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1. TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star

Author

Hobson, MJ, Jordán, A, Bryant, EM, Brahm, R, Bayliss, D, Hartman, JD, Bakos, GI, Henning, T, Almenara, JM, Barkaoui, K, Benkhaldoun, Z, Bonfils, X, Bouchy, F, Charbonneau, D, Cointepas, M, Collins, KA, Eastman, JD, Ghachoui, M, Gillon, M, Goeke, RF, Horne, K, Irwin, JM, Jehin, E, Jenkins, JM, Latham, DW, Moldovan, D, Murgas, F, Pozuelos, FJ, Ricker, GR, Schwarz, RP, Seager, S, Srdoc, G, Striegel, S, Timmermans, M, Vanderburg, A, Vanderspek, R, Winn, JN, Hobson, MJ [0000-0002-5945-7975], Jordán, A [0000-0002-5389-3944], Bryant, EM [0000-0001-7904-4441], Brahm, R [0000-0002-9158-7315], Bayliss, D [0000-0001-6023-1335], Hartman, JD [0000-0001-8732-6166], Bakos, GI [0000-0001-7204-6727], Henning, T [0000-0002-1493-300X], Almenara, JM [0000-0003-3208-9815], Barkaoui, K [0000-0003-1464-9276], Benkhaldoun, Z [0000-0001-6285-9847], Bonfils, X [0000-0001-9003-8894], Bouchy, F [0000-0002-7613-393X], Charbonneau, D [0000-0002-9003-484X], Collins, KA [0000-0001-6588-9574], Eastman, JD [0000-0003-3773-5142], Ghachoui, M [0000-0003-3986-0297], Gillon, M [0000-0003-1462-7739], Horne, K [0000-0003-1728-0304], Jehin, E [0000-0001-8923-488X], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Murgas, F [0000-0001-9087-1245], Pozuelos, FJ [0000-0003-1572-7707], Ricker, GR [0000-0003-2058-6662], Schwarz, RP [0000-0001-8227-1020], Seager, S [0000-0002-6892-6948], Vanderburg, A [0000-0001-7246-5438], Vanderspek, R [0000-0001-6763-6562], Winn, JN [0000-0002-4265-047X], Apollo - University of Cambridge Repository, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, 5101 Astronomical Sciences, MCP, FOS: Physical sciences, Astronomy and Astrophysics, 3rd-DAS, 5109 Space Sciences, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M-dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry, and confirmed with radial velocities from ESPRESSO, and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of $\mathrm{0.665\pm0.025\,M_J}$ and a radius of $\mathrm{1.017\pm0.044\,R_J}$. It orbits close to its host star, with an orbital period of $\mathrm{2.5926\,d}$, but has an equilibrium temperature of $\mathrm{\approx 604 \, K}$, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of $\mathrm{0.3939\pm0.0030\,M_\odot}$, a radius of $\mathrm{0.3697\pm0.0018\,R_\odot}$, an effective temperature of $\mathrm{3389 \, K}$, and a J-band magnitude of $\mathrm{11.706\pm0.025}$. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M-dwarfs for atmospheric characterization., 15 pages, 4 figures. Accepted for publication in APJL

