18 research outputs found
Golf’s Civil War: The Antitrust Lessons to Learn from the PGA Tour’s Rivalry with LIV Golf
Get PDFThe regulation of professional sports leagues under the Sherman Act presents a unique and, up to this point, unsolved problem. Increased regulation of the United States’ beloved sports is not something that many US citizens would necessarily welcome. And yet, courts are consistently confronted with the dilemma of checking competition “off the field” while attempting to leave unaffected the competition “on the field.” In doing so, courts must reconcile the principles and objectives of the Sherman Act (the Act) with the restraints necessary for the success of sports as an enterprise. While mirroring some of the aspects of traditional trade and business usually subject to the Sherman Act, the inescapable fact is that sports leagues are unique entities and, as such, require different perspectives in the application of governing law.
Using a now-resolved lawsuit filed against the PGA Tour as a case study, this Note explores the application of the Sherman Act to professional sports leagues and how the results have led to an inconsistent, noncommittal string of decisions, leaving the state of the law in flux. Furthermore, this Note addresses the proposition of a more consistent application of the Sherman Act and its intricacies, comparing economically grounded goals of preserving “on the field” competition with the Act’s inherent goals of promoting a competitive “off the field” marketplace
A hop, a frock, a hairdo: a hop, a frock, a hairdo: Irene Castle and her female networks of theatrical business
No full textFocusing on American dancer/performer Irene Castle (1893-1969) and following the merchandising strategies and aesthetic and societal impact of her widely discussed short haircut, her costumes, and her dancing school, this article aims at describing and disentangling the tight network of theatrical and popular entertainment, economy, and urbanity in the 1910s. Through an interdisciplinary approach and with a focus on a limited time frame of five years (1910-1915), the author discusses various strands, agents, contact zones and business strategies that are part and parcel of this network. Next to Irene Castle, two female theatre professionals are of particular interest here: costume designer Lady Duff-Gordon (1863-1935) and theatrical agent Elizabeth Marbury (1856-1933). Nic Leonhardt is a theatre and media historian with a special interest in historiography, visual culture, popular culture, and urban history. She is currently associate director and researcher of the DFG research project “Global Theatre Histories” at LMU Munich, Germany, and a lecturer in theatre studies
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Session A8: An Evaluation of Fishway Passage for Alewife (Alosa pseudoharengus)
No full textPresenting Author Bio: MJWS is a Tier II Canada Research Chair in the Ecology of Coastal Environments, and an Associate Professor in the Biology Department at Acadia University.Abstract: Alewives (Alosa pseudoharengus) are anadromous fish that often encounter fishways when migrating upstream to their spawning habitat. In partnership with Ducks Unlimited Canada, we are quantifying attraction efficiency, passage efficiency and time of movement of alewife through fishways. To do this we tagged 790 fish with Passive Integrated Transponders (PIT) and tracked their movement through two Denil style fishways. Overall attraction efficiency to fishways was 44%, but passage efficiency was ≥74%. Tagged fish were most active at dawn and dusk. Tagged alewife detected at the base of the fishway were significantly longer than undetected individuals, and may have been experienced migrants. Our data suggest that quantification of the number of migrants that are motivated to attempt passage of fishways has implications for measures of true fishway attraction and passage efficiency for defining “effective fishways”
Health-state estimation and prognostics in machining processes
Get PDFFailure mechanisms of electromechanical systems usually involve several degraded
health-states. Tracking and forecasting the evolution of health-states and
impending failures, in the form of remaining-useful-life (RUL), is a critical
challenge and regarded as the Achilles' heel of condition-based-maintenance
(CBM). This paper demonstrates how this difficult problem can be addressed
through Hidden Markov models (HMMs) that are able to estimate unobservable
health-states using observable sensor signals. In particular, implementation of
HMM based models as dynamic Bayesian networks (DBNs) facilitates compact
representation as well as additional flexibility with regard to model structure.
Both regular HMM pools and hierarchical HMMs are employed here to estimate
online the health-state of drill-bits as they deteriorate with use on a CNC
drilling machine. Hierarchical HMM is composed of sub-HMMs in a pyramid
structure, providing functionality beyond an HMM for modeling complex systems.
