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A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of PlanetsHurt, Spencer A.Quinn, Samuel N.Latham, David W.Vanderburg, AndrewEsquerdo, Gilbert A.Calkins, Michael L.Berlind, PerryAngus, RuthLatham, Christian A.Zhou, GeorgeDOI: info:10.3847/1538-3881/abdec8v. 161157
Hurt, Spencer A., Quinn, Samuel N., Latham, David W., Vanderburg, Andrew, Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Angus, Ruth, Latham, Christian A., and Zhou, George. 2021. "A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets." The Astronomical Journal 161:157. https://doi.org/10.3847/1538-3881/abdec8
ID: 159324
Type: article
Authors: Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth; Latham, Christian A.; Zhou, George
Abstract: We present an analysis of 1524 spectra of Vega spanning 10 yr, in which we search for periodic radial-velocity variations. A signal with a periodicity of 0.676 day and a semi-amplitude of ∼10 m s-1 is consistent with the rotation period measured over much shorter time spans by previous spectroscopic and spectropolarimetric studies, confirming the presence of surface features on this A0 star. The activity signal appears to evolve on long timescales, which may indicate the presence of failed fossil magnetic fields on Vega. TESS data reveal Vega's photometric rotational modulation for the first time, with a total amplitude of only 10 ppm. A comparison of the spectroscopic and photometric amplitudes suggests that the surface features may be dominated by bright plages rather than dark spots. For the shortest orbital periods, transit and radial-velocity injection recovery tests exclude the presence of transiting planets larger than 2 R and most non-transiting giant planets. At long periods, we combine our radial velocities with direct imaging from the literature to produce detection limits for Vegan planets and brown dwarfs out to distances of 15 au. Finally, we detect a candidate radial-velocity signal with a period of 2.43 days and a semi-amplitude of 6 m s-1. If caused by an orbiting companion, its minimum mass would be ∼20 M; because of Vega's pole-on orientation, this would correspond to a Jovian planet if the orbit is aligned with the stellar spin. We discuss the prospects for confirmation of this candidate planet.
TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame ImagesRodriguez, Joseph E.Quinn, Samuel N.Zhou, GeorgeVanderburg, AndrewNielsen, Louise D.Wittenmyer, Robert A.Brahm, RafaelReed, Phillip A.Huang, Chelsea X.Vach, SydneyCiardi, David R.Oelkers, Ryan J.Stassun, Keivan G.Hellier, CoelGaudi, B. ScottEastman, Jason D.Collins, Karen A.Bieryla, AllysonChristian, SamLatham, David W.Carleo, IlariaWright, Duncan J.Matthews, ElisabethGonzales, Erica J.Ziegler, CarlDressing, Courtney D.Howell, Steve B.Tan, Thiam-GuanWittrock, JustinPlavchan, PeterMcLeod, Kim K.Baker, DavidWang, GavinRadford, Don J.Schwarz, Richard P.Esposito, MassimilianoRicker, George R.Vanderspek, Roland K.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Addison, BrettAnderson, D. R.Barclay, ThomasBeatty, Thomas G.Berlind, PerryBouchy, FrancoisBowen, MichaelBowler, Brendan P.Brasseur, C. E.Briceño, CésarCaldwell, Douglas A.Calkins, Michael L.Cartwright, ScottChaturvedi, PriyankaChaverot, GuillaumeChimaladinne, SudhishChristiansen, Jessie L.Collins, Kevin I.Crossfield, Ian J. M.Eastridge, KevinEspinoza, NéstorEsquerdo, Gilbert A.Feliz, Dax L.Fenske, TylerFong, WilliamGan, TianjunGiacalone, StevenGill, HoldenGordon, LindseyGranados, A.Grieves, NolanGuenther, Eike W.Guerrero, NataliaHenning, ThomasHenze, Christopher E.Hesse, KatharineHobson, Melissa J.Horner, JonathanJames, David J.Jensen, Eric L. N.Jimenez, MaryJordán, AndrésKane, Stephen R.Kielkopf, JohnKim, KingsleyKuhn, Rudolf B.Latouf, NatashaLaw, Nicholas M.Levine, Alan M.Lund, Michael B.Mann, Andrew W.Mao, ShudeMatson, Rachel A.Mengel, Matthew W.Mink, JessicaNewman, PatrickO'Dwyer, TannerOkumura, JackPalle, EnricPepper, JoshuaQuintana, Elisa V.Sarkis, PaulaSavel, Arjun B.Schlieder, Joshua E.Schnaible, ChloeShporer, AviSefako, RamotholoSeidel, Julia V.Siverd, Robert J.Skinner, BrettStalport, ManuStevens, Daniel J.Stibbards, CaitlinTinney, C. G.West, R. G.Yahalomi, Daniel A.Zhang, HuiDOI: info:10.3847/1538-3881/abe38av. 161194
Rodriguez, Joseph E., Quinn, Samuel N., Zhou, George, Vanderburg, Andrew, Nielsen, Louise D., Wittenmyer, Robert A., Brahm, Rafael, Reed, Phillip A., Huang, Chelsea X., Vach, Sydney, Ciardi, David R., Oelkers, Ryan J., Stassun, Keivan G., Hellier, Coel, Gaudi, B. Scott, Eastman, Jason D., Collins, Karen A., Bieryla, Allyson, Christian, Sam, Latham, David W., Carleo, Ilaria, Wright, Duncan J., Matthews, Elisabeth, Gonzales, Erica J., Ziegler, Carl et al. 2021. "TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images." The Astronomical Journal 161:194. https://doi.org/10.3847/1538-3881/abe38a
ID: 159316
Type: article
Authors: Rodriguez, Joseph E.; Quinn, Samuel N.; Zhou, George; Vanderburg, Andrew; Nielsen, Louise D.; Wittenmyer, Robert A.; Brahm, Rafael; Reed, Phillip A.; Huang, Chelsea X.; Vach, Sydney; Ciardi, David R.; Oelkers, Ryan J.; Stassun, Keivan G.; Hellier, Coel; Gaudi, B. Scott; Eastman, Jason D.; Collins, Karen A.; Bieryla, Allyson; Christian, Sam; Latham, David W.; Carleo, Ilaria; Wright, Duncan J.; Matthews, Elisabeth; Gonzales, Erica J.; Ziegler, Carl; Dressing, Courtney D.; Howell, Steve B.; Tan, Thiam-Guan; Wittrock, Justin; Plavchan, Peter; McLeod, Kim K.; Baker, David; Wang, Gavin; Radford, Don J.; Schwarz, Richard P.; Esposito, Massimiliano; Ricker, George R.; Vanderspek, Roland K.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison, Brett; Anderson, D. R.; Barclay, Thomas; Beatty, Thomas G.; Berlind, Perry; Bouchy, Francois; Bowen, Michael; Bowler, Brendan P.; Brasseur, C. E.; Briceño, César; Caldwell, Douglas A.; Calkins, Michael L.; Cartwright, Scott; Chaturvedi, Priyanka; Chaverot, Guillaume; Chimaladinne, Sudhish; Christiansen, Jessie L.; Collins, Kevin I.; Crossfield, Ian J. M.; Eastridge, Kevin; Espinoza, Néstor; Esquerdo, Gilbert A.; Feliz, Dax L.; Fenske, Tyler; Fong, William; Gan, Tianjun; Giacalone, Steven; Gill, Holden; Gordon, Lindsey; Granados, A.; Grieves, Nolan; Guenther, Eike W.; Guerrero, Natalia; Henning, Thomas; Henze, Christopher E.; Hesse, Katharine; Hobson, Melissa J.; Horner, Jonathan; James, David J.; Jensen, Eric L. N.; Jimenez, Mary; Jordán, Andrés; Kane, Stephen R.; Kielkopf, John; Kim, Kingsley; Kuhn, Rudolf B.; Latouf, Natasha; Law, Nicholas M.; Levine, Alan M.; Lund, Michael B.; Mann, Andrew W.; Mao, Shude; Matson, Rachel A.; Mengel, Matthew W.; Mink, Jessica; Newman, Patrick; O'Dwyer, Tanner; Okumura, Jack; Palle, Enric; Pepper, Joshua; Quintana, Elisa V.; Sarkis, Paula; Savel, Arjun B.; Schlieder, Joshua E.; Schnaible, Chloe; Shporer, Avi; Sefako, Ramotholo; Seidel, Julia V.; Siverd, Robert J.; Skinner, Brett; Stalport, Manu; Stevens, Daniel J.; Stibbards, Caitlin; Tinney, C. G.; West, R. G.; Yahalomi, Daniel A.; Zhang, Hui
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 (RP = 1.01-1.77 RJ) and have masses that range from 0.85 to 6.33 MJ. The host stars of these systems have F and G spectral types (5595 ≤ Teff ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 P > 1.7 RJ, 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 ${6.31}_{-0.30}^{+0.28}$ MJ 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.
TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey SatelliteBrahm, RafaelNielsen, Louise D.Wittenmyer, Robert A.Wang, SonghuRodriguez, Joseph E.Espinoza, NéstorJones, Matías I.Jordán, AndrésHenning, ThomasHobson, MelissaKossakowski, DianaRojas, FelipeSarkis, PaulaSchlecker, MartinTrifonov, TrifonShahaf, SaharRicker, GeorgeVanderspek, RolandLatham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Addison, Brett C.Bakos, Gáspár Á.Bhatti, WaqasBayliss, DanielBerlind, PerryBieryla, AllysonBouchy, FrancoisBowler, Brendan P.Briceño, CésarBrown, Timothy M.Bryant, Edward M.Caldwell, Douglas A.Charbonneau, DavidCollins, Karen A.Davis, Allen B.Esquerdo, Gilbert A.Fulton, Benjamin J.Guerrero, Natalia M.Henze, Christopher E.Hogan, AleishaHorner, JonathanHuang, Chelsea X.Irwin, JonathanKane, Stephen R.Kielkopf, JohnMann, Andrew W.Mazeh, TseviMcCormac, JamesMcCully, CurtisMengel, Matthew W.Mireles, IsmaelOkumura, JackPlavchan, PeterQuinn, Samuel N.Rabus, MarkusSaesen, SophieSchlieder, Joshua E.Segransan, DamienShiao, BernieShporer, AviSiverd, Robert J.Stassun, Keivan G.Suc, VincentTan, Thiam-GuanTorres, PascalTinney, Chris G.Udry, StephaneVanzi, LeonardoVezie, MichaelVines, Jose I.Vuckovic, MajaWright, Duncan J.Yahalomi, Daniel A.Zapata, AbnerZhang, HuiZiegler, CarlDOI: info:10.3847/1538-3881/abba3bv. 160235
Brahm, Rafael, Nielsen, Louise D., Wittenmyer, Robert A., Wang, Songhu, Rodriguez, Joseph E., Espinoza, Néstor, Jones, Matías I., Jordán, Andrés, Henning, Thomas, Hobson, Melissa, Kossakowski, Diana, Rojas, Felipe, Sarkis, Paula, Schlecker, Martin, Trifonov, Trifon, Shahaf, Sahar, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett C., Bakos, Gáspár Á., Bhatti, Waqas et al. 2020. "TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite." The Astronomical Journal 160:235. https://doi.org/10.3847/1538-3881/abba3b
ID: 158644
Type: article
Authors: Brahm, Rafael; Nielsen, Louise D.; Wittenmyer, Robert A.; Wang, Songhu; Rodriguez, Joseph E.; Espinoza, Néstor; Jones, Matías I.; Jordán, Andrés; Henning, Thomas; Hobson, Melissa; Kossakowski, Diana; Rojas, Felipe; Sarkis, Paula; Schlecker, Martin; Trifonov, Trifon; Shahaf, Sahar; Ricker, George; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison, Brett C.; Bakos, Gáspár Á.; Bhatti, Waqas; Bayliss, Daniel; Berlind, Perry; Bieryla, Allyson; Bouchy, Francois; Bowler, Brendan P.; Briceño, César; Brown, Timothy M.; Bryant, Edward M.; Caldwell, Douglas A.; Charbonneau, David; Collins, Karen A.; Davis, Allen B.; Esquerdo, Gilbert A.; Fulton, Benjamin J.; Guerrero, Natalia M.; Henze, Christopher E.; Hogan, Aleisha; Horner, Jonathan; Huang, Chelsea X.; Irwin, Jonathan; Kane, Stephen R.; Kielkopf, John; Mann, Andrew W.; Mazeh, Tsevi; McCormac, James; McCully, Curtis; Mengel, Matthew W.; Mireles, Ismael; Okumura, Jack; Plavchan, Peter; Quinn, Samuel N.; Rabus, Markus; Saesen, Sophie; Schlieder, Joshua E.; Segransan, Damien; Shiao, Bernie; Shporer, Avi; Siverd, Robert J.; Stassun, Keivan G.; Suc, Vincent; Tan, Thiam-Guan; Torres, Pascal; Tinney, Chris G.; Udry, Stephane; Vanzi, Leonardo; Vezie, Michael; Vines, Jose I.; Vuckovic, Maja; Wright, Duncan J.; Yahalomi, Daniel A.; Zapata, Abner; Zhang, Hui; Ziegler, Carl
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 ${R}_{{\rm{J}}}$ and 1.07 ± 0.02 ${R}_{{\rm{J}}}$ , respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 ${M}_{{\rm{J}}}$ versus 0.95 ± 0.07 ${M}_{{\rm{J}}}$ , respectively). Both planets orbit metal-rich stars ( $[\mathrm{Fe}/{\rm{H}}]$ = $+0.26\pm 0.05$ dex and $[\mathrm{Fe}/{\rm{H}}]$ = $+0.24\pm 0.05$ for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a ${M}_{\star }$ = 1.14 ± 0.02 ${M}_{\odot }$ , ${R}_{\star }$ = 1.66 ± 0.02 ${R}_{\odot }$ G-type star ( ${T}_{\mathrm{eff}}$ = $5735\pm 72$ 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 ( ${T}_{\mathrm{eff}}$ = $6261\pm 80$ K), which has a mass of ${M}_{\star }$ = 1.28 ± 0.03 ${M}_{\odot }$ and a radius of ${R}_{\star }$ = 1.39 ± 0.02 ${R}_{\odot }$ . 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.
TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESSDavis, Allen B.Wang, SonghuJones, MatiasEastman, Jason D.Günther, Maximilian N.Stassun, Keivan G.Addison, Brett C.Collins, Karen A.Quinn, Samuel N.Latham, David W.Trifonov, TrifonShahaf, SaharMazeh, TseviKane, Stephen R.Narita, NorioWang, Xian-YuTan, Thiam-GuanCiardi, David R.Tokovinin, AndreiZiegler, CarlTronsgaard, RenéMillholland, SarahCruz, BryndisBerlind, PerryCalkins, Michael L.Esquerdo, Gilbert A.Collins, Kevin I.Conti, Dennis M.Murgas, FelipeEvans, PhilLewin, PabloRadford, Don J.Paredes, Leonardo A.Henry, Todd J.Hodari-Sadiki, JamesLund, Michael B.Christiansen, Jessie L.Law, Nicholas M.Mann, Andrew W.Briceño, CésarParviainen, HannuPalle, EnricWatanabe, NoriharuRicker, George R.Vanderspek, RolandSeager, SaraWinn, Joshua N.Jenkins, Jon M.Krishnamurthy, AkshataBatalha, Natalie M.Burt, JenniferColón, Knicole D.Dynes, ScottCaldwell, Douglas A.Morris, RobertHenze, Christopher E.Fischer, Debra A.DOI: info:10.3847/1538-3881/aba49dv. 160229
Davis, Allen B., Wang, Songhu, Jones, Matias, Eastman, Jason D., Günther, Maximilian N., Stassun, Keivan G., Addison, Brett C., Collins, Karen A., Quinn, Samuel N., Latham, David W., Trifonov, Trifon, Shahaf, Sahar, Mazeh, Tsevi, Kane, Stephen R., Narita, Norio, Wang, Xian-Yu, Tan, Thiam-Guan, Ciardi, David R., Tokovinin, Andrei, Ziegler, Carl, Tronsgaard, René, Millholland, Sarah, Cruz, Bryndis, Berlind, Perry, Calkins, Michael L. et al. 2020. "TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESS." The Astronomical Journal 160:229. https://doi.org/10.3847/1538-3881/aba49d
ID: 158650
Type: article
Authors: Davis, Allen B.; Wang, Songhu; Jones, Matias; Eastman, Jason D.; Günther, Maximilian N.; Stassun, Keivan G.; Addison, Brett C.; Collins, Karen A.; Quinn, Samuel N.; Latham, David W.; Trifonov, Trifon; Shahaf, Sahar; Mazeh, Tsevi; Kane, Stephen R.; Narita, Norio; Wang, Xian-Yu; Tan, Thiam-Guan; Ciardi, David R.; Tokovinin, Andrei; Ziegler, Carl; Tronsgaard, René; Millholland, Sarah; Cruz, Bryndis; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.; Collins, Kevin I.; Conti, Dennis M.; Murgas, Felipe; Evans, Phil; Lewin, Pablo; Radford, Don J.; Paredes, Leonardo A.; Henry, Todd J.; Hodari-Sadiki, James; Lund, Michael B.; Christiansen, Jessie L.; Law, Nicholas M.; Mann, Andrew W.; Briceño, César; Parviainen, Hannu; Palle, Enric; Watanabe, Noriharu; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Krishnamurthy, Akshata; Batalha, Natalie M.; Burt, Jennifer; Colón, Knicole D.; Dynes, Scott; Caldwell, Douglas A.; Morris, Robert; Henze, Christopher E.; Fischer, Debra A.
Abstract: We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 and 3.739 days, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of ${1.463}_{-0.096}^{+0.10}$ MJ and a radius of ${1.02}_{-0.29}^{+0.71}$ RJ. Also a classical hot Jupiter, TOI 905 b has a mass of ${0.667}_{-0.041}^{+0.042}$ MJ and radius of ${1.171}_{-0.051}^{+0.053}$ RJ. Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with V ˜ 11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of ${0.994}_{-0.049}^{+0.083}$ , making it one of only ˜20 known systems to exhibit a grazing transit and one of the brightest host stars among them. Therefore, TOI 564 b is one of the most attractive systems to search for additional nontransiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over a timescale of several years.
TESS Hunt for Young and Maturing Exoplanets (THYME). III. A Two-planet System in the 400 Myr Ursa Major GroupMann, Andrew W.Johnson, Marshall C.Vanderburg, AndrewKraus, Adam L.Rizzuto, Aaron C.Wood, Mackenna L.Bush, Jonathan L.Rockcliffe, KeighleyNewton, Elisabeth R.Latham, David W.Mamajek, Eric E.Zhou, GeorgeQuinn, Samuel N.Thao, Pa ChiaBenatti, SerenaCosentino, RosarioDesidera, SilvanoHarutyunyan, AvetLovis, ChristopheMortier, AnneliesPepe, Francesco A.Poretti, EnnioWilson, Thomas G.Kristiansen, Martti H.Gagliano, RobertJacobs, ThomasLaCourse, Daryll M.Omohundro, MarkSchwengeler, Hans MartinTerentev, Ivan A.Kane, Stephen R.Hill, Michelle L.Rabus, MarkusEsquerdo, Gilbert A.Berlind, PerryCollins, Karen A.Murawski, GabrielSallam, Nezar HazamAitken, Michael M.Massey, BobRicker, George R.Vanderspek, RolandSeager, SaraWinn, Joshua N.Jenkins, Jon M.Barclay, ThomasCaldwell, Douglas A.Dragomir, DianaDoty, John P.Glidden, AnaTenenbaum, PeterTorres, GuillermoTwicken, Joseph D.Villanueva, Steven, Jr.DOI: info:10.3847/1538-3881/abae64v. 160179
Mann, Andrew W., Johnson, Marshall C., Vanderburg, Andrew, Kraus, Adam L., Rizzuto, Aaron C., Wood, Mackenna L., Bush, Jonathan L., Rockcliffe, Keighley, Newton, Elisabeth R., Latham, David W., Mamajek, Eric E., Zhou, George, Quinn, Samuel N., Thao, Pa Chia, Benatti, Serena, Cosentino, Rosario, Desidera, Silvano, Harutyunyan, Avet, Lovis, Christophe, Mortier, Annelies, Pepe, Francesco A., Poretti, Ennio, Wilson, Thomas G., Kristiansen, Martti H., Gagliano, Robert et al. 2020. "TESS Hunt for Young and Maturing Exoplanets (THYME). III. A Two-planet System in the 400 Myr Ursa Major Group." The Astronomical Journal 160:179. https://doi.org/10.3847/1538-3881/abae64
ID: 157597
Type: article
Authors: Mann, Andrew W.; Johnson, Marshall C.; Vanderburg, Andrew; Kraus, Adam L.; Rizzuto, Aaron C.; Wood, Mackenna L.; Bush, Jonathan L.; Rockcliffe, Keighley; Newton, Elisabeth R.; Latham, David W.; Mamajek, Eric E.; Zhou, George; Quinn, Samuel N.; Thao, Pa Chia; Benatti, Serena; Cosentino, Rosario; Desidera, Silvano; Harutyunyan, Avet; Lovis, Christophe; Mortier, Annelies; Pepe, Francesco A.; Poretti, Ennio; Wilson, Thomas G.; Kristiansen, Martti H.; Gagliano, Robert; Jacobs, Thomas; LaCourse, Daryll M.; Omohundro, Mark; Schwengeler, Hans Martin; Terentev, Ivan A.; Kane, Stephen R.; Hill, Michelle L.; Rabus, Markus; Esquerdo, Gilbert A.; Berlind, Perry; Collins, Karen A.; Murawski, Gabriel; Sallam, Nezar Hazam; Aitken, Michael M.; Massey, Bob; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Barclay, Thomas; Caldwell, Douglas A.; Dragomir, Diana; Doty, John P.; Glidden, Ana; Tenenbaum, Peter; Torres, Guillermo; Twicken, Joseph D.; Villanueva, Steven, Jr.
