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37th International Cosmic Ray Conference, ICRC 2021

作者： Ohtani, Y. Berti, A. Depaoli, D. Di Pierro, F. Green, D. Heckmann, L. Hütten, M. Inada, T. López-Coto, R. Medina, E. Moralejo, A. Morcuende, D. Pirola, G. Strzys, M. Suda, Y. Vovk, I. Abe, H. Aguasca, A. Agudo, I. Antonelli, L.A. Aramo, C. Armstrong, T. Artero, M. Asano, K. Ashkar, H. Aubert, P. Baktash, A. Bamba, A. Baquero Larriva, A. Baroncelli, L. Barres de Almeida, U. Barrio, J.A. Batkovic, I. Becerra González, J. Bernardos, M.I. Biederbeck, N. Bigongiari, C. Blanch, O. Bonnoli, G. Bordas, P. Bose, D. Bulgarelli, A. Burelli, I. Buscemi, M. Cardillo, M. Caroff, S. Carosi, A. Cassol, F. Cerruti, M. Chai, Y. Cheng, K. Chikawa, M. Chytka, L. Contreras, J.L. Cortina, J. Costantini, H. Dalchenko, M. De Angelis, A. de Bony de Lavergne, M. Deleglise, G. Delgado, C. Delgado Mengual, J. della Volpe, D. Di Venere, L. Díaz, C. Dominik, R.M. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsässer, D. Emery, G. Escudero, J. Fiasson, A. Foffano, L. Fonseca, M.V. Freixas Coromina, L. Fukami, S. Fukazawa, Y. Garcia, E. Garcia López, R. Giglietto, N. Giordano, F. Gliwny, P. Godinovic, N. Grespan, P. Gunji, S. Hackfeld, J. Hadasch, D. Hahn, A. Hassan, T. Hayashi, K. Heller, M. Herrera Llorente, J. Hirotani, K. Hoffmann, D. Horns, D. Houles, J. Hrabovsky, M. Hrupec, D. Hui, D. Inome, Y. Iori, M. Ishio, K. Iwamura, Y. Jacquemont, M. Jimenez Martinez, I. Jouvin, L. Jurysek, J. Kagaya, M. Karas, V. Katagiri, H. Kataoka, J. Kerszberg, D. Kobayashi, Y. Kong, A. Kubo, H. Kushida, J. Lamanna, G. Lamastra, A. Le Flour, T. Longo, F. López-Moya, M. López-Oramas, A. Luque-Escamilla, P.L. Majumdar, P. Makariev, M. Mandat, D. Manganaro, M. Mannheim, K. Mariotti, M. Marquez, P. Marsella, G. Martí, J. Martinez, O. Martínez, G. Martínez, M. Marusevec, P. Mas, A. Maurin, G. Mazin, D. Mestre Guillen, E. Micanovic, S. Miceli, D. Miener, T. Miranda, J.M. Miranda, L.D.M. Mirzoyan, R. Mizuno, T. Molina, E. Montaruli, T. Monteiro, I. Moretti, E. ICRR The University of Tokyo 1-5-1 Kashiwa-no-ha Chiba Kashiwa City Japan Max Planck Institute for Physics Föhringer Ring 6 München80805 Germany INFN Sezione di Torino Via Pietro Giuria 1 Torino10125 Italy INFN Sezione di Padova Via Francesco Marzolo 8 Padova35131 Italy IFAE Edifici Cn Campus Universitat Autònoma de Barcelona Barcelona08193 Spain Universidad Complutense de Madrid Av. Séneca 2 Madrid28040 Spain Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Spain Instituto de Astrofísica de Andalucía-CSIC Spain INFN Sezione di Napoli Italy Aix Marseille Univ CNRS IN2P3 CPPM France IRFU CEA Université Paris-Saclay France LAPP Univ. Grenoble Alpes Univ. Savoie Mont Blanc CNRS-IN2P3 Annecy France Universität Hamburg Institut für Experimentalphysik Germany Graduate School of Science University of Tokyo Japan INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Italy INFN Sezione di Padova Università degli Studi di Padova Italy Instituto de Astrofísica de Canarias Departamento de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Department of Physics TU Dortmund University Germany INFN Sezione di Trieste Università degli Studi di Udine Italy INFN Sezione di Catania Italy University of Geneva Département de Physique Nucléaire et Corpusculaire Italy Palacky University Olomouc Faculty of Science Czech Republic Port d'Informació Científica Spain Dipartimento di Fisica Universitá degli Studi di Torino Italy University of Rijeka Department of Physics Croatia Institute for Theoretical Physics and Astrophysics Universität Würzburg Germany Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Japan INFN Sezione di Bari Politecnico di Bari Italy Faculty of Physics and Applied Informatics University of

