Search

Your search keyword '"Barkaoui K"' showing total 2 results
Start Over Author "Barkaoui K" Database eScholarship
2 results on '"Barkaoui K"'

1. Vetting of 384 TESS Objects of Interest with TRICERATOPS and Statistical Validation of 12 Planet Candidates

Author

Giacalone, S, Dressing, CD, Jensen, ELN, Collins, KA, Ricker, GR, Vanderspek, R, Seager, S, Winn, JN, Jenkins, JM, Barclay, T, Barkaoui, K, Cadieux, C, Charbonneau, D, Collins, KI, Conti, DM, Doyon, R, Evans, P, Ghachoui, M, Gillon, M, Guerrero, NM, Hart, R, Jehin, E, Kielkopf, JF, McLean, B, Murgas, F, Palle, E, Parviainen, H, Pozuelos, FJ, Relles, HM, Shporer, A, Socia, Q, Stockdale, C, Tan, TG, Torres, G, Twicken, JD, Waalkes, WC, and Waite, IA

Subjects
Exoplanet astronomy, Astrostatistics, Planet hosting stars, Exoplanets, astro-ph.EP, astro-ph.IM, astro-ph.SR, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We present TRICERATOPS, a new Bayesian tool that can be used to vet and validate TESS Objects of Interest (TOIs). We test the tool on 68 TOIs that have been previously confirmed as planets or rejected as astrophysical false positives. By looking in the false-positive probability (FPP)-nearby false-positive probability (NFPP) plane, we define criteria that TOIs must meet to be classified as validated planets (FPP < 0.015 and NFPP < 10-3), likely planets (FPP < 0.5 and NFPP < 10-3), and likely nearby false positives (NFPP > 10-1). We apply this procedure on 384 unclassified TOIs and statistically validate 12, classify 125 as likely planets, and classify 52 as likely nearby false positives. Of the 12 statistically validated planets, 9 are newly validated. TRICERATOPS is currently the only TESS vetting and validation tool that models transits from nearby contaminant stars in addition to the target star. We therefore encourage use of this tool to prioritize follow-up observations that confirm bona fide planets and identify false positives originating from nearby stars.

Published
2021

2. A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266

Author

Demory, B-O, Pozuelos, FJ, Chew, Y Gómez Maqueo, Sabin, L, Petrucci, R, Schroffenegger, U, Grimm, SL, Sestovic, M, Gillon, M, McCormac, J, Barkaoui, K, Benz, W, Bieryla, A, Bouchy, F, Burdanov, A, Collins, KA, de Wit, J, Dressing, CD, Garcia, LJ, Giacalone, S, Guerra, P, Haldemann, J, Heng, K, Jehin, E, Jofré, E, Kane, SR, Lillo-Box, J, Maigné, V, Mordasini, C, Morris, BM, Niraula, P, Queloz, D, Rackham, BV, Savel, AB, Soubkiou, A, Srdoc, G, Stassun, KG, Triaud, AHMJ, Zambelli, R, Ricker, G, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Calvario-Velásquez, T, Herrera, JA Franco, Colorado, E, Zepeda, EO Cadena, Figueroa, L, Watson, AM, Lugo-Ibarra, EE, Carigi, L, Guisa, G, Herrera, J, Díaz, G Sierra, Suárez, JC, Barrado, D, Batalha, NM, Benkhaldoun, Z, Chontos, A, Dai, F, Essack, Z, Ghachoui, M, Huang, CX, Huber, D, Isaacson, H, Lissauer, JJ, Morales-Calderón, M, Robertson, P, Roy, A, Twicken, JD, Vanderburg, A, and Weiss, LM

Subjects
instrumentation: detectors, planets and satellites: detection, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We report the discovery and characterisation of a super-Earth and a sub-Neptune transiting the bright (K = 8.8), quiet, and nearby (37 pc) M3V dwarf TOI-1266. We validate the planetary nature of TOI-1266 b and c using four sectors of TESS photometry and data from the newly-commissioned 1-m SAINT-EX telescope located in San Pedro Mártir (México). We also include additional ground-based follow-up photometry as well as high-resolution spectroscopy and high-angular imaging observations. The inner, larger planet has a radius of R = 2.37-0.12+0.16 R and an orbital period of 10.9 days. The outer, smaller planet has a radius of R = 1.56-0.13+0.15 R on an 18.8-day orbit. The data are found to be consistent with circular, co-planar and stable orbits that are weakly influenced by the 2:1 mean motion resonance. Our TTV analysis of the combined dataset enables model-independent constraints on the masses and eccentricities of the planets. We find planetary masses of Mp = 13.5-9.0+11.0 M (

Published
2020

Catalog

Books, media, physical & digital resources
See catalog results