Abstract: Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets ( and 2.67 ± 0.12 R, the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than about 0.2. Using High Accuracy Radial velocity Planet Searcher for the Northern hemisphere velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating that the orbit is prograde. Since the host star is bright (V = 6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.
An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELTStevens, Daniel J.Zhou, GeorgeJohnson, Marshall C.Rizzuto, Aaron C.Rodriguez, Joseph E.Bieryla, AllysonCollins, Karen A.Villanueva, Steven, Jr.Wright, Jason T.Gaudi, B. ScottLatham, David W.Beatty, Thomas G.Lund, Michael B.Siverd, Robert J.Kraus, Adam L.Wachiraphan, PatcharapolBerlind, PerryCalkins, Michael L.Esquerdo, Gilbert A.Kielkopf, John F.Kuhn, Rudolf B.Manner, MarkPepper, JoshuaStassun, Keivan G.DOI: info:10.1093/mnras/staa3142v. 4993775–3791
Stevens, Daniel J., Zhou, George, Johnson, Marshall C., Rizzuto, Aaron C., Rodriguez, Joseph E., Bieryla, Allyson, Collins, Karen A., Villanueva, Steven, Jr., Wright, Jason T., Gaudi, B. Scott, Latham, David W., Beatty, Thomas G., Lund, Michael B., Siverd, Robert J., Kraus, Adam L., Wachiraphan, Patcharapol, Berlind, Perry, Calkins, Michael L., Esquerdo, Gilbert A., Kielkopf, John F., Kuhn, Rudolf B., Manner, Mark, Pepper, Joshua, and Stassun, Keivan G. 2020. "An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELT." Monthly Notices of the Royal Astronomical Society 499:3775– 3791. https://doi.org/10.1093/mnras/staa3142
ID: 158638
Type: article
Authors: Stevens, Daniel J.; Zhou, George; Johnson, Marshall C.; Rizzuto, Aaron C.; Rodriguez, Joseph E.; Bieryla, Allyson; Collins, Karen A.; Villanueva, Steven, Jr.; Wright, Jason T.; Gaudi, B. Scott; Latham, David W.; Beatty, Thomas G.; Lund, Michael B.; Siverd, Robert J.; Kraus, Adam L.; Wachiraphan, Patcharapol; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.; Kielkopf, John F.; Kuhn, Rudolf B.; Manner, Mark; Pepper, Joshua; Stassun, Keivan G.
Abstract: We present the discovery of KELT J072709 + 072007 (HD 58730), a very low mass ratio (q = M2/M1 ? 0.07) eclipsing binary (EB) identified by the Kilodegree Extremely Little Telescope (KELT) survey. We present the discovery light curve and perform a global analysis of four high-precision ground-based light curves, the Transiting Exoplanets Survey Satellite (TESS) light curve, radial velocity (RV) measurements, Doppler Tomography (DT) measurements, and the broad-band spectral energy distribution. Results from the global analysis are consistent with a fully convective ( $M_2 = 0.22 \pm 0.02\ \, \mathrm{M}_{\odot })$ M star transiting a late-B primary ( $M_1 = 3.34^{+0.07}_{-0.09}\ \, \mathrm{M}_{\odot }\,\mathrm{ and}\,\ T_{\rm eff,1} = 11960^{+430}_{-520}\ {\rm K}$ ). We infer that the primary star is $183_{-30}^{+33}$ Myr old and that the companion star's radius is inflated by $26 \pm 8{{\ \rm per\ cent}}$ relative to the predicted value from a low-mass isochrone of similar age. We separately and analytically fit for the variability in the out-of-eclipse TESS phase curve, finding good agreement between the resulting stellar parameters and those from the global fit. Such systems are valuable for testing theories of binary star formation and understanding how the environment of a star in a close-but-detached binary affects its physical properties. In particular, we examine how a star's properties in such a binary might differ from the properties it would have in isolation.
TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS MissionŠubjak, JánSharma, RishikeshCarmichael, Theron W.Johnson, Marshall C.Gonzales, Erica J.Matthews, ElisabethBoffin, Henri M. J.Brahm, RafaelChaturvedi, PriyankaChakraborty, AbhijitCiardi, David R.Collins, Karen A.Esposito, MassimilianoFridlund, MalcolmGan, TianjunGandolfi, DavideGarcía, Rafael A.Guenther, EikeHatzes, ArtieLatham, David W.Mathis, StéphaneMathur, SavitaPersson, Carina M.Relles, Howard M.Schlieder, Joshua E.Barclay, ThomasDressing, Courtney D.Crossfield, IanHoward, Andrew W.Rodler, FlorianZhou, GeorgeQuinn, Samuel N.Esquerdo, Gilbert A.Calkins, Michael L.Berlind, PerryStassun, Keivan G.Blažek, MartinSkarka, MarekŠpoková, MagdalenaŽák, JiříAlbrecht, SimonSobrino, Roi AlonsoBeck, PaulCabrera, JuanCarleo, IlariaCochran, William D.Csizmadia, SzilardDai, FeiDeeg, Hans J.de Leon, Jerome P.Eigmüller, PhilippEndl, MichaelErikson, AndersFukui, AkihikoGeorgieva, IskraGonzález-Cuesta, LucíaGrziwa, SaschaHidalgo, DiegoHirano, TeruyukiHjorth, MariaKnudstrup, EmilKorth, JudithLam, Kristine W. F.Livingston, John H.Lund, Mikkel N.Luque, RafaelRodríguez, Pilar MontanesMurgas, FelipeNarita, NorioNespral, DavidNiraula, PrajwalNowak, GrzegorzPallé, EnricPätzold, MartinPrieto-Arranz, JorgeRauer, HeikeRedfield, SethRibas, IgnasiSmith, Alexis M. S.Eylen, Vincent VanKabáth, PetrDOI: info:10.3847/1538-3881/ab7245v. 159151
Šubjak, Ján, Sharma, Rishikesh, Carmichael, Theron W., Johnson, Marshall C., Gonzales, Erica J., Matthews, Elisabeth, Boffin, Henri M. J., Brahm, Rafael, Chaturvedi, Priyanka, Chakraborty, Abhijit, Ciardi, David R., Collins, Karen A., Esposito, Massimiliano, Fridlund, Malcolm, Gan, Tianjun, Gandolfi, Davide, García, Rafael A., Guenther, Eike, Hatzes, Artie, Latham, David W., Mathis, Stéphane, Mathur, Savita, Persson, Carina M., Relles, Howard M., Schlieder, Joshua E. et al. 2020. "TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS Mission." The Astronomical Journal 159:151. https://doi.org/10.3847/1538-3881/ab7245
ID: 157123
Type: article
Authors: Šubjak, Ján; Sharma, Rishikesh; Carmichael, Theron W.; Johnson, Marshall C.; Gonzales, Erica J.; Matthews, Elisabeth; Boffin, Henri M. J.; Brahm, Rafael; Chaturvedi, Priyanka; Chakraborty, Abhijit; Ciardi, David R.; Collins, Karen A.; Esposito, Massimiliano; Fridlund, Malcolm; Gan, Tianjun; Gandolfi, Davide; García, Rafael A.; Guenther, Eike; Hatzes, Artie; Latham, David W.; Mathis, Stéphane; Mathur, Savita; Persson, Carina M.; Relles, Howard M.; Schlieder, Joshua E.; Barclay, Thomas; Dressing, Courtney D.; Crossfield, Ian; Howard, Andrew W.; Rodler, Florian; Zhou, George; Quinn, Samuel N.; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Stassun, Keivan G.; Blažek, Martin; Skarka, Marek; Špoková, Magdalena; Žák, Jiří; Albrecht, Simon; Sobrino, Roi Alonso; Beck, Paul; Cabrera, Juan; Carleo, Ilaria; Cochran, William D.; Csizmadia, Szilard; Dai, Fei; Deeg, Hans J.; de Leon, Jerome P.; Eigmüller, Philipp; Endl, Michael; Erikson, Anders; Fukui, Akihiko; Georgieva, Iskra; González-Cuesta, Lucía; Grziwa, Sascha; Hidalgo, Diego; Hirano, Teruyuki; Hjorth, Maria; Knudstrup, Emil; Korth, Judith; Lam, Kristine W. F.; Livingston, John H.; Lund, Mikkel N.; Luque, Rafael; Rodríguez, Pilar Montanes; Murgas, Felipe; Narita, Norio; Nespral, David; Niraula, Prajwal; Nowak, Grzegorz; Pallé, Enric; Pätzold, Martin; Prieto-Arranz, Jorge; Rauer, Heike; Redfield, Seth; Ribas, Ignasi; Smith, Alexis M. S.; Eylen, Vincent Van; Kabáth, Petr
Abstract: We report the discovery of an intermediate-mass transiting brown dwarf (BD), TOI-503b, from the TESS mission. TOI-503b is the first BD discovered by TESS, and it has circular orbit around a metallic-line A-type star with a period of P = 3.6772 ± 0.0001 days. The light curve from TESS indicates that TOI-503b transits its host star in a grazing manner, which limits the precision with which we measure the BD's radius ( ${R}_{b}={1.34}_{-0.15}^{+0.26}{R}_{{\rm{J}}} ). We obtained high- resolution spectroscopic observations with the FIES, Ondřejov, PARAS, Tautenburg, and TRES spectrographs, and measured the mass of TOI-503b to be Mb = 53.7 ± 1.2 ${M}_{{\rm{J}}} . The host star has a mass of M = 1.80 ± 0.06 M, a radius of R = 1.70 ± 0.05R, an effective temperature of Teff = 7650 ± 160 K, and a relatively high metallicity of 0.61 ± 0.07 dex. We used stellar isochrones to derive the age of the system to be ∼180 Myr, which places its age between that of RIK 72b (a ∼10 Myr old BD in the Upper Scorpius stellar association) and AD 3116b (a ∼600 Myr old BD in the Praesepe cluster). Given the difficulty in measuring the tidal interactions between BDs and their host stars, we cannot precisely say whether this BD formed in situ or has had its orbit circularized by its host star over the relatively short age of the system. Instead, we offer an examination of plausible values for the tidal quality factor for the star and BD. TOI-503b joins a growing number of known short-period, intermediate-mass BDs orbiting main-sequence stars, and is the second such BD known to transit an A star, after HATS-70b. With the growth in the population in this regime, the driest region in the BD desert ( $35\mbox{--}55{M}_{{\rm{J}}}\sin i ) is reforesting.