The Cherenkov Telescope Array (CTA) will be the next generation gamma-ray observatory, which will consist of three kinds of telescopes of different sizes. Among those, the Large Size Telescope (LST) will be the most sensitive in the low energy range starting from 20 GeV. The prototype LST (LST-1) proposed for CTA was inaugurated in October 2018 in the northern hemisphere site, La Palma (Spain), and is currently in its commissioning phase. MAGIC is a system of two gamma-ray Cherenkov telescopes of the current generation, located approximately 100 m away from LST-1, that have been operating in stereoscopic mode since 2009. Since LST-1 and MAGIC can observe the same air shower events, we can compare the brightness of showers, estimated energies of gamma rays, and other parameters event by event, which can be used to cross-calibrate the telescopes. Ultimately, by performing combined analyses of the events triggering the three telescopes, we can reconstruct the shower geometry more accurately, leading to better energy and angular resolutions, and a better discrimination of the background showers initiated by cosmic rays. For that purpose, as part of the commissioning of LST-1, we performed joint observations of established gamma-ray sources with LST-1 and MAGIC. Also, we have developed Monte Carlo simulations for such joint observations and an analysis pipeline which finds event coincidence in the offline analysis based on their timestamps. In this work, we present the first detection of an astronomical source, the Crab Nebula, with combined observation of LST-1 and MAGIC. Moreover, we show results of the inter-telescope cross-calibration obtained using Crab Nebula data taken during joint observations with LST-1 and MAGIC. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)

关键词： Telescopes

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NuSTAR Observations of Candidate Subparsec Binary Supermassive Black Holes

arXiv

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arXiv 2023年

作者： Saade, M. Lynne Brightman, Murray Stern, Daniel Connor, Thomas Djorgovski, S.G. D’Orazio, Daniel J. Ford, K.E.S. Graham, Matthew J. Haiman, Zoltán Jun, Hyunsung D. Kammoun, Elias Kraft, Ralph P. McKernan, Barry Vikhlinin, Alexei Walton, Dominic J. Department of Physics and Astronomy University of California 475 Portola Plaza Los AngelesCA90095 United States Science & Technology Institute Universities Space Research Association 320 Sparkman Drive HuntsvilleAL35805 United States Cahill Center for Astronomy and Astrophysics California Institute of Technology 1216 E. California Blvd. PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Niels Bohr International Academy Niels Bohr Institute Blegdamsvej 17 Copenhagen2100 Denmark Department of Astrophysics American Museum of Natural History Central Park West at 79th Street New YorkNY10024 United States Department of Science Borough of Manhattan Community College City University of New York New YorkNY10007 United States Physics Program The Graduate Center City University of New York New YorkNY10016 United States Department of Astronomy Columbia University New YorkNY10027 United States SNU Astronomy Research Center Astronomy Program Dept. of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of IRAP Université de Toulouse CNRS UPS CNES 9 Avenue du Colonel Roche BP 44346 ToulouseF-31028 Cedex 4 France INAF – Osservatorio Astrofisico di Arcetri Largo Enrico Fermi 5 FirenzeI-50125 Italy Centre for Astrophysics Research University of Hertfordshire College Lane HatfieldAL10 9AB United Kingdom Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom

We present analysis of NuSTAR X-ray observations of three AGN that were identified as candidate subparsec binary supermassive black hole (SMBH) systems in the Catalina Real-Time Transient Survey based on apparent periodicity in their optical light curves. Simulations predict that close-separation accreting SMBH binaries will have different X-ray spectra than single accreting SMBHs. We previously observed these AGN with Chandra and found no differences between their low energy X-ray properties and the larger AGN population. However some models predict differences to be more prominent at energies higher than probed by Chandra. We find that even at the higher energies probed by NuSTAR, the spectra of these AGN are indistinguishable from the larger AGN population. This could rule out models predicting large differences in the X-ray spectra in the NuSTAR bands. Alternatively, it might mean that these three AGN are not binary SMBHs. © 2023, CC BY-NC-SA.