Published
2023

3. Toi-1235 b: A keystone super-earth for testing radius valley emergence models around early m dwarfs

Author

Cloutier, R, Rodriguez, JE, Irwin, J, Charbonneau, D, Stassun, KG, Mortier, A, Latham, DW, Isaacson, H, Howard, AW, Udry, S, Wilson, TG, Watson, CA, Pinamonti, M, Lienhard, F, Giacobbe, P, Guerra, P, Collins, KA, Beiryla, A, Esquerdo, GA, Matthews, E, Matson, RA, Howell, SB, Furlan, E, Crossfield, IJM, Winters, JG, Nava, C, Ment, K, Lopez, ED, Ricker, G, Vanderspek, R, Seager, S, Jenkins, JM, Ting, EB, Tenenbaum, P, Sozzetti, A, Sha, L, Ségransan, D, Schlieder, JE, Sasselov, D, Roy, A, Robertson, P, Rice, K, Poretti, E, Piotto, G, Phillips, D, Pepper, J, Pepe, F, Molinari, E, Mocnik, T, Micela, G, Mayor, M, Martinez Fiorenzano, AF, Mallia, F, Lubin, J, Lovis, C, López-Morales, M, Kosiarek, MR, Kielkopf, JF, Kane, Jensen, ELN, Isopi, G, Huber, D, Hill, ML, Harutyunyan, A, Gonzales, E, Giacalone, S, Ghedina, A, Ercolino, A, Dumusque, X, Dressing, CD, Damasso, M, Dalba, PA, Cosentino, R, Conti, DM, Colón, KD, Collins, KI, Cameron, AC, Ciardi, D, Christiansen, J, Chontos, A, Cecconi, M, Caldwell, DA, Burke, C, Buchhave, L, Beichman, C, Behmard, A, Beard, C, Akana Murphy, JM, Cloutier, R [0000-0001-5383-9393], Rodriguez, JE [0000-0001-8812-0565], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Mortier, A [0000-0001-7254-4363], Latham, DW [0000-0001-9911-7388], Isaacson, H [0000-0002-0531-1073], Howard, AW [0000-0001-8638-0320], Udry, S [0000-0001-7576-6236], Collins, KA [0000-0001-6588-9574], Beiryla, A [0000-0001-6637-5401], Esquerdo, GA [0000-0002-9789-5474], Matthews, E [0000-0003-0593-1560], Matson, RA [0000-0001-7233-7508], Howell, SB [0000-0002-2532-2853], Winters, JG [0000-0001-6031-9513], Nava, C [0000-0001-8838-3883], Ment, K [0000-0001-5847-9147], Ricker, G [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Ting, EB [0000-0002-8219-9505], Tenenbaum, P [0000-0002-1949-4720], Sozzetti, A [0000-0002-7504-365X], Sha, L [0000-0001-5401-8079], Ségransan, D [0000-0003-2355-8034], Schlieder, JE [0000-0001-5347-7062], Sasselov, D [0000-0001-7014-1771], Roy, A [0000-0001-8127-5775], Robertson, P [0000-0003-0149-9678], Poretti, E [0000-0003-1200-0473], Piotto, G [0000-0002-9937-6387], Pepper, J [0000-0002-3827-8417], Molinari, E [0000-0002-1742-7735], Mocnik, T [0000-0003-4603-556X], Micela, G [0000-0002-9900-4751], Lubin, J [0000-0001-8342-7736], López-Morales, M [0000-0003-3204-8183], Kielkopf, JF [0000-0003-0497-2651], Kane, SR [0000-0002-7084-0529], Jensen, ELN [0000-0002-4625-7333], Huber, D [0000-0001-8832-4488], Hill, ML [0000-0002-0139-4756], Giacalone, S [0000-0002-8965-3969], Ghedina, A [0000-0003-4702-5152], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Dalba, PA [0000-0002-4297-5506], Cosentino, R [0000-0003-1784-1431], Conti, DM [0000-0003-2239-0567], Colón, KD [0000-0001-8020-7121], Collins, KI [0000-0003-2781-3207], Ciardi, D [0000-0002-5741-3047], Christiansen, J [0000-0002-8035-4778], Chontos, A [0000-0003-1125-2564], Caldwell, DA [0000-0003-1963-9616], Burke, C [0000-0002-7754-9486], Buchhave, L [0000-0003-1605-5666], Behmard, A [0000-0003-0012-9093], Beard, C [0000-0001-7708-2364], Akana Murphy, JM [0000-0001-8898-8284], and Apollo - University of Cambridge Repository

Subjects
Radial velocity, Exoplanet formation, Transit photometry, M dwarf stars, Exoplanet structure
Abstract

Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally-driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/non-rocky transition in period-radius space. Here we present the confirmation of TOI-1235 b ($P=3.44$ days, $r_p=1.738^{+0.087}_{-0.076}$ R$_{\oplus}$), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/non-rocky transition around early M dwarfs ($R_s=0.630\pm 0.015$ R$_{\odot}$, $M_s=0.640\pm 0.016$ M$_{\odot}$). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial-velocities from HARPS-N and HIRES. We measure a planet mass of $6.91^{+0.75}_{-0.85}$ M$_{\oplus}$ which implies an iron core mass fraction of $20^{+15}_{-12}$% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like and we constrain a H/He envelope mass fraction to be $

