J/AJ/148/29 Spectroscopy and differential photometry of HATS-4 (Jordan+, 2014)
HATS-4b: a dense hot Jupiter transiting a super metal-rich G star.
Jordan A., Brahm R., Bakos G.A., Bayliss D., Penev K., Hartman J.D.,
Zhou G., Mancini L., Mohler-Fischer M., Ciceri S., Sato B., Csubry Z.,
Rabus M., Suc V., Espinoza N., Bhatti W., de Val Borro M., Buchhave L.,
Csak B., Henning T., Schmidt B., Tan T.G., Noyes R.W., Beky B.,
Butler R.P., Shectman S., Crane J., Thompson I., Williams A., Martin R.,
Contreras C., Lazar J., Papp I., Sari P.
<Astron. J., 148, 29 (2014)>
=2014AJ....148...29J 2014AJ....148...29J
ADC_Keywords: Planets ; Stars, double and multiple ; Photometry ;
Radial velocities
Keywords: planetary systems - stars: individual: ({HATS-4,GSC 6505-00217) -
techniques: photometric - techniques: spectroscopic
Abstract:
We report the discovery by the HATSouth survey of HATS-4b, an
extrasolar planet transiting a V=13.46mag G star. HATS-4b has a period
of P~2.5167days, mass of Mp~1.32MJup, radius of
Rp~1.02RJup, and density of
ρp=1.55±0.16g/cm3~1.24ρJup. The host star has a
mass of 1.00 M☉, a radius of 0.92 R☉, and a very high
metallicity [Fe/H]=0.43±0.08. HATS-4b is among the densest known
planets with masses between 1 and 2MJ and is thus likely to have a
significant content of heavy elements of the order of 75M⊕. In
this paper we present the data reduction, radial velocity
measurements, and stellar classification techniques adopted by the
HATSouth survey for the CORALIE spectrograph. We also detail a
technique for simultaneously estimating vsini and macroturbulence
using high resolution spectra.
Description:
The photometric measurements were obtained with the full set of six HS
units of the HATSouth project, a global network of fully automated
telescopes located at Las Campanas Observatory (LCO) in Chile (HS-1
and HS-2), at the location of the High Energy Spectroscopic Survey in
Namibia (HS-3 and HS-4), and at Siding Spring Observatory (SSO) in
Australia (HS-5 and HS-6). Each of the HATSouth units consists of four
0.18m f/2.8 Takahasi astrographs, each coupled with an Apogee U16M
Alta 4k*4k CCD camera. Observations were taken through a Sloan r
filter with HS-1 on 2009 Dec-2011 Apr, with HS-2 on 2009 Sep-2010 Sep,
with HS-3 on 2009 Dec-2011 Feb, with HS-4 on 2009 Sep-2010 Sep, with
HS-5 on 2010 Jan-2011 May, and with HS-6 on 2010 Apr-2010 Sep.
High-precision photometric follow-up of HATS-4, was performed using
four facilities: the spectral camera on the 2m Faulkes Telescope South
(FTS) at SSO with a Sloan i filter on 2012 Oct 20, the SITe3 camera on
the Swope 1m telescope at LCO with a Sloan i filter on 2012 Dec 30,
the 0.3m Perth Exoplanet Survey Telescope (PEST) with a Cousins RC
filter on 2013 Jan 21, and the Andor camera on the 0.6m Perth-Lowell
Automated Telescope at Perth Observatory, Australia, with a Sloan r
filter on 2012 Nov 09.
We obtained spectroscopic reconnaissance observations of HATS-4 on
2012 May 8 (R=3000) and on 2012 May 10-12 (R=7000) with the Wide Field
Spectrograph (WiFeS) mounted on the Australian National University
(ANU) 2.3m telescope at SSO.