关键词： Active Galactic Nuclei

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The K2 & TESS Synergy III: search and rescue of the lost ephemeris for K2’s first planet

arXiv

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arXiv 2024年

作者： Thygesen, Erica Rodriguez, Joseph E. Beurs, Zoë L.D.E. Vanderburg, Andrew Livingston, John H. Irwin, Jonathon Venner, Alexander Cretignier, Michael Collins, Karen A. Bieryla, Allyson Charbonneau, David Crossfield, Ian J.M. Dumusque, Xavier Kielkopf, John Latham, David W. Werner, Michael Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Earth Atmospheric and Planetary Sciences Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Centre for Astrophysics University of Southern Queensland West Street ToowoombaQLD4350 Australia Department of Physics University of Oxford OxfordOX13RH United Kingdom Center for Astrophysics Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States Department of Physics and Astronomy University of Kansas LawrenceKS66045 United States Geneva Observatory University of Geneva Chemin des Mailettes 51 Versoix1290 Switzerland Department of Physics and Astronomy University of Louisville LouisvilleKY40292 United States NASA Jet Propulsion Laboratory PasadenaCA United States

K2-2 b/HIP 116454 b, the first exoplanet discovery by K2 during its Two-Wheeled Concept Engineering Test, is a sub-Neptune (formula presented) orbiting a relatively bright (KS = 8.03) K-dwarf on a 9.1 day period. Unfortunately, due to a spurious follow-up transit detection and ephemeris degradation, the transit ephemeris for this planet was lost. In this work, we recover and refine the transit ephemeris for K2-2 b, showing a ∼40σ discrepancy from the discovery results. To accurately measure the transit ephemeris and update the parameters of the system, we jointly fit space-based photometric observations from NASA’s K2, TESS, and Spitzer missions with new photometric observations from the ground, as well as radial velocities from HARPS-N that are corrected for stellar activity using a new modeling technique. Ephemerides becoming lost or significantly degraded, as is the case for most transiting planets, highlights the importance of systematically updating transit ephemerides with upcoming large efforts expected to characterize hundreds of exoplanet atmospheres. K2-2 b sits at the high-mass peak of the known radius valley for sub-Neptunes, and is now well-suited for transmission spectroscopy with current and future facilities. Our updated transit ephemeris will ensure no more than a 13-minute uncertainty through 2030. Copyright © 2024, The Authors. All rights reserved.

关键词： NASA

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JCMT 850 µm continuum observations of density structures in the G35 molecular complex

arXiv

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arXiv 2024年

作者： Shen, Xianjin Liu, Hong-Li Ren, Zhiyuan Tej, Anandmayee Li, Di Liu, Hauyu Baobab Fuller, Gary A. Xie, Jinjin Jiao, Sihan Yang, Aiyuan Koch, Patrick M. Xu, Fengwei Sanhueza, Patricio Diep, Pham Ngoc Peretto, Nicolas Yadav, Ram K. Kramer, Busaba H. Sugiyama, Koichiro Rawlings, Mark G. Lee, Chang Won Tatematsu, Kenichi Harsono, Daniel Eden, David Kwon, Woojin Tsai, Chao-Wei White, Glenn J. Kim, Kee-Tae Liu, Tie Wang, Ke Zhang, Siju Jiao, Wenyu Yang, Dongting Swagat, R. Das Wu, Jingwen Wang, Chen School of Physics and Astronomy Yunnan University Kunming650091 China National Astronomical Observatories Chinese Academy of Sciences Datun Road A20 Beijing China CAS Key Laboratory of FAST NAOC Chinese Academy of Sciences Beijing China University of Chinese Academy of Sciences Beijing China Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India University of KwaZulu-Natal Durban4000 South Africa Department of Physics National Sun Yat-Sen University No. 70 Lien-Hai Road Kaohsiung City80424 Taiwan Center of Astronomy and Gravitation National Taiwan Normal University Taipei116 Taiwan Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Physikalisches Institut University of Cologne Zülpicher Str. 77 KölnD-50937 Germany Key Laboratory of Radio Astronomy and Technology Chinese Academy of Sciences A20 Datun Road Datun Road A20 Beijing China Max-Plank-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Academia Sinica Institute of Astronomy and Astrophysics No. 1 Sec. 4 Roosevelt Road Taipei10617 Taiwan Kavli Institute for Astronomy and Astrophysics Peking University 5 Yiheyuan Road Haidian District Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Vietnam National Space Center Vietnam Academy of Science and Technology 18 Hoang Quoc Viet Hanoi Viet Nam Cardiff Hub for Astrophysics Research & Technology School of Physics & Astronomy Cardiff University Queens Buildings The Parade CardiffCF24 3AA United Kingdom Sirindhorn AstroPark 260 Moo 4 T. Donkaew A. Maerim Chiangmai50180 Thailand Gemini Observato