Published
2020

4. A dearth of small particles in the transiting material around the white dwarfWD 1145+017

Author

Xu, S, Rappaport, S, Van Lieshout, R, Vanderburg, A, Gary, B, Hallakoun, N, Ivanov, VD, Wyatt, MC, DeVore, J, Bayliss, D, Bento, J, Bieryla, A, Cameron, A, Cann, JM, Croll, B, Collins, KA, Dalba, PA, Debes, J, Doyle, D, Dufour, P, Ely, J, Espinoza, N, Joner, MD, Jura, M, Kaye, T, McClain, JL, Muirhead, P, Palle, E, Panka, PA, Provencal, J, Randall, S, Rodriguez, JE, Scarborough, J, Sefako, R, Shporer, A, Strickland, W, Zhou, G, Zuckerman, B, Wyatt, Mark [0000-0001-9064-5598], and Apollo - University of Cambridge Repository

Subjects
stars: individual: WD 1145+017, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, minor planets, asteroids: general, eclipses, Astrophysics::Galaxy Astrophysics, white dwarfs
Abstract

White dwarf WD 1145+017 is orbited by several clouds of dust, possibly emanating from actively disintegrating bodies. These dust clouds reveal themselves through deep, broad, and evolving transits in the star's light curve. Here, we report two epochs of multi-wavelength photometric observations of WD 1145+017, including several filters in the optical, K$_\mathrm{s}$ and 4.5 $\mu$m bands in 2016 and 2017. The observed transit depths are different at these wavelengths. However, after correcting for excess dust emission at K$_\mathrm{s}$ and 4.5 $\mu$m, we find the transit depths for the white dwarf itself are the same at all wavelengths, at least to within the observational uncertainties of $\sim$5%-10%. From this surprising result, and under the assumption of low optical depth dust clouds, we conclude that there is a deficit of small particles (with radii $s \lesssim$ 1.5 $\mu$m) in the transiting material. We propose a model wherein only large particles can survive the high equilibrium temperature environment corresponding to 4.5 hr orbital periods around WD 1145+017, while small particles sublimate rapidly. In addition, we evaluate dust models that are permitted by our measurements of infrared emission.

Published
2018

5. ChAd63-MVA–vectored Blood-stage Malaria Vaccines Targeting MSP1 and AMA1: Assessment of Efficacy Against Mosquito Bite Challenge in Humans

Author

Sheehy, SH, Duncan, CJ, Elias, SC, Choudhary, P, Biswas, S, Halstead, FD, Collins, KA, Edwards, NJ, Douglas, AD, Anagnostou, NA, Ewer, KJ, Havelock, T, Mahungu, T, Bliss, CM, Miura, K, Poulton, ID, Lillie, PJ, Antrobus, RD, Berrie, E, Moyle, S, Gantlett, K, Colloca, S, Cortese, R, Long, CA, Sinden, RE, Gilbert, SC, Lawrie, AM, Doherty, T, Faust, SN, Nicosia, A, Hill, AV, Draper, SJ, Sheehy, Sh, Duncan, Cj, Elias, Sc, Choudhary, P, Biswas, S, Halstead, Fd, Collins, Ka, Edwards, Nj, Douglas, Ad, Anagnostou, Na, Ewer, Kj, Havelock, T, Mahungu, T, Bliss, Cm, Miura, K, Poulton, Id, Lillie, Pj, Antrobus, Rd, Berrie, E, Moyle, S, Gantlett, K, Colloca, S, Cortese, R, Long, Ca, Sinden, Re, Gilbert, Sc, Lawrie, Am, Doherty, T, Faust, Sn, Nicosia, Alfredo, Hill, Av, and Draper, Sj

Subjects
Pharmacology, MEROZOITE SURFACE PROTEIN-1, PLASMODIUM-FALCIPARUM, POLYMERASE-CHAIN-REACTION, IMMUNE-RESPONSES, IN-VITRO, PARASITE GROWTH, ANTIBODY, parasitic diseases, Drug Discovery, T-CELLS, Genetics, Molecular Medicine, PROTECTION, APICAL MEMBRANE ANTIGEN-1, Molecular Biology
Abstract

