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The GAPS Programme at TNG L TOI-4515 b: An eccentric warm Jupiter orbiting a 1.2 Gyr-old G-star

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arXiv 2023年

作者： Carleo, I. Malavolta, L. Desidera, S. Nardiello, D. Wang, S. Turrini, D. Lanza, A.F. Baratella, M. Marzari, F. Benatti, S. Biazzo, K. Bieryla, A. Brahm, R. Bonavita, M. Collins, K.A. Hellier, C. Locci, D. Hobson, M.J. Maggio, A. Mantovan, G. Pinamonti, S. Messina, M. Rodriguez, J.E. Sozzetti, A. Stassun, K. Wang, X.Y. Ziegler, C. Damasso, M. Giacobbe, P. Murgas, F. Parviainen, H. Andreuzzi, G. Barkaoui, K. Berlind, P. Bignamini, A. Borsa, F. Briceno, C. Brogi, M. Cabona, L. Calkins, M.L. Capuzzo-Dolcetta, R. Cecconi, M. Colon, K.D. Cosentino, R. Dragomir, D. Esquerdo, G.A. Henning, T. Ghedina, A. Goeke, R.F. Gratton, R. Grau Horta, F. Gupta, A.F. Jenkins, J.M. Jordan, A. Knapic, C. Latham, D.W. Mireles, I. Law, N. Lorenzi, V. Lund, M.B. Maldonado, J. Mann, A.W. Molinari, E. Palle, E. Paegert, M. Pedani, M. Quinn, S.N. Scandariato, G. Seager, S. Winn, J.N. Wohler, B. Zingales, T. Calle Via Lactea s/n Tenerife La Laguna38200 Spain Tenerife La Laguna38206 Spain INAF - Osservatorio Astrofisico di Torino Via Osservatorio 20 Pino TorineseI-10025 Italy Dipartimento di Fisica e Astronomia "Galileo Galilei" Universita di Padova Vicolo dellOsservatorio 3 PadovaI-35122 Italy INAF - Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 PadovaI-35122 Italy Astronomy Department Indiana University BloomingtonIN47405-7105 United States INAF - Osservatorio Astrofisico di Catania Via S. Sofia 78 CataniaI-95123 Italy An der Sternwarte 16 PotsdamD-14482 Germany INAF - Osservatorio Astronomico di Palermo Piazza del Parlamento1 PalermoI-90134 Italy Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Facultad de Ingeniera y Ciencias Universidad Adolfo Ibanez Av. Diagonal las Torres 2640 Penalolen Santiago Chile Millennium Institute for Astrophysics Chile Data Observatory Foundation Chile SUPA Institute for Astronomy University of Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom Astrophysics Group Keele University Staffs ST5 5BG United Kingdom Max-Planck-Institut fur Astronomie Konigstuhl 17 Heidelberg69117 Germany Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Physics & Astronomy Vanderbilt University NashvilleTN United States Department of Physics Engineering and Astronomy Stephen F. Austin State University 1936 North St. NacogdochesTX75962 United States Fundacion Galileo Galilei-INAF Rambla Jose Ana Fernandez Perez 7 TF Brena Baja38712 Spain INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monte Porzio Catone00078 Italy Astrobiology Research Unit Universite de Liege 19C Allee du 6 Aout Liege4000 Belgium Department of Earth Atmospheric and Planetary Science Massachusetts Institute of Technology 77 Massachusetts Avenue Cambridge

