|   | 
Details
   web
Records
Author Bouma, L.G.; Hartman, J.D.; Brahm, R.; Evans, P.; Collins, K.A.; Zhou, G.; Sarkis, P.; Quinn, S.N.; de Leon, J.; Livingston, J.; Bergmann, C.; Stassun, K.G.; Bhatti, W.; Winn, J.N.; Bakos, G.A.; Abe, L.; Crouzet, N.; Dransfield, G.; Guillot, T.; Marie-Sainte, W.; Mekarnia, D.; Triaud, A.H.M.J.; Tinney, C.G.; Henning, T.; Espinoza, N.; Jordan, A.; Barbieri, M.; Nandakumar, S.; Trifonov, T.; Vines, J.I.; Vuckovic, M.; Ziegler, C.; Law, N.; Mann, A.W.; Ricker, G.R.; Vanderspek, R.; Seager, S.; Jenkins, J.M.; Burke, C.J.; Dragomir, D.; Levine, A.M.; Quintana, E.V.; Rodriguez, J.E.; Smith, J.C.; Wohler, B.
Title Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602 Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 5 Pages 20 pp
Keywords
Abstract We report the discovery of TOI 837b and its validation as a transiting planet. We characterize the system using data from the NASA Transiting Exoplanet Survey Satellite mission, the ESA Gaia mission, ground-based photometry from El Sauce and ASTEP400, and spectroscopy from CHIRON, FEROS, and Veloce. We find that TOI 837 is a T = 9.9 mag G0/F9 dwarf in the southern open cluster IC 2602. The star and planet are therefore 35(-5)(+11) million years old. Combining the transit photometry with a prior on the stellar parameters derived from the cluster color-magnitude diagram, we find that the planet has an orbital period of 8.3 days and is slightly smaller than Jupiter (R-p = 0.77(0.07)(+0.09) R-Jup). From radial velocity monitoring, we limit M-p sin i to less than 1.20 M-Jup (3 sigma). The transits either graze or nearly graze the stellar limb. Grazing transits are a cause for concern, as they are often indicative of astrophysical false-positive scenarios. Our follow-up data show that such scenarios are unlikely. Our combined multicolor photometry, high-resolution imaging, and radial velocities rule out hierarchical eclipsing binary scenarios. Background eclipsing binary scenarios, though limited by speckle imaging, remain a 0.2% possibility. TOI 837b is therefore a validated adolescent exoplanet. The planetary nature of the system can be confirmed or refuted through observations of the stellar obliquity and the planetary mass. Such observations may also improve our understanding of how the physical and orbital properties of exoplanets change in time.
Address [Bouma, L. G.; Hartman, J. D.; Bhatti, W.; Winn, J. N.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08540 USA, Email: luke@astro.princeton.edu
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000585065500001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1260
Permanent link to this record
 

 
Author Brahm, R.; Nielsen, L.D.; Wittenmyer, R.A.; Wang, S.H.; Rodriguez, J.E.; Espinoza, N.; Jones, M.I.; Jordan, A.; Henning, T.; Hobson, M.; Kossakowski, D.; Rojas, F.; Sarkis, P.; Schlecker, M.; Trifonov, T.; Shahaf, S.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Addison, B.C.; Bakos, G.A.; Bhatti, W.; Bayliss, D.; Berlind, P.; Bieryla, A.; Bouchy, F.; Bowler, B.P.; Briceno, C.; Brown, T.M.; Bryant, E.M.; Caldwell, D.A.; Charbonneau, D.; Collins, K.A.; Davis, A.B.; Esquerdo, G.A.; Fulton, B.J.; Guerrero, N.M.; Henze, C.E.; Hogan, A.; Horner, J.; Huang, C.X.; Irwin, J.; Kane, S.R.; Kielkopf, J.; Mann, A.W.; Mazeh, T.; McCormac, J.; McCully, C.; Mengel, M.W.; Mireles, I.; Okumura, J.; Plavchan, P.; Quinn, S.N.; Rabus, M.; Saesen, S.; Schlieder, J.E.; Segransan, D.; Shiao, B.; Shporer, A.; Siverd, R.J.; Stassun, K.G.; Suc, V.; Tan, T.G.; Torres, P.; Tinney, C.G.; Udry, S.; Vanzi, L.; Vezie, M.; Vines, J.I.; Vuckovic, M.; Wright, D.J.; Yahalomi, D.A.; Zapata, A.; Zhang, H.; Ziegler, C.
Title TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 5 Pages 14 pp
Keywords Exoplanet detection methods; Transit photometry; Radial velocity; Exoplanet astronomy
Abstract We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481.b and TOI-892.b have similar radii (0.99.+/-.0.01 R-J and 1.07.+/-.0.02 R-J, respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53.+/-.0.03 MJ versus 0.95.+/-.0.07 MJ, respectively). Both planets orbit metal-rich stars ([Fe H] = + 0.26. 0.05 dex and [Fe H] = +0.24. 0.05 for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a M*=.1.14.+/-.0.02 M., R*=.1.66.+/-.0.02 R. G-type star (T-eff = 5735 +/- 72 K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star (T-eff = 6261 +/- 80 K), which has a mass of M*=.1.28.+/-.0.03 M-circle dot and a radius of R*=.1.39.+/-.0.02 R-circle dot. TOI-481.b and TOI-892.b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.
Address [Brahm, Rafael; Jordan, Andres; Suc, Vincent] Univ Adolfo Ibanez, Santiago, Chile, Email: rbrahm@gmail.com
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000584302400001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1263
Permanent link to this record
 