The induction of cellular immunity, in conjunction with antibodies, may be essential for vaccines to protect against blood-stage infection with the human malaria parasite Plasmodium falciparum. We have shown that prime-boost delivery of P. falciparum blood-stage antigens by chimpanzee adenovirus 63 (ChAd63) followed by the attenuated orthopoxvirus MVA is safe and immunogenic in healthy adults. Here, we report on vaccine efficacy against controlled human malaria infection delivered by mosquito bites. The blood-stage malaria vaccines were administered alone, or together (MSP1+AMA1), or with a pre-erythrocytic malaria vaccine candidate (MSP1+ME-TRAP). In this first human use of coadministered ChAd63-MVA regimes, we demonstrate immune interference whereby responses against merozoite surface protein 1 (MSP1) are dominant over apical membrane antigen 1 (AMA1) and ME-TRAP. We also show that induction of strong cellular immunity against MSP1 and AMA1 is safe, but does not impact on parasite growth rates in the blood. In a subset of vaccinated volunteers, a delay in time to diagnosis was observed and sterilizing protection was observed in one volunteer coimmunized with MSP1+AMA1-results consistent with vaccine-induced pre-erythrocytic, rather than blood-stage, immunity. These data call into question the utility of T cell-inducing blood-stage malaria vaccines and suggest that the focus should remain on high-titer antibody induction against susceptible antigen targets.

Published
2012
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6. Angiotropic large cell lymphoma

Author

Collins Ka and Davis Gj

Subjects
Male, Pathology, medicine.medical_specialty, Autopsy, Diagnosis, Differential, Fatal Outcome, Medicine, Humans, Fever of unknown origin, medicine.diagnostic_test, business.industry, Brain biopsy, Cytogenetics, Brain, General Medicine, Middle Aged, medicine.disease, Neoplastic Cells, Circulating, Capillaries, Lymphatic system, Dyspnea, Spinal Cord, Infarction, Skin biopsy, Immunohistochemistry, Lymphoma, Large B-Cell, Diffuse, business, Pulmonary Embolism, Infiltration (medical)
Abstract

Lymphomas are malignant neoplasms of cells native to lymphoid tissue that can arise anywhere in the body. Angiotropic large cell lymphoma (ALCL) is characterized by a proliferation of neoplastic mononuclear cells within the lumina of small blood vessels. The clinical manifestations are usually neurologic, including progressive dementia and nonlocalizing deficits, cutaneous infiltration, adrenal masses, or fever of unknown origin. The diagnosis is made at autopsy or on skin biopsy, brain biopsy, or other surgical resection. Differential diagnoses include metastatic malignant neoplasms and vascular tumors. We report the case of a 63-year-old white man who had neurologic signs and symptoms as well as dyspnea. Autopsy revealed ALCL involving multiple organ systems, including the central nervous system. Diagnostic techniques currently used to confirm the nature of this malignant neoplasm include immunohistochemistry, ultrastructural analysis, cytogenetics, and molecular biologic studies.

Published
1995

7. An ultrahot Neptune in the Neptune desert

Author

Jenkins, JS, Díaz, MR, Kurtovic, NT, Espinoza, N, Vines, JI, Rojas, PAP, Brahm, R, Torres, P, Cortés-Zuleta, P, Soto, MG, Lopez, ED, King, GW, Wheatley, PJ, Winn, JN, Ciardi, DR, Ricker, G, Vanderspek, R, Latham, DW, Seager, S, Jenkins, JM, Beichman, CA, Bieryla, A, Burke, CJ, Christiansen, JL, Henze, CE, Klaus, TC, McCauliff, S, Mori, M, Narita, N, Nishiumi, T, Tamura, M, De Leon, JP, Quinn, SN, Villaseñor, JN, Vezie, M, Lissauer, JJ, Collins, KA, Collins, KI, Isopi, G, Mallia, F, Ercolino, A, Petrovich, C, Jordán, A, Acton, JS, Armstrong, DJ, Bayliss, D, Bouchy, F, Belardi, C, Bryant, EM, Burleigh, MR, Cabrera, J, Casewell, SL, Chaushev, A, Cooke, BF, Eigmüller, P, Erikson, A, Foxell, E, Gänsicke, BT, Gill, S, Gillen, E, Günther, MN, Goad, MR, Hooton, MJ, Jackman, JAG, Louden, T, McCormac, J, Moyano, M, Nielsen, LD, Pollacco, D, Queloz, D, Rauer, H, Raynard, L, Smith, AMS, Tilbrook, RH, Titz-Weider, R, Turner, O, Udry, S, Walker, Watson, CA, West, RG, Palle, E, Ziegler, C, Law, N, and Mann, AW

Subjects
astro-ph.SR, 13. Climate action, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters, with sizes above 10 Earth radii (Re), or apparently rocky planets smaller than 2 Re. Such lack of planets of intermediate size (the "hot Neptune desert") has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here, we report the discovery of an ultra-short-period planet with a radius of 4.6 Re and a mass of 29 Me, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite (Ricker et al. 2015) revealed transits of the bright Sun-like star \starname\, every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0^(+2.7)_(-2.9)% of the total mass. With an equilibrium temperature around 2000 K, it is unclear how this "ultra-hot Neptune" managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag=9.8).