Context. Different theories have been developed to explain the origins and properties of close-in giant planets, but none of them alone can explain all of the properties of the warm Jupiters (WJs, Porb = 10 - 200 days). One of the most intriguing characteristics of WJs is that they have a wide range of orbital eccentricities, challenging our understanding of their formation and evolution. Aims. The investigation of these systems is crucial in order to put constraints on formation and evolution theories. TESS is providing a significant sample of transiting WJs around stars bright enough to allow spectroscopic follow-up studies. Methods. We carried out a radial velocity (RV) follow-up study of the TESS candidate TOI-4515 b with the high-resolution spectrograph HARPSN in the context of the GAPS project, the aim of which is to characterize young giant planets, and the TRES and FEROS spectrographs. We then performed a joint analysis of the HARPS-N, TRES, FEROS, and TESS data in order to fully characterize this planetary system. Results. We find that TOI-4515 b orbits a 1.2 Gyr-old G-star, has an orbital period of Pb = 15.266446 ± 0.000013 days, a mass of Mb = 2.01 ± 0.05 MJ, and a radius of Rb = 1.09 ± 0.04 RJ. We also find an eccentricity of e = 0.46 ± 0.01, placing this planet among the WJs with highly eccentric orbits. As no additional companion has been detected, this high eccentricity might be the consequence of past violent scattering events. Copyright © 2023, The Authors. All rights reserved.

关键词： Stars

Hubble space telescope imaging of isolated local volume dwarfs GALFA-Dw3 and Dw4

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arXiv 2021年

作者： Bennet, Paul Sand, D.J. Crnojević, D. Weisz, D.R. Caldwell, N. Guhathakurta, P. Hargis, J.R. Karunakaran, A. Mutlu-Pakdil, B. Olszewski, E. Salzer, J.J. Seth, A.C. Simon, J.D. Spekkens, K. Stark, D.P. Strader, J. Tollerud, E.J. Toloba, E. Willman, B. Physics & Astronomy Department Texas Tech University Box 41051 LubbockTX79409-1051 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Astronomy/Steward Observatory The University of Arizona 933 North Cherry Avenue Rm. N204 TucsonAZ85721-0065 United States University of Tampa Department of Chemistry Biochemistry and Physics 401 West Kennedy Boulevard TampaFL33606 United States University of California Berkeley Department of Astronomy 501 Campbell Hall # 3411 BerkeleyCA94720-3411 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States UCO/Lick Observatory University of California Santa Cruz 1156 High Street Santa CruzCA95064 United States Space Telescope Science Institute 3800 San Martin Drive BaltimoreMD21208 United States Department of Physics Engineering Physics and Astronomy Queen’s University KingstonONK7L 3N6 Canada Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Department of Astronomy Indiana University 727 East Third Street BloomingtonIN47405 United States Department of Physics and Astronomy University of Utah 115 South 1400 East Salt Lake CityUT84112 United States Observatories of the Carnegie Institution for Science PasadenaCA91101 United States Department of Physics and Space Science Royal Military College of Canada P.O. Box 17000 Station Forces KingstonONK7K 7B4 Canada Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Physics University of the Pacific 3601 Pacific Avenue StocktonCA95211 United States LSST and Steward Observatory 933 North Cherry Avenue TucsonAZ85721 United States

We present observations of the dwarf galaxies GALFA Dw3 and GALFA Dw4 with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST). These galaxies were initially discovered as optical counterparts to compact HI clouds in the GALFA survey. Both objects resolve into stellar populations which display an old red giant branch, younger helium burning, and massive main sequence stars. We use the tip of the red giant branch method to determine the distance to each galaxy, finding distances of 7.61+0−0..2829 Mpc and 3.10+0−0..1617 Mpc, respectively. With these distances we show that both galaxies are extremely isolated, with no other confirmed objects within ∼1.5 Mpc of either dwarf. GALFA Dw4 is also found to be unusually compact for a galaxy of its luminosity. GALFA Dw3 & Dw4 contain HII regions with young star clusters and an overall irregular morphology;they show evidence of ongoing star formation through both ultraviolet and Hα observations and are therefore classified as dwarf irregulars (dIrrs). The star formation histories of these two dwarfs show distinct differences: Dw3 shows signs of a recently ceased episode of active star formation across the entire dwarf, while Dw4 shows some evidence for current star formation in spatially limited HII regions. Compact HI sources offer a promising method for identifying isolated field dwarfs in the Local Volume, including GALFA Dw3 & Dw4, with the potential to shed light on the driving mechanisms of dwarf galaxy formation and evolution. © 2021, CC BY.