 
Author Carleo, I.; Gandolfi, D.; Barragan, O.; Livingston, J.H.; Persson, C.M.; Lam, K.W.F.; Vidotto, A.; Lund, M.B.; D'Angelo, C.V.; Collins, K.A.; Fossati, L.; Howard, A.W.; Kubyshkina, D.; Brahm, R.; Oklopcic, A.; Molliere, P.; Redfield, S.; Serrano, L.M.; Dai, F.; Fridlund, M.; Borsa, F.; Korth, J.; Esposito, M.; Diaz, M.R.; Nielsen, L.D.; Hellier, C.; Mathur, S.; Deeg, H.J.; Hatzes, A.P.; Benatti, S.; Rodler, F.; Alarcon, J.; Spina, L.; Santos, A.R.G.; Georgieva, I.; Garcia, R.A.; Gonzalez-Cuesta, L.; Ricker, G.R.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Albrecht, S.; Batalha, N.M.; Beard, C.; Boyd, P.T.; Bouchy, F.; Burt, J.A.; Butler, R.P.; Cabrera, J.; Chontos, A.; Ciardi, D.R.; Cochran, W.D.; Collins, K.I.; Crane, J.D.; Crossfield, I.; Csizmadia, S.; Dragomir, D.; Dressing, C.; Eigmuller, P.; Endl, M.; Erikson, A.; Espinoza, N.; Fausnaugh, M.; Feng, F.B.; Flowers, E.; Fulton, B.; Gonzales, E.J.; Grieves, N.; Grziwa, S.; Guenther, E.W.; Guerrero, N.M.; Henning, T.; Hidalgo, D.; Hirano, T.; Hjorth, M.; Huber, D.; Isaacson, H.; Jones, M.; Jordan, A.; Kabath, P.; Kane, S.R.; Knudstrup, E.; Lubin, J.; Luque, R.; Mireles, I.; Narita, N.; Nespral, D.; Niraula, P.; Nowak, G.; Palle, E.; Patzold, M.; Petigura, E.A.; Prieto-Arranz, J.; Rauer, H.; Robertson, P.; Rose, M.E.; Roy, A.; Sarkis, P.; Schlieder, J.E.; Segransan, D.; Shectman, S.; Skarka, M.; Smith, A.M.S.; Smith, J.C.; Stassun, K.; Teske, J.; Twicken, J.D.; Van Eylen, V.; Wang, S.R.; Weiss, L.M.; Wyttenbach, A.
Title The Multiplanet System TOI-421* Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 3 Pages 23 pp
Keywords
Abstract We report the discovery of a warm Neptune and a hot sub-Neptune transiting TOI-421 (BD-14 1137, TIC 94986319), a bright (V = 9.9) G9 dwarf star in a visual binary system observed by the Transiting Exoplanet Survey Satellite (TESS) space mission in Sectors 5 and 6. We performed ground-based follow-up observations-comprised of Las Cumbres Observatory Global Telescope transit photometry, NIRC2 adaptive optics imaging, and FIbre-fed Echelle Spectrograph, CORALIE, High Accuracy Radial velocity Planet Searcher, High Resolution echelle Spectrometer, and Planet Finder Spectrograph high-precision Doppler measurements-and confirmed the planetary nature of the 16 day transiting candidate announced by the TESS team. We discovered an additional radial velocity signal with a period of five days induced by the presence of a second planet in the system, which we also found to transit its host star. We found that the inner mini-Neptune, TOI-421 b, has an orbital period of P-b = 5.19672 +/- 0.00049 days, a mass of M-b = 7.17 +/- 0.66 M-circle plus, and a radius of R-b = R-circle plus, whereas the outer warm Neptune, TOI-421 c, has a period of P-c = 16.06819 +/- 0.00035 days, a mass of M-c = 16.42(-1.04)(+1.06)M(circle plus), a radius of R-c = 5.09(-0.15)(+0.16)R(circle plus), and a density of rho(c) = 0.685(-0.072)(+0.080) cm(-3). With its characteristics, the outer planet (rho(c) = 0.685(-0.0072)(+0.080) cm(-3)) is placed in the intriguing class of the super-puffy mini-Neptunes. TOI-421 b and TOI-421 c are found to be well-suited for atmospheric characterization. Our atmospheric simulations predict significant Ly alpha transit absorption, due to strong hydrogen escape in both planets, as well as the presence of detectable CH4 in the atmosphere of TOI-421 c if equilibrium chemistry is assumed.
Address [Carleo, Ilaria; Redfield, Seth] Wesleyan Univ, Astron Dept, Middletown, CT 06459 USA, Email: icarleo@wesleyan.edu
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000561609000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1254
Permanent link to this record
 

 
Author Carmichael, T.W.; Quinn, S.N.; Mustill, A.J.; Huang, C.; Zhou, G.; Persson, C.M.; Nielsen, L.D.; Collins, K.A.; Ziegler, C.; Collins, K.I.; Rodriguez, J.E.; Shporer, A.; Brahm, R.; Mann, A.W.; Bouchy, F.; Fridlund, M.; Stassun, K.G.; Hellier, C.; Seidel, J.V.; Stalport, M.; Udry, S.; Pepe, F.; Ireland, M.; Zerjal, M.; Briceno, C.; Law, N.; Jordan, A.; Espinoza, N.; Henning, T.; Sarkis, P.; Latham, D.W.
Title Two Intermediate-mass Transiting Brown Dwarfs from the TESS Mission Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 1 Pages 15 pp
Keywords Brown dwarfs; Radial velocity; Transit photometry; Spectroscopy; Photometry; Substellar companion stars
Abstract We report the discovery of two intermediate-mass transiting brown dwarfs (BDs), TOI-569b and TOI-1406b, from NASA's Transiting Exoplanet Survey Satellite mission. TOI-569b has an orbital period of P = 6.55604 0.00016 days, a mass of M-b = 64.1 1.9 , and a radius of R-b = 0.75 0.02 . Its host star, TOI-569, has a mass of M-star = 1.21 0.05, a radius of R-star = 1.47 0.03 dex, and an effective temperature of T-eff = 5768 110 K. TOI-1406b has an orbital period of P = 10.57415 0.00063 days, a mass of M-b = 46.0 2.7 , and a radius of R-b = 0.86 0.03 . The host star for this BD has a mass of M-star = 1.18 0.09 a radius of R-star = 1.35 0.03 dex, and an effective temperature of T-eff = 6290 100 K. Both BDs are in circular orbits around their host stars and are older than 3 Gyr based on stellar isochrone models of the stars. TOI-569 is one of two slightly evolved stars known to host a transiting BD (the other being KOI-415). TOI-1406b is one of three known transiting BDs to occupy the mass range of 40-50 and one of two to have a circular orbit at a period near 10 days (with the first being KOI-205b). Both BDs have reliable ages from stellar isochrones, in addition to their well-constrained masses and radii, making them particularly valuable as tests for substellar isochrones in the BD mass-radius diagram.
Address [Carmichael, Theron W.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA, Email: tcarmich@cfa.harvard.edu
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000549117200001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1179
Permanent link to this record
 

