2022A&A...666A..47Z


Query : 2022A&A...666A..47Z

2022A&A...666A..47Z - Astronomy and Astrophysics, volume 666A, 47 (2022/10-1)

Transmission spectroscopy of the ultra-hot Jupiter MASCARA-4 b Disentangling the hydrostatic and exospheric regimes of ultra-hot Jupiters.

ZHANG Y., SNELLEN I.A.G., WYTTENBACH A., NIELSEN L.D., LENDL M., CASASAYAS-BARRIS N., CHAVEROT G., KESSELI A.Y., LOVIS C., PEPE F.A., PSARIDI A., SEIDEL J.V., UDRY S. and ULMER-MOLL S.

Abstract (from CDS):


Context. Ultra-hot Jupiters (UHJs), rendering the hottest planetary atmospheres, offer great opportunities of detailed characterisation with high-resolution spectroscopy. MASCARA-4 b is a recently discovered close-in gas giant belonging to this category.
Aims. We aim to characterise MASCARA-4 b, search for chemical species in its atmosphere, and put these in the context of the growing knowledge on the atmospheric properties of UHJs.
Methods. In order to refine system and planet parameters, we carried out radial velocity measurements and transit photometry with the CORALIE spectrograph and EulerCam at the Swiss 1.2 m Euler telescope. We observed two transits of MASCARA-4 b with the high-resolution spectrograph ESPRESSO at ESO's Very Large Telescope. We searched for atomic, ionic, and molecular species via individual absorption lines and cross-correlation techniques. These results are compared to literature studies on UHJs characterised to date.
Results. With CORALIE and EulerCam observations, we update the mass of MASCARA-4 b (Mp = 1.675 ± 0.241 MJup) as well as other system and planet parameters. In the transmission spectrum derived from ESPRESSO observations, we resolve excess absorption by Hα, Hβ, NaI D1&D2, CaII H&K, and a few strong lines of MgI, FeI, and FeII. We also present the cross-correlation detection of Mg I, CaI, Cr I, Fe I, and Fe II. The absorption strength of Fe II significantly exceeds the prediction from a hydrostatic atmospheric model, as commonly observed in other UHJs. We attribute this to the presence of Fe II in the exosphere due to hydrodynamic outflows. This is further supported by the positive correlation of absorption strengths of Fe II with the Hα line, which is expected to probe the extended upper atmosphere and the mass loss process. Comparing transmission signatures of various species in the UHJ population allows us to disentangle the hydrostatic regime (as traced via the absorption by Mg I and Fe I) from the exospheres (as probed by Hα and Fe II) of the strongly irradiated atmospheres.

Abstract Copyright: © Y. Zhang et al. 2022

Journal keyword(s): planets and satellites: atmospheres - techniques: spectroscopic

VizieR on-line data: <Available at CDS (J/A+A/666/A47): phot.dat rv.dat>

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 BD+01 316b Pl 01 46 31.8575937456 +02 42 02.030065560           ~ 207 0
2 HAT-P-70b Pl 04 58 12.5627969184 +09 59 52.804564656           ~ 36 0
3 CD-38 3220b Pl 07 10 24.0604565856 -39 05 50.571250476           ~ 298 0
4 HD 85628 * 09 50 19.2009107592 -66 06 49.897904652   8.40 8.19     A3V 20 0
5 HD 85628b Pl 09 50 19.2009107592 -66 06 49.897904652           ~ 24 0
6 WASP-189b Pl? 15 02 44.8678907928 -03 01 52.986571896           ~ 84 0
7 HD 133112 PM* 15 02 44.8678907928 -03 01 52.986571896   6.788 6.618     A4/5IV/V 60 0
8 HD 185603b Pl 19 38 38.7352230144 +31 13 09.217127532           ~ 128 0
9 HD 195689b Pl 20 31 26.3534153736 +39 56 19.773037500           ~ 279 0
10 BD+66 1610b Pl 23 29 04.2251836392 +67 02 05.378578800           ~ 14 0

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