In the case of regular HMMs, each HMM within the pool competes to represent a
distinct health-state and adapts through competitive learning. In the case of
hierarchical HMMs, health-states are represented as distinct nodes at the top of
the hierarchy. Monte Carlo simulation, with state transition probabilities
derived from a hierarchical HMM, is employed for RUL estimation. Detailed
results on health-state and RUL estimation are very promising and are reported
in this paper. Hierarchical HMMs seem to be particularly effective and efficient
and outperform other HMM methods from literature
Who is going to save the final girl? the politics of representation in the films halloween and the silence of the lambs
Get PDFTese (doutorado) - Universidade Federal de Santa Catarina, Centro de Comunicação e Expressão, Programa de Pós-Graduação em Inglês: Estudos Linguísticos e Literários, Florianópolis, 2014Abstract: This dissertation aims at analyzing female representations in two film productions of the North American horror cinema, specifically of its subgenre slasher films, namely Halloween, directed by John Carpenter (1978) and The Silence of the Lambs, directed by Jonathan Demme (1991). My main theoretical framework is film, representation, gender, feminist and queer theories (Butler, 1990, 1993; Clover, 1989; Dika, 1985, Halberstam, 1995; Hall 1973, 1997; Mulvey, 1975, 1981; 2006; Rockoff, 2006; Weedon, 1995). My hypothesis is that the figure of the final girl, in the two films selected for analysis, is not progressive as suggested by the author Carol Clover in her work Men, Women and Chainsaws (1989). On the contrary, the two female characters are represented, in the narrative, as subjugated by the patriarchal system that has been conventionalized in the slasher subgenre. In order to provide arguments for my hypothesis, I analyze general aspects of both form and content of the two films, as well as specific scenes, using the cinematic elements of mise-en-scène, props, characterization, editing and lighting in order to obtain relevant results for my research.Esta tese de doutorado objetiva analisar as representações femininas em duas produções cinematográficas do cinema de horror Norte-americano, especificamente do seu subgênero slasher films, intituladas Halloween, dirigido por John Carpenter (1978) e The Silenceof the Lambs, dirigido por Jonathan Demme (1991). Para tal análise, eu utilizo como referencial teórico as teorias de estudos de cinema, representação, gênero, feministas e queer (Butler, 1990, 1993; Clover, 1989; Dika, 1985; Halberstam, 1995; Hall, 1973, 1997; Halberstam, 1995; Mulvey, 1975; 1981; 2006; Rockoff, 2006; Weedon, 1995) para compor os meus argumentos. A minha hipótese consiste no fato de que a figura da final girl não é inovadora como sugere a autora Carol Clover em sua obra Men, Women and Chainsaws (1989). Ao contrário, a personagem feminina é representada na narrativa como subjugada pelo sistema patriarcal que se convencionou em filmes do gênero. Para a investigação da minha hipótese, foram feitas análises gerais dos filmes propostos, tanto considerando suas formas quanto conteúdos, bem como a de cenas específicas, utilizando-se dos elementos de cinema tais como mise-èn-scene, elementos de cena, caracterização de personagens, edição e luz a fim de obter resultados relevantes para a minha pesquisa
VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
No full textMistry, Priyashkumar et al.--Full list of authors: Mistry, Priyashkumar; Pathak, Kamlesh; Prasad, Aniket; Lekkas, Georgios; Bhattarai, Surendra; Gharat, Sarvesh; Maity, Mousam; Kumar, Dhruv; Collins, Karen A.; Schwarz, Richard P.; Mann, Christopher R.; Furlan, Elise; Howell, Steve B.; Ciardi, David; Bieryla, Allyson; Matthews, Elisabeth C.; Gonzales, Erica; Ziegler, Carl; Crossfield, Ian; Giacalone, Steven; Tan, Thiam-Guan; Evans, Phil; Helminiak, Krzysztof G.; Collins, Kevin I.; Narita, Norio; Fukui, Akihiko; Pozuelos, Francisco J.; Dressing, Courtney; Soubkiou, Abderahmane; Benkhaldoun, Zouhair; Schlieder, Joshua E.; Suarez, Olga; Barkaoui, Khalid; Palle, Enric; Murgas, Felipe; Srdoc, Gregor; Goliguzova, Maria V.; Strakhov, Ivan A.; Gnilka, Crystal; Lester, Kathryn; Littlefield, Colin; Scott, Nic; Matson, Rachel; Gillon, Michael; Jehin, Emmanuel; Timmermans, Mathilde; Ghachoui, Mourad; Abe, Lyu; Bendjoya, Philippe; Guillot, Tristan; Triaud, Amaury H. M. J.NASA's Transiting Exoplanet Survey Satellite (TESS) is an all-sky survey mission designed to find transiting exoplanets orbiting nearby bright stars. It has identified more than 329 transiting exoplanets, and almost 6000 candidates remain unvalidated. In this manuscript, we discuss the findings from the ongoing Validation of Transiting Exoplanets using Statistical Tools (VaTEST) project, which aims to validate new exoplanets for further characterization. We validated 11 new exoplanets by examining the light curves of 24 candidates using the LATTE and TESS-Plot tools and computing the false-positive probabilities using the statistical validation tool TRICERATOPS. These include planets suitable for atmospheric characterization using transmission spectroscopy (TOI-2194b), emission spectroscopy (TOI-3082b and TOI-5704b) and for both transmission and emission spectroscopy (TOI-672b, TOI-1694b, and TOI-2443b). Our validated planets have one super-Earth (TOI-2194b) orbiting a bright (V = 8.42 mag), metal-poor ([Fe/H] = −0.3720 ± 0.1) star, and one short-period Neptune-like planet (TOI-5704) in the hot-Neptune desert. In total, we validated one super-Earth, seven sub-Neptunes, one Neptune-like, and two sub-Saturn or super-Neptune-like exoplanets. Additionally, we identify five likely planet candidates (TOI-323, TOI-1180, TOI-2200, TOI-2408, and TOI-3913), which can be further studied to establish their planetary nature. © 2023. The Author(s). Published by the American Astronomical Society.M.V.G. and I.A.S. acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). Funding for the TESS mission is provided by NASA's Science Mission Directorate. KAC acknowledges support from the TESS mission via subaward s3449 from MIT. Some of the observations in this paper made use of the High-Resolution Imaging instruments 'Alopeke and Zorro and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. 'Alopeke and Zorro were funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. 'Alopeke was mounted on the Gemini North telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. On behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper makes use of observations made with the MuSCAT2 instrument, developed by the Astrobiology Center, at TCS operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This paper is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI:10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This publication makes use of data products collected by the TESS mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). The light curve and target pixel file data used in this paper can be found in 10.17909/t9-nmc8-f686. C.M. would like to gratefully acknowledge the entire Dragonfly Telephoto Array team, and Bob Abraham in particular, for allowing their telescope bright time to be put to use observing exoplanets. TRAPPIST-South is funded by the Belgian National Fund for Scientific Research (F.R.S.-FNRS) under grant PDR T.0120.21, with the participation of the Swiss National Science Fundation (SNF). M.G. is F.R.S-FNRS Research Director. E.J. is F.R.S-FNRS Senior Research Associate. The postdoctoral fellowship of KB is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to MT. F.J.P. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. This research received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement n° 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1). This work makes use of observations from the ASTEP telescope. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from INSU, ESA, the University of Birmingham, and STFC.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
Validation of 13 Hot and Potentially Terrestrial TESS Planets
No full textAuthors: Steven Giacalone , Courtney D. Dressing , Christina Hedges, Veselin B. Kostov, Karen A. Collins , Eric L. N. Jensen , Daniel A. Yahalomi, Allyson Bieryla , David R. Ciardi , Steve B. Howell , Jorge Lillo-Box , Khalid Barkaoui, Jennifer G. Winters , Elisabeth Matthews , John H. Livingston , Samuel N. Quinn , Boris S. Safonov , Charles Cadieux, E. Furlan , Ian J. M. Crossfield, Avi M. Mandell , Emily A. Gilbert, Ethan Kruse , Elisa V. Quintana , George R. Ricker , S. Seager, Joshua N. Winn , Jon M. Jenkins , Britt Duffy Adkins, David Baker , Thomas Barclay, David Barrado , Natalie M. Batalha , Alexander A. Belinski , Zouhair Benkhaldoun , Lars A. Buchhave , Luca Cacciapuoti, David Charbonneau , Ashley Chontos, Jessie L. Christiansen , Ryan Cloutier, Kevin I. Collins , Dennis M. Conti , Neil Cutting, Scott Dixon, René Doyon, Mohammed El Mufti, Emma Esparza-Borges, Zahra Essack, Akihiko Fukui, Tianjun Gan , Kaz Gary , Mourad Ghachoui, Michaël Gillon , Eric Girardin , Ana Glidden, Erica J. Gonzales, Pere Guerra, Elliott P. Horch , Krzysztof G. Hełminiak , Andrew W. Howard , Daniel Huber , Jonathan M. Irwin , Giovanni Isopi, Emmanuël Jehin , Taiki Kagetani , Stephen R. Kane , Kiyoe Kawauchi , John F. Kielkopf , Pablo Lewin , Lindy Luker, Michael B. Lund , Franco Mallia, Shude Mao, Bob Massey , Rachel A. Matson , Ismael Mireles , Mayuko Mori , Felipe Murgas, Norio Narita, Tanner O’Dwyer, Erik A. Petigura , Alex S. Polanski , Francisco J. Pozuelos, Enric Palle, Hannu Parviainen, Peter P. Plavchan , Howard M. Relles , Paul Robertson , Mark E. Rose , Pamela Rowden , Arpita Roy, Arjun B. Savel , Joshua E. Schlieder , Chloe Schnaible, Richard P. Schwarz , Ramatholo Sefako, Aleksandra Selezneva , Brett Skinner, Chris Stockdale , Ivan A. Strakhov , Thiam-Guan Tan , Guillermo Torres , René Tronsgaard , Joseph D. Twicken, David Vermilion, Ian A. Waite , Bradley Walter, Gavin Wang, Carl Ziegler, and Yujie ZouThe Astronomical Journal
The American Astronomical Society, find out more
The Institute of Physics, find out more
THE FOLLOWING ARTICLE ISOPEN ACCESS
Validation of 13 Hot and Potentially Terrestrial TESS Planets
Steven Giacalone1, Courtney D. Dressing1, Christina Hedges2,3, Veselin B. Kostov4,5, Karen A. Collins6, Eric L. N. Jensen7, Daniel A. Yahalomi6,8, Allyson Bieryla6, David R. Ciardi9, Steve B. Howell3Show full author list
Published 2022 January 28 • © 2022. The Author(s). Published by the American Astronomical Society.
