J/AJ/152/108 i filter photometry for HATS-25 through HATS-30 (Espinoza+, 2016)
HATS-25b through HATS-30b: a half-dozen new inflated transiting hot Jupiters
from the HATSouth survey.
Espinoza N., Bayliss D., Hartman J.D., Bakos G.A., Jordan A., Zhou G.,
Mancini L., Brahm R., Ciceri S., Bhatti W., Csubry Z., Rabus M., Penev K.,
Bento J., de Val-Borro M., Henning T., Schmidt B., Suc V., Wright D.J.,
Tinney C.G., Tan T.G., Noyes R.
<Astron. J., 152, 108-108 (2016)>
=2016AJ....152..108E 2016AJ....152..108E (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Stars, double and multiple ; Radial velocities ;
Photometry, ugriz
Keywords: stars: individual: (HATS-25,HATS-26,HATS-27,HATS-28,HATS-29,HATS-30)
Abstract:
We report six new inflated hot Jupiters (HATS-25b through HATS-30b)
discovered using the HATSouth global network of automated telescopes.
The planets orbit stars with V magnitudes in the range of ∼12-14 and
have masses in the largely populated 0.5MJ--0.7MJ region of
parameter space but span a wide variety of radii, from 1.17RJ to
1.75RJ. HATS-25b, HATS-28b, HATS-29b, and HATS-30b are typical
inflated hot Jupiters (Rp=1.17--1.26RJ) orbiting G-type stars in
short period (P=3.2-4.6 days) orbits. However, HATS-26b
(Rp=1.75RJ, P=3.3024days) and HATS-27b (Rp=1.50RJ,
P=4.6370days) stand out as highly inflated planets orbiting slightly
evolved F stars just after and in the turn-off points, respectively,
which are among the least dense hot Jupiters, with densities of
0.153g/cm3 and 0.180g/cm3, respectively. All the presented
exoplanets but HATS-27b are good targets for future atmospheric
characterization studies, while HATS-27b is a prime target for
Rossiter-McLaughlin monitoring in order to determine its spin-orbit
alignment given the brightness (V=12.8) and stellar rotational
velocity (vsini∼9.3km/s) of the host star. These discoveries
significantly increase the number of inflated hot Jupiters known,
contributing to our understanding of the mechanism(s) responsible for
hot Jupiter inflation.
Description:
The photometric detection data of the six exoplanets come from the
three HATSouth sites, namely, the site at Las Campanas Observatory in
Chile (LCO, whose stations are designated HS-1 and HS-2), the site at
of the High Energy Spectroscopic Survey (HESS) in Namibia (whose
stations are designated HS-3 and HS-4) and the site at the Siding
Spring Observatory (SSO) in Australia whose stations are designated
HS-5 and HS-6).
HATS-25 was observed with an r SDSS filter on 2011 Mar-2011 Aug using
HS-2.1, on 2011 Jul-2011 Aug using HS-4.1, and on 2011 May with
HS-6.1. HATS-26 was observed with an r SDSS filter on 2012 Feb-2012
Jun using HS-2.3, HS-4.3, and HS-6.3. HATS-27 was observed with an r
SDSS filter on 2011 Apr-2012 Jul using HS-2.1, on 2011 Jul-2012 Jul
using HS-4.1, and on 2011 May-2012 Jul using HS-6.1. HATS-28 was
observed with an r SDSS filter on 2013 Mar-2013 Oct using HS-1.2, on
2013 Sep-2013 Oct using HS-2.2, on 2013 Apr-2013 Nov using HS-3.2, on
2013 Sep-2013 Nov using HS-4.2 and HS-6.2, and 2013 Mar-2013 Nov using
HS-5.2. HATS-29 was observed with an r SDSS filter on 2013 Apr-2013
May using HS-1.1, on 2013 Sep-2013 Oct using HS-2.1, on 2013
Apr-2013 Nov using HS-3.1, on 2013 Sep-2013 Nov using HS-4.1 and
HS-6.1, and on 2013 Mar-2013 Nov using HS-5.1. HATS-30 was observed
using an r SDSS filter on 2012 Sep-2012 Dec using HS-2.3, HS-6.3 and
HS-2.4, on 2012 Sep-2013 Jan using HS-4.4, on 2012 Sep-2012 Dec using
HS-6.4, and on 2011 Jul-2012 Oct using HS-1.1, HS-3.1 and HS-5.1.