 
Author Dawson, RI.; Huang, CLX.; Brahm, R.; Collins, KA.; Hobson, MJ.; Jordan, A.; Dong, JY.; Korth, J.; Trifonov, T.; Abe, L.; Agabi, A.; Bruni, I.; Butler, RP.; Barbieri, M.; Collins, KI.; Conti, DM.; Crane, JD.; Crouzet, N.; Dransfield, G.; Evans, P.; Espinoza, N.; Gan, TJ.; Guillot, T.; Henning, T.; Lissauer, JJ.; Jensen, ELN.; Sainte, WM.; Mekarnia, D.; Myers, G.; Nandakumar, S.; Relles, HM.; Sarkis, P.; Torres, P.; Shectman, S.; Schmider, FX.; Shporer, A.; Stockdale, C.; Teske, J.; Triaud, AHMJ.; Wang, SX.; Ziegler, C.; Ricker, G.; Vanderspek, R.; Latham, DW.; Seager, S.; Winn, J.; Jenkins, JM.; Bouma, LG.; Burt, JA.; Charbonneau, D.; Levine, AM.; McDermott, S.; McLean, B.; Rose, ME.; Vanderburg, A.; Wohler, B.
Title Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216b Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 4 Pages 161
Keywords
Abstract TOI-216 hosts a pair of warm, large exoplanets discovered by the TESS mission. These planets were found to be in or near the 2:1 resonance, and both of them exhibit transit timing variations (TTVs). Precise characterization of the planets' masses and radii, orbital properties, and resonant behavior can test theories for the origins of planets orbiting close to their stars. Previous characterization of the system using the first six sectors of TESS data suffered from a degeneracy between planet mass and orbital eccentricity. Radial-velocity measurements using HARPS, FEROS, and the Planet Finder Spectrograph break that degeneracy, and an expanded TTV baseline from TESS and an ongoing ground-based transit observing campaign increase the precision of the mass and eccentricity measurements. We determine that TOI-216c is a warm Jupiter, TOI-216b is an eccentric warm Neptune, and that they librate in 2:1 resonance with a moderate libration amplitude of deg, a small but significant free eccentricity of for TOI-216b, and a small but significant mutual inclination of 12-39 (95% confidence interval). The libration amplitude, free eccentricity, and mutual inclination imply a disturbance of TOI-216b before or after resonance capture, perhaps by an undetected third planet.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000625759900001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1363
Permanent link to this record
 

 
Author Forster, F.; Cabrera-Vives, G.; Castillo-Navarrete, E.; Estevez, PA.; Sanchez-Saez, P.; Arredondo, J.; Bauer, FE.; Carrasco-Davis, R.; Catelan, M.; Elorrieta, F.; Eyheramendy, S.; Huijse, P.; Pignata, G.; Reyes, E.; Reyes, I.; Rodriguez-Mancini, D.; Ruz-Mieres, D.; Valenzuela, C.; Alvarez-Maldonado, I.; Astorga, N.; Borissova, J.; Clocchiatti, A.; De Cicco, D.; Donoso-Oliva, C.; Hernandez-Garcia, L.; Graham, MJ.; Jordan, A.; Kurtev, R.; Mahabal, A.; Maureira, JC.; Munoz-Arancibia, A.; Molina-Ferreiro, R.; Moya, A.; Palma, W.; Perez-Carrasco, M.; Protopapas, P.; Romero, M.; Sabatini-Gacitua, L.; Sanchez, A.; San Martin, J.; Sepulveda-Cobo, C.; Vera, E.; Vergara, JR.
Title The Automatic Learning for the Rapid Classification of Events (ALeRCE) Alert Broker Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 5 Pages 242
Keywords
Abstract We introduce the Automatic Learning for the Rapid Classification of Events (ALeRCE) broker, an astronomical alert broker designed to provide a rapid and self-consistent classification of large etendue telescope alert streams, such as that provided by the Zwicky Transient Facility (ZTF) and, in the future, the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST). ALeRCE is a Chilean-led broker run by an interdisciplinary team of astronomers and engineers working to become intermediaries between survey and follow-up facilities. ALeRCE uses a pipeline that includes the real-time ingestion, aggregation, cross-matching, machine-learning (ML) classification, and visualization of the ZTF alert stream. We use two classifiers: a stamp-based classifier, designed for rapid classification, and a light curve-based classifier, which uses the multiband flux evolution to achieve a more refined classification. We describe in detail our pipeline, data products, tools, and services, which are made public for the community (see ). Since we began operating our real-time ML classification of the ZTF alert stream in early 2019, we have grown a large community of active users around the globe. We describe our results to date, including the real-time processing of 1.5 x 10(8) alerts, the stamp classification of 3.4 x 10(7) objects, the light-curve classification of 1.1 x 10(6) objects, the report of 6162 supernova candidates, and different experiments using LSST-like alert streams. Finally, we discuss the challenges ahead in going from a single stream of alerts such as ZTF to a multistream ecosystem dominated by LSST.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN ISBN Medium
Area Expedition Conference
Notes WOS:000645164000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1380
Permanent link to this record
 