8. TOI-4010: A System of Three Large Short-Period Planets With a Massive Long-Period Companion

Author

Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., Rose, Mark E., Kunimoto, M [0000-0001-9269-8060], Vanderburg, A [0000-0001-7246-5438], Huang, CX [0000-0003-0918-7484], Davis, MR [0000-0002-7451-4704], Affer, L [0000-0001-5600-3778], Cameron, AC [0000-0002-8863-7828], Charbonneau, D [0000-0002-9003-484X], Cosentino, R [0000-0003-1784-1431], Damasso, M [0000-0001-9984-4278], Dumusque, X [0000-0002-9332-2011], Fiorenzano, AFM [0000-0002-4272-4272], Ghedina, A [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Lienhard, F [0000-0003-4047-0771], López-Morales, M [0000-0003-3204-8183], Mayor, M [0000-0002-9352-5935], Pepe, F [0000-0002-9815-773X], Pinamonti, M [0000-0002-4445-1845], Poretti, E [0000-0003-1200-0473], Maldonado, J [0000-0002-2218-5689], Rice, K [0000-0002-6379-9185], Sozzetti, A [0000-0002-7504-365X], Wilson, TG [0000-0001-8749-1962], Udry, S [0000-0001-7576-6236], Baptista, J [0000-0002-9306-1704], Barkaoui, K [0000-0003-1464-9276], Becker, J [0000-0002-7733-4522], Benni, P [0000-0001-6981-8722], Bieryla, A [0000-0001-6637-5401], Bosch-Cabot, P [0000-0002-1514-5558], Ciardi, DR [0000-0002-5741-3047], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Dupuy, TJ [0000-0001-9823-1445], Goliguzova, MV [0000-0003-2228-7914], Guerra, P [0000-0002-4308-2339], Kraus, A [0000-0001-9811-568X], Lissauer, JJ [0000-0001-6513-1659], Huber, D [0000-0001-8832-4488], Murgas, F [0000-0001-9087-1245], Palle, E [0000-0003-0987-1593], Quinn, SN [0000-0002-8964-8377], Safonov, BS [0000-0003-1713-3208], Schwarz, RP [0000-0001-8227-1020], Shporer, A [0000-0002-1836-3120], Stassun, KG [0000-0002-3481-9052], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Ricker, GR [0000-0003-2058-6662], Seager, S [0000-0002-6892-6948], Vanderspek, R [0000-0001-6763-6562], Winn, J [0000-0002-4265-047X], Essack, Z [0000-0002-2482-0180], Lewis, HM [0000-0002-7871-085X], Rose, ME [0000-0003-4724-745X], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCC, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Exoplanet dynamics, FOS: Physical sciences, DAS, 5109 Space Sciences, Hot Neptunes, QB Astronomy, Transit photometry, Exoplanet systems, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We report the confirmation of three exoplanets transiting TOI-4010 (TIC-352682207), a metal-rich K dwarf observed by TESS in Sectors 24, 25, 52, and 58. We confirm these planets with HARPS-N radial velocity observations and measure their masses with 8 - 12% precision. TOI-4010 b is a sub-Neptune ($P = 1.3$ days, $R_{p} = 3.02_{-0.08}^{+0.08}~R_{\oplus}$, $M_{p} = 11.00_{-1.27}^{+1.29}~M_{\oplus}$) in the hot Neptune desert, and is one of the few such planets with known companions. Meanwhile, TOI-4010 c ($P = 5.4$ days, $R_{p} = 5.93_{-0.12}^{+0.11}~R_{\oplus}$, $M_{p} = 20.31_{-2.11}^{+2.13}~M_{\oplus}$) and TOI-4010 d ($P = 14.7$ days, $R_{p} = 6.18_{-0.14}^{+0.15}~R_{\oplus}$, $M_{p} = 38.15_{-3.22}^{+3.27}~M_{\oplus}$) are similarly-sized sub-Saturns on short-period orbits. Radial velocity observations also reveal a super-Jupiter-mass companion called TOI-4010 e in a long-period, eccentric orbit ($P \sim 762$ days and $e \sim 0.26$ based on available observations). TOI-4010 is one of the few systems with multiple short-period sub-Saturns to be discovered so far., Comment: 26 pages, 16 figures, published in AJ; (v3) added missing citation