关键词： Galaxies

Young, blue, and isolated stellar systems in the Virgo Cluster I. 2-D Optical spectroscopy

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arXiv 2022年

作者： Bellazzini, Michele Magrini, Laura Jones, Michael G. Sand, David J. Beccari, Giacomo Cresci, Giovanni Spekkens, Kristine Karunakaran, Ananthan Adams, Elizabeth A.K. Zaritsky, Dennis Battaglia, Giuseppina Seth, Anil Cannon, John M. Fuson, Jackson Inoue, John L. Mutlu-Pakdil, Burçin Guhathakurta, Puragra Muñoz, Ricardo R. Bennet, Paul Crnojević, Denija Caldwell, Nelson Strader, Jay Toloba, Elisa INAF Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna Via Gobetti 93/3 Bologna40129 Italy INAF-Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze50125 Italy Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States European Southern Observatory Karl-Schwarzschild-Straße 2 Garching bei MünchenD-85748 Germany Department of Physics and Space Science Royal Military College of Canada P.O. Box 17000 Station Forces Kingston ONK7K 7B4 Canada Department of Physics Engineering Physics and Astronomy Queens University KingstonONK7L 3N6 Canada Glorieta de la Astronomía Granada18008 Spain Department of Physics Engineering Physics and Astronomy Queens University KingstonONK7L 3N6 Canada ASTRON Netherlands Institute for Radio Astronomy Oude Hoogeveensedijk 4 Dwingeloo7991 PD Netherlands Kapteyn Astronomical Institute University of Groningen PO Box 800 Groningen9700 AV Netherlands Instituto de Astrofísica de Canarias Vía Láctea s/n La Laguna38205 Spain Department of Astrophysics University of la Laguna San Cristóbal de La LagunaE-38206 Spain Department of Physics & Astronomy University of Utah Salt Lake CityUT84112 United States Department of Physics & Astronomy Macalester College 1600 Grand Avenue Saint PaulMN55105 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States UCO/Lick Observatory University of California Santa Cruz 1156 High Street Santa CruzCA95064 United States Departamento de Astronomía Universidad de Chile Camino El Observatorio 1515 Las Condes Santiago Chile Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States University of Tampa 401 West Kennedy Boulevard TampaFL33606 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United State

We use panoramic optical spectroscopy obtained with MUSE@VLT to investigate the nature of five candidate extremely isolated low-mass star forming regions (Blue Candidates, BCs hereafter) toward the Virgo cluster of galaxies. Four of the five (BC1, BC3, BC4, BC5) are found to host several Hii regions and to have radial velocities fully compatible with being part of the Virgo cluster. All the confirmed candidates have mean metallicity significantly in excess of that expected from their stellar mass, indicating that they originated from gas stripped from larger galaxies. In summary, these four candidates share the properties of the prototype system SECCO 1, suggesting the possible emergence of a new class of stellar systems, intimately linked to the complex duty cycle of gas within clusters of galaxies. A thorough discussion on the nature and evolution of these objects is presented in a companion paper, where the results obtained here from MUSE data are complemented with Hubble Space Telescope (optical) and Very Large Array (Hi) observations. Copyright © 2022, The Authors. All rights reserved.

