J/AJ/155/112 Radial velocities & light curves for HATS-43-HATS-46 (Brahm+, 2018)
HATS-43b, HATS-44b, HATS-45b, and HATS-46b: four short-period transiting giant
planets in the Neptune-Jupiter mass range.
Brahm R., Hartman J.D., Jordan A., Bakos G.A., Espinoza N., Rabus M.,
Bhatti W., Penev K., Sarkis P., Suc V., Csubry Z., Bayliss D., Bento J.,
Zhou G., Mancini L., Henning T., Ciceri S., de Val-Borro M., Shectman S.,
Crane J.D., Arriagada P., Butler P., Teske J., Thompson I., Osip D.,
Diaz M., Schmidt B., Lazar J., Papp I., Sari P.
<Astron. J., 155, 112 (2018)>
=2018AJ....155..112B 2018AJ....155..112B (SIMBAD/NED BibCode)
ADC_Keywords: Exoplanets ; Stars, bright ; Stars, dwarfs ; Radial velocities ;
Photometry, SDSS
Keywords: planetary systems -
stars: individual (HATS-43, HATS-44, HATS-45, HATS-46)
Abstract:
We report the discovery of four short-period extrasolar planets transiting
moderately bright stars from photometric measurements of the HATSouth
network coupled to additional spectroscopic and photometric follow-up
observations. While the planet masses range from 0.26 to 0.90 MJ, the
radii are all approximately a Jupiter radii, resulting in a wide range
of bulk densities. The orbital period of the planets ranges from 2.7 days
to 4.7 days, with HATS-43b having an orbit that appears to be marginally
non-circular (e=0.173±0.089). HATS-44 is notable for having a high
metallicity ([Fe/H]=0.320±0.071). The host stars spectral types range
from late F to early K, and all of them are moderately bright
(13.3<V<14.4), allowing the execution of future detailed follow-up
observations. HATS-43b and HATS-46b, with expected transmission signals of
2350 ppm and 1500 ppm, respectively, are particularly well suited targets
for atmospheric characterization via transmission spectroscopy.
Description:
The discovery of the periodic planetary-like photometric signals for
the four systems presented in this study were obtained from the images
registered by the three stations of the HATSouth network (the HS1 and
HS2 instruments in Chile, HS3 and HS4 in Namibia, and HS5 and HS6 in
Australia). Observations were performed with a typical cadence of
5 minutes using a Sloan r photometric filter. The original images were
reduced to photometric light curves by following the procedures
described in Penev et al. (2013, J/AJ/145/5).
Precision radial velocities are required to confirm the planetary nature
of a transiting companion by providing the means to estimate its mass
and orbital parameters. For this purpose, we used the FEROS spectrograph
(Kaufer & Pasquini 1998SPIE.3355..844K 1998SPIE.3355..844K) installed at the MPG 2.2 m
telescope. HATS-43 and HATS-45 were observed with the HARPS instrument
(Mayor et al. 2003Msngr.114...20M 2003Msngr.114...20M) mounted on the ESO 3.6 m telescope,
which is located at the ESO La Silla Observatory. Finally, HATS-46 was
observed with the Planet Finder Spectrograph (PFS; Crane et al.
2010SPIE.7735E..53C 2010SPIE.7735E..53C) mounted on the Magellan/Clay 6.5 m telescope at
Las Campanas Observatory.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 41 4 List of stars
table6.dat 56 83 Relative radial velocities and bisector spans
for HATS-43-HATS-46
table7.dat 59 71227 Light curve data for HATS-43-HATS-46
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See also:
J/AJ/145/5 : Follow-up photometry of HATS-1 (Penev+, 2013)
J/AJ/155/79 : RV + light curves data for 4 G-type dwarf stars (Henning+, 2018)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- ID Object identifier (HATS-43, HATS-44, HATS-45 or
HATS-46)
9- 10 I2 h RAh Hour of Right Ascension (J2000) (1)
12- 13 I2 min RAm Minute of Right Ascension (J2000) (1)
15- 19 F5.2 s RAs Second of Right Ascension (J2000) (1)
21 A1 --- DE- Sign of the Declination (J2000) (1)
22- 23 I2 deg DEd Degree of Declination (J2000) (1)
25- 26 I2 arcmin DEm Arcminute of Declination (J2000) (1)
28- 31 F4.1 arcsec DEs Arcsecond of Declination (J2000) (1)
33- 41 F9.7 d Per [2.7439/4.7423729] Orbital period (2)
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Note (1): Values taken from Table 3 of this paper.
Note (2): Values taken from Table 4 of this paper.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Object identifier (HATS-43, HATS-44, HATS-45 or
HATS-46)
9- 18 F10.5 d BJD [7030.85/7742.78] Barycentric Julian Date
(BJD-2450000)
20- 26 F7.2 m/s RV [-147.7/105.1]? Radial velocity (1)
28- 32 F5.2 m/s e_RV [7.76/60]? Uncertainty in RV (2)
34- 39 F6.1 m/s BS [-199/227]? Bisector span
41- 44 F4.1 m/s e_BS [12/37]? Uncertainty in BS
46- 50 F5.3 --- Phase [0.014/0.967] Phase
52- 56 A5 --- Inst Instrument used
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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.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Object identifier (HATS-43, HATS-44, HATS-45 or
HATS-46)
9- 21 F13.5 d BJD Barycentric Julian Date (UTC) (1)
23- 30 F8.5 mag mag [-0.06372/0.05217] Out-of-transit subtracted
magnitude in Filter (2)
32- 38 F7.5 mag e_mag [0/0.02973] The 1σ error in mag
40- 47 F8.5 mag Omag [-0.024/13.218]? Original magnitude in Filter (3)
49 A1 --- Filter [gri] Filter used
51- 59 A9 --- Inst Instrument used
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Note (1): Computed directly from the UTC time without correction for leap
seconds.
Note (2): 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 Table 4. 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 up to three 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 seeing. These are only reported for
the follow-up observations.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 29-Oct-2018