The Astronomical Journal, Volume 163, Number 2
Citation Steven Giacalone et al 2022 AJ 163 99
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Abstract
The James Webb Space Telescope will be able to probe the atmospheres and surface properties of hot, terrestrial planets via emission spectroscopy. We identify 18 potentially terrestrial planet candidates detected by the Transiting Exoplanet Survey Satellite (TESS) that would make ideal targets for these observations. These planet candidates cover a broad range of planet radii (Rₚ ∼ 0.6–2.0R⊕) and orbit stars of various magnitudes (Kₛ = 5.78–10.78, V = 8.4–15.69) and effective temperatures (Tₑᶠᶠ ∼ 3000–6000 K). We use ground-based observations collected through the TESS Follow-up Observing Program (TFOP) and two vetting tools—DAVE and TRICERATOPS—to assess the reliabilities of these candidates as planets. We validate 13 planets: TOI-206 b, TOI-500 b, TOI-544 b, TOI-833 b, TOI-1075 b, TOI-1411 b, TOI-1442 b, TOI-1693 b, TOI-1860 b, TOI-2260 b, TOI-2411 b, TOI-2427 b, and TOI-2445 b. Seven of these planets (TOI-206 b, TOI-500 b, TOI-1075 b, TOI-1442 b, TOI-2260 b, TOI-2411 b, and TOI-2445 b) are ultra-short-period planets. TOI-1860 is the youngest (133 ± 26 Myr) solar twin with a known planet to date. TOI-2260 is a young (321 ± 96 Myr) G dwarf that is among the most metal-rich ([Fe/H] = 0.22 ± 0.06 dex) stars to host an ultra-short-period planet. With an estimated equilibrium temperature of ∼2600 K, TOI-2260 b is also the fourth hottest known planet with Rₚ < 2 R⊕.We thank the NASA TESS Guest Investigator Program for
supporting this work through grant 80NSSC18K1583 (awarded
to C.D.D.). S.G. and C.D.D. also appreciate and acknowledge
support from the Hellman Fellows Fund, the Alfred P. Sloan
Foundation, the David and Lucile Packard Foundation, and the
NASA Exoplanets Research Program (XRP) through grant
80NSSC20K0250.
We acknowledge the use of public TESS Alert data from the
pipelines at the TESS Science Office and at the TESS Science
Processing Operations Center. Resources supporting this work
were provided by the NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center for the production of the
SPOC data products.
Data presented herein were obtained at the WIYN
Observatory from telescope time allocated to NN-EXPLORE
through the scientific partnership of the National Aeronautics
and Space Administration, the National Science Foundation,
and the National Optical Astronomy Observatory. NESSI was
funded by the NASA Exoplanet Exploration Program and the
NASA Ames Research Center. NESSI was built at the Ames
Research Center by S.B.H., Nic Scott, E.P.H., and Emmett
Quigley. The authors are honored to be permitted to conduct
observations on Iolkam Du’ag (Kitt Peak), a mountain within
the Tohono O’odham Nation with particular significance to the
Tohono O’odham people.
MEarth is funded by the David and Lucile Packard
Fellowship for Science and Engineering, the National Science
Foundation under grants AST-0807690, AST-1109468, AST 1004488 (Alan T. Waterman Award) and AST-1616624, and
the John Templeton Foundation. This publication was made
possible through the support of a grant from the John
Templeton Foundation. The opinions expressed in this
publication are those of the authors and do not necessarily
reflect the views of the John Templeton Foundation.
The authors wish to recognize and acknowledge the very
significant cultural role and reverence that the summit of
Maunakea has always had within the indigenous Hawaiian
community. We are most fortunate to have the opportunity to
conduct observations from this mountain. D.H. acknowledges
support from the Alfred P. Sloan Foundation, the National
Aeronautics and Space Administration (80NSSC18K1585,
80NSSC19K0379), and the National Science Foundation
(AST-1717000).