关键词： Galaxies

Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

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arXiv 2024年

作者： Carleo, Ilaria Barragan, Oscar Persson, Carina M. Fridlund, Malcolm Lam, Kristine W.F. Messina, Sergio Gandolfi, Davide Smith, Alexis M.S. Johnson, Marshall C. Cochran, William Osborne, Hannah L.M. Brahm, Rafael Ciardi, David R. Collins, Karen A. Everett, Mark E. Giacalone, Steven Guenther, Eike W. Hatzes, Artie Hellier, Coel Horner, Jonathan Kabath, Petr Korth, Judith MacQueen, Phillip Masseron, Thomas Murgas, Felipe Nowak, Grzegorz Rodriguez, Joseph E. Watkins, Cristilyn N. Wittenmyer, Rob Zhou, George Ziegler, Carl Bieryla, Allyson Boyd, Patricia T. Clark, Catherine A. Dressing, Courtney D. Eastman, Jason D. Eberhardt, Jan Endl, Michael Espinoza, Nestor Fausnaugh, Michael Guerrero, Natalia M. Henning, Thomas Hesse, Katharine Hobson, Melissa J. Howell, Steve B. Jordan, Andres Latham, David W. Lund, Michael B. Mireles, Ismael Narita, Norio Pinto, Marcelo Tala Pugh, Teznie Quinn, Samuel N. Ricker, George Rodriguez, David R. Rojas, Felipe I. Rose, Mark E. Rudat, Alexander Sarkis, Paula Savel, Arjun B. Schlecker, Martin Schwarz, Richard P. Seager, Sara Shporer, Avi Smith, Jeffrey C. Stassun, Keivan G. Stockdale, Chris Trifonov, Trifon Vanderspek, Roland Winn, Joshua N. Wright, Duncan INAF-Osservatorio Astrofisico di Torino Via Osservatorio 20 Pino TorineseI-10025 Italy Tenerife La Laguna38205 Spain Tenerife La LagunaE-38206 Spain Sub-department of Astrophysics Department of Physics University of Oxford OxfordOX1 3RH United Kingdom Chalmers University of Technology Department of Space Earth and Environment Onsala Space Observatory OnsalaSE-439 92 Sweden Leiden Observatory University of Leiden PO Box 9513 Leiden2300 RA Netherlands Rutherfordstrasse 2 Berlin12489 Germany INAF - Osservatorio Astrofisico di Catania Via S. Sofia 78 CataniaI-95123 Italy Dipartimento di Fisica Universita degli Studi di Torino via Pietro Giuria 1 TorinoI-10125 Italy Department of Astronomy The Ohio State University 4055 McPherson Laboratory 140 West 18th Avenue ColumbusOH43210 United States Mullard Space Science Laboratory University College London Holmbury St Mary Dorking SurreyRH5 6NT United Kingdom European Southern Observatory Karl-Schwarzschild-Strase 2 Garching bei MunchenD-85748 Germany Facultad de Ingeniera y Ciencias Universidad Adolfo Ibanez Av. Diagonallas Torres 2640 Penalolen Santiago Chile Millennium Institute for Astrophysics Chile NASA Exoplanet Science Institute-Caltech IPAC PasadenaCA91125 United States Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Astronomy and McDonald Observatory University of Texas at Austin 2515 Speedway Stop C1400 AustinTX78712 United States NSF National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Department of Astronomy California Institute of Technology PasadenaCA91125 United States Thuringer Landessternwarte Tautenburg Sternwarte 5 TautenburgD-07778 Germany Astrophysics Group Keele University StaffordshireST5 5BG United Kingdom Astronomical Institute Czech Academy of Sciences Fričova 298 Ondřejov25165 Czech Republic Lund Observatory Division of Astrophysics

Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters, challenging our understanding on their actual origin. Aims. The present work, which is the results of our warm Jupiters survey carried out with the CHIRON spectrograph within the KESPRINT collaboration, aims to address this challenge by studying two planets that could help bridge the gap between the two populations. *** report the confirmation and mass determination of a hot Jupiter (orbital period shorter than 10 days), TOI-2420 b, and a warm Jupiter, TOI-2485 b. We performed a joint analysis using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of Pb=5.8 days, a mass of Mb=0.9 MJ and a radius of Rb=1.3 RJ, with a planetary density of 0.477 g cm-3;while TOI-2485 b has an orbital period of Pb=11.2 days, a mass of Mb=2.4 MJ and a radius of Rb=1.1 RJ with density 2.36 g cm-3. Conclusions. With current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: the high-eccentricity migration scenarios cannot be ruled out, and TOI-2485 b's characteristics may rather support this scenario. Copyright © 2024, The Authors. All rights reserved.