 
Author Hartman, J.D.; Jordan, A.; Bayliss, D.; Bakos, G.A.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Henning, T.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, G.; Crane, J.D.; Shectman, S.; Teske, J.K.; Wang, S.X.; Butler, R.P.; Lazar, J.; Papp, I.; Sari, P.; Anderson, D.R.; Hellier, C.; West, R.G.; Barkaoui, K.; Pozuelos, F.J.; Jehin, E.; Gillon, M.; Nielsen, L.; Lendl, M.; Udry, S.; Ricker, G.R.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Christiansen, J.; Crossfield, I.J.M.; Henze, C.E.; Jenkins, J.M.; Smith, J.C.; Ting, E.B.
Title HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 159 Issue 4 Pages 23 pp
Keywords Exoplanets; Extrasolar gas giants; Hot Jupiters; Transits
Abstract We report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS49b, and HATS-72b have masses of 0.369+ 0.0210.031MJ, 0.243+ 0.0300.022 MJ, 0.353+ 0.0270.038 MJ, and 0.1254. 0.0039 MJ, respectively, and radii of 1.117. 0.014 RJ, 0.800. 0.015 RJ, 0.765. 0.013 RJ, and 0.7224. 0.0032 RJ, respectively. The planets orbit close to their host stars with orbital periods of 3.9228 days, 3.1317 days, 4.1480 days, and 7.3279 days, respectively. The hosts are main-sequence K dwarfs with masses of 0.674+ 0.0120.016.M, 0.7279. 0.0066.M, 0.7133. 0.0075.M, and 0.7311. 0.0028, and with V-band magnitudes of V = 14.829. 0.010, 14.35. 0.11, 14.998. 0.040 and 12.469. 0.010. The super-Neptune HATS-72b (a.k.a. WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP, and TESS surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS, and Magellan/PFS. We also incorporate TESS observations of the warm Saturn-hosting systems HATS-47 (a.k.a. TOI.1073.01), HATS-48A, and HATS-49. HATS-47 was independently identified as a candidate by the TESS team, while the other two systems were not previously identified from the TESS data. The RV orbital variations are measured for these systems using Magellan/PFS. HATS-48A has a resolved 5.. 4 neighbor in Gaia.DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of 0.22.M and a current projected physical separation of similar to 1400 au.
Address [Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Csubry, Z.; Winn, Joshua N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA, Email: jhartman@astro.princeton.edu
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000522443100001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1155
Permanent link to this record
 

 
Author Hobson, MJ.; Brahm, R.; Jordan, A .; Espinoza, N.; Kossakowski, D.; Henning, T.; Rojas, F.; Schlecker, M.; Sarkis, P.; Trifonov, T.; Thorngren, D.; Binnenfeld, A.; Shahaf, S.; Zucker, S.; Ricker, GR.; Latham, DW.; Seager, S.; Winn, JN.; Jenkins, JM.; Addison, B.; Bouchy, F.; Bowler, BP.; Briegal, JT.; Bryant, EM.; Collins, KA.; Daylan, T.; Grieves, N.; Horner, J.; Huang, CL.; Kane, SR.; Kielkopf, J.; McLean, B.; Mengel, MW.; Nielsen, LD.; Okumura, J.; Jones, M.; Plavchan, P.; Shporer, A.; Smith, AMS.; Tilbrook, R.; Tinney, CG.; Twicken, JD.; Udry, S.; Unger, N.; West, R.; Wittenmyer, RA.; Wohler, B.; Torres, P.; Wright, DJ.
Title A Transiting Warm Giant Planet around the Young Active Star TOI-201 Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 5 Pages 235
Keywords MAGNETIC ACTIVITY; ERROR-CORRECTION; EXOPLANETS; ROTATION; TEMPERATURES; EVOLUTION; VELOCITY; SYSTEMS; TOOL
Abstract We present the confirmation of the eccentric warm giant planet TOI-201 b, first identified as a candidate in Transiting Exoplanet Survey Satellite photometry (Sectors 1-8, 10-13, and 27-28) and confirmed using groundbased photometry from Next Generation Transit Survey and radial velocities from FEROS, HARPS, CORALIE, and MINERVA-Australis. TOI-201 b orbits a young (0.87(-0.49)(+0.46)) and bright (V = 9.07 mag) F-type star with a 52.9781 day period. The planet has a mass of 0.42(-0.03)(+0.05) M-J, a radius of 1.008(-0.015)(+0.012) R-J, and an orbital eccentricity of 0.28(-0.09)(+0.06); it appears to still be undergoing fairly rapid cooling, as expected given the youth of the host star. The star also shows long-term variability in both the radial velocities and several activity indicators, which we attribute to stellar activity. The discovery and characterization of warm giant planets such as TOI-201 b are important for constraining formation and evolution theories for giant planets.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN ISBN Medium
Area Expedition Conference
Notes WOS:000645139000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1381
Permanent link to this record
 

 
Author Jackson, JM.; Dawson, RI.; Shannon, A.; Petrovich, C
Title Observable Predictions from Perturber-coupled High-eccentricity Tidal Migration of Warm Jupiters Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 4 Pages 200
Keywords Exoplanet systems; Exoplanet dynamics; Exoplanet evolution; Hot Jupiters
Abstract The origin of warm Jupiters (gas giant planets with periods between 10 and 200 days) is an open question in exoplanet formation and evolution. We investigate a particular migration theory in which a warm Jupiter is coupled to a perturbing companion planet that excites secular eccentricity oscillations in the warm Jupiter, leading to periodic close stellar passages that can tidally shrink and circularize its orbit. If such companions exist in warm Jupiter systems, they are likely to be massive and close-in, making them potentially detectable. We generate a set of warm Jupiter-perturber populations capable of engaging in high-eccentricity tidal migration and calculate the detectability of the perturbers through a variety of observational metrics. We show that a small percentage of these perturbers should be detectable in the Kepler light curves, but most should be detectable with precise radial velocity measurements over a 3 month baseline and Gaia astrometry. We find these results to be robust to the assumptions made for the perturber parameter distributions. If a high-precision radial velocity search for companions to warm Jupiters does not find evidence of a significant number of massive companions over a 3 month baseline, it will suggest that perturber-coupled high-eccentricity migration is not the predominant delivery method for warm Jupiters.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000632894600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1359
Permanent link to this record
 

 
Author Jordan, A.; Bakos, G.A.; Bayliss, D.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Hartman, J.D.; Henning, T.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, G.; Butler, R.P.; Teske, J.; Crane, J.; Shectman, S.; Tan, T.G.; Thompson, I.; Wallace, J.J.; Lazar, J.; Papp, I.; Sari, P.
Title HATS-37Ab and HATS-38b: Two Transiting Hot Neptunes in the Desert* Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 5 Pages 14 pp
Keywords Exoplanets; Hot Neptunes
Abstract We report the discovery of two transiting Neptunes by the HATSouth survey. The planet HATS-37Ab has a mass of 0.099 +/- 0.042 MJ (31.5.+/-.13.4M(circle dot)) and a radius of 0.606 +/- 0.016 R-J, and is on a P = 4.3315 day orbit around a V = 12.266 +/- 0.030 mag, 0.843(-0.012)(+0.017)M(circle dot) star with a radius of 0.877(-0.012)(+0.019) R-circle dot We also present evidence that the star HATS-37A has an unresolved stellar companion HATS-37B, with a photometrically estimated mass of 0.654 +/- 0.033.M-circle dot The planet HATS-38b has a mass of 0.074. 0.011MJ (23.5 +/- 3.5M(circle dot)) and a radius of 0.614 +/- 0.017 R-J, and is on a P = 4.3750 day orbit around a V = 12.411 +/- 0.030 mag, 0.890(-0.012)(+0.016) M-circle dot star with a radius of 1.105 +/- 0.016.R-circle dot Both systems appear to be old, with isochrone-based ages of 11.46(-1.45)(+0.79) Gyr, and 11.89 +/- 0.60 Gyr, respectively. Both HATS-37Ab and HATS-38b lie in the Neptune desert and are thus examples of a population with a low occurrence rate. They are also among the lowest-mass planets found from ground-based wide-field surveys to date.
Address [Jordan, A.; Brahm, R.; Suc, V] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Av Diagonal Tones 2640, Santiago, Chile, Email: andres.jordan@uai.cl
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000584931800001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1261
Permanent link to this record
 