Some of the observations in the paper made use of the High Resolution Imaging instrument(s) ‘Alopeke (and/or Zorro).
‘Alopeke (and/or Zorro) was funded by the NASA Exoplanet
Exploration Program and built at the NASA Ames Research
Center by S.B.H., Nic Scott, E.P.H., and Emmett Quigley. Data were reduced using a software pipeline originally written by
E. P. Horch and Mark Everett. ‘Alopeke (and/or Zorro) was
mounted on the Gemini North (and/or South) telescope of the
international Gemini Observatory, a program of NSFʼs OIR
Lab, which is managed by the Association of Universities for
Research in Astronomy (AURA) under a cooperative agree ment with the National Science Foundation. on behalf of the
Gemini partnership: the National Science Foundation (United
States), National Research Council (Canada), Agencia Nacio nal de Investigación y Desarrollo (Chile), Ministerio de
Ciencia, Tecnología e Innovación (Argentina), Ministério da
Ciência, Tecnologia, Inovações e Comunicações (Brazil), and
Korea Astronomy and Space Science Institute (Republic of
Korea). These observations were collected under program GN 2019B-LP-101. Observations acquired with Gemini-S/DSSI
were collected as a part of program GS-2018A-Q-202 (PI: J.
Winters).
Some of the results in this paper are based on observations
made with the Nordic Optical Telescope, operated by the
Nordic Optical Telescope Scientific Association at the
Observatorio del Roque de los Muchachos, La Palma, Spain,
of the Instituto de Astrofisica de Canarias. A.A.B., B.S.S., and
I.A.S. acknowledge the support of the Ministry of Science and
Higher Education of the Russian Federation under grant 075-
15-2020-780 (N13.1902.21.0039).
This paper is partially based on observations made at the
CMO SAI MSU with the support of the M.V. Lomonosov
Moscow State University Program of Development.
Based on observations at Cerro Tololo Inter-American
Observatory at NSFʼs NOIRLab (NOIRLab Prop. IDs
2019A-0294, 2019B-0302, 2020A-0390, 2020B-0262,
2021A-0268; PI: S. Quinn), which is managed by the
Association of Universities for Research in Astronomy
(AURA) under a cooperative agreement with the National
Science Foundation. This research has been supported by
RECONS (www.recons.org) members Todd Henry, Hodari
James, Leonardo Paredes, and Wei-Chun Jao, who provided
data as part of the CHIRON program on the CTIO/SMARTS
1.5 m, which is operated as part of the SMARTS Consortium.
The research leading to these results has received funding
from the ARC grant for Concerted Research Actions, financed
by the Wallonia-Brussels Federation. TRAPPIST is funded by
the Belgian Fund for Scientific Research (Fond National de la
Recherche Scientifique, FNRS) under the grant PDR
T.0120.21, with the participation of the Swiss National Science
Foundation (SNF). M. Gillon and E.J. are F.R.S.-FNRS Senior
Research Associate.
This work is partly supported by JSPS KAKENHI grant
Nos. JP20K14518, JP17H04574, and JP18H05439, grant-in Aid for JSPS Fellows, grant No. JP20J21872, JST PRESTO
grant No. JPMJPR1775, JST CREST grant No. JPMJCR1761,
and the Astrobiology Center of National Institutes of Natural
Sciences (NINS) (grant No. AB031010).
This paper is based on observations made with the
MuSCAT2 instrument, developed by ABC, at Telescopio
Carlos Sánchez operated on the island of Tenerife by the IAC
in the Spanish Observatorio del Teide.
This paper is based on observations made with the
MuSCAT3 instrument, developed by the Astrobiology Center
and under financial supports by JSPS KAKENHI
(JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres
Observatory.
This work makes use of observations from the LCOGT
network.
Work by J.N.W. was supported by the Heising-Simons
Foundation.
We thank Rhodes Hart for his contributions to this paper.