Filaments are believed to play a key role in high-mass star formation. We present a systematic study of the filaments and their hosting clumps in the G35 molecular complex using JCMT SCUBA-2 850 µm continuum data. We identified five clouds in the complex and 91 filaments within them, some of which form 10 hub-filament systems (HFSs), each with at least 3 hub-composing filaments. We also compiled a catalogue of 350 dense clumps, 183 of which are associated with the filaments. We investigated the physical properties of the filaments and clumps, such as mass, density, and size, and their relation to star formation. We find that the global mass-length trend of the filaments is consistent with a turbulent origin, while the hub-composing filaments of high line masses (ml > 230 M☉ pc−1) in HFSs deviate from this relation, possibly due to feedback from massive star formation. We also find that the most massive and densest clumps (R > 0.2 pc, M > 35 M☉, Σ > 0.05 g cm−2) are located in the filaments and in the hubs of HFS with the latter bearing a higher probability of occurrence of high-mass star-forming signatures, highlighting the preferential sites of HFSs for high-mass star formation. We do not find significant variation in the clump mass surface density across different evolutionary environments of the clouds, which may reflect the balance between mass accretion and stellar feedback. Copyright © 2024, The Authors. All rights reserved.

关键词： Giant stars

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A Fourth Planet in the Kepler-51 System Revealed by Transit Timing Variations

arXiv

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arXiv 2024年

作者： Masuda, Kento Libby-Roberts, Jessica E. Livingston, John H. Stevenson, Kevin B. Gao, Peter Vissapragada, Shreyas Fu, Guangwei Han, Te Greklek-McKeon, Michael Mahadevan, Suvrath Agol, Eric Bello-Arufe, Aaron Berta-Thompson, Zachory Cañas, Caleb I. Chachan, Yayaati Hebb, Leslie Hu, Renyu Kawashima, Yui Knutson, Heather A. Morley, Caroline V. Murray, Catriona A. Ohno, Kazumasa Tokadjian, Armen Zhang, Xi Welbanks, Luis Nixon, Matthew C. Freedman, Richard Narita, Norio Fukui, Akihiko de Leon, Jerome P. Mori, Mayuko Palle, Enric Murgas, Felipe Parviainen, Hannu Esparza-Borges, Emma Jontof-Hutter, Daniel Collins, Karen A. Benni, Paul Barkaoui, Khalid Pozuelos, Francisco J. Gillon, Michaël Jehin, Emmanuël Benkhaldoun, Zouhair Hawley, Suzanne Lin, Andrea S.J. Stefánsson, Guðmundur Bieryla, Allyson Yilmaz, Mesut Senavci, Hakan Volkan Girardin, Eric Marino, Giuseppe Wang, Gavin Department of Earth and Space Science Osaka University Osaka560-0043 Japan Department of Astronomy & Astrophysics 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Center for Exoplanets and Habitable Worlds 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan JHU Applied Physics Laboratory 11100 Johns Hopkins Rd LaurelMD20723 United States Carnegie Science Earth and Planets Laboratory 5241 Broad Branch Road NW WashingtonDC20015 United States Carnegie Science Observatories 813 Santa Barbara Street PasadenaCA91101 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD United States Department of Physics & Astronomy The University of California Irvine IrvineCA92697 United States Division of Geological and Planetary Sciences California Institute of Technology PasadenaCA91125 United States Department of Astronomy University of Washington SeattleWA98195 United States Jet Propulsion Laboratory California Institute of Technology PasadenaCA91011 United States Department of Astrophysical and Planetary Sciences University of Colorado Boulder BoulderCO80309 United States NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Department of Physics Trottier Space Institute McGill University 3600 rue University MontréalQCH3A 2T8 Canada Université de Montréal Quebec Canada Hobart and William Smith Colleges GenevaNY14456 United States Cornell University IthacaNY14853 United States Frontier Research Institute for Interdisciplinary Sciences Tohoku University 6-3 Aramaki aza Aoba Aoba-ku Sendai Miyagi980-8578 Japan Department o