 
Author Jordan, A.; Brahm, R.; Espinoza, N.; Henning, T.; Jones, M.I.; Kossakowski, D.; Sarkis, P.; Trifonov, T.; Rojas, F.; Torres, P.; Drass, H.; Nandakumar, S.; Barbieri, M.; Davis, A.; Wang, S.H.; Bayliss, D.; Bouma, L.; Dragomir, D.; Eastman, J.D.; Daylan, T.; Guerrero, N.; Barclay, T.; Ting, E.B.; Henze, C.E.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.; Jenkins, J.M.; Wittenmyer, R.A.; Bowler, B.P.; Crossfield, I.; Horner, J.; Kane, S.R.; Kielkopf, J.F.; Morton, T.D.; Plavchan, P.; Tinney, C.G.; Addison, B.; Mengel, M.W.; Okumura, J.; Shahaf, S.; Mazeh, T.; Rabus, M.; Shporer, A.; Ziegler, C.; Mann, A.W.; Hart, R.
Title TOI-677b: A Warm Jupiter (P=11.2 days) on an Eccentric Orbit Transiting a Late F-type Star Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 159 Issue 4 Pages 10 pp
Keywords Exoplanets; Extrasolar gas giants; Exoplanet astronomy; Transit photometry; Radial velocity; Planet hosting stars
Abstract We report the discovery of TOI-677.b, first identified as a candidate in light curves obtained within Sectors 9 and 10 of the Transiting Exoplanet Survey Satellite (TESS) mission and confirmed with radial velocities. TOI-677.b has a mass of M-p = 1.236(-0.067)(+0.069) M-J, a radius of R-P = 1.170 +/- 0.03 R-J, and orbits its bright host star (V=.9.8 mag) with an orbital period of 11.23660 +/- 0.00011 d, on an eccentric orbit with e = 0.435 +/- 0.024. The host star has a mass of M-star = 1.181 +/- 0.058 M-circle dot, a radius of R. = 1.28(-0.03)(+0.03) R-circle dot, an age of 2.92(-0.73)(+0.80) Gyr and solar metallicity, properties consistent with a main-sequence late-F star with T-eff = 6295 +/- 77 K. We find evidence in the radial velocity measurements of a secondary long-term signal, which could be due to an outer companion. The TOI-677.b system is a well-suited target for Rossiter-Mclaughlin observations that can constrain migration mechanisms of close-in giant planets.
Address [Jordan, Andres] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Ave Diagonal Torres 2640, Santiago, Chile
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000521218500001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1129
Permanent link to this record
 

 
Author Kirk, J.; Rackham, B.V.; MacDonald, R.J.; Lopez-Morales, M.; Espinoza, N.; Lendl, M.; Wilson, J.; D.J.; Wheatley, P.J.; Skillen, I.; Apai, D.; Bixel, A.; Gibson, N.P.; Jordan, A.; Lewis, N.K.; Louden, T.; McGruder, C.D.; Nikolov, N.; Rodler, F.; Weaver, I.C.
Title ACCESS and LRG-BEASTS: A Precise New Optical Transmission Spectrum of the Ultrahot Jupiter WASP-103b Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 162 Issue 1 Pages 34
Keywords GAS-GIANT EXOPLANET; HOT JUPITERS; ATMOSPHERES; TRANSIT; PLANET; EFFICIENT; SPECTROSCOPY; RETRIEVAL; CHEMISTRY; EXPLAIN
Abstract We present a new ground-based optical transmission spectrum of the ultrahot Jupiter WASP-103b (Teq=2484
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000667942900001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1434
Permanent link to this record
 

 
Author McGruder, C.D.; Lopez-Morales, M.; Espinoza, N.; Rackham, B.V.; Apai, D.; Jordan, A.; Osip, D.J.; Alam, M.K.; Bixel, A.; Fortney, J.J.; Henry, G.W.; Kirk, J.; Lewis, N.K.; Rodler, F.; Weaver, I.C.
Title ACCESS: Confirmation of No Potassium in the Atmosphere of WASP-31b Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 5 Pages 22 pp
Keywords
Abstract We present a new optical (400-950 nm) transmission spectrum of the hot Jupiter WASP-31b (M = 0.48 M-J; R = 1.54 R-J; P = 3.41 days), obtained by combining four transit observations. These transits were observed with IMACS on the Magellan Baade Telescope at Las Campanas Observatory as part of the ACCESS project. We investigate the presence of clouds/hazes in the upper atmosphere of this planet, as well as the contribution of stellar activity on the observed features. In addition, we search for absorption features of the alkali elements Na i and K i, with particular focus on K i, for which there have been two previously published disagreeing results. Observations with Hubble Space Telescope (HST)/STIS detected K i, whereas ground-based low- and high-resolution observations did not. We use equilibrium and nonequilibrium chemistry retrievals to explore the planetary and stellar parameter space of the system with our optical data combined with existing near-IR observations. Our best-fit model is that with a scattering slope consistent with a Rayleigh slope (alpha = 5(-3.1)(+2.9)), high-altitude clouds at a log cloud top pressure of -3.6(-2.1)(+2.7) bars, and possible muted H2O features. We find that our observations support other ground-based claims of no K I. Clouds are likely why signals like H2O are extremely muted and Na or K cannot be detected. We then juxtapose our Magellan/IMACS transmission spectrum with existing VLT/FORS2, HST/WFC3, HST/STIS, and Spitzer observations to further constrain the optical-to-infrared atmospheric features of the planet. We find that a steeper scattering slope (alpha = 8.3 +/- 1.5) is anchored by STIS wavelengths blueward of 400 nm and only the original STIS observations show significant potassium signal.
Address [McGruder, Chima D.; Lopez-Morales, Mercedes; Alam, Munazza K.; Kirk, James; Weaver, Ian C.] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA, Email: chima.mcgruder@cfa.harvard.edu
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000584919200001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1262
Permanent link to this record
 

