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Nielsen, LD, Bouchy, F, Turner, OD, Anderson, DR, Barkaoui, K, Benkhaldoun, Z, Burdanov, A, Cameron, AC, Delrez, L, Gillon, M, Ducrot, E, Hellier, C ORCID: https://orcid.org/0000-0002-3439-1439, Jehin, E, Lendl, M, Maxted, PFL, Pepe, F, Pollacco, D, Pozuelos, FJ, Queloz, D, Ségransan, D, Smalley, B, Triaud, AHMJ, Udry, S and West, RG (2019) WASP-169, WASP-171, WASP-175, and WASP-182: three hot Jupiters and one bloated sub-Saturn mass planet discovered by WASP-South. Monthly Notices of the Royal Astronomical Society, 489 (2). 2478 -2487.

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Abstract

We present the discovery of four new giant planets from the Wide Angle Search for Planets-South (WASP-South), three hot Jupiters and one bloated sub-Saturn mass planet: WASP-169b, WASP-171b, WASP-175b, and WASP-182b. Besides the discovery photometry from WASP-South we use radial velocity measurements from CORALIE and HARPS and follow-up photometry from EulerCam, TRAPPIST-North and -South, and SPECULOOS. WASP-169b is a low-density Jupiter ($M=0.561 \pm 0.061\,M_\rm Jup, R=1.304^+0.150_-0.073\,R_\rm Jup$) orbiting a V = 12.17 F8 subgiant in a 5.611 d orbit. WASP-171b is a typical hot Jupiter ($M=1.084 \pm 0.094\,M_\rm Jup, R=0.98^+0.07_-0.04\,R_\rm Jup$, P = 3.82 d) around a V = 13.05 G0 star. We find a linear drift in the radial velocities of WASP-171 spanning 3.5 yr, indicating the possibility of an additional outer planet or stellar companion. WASP-175b is an inflated hot Jupiter (M = 0.99 ± 0.13 MJup, R = 1.208 ± 0.081 RJup, P = 3.07 d) around a V = 12.04 F7 star, which possibly is part of a binary system with a star 7.9 arcsec away. WASP-182b is a bloated sub-Saturn mass planet (M = 0.148 ± 0.011 MJup, R = 0.850 ± 0.030 RJup) around a metal-rich V = 11.98 G5 star ([Fe/H] = 0.27 ± 0.11). With an orbital period of P = 3.377 d, it sits right in the apex of the sub-Jovian desert, bordering the upper and lower edge of the desert in both the mass–period and radius–period plane. WASP-169b, WASP-175b, and WASP-182b are promising targets for atmospheric characterization through transmission spectroscopy, with expected transmission signals of 121, 150, and 264 ppm, respectively.

Item Type: Article
Additional Information: This article has been accepted for publication in the Monthly Notices of the Royal Astronomical Society © 2019, published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Subjects: Q Science > QB Astronomy > QB600 Planets. Planetology
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 24 Oct 2019 10:32
Last Modified: 24 Oct 2019 10:34
URI: https://eprints.keele.ac.uk/id/eprint/7073

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