Kepler-51 is a 1 Gyr-old Sun-like star hosting three transiting planets with radii ≈ 6–9 R and orbital periods ≈ 45–130 days. Transit timing variations (TTVs) measured with past Kepler and Hubble space Telescope (HST) observations have been successfully modeled by considering gravitational interactions between the three transiting planets, yielding low masses and low mean densities ( 0.1 g/cm3) for all three planets. However, the transit time of the outermost transiting planet Kepler-51d recently measured by the James Webb space Telescope (JWST) 10 years after the Kepler observations is significantly discrepant from the prediction made by the three-planet TTV model, which we confirmed with ground-based and follow-up HST observations. We show that the departure from the three-planet model is explained by including a fourth outer planet, Kepler-51e, in the TTV model. A wide range of masses ( MJup) and orbital periods ( 10 yr) are possible for Kepler-51e. Nevertheless, all the coplanar solutions found from our brute-force search imply masses 10 M for the inner transiting planets. Thus their densities remain low, though with larger uncertainties than previously estimated. Unlike other possible solutions, the one in which Kepler-51e is around the 2: 1 mean motion resonance with Kepler-51d implies low orbital eccentricities ( 0.05) and comparable masses (∼ 5 M) for all four planets, as is seen in other compact multi-planet systems. This work demonstrates the importance of long-term follow-up of TTV systems for probing longer period planets in a system. © 2024, CC BY.

关键词： space telescopes

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Is there any linkage between interstellar aldehyde and alcohol?

arXiv

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arXiv 2021年

作者： Mondal, Suman Kumar Gorai, Prasanta Sil, Milan Ghosh, Rana Etim, Emmanuel E. Chakrabarti, Sandip K. Shimonishi, Takashi Nakatani, Naoki Furuya, Kenji Tan, Jonathan C. Das, Ankan Indian Centre for Space Physics 43 Chalantika Garia Station Road Kolkata700084 India Department of Space Earth and Environment Chalmers University of Technology GothenburgSE-412 96 Sweden Department of Chemical Sciences Federal University Wukari Katsina-Ala Road P.M.B. 1020 Taraba State Wukari Nigeria Center for Transdisciplinary Research Niigata University Nishi-ku Niigata950-2181 Japan Environmental Science Program Department of Science Faculty of Science Niigata University Nishi-ku Niigata950-2181 Japan Institute for Catalysis Hokkaido University N21W10 Kita-ku Hokkaido Sapporo001-0021 Japan Center for Computational Sciences University of Tsukuba Tsukuba305-8577 Japan Department of Astronomy University of Virginia CharlottesvilleVA22904 United States Department of Chemistry Graduate School of Science and Engineering Tokyo Metropolitan University 1-1 Minami-Osawa Hachioji Tokyo192-0397 Japan National Astronomical Observatory of Japan Tokyo181-8588 Japan

It is speculated that there might be some linkage between interstellar aldehydes and their corresponding alcohols. Here, an observational study and astrochemical modeling are coupled together to illustrate the connection between them. The ALMA cycle 4 data of a hot molecular core, G10.47+0.03 is utilized for this study. Various aldehydes (acetaldehyde, propanal, and glycolaldehyde), alcohols (methanol and ethylene glycol), and a ketone (acetone) are identified in this source. The excitation temperatures and the column densities of these species were derived via the rotation diagram method assuming LTE conditions. An extensive investigation is carried out to understand the formation of these species. Six pairs of aldehyde-alcohol: i) methanal and methanol;ii) ethanal and ethanol;iii) propanal and 1-propanol;iv) propenal and allyl alcohol;v) propynal and propar gyl alcohol;vi) glycolaldehyde and ethylene glycol;vii) along with one pair of ketone-alcohol (acetone and isopropanol) and viii) ketene-alcohol (ethenone and vinyl alcohol) are considered for this study. Two succes sive hydrogenation reactions in the ice phase are examined to form these alcohols from aldehydes, ketone, and ketene, respectively. Quantum chemical methods are extensively executed to review the ice phase formation route and the kinetics of these species. Based on the obtained kinetic data, astrochemical modeling is employed to derive the abundances of these aldehydes, alcohols, ketone, and ketene in this source. It is seen that our model could successfully explain the observed abundances of various species in this hot molecular core. Copyright © 2021, The Authors. All rights reserved.