关键词： Planets

QTT-isogeometric solver in two dimensions

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arXiv 2018年

作者： Markeeva, L. Tsybulin, I. Oseledets, I. Center for Computational and Data-Intensive Science and Engineering Skolkovo Institute of Science and Technology Moscow Russia Department of Applied Math and Control Moscow Institute of Physics and Technology Moscow Russia Laboratory of Fluid Dynamics and Seismics Moscow Institute of Physics and Technology Moscow Russia Institute of Numerical Mathematics Russian Academy of Sciences Moscow Russia

APOGEE-centric Ananke Simulations in a SciServer SQL database

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Research Notes of the AAS 2022年第6期6卷 125-125页

作者： Rachael L. Beaton Suzanne Werner Arik W. Mitschang Gerard Lemson Aniruddha Thakar Anne-Marie Weijmans Joel R. Brownstein Farnik Nikakhtar Robyn E. Sanderson Andrew Wetzel Sarah Loebman Sanjib Sharma Space Telescope Science Institute 3700 San Martin Drive Baltimore MD 21218 USA rbeaton@princeton.edu Department of Astrophysical Sciences Princeton University 4 Ivy Lane Princeton NJ 08544 USA The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. Pasadena CA 91101 USA Institute For Data Intensive Engineering and Science Johns Hopkins University. 3701 San Martin Drive Baltimore MD 21218 USA Center for Astrophysical Sciences Department of Physics and Astronomy Johns Hopkins University 3400 North Charles Street Baltimore MD 21218 USA School of Physics and Astronomy University of St Andrews North Haugh St Andrews KY16 9SS UK Department of Physics and Astronomy University of Utah 115 S. 1400 E. Salt Lake City UT 84112 USA Department of Physics & Astronomy University of Pennsylvania 209 S 33rd St. Philadelphia PA 19104 USA Center for Computational Astrophysics Flatiron Institute 162 5th Ave New York NY 10010 USA Department of Physics & Astronomy University of California Davis CA 95616 USA Department of Physics University of California Merced 5200 North Lake Rd. Merced CA 95343 USA Sydney Institute for Astronomy School of Physics A28 The University of Sydney NSW 2006 Australia Center of Excellence for Astrophysics in Three Dimensions (ASTRO-3D) Australia

Modern galaxy simulations have reached the complexity required to create sophisticated mock catalogs. Ananke is a set of nine mock catalogs constructed from synthetic surveys of three Milky Way-like galaxies from the Latte suite of FIRE simulations. Ananke provides observed quantities for comparison with modern large-scale stellar surveys. In SDSS-IV DR17, mock catalogs for the Apache Point Galactic Evolution Experiment (APOGEE) were built from Ananke synthetic surveys as a Value-Added Catalog, but were only provided as large flat files (∼>10's GB). Here we announce an >40 Tb SQL database for nine APOGEE-specific mock catalogs and describe additions to the data model necessary for effective user queries. The catalogs can be accessed on the free, science platform, SciServer—supported by the Institute for data intensive engineering and science at the Johns Hopkins University (IDIES); SciServer supports server-side analysis with commonly used coding languages and tools.

关键词： Catalogs Milky Way Galaxy Surveys Redshift surveys Astronomy databases

Migration and Evolution of giant ExoPlanets (MEEP) I: Nine Newly Confirmed Hot Jupiters from the TESS Mission