Spectroscopic Orbits of 11 Nearby, Mid-to-late M-dwarf BinariesWinters, Jennifer G.Irwin, Jonathan M.Charbonneau, DavidLatham, David W.Medina, Amber M.Mink, JessicaEsquerdo, Gilbert A.Berlind, PerryCalkins, Michael L.Berta-Thompson, Zachory K.DOI: info:10.3847/1538-3881/ab8d31v. 159290
Winters, Jennifer G., Irwin, Jonathan M., Charbonneau, David, Latham, David W., Medina, Amber M., Mink, Jessica, Esquerdo, Gilbert A., Berlind, Perry, Calkins, Michael L., and Berta-Thompson, Zachory K. 2020. "Spectroscopic Orbits of 11 Nearby, Mid-to-late M-dwarf Binaries." The Astronomical Journal 159:290. https://doi.org/10.3847/1538-3881/ab8d31
ID: 156878
Type: article
Authors: Winters, Jennifer G.; Irwin, Jonathan M.; Charbonneau, David; Latham, David W.; Medina, Amber M.; Mink, Jessica; Esquerdo, Gilbert A.; Berlind, Perry; Calkins, Michael L.; Berta-Thompson, Zachory K.
Abstract: We present the spectroscopic orbits of 11 nearby, mid-to-late M dwarf binary systems in a variety of configurations: 2 single-lined binaries (SB1s), 7 double-lined binaries (SB2s), 1 double-lined triple (ST2), and 1 triple-lined triple (ST3). Eight of these orbits are the first published for these systems, while five are newly identified multiples. We obtained multi-epoch, high-resolution spectra with the TRES instrument on the 1.5 m Tillinghast Reflector at the Fred Lawrence Whipple Observatory located on Mt. Hopkins in AZ. Using the TiO molecular bands at 7065-7165 Å, we calculated radial velocities for these systems, from which we derived their orbits. We find LHS 1817 to have in a 7 hr period a companion that is likely a white dwarf, due to the ellipsoidal modulation we see in our MEarth-North light-curve data. We find G 123-45 and LTT 11586 to host companions with minimum masses of 41 MJup and 44 MJup with orbital periods of 35 and 15 days, respectively. We find 2MA 0930+0227 to have a rapidly rotating stellar companion in a 917 day orbital period. GJ 268, GJ 1029, LP 734-34, GJ 1182, G 258-17, and LTT 7077are SB2s with stellar companions with orbital periods of 10, 96, 34, 154, 5, and 84 days; LP 655-43 is an ST3 with one companion in an 18 day orbital period and an outer component in a longer undetermined period. In addition, we present radial velocities for both components of L 870-44AB and for the outer components of LTT 11586 and LP 655-43.
The CIDA Variability Survey of Orion OB1. II. Demographics of the Young, Low-mass Stellar PopulationsBriceño, CésarCalvet, NuriaHernández, JesúsVivas, A. KatherinaMateu, CeciliaDownes, Juan JoséLoerincs, JaquelinePérez-Blanco, AliceBerlind, PerryEspaillat, CatherineAllen, LoriHartmann, LeeMateo, MarioBailey, John I., IIIDOI: info:10.3847/1538-3881/aaf79bv. 15785
Briceño, César, Calvet, Nuria, Hernández, Jesús, Vivas, A. Katherina, Mateu, Cecilia, Downes, Juan José, Loerincs, Jaqueline, Pérez-Blanco, Alice, Berlind, Perry, Espaillat, Catherine, Allen, Lori, Hartmann, Lee, Mateo, Mario, and Bailey, John I., III. 2019. "The CIDA Variability Survey of Orion OB1. II. Demographics of the Young, Low-mass Stellar Populations." The Astronomical Journal 157:85. https://doi.org/10.3847/1538-3881/aaf79b
ID: 155449
Type: article
Authors: Briceño, César; Calvet, Nuria; Hernández, Jesús; Vivas, A. Katherina; Mateu, Cecilia; Downes, Juan José; Loerincs, Jaqueline; Pérez-Blanco, Alice; Berlind, Perry; Espaillat, Catherine; Allen, Lori; Hartmann, Lee; Mateo, Mario; Bailey, John I., III
Abstract: We present results of our large-scale, optical, multi-epoch photometric survey across ∼180 square degrees in the Orion OB1 association, complemented with extensive follow-up spectroscopy. Our focus is mapping and characterizing the off-cloud, low-mass, pre-main-sequence (PMS) populations. We report 2062 K- and M-type confirmed T Tauri members; 59% are located in the OB1a subassociation, 27% in the OB1b subassociation, and the remaining 14% in the A and B molecular clouds. We characterize two new clusterings of T Tauri stars, the HD 35762 and HR 1833 groups, both located in OB1a not far from the 25 Ori cluster. We also identify two stellar overdensities in OB1b, containing 231 PMS stars, and find that the OB1b region is composed of two populations at different distances, possibly due to the OB1a subassociation overlapping with the front of OB1b. A ∼2 deg wide halo of young stars surrounds the Orion Nebula Cluster, corresponding in part to the low-mass populations of NGC 1977 and NGC 1980. We use the strength of Hα in emission, combined with the IR excess and optical variability, to define a new type of T Tauri star, the C/W class, stars we propose may be nearing the end of their accretion phase, in an evolutionary state between classical and weak- lined T Tauri stars. The evolution of the ensemble-wide equivalent width of Li I λ6707 indicates a Li depletion timescale of ∼8.5 Myr. Disk accretion declines with an e-folding timescale of ∼2 Myr, consistent with previous studies. Based on observations obtained at the Llano del Hato National Astronomical Observatory of Venezuela, operated by CIDA for the Ministerio del Poder Popular para la Educación Universitaria, Ciencia, Tecnología, the Fred Lawrence Whipple Observatory of the Smithsonian Institution, the WIYN 3.5 m telescope, the 6.5 m Magellan Telescopes at Las Campanas Observatory, and the Southern Astrophysical Research (SOAR) telescope.
Mapping the Stellar Halo with the H3 Spectroscopic SurveyConroy, CharlieBonaca, AnaCargile, PhillipJohnson, Benjamin D.Caldwell, NelsonNaidu, Rohan P.Zaritsky, DennisFabricant, DanielMoran, SeanRhee, JaehyonSzentgyorgyi, AndrewBerlind, PerryCalkins, Michael L.Kattner, ShiAnneLy, ChunDOI: info:10.3847/1538-4357/ab38b8v. 883107
Conroy, Charlie, Bonaca, Ana, Cargile, Phillip, Johnson, Benjamin D., Caldwell, Nelson, Naidu, Rohan P., Zaritsky, Dennis, Fabricant, Daniel, Moran, Sean, Rhee, Jaehyon, Szentgyorgyi, Andrew, Berlind, Perry, Calkins, Michael L., Kattner, ShiAnne, and Ly, Chun. 2019. "Mapping the Stellar Halo with the H3 Spectroscopic Survey." The Astrophysical Journal 883:107. https://doi.org/10.3847/1538-4357/ab38b8
ID: 154407
Type: article
Authors: Conroy, Charlie; Bonaca, Ana; Cargile, Phillip; Johnson, Benjamin D.; Caldwell, Nelson; Naidu, Rohan P.; Zaritsky, Dennis; Fabricant, Daniel; Moran, Sean; Rhee, Jaehyon; Szentgyorgyi, Andrew; Berlind, Perry; Calkins, Michael L.; Kattner, ShiAnne; Ly, Chun
Abstract: Modern theories of galaxy formation predict that the Galactic stellar halo was hierarchically assembled from the accretion and disruption of smaller systems. This hierarchical assembly is expected to produce a high degree of structure in the combined phase and chemistry space; this structure should provide a relatively direct probe of the accretion history of our Galaxy. Revealing this structure requires precise 3D positions (including distances), 3D velocities, and chemistry for large samples of stars. The Gaia satellite is delivering proper motions and parallaxes for >1 billion stars to G ≈ 20. However, radial velocities and metallicities will only be available to G ≈ 15, which is insufficient to probe the outer stellar halo (≳10 kpc). Moreover, parallaxes will not be precise enough to deliver high-quality distances for stars beyond ̃10 kpc. Identifying accreted systems throughout the stellar halo therefore requires a large ground-based spectroscopic survey to complement Gaia. Here we provide an overview of the H3 Stellar Spectroscopic Survey, which will deliver precise stellar parameters and spectrophotometric distances for ≈200,000 stars to r = 18. Spectra are obtained with the Hectochelle instrument at the MMT, which is configured for the H3 Survey to deliver resolution R ≈ 23,000 spectra covering the wavelength range 5150-5300 Å. The survey is optimized for stellar halo science and therefore focuses on high Galactic latitude fields (| b| > 30^\circ ), sparsely sampling 15,000 sq. degrees. Targets are selected on the basis of Gaia parallaxes, enabling very efficient selection of bona fide halo stars. The survey began in the fall of 2017 and has collected 88,000 spectra to-date. All of the data, including the derived stellar parameters, will eventually be made publicly available via the survey website: h3s urvey.rc.fas.harvard.edu.