关键词： Acetone

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ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XIX. The origin of SiO emission

arXiv

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arXiv 2024年

作者： Liu, Rong Liu, Tie Jiménez-Serra, Izaskun Li, Jin-Zeng Martín-Pintado, Jesús Liu, Xunchuan Lee, Chang Won Sanhueza, Patricio Chibueze, James O. Rivilla, Víctor M. Juvela, Mika Colzi, Laura Bronfman, Leonardo Liu, Hong-Li Sanz-Novo, Miguel López-Gallifa, Álvaro Li, Shanghuo Megías, Andrés Andrés, David San Garay, Guido Hwang, Jihye Zhou, Jianwen Xu, Fengwei Martínez-Henares, Antonio Saha, Anindya Nazeer, Hafiz National Astronomical Observatories of China Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China CSIC-INTA Carretera de Ajalvir km 4 Torrejón de Ardoz28850 Spain Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Mathematical Sciences University of South Africa Cnr Christian de Wet Rd and Pioneer Avenue Florida Park Roodepoort1709 South Africa Department of Physics and Astronomy Faculty of Physical Sciences University of Nigeria Carver Building 1 University Road Nsukka410001 Nigeria Department of Physics University of Helsinki P.O. Box 64 FI-00014 Finland Departamento de Astronomía Universidad de Chile Las Condes Santiago Chile School of Physics and Astronomy Yunnan University Kunming650091 China Max Planck Institute for Astronomy Königstuhl 17 HeidelbergD-69117 Germany Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53125 Germany Kavli Institute for Astronomy and Astrophysics Peking University Haidian District Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China

The production of silicon monoxide (SiO) can be considered as a fingerprint of shock interaction. In this work, we use high-sensitivity observations of the SiO (2-1) and H13CO+ (1-0) emission to investigate the broad and narrow SiO emission toward 146 massive star-forming regions in the ATOMS survey. We detected SiO emission in 136 regions and distinguished broad and narrow components across the extension of 118 sources (including 58 UC Hii regions) with an average angular resolution of 2.5′′. The derived SiO luminosity (LSiO) across the whole sample shows that the majority of LSiO (above 66%) can be attributed to broad SiO, indicating its association with strong outflows. The comparison of the ALMA SiO images with the filamentary skeletons identified from H13CO+ and in the infrared data (at 4.5, 8, and 24 µm), further confirms that most SiO emission originates from outflows. However, note that for nine sources in our sample, the observed SiO emission may be generated by expanding UC Hii regions. There is a moderate positive correlation between the bolometric luminosity (Lbol) and LSiO for both components (narrow and broad). The UC Hii sources show a weaker positive correlation between Lbol and LSiO and higher LSiO compared to the sources without UC Hii regions. These results imply that the SiO emission from UC Hii sources might be affected by UV-photochemistry induced by UC Hii regions. © 2024, CC BY.

关键词： Giant stars

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Physics Performance of the Large-Sized Telescope prototype of the Cherenkov Telescope Array 37