 
Author Mireles, I.; Shporer, A.; Grieves, N.; Zhou, G.; Gunther, M.N.; Brahm, R.; Ziegler, C.; Stassun, K.G.; Huang, C.X.; Nielsen, L.; dos Santos, L.A.; Udry, S.; Bouchy, F.; Ireland, M.; Wallace, A.; Sarkis, P.; Henning, T.; Jordan, A.; Law, N.; Mann, A.W.; Paredes, L.A.; James, H.S.; Jao, W.C.; Henry, T.J.; Butler, R.P.; Rodriguez, J.E.; Yu, L.; Flowers, E.; Ricker, G.R.; Latham, D.W.; Vanderspek, R.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Furesz, G.; Hesse, K.; Quintana, E.V.; Rose, M.E.; Smith, J.C.; Tenenbaum, P.; Vezie, M.; Yahalomi, D.A.; Zhan, Z.C.
Title TOI 694b and TIC 220568520b: Two Low-mass Companions near the Hydrogen-burning Mass Limit Orbiting Sun-like Stars Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 3 Pages 13 pp
Keywords Low mass stars; M dwarf stars; Eclipsing binary stars
Abstract We report the discovery of TOI 694 b and TIC 220568520 b, two low-mass stellar companions in eccentric orbits around metal-rich Sun-like stars, first detected by the Transiting Exoplanet Survey Satellite (TESS). TOI 694 b has an orbital period of 48.05131 +/- 0.00019 days and eccentricity of 0.51946 +/- 0.00081, and we derive a mass of 89.0 +/- 5.3 M-Jup (0.0849 +/- 0.0051 M-circle dot) and radius of 1.111 +/- 0.017 R-Jup (0.1142 +/- 0.0017 R-circle dot). TIC 220568520 b has an orbital period of 18.55769 +/- 0.00039 days and eccentricity of 0.0964 +/- 0.0032, and we derive a mass of 107.2 +/- 5.2 M-Jup (0.1023 +/- 0.0050 M-circle dot) and radius of 1.248 +/- 0.018 R-Jup (0.1282 +/- 0.0019 R-circle dot). Both binary companions lie close to and above the hydrogen-burning mass threshold that separates brown dwarfs and the lowest-mass stars, with TOI 694 b being 2s above the canonical mass threshold of 0.075 M-circle dot. The relatively long periods of the systems mean that the magnetic fields of the low-mass companions are not expected to inhibit convection and inflate the radius, which according to one leading theory is common in similar objects residing in short-period tidally synchronized binary systems. Indeed we do not find radius inflation for these two objects when compared to theoretical isochrones. These two new objects add to the short but growing list of low-mass stars with well-measured masses and radii, and highlight the potential of the TESS mission for detecting such rare objects orbiting bright stars.
Address [Mireles, Ismael; Shporer, Avi; Guenther, Maximilian N.; Huang, Chelsea X.; Yu, Liang; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Furesz, Gabor] MIT, Dept Phys, Cambridge, MA 02139 USA
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000565724400001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1253
Permanent link to this record
 

 
Author Rodriguez, JE.; Quinn, SN.; Zhou, G.; Vanderburg, A.; Nielsen, LD.; Wittenmyer, RA.; Brahm, R.; Reed, PA.; Huang, CLX.; Vach, S.; Ciardi, DR.; Oelkers, RJ.; Stassun, KG.; Hellier, C.; Gaudi, BS.; Eastman, JD.; Collins, KA.; Bieryla, A.; Christian, S.; Latham, DW.; Carleo, I.; Wright, DJ.; Matthews, E.; Gonzales, EJ.; Ziegler, C.; Dressing, CD.; Howell, SB.; Tan, TG.; Wittrock, J.; Plavchan, P.; McLeod, KK.; Baker, D.; Wang, GV.; Radford, DJ.; Schwarz, RP.; Esposito, M.; Ricker, GR.; Vanderspek, RK.; Seager, S.; Winn, JN.; Jenkins, JM.; Addison, B.; Anderson, DR.; Barclay, T.; Beatty, TG.; Berlind, P.; Bouchy, F.; Bowen, M.; Bowler, BP.; Brasseur, CE.; Briceno, C.; Caldwell, DA.; Calkins, ML.; Cartwright, S.; Chaturvedi, P.; Chaverot, G.; Chimaladinne, S.; Christiansen, JL.; Collins, KI.; Crossfield, IJM.; Eastridge, K.; Espinoza, N.; Esquerdo, GA.; Feliz, DL.; Fenske, T.; Fong, W.; Gan, TJ.; Giacalone, S.; Gill, H.; Gordon, L.; Granados, A.; Grieves, N.; Guenther, EW.; Guerrero, N.; Henning, T.; Henze, CE.; Hesse, K.; Hobson, MJ.; Horner, J.; James, DJ.; Jensen, ELN.; Jimenez, M.; Jordan, A.; Kane, SR.; Kielkopf, J.; Kim, K.; Kuhn, RB.; Latouf, N.; Law, NM.; Levine, AM.; Lund, MB.; Mann, AW.; Mao, SD.; Matson, RA.; Mengel, MW.; Mink, J.; Newman, P.; O'Dwyer, T.; Okumura, J.; Palle, E.; Pepper, J.; Quintana, EV.; Sarkis, P.; Savel, AB.; Schlieder, JE.; Schnaible, C.; Shporer, A.; Sefako, R.; Seidel, JV.; Siverd, RJ.; Skinner, B.; Stalport, M.; Stevens, DJ.; Stibbards, C.; Tinney, CG.; West, RG.; Yahalomi, DA.; Zhang, H.
Title TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 4 Pages 194
Keywords Exoplanet astronomy; Exoplanet migration; Exoplanet detection methods; Exoplanets; Transits; Radial velocity; Direct imaging
Abstract We present the discovery and characterization of five hot and warm Jupiters-TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b ( TIC 139375960)-based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (R-P = 1.01-1.77 R-J) and have masses that range from 0.85 to 6.33 M-J. The host stars of these systems have F and G spectral types (5595 <= T-eff <= 6460 K) and are all relatively bright (9.5 < V < 10.8, 8.2 < K < 9.3), making them well suited for future detailed characterization efforts. Three of the systems in our sample (TOI-640 b, TOI-1333 b, and TOI-1601 b) orbit subgiant host stars (log g < 4.1). TOI-640 b is one of only three known hot Jupiters to have a highly inflated radius (R-P > 1.7 R-J, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of 6.31(-0.30)(+) (0.28) M-J and a statistically significant, nonzero orbital eccentricity of e = 0.074(-0.022)(+) (0.021). This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA's TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000632893600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1358
Permanent link to this record
 