Identifying Exoplanets with Deep Learning. II. Two New Super-Earths Uncovered by a Neural Network in K2 DataDattilo, AnneVanderburg, AndrewShallue, Christopher J.Mayo, Andrew W.Berlind, PerryBieryla, AllysonCalkins, Michael L.Esquerdo, Gilbert A.Everett, Mark E.Howell, Steve B.Latham, David W.Scott, Nicholas J.Yu, LiangDOI: info:10.3847/1538-3881/ab0e12v. 157169
Dattilo, Anne, Vanderburg, Andrew, Shallue, Christopher J., Mayo, Andrew W., Berlind, Perry, Bieryla, Allyson, Calkins, Michael L., Esquerdo, Gilbert A., Everett, Mark E., Howell, Steve B., Latham, David W., Scott, Nicholas J., and Yu, Liang. 2019. "Identifying Exoplanets with Deep Learning. II. Two New Super-Earths Uncovered by a Neural Network in K2 Data." The Astronomical Journal 157:169. https://doi.org/10.3847/1538-3881/ab0e12
ID: 151839
Type: article
Authors: Dattilo, Anne; Vanderburg, Andrew; Shallue, Christopher J.; Mayo, Andrew W.; Berlind, Perry; Bieryla, Allyson; Calkins, Michael L.; Esquerdo, Gilbert A.; Everett, Mark E.; Howell, Steve B.; Latham, David W.; Scott, Nicholas J.; Yu, Liang
Abstract: For years, scientists have used data from NASA’s Kepler Space Telescope to look for and discover thousands of transiting exoplanets. In its extended K2 mission, Kepler observed stars in various regions of the sky all across the ecliptic plane, and therefore in different galactic environments. Astronomers want to learn how the populations of exoplanets are different in these different environments. However, this requires an automatic and unbiased way to identify exoplanets in these regions and rule out false-positive signals that mimic transiting planet signals. We present a method for classifying these exoplanet signals using deep learning, a class of machine learning algorithms that have become popular in fields ranging from medical science to linguistics. We modified a neural network previously used to identify exoplanets in the Kepler field to be able to identify exoplanets in different K2 campaigns that exist in a range of galactic environments. We train a convolutional neural network, called AstroNet- K2, to predict whether a given possible exoplanet signal is really caused by an exoplanet or a false positive. AstroNet- K2 is highly successful at classifying exoplanets and false positives, with accuracy of 98% on our test set. It is especially efficient at identifying and culling false positives, but for now, it still needs human supervision to create a complete and reliable planet candidate sample. We use AstroNet- K2 to identify and validate two previously unknown exoplanets. Our method is a step toward automatically identifying new exoplanets in K2 data and learning how exoplanet populations depend on their galactic birthplace.
KELT-22Ab: A Massive, Short-Period Hot Jupiter Transiting a Near-solar TwinLabadie-Bartz, JonathanRodriguez, Joseph E.Stassun, Keivan G.Ciardi, David R.Penev, KaloyanJohnson, Marshall C.Gaudi, B. ScottColón, Knicole D.Bieryla, AllysonLatham, David W.Pepper, JoshuaCollins, Karen A.Evans, PhilRelles, HowardSiverd, Robert J.Bento, JoaoYao, XinyuStockdale, ChrisTan, Thiam-GuanZhou, GeorgeEastman, Jason D.Albrow, Michael D.Bayliss, DanielBeatty, Thomas G.Berlind, PerryBozza, ValerioCalkins, Michael L.Cohen, David H.Curtis, Ivan A.Esquerdo, Gilbert A.Feliz, DaxFulton, Benjamin J.Gregorio, JoaoJames, DavidJensen, Eric L. N.Johnson, John AsherJohnson, Samson A.Joner, Michael D.Kasper, DavidKielkopf, John F.Kuhn, Rudolf B.Lund, Michael B.Malpas, AmberManner, MarkMcCrady, NateMcLeod, Kim K.Oberst, Thomas E.Penny, Matthew T.Reed, Phillip A.Sliski, David H.Stephens, Denise C.Stevens, Daniel J.Villanueva, Steven, Jr.Wittenmyer, Robert A.Wright, J. T.Zambelli, RobertoDOI: info:10.3847/1538-4365/aaee7ev. 24013
Labadie-Bartz, Jonathan, Rodriguez, Joseph E., Stassun, Keivan G., Ciardi, David R., Penev, Kaloyan, Johnson, Marshall C., Gaudi, B. Scott, Colón, Knicole D., Bieryla, Allyson, Latham, David W., Pepper, Joshua, Collins, Karen A., Evans, Phil, Relles, Howard, Siverd, Robert J., Bento, Joao, Yao, Xinyu, Stockdale, Chris, Tan, Thiam-Guan, Zhou, George, Eastman, Jason D., Albrow, Michael D., Bayliss, Daniel, Beatty, Thomas G., Berlind, Perry et al. 2019. "KELT-22Ab: A Massive, Short-Period Hot Jupiter Transiting a Near-solar Twin." The Astrophysical Journal Supplement Series 240:13. https://doi.org/10.3847/1538-4365/aaee7e
ID: 150442
Type: article
Authors: Labadie-Bartz, Jonathan; Rodriguez, Joseph E.; Stassun, Keivan G.; Ciardi, David R.; Penev, Kaloyan; Johnson, Marshall C.; Gaudi, B. Scott; Colón, Knicole D.; Bieryla, Allyson; Latham, David W.; Pepper, Joshua; Collins, Karen A.; Evans, Phil; Relles, Howard; Siverd, Robert J.; Bento, Joao; Yao, Xinyu; Stockdale, Chris; Tan, Thiam-Guan; Zhou, George; Eastman, Jason D.; Albrow, Michael D.; Bayliss, Daniel; Beatty, Thomas G.; Berlind, Perry; Bozza, Valerio; Calkins, Michael L.; Cohen, David H.; Curtis, Ivan A.; Esquerdo, Gilbert A.; Feliz, Dax; Fulton, Benjamin J.; Gregorio, Joao; James, David; Jensen, Eric L. N.; Johnson, John Asher; Johnson, Samson A.; Joner, Michael D.; Kasper, David; Kielkopf, John F.; Kuhn, Rudolf B.; Lund, Michael B.; Malpas, Amber; Manner, Mark; McCrady, Nate; McLeod, Kim K.; Oberst, Thomas E.; Penny, Matthew T.; Reed, Phillip A.; Sliski, David H.; Stephens, Denise C.; Stevens, Daniel J.; Villanueva, Steven, Jr.; Wittenmyer, Robert A.; Wright, J. T.; Zambelli, Roberto
Abstract: We present the discovery of KELT-22Ab, a hot Jupiter from the KELT-South survey. KELT-22Ab transits the moderately bright (V ∼ 11.1) Sun-like G2V star TYC 7518-468-1. The planet has an orbital period of P =1.3866529+/- 0.0000027 days, a radius of {R}P={1.285}-0.071+0.12 {R}J, and a relatively large mass of {M}P={3.47}-0.14+0.15 {M}J. The star has {R}\star ={1.099}-0.046+0.079 {R}ȯ , {M}\star ={1.092}-0.041+0.045 {M}ȯ , {T}eff} ={5767}-49+50 K, {log}{g}\star ={4.393}-0.060+0.039 (cgs), and [m/H] = +{0.259}-0.083+0.085; thus other than its slightly super-solar metallicity, it appears to be a near-solar twin. Surprisingly, KELT-22A exhibits kinematics and a Galactic orbit that are somewhat atypical for thin-disk stars. Nevertheless, the star is rotating rapidly for its estimated age, and shows evidence of chromospheric activity. Imaging reveals a slightly fainter companion to KELT-22A that is likely bound, with a projected separation of 6″ (∼1400 au). In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT-22A, suggesting the presence of another relatively nearby body that is perhaps non-stellar. KELT-22Ab is highly irradiated (as a consequence of the small semimajor axis of a/{R}\star =4.97), and is mildly inflated. At such small separations, tidal forces become significant. The configuration of this system is optimal for measuring the rate of tidal dissipation within the host star. Our models predict that, due to tidal forces, the semimajor axis is decreasing rapidly, and KELT-22Ab is predicted to spiral into the star within the next Gyr.
The 2MASS Redshift Survey in the Zone of AvoidanceMacri, Lucas M.Kraan-Korteweg, Renée C.Lambert, TrystanAlonso, María VictoriaBerlind, PerryCalkins, MichaelErdoğdu, PirinFalco, Emilio E.Jarrett, Thomas H.Mink, Jessica D.DOI: info:10.3847/1538-4365/ab465av. 2456
Macri, Lucas M., Kraan-Korteweg, Renée C., Lambert, Trystan, Alonso, María Victoria, Berlind, Perry, Calkins, Michael, Erdoğdu, Pirin, Falco, Emilio E., Jarrett, Thomas H., and Mink, Jessica D. 2019. "The 2MASS Redshift Survey in the Zone of Avoidance." The Astrophysical Journal Supplement Series 245:6. https://doi.org/10.3847/1538-4365/ab465a
ID: 154579
Type: article
Authors: Macri, Lucas M.; Kraan-Korteweg, Renée C.; Lambert, Trystan; Alonso, María Victoria; Berlind, Perry; Calkins, Michael; Erdoğdu, Pirin; Falco, Emilio E.; Jarrett, Thomas H.; Mink, Jessica D.
Abstract: The Two Micron All-Sky Survey (2MASS) Redshift Survey was started two decades ago with the goal of mapping the three-dimensional distribution of an all-sky flux-limited (K s < 11.75 mag) sample of ∼45,000 galaxies. Our first data release presented an unprecedented uniform coverage for most of the celestial sphere, with redshifts for ∼98% of our sample. However, we were missing redshifts for ∼18% of the catalog entries that were located within the "Zone of Avoidance" (| b| < 10^\circ )-an important region of the sky for studies of the large- scale structure and cosmic flows. In this second and final data release, we present redshifts for all 1041 2MRS galaxies that previously lacked this information, as well as updated measurements for 27 others.
