Bento, J.Hartman, J. D.Bakos, G. A.Bhatti, W.Csubry, Z.Penev, KaloyanBayliss, D.de Val-Borro, M.Zhou, G.Brahm, R.Espinoza, N.Rabus, M.Jordan, A.Suc, V.Ciceri, S.Sarkis, P.Henning, T.Mancini, L.Tinney, C. G.Wright, D. J.Durkan, S.Tan, T. G.Lazar, J.Papp, I.Sari, P.2019-07-262019-07-262018-03-200035-8711https://hdl.handle.net/10735.1/6752Full text access from Treasures at UT Dallas is restricted to current UTD affiliates (use the provided Link to Article). Non UTD affiliates will find the web address for this item by clicking the "Show full item record" link, copying the "dc.relation.uri" metadata and pasting it into a browser.Includes supplementary materialWe report the discovery of four transiting hot Jupiters from the HATSouth survey: HATS39b, HATS-40b, HATS-41b, and HATS-42b. These discoveries add to the growing number of transiting planets orbiting moderately bright (12.5 ≲ V ≲ 13.7) F dwarf stars on short (2-5 d) periods. The planets have similar radii, ranging from 1.33{_{0.20}^{+0.29}} R_J for HATS-41b to 1.58{_{-0.12} ^{+0.16}} R_J for HATS-40b. Their masses and bulk densities, however, span more than an order of magnitude. HATS-39b has a mass of 0.63 ± 0.13M(J), and an inflated radius of 1.57 ± 0.12 R-J, making it a good target for future transmission spectroscopic studies. HATS41b is a very massive 9.7 ± 1.6M_J planet and one of only a few hot Jupiters found to date with a mass over 5 M_J. This planet orbits the highest metallicity star ([Fe/H] = 0.470 ± 0.010) known to host a transiting planet and is also likely on an eccentric orbit. The high mass, coupled with a relatively young age (1.34{_{-0.51} ^{+0.31}} Gyr) for the host star, is a factor that may explain why this planet's orbit has not yet circularized.en©2018 The AuthorsKepler's lawsTelescopesPhotometry--TechniquesAstronomical spectroscopyStarsPlanetary systemsarticleBento, J., J. D. Hartman, G. A. Bakos, W. Bhatti, et al. 2018. "HATS-39b, HATS-40b, HATS-41b, and HATS-42b: three inflated hot Jupiters and a super-Jupiter transiting F stars." Monthly Notices of the Royal Astronomical Society 477(3): 3406-3423, doi:10.1093/mnras/sty7264773