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arXiv 2024年

作者： Schulte, Jack Rodriguez, Joseph E. Bieryla, Allyson Quinn, Samuel N. Collins, Karen A. Yee, Samuel W. Nine, Andrew C. Soares-Furtado, Melinda Latham, David W. Eastman, Jason D. Barkaoui, Khalid Ciardi, David R. Dragomir, Diana Everett, Mark E. Giacalone, Steven Mireles, Ismael Murgas, Felipe Narita, Norio Shporer, Avi Strakhov, Ivan A. Striegel, Stephanie Vaňko, Martin Vowell, Noah Wang, Gavin Ziegler, Carl Bellaver, Michael Benni, Paul Bergeron, Serge Boffin, Henri M.J. Briceño, César Clark, Catherine A. Collins, Kevin I. de Leon, Jerome P. Dressing, Courtney D. Evans, Phil Esparza-Borges, Emma Fedewa, Jeremy Fukui, Akihiko Gan, Tianjun Gerasimov, Ivan S. Hartman, Joel D. Gill, Holden Gillon, Michaël Horne, Keith Horta, Ferran Grau Howell, Steve B. Isogai, Keisuke Jehin, Emmanuël Jenkins, Jon M. Karjalainen, Raine Kielkopf, John F. Lester, Kathryn V. Littlefield, Colin Lund, Michael B. Mann, Andrew W. McCormack, Mason Michaels, Edward J. Painter, Shane Palle, Enric Parviainen, Hannu Peterson, David-Michael Pozuelos, Francisco J. Raup, Zachary Reed, Phillip Relles, Howard M. Ricker, George R. Savel, Arjun B. Schwarz, Richard P. Seager, S. Sefako, Ramotholo Srdoc, Gregor Stockdale, Chris Sullivan, Hannah Timmermans, Mathilde Winn, Joshua N. Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Center for Astrophysics | Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Astronomy University of Wisconsin-Madison 475 N Charter St. MadisonWI53706 United States Department of Physics and Astronomy Carleton College 215 Goodsell Circle NorthfieldMN55057 United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Astrobiology Research Unit Université de Liège 19C Allée du 6 Août Liège4000 Belgium Department of Earth Atmospheric and Planetary Science Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Tenerife La Laguna38200 Spain NASA Exoplanet Science Institute-Caltech IPAC PasadenaCA91125 United States Department of Physics and Astronomy University of New Mexico 210 Yale Blvd NE AlbuquerqueNM87106 United States NSF's National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Department of Astronomy California Institute of Technology PasadenaCA91125 United States Tenerife La Laguna38206 Spain Komaba Institute for Science The University of Tokyo 3-8-1 Komaba Meguro Tokyo153-8902 Japan Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Sternberg Astronomical Institute Lomonosov Moscow State University Universitetsky pr. 13 Moscow119234 Russia SETI Institute Mountain ViewCA94043 United States NASA Ames Research Center Moffett FieldCA94035 United States Astronomical Institute Slovak Academy of Sciences Tatranská Lomnica059 60 Slovakia Tsinghua International School Beijing100084 China Department of Physics Engineering and Astronomy Stephen F. Aust

Hot Jupiters were many of the first exoplanets discovered in the 1990s, but in the decades since their discovery, the mysteries surrounding their origins remain. Here, we present nine new hot Jupiters (TOI-1855 b, TOI-2107 b, TOI-2368 b, TOI-3321 b, TOI-3894 b, TOI-3919 b, TOI-4153 b, TOI-5232 b, and TOI-5301 b) discovered by NASA's TESS mission and confirmed using ground-based imaging and spectroscopy. These discoveries are the first in a series of papers named the Migration and Evolution of giant ExoPlanets (MEEP) survey and are part of an ongoing effort to build a complete sample of hot Jupiters orbiting FGK stars, with a limiting Gaia G-band magnitude of 12.5. This effort aims to use homogeneous detection and analysis techniques to generate a set of precisely measured stellar and planetary properties that is ripe for statistical analysis. The nine planets presented in this work occupy a range of masses (0.55 Jupiter masses (MJ) P J) and sizes (0.967 Jupiter radii (RJ) P J) and orbit stars that range in temperature from 5360 K eff Copyright © 2024, The Authors. All rights reserved.

关键词： Stars

The TESS-Keck Survey XXI: 13 New Planets and Homogeneous Properties for 21 Subgiant Systems