Published
2023
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9. An Ultra-Hot Neptune in the Neptune desert

Author

Todd C. Klaus, Jose I. Vines, Ruth Titz-Weider, Motohide Tamura, Jessie L. Christiansen, Samuel N. Quinn, M. G. Soto, J. Villasenor, Pablo Rojas, George R. Ricker, Simon R. Walker, Maximiliano Moyano, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Andrés Jordán, Juan Cabrera, Pascal Torres, Michael R. Goad, Jerome de Leon, Giovanni Isopi, David R. Ciardi, Daniel Bayliss, K. I. Collins, Peter J. Wheatley, Jack J. Lissauer, Norio Narita, David W. Latham, François Bouchy, Sarah L. Casewell, Oliver Turner, Mayuko Mori, Andrea Ercolino, Cristobal Petrovich, Richard G. West, E. Foxell, Claudia Belardi, Philipp Eigmüller, James McCormac, Tom Louden, Eric D. Lopez, Liam Raynard, Benjamin F. Cooke, Edward Gillen, George W. King, Allyson Bieryla, Karen A. Collins, Matias Diaz, Heike Rauer, David J. Armstrong, Jack S. Acton, James A. G. Jackman, Don Pollacco, Anders Erikson, Néstor Espinoza, Michael Vezie, Samuel Gill, Nicholas M. Law, Carl Ziegler, Jon M. Jenkins, Edward M. Bryant, Rafael Brahm, Alexis M. S. Smith, Charles Beichman, Boris T. Gänsicke, Roland Vanderspek, Andrew W. Mann, Taku Nishiumi, Pía Cortés-Zuleta, Didier Queloz, Rosanna H. Tilbrook, Matthew J. Hooton, Louise D. Nielsen, Joshua N. Winn, Christopher J. Burke, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, James S. Jenkins, Christopher E. Henze, Stéphane Udry, F. Mallia, Christopher A. Watson, Jenkins, JS [0000-0003-2733-8725], Espinoza, N [0000-0001-9513-1449], Brahm, R [0000-0002-9158-7315], Cortés-Zuleta, P [0000-0002-6174-4666], Wheatley, PJ [0000-0003-1452-2240], Winn, JN [0000-0002-4265-047X], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Bieryla, A [0000-0001-6637-5401], Christiansen, JL [0000-0002-8035-4778], Mori, M [0000-0003-1368-6593], Narita, N [0000-0001-8511-2981], Nishiumi, T [0000-0003-1510-8981], Tamura, M [0000-0002-6510-0681], Lissauer, JJ [0000-0001-6513-1659], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Armstrong, DJ [0000-0002-5080-4117], Bayliss, D [0000-0001-6023-1335], Cabrera, J [0000-0001-6653-5487], Casewell, SL [0000-0003-2478-0120], Eigmüller, P [0000-0003-4096-0594], Günther, MN [0000-0002-3164-9086], Hooton, MJ [0000-0003-0030-332X], Queloz, D [0000-0002-3012-0316], Smith, AMS [0000-0002-2386-4341], Udry, S [0000-0001-7576-6236], Watson, CA [0000-0002-9718-3266], West, RG [0000-0001-6604-5533], and Apollo - University of Cambridge Repository

Subjects
Extrasolare Planeten und Atmosphären, Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, 010504 meteorology & atmospheric sciences, Leitungsbereich PF, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Northern ireland, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Political science, 0103 physical sciences, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Research center, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract

About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters, with sizes above 10 Earth radii (Re), or apparently rocky planets smaller than 2 Re. Such lack of planets of intermediate size (the "hot Neptune desert") has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here, we report the discovery of an ultra-short-period planet with a radius of 4.6 Re and a mass of 29 Me, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite (Ricker et al. 2015) revealed transits of the bright Sun-like star \starname\, every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0^(+2.7)_(-2.9)% of the total mass. With an equilibrium temperature around 2000 K, it is unclear how this "ultra-hot Neptune" managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag=9.8)., Comment: 26 pages, 10 figures, 3 tables. Published in Nature Astronomy (21/09/2020)