Facilities: TESS, CAO:2.2 m (AstraLux), WIYN (NESSI),
SOAR (HRCam), Shane (ShARCS), Hale (PHARO),
Gemini:Gillett (’Alopeke), Gemini:South (Zorro and DSSI),
Keck:II (NIRC2), FLWO:1.5 m (TRES), NOT (FIES),
CTIO:1.5 m (CHIRON), Keck:I (HIRES), MEearth, LCOGT,
OMM:1.6 (PESTO), OAO:1.88 m (MuSCAT), TRAPPIST,
SAAO:0.5 m, Sanchez (MuSCAT2).https://iopscience.iop.org/article/10.3847/1538-3881/ac4334/met
The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs
No full textHori, Yasunori et al.--Full list of authors: Hori, Yasunori; Fukui, Akihiko; Hirano, Teruyuki; Narita, Norio; de Leon, Jerome P.; Ishikawa, Hiroyuki Tako; Hartman, Joel D.; Morello, Giuseppe; García, Nestor Abreu; Álvarez Hernández, Leticia ; Béjar, Víctor J. S.; Calatayud-Borras, Yéssica; Carleo, Ilaria; Enoc, Gareb; Esparza-Borges, Emma; Fukuda, Izuru; Galán, Daniel; Geraldía-González, Samuel; Hayashi, Yuya; Ikoma, Masahiro; Ikuta, Kai; Isogai, Keisuke; Kagetani, Taiki; Kawai, Yugo; Kawauchi, Kiyoe; Kimura, Tadahiro; Kodama, Takanori; Korth, Judith; Kusakabe, Nobuhiko; Laza-Ramos, Andrés; Livingston, John H.; Luque, Rafael; Miyakawa, Kohei; Mori, Mayuko; Murgas, Felipe; Orell-Miquel, Jaume; Palle, Enric; Parviainen, Hannu; Peláez-Torres, Alberto; Puig-Subirà, Marta; Sánchez-Benavente, Manuel; Sosa-Guillén, Paula; Stangret, Monika; Terada, Yuka; Muñoz Torres, Sara; Watanabe, Noriharu; Bakos, Gaspar Á.; Barkaoui, Khalid; Beichman, Charles; Benkhaldoun, Zouhair; Boyle, Andrew W.; Ciardi, David R.; Clark, Catherine A.; Collins, Karen A.; Collins, Kevin I.; Conti, Dennis M.; Crossfield, Ian J. M.; Everett, Mark E.; Furlan, Elise; Ghachoui, Mourad; Gillon, Michaël; Gonzales, Erica J.; Higuera, Jesus; Horne, Keith; Howell, Steve B.; Jehin, Emmanuël; Lester, Kathryn V.; Lund, Michael B.; Matson, Rachel; Matthews, Elisabeth C.; Pozuelos, Francisco J.; Safonov, Boris S.; Schlieder, Joshua E.; Schwarz, Richard P.; Sefako, Ramotholo; Srdoc, Gregor; Strakhov, Ivan A.; Timmermans, Mathilde; Waalkes, William C.; Ziegler, Carl; Charbonneau, David; Essack, Zahra; Guerrero, Natalia M.; Harakawa, Hiroki; Hedges, Christina; Ishizuka, Masato; Jenkins, Jon M.; Konishi, Mihoko; Kotani, Takayuki; Kudo, Tomoyuki; Kurokawa, Takashi; Kuzuhara, Masayuki; Nishikawa, Jun; Omiya, Masashi; Ricker, George R.; Seager, Sara; Serizawa, Takuma; Striegel, Stephanie; Tamura, Motohide; Ueda, Akitoshi; Vanderspek, Roland; Vievard, Sébastien; Winn, Joshua N.Sub-Neptunes with radii of 2–3 R⊕ are intermediate in size between rocky planets and Neptune-sized planets. The orbital properties and bulk compositions of transiting sub-Neptunes provide clues to the formation and evolution of close-in small planets. In this paper, we present the discovery and follow-up of four sub-Neptunes orbiting M dwarfs (TOI-782, TOI-1448, TOI-2120, and TOI-2406), three of which were newly validated by ground-based follow-up observations and statistical analyses. TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b have radii of {R}_{{\rm{p}}}={2.740}_{-0.079}^{+0.082}\,{R}_{\oplus } {R}_{{\rm{p}}}={2.740}_{-0.079}^{+0.082}\,{R}_{\oplus } 2.120 ± 0.067 R⊕, and {2.830}_{-0.066}^{+0.068}\,{R}_{\oplus } and orbital periods of P = 8.02, 8.11, 5.80, and 3.08 days, respectively. Doppler monitoring with the Subaru/InfraRed Doppler instrument led to 2σ upper limits on the masses of <19.1 M⊕, <19.5 M⊕, <6.8 M⊕, and <15.6 M⊕ for TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b, respectively. The mass–radius relationship of these four sub-Neptunes testifies to the existence of volatile material in their interiors. These four sub-Neptunes, which are located above the so-called "radius valley," are likely to retain a significant atmosphere and/or an icy mantle on the core, such as a water world. We find that at least three of the four sub-Neptunes (TOI-782 b, TOI-2120 b, and TOI-2406 b), orbiting M dwarfs older than 1 Gyr, are likely to have eccentricities of e ∼ 0.2–0.3. The fact that tidal circularization of their orbits is not achieved over 1 Gyr suggests inefficient tidal dissipation in their interiors.