 
Author Sanchez-Saez, P.; Reyes, I.; Valenzuela, C.; Forster, F.; Eyheramendy, S.; Elorrieta, F.; Bauer, FE.; Cabrera-Vives, G.; Estevez, PA.; Catelan, M.; Pignata, G.; Huijse, P.; De Cicco, D.; Arevalo, P.; Carrasco-Davis, R.; Abril, J.; Kurtev, R.; Borissova, J.; Arredondo, J.; Castillo-Navarrete, E.; Rodriguez, D.; Ruz-Mieres, D.; Moya, A.; Sabatini-Gacitua, L.; Sepulveda-Cobo, C.; Camacho-Iniguez, E.
Title Alert Classification for the ALeRCE Broker System: The Light Curve Classifier Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 3 Pages 141
Keywords Active galaxies; Astronomy data analysis; Variable stars; Supernovae; Surveys
Abstract We present the first version of the Automatic Learning for the Rapid Classification of Events (ALeRCE) broker light curve classifier. ALeRCE is currently processing the Zwicky Transient Facility (ZTF) alert stream, in preparation for the Vera C. Rubin Observatory. The ALeRCE light curve classifier uses variability features computed from the ZTF alert stream and colors obtained from AllWISE and ZTF photometry. We apply a balanced random forest algorithm with a two-level scheme where the top level classifies each source as periodic, stochastic, or transient, and the bottom level further resolves each of these hierarchical classes among 15 total classes. This classifier corresponds to the first attempt to classify multiple classes of stochastic variables (including core- and host-dominated active galactic nuclei, blazars, young stellar objects, and cataclysmic variables) in addition to different classes of periodic and transient sources, using real data. We created a labeled set using various public catalogs (such as the Catalina Surveys and Gaia DR2 variable stars catalogs, and the Million Quasars catalog), and we classify all objects with >= 6 g-band or >= 6 r-band detections in ZTF (868,371 sources as of 2020 June 9), providing updated classifications for sources with new alerts every day. For the top level we obtain macro-averaged precision and recall scores of 0.96 and 0.99, respectively, and for the bottom level we obtain macro-averaged precision and recall scores of 0.57 and 0.76, respectively. Updated classifications from the light curve classifier can be found at the ALeRCE Explorer website (http://alerce.online)..
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000620974000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1347
Permanent link to this record
 

 
Author Schlecker, M.; Kossakowski, D.; Brahm, R.; Espinoza, N.; Henning, T.; Carone, L.; Molaverdikhani, K.; Trifonov, T.; Molliere, P.; Hobson, MJ.; Jordan, A.; Rojas, FI.; Klahr, H.; Sarkis, P.; Bakos, GA.; Bhatti, W.; Osip, D.; Suc, V.; Ricker, G.; Vanderspek, R.; Latham, DW.; Seager, S.; Winn, JN.; Jenkins, JM.; Vezie, M.; Villasenor, JN.; Rose, ME.; Rodriguez, DR.; Rodriguez, JE.; Quinn, SN.; Shporer, A.
Title A highly eccentric warm jupiter orbiting TIC 237913194 Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 6 Pages 275
Keywords Exoplanet astronomy; Transit photometry; Radial velocity; Exoplanet dynamics; Exoplanet atmospheres; Exoplanet structure; Hot Jupiters; Extrasolar gas giants
Abstract The orbital parameters of warm Jupiters serve as a record of their formation history, providing constraints on formation scenarios for giant planets on close and intermediate orbits. Here, we report the discovery of TIC.237913194b, detected in full-frame images from Sectors 1 and 2 of the Transiting Exoplanet Survey Satellite (TESS), ground-based photometry (Chilean-Hungarian Automated Telescope, Las Cumbres Observatory Global Telescope), and Fiber-fed Extended Range Optical Spectrograph radial velocity time series. We constrain its mass to M-P = 1.942(-0.091)(+0.091) M-J and its radius to R-P = 1.117(-0.047)(+0.054) R-J, implying a bulk density similar to Neptune's. It orbits a G-type star (M-* = 1.026(-0.055)(+0.057) M-circle dot, V = 12.1 mag) with a period of 15.17 days on one of the most eccentric orbits of all known warm giants (e approximate to 0.58). This extreme dynamical state points to a past interaction with an additional, undetected massive companion. A tidal evolution analysis showed a large tidal dissipation timescale, suggesting that the planet is not a progenitor for a hot Jupiter caught during its high-eccentricity migration. TIC.237913194b further represents an attractive opportunity to study the energy deposition and redistribution in the atmosphere of a warm Jupiter with high eccentricity.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes Approved
Call Number UAI @ alexi.delcanto @ Serial 1286
Permanent link to this record
 