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arXiv 2024年

作者： Chontos, Ashley Huber, Daniel Grunblatt, Samuel K. Saunders, Nicholas Winn, Joshua N. McCormack, Mason Knudstrup, Emil Albrecht, Simon H. Crossfield, Ian J.M. Rodriguez, Joseph E. Ciardi, David R. Collins, Karen A. Jenkins, Jon M. Bieryla, Allyson Batalha, Natalie M. Beard, Corey Dai, Fei Dalba, Paul A. Fetherolf, Tara Giacalone, Steven Hill, Michelle L. Howard, Andrew W. Isaacson, Howard Kane, Stephen R. Lubin, Jack Macdougall, Mason G. Močnik, Teo Akana Murphy, Joseph M. Petigura, Erik A. Pidhorodetska, Daria Polanski, Alex S. Robertson, Paul Rubenzahl, Ryan A. Turtelboom, Emma V. Weiss, Lauren M. van Zandt, Judah Ricker, George R. Vanderspek, Roland Latham, David W. Seager, Sara Quinn, Samuel N. Shporer, Avi Eisner, Nora L. Goeke, Robert F. Levine, Alan M. Ting, Eric B. Howell, Steve Schlieder, Joshua E. Benni, Paul Boyle, Andrew W. Gan, Tianjun Girardin, Eric Gonzalez, Erica Gregorio, Joao Horne, Keith Livingston, John Lund, Michael B. Mann, Christopher R. Massey, Bob Matthews, Elisabeth C. McLeod, Kim K. Palle, Enric Popowicz, Adam Relles, Howard M. Schwarz, Richard P. Sefako, Ramotholo Srdoc, Gregor Tan, Thiam-Guan Wang, Gavin Ziegler, Carl Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive HonoluluHI96822 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States School of Physics University of Sydney NSW2006 Australia Department of Physics and Astronomy Johns Hopkins University 3400 N Charles St BaltimoreMD21218 United States Department of Astronomy & Astrophysics University of Chicago ChicagoIL60637 United States Department of Space Earth and Environment Chalmers University of Technology Gothenburg412 93 Sweden Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Department of Physics & Astronomy University of Kansas 1251 Wescoe Hall Dr. 1082 Malott LawrenceKS66045 United States Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Caltech/IPAC-NASA Exoplanet Science Institute 770 S. Wilson Avenue PasadenaCA91106 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States NASA Ames Research Center Moffett FieldCA94035 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95060 United States Department of Physics & Astronomy University of California Irvine IrvineCA92697 United States Division of Geological and Planetary Sciences 1200 E California Blvd PasadenaCA91125 United States Department of Astronomy California Institute of Technology PasadenaCA91125 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Department of Physics California State University San MarcosCA92096 United States Department of Earth and Planetary Sciences University of California RiversideCA92521 United States Department of Astronomy University of California Berkeley BerkeleyCA94720 United States

We present a dedicated transit and radial velocity survey of planets orbiting subgiant stars observed by the TESS Mission. Using ∼16 nights on Keck/HIRES, we confirm and characterize 12 new transiting planets - TOI-329 b, HD 39688 b (TOI-480), TOI-603 b, TOI-1199 b, TOI-1294 b, TOI-1439 b, TOI-1605 b, TOI-1828 b, HD 148193 b (TOI-1836), TOI-1885 b, HD 83342 b (TOI-1898), TOI-2019 b - and provide updated properties for 9 previously confirmed TESS subgiant systems (TOI-197, TOI-954, TOI-1181, TOI-1296, TOI-1298, TOI-1601, TOI-1736, TOI-1842, TOI-2145). We also report the discovery of an outer, non-transiting planet, TOI-1294 (Equation presented) and three additional stars with long-term RV trends. We find that at least 19±8% of subgiants in our sample of 21 stars have outer companions, comparable to main-sequence stars. We perform a homogeneous analysis of the stars and planets in the sample, with median uncertainties of 3%, 8% and 15% for planet radii, masses and ages, doubling the number of known planets orbiting subgiant stars with bulk densities measured to better than 10%. We observe a dearth of giant planets around evolved stars with short orbital periods, consistent with tidal dissipation theories that predict the rapid inspiral of planets as their host stars leave the main sequence. We note the possible evidence for two distinct classes of hot Jupiter populations, indicating multiple formation channels to explain the observed distributions around evolved stars. Finally, continued RV monitoring of planets in this sample will provide a more comprehensive understanding of demographics for evolved planetary systems. © 2024, CC BY.