Photometric follow-up for the six systems was obtained mainly from
1m-class telescopes at different sites of the Las Cumbres Observatory
Global Telescope (LCOGT) network, using the i filter. In particular,
one partial transit and a full transit was observed for HATS-25b on
2015 February 23 at Cerro Tololo Inter-American Observatory (CTIO) and
2015 March 16 at SSO, respectively; three partial transits were
observed for HATS-26b on 2015 April 19 and 2015 May 21 at CTIO, and
2015 June 04 at SSO; one full transit was observed for HATS-27b on
2015 April 09 at SSO; two partial transits were observed for HATS-28b
on 2015 August 31 and 2015 September 03 at CTIO; one full transit and
a partial transit were observed for HATS-29b on 2015 and 2014 June,
respectively, at CTIO; and two partial transits were observed for
HATS-30b on 2014 October 19 at South African Astronomical Observatory
(SAAO) and on 2014 Oct 23 at CTIO. In addition, one full transit of
HATS-27b was observed using the 0.3m Perth Exoplanet Survey Telescope
(PEST) on 2015 March 12 using a RC filter.
The reconnaissance spectroscopy of our candidates was made using the
Wide Field Spectrograph (WiFeS), located on the Australian National
University (ANU) 2.3m telescope. The observing strategy usually
consists of taking data with two resolutions:
R=λ/Δλ=7000 (medium) and R=3000 (low). For
HATS-25, four medium resolution spectra (2014 Jun-Aug) and one low
resolution spectrum (2014 Aug 5) were obtained. For HATS-26, two
medium resolution spectra (2014 Jun 3-5) and one low resolution
spectrum (2014 Jun 4) were obtained. For HATS-27, three medium
resolution (2014 Jun 3-5) and one low resolution (2014 Jun 2) spectra
were obtained. For HATS-28, only one low resolution spectrum (2015 Jun
1) was obtained. For HATS-29, four medium resolution spectra (2014
Dec-2015 Mar) and one low resolution spectrum (2015 Mar 2) were
obtained. For HATS-30, three medium resolution spectra (2014 Oct 4-10)
and one low resolution spectrum (2014 Oct 4) were obtained.
High-precision spectroscopy was obtained for our targets with
different instruments. Several R=115000 spectra were taken with the
High Accuracy Radial Velocity Planet Searcher (HARPS) on the ESO 3.6m
telescope at La Silla Observatory (LSO) between 2015 February and 2016
March in order to obtain high-precision radial velocities for HATS-25,
HATS-26, HATS-27, and HATS-29. Spectra with R=48000 were also taken
with the Fiber-fed Extended Range Optical Spectrograph (FEROS) mounted
on the Max Planck Gesellschaft (MPG) 2.2m telescope at La Silla
Observatory (LSO) between 2014 July and 2015 July in order to both
extract precise spectroscopic parameters of the host stars and obtain
precise radial velocities for all of our targets. In addition, R=60000
spectra were also taken with the CORALIE spectrograph mounted on the
1.2m Euler telescope at LSO between 2014 June and November for
HATS-26, HATS-27, HATS-29, and HATS-30. Finally, eight R=70000 spectra
were obtained for HATS-29 on 2015 May to measure radial velocities,
using the CYCLOPS2 fiber feed with the University College London
Echelle Spectrograph (UCLES) on the 3.9m Anglo-Australian Telescope
(AAT).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stars.dat 68 6 Stars observed
table3.dat 65 98275 Light curve data for HATS-25--HATS-30
table8.dat 58 98 Relative radial velocities and bisector spans
for HATS-25--HATS-30
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See also:
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/147/144 : Differential griz photometry of HATS-5 (Zhou+, 2014)
J/AJ/146/113 : Differential griz photometry of HATS-3 (Bayliss+, 2013)
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
--------------------------------------------------------------------------------
1- 7 A7 --- Name Object name
9- 24 A16 --- 2MASS 2MASS identifier
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)
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Note (1): From Table 4 or 5 in the paper (taken from 2MASS; see Cutri et al.
