2024A&A...692A..83P


Query : 2024A&A...692A..83P

2024A&A...692A..83P - Astronomy and Astrophysics, volume 692A83 (2024/12-1)

Detection of faculae in the transit and transmission spectrum of WASP-69b.

PETIT DIT DE LA ROCHE D.J.M., CHAKRABORTY H., LENDL M., KITZMANN D., PIETROW A.G.M., AKINSANMI B., BOFFIN H.M.J., CUBILLOS P.E., DELINE A., EHRENREICH D., FOSSATI L. and SEDAGHATI E.

Abstract (from CDS):

Context. Transmission spectroscopy is a powerful tool for understanding exoplanet atmospheres. At optical wavelengths, this technique makes it possible to infer the composition and the presence of aerosols in the atmosphere. However, unocculted stellar activity can result in contamination of atmospheric transmission spectra by introducing spurious slopes and molecular signals.
Aims. We aim to characterise the atmosphere of the transiting exoplanet WASP-69b, a hot Jupiter orbiting an active K star, and characterise the activity levels of the host star.
Methods. We obtained three nights of spectrophotometric data with the FORS2 instrument on the VLT, covering a wavelength range of 340-1100 nm. These were divided into 10 nm binned spectroscopic light curves, which were fit with a combination of Gaussian processes and parametric models to obtain a transmission spectrum. We performed retrievals on the full spectrum with combined stellar activity and planet atmosphere models.
Results. We directly detect a facula in the form of a hot-spot-crossing event in one of the transits and indirectly detect unocculted faculae through an apparently decreasing radius towards the blue end of the transmission spectrum. We determine a facula temperature of ΔT = + 644–263+427 K for the former and a stellar coverage fraction of around 30% with a temperature of ΔT = +231 ± 72 K for the latter. The planetary atmosphere is best fit with a high-altitude cloud deck at 1.4 mbar that mutes atomic and molecular features. We find indications of water and ammonia with log(H2O)=- 2.01–0.86+0.54 and log(NH3)=-3.4–5.20+0.96, respectively, and place 3σ upper limits on TiO (<10–7.65) and K (<10–7). We see a lack of evidence of Na, which we attribute to the presence of clouds.
Conclusions. The simultaneous multi-wavelength observations allow us to break the size-contrast degeneracy for facula crossings, meaning we can obtain temperatures for both the directly and indirectly detected faculae, which are consistent with each other.

Abstract Copyright: © The Authors 2024

Journal keyword(s): methods: observational - planets and satellites: atmospheres - stars: activity - planets and satellites: individual: WASP-69b

VizieR on-line data: <Available at CDS (J/A+A/692/A83): table-b.dat table-ri.dat table-z.dat>

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 HATS-2 * 11 46 57.3702458424 -22 33 46.817348148   14.53 13.62 13.40   ~ 50 1
2 HAT-P-12 PM* 13 57 33.4668726399 +43 29 36.601508739   13.851 12.766 12.428   K5 113 1
3 Kepler-45 Ro* 19 31 29.4966491088 +41 03 51.356401092     16.88 16.63   M1V 120 1
4 Kepler-71 Ro* 19 39 27.7155573840 +46 17 08.941351920       15.35   G8V 78 1
5 TYC 5187-1718-1 * 20 59 58.9759457280 -05 07 53.763623508   11.63 10.60     ~ 3 0
6 BD-05 5432b Pl 21 00 06.1968214728 -05 05 40.034944176           ~ 219 1
7 BD-05 5432 PM* 21 00 06.1968214728 -05 05 40.034944176   10.93 9.87     ~ 103 1
8 WASP-52 * 23 13 58.7576098848 +08 45 40.572305352   12.9 12.0 12.03   K2V 106 1

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