© 2024. The Author(s). Published by the American Astronomical Society.C.A.C. acknowledges that this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). This work makes use of NASA Exoplanet Archive (Confirmed Planets Table; DOI:10.26133/NEA12) website and the Exoplanet Follow-up Observation Program (ExoFOP; DOI:10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program and observations from the LCOGT network and the MuSCAT2-MuSCAT3 network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by the NSF. The MuSCAT2 instrument at TCS operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide and the MuSCAT3 instrument at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory were developed by the Astrobiology Center under financial supports by JSPS KAKENHI (18H05439) and JST PRESTO (JPMJPR1775). K.A.C. acknowledges support from the TESS mission via subaward s3449 from MIT. Funding for the TESS mission is provided by NASA's Science Mission Directorate. D.R.C. acknowledges partial support from NASA grant 18-2XRP18_2-0007. This work was partly supported by a Grant-in-Aid for Scientific Research on Innovative Areas (JSPS KAKENHI grant No. 18H05439). TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation (SNF). I.A.S. acknowledges the support of the Ministry of Science and Higher Education of the Russian Federation under grant 075-15-2020-780 (N13.1902.21.0039). The NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI) was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Some of the observations in this paper made use of the High-Resolution Imaging instrument 'Alopeke and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. 'Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. 'Alopeke was mounted on the Gemini North telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and the Korea Astronomy and Space Science Institute (Republic of Korea). J.K. gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020-00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017-04945. G.M. has received funding from the Ariel Postdoctoral Fellowship program of the Swedish National Space Agency (SNSA). M.T. is supported by JSPS KAKENHI grant No.18H05442. R.L. acknowledges funding from University of La Laguna through the Margarita Salas Fellowship from the Spanish Ministry of Universities ref. UNI/551/2021 May 26, and under the EU Next Generation funds. W.W. was supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1650115. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). M.G. is F.R.S.-FNRS Research Director and E.J. is F.R.S.-FNRS Senior Research Associate. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. F.J.P. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to M.T. We thank the anonymous referee for valuable comments and suggestions that improved our manuscript. This research is based in part on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has the cultural, historical, and natural significance in Hawaii.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
NGTS-28Ab: a short period transiting brown dwarf
No full textHenderson, Beth A. et al.-- Full list of authors: Henderson, Beth A.; Casewell, Sarah L.; Goad, Michael R.; Acton, Jack S.; Günther, Maximilian N.; Nielsen, Louise D.; Burleigh, Matthew R.; Belardi, Claudia; Tilbrook, Rosanna H.; Turner, Oliver; Howell, Steve B.; Clark, Catherine A.; Littlefield, Colin; Barkaoui, Khalid; Alves, Douglas R.; Anderson, David R.; Bayliss, Daniel; Bouchy, Francois; Bryant, Edward M.; Dransfield, George; Ducrot, Elsa; Eigmüller, Philipp; Gill, Samuel; Gillen, Edward; Gillon, Michaël; Hawthorn, Faith; Hooton, Matthew J.; Jackman, James A. G.; Jehin, Emmanuel; Jenkins, James S.; Kendall, Alicia; Lendl, Monika; McCormac, James; Moyano, Maximiliano; Pedersen, Peter Pihlmann; Pozuelos, Francisco J.; Ramsay, Gavin; Sefako, Ramotholo R.; Timmermans, Mathilde; Triaud, Amaury H. M. J.; Udry, Stephane; Vines, Jose I.; Watson, Christopher A.; West, Richard G.; Wheatley, Peter J.; Zúñiga-Fernández, Sebastián.-- This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.We report the disco v ery of a brown dwarf orbiting a M1 host star. We first identified the brown dwarf within the Next Generation Transit Surv e y data, with supporting observations found in TESS sectors 11 and 38. We confirmed the disco v ery with follow- up photometry from the South African Astronomical Observatory, SPECULOOS-S, and TRAPPIST-S, and radial velocity measurements from HARPS, which allowed us to characterize the system. We find an orbital period of ∼1.25 d, a mass of 69 . 0 + 5 . 3 -4 . 8 M J , close to the hydrogen burning limit, and a radius of 0.95 ±0.05 R J . We determine the age to be > 0.5 Gyr, using model isochrones, which is found to be in agreement with spectral energy distribution fitting within errors. NGTS-28Ab is one of the shortest period systems found within the brown dwarf desert, as well as one of the highest mass brown dwarfs that transits an M dwarf. This makes NGTS-28Ab another important disco v ery within this scarcely populated region. © 2024 The Author(s)This work is based on data collected under the NGTS project
at the European Southern Observatory (ESO) La Silla Paranal
Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities
Council (STFC) under projects ST/M001962/1, ST/S002642/1, and
ST/W003163/1. This study is based on observations collected at the
European Southern Observatory under ESO programme 105.20G9.