2003, Cat. II/246).
Note (2): From Table 6 or 7.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Object name (either HATS-25, HATS-26, HATS-27,
HATS-28, HATS-29 or HATS-30)
9- 19 F11.5 d BJD [55644/57270] UTC Barycentric Julian date
(BJD-2400000) (1)
21- 28 F8.5 mag Dmag [-0.06/12.3] Δ magnitude observed in
filter (2)
30- 36 F7.5 mag e_Dmag [0.0005/0.022] Uncertainty in mag
38- 45 F8.5 mag omag [-0.05/13.1]? Raw, observed magnitude (3)
47- 48 A2 --- Flt Filter used in the observation (RC, i, or
SDSS r)
50- 65 A16 --- Inst Instrument used in the observation (HS,
HS/G754.3, HS/G754.4, HS/G755.1, LCOGT1m/SBIG,
LCOGT1m/sinistro, or PEST03m) (4)
--------------------------------------------------------------------------------
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 "Instrument"
column) these magnitudes have been corrected for trends using the External
Parameter Decorrelation (EPD) and Trend Filtering Algorithm (TFA)
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 HATSouth 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 telescope;
PEST03m = 0.3m Perth Exoplanet Survey Telescope (PEST);
HS/G754.3 = HATSouth telescope, unit 3, Field 754 for HATS-30;
HS/G754.4 = HATSouth telescope, unit 4, Field 754 for HATS-30;
HS/G755.1 = HATSouth telescope, unit 1, Field 755 for HATS-30;
LCOGT1m/SBIG = Las Cumbres Observatory Global Telescope (LCOGT) 1m
telescope + Siding Spring Observatory (SSO)/SBIG camera;
LCOGT1m/sinistro = LCOGT 1m telescope + Cerro Tololo Inter-American
Observatory (CTIO)/sinistro camera.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Object name (either HATS-25, HATS-26, HATS-27,
HATS-28, HATS-29 or HATS-30)
9- 18 F10.5 d BJD [6828/7469] Barycentric Julian Date (BJD-2450000)
20- 26 F7.2 m/s RV [-139/225] Relative radial velocity (1)
28- 32 F5.2 m/s e_RV [7/41] Error in RV (σRV) (2)
34- 39 F6.1 m/s BS [-149/468]? Bisector span
41- 44 F4.1 m/s e_BS [10/72]? Error in BS (σBS)
46- 50 F5.3 --- Phase [0/1] Phase
52- 58 A7 --- Inst Instrument (CYCLOPS, Coralie, FEROS, or HARPS) (3)
--------------------------------------------------------------------------------
Note (1): The zero-point of these velocities is arbitrary. An overall offset of
γrel is 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 Planet Searcher (HARPS) on the
ESO 3.6m telescope at La Silla Observatory (LSO);
FEROS = Fiber-fed Extended Range Optical Spectrograph mounted on the Max
Planck Gesellschaft (MPG) 2.2m telescope at LSO;
Coralie = CORALIE spectrograph mounted on the 1.2m Euler telescope at LSO;
CYCLOPS = CYCLOPS2 fiber feed with the University College London Echelle
Spectrograph (UCLES) on the 3.9m Anglo-Australian Telescope
(AAT).
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History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 22-May-2017