J/MNRAS/500/5420 Transit light curves of WASP-104b (Chen+, 2021)
An enhanced slope in the transmission spectrum of the hot Jupiter WASP-104b.
Chen G., Palle E., Parviainen H., Wang H., van Boekel R., Murgas F.,
Yan F., Bejar V.J.S., Casasayas-Barris N., Crouzet N., Esparza-Borges E.,
Fukui A., Garai Z., Kawauchi K., Kurita S., Kusakabe N., de Leon J.P.,
Livingston J., Luque R., Madrigal-Aguado A., Mori M., Narita N.,
Nishiumi T., Oshagh M., Sanchez-Benavente M., Tamura M., Terada Y.,
Watanabe N.
<Mon. Not. R. Astron. Soc. 500, 5420-5435 (2021)>
=2021MNRAS.500.5420C 2021MNRAS.500.5420C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Spectroscopy; Photometry
Keywords: techniques: photometric - techniques: spectroscopic -
planets and satellites: atmospheres -
planets and satellites: individual: WASP-104b - planetary systems
Abstract:
We present the optical transmission spectrum of the hot Jupiter
WASP-104b based on one transit observed by the blue and red channels
of the DBSP spectrograph at the Palomar 200-inch telescope and 14
transits observed by the MuSCAT2 four-channel imager at the 1.52m
Telescopio Carlos Sanchez. We also analyse 45 additional K2 transits,
after correcting for the flux contamination from a companion star.
Together with the transit light curves acquired by DBSP and MuSCAT2,
we are able to revise the system parameters and orbital ephemeris,
confirming that no transit timing variations exist. Our DBSP and
MuSCAT2 combined transmission spectrum reveals an enhanced slope at
wavelengths shorter than 630nm and suggests the presence of a cloud
deck at longer wavelengths. While the Bayesian spectral retrieval
analyses favour a hazy atmosphere, stellar spot contamination cannot
be completely ruled out. Further evidence, from transmission
spectroscopy and detailed characterisation of the host star's
activity, is required to distinguish the physical origin of the
enhanced slope.
Description:
We provide here the transit light curves of the hot Jupiter WASP-104b
obtained on the night of 2015/2/13 using the DBSP spectrograph at the
Palomar 200-inch telescope. They include one white light curve (wlc)
in the blue camera and one white light curve in the red camera, which
are also divided into spectroscopic light curves (slc) in different
wavelength bins. We also provide 49 transit light curves of WASP-104b
based on 14 transits observed using the MuSCAT2 imager at the 1.52m
TCS telescope, where the g, r, i, zs bands are denoted as 1, 2, 3, 4
in the table. All the DBSP and MuSCAT2 light curves contain time,
flux, flux uncertainty, and auxiliary information.
Objects:
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RA (2000) DE Designation(s)
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10 42 24.60 +07 26 06.3 WASP-104 = 2MASS J10422458+0726060
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tmus2.dat 93 47823 WASP-104 TCS/MuSCAT2 transit light
pbluewlc.dat 103 188 WASP-104 P200/DBSP-blue white light curve
pblueslc.dat 102 752 WASP-104 P200/DBSP-blue spectroscopic light curves
predwlc.dat 102 89 WASP-104 P200/DBSP-red white light curve
predslc.dat 104 1424 WASP-104 P200/DBSP-red spectroscopic light curves
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See also:
J/A+A/570/A64 : WASP-104b and WASP-106b photometry (Smith+, 2014)
Byte-by-byte Description of file: tmus2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 F15.7 d BJD Barycentric Julian Date (TDB standard)
17- 24 F8.6 --- Flux Relative flux
26- 33 F8.6 --- e_Flux Uncertainty of relative flux
35- 44 F10.6 pix posX Drift of star on CCD in X direction
46- 55 F10.6 pix posY Drift of star on CCD in Y direction
57- 65 F9.6 pix fwhmX Full width at half maximum in X direction
67- 75 F9.6 pix fwhmY Full width at half maximum in Y direction
77- 84 F8.6 --- Airmass Airmass during observation
86- 91 I6 --- Night Starting night
93 I1 --- Band [1/4] Band name (1)
--------------------------------------------------------------------------------
Note (1): Band name as follows:
1 = g
2 = r
3 = i
4 = zs
--------------------------------------------------------------------------------
Byte-by-byte Description of file: p*.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 F15.7 d BJD Barycentric Julian Date (TDB standard)
17- 24 F8.6 --- Flux Relative flux
26- 33 F8.6 --- e_Flux Uncertainty of relative flux
35- 43 F9.6 pix posX Drift of star on CCD in dispersion direction
45- 53 F9.6 pix posY Drift of star on CCD in spatial direction
55- 63 F9.6 pix fwhmX Relative change of full width at half
maximum of the stellar absorption line
profile
65- 72 F8.6 pix fwhmY Full width at half maximum of the stellar
spatial profile
74- 81 F8.6 --- Airmass Airmass during observation
83- 88 I6 --- Night Starting night
90- 94 F5.1 nm wave-left Wavelength at the left border
96-100 F5.1 nm wave-right Wavelength at the right border
102-104 A3 --- Band Band sequence (1)
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Note (1): Band sequence as follows:
b = 330.0-465.0nm
r = 465.0-985.0nm
b1 = 330.0-375.0nm
b2 = 375.0-405.0nm
b3 = 405.0-435.0nm
b4 = 435.0-465.0nm
r1 = 465.0-515.0nm
r2 = 515.0-545.0nm
r3 = 545.0-575.0nm
r4 = 575.0-605.0nm
r5 = 605.0-635.0nm
r6 = 635.0-665.0nm
r7 = 665.0-695.0nm
r8 = 695.0-725.0nm
r9 = 725.0-755.0nm
r10 = 755.0-785.0nm
r11 = 785.0-815.0nm
r12 = 815.0-845.0nm
r13 = 845.0-875.0nm
r14 = 875.0-905.0nm
r15 = 905.0-935.0nm
r16 = 935.0-985.0nm
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Acknowledgements:
Guo Chen, guochen(at)pmo.ac.cn
(End) Guo Chen [PMO], Patricia Vannier [CDS] 12-Nov-2020