (MPG) 2.2m telescope (8 spectra on 2014 Jul-2015
Jun for HATS-32; 4 spectra on 2015 May-Jul for HATS-33; 10 spectra on
2015 Jun-Jul for HATS-34; 10 spectra on 2015 Jun-Jul for HATS-35).
The photometric data are available in Table3. The high-resolution
spectroscopic data are provided in Table8.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stars.dat 68 5 Stars observed
table3.dat 68 68236 Light-curve data for HATS-31--HATS-35
table8.dat 61 61 Relative radial velocities and bisector spans
for HATS-31--HATS-35
--------------------------------------------------------------------------------
See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
J/A+A/580/A63 : HATS-13b and HATS-14b light and RV curves (Mancini+, 2015)
J/AJ/150/33 : Phot. and spectroscopy 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 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)
Byte-by-byte Description of file: stars.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Name of the observed star
9- 24 A16 --- 2MASS 2MASS identification
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 (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 (J2000) (1)
50- 58 F9.7 d Per Period (2)
60- 68 F9.7 d e_Per Error in Per (2)
--------------------------------------------------------------------------------
Note (1): From Table 4 or 5 in the paper (taken from 2MASS; see Cutri at al.
2003, Cat. II/246).
Note (2): From Table 6 or 7.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Object identifier (HATS-31, HATS-32, HATS-33,
HATS-34, or HATS-35)
10- 22 F13.5 d BJD Barycentric Julian date (1)
24- 31 F8.5 mag mag [-0.07/0.06]? Observed magnitude in Filter (2)
33- 39 F7.5 mag e_mag [0.0008/0.029] Uncertainty in mag
41- 48 F8.5 mag omag [-0.024/14.24]? Observed magnitude in Filter (3)
50- 51 A2 --- Flt Filter (Ks, R, Rc, i, or Sloan-r)
53- 68 A16 --- Inst Instrument (HS, AAT3.9m/iris2, DK1.54m/DFOSC,
LCOGT1m/SBIG, LCOGT1m/sinistro, PEST0.3m, or
Swope1m/e2v) (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 HATSouth instruments (identified by "HS" in the "Inst" column)
these magnitudes have been corrected for trends using the External
Parameter Decorrelation (EPD; Bakos et al. 2010, Cat. J/ApJ/710/1724) 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. The blend factors for
the HAT-South light curves are listed in Tables 6 and 7. For observations
made with follow-up instruments (anything other than "HS" in the
"Instrument" column), the magnitudes have been corrected for a quadratic
trend in time, and for variations correlated with three Point Spread
Function (PSF) shape parameters, 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 PSF. These are only
reported for the follow-up observations.
Note (4): The instruments are defined as follows:
HS = HATSouth network;
AAT3.9m/iris2 = The InfraRed Imaging Spectrograph 2 (IRIS2) on the
Anglo-Australian Telescope 3.9m;
DK1.54m/DFOSC = Danish Faint Object Spectrograph and Camera (DFOSC) on
the Danish 1.54-m Telescope (DK1.54m);
LCOGT1m/SBIG = Santa Barbara Instrument Group (SBIG) at Las Cumbres
Observatory Global Telescope (LCOGT) 1m;
LCOGT1m/sinistro = Sinistro imaging camera at LCOGT1m;
PEST0.3m = Perth Exoplanet Survey Telescope (PEST) 0.3m;
Swope1m/e2v = 1m SWOPE telescope with the E2V imaging camera.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Star name (HATS-31, HATS-32, HATS-33, HATS-34, or
HATS-35)
9- 18 F10.5 d BJD [6857/7231] Barycentric Julian Date (BJD-2450000)
20 A1 --- f_BJD [d] Flag "d" on BJD (not explained in the text)
22- 28 F7.2 m/s RV [-170.2/400.7] Radial velocity (1)
30- 34 F5.2 m/s e_RV [6/53] Error in RV (σRV) (2)
36- 41 F6.1 m/s BS [-147/138]? Bisector span
43- 46 F4.1 m/s e_BS [11/66]? Error in BS
48- 52 F5.3 --- Phase [0/1] Phase
54- 61 A8 --- Inst Instrument (CYCLOPS2, Coralie, FEROS, or HARPS) (3)
--------------------------------------------------------------------------------
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
considered in Section 3.3.
Note (3): The instruments are defined as follows:
HARPS = High-Accuracy Radial velocity Planetary Searcher on the European
Southern Observatory (ESO) 3.6m telescope;
CYCLOPS2 = CYCLOPS2 on the University College London Echelle Spectrograph;
Coralie = CORALIE on the Euler 1.2m telescope;
FEROS = Fiber-fed Extended Range Optical Spectrograph (FEROS) at the Max
Planck Gesellschaft (MPG) 2.2m telescope.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 17-May-2017