 
Author Sha, LZ.; Huang, CLX.; Shporer, A.; Rodriguez, JE.; Vanderburg, A.; Brahm, R.; Hagelberg, J.; Matthews, EC.; Ziegler, C.; Livingston, JH.; Stassun, KG.; Wright, DJ.; Crane, JD.; Espinoza, N.; Bouchy, F.; Bakos, GA.; Collins, KA.; Zhou, GR.; Bieryla, A.; Hartman, JD.; Wittenmyer, RA.; Nielsen, LD.; Plavchan, P.; Bayliss, D.; Sarkis, P.; Tan, TG.; Cloutier, R.; Mancini, L.; Jordan, A.; Wang, SR.; Henning, T.; Narita, N.; Penev, K.; Teske, JK.; Kane, SR.; Mann, AW.; Addison, BC.; Tamura, M.; Horner, J.; Barbieri, M.; Burt, JA.; Diaz, MR.; Crossfield, IJM.; Dragomir, D.; Drass, H.; Feinstein, AD.; Zhang, H.; Hart, R.; Kielkopf, JF.; Jensen, ELN.; Montet, BT.; Ottoni, G.; Schwarz, RP.; Rojas, F.; Nespral, D.; Torres, P.; Mengel, MW.; Udry, S.; Zapata, A.; Snoddy, E.; Okumura, J.; Ricker, GR.; Vanderspek, RK.; Latham, DW.; Winn, JN.; Seager, S.; Jenkins, JM.; Colon, KD.; Henze, CE.; Krishnamurthy, A.; Ting, EB.; Vezie, M.; Villanueva, S.
Title TOI-954 b and K2-329 b: Short-period Saturn-mass Planets that Test whether Irradiation Leads to Inflation Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 2 Pages 82
Keywords STARS; 1ST; ALGORITHM; RADIUS; HOST; NAOS; RICH
Abstract We report the discovery of two short-period Saturn-mass planets, one transiting the G subgiant TOI-954 (TIC 44792534, V = 10.343, T = 9.78) observed in TESS sectors 4 and 5 and one transiting the G dwarf K2-329 (EPIC 246193072, V = 12.70, K = 10.67) observed in K2 campaigns 12 and 19. We confirm and characterize these two planets with a variety of ground-based archival and follow-up observations, including photometry, reconnaissance spectroscopy, precise radial velocity, and high-resolution imaging. Combining all available data, we find that TOI-954 b has a radius of 0.852(-0.062)(+0.053) R-J and a mass of 0.174(-0.017)(+0.018) M-J and is in a 3.68 day orbit, while K2-329 b has a radius of 0.774(-0.024)(+0.026) R-J and a mass if 0.260(-0.022)(+0.020) M-J and is in a 12.46 day orbit. As TOI-954 b is 30 times more irradiated than K2-329 b but more or less the same size, these two planets provide an opportunity to test whether irradiation leads to inflation of Saturn-mass planets and contribute to future comparative studies that explore Saturn-mass planets at contrasting points in their lifetimes.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000610062100001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1327
Permanent link to this record
 

 
Author van der Marel, N.; Mulders, G.D.
Title A Stellar Mass Dependence of Structured Disks: A Possible Link with Exoplanet Demographics Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 162 Issue 1 Pages 28
Keywords GIANT PLANET OCCURRENCE; X-SHOOTER SPECTROSCOPY; MAIN-SEQUENCE STARS; CIRCLE-DOT STARS; ALMA SURVEY; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; TRANSITION DISKS; MILLIMETER CONTINUUM; CLASS-II
Abstract Gaps in protoplanetary disks have long been hailed as signposts of planet formation. However, a direct link between exoplanets and disks remains hard to identify. We present a large sample study of ALMA disk surveys of nearby star-forming regions to disentangle this connection. All disks are classified as either structured (transition, ring, extended) or nonstructured (compact) disks. Although low-resolution observations may not identify large-scale substructure, we assume that an extended disk must contain substructure from a dust evolution argument. A comparison across ages reveals that structured disks retain high dust masses up to at least 10 Myr, whereas the dust mass of compact, nonstructured disks decreases over time. This can be understood if the dust mass evolves primarily by radial drift, unless drift is prevented by pressure bumps. We identify a stellar mass dependence of the fraction of structured disks. We propose a scenario linking this dependence with that of giant exoplanet occurrence rates. We show that there are enough exoplanets to account for the observed disk structures if transitional disks are created by exoplanets more massive than Jupiter and ring disks by exoplanets more massive than Neptune, under the assumption that most of those planets eventually migrate inwards. On the other hand, the known anticorrelation between transiting super-Earths and stellar mass implies those planets must form in the disks without observed structure, consistent with formation through pebble accretion in drift-dominated disks. These findings support an evolutionary scenario where the early formation of giant planets determines the disk's dust evolution and its observational appearance.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000664728300001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1431
Permanent link to this record
 

 
Author Weaver, I.C.; Lopez-Morales, M.; Espinoza, N.; Rackham, B.V.; Osip, D.J.; Apai, D.; Jordan, A.; Bixel, A.; Lewis, N.K.; Alam, M.K.; Kirk, J.; McGruder, C.; Rodler, F.; Fienco, J.
Title ACCESS: A Visual to Near-infrared Spectrum of the Hot Jupiter WASP-43b with Evidence of H2O, but No Evidence of Na or K Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 159 Issue 1 Pages 21 pp
Keywords
Abstract We present a new ground-based visual transmission spectrum of the hot Jupiter WASP-43b, obtained as part of the ACCESS Survey. The spectrum was derived from four transits observed between 2015 and 2018, with combined wavelength coverage between 5300 and 9000 A and an average photometric precision of 708 ppm in 230 A bins. We perform an atmospheric retrieval of our transmission spectrum combined with literature Hubble Space Telescope/WFC3 observations to search for the presence of clouds/hazes as well as Na, K, H alpha, and H2O planetary absorption and stellar spot contamination over a combined spectral range of 5318-16420 A. We do not detect a statistically significant presence of Na i or K i alkali lines, or H alpha in the atmosphere of WASP-43b. We find that the observed transmission spectrum can be best explained by a combination of heterogeneities on the photosphere of the host star and a clear planetary atmosphere with H2O. This model yields a log evidence of 8.26 0.42 higher than a flat (featureless) spectrum. In particular, the observations marginally favor the presence of large, low-contrast spots over the four ACCESS transit epochs with an average covering fraction T = 132 K 132 K. Within the planet's atmosphere, we recover a log H2O volume mixing ratio of -2.78(-1.47)(+1.38), which is consistent with previous H2O abundance determinations for this planet.
Address [Weaver, Ian C.; Lopez-Morales, Mercedes; Alam, Munazza K.; Kirk, James; McGruder, Chima] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA, Email: iweaver@cfa.harvard.edu
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000519136000001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1168
Permanent link to this record