Twenty-four high precision radial velocities observations were
obtained with the Planet Finder Spectrograph (PFS) mounted on the
Magellan II (Clay) 6.5m telescope at LCO. We obtained two I2-free
templates on the night of 2012 December 28 UT with a slit width of
0.3" (R=127000), while the remaining observations were taken through
an I2 cell and a slit width of 0.5" (R=76000) on the nights of 2012
December 28-31. We also observed HATS-4 with the High Dispersion
Spectrograph (HDS) mounted on the Subaru 8.2m telescope on the nights
of 2012 September 19-22, obtaining three I2-free templates and eight
spectra taken through an I2 cell. We used the KV370 filter with a
0.6''*2'' slit, resulting in a resolution R=60000 and wavelength
coverage of 3500-6200Å. Finally, observations were also obtained
with the FEROS spectrograph mounted on the ESO/MPG 2.2m telescope
(with a resolution of 48000) on 2012 Aug 6, 2012 Dec 29-31, 2013 Jan
22-27, and 2013 Feb 24, 26, and with the CORALIE spectrograph mounted
on the Euler 1.2m telescope (with a resolution of 60000) in La Silla
on 2012 Aug 21-25 and 2012 Nov 6-11.
Objects:
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RA (ICRS) DE Designation(s) (Period)
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06 16 26.90 -22 32 48.8 HATS-4 = GSC 06505-00217 (P=2.516729)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 52 54 Relative radial velocities and bisector span
measurements of HATS-4
table4.dat 49 33495 Differential photometry of HATS-4
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See also:
J/A+A/558/A55 : HATS-2b griz light curves (Mohler-Fischer+, 2013)
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/AJ/145/5 : Follow-up photometry of HATS-1 (Penev+, 2013)
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: table3.dat
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Bytes Format Units Label Explanations
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1- 10 F10.5 d BJD Barycentric Julian Date (BJD-2454000)
12 A1 --- f_BJD [cd] Flag about observations (1)
14- 20 F7.2 m/s RV [-206.68/327.34]? Radial velocity (2)
22- 27 F6.2 m/s e_RV ? 1σ uncertainty in RV (3)
29- 33 F5.1 m/s BS ? Bissector span measurement
35- 38 F4.1 m/s e_BS ? 1σ uncertainty in BS
40- 44 F5.3 --- Phase [0/1] Phase
46- 52 A7 --- Inst Instrument (4)
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Note (1): Flag as follows:
c = These HDS observations were taken without the iodine cell to be used as a
template. RVs are not measured for these observations, but BS values are
measured.
d = These observations were obtained in transit and were excluded from our
joint-fit analysis.
Note (2): The zero point of these velocities is arbitrary. An overall offset
γrel fitted separately to the CORALIE and HDS velocities in
Section 3 has been subtracted.
Note (3): Internal errors excluding the component of astrophysical/instrumental
jitter considered in Section 3.
Note (4): Instruments used are defined as follows:
Coralie = CORALIE spectrograph (mounted on the Euler 1.2m telescope in
La Silla);
FEROS = FEROS spectrograph (mounted on the ESO/MPG 2.2m telescope);
HDS = High Dispersion Spectrograph (mounted on the Subaru telescope);
PFS = Planet Finder Spectrograph (mounted on the Magellan II (Clay)
telescope at Las Campanas Observatory in Chile.
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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- 11 F11.5 d BJD Barycentric Julian Date (BJD-2400000)
13- 20 F8.5 mag dmag Differential detrended magnitude (1)
22- 28 F7.5 mag e_dmag Estimated error in mag
30- 37 F8.5 mag Omag ? Original magnitude (2)
39 A1 --- Flt [Rir] Filter used (Sloan r, Sloan i, Cousins RC)
41- 49 A9 --- Inst Instrument used (3)
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Note (1): The out-of-transit level has been subtracted. For the HATSouth light
curve, these magnitudes have been detrended using the External Parameter
Decorrelation (EPD) and Trend Filtering Algorithm (TFA; for a description
of these procedures, see the Appendix in Bakos et al. 2010,
cat. J/ApJ/710/1724, and references therein) 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 92-100% that of the true depth, depending on
the field+detector combination). For the follow-up light curves (rows with
Inst 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 application of the EPD procedure. This
is only reported for the follow-up light curves.
Note (3): Instruments used are defined as follows:
HS = HATSouth project;
FTS = The Spectral camera on the 2m Faulkes Telescope South at
Siding Spring Observatory (SSO) in Australia;
PERTH0.6m = The Andor camera on the Perth 0.6m telescope;
SWOPE1m = The SITe3 camera on the Swope 1m telescope at
Las Campanas Observatory (LCO) in Chile;
TGTan0.3m = The 0.3m Perth Exoplanet Survey Telescope.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 14-Oct-2014