A Hot Saturn Near (but Unassociated with) the Open Cluster NGC 1817Rampalli, RaynaVanderburg, AndrewBieryla, AllysonLatham, David W.Quinn, Samuel N.Baranec, ChristophBerlind, PerryCalkins, Michael L.Cochran, William D.Duev, Dmitry A.Endl, MichaelEsquerdo, Gilbert A.Jensen-Clem, RebeccaLaw, Nicholas M.Mayo, Andrew W.Riddle, ReedSalama, MaïssaDOI: info:10.3847/1538-3881/ab27c2v. 15862
Rampalli, Rayna, Vanderburg, Andrew, Bieryla, Allyson, Latham, David W., Quinn, Samuel N., Baranec, Christoph, Berlind, Perry, Calkins, Michael L., Cochran, William D., Duev, Dmitry A., Endl, Michael, Esquerdo, Gilbert A., Jensen-Clem, Rebecca, Law, Nicholas M., Mayo, Andrew W., Riddle, Reed, and Salama, Maïssa. 2019. "A Hot Saturn Near (but Unassociated with) the Open Cluster NGC 1817." The Astronomical Journal 158:62. https://doi.org/10.3847/1538-3881/ab27c2
ID: 154287
Type: article
Authors: Rampalli, Rayna; Vanderburg, Andrew; Bieryla, Allyson; Latham, David W.; Quinn, Samuel N.; Baranec, Christoph; Berlind, Perry; Calkins, Michael L.; Cochran, William D.; Duev, Dmitry A.; Endl, Michael; Esquerdo, Gilbert A.; Jensen-Clem, Rebecca; Law, Nicholas M.; Mayo, Andrew W.; Riddle, Reed; Salama, Maïssa
Abstract: We report on the discovery of a hot Saturn-sized planet (9.916 ± 0.985 R ) around a late F-star, K2-308, observed in Campaign 13 of the K2 mission. We began studying this planet candidate because prior to the release of Gaia DR2, the host star was thought to have been a member (≥slant 90 % membership probability) of the ≈ 1 {Gyr} open cluster NGC 1817 based on its kinematics and photometric distance. We identify the host star (among three stars within the K2 photometric aperture) using seeing-limited photometry and rule out false-positive scenarios using adaptive optics imaging and radial velocity observations. We statistically validate K2-308b by calculating a false-positive probability rate of 0.01 % . However, we also show using new kinematic measurements provided by Gaia DR2 and our measured radial velocity of the system that K2-308 is unassociated with the cluster NGC 1817. Therefore, the long running search for a giant transiting planet in an open cluster remains fruitless. Finally, we note that our use of seeing-limited photometry is a good demonstration of similar techniques that are already being used to follow up Transiting Exoplanet Survey Satellite (TESS) planet candidates, especially in crowded regions.
KELT-24b: A 5M J Planet on a 5.6 day Well-aligned Orbit around the Young V = 8.3 F-star HD 93148Rodriguez, Joseph E.Eastman, Jason D.Zhou, GeorgeQuinn, Samuel N.Beatty, Thomas G.Penev, KaloyanJohnson, Marshall C.Cargile, Phillip A.Latham, David W.Bieryla, AllysonCollins, Karen A.Dressing, Courtney D.Ciardi, David R.Relles, Howard M.Murawski, GabrielNishiumi, TakuYonehara, AtsunoriIshimaru, RyoYoshida, FumiGregorio, JoaoLund, Michael B.Stevens, Daniel J.Stassun, Keivan G.Gaudi, B. ScottColón, Knicole D.Pepper, JoshuaNarita, NorioAwiphan, SupachaiChuanraksasat, PongpichitBenni, PaulZambelli, RobertoGarrison, Lehman H.Wilson, Maurice L.Cornachione, Matthew A.Wang, Sharon X.Labadie-Bartz, JonathanRodríguez, RomySiverd, Robert J.Yao, XinyuBayliss, DanielBerlind, PerryCalkins, Michael L.Christiansen, Jessie L.Cohen, David H.Conti, Dennis M.Curtis, Ivan A.DePoy, D. L.Esquerdo, Gilbert A.Evans, PhilFeliz, DaxFulton, Benjamin J.Holoien, Thomas W. -SJames, David J.Jayasinghe, TharinduJang-Condell, HannahJensen, Eric L. N.Johnson, John A.Joner, Michael D.Khakpash, SomayehKielkopf, John F.Kuhn, Rudolf B.Manner, MarkMarshall, Jennifer L.McLeod, Kim K.McCrady, NateOberst, Thomas E.Oelkers, Ryan J.Penny, Matthew T.Reed, Phillip A.Sliski, David H.Shappee, B. J.Stephens, Denise C.Stockdale, ChrisTan, Thiam-GuanTrueblood, MarkTrueblood, PatVillanueva, Steven, Jr.Wittenmyer, Robert A.Wright, Jason T.DOI: info:10.3847/1538-3881/ab4136v. 158197
Rodriguez, Joseph E., Eastman, Jason D., Zhou, George, Quinn, Samuel N., Beatty, Thomas G., Penev, Kaloyan, Johnson, Marshall C., Cargile, Phillip A., Latham, David W., Bieryla, Allyson, Collins, Karen A., Dressing, Courtney D., Ciardi, David R., Relles, Howard M., Murawski, Gabriel, Nishiumi, Taku, Yonehara, Atsunori, Ishimaru, Ryo, Yoshida, Fumi, Gregorio, Joao, Lund, Michael B., Stevens, Daniel J., Stassun, Keivan G., Gaudi, B. Scott, Colón, Knicole D. et al. 2019. "KELT-24b: A 5M J Planet on a 5.6 day Well-aligned Orbit around the Young V = 8.3 F-star HD 93148." The Astronomical Journal 158:197. https://doi.org/10.3847/1538-3881/ab4136
ID: 154595
Type: article
Authors: Rodriguez, Joseph E.; Eastman, Jason D.; Zhou, George; Quinn, Samuel N.; Beatty, Thomas G.; Penev, Kaloyan; Johnson, Marshall C.; Cargile, Phillip A.; Latham, David W.; Bieryla, Allyson; Collins, Karen A.; Dressing, Courtney D.; Ciardi, David R.; Relles, Howard M.; Murawski, Gabriel; Nishiumi, Taku; Yonehara, Atsunori; Ishimaru, Ryo; Yoshida, Fumi; Gregorio, Joao; Lund, Michael B.; Stevens, Daniel J.; Stassun, Keivan G.; Gaudi, B. Scott; Colón, Knicole D.; Pepper, Joshua; Narita, Norio; Awiphan, Supachai; Chuanraksasat, Pongpichit; Benni, Paul; Zambelli, Roberto; Garrison, Lehman H.; Wilson, Maurice L.; Cornachione, Matthew A.; Wang, Sharon X.; Labadie-Bartz, Jonathan; Rodríguez, Romy; Siverd, Robert J.; Yao, Xinyu; Bayliss, Daniel; Berlind, Perry; Calkins, Michael L.; Christiansen, Jessie L.; Cohen, David H.; Conti, Dennis M.; Curtis, Ivan A.; DePoy, D. L.; Esquerdo, Gilbert A.; Evans, Phil; Feliz, Dax; Fulton, Benjamin J.; Holoien, Thomas W. -S; James, David J.; Jayasinghe, Tharindu; Jang-Condell, Hannah; Jensen, Eric L. N.; Johnson, John A.; Joner, Michael D.; Khakpash, Somayeh; Kielkopf, John F.; Kuhn, Rudolf B.; Manner, Mark; Marshall, Jennifer L.; McLeod, Kim K.; McCrady, Nate; Oberst, Thomas E.; Oelkers, Ryan J.; Penny, Matthew T.; Reed, Phillip A.; Sliski, David H.; Shappee, B. J.; Stephens, Denise C.; Stockdale, Chris; Tan, Thiam-Guan; Trueblood, Mark; Trueblood, Pat; Villanueva, Steven, Jr.; Wittenmyer, Robert A.; Wright, Jason T.
Abstract: We present the discovery of KELT-24 b, a massive hot Jupiter orbiting a bright (V = 8.3 mag, K = 7.2 mag) young F-star with a period of 5.6 days. The host star, KELT-24 (HD 93148), has a T eff = {6509}-49+50 K, a mass of M * = {1.460}-0.059+0.055 M , a radius of R * = 1.506 ± 0.022 R , and an age of {0.78}-0.42+0.61 Gyr. Its planetary companion (KELT-24 b) has a radius of R P = 1.272 ± 0.021 R J and a mass of M P = {5.18}-0.22+0.21 M J, and from Doppler tomographic observations, we find that the planet's orbit is well- aligned to its host star's projected spin axis (λ ={2.6}-3.6+5.1). The young age estimated for KELT-24 suggests that it only recently started to evolve from the zero- age main sequence. KELT-24 is the brightest star known to host a transiting giant planet with a period between 5 and 10 days. Although the circularization timescale is much longer than the age of the system, we do not detect a large eccentricity or significant misalignment that is expected from dynamical migration. The brightness of its host star and its moderate surface gravity make KELT-24b an intriguing target for detailed atmospheric characterization through spectroscopic emission measurements since it would bridge the current literature results that have primarily focused on lower mass hot Jupiters and a few brown dwarfs.