Published
2020
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10. TESS Hunt for Young and Maturing Exoplanets (THYME) III: a two-planet system in the 400 Myr Ursa Major Group

Author

Pa Chia Thao, Silvano Desidera, Elisabeth R. Newton, Ivan Terentev, Roland Vanderspek, Martti H. Kristiansen, Peter Tenenbaum, Aaron C. Rizzuto, Eric E. Mamajek, Andrew W. Mann, David W. Latham, George R. Ricker, Nezar Hazam Sallam, John P. Doty, Douglas A. Caldwell, Francesco Pepe, Joseph D. Twicken, George Zhou, Stephen R. Kane, Michael M. Aitken, Gabriel Murawski, Adam L. Kraus, Gilbert A. Esquerdo, Guillermo Torres, Markus Rabus, Sara Seager, Marshall C. Johnson, Annelies Mortier, Serena Benatti, Bob Massey, Robert Gagliano, Tom Jacobs, Ennio Poretti, Karen A. Collins, Jon M. Jenkins, Ana Glidden, Andrew Vanderburg, Steven Villanueva, Keighley Rockcliffe, Mackenna L. Wood, Thomas Barclay, Thomas G. Wilson, Jonathan L. Bush, Perry Berlind, Rosario Cosentino, Michelle L. Hill, Diana Dragomir, Christophe Lovis, Avet Harutyunyan, Mark Omohundro, Joshua N. Winn, Hans Martin Schwengeler, Samuel N. Quinn, Daryll LaCourse, University of St Andrews. School of Physics and Astronomy, Mann, AW [0000-0003-3654-1602], Johnson, MC [0000-0002-5099-8185], Vanderburg, A [0000-0001-7246-5438], Kraus, AL [0000-0001-9811-568X], Rizzuto, AC [0000-0001-9982-1332], Wood, ML [0000-0001-7336-7725], Bush, JL [0000-0002-9446-9250], Rockcliffe, K [0000-0003-1337-723X], Newton, ER [0000-0003-4150-841X], Latham, DW [0000-0001-9911-7388], Mamajek, EE [0000-0003-2008-1488], Zhou, G [0000-0002-4891-3517], Quinn, SN [0000-0002-8964-8377], Thao, PC [0000-0001-5729-6576], Benatti, S [0000-0002-4638-3495], Desidera, S [0000-0001-8613-2589], Mortier, A [0000-0001-7254-4363], Poretti, E [0000-0003-1200-0473], Wilson, TG [0000-0001-8749-1962], Kristiansen, MH [0000-0002-2607-138X], Gagliano, R [0000-0002-5665-1879], Jacobs, T [0000-0003-3988-3245], Lacourse, DM [0000-0002-8527-2114], Kane, SR [0000-0002-7084-0529], Hill, ML [0000-0002-0139-4756], Rabus, M [0000-0003-2935-7196], Esquerdo, GA [0000-0002-9789-5474], Collins, KA [0000-0001-6588-9574], Murawski, G [0000-0001-7809-1457], Sallam, NH [0000-0003-0614-2571], Aitken, MM [0000-0002-0169-0766], Massey, B [0000-0001-8879-7138], Ricker, GR [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Winn, JN [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Barclay, T [0000-0001-7139-2724], Caldwell, DA [0000-0003-1963-9616], Dragomir, D [0000-0003-2313-467X], Glidden, A [0000-0002-5322-2315], Tenenbaum, P [0000-0002-1949-4720], Torres, G [0000-0002-5286-0251], Twicken, JD [0000-0002-6778-7552], Villanueva, S [0000-0001-6213-8804], and Apollo - University of Cambridge Repository

Subjects
ComputerSystemsOrganization_COMPUTERSYSTEMIMPLEMENTATION, 010504 meteorology & atmospheric sciences, Exoplanet astronomy, Exoplanet evolution, Library science, FOS: Physical sciences, ComputerApplications_COMPUTERSINOTHERSYSTEMS, Astrophysics::Cosmology and Extragalactic Astrophysics, 5109 Space Sciences, 01 natural sciences, Transits, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Stellar rotation, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, Computer Science::Databases, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Stellar activity, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanet dynamics, Astronomy and Astrophysics, 3rd-DAS, Exoplanet, Young star clusters, Graduate research, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics::Earth and Planetary Astrophysics, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets ($, Comment: Published in AJ. Oct 19: fixed a citation issue

Published
2020
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