This paper includes public data collected by the TESS mission.
Funding for the TESS mission is provided by the NASA Explorer
Program. This paper uses observations made at the South African
Astronomical Observatory (SAAO). This work has made use of
data from the European Space Agency (ESA) mission Gaia (https:
//www.cosmos.esa.int/gaia), processed by the Gaia Data Processing
and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web
/gaia/dpac/consortium). Funding for the DPAC has been provided by
national institutions, in particular, the institutions participating in the
Gaia Multilateral Agreement.
This publication makes use of data products from the Two
Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National
Aeronautics and Space Administration and the National Science
Foundation. The Pan-STARRS1 Surveys (PS1) and the PS1 public
science archive have been made possible through contributions by
the Institute for Astronomy, the University of Hawaii, the PanSTARRS Project Office, the Max-Planck Society and its participating
institutes, the Max Planck Institute for Astronomy, Heidelberg and
the Max Planck Institute for Extraterrestrial Physics, Garching, The
Johns Hopkins University, Durham University, the University of
Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian
Center for Astrophysics, the Las Cumbres Observatory Global
Telescope Network Incorporated, the National Central University
of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G
issued through the Planetary Science Division of the NASA Science
Mission Directorate, the National Science Foundation grant no. AST1238877, the University of Maryland, Eotvos Lorand University
(ELTE), the Los Alamos National Laboratory, and the Gordon and
Betty Moore Foundation.
Some of the Observations in the paper made use of the highresolution Imaging instrument Zorro. Zorro was funded by the
NASA Exoplanet Exploration Program and built at the NASA Ames
Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch,
and Emmett Quigley. Zorro was mounted on the Gemini South
telescope of the international Gemini Observatory, a programme
of NSF’s NOIRLab, which is managed by the Association
of Universities for Research in Astronomy (AURA) under a
cooperative agreement with the National Science Foundation on
behalf of the Gemini partnership: the National Science Foundation
(United States), National Research Council (Canada), Agencia
Nacional de Investigacion´ y Desarrollo (Chile), Ministerio de
Ciencia, Tecnolog´ıa e Innovacion´ (Argentina), Ministerio ´ da
Ciencia, ˆ Tecnologia, Inovac¸oes ˜ e Comunicac¸oes ˜ (Brazil), and Korea
Astronomy and Space Science Institute (Republic of Korea).
BH is supported by an STFC studentship (ST/S505511/1 and
ST/T506242/1). SLC acknowledges support from an STFC Ernest
Rutherford Fellowship (ST/R003726/1). The contribution of FB,
ML, OT, and SU has been carried out within the framework of the
NCCR PlanetS supported by the Swiss National Science Foundation
under grants 51NF40 182901 and 51NF40 205606. ML acknowledges support of the Swiss National Science Foundation under grant
number PCEFP2 194576. The contribution of EMB has been supported by STFCthrough the consolidated grant ST/W001136/1.CAC
acknowledges that this research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA (80NM0018D0004). JSJ gratefully acknowledges support by
FONDECYT grant 1201371 and from the ANID BASAL projects
ACE210002 and FB210003. The postdoctoral fellowship of KB
is funded by FRS-FNRS grant T.0109.20 and by the Francqui
Foundation. This publication benefits from the support of the French
Community of Belgium in the context of the FRIA Doctoral grant
awarded to MT. MG is FRS-FNRS Research Director and EJ is
FRS–FNRS Senior Research Associate. FJP acknowledges financial
support from the grant CEX2021-001131-S funded by MCIN/AEI/
10.13039/501100011033 and through projects PID2019-109522GBC52 and PID2022-137241NB-C43. This research is in part funded
by the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 803193/BEBOP), from the MERAC
foundation, and from the Science and Technology Facilities Council
(STFC; grant no. ST/S00193X/1 and ST/W000385/1). Based on
data collected by the SPECULOOS-South Observatory at the ESO
Paranal Observatory in Chile. The ULiege’s contribution to SPECULOOS has received funding from the European Research Councilunderthe European Union’s Seventh Framework Programme (FP/2007-
2013) (grant agreement no. 336480/SPECULOOS), from the Balzan
Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (FRS-FNRS; grant no. T.0109.20), from the
University of Liege, and from the ARC grant for Concerted Research
Actions financed by the Wallonia-Brussels Federation. This work is
supported by a grant from the Simons Foundation (PI Queloz, grant
number 327127). Based on data collected by the TRAPPIST-South
telescope at the ESO La Silla Observatory. TRAPPIST is funded
by the Belgian Fund for Scientific Research (Fond National de la
Recherche Scientifique, FNRS) under the grant PDR T.0120.21, with
the participation of the Swiss National Science Foundation (SNF).With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
