J/AJ/147/84 Photometry and spectroscopy of HAT-P-49 (Bieryla+, 2014)
HAT-P-49b: a 1.7 MJ planet transiting a bright 1.5 M☉ F-star.
Bieryla A., Hartman J.D., Bakos G.A., Bhatti W., Kovacs G., Boisse I.,
Latham D.W., Buchhave L.A., Csubry Z., Penev K., De Val-Borro M., Beky B.,
Falco E., Torres G., Noyes R.W., Berlind P., Calkins M.C., Esquerdo G.A.,
Lazar J., Papp I., Sari P.
<Astron. J., 147, 84 (2014)>
=2014AJ....147...84B 2014AJ....147...84B
ADC_Keywords: Planets ; Stars, double and multiple ; Stars, F-type ;
Photometry ; Radial velocities ; Spectroscopy
Keywords: planetary systems - stars: individual (HAT-P-49, HD 340099) -
techniques: photometric - techniques: spectroscopic
Abstract:
We report the discovery of the transiting extrasolar planet HAT-P-49b.
The planet transits the bright (V=10.3) slightly evolved F-star
HD340099 with a mass of 1.54M☉ and a radius of 1.83R☉.
HAT-P-49b is orbiting one of the 25 brightest stars to host a
transiting planet which makes this a favorable candidate for detailed
follow-up. This system is an especially strong target for
Rossiter-McLaughlin follow-up due to the host star's fast rotation,
16km/s. The planetary companion has a period of 2.6915 days, mass of
1.73MJ, and radius of 1.41RJ. The planetary characteristics are
consistent with that of a classical hot Jupiter but we note that this
is the fourth most massive star to host a transiting planet with both
Mp and Rp well determined.
Description:
The initial identification of HAT-P-49 as a potential transiting
planet system was based on photometric observations made with the
fully automated HATNet system. HAT-P-49 was observed between 2008
September 15 and 2009 May 19 using the HAT-7 telescope at the Fred
Lawrence Whipple Observatory (FLWO) in Arizona, and the HAT-8
telescope at Mauna Kea Observatory in Hawaii. Observations were made
through a Sloan r band-filter.
The new planet orbiting HD 340099 was confirmed with photometry and
spectroscopy. Spectroscopic observations were made with the
Tillinghast Reflector Echelle Spectrograph (TRES) on the 1.5m
telescope at FLWO in Arizona and with the SOPHIE spectrograph on the
Observatoire de Haute Provence (OHP) 1.93m telescope. We conducted
additional photometric observations of HAT-P-49 using KeplerCam on the
FLWO 1.2m telescope in Arizona. We observed a transit egress in the
Sloan z band on the night of 2012 October 15, and an ingress in the
Sloan z band on the night of 2013 June 22.
Objects:
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RA (ICRS) DE Designation(s) (Period)
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20 21 45.93 +26 41 33.7 HAT-P-49 = HD 340099 (P=2.691548)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 50 4699 Differential photometry of HAT-P-49
table2.dat 60 24 Relative radial velocities, bisector span
measurements, and stellar atmospheric
parameters of HAT-P-49
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See also:
J/A+A/558/A86 : HAT-P-42b and HAT-P-43b ri light curves (Boisse+, 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/720/1118 : i-band photometry of HAT-P-16 (Buchhave+, 2010)
J/ApJ/710/1724 : Follow-up photometry for HAT-P-11 (Bakos+, 2010)
J/ApJ/704/1107 : Transiting planet in HATNet field 205 (Latham+, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 F12.5 d BJD Barycentric Julian Date (UTC; BJD-2400000) (G1)
14- 21 F8.5 mag Dmag Differential magnitude in Flt (1)
23- 29 F7.5 mag e_Dmag The 1σ error in Dmag
31- 38 F8.5 mag Dmago ? Original raw magnitude in Flt (2)
40 A1 --- Flt [rz] Filter used in observation (Sloan r, Sloan z)
42- 50 A9 --- Inst Instrument used (HATNet, Keplercam) (3)
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Note (1): The out-of-transit level has been subtracted. These magnitudes have
been subjected to the External Parameter Decorrelation (EPD; see Bakos et
al., 2010, cat. J/ApJ/710/1724) and Trend Filtering Algorithm (TFA; see
Kovacs et al., 2005MNRAS.356..557K 2005MNRAS.356..557K) procedures, carried out simultaneously
with the transit fit.
Note (2): Raw magnitude values after correction using comparison stars, but
without application of the EPD and TFA procedures. This is only reported
for the follow-up light curves.
Note (3): Instrument used in the observation are described as follows:
Keplercam = KeplerCam on the Fred Lawrence Whipple Observatory (FLWO) 1.2m
telescope in Arizona;
HATNet = HAT-7 telescope at FLWO in Arizona, and HAT-8 telescope at Mauna
Kea Observatory in Hawaii.
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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- 10 F10.5 d BJD Barycentric Julian Date (UTC; BJD-2454000) (G1)
12 A1 --- n_BJD [f] Observation obtained during transit (1)
14- 17 I4 m/s RV Radial velocity (2)
19- 20 I2 m/s e_RV The 1σ uncertainty in RV (3)
22- 24 I3 m/s BS Bissector span measurement
26- 27 I2 m/s e_BS The 1σ uncertainty in BS
29- 32 F4.1 --- S/N ? Signal-to-noise per resolution element (SNRe) (4)
34- 37 I4 K Teff ? Effective temperature (5)
39- 42 F4.2 [Sun] [Fe/H] ? Metallicity (5)
44- 47 F4.1 km/s vsini ? Rotational velocity (5)
49- 53 F5.3 --- Phase [0/1] Phase
55- 60 A6 --- Inst Instrument (SOPHIE or TRES) (6)
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Note (1): These observations were excluded from our modeling of the orbit.
Note (2): The zero point of these velocities is arbitrary. An overall offset
γrel fitted to these velocities in Section 3 has not been subtracted.
Note (3): Internal errors excluding the component of astrophysical jitter
considered in Section 3.
Note (4): The SNRe takes into account the resolution of the instrument. SNRe is
calculated near the MgB region.
Note (5): Spectroscopic parameters measured from the individual TRES spectra
using Stellar Parameter Classification (SPC) with the surface gravity fixed
to logg*=4.10±0.04 as determined from our global modeling. The
uncertainties are ∼50K, 0.08dex, and 0.5km/s on Teff, [Fe/H], and vsini,
respectively. We note that due to the rapid rotation of this star there is
some discrepancy in the stellar classification of the observations with
lower SNRe. The observations with lower SNRe have lower temperature and
higher metallicity and we found that due to the rapid rotation of the star
we needed a higher SNRe to get reliable classifications.
Note (6): Instruments used in the observation are described as follows:
SOPHIE = SOPHIE spectrograph on the Observatoire de Haute Provence (OHP)
1.93m telescope;
TRES = Tillinghast Reflector Echelle Spectrograph on the 1.5m telescope at
the Fred Lawrence Whipple Observatory (FLWO) in Arizona.
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Global notes:
Note (G1): Calculated directly from UTC, without correction for leap seconds.
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 11-Sep-2014