An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame ImagesRodriguez, Joseph E.Quinn, Samuel N.Huang, Chelsea X.Vanderburg, AndrewPenev, KaloyanBrahm, RafaelJordán, AndrésIkwut-Ukwa, MmaTsirulik, ShellyLatham, David W.Stassun, Keivan G.Shporer, AviZiegler, CarlMatthews, ElisabethEastman, Jason D.Gaudi, B. ScottCollins, Karen A.Guerrero, NataliaRelles, Howard M.Barclay, ThomasBatalha, Natalie M.Berlind, PerryBieryla, AllysonBouma, L. G.Boyd, Patricia T.Burt, JenniferCalkins, Michael L.Christiansen, JessieCiardi, David R.Colón, Knicole D.Conti, Dennis M.Crossfield, Ian J. M.Daylan, TansuDittmann, JasonDragomir, DianaDynes, ScottEspinoza, NéstorEsquerdo, Gilbert A.Essack, ZahraGarcia Soto, AylinGlidden, AnaGünther, Maximilian N.Henning, ThomasJenkins, Jon M.Kielkopf, John F.Krishnamurthy, AkshataLaw, Nicholas M.Levine, Alan M.Lewin, PabloMann, Andrew W.Morgan, Edward H.Morris, Robert L.Oelkers, Ryan J.Paegert, MartinPepper, JoshuaQuintana, Elisa V.Ricker, George R.Rowden, PamelaSeager, SaraSarkis, PaulaSchlieder, Joshua E.Sha, LizhouTokovinin, AndreiTorres, GuillermoVanderspek, Roland K.Villanueva, Steven, Jr.Villaseñor, Jesus NoelWinn, Joshua N.Wohler, BillWong, IanYahalomi, Daniel A.Yu, LiangZhan, ZhuchangZhou, GeorgeDOI: info:10.3847/1538-3881/ab11d9v. 157191
Rodriguez, Joseph E., Quinn, Samuel N., Huang, Chelsea X., Vanderburg, Andrew, Penev, Kaloyan, Brahm, Rafael, Jordán, Andrés, Ikwut-Ukwa, Mma, Tsirulik, Shelly, Latham, David W., Stassun, Keivan G., Shporer, Avi, Ziegler, Carl, Matthews, Elisabeth, Eastman, Jason D., Gaudi, B. Scott, Collins, Karen A., Guerrero, Natalia, Relles, Howard M., Barclay, Thomas, Batalha, Natalie M., Berlind, Perry, Bieryla, Allyson, Bouma, L. G., Boyd, Patricia T. et al. 2019. "An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images." The Astronomical Journal 157:191. https://doi.org/10.3847/1538-3881/ab11d9
ID: 151870
Type: article
Authors: Rodriguez, Joseph E.; Quinn, Samuel N.; Huang, Chelsea X.; Vanderburg, Andrew; Penev, Kaloyan; Brahm, Rafael; Jordán, Andrés; Ikwut-Ukwa, Mma; Tsirulik, Shelly; Latham, David W.; Stassun, Keivan G.; Shporer, Avi; Ziegler, Carl; Matthews, Elisabeth; Eastman, Jason D.; Gaudi, B. Scott; Collins, Karen A.; Guerrero, Natalia; Relles, Howard M.; Barclay, Thomas; Batalha, Natalie M.; Berlind, Perry; Bieryla, Allyson; Bouma, L. G.; Boyd, Patricia T.; Burt, Jennifer; Calkins, Michael L.; Christiansen, Jessie; Ciardi, David R.; Colón, Knicole D.; Conti, Dennis M.; Crossfield, Ian J. M.; Daylan, Tansu; Dittmann, Jason; Dragomir, Diana; Dynes, Scott; Espinoza, Néstor; Esquerdo, Gilbert A.; Essack, Zahra; Garcia Soto, Aylin; Glidden, Ana; Günther, Maximilian N.; Henning, Thomas; Jenkins, Jon M.; Kielkopf, John F.; Krishnamurthy, Akshata; Law, Nicholas M.; Levine, Alan M.; Lewin, Pablo; Mann, Andrew W.; Morgan, Edward H.; Morris, Robert L.; Oelkers, Ryan J.; Paegert, Martin; Pepper, Joshua; Quintana, Elisa V.; Ricker, George R.; Rowden, Pamela; Seager, Sara; Sarkis, Paula; Schlieder, Joshua E.; Sha, Lizhou; Tokovinin, Andrei; Torres, Guillermo; Vanderspek, Roland K.; Villanueva, Steven, Jr.; Villaseñor, Jesus Noel; Winn, Joshua N.; Wohler, Bill; Wong, Ian; Yahalomi, Daniel A.; Yu, Liang; Zhan, Zhuchang; Zhou, George
Abstract: We report the discovery of TOI-172 b from the Transiting Exoplanet Survey Satellite (TESS) mission, a massive hot Jupiter transiting a slightly evolved G star with a 9.48-day orbital period. This is the first planet to be confirmed from analysis of only the TESS full frame images, because the host star was not chosen as a two-minute cadence target. From a global analysis of the TESS photometry and follow-up observations carried out by the TESS Follow-up Observing Program Working Group, TOI-172 (TIC 29857954) is a slightly evolved star with an effective temperature of T eff = 5645 ± 50 K, a mass of M = {1.128}-0.061+0.065 M , radius of R = {1.777}-0.044+0.047 R , a surface gravity of log g = {3.993}-0.028+0.027, and an age of {7.4}-1.5+1.6 {Gyr}. Its planetary companion (TOI-172 b) has a radius of R P = {0.965}-0.029+0.032 R J, a mass of M P = {5.42}-0.20+0.22 M J, and is on an eccentric orbit (e={0.3806}-0.0090+0.0093). TOI-172 b is one of the few known massive giant planets on a highly eccentric short-period orbit. Future study of the atmosphere of this planet and its system architecture offer opportunities to understand the formation and evolution of similar systems.
A noninteracting low-mass black hole─giant star binary systemThompson, Todd A.Kochanek, Christopher S.Stanek, Krzysztof Z.Badenes, CarlesPost, Richard S.Jayasinghe, TharinduLatham, David W.Bieryla, AllysonEsquerdo, Gilbert A.Berlind, PerryCalkins, Michael L.Tayar, JamieLindegren, LennartJohnson, Jennifer A.Holoien, Thomas W. -SAuchettl, KatieCovey, KevinDOI: info:10.1126/science.aau4005v. 366637–640
Thompson, Todd A., Kochanek, Christopher S., Stanek, Krzysztof Z., Badenes, Carles, Post, Richard S., Jayasinghe, Tharindu, Latham, David W., Bieryla, Allyson, Esquerdo, Gilbert A., Berlind, Perry, Calkins, Michael L., Tayar, Jamie, Lindegren, Lennart, Johnson, Jennifer A., Holoien, Thomas W. -S, Auchettl, Katie, and Covey, Kevin. 2019. "A noninteracting low-mass black hole─giant star binary system." Science 366:637– 640. https://doi.org/10.1126/science.aau4005
ID: 154593
Type: article
Authors: Thompson, Todd A.; Kochanek, Christopher S.; Stanek, Krzysztof Z.; Badenes, Carles; Post, Richard S.; Jayasinghe, Tharindu; Latham, David W.; Bieryla, Allyson; Esquerdo, Gilbert A.; Berlind, Perry; Calkins, Michael L.; Tayar, Jamie; Lindegren, Lennart; Johnson, Jennifer A.; Holoien, Thomas W. -S; Auchettl, Katie; Covey, Kevin
Abstract: Black hole binary systems with companion stars are typically found via their x-ray emission, generated by interaction and accretion. Noninteracting binaries are expected to be plentiful in the Galaxy but must be observed using other methods. We combine radial velocity and photometric variability data to show that the bright, rapidly rotating giant star 2MASS J05215658+4359220 is in a binary system with a massive unseen companion. The system has an orbital period of ~83 days and near- zero eccentricity. The photometric variability period of the giant is consistent with the orbital period, indicating star spots and tidal synchronization. Constraints on the giant's mass and radius imply that the unseen companion is 3.3−0.7+2.8 solar masses, indicating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star.
First Radial Velocity Results From the MINiature Exoplanet Radial Velocity Array (MINERVA)Wilson, Maurice L.Eastman, Jason D.Cornachione, Matthew A.Wang, Sharon X.Johnson, Samson A.Sliski, David H.Schap, William J.,IIIMorton, Timothy D.Johnson, John AsherMcCrady, NateWright, Jason T.Wittenmyer, Robert A.Plavchan, PeterBlake, Cullen H.Swift, Jonathan J.Bottom, MichaelBaker, Ashley D.Barnes, Stuart I.Berlind, PerryBlackhurst, EricBeatty, Thomas G.Bolton, Adam S.Cale, BrysonCalkins, Michael L.Colón, Anade Vera, JonEsquerdo, GilbertFalco, Emilio E.Fortin, PascalGarcia-Mejia, JulianaGeneser, ClaireGibson, Steven R.Grell, GabrielGroner, TedHalverson, SamuelHamlin, JohnHenderson, M.Horner, J.Houghton, AudreyJanssens, StefaanJonas, GraemeJones, DamienKirby, AnnieLawrence, GeorgeLuebbers, Julien AndrewMuirhead, Philip S.Myles, JustinNava, ChantanelleRivera-García, Kevin O.Reed, TonyRelles, Howard M.Riddle, ReedRobinson, ConnorChaput de Saintonge, ForestSergi, AnthonyDOI: info:10.1088/1538-3873/ab33c5v. 131115001
Wilson, Maurice L., Eastman, Jason D., Cornachione, Matthew A., Wang, Sharon X., Johnson, Samson A., Sliski, David H., Schap, William J.,III, Morton, Timothy D., Johnson, John Asher, McCrady, Nate, Wright, Jason T., Wittenmyer, Robert A., Plavchan, Peter, Blake, Cullen H., Swift, Jonathan J., Bottom, Michael, Baker, Ashley D., Barnes, Stuart I., Berlind, Perry, Blackhurst, Eric, Beatty, Thomas G., Bolton, Adam S., Cale, Bryson, Calkins, Michael L., Colón, Ana et al. 2019. "First Radial Velocity Results From the MINiature Exoplanet Radial Velocity Array (MINERVA)." Publications of the Astronomical Society of the Pacific 131:115001. https://doi.org/10.1088/1538-3873/ab33c5
ID: 154440
Type: article
Authors: Wilson, Maurice L.; Eastman, Jason D.; Cornachione, Matthew A.; Wang, Sharon X.; Johnson, Samson A.; Sliski, David H.; Schap, William J.,III; Morton, Timothy D.; Johnson, John Asher; McCrady, Nate; Wright, Jason T.; Wittenmyer, Robert A.; Plavchan, Peter; Blake, Cullen H.; Swift, Jonathan J.; Bottom, Michael; Baker, Ashley D.; Barnes, Stuart I.; Berlind, Perry; Blackhurst, Eric; Beatty, Thomas G.; Bolton, Adam S.; Cale, Bryson; Calkins, Michael L.; Colón, Ana; de Vera, Jon; Esquerdo, Gilbert; Falco, Emilio E.; Fortin, Pascal; Garcia-Mejia, Juliana; Geneser, Claire; Gibson, Steven R.; Grell, Gabriel; Groner, Ted; Halverson, Samuel; Hamlin, John; Henderson, M.; Horner, J.; Houghton, Audrey; Janssens, Stefaan; Jonas, Graeme; Jones, Damien; Kirby, Annie; Lawrence, George; Luebbers, Julien Andrew; Muirhead, Philip S.; Myles, Justin; Nava, Chantanelle; Rivera-García, Kevin O.; Reed, Tony; Relles, Howard M.; Riddle, Reed; Robinson, Connor; Chaput de Saintonge, Forest; Sergi, Anthony
Abstract: The MINiature Exoplanet Radial Velocity Array (MINERVA) is a dedicated observatory of four 0.7 m robotic telescopes fiber-fed to a KiwiSpec spectrograph. The MINERVA mission is to discover super-Earths in the habitable zones of nearby stars. This can be accomplished with MINERVA's unique combination of high precision and high cadence over long time periods. In this work, we detail changes to the MINERVA facility that have occurred since our previous paper. We then describe MINERVA's robotic control software, the process by which we perform 1D spectral extraction, and our forward modeling Doppler pipeline. In the process of improving our forward modeling procedure, we found that our spectrograph's intrinsic instrumental profile is stable for at least nine months. Because of that, we characterized our instrumental profile with a time-independent, cubic spline function based on the profile in the cross dispersion direction, with which we achieved a radial velocity precision similar to using a conventional "sum-of-Gaussians" instrumental profile: 1.8 m s-1 over 1.5 months on the RV standard star HD 122064. Therefore, we conclude that the instrumental profile need not be perfectly accurate as long as it is stable. In addition, we observed 51 Peg and our results are consistent with the literature, confirming our spectrograph and Doppler pipeline are producing accurate and precise radial velocities.
Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pcWinters, Jennifer G.Medina, Amber A.Irwin, Jonathan M.Charbonneau, DavidAstudillo-Defru, NicolaHorch, Elliott P.Eastman, Jason D.Halley Vrijmoet, EliotHenry, Todd J.Diamond-Lowe, HannahWinston, ElaineBarclay, ThomasBonfils, XavierRicker, George R.Vanderspek, RolandLatham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Udry, StéphaneTwicken, Joseph D.Teske, Johanna K.Tenenbaum, PeterPepe, FrancescoMurgas, FelipeMuirhead, Philip S.Mink, JessicaLovis, ChristopheLevine, Alan M.Lépine, SébastienJao, Wei-ChunHenze, Christopher E.Furész, GáborForveille, ThierryFigueira, PedroEsquerdo, Gilbert A.Dressing, Courtney D.Díaz, Rodrigo F.Delfosse, XavierBurke, Christopher J.Bouchy, FrançoisBerlind, PerryAlmenara, Jose-ManuelDOI: info:10.3847/1538-3881/ab364dv. 158152
Winters, Jennifer G., Medina, Amber A., Irwin, Jonathan M., Charbonneau, David, Astudillo-Defru, Nicola, Horch, Elliott P., Eastman, Jason D., Halley Vrijmoet, Eliot, Henry, Todd J., Diamond-Lowe, Hannah, Winston, Elaine, Barclay, Thomas, Bonfils, Xavier, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Udry, Stéphane, Twicken, Joseph D., Teske, Johanna K., Tenenbaum, Peter, Pepe, Francesco, Murgas, Felipe et al. 2019. "Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pc." The Astronomical Journal 158:152. https://doi.org/10.3847/1538-3881/ab364d
ID: 154724
Type: article
Authors: Winters, Jennifer G.; Medina, Amber A.; Irwin, Jonathan M.; Charbonneau, David; Astudillo-Defru, Nicola; Horch, Elliott P.; Eastman, Jason D.; Halley Vrijmoet, Eliot; Henry, Todd J.; Diamond-Lowe, Hannah; Winston, Elaine; Barclay, Thomas; Bonfils, Xavier; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Udry, Stéphane; Twicken, Joseph D.; Teske, Johanna K.; Tenenbaum, Peter; Pepe, Francesco; Murgas, Felipe; Muirhead, Philip S.; Mink, Jessica; Lovis, Christophe; Levine, Alan M.; Lépine, Sébastien; Jao, Wei-Chun; Henze, Christopher E.; Furész, Gábor; Forveille, Thierry; Figueira, Pedro; Esquerdo, Gilbert A.; Dressing, Courtney D.; Díaz, Rodrigo F.; Delfosse, Xavier; Burke, Christopher J.; Bouchy, François; Berlind, Perry; Almenara, Jose-Manuel
Abstract: We present the discovery from Transiting Exoplanet Survey Satellite (TESS) data of LTT 1445Ab. At a distance of 6.9 pc, it is the second nearest transiting exoplanet system found to date, and the closest one known for which the primary is an M dwarf. The host stellar system consists of three mid-to-late M dwarfs in a hierarchical configuration, which are blended in one TESS pixel. We use MEarth data and results from the Science Processing Operations Center data validation report to determine that the planet transits the primary star in the system. The planet has a radius of {1.38}-0.12+0.13 {R}\oplus , an orbital period of {5.35882}-0.00031+0.00030 days, and an equilibrium temperature of {433}-27+28 K. With radial velocities from the High Accuracy Radial Velocity Planet Searcher, we place a 3σ upper mass limit of 8.4 {M}\oplus on the planet. LTT 1445Ab provides one of the best opportunities to date for the spectroscopic study of the atmosphere of a terrestrial world. We also present a detailed characterization of the host stellar system. We use high-resolution spectroscopy and imaging to rule out the presence of any other close stellar or brown dwarf companions. Nineteen years of photometric monitoring of A and BC indicate a moderate amount of variability, in agreement with that observed in the TESS light-curve data. We derive a preliminary astrometric orbit for the BC pair that reveals an edge-on and eccentric configuration. The presence of a transiting planet in this system hints that the entire system may be co- planar, implying that the system may have formed from the early fragmentation of an individual protostellar core.
Two New HATNet Hot Jupiters around A Stars and the First Glimpse at the Occurrence Rate of Hot Jupiters from TESSZhou, GeorgeHuang, C. X.Bakos, G. Á.Hartman, J. D.Latham, David W.Quinn, Samuel N.Collins, Karen A.Winn, J. N.Wong, I.Kovács, G.Csubry, Z.Bhatti, W.Penev, K.Bieryla, AllysonEsquerdo, Gilbert A.Berlind, PerryCalkins, Michael L.de Val-Borro, M.Noyes, R. W.Lázár, J.Papp, I.Sári, P.Kovács, T.Buchhave, Lars A.Szklenar, T.Béky, B.Johnson, M. C.Cochran, W. D.Kniazev, A. Y.Stassun, K. G.Fulton, B. J.Shporer, A.Espinoza, N.Bayliss, D.Everett, M.Howell, S. B.Hellier, C.Anderson, D. R.Collier Cameron, A.West, R. G.Brown, D. J. A.Schanche, N.Barkaoui, K.Pozuelos, F.Gillon, M.Jehin, E.Benkhaldoun, Z.Daassou, A.Ricker, G.Vanderspek, R.Seager, S.Jenkins, J. M.Lissauer, Jack J.Armstrong, J. D.Collins, K. I.Gan, T.Hart, R.Horne, K.Kielkopf, J. F.Nielsen, L. D.Nishiumi, T.Narita, N.Palle, E.Relles, Howard M.Sefako, R.Tan, T. G.Davies, M.Goeke, Robert F.Guerrero, N.Haworth, K.Villanueva, S.DOI: info:10.3847/1538-3881/ab36b5v. 158141
Zhou, George, Huang, C. X., Bakos, G. Á., Hartman, J. D., Latham, David W., Quinn, Samuel N., Collins, Karen A., Winn, J. N., Wong, I., Kovács, G., Csubry, Z., Bhatti, W., Penev, K., Bieryla, Allyson, Esquerdo, Gilbert A., Berlind, Perry, Calkins, Michael L., de Val-Borro, M., Noyes, R. W., Lázár, J., Papp, I., Sári, P., Kovács, T., Buchhave, Lars A., Szklenar, T. et al. 2019. "Two New HATNet Hot Jupiters around A Stars and the First Glimpse at the Occurrence Rate of Hot Jupiters from TESS." The Astronomical Journal 158:141. https://doi.org/10.3847/1538-3881/ab36b5
ID: 154718
Type: article
Authors: Zhou, George; Huang, C. X.; Bakos, G. Á.; Hartman, J. D.; Latham, David W.; Quinn, Samuel N.; Collins, Karen A.; Winn, J. N.; Wong, I.; Kovács, G.; Csubry, Z.; Bhatti, W.; Penev, K.; Bieryla, Allyson; Esquerdo, Gilbert A.; Berlind, Perry; Calkins, Michael L.; de Val-Borro, M.; Noyes, R. W.; Lázár, J.; Papp, I.; Sári, P.; Kovács, T.; Buchhave, Lars A.; Szklenar, T.; Béky, B.; Johnson, M. C.; Cochran, W. D.; Kniazev, A. Y.; Stassun, K. G.; Fulton, B. J.; Shporer, A.; Espinoza, N.; Bayliss, D.; Everett, M.; Howell, S. B.; Hellier, C.; Anderson, D. R.; Collier Cameron, A.; West, R. G.; Brown, D. J. A.; Schanche, N.; Barkaoui, K.; Pozuelos, F.; Gillon, M.; Jehin, E.; Benkhaldoun, Z.; Daassou, A.; Ricker, G.; Vanderspek, R.; Seager, S.; Jenkins, J. M.; Lissauer, Jack J.; Armstrong, J. D.; Collins, K. I.; Gan, T.; Hart, R.; Horne, K.; Kielkopf, J. F.; Nielsen, L. D.; Nishiumi, T.; Narita, N.; Palle, E.; Relles, Howard M.; Sefako, R.; Tan, T. G.; Davies, M.; Goeke, Robert F.; Guerrero, N.; Haworth, K.; Villanueva, S.
Abstract: Wide-field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of planets and their parent stars. We report the discovery of HAT-P-69 b (TOI 625.01) and HAT-P-70 b (TOI 624.01), two new hot Jupiters around A stars from the Hungarian-made Automated Telescope Network (HATNet) survey that have also been observed by the Transiting Exoplanet Survey Satellite. HAT-P-69 b has a mass of {3.58}-0.58+0.58 M Jup and a radius of {1.676}-0.033+0.051 R Jup and resides in a prograde 4.79 day orbit. HAT-P-70 b has a radius of {1.87}-0.10+0.15 R Jup and a mass constraint of and a mass constraint of Jup and resides in a retrograde 2.74 day orbit. We use the confirmation of these planets around relatively massive stars as an opportunity to explore the occurrence rate of hot Jupiters as a function of stellar mass. We define a sample of 47,126 main-sequence stars brighter than T mag = 10 that yields 31 giant planet candidates, including 18 confirmed planets, 3 candidates, and 10 false positives. We find a net hot Jupiter occurrence rate of 0.41 ± 0.10% within this sample, consistent with the rate measured by Kepler for FGK stars. When divided into stellar mass bins, we find the occurrence rate to be 0.71 ± 0.31% for G stars, 0.43 ± 0.15% for F stars, and 0.26 ± 0.11% for A stars. Thus, at this point, we cannot discern any statistically significant trend in the occurrence of hot Jupiters with stellar mass. Based on observations obtained with the Hungarian-made Automated Telescope Network. Based in part on observations obtained with the Tillinghast Reflector 1.5 m telescope and the 1.2 m telescope, both operated by the Smithsonian Astrophysical Observatory at the Fred Lawrence Whipple Observatory in Arizona. This work makes use of the Smithsonian Institution High Performance Cluster (SI/HPC). Based in part on observations made with the Southern African Large Telescope (SALT).