关键词： Planets

SN 2022acko: the First Early Far-Ultraviolet Spectra of a Type IIP Supernova

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arXiv 2023年

作者： Bostroem, K. Azalee Dessart, Luc Hillier, D. John Lundquist, Michael Andrews, Jennifer E. Sand, David J. Dong, Yize Valenti, Stefano Haislip, Joshua Hoang, Emily T. Hosseinzadeh, Griffin Janzen, Daryl Jencson, Jacob E. Jha, Saurabh W. Kouprianov, Vladimir Pearson, Jeniveve Meza Retamal, Nicolas E. Reichart, Daniel E. Shrestha, Manisha Ashall, Christopher Baron, E. Brown, Peter J. DerKacy, James M. Farah, Joseph Galbany, Lluís Hernández, J.I. González Green, Elizabeth Hoeflich, Peter Howell, D. Andrew Kwok, Lindsey A. McCully, Curtis Müller-Bravo, Tomás E. Newsome, Megan Gonzalez, Estefania Padilla Pellegrino, Craig Rho, Jeonghee Rowe, Micalyn Schwab, Michaela Shahbandeh, Melissa Smith, Nathan Strader, Jay Terreran, Giacomo Van Dyk, Schuyler D. Wyatt, Samuel Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States Institut d’Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago Paris75014 France University of Pittsburgh 3941 O’Hara Street PittsburghPA15260 United States W. M. Keck Observatory 65-1120 Māmalahoa Highway KamuelaHI96743-8431 United States Gemini Observatory 670 North A‘ohoku Place HiloHI96720-2700 United States Department of Physics and Astronomy University of California Davis 1 Shields Avenue DavisCA95616-5270 United States Department of Physics and Astronomy University of North Carolina 120 East Cameron Avenue Chapel HillNC27599 United States Department of Physics and Engineering Physics University of Saskatchewan 116 Science Place SaskatoonSKS7N 5E2 Canada Department of Physics and Astronomy The Johns Hopkins University 3400 North Charles Street BaltimoreMD21218 United States Department of Physics and Astronomy Rutgers the State University of New Jersey 136 Frelinghuysen Road PiscatawayNJ08854-8019 United States Department of Physics Virginia Tech BlacksburgVA24061 United States Planetary Science Institute 1700 East Fort Lowell Suite 106 TucsonAZ85719-2395 United States Hamburger Sternwarte Gojenbergsweg 112 HamburgD-21029 Germany Homer L. Dodge Department of Physics and Astronomy University of Oklahoma 440 W. Brooks Rm 100 NormanOK73019-2061 United States Department of Physics and Astronomy Texas A&M University 4242 TAMU College StationTX77843 United States Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain Institut d’Estudis Espacials de Catalunya Gran Capità 2-4 Edifici Nexus Desp. 201 BarcelonaE-08034 Spain Instituto de Astrofísica de Canarias La Laguna TenerifeE-38205 Spain Universidad de La Lag

We present five far- and near-ultraviolet spectra of the Type II plateau supernova, SN 2022acko, obtained 5, 6, 7, 19, and 21 days after explosion, all observed with the Hubble Space Telescope/Space Telescope Imaging Spectrograph. The first three epochs are earlier than any Type II plateau supernova has been observed in the far-ultraviolet revealing unprecedented characteristics. These three spectra are dominated by strong lines, primarily from metals, which contrasts with the featureless early optical spectra. The flux decreases over the initial time series as the ejecta cool and line-blanketing takes effect. We model this unique dataset with the non-local thermodynamic equilibrium radiation transport code CMFGEN, finding a good match to the explosion of a low-mass red supergiant with energy Ekin = 6 × 1050 erg. With these models we identify, for the first time, the ions that dominate the early ultraviolet spectra. We present optical photometry and spectroscopy, showing that SN 2022acko has a peak absolute magnitude of V = −15.4 mag and plateau length of ∼ 115d. The spectra closely resemble those of SN 2005cs and SN 2012A. Using the combined optical and ultraviolet spectra, we report the fraction of flux as a function of bluest wavelength on days 5, 7, and 19. We create a spectral time-series of Type II supernovae in the ultraviolet, demonstrating the rapid decline of flux over the first few weeks of evolution. Future observations of Type II supernovae are required to map out the landscape of exploding red supergiants, with and without circumstellar material, which is best revealed in high-quality ultraviolet spectra. © 2023, CC BY.

关键词： Supernovae