Physics Performance of the Large-Sized Telescope prototype o...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Abe, H. Aguasca, A. Agudo, I. Antonelli, L.A. Aramo, C. Armstrong, T. Artero, M. Asano, K. Ashkar, H. Aubert, P. Baktash, A. Bamba, A. Baquero Larriva, A. Baroncelli, L. Barres de Almeida, U. Barrio, J.A. Batkovic, I. Becerra González, J. Bernardos, M.I. Berti, A. Biederbeck, N. Bigongiari, C. Blanch, O. Bonnoli, G. Bordas, P. Bose, D. Bulgarelli, A. Burelli, I. Buscemi, M. Cardillo, M. Caroff, S. Carosi, A. Cassol, F. Cerruti, M. Chai, Y. Cheng, K. Chikawa, M. Chytka, L. Contreras, J.L. Cortina, J. Costantini, H. Dalchenko, M. De Angelis, A. de Bony de Lavergne, M. Deleglise, G. Delgado, C. Delgado Mengual, J. della Volpe, D. Depaoli, D. Di Pierro, F. Di Venere, L. Díaz, C. Dominik, R.M. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsässer, D. Emery, G. Escudero, J. Fiasson, A. Foffano, L. Fonseca, M.V. Freixas Coromina, L. Fukami, S. Fukazawa, Y. Garcia, E. Garcia López, R. Giglietto, N. Giordano, F. Gliwny, P. Godinovic, N. Green, D. Grespan, P. Gunji, S. Hackfeld, J. Hadasch, D. Hahn, A. Hassan, T. Hayashi, K. Heckmann, L. Heller, M. Herrera Llorente, J. Hirotani, K. Hoffmann, D. Horns, D. Houles, J. Hrabovsky, M. Hrupec, D. Hui, D. Hütten, M. Inada, T. Inome, Y. Iori, M. Ishio, K. Iwamura, Y. Jacquemont, M. Jimenez Martinez, I. Jouvin, L. Jurysek, J. Kagaya, M. Karas, V. Katagiri, H. Kataoka, J. Kerszberg, D. Kobayashi, Y. Kong, A. Kubo, H. Kushida, J. Lamanna, G. Lamastra, A. Le Flour, T. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Luque-Escamilla, P.L. Majumdar, P. Makariev, M. Mandat, D. Manganaro, M. Mannheim, K. Mariotti, M. Marquez, P. Marsella, G. Martí, J. Martinez, O. Martínez, G. Martínez, M. Marusevec, P. Mas, A. Maurin, G. Mazin, D. Mestre Guillen, E. Micanovic, S. Miceli, D. Miener, T. Miranda, J.M. Miranda, L.D.M. Mirzoyan, R. Mizuno, T. Molina, E. Montaruli, T. Monteiro, I. Moralejo, A. Morcuende, D. Moretti, E. Morselli, A. Mrakovcic, K. Murase, K. Nagai, A. Nakamori, T. Nickel, L. Nieto, D. Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Kashiwa Chiba277-8582 Japan Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Spain Instituto de Astrofísica de Andalucía-CSIC Granada18080 Spain INAF Osservatorio Astronomico di Roma Italy INFN Sezione di Napoli Italy Aix Marseille Univ CNRS IN2P3 CPPM France 08193 Spain IRFU CEA Université Paris-Saclay France LAPP Univ. Grenoble Alpes Univ. Savoie Mont Blanc CNRS-IN2P3 9 Chemin de Bellevue - BP 110 AnnecyCedex 74941 France Universität Hamburg Institut für Experimentalphysik Germany Graduate School of Science University of Tokyo Japan EMFTEL Department IPARCOS Universidad Complutense de Madrid MadridE-28040 Spain INAF Osservatorio di Astrofisica e Scienza Spazio di Bologna Italy Centro Brasileiro de Pesquisas Físicas Brazil INFN Sezione di Padova PadovaI-35131 Italy Università degli Studi di Padova Via Marzolo 8 Padova35131 Italy Instituto de Astrofísica de Canarias Departamento de Astrofísica Universidad de La Laguna Spain Max-Planck-Institut für Physik München80805 Germany Department of Physics TU Dortmund University Otto-Hahn-Str. 4 Dortmund44221 Germany Saha Institute of Nuclear Physics INFN Sezione di Trieste Università degli Studi di Udine Italy INFN Sezione di Catania Italy Italy University of Geneva Département de Physique Nucléaire et Corpusculaire Switzerland Palacky University Olomouc Faculty of Science Czech Republic CIEMAT Port d'Informació Científica Spain INFN Sezione di Torino via P. Giuria 1 Torino10125 Italy Dipartimento di Fisica Universitá degli Studi di Torino Italy INFN Sezione di Bari Università di Bari Italy University of Rijeka Department of Physics Croatia Institute for Theoretical Physics and Astrophysics Universität Würzburg Germany Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Japan INFN Sezione di Bari Politecnico di B

The Large-Sized Telescope (LST) prototype of the future Cherenkov Telescope Array (CTA) is located at the Northern site of CTA, on the Canary Island of La Palma. It is designed to provide optimal performance in the lowest part of the energy range covered by CTA, observing gamma rays down to energies of tens of GeV. The LST prototype started performing astronomical observations in November 2019 during the commissioning of the telescope and it has been taking data since then. In this contribution, we will present the tuning of the characteristics of the telescope in the Monte Carlo (MC) simulations to describe the data obtained, the estimation of its angular and energy resolution, and an evaluation of its sensitivity, both with simulations and with observations of the Crab Nebula. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)

关键词： Telescopes

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ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions − XVII. High-mass star-formation through a large-scale collapse in IRAS 15394−5358

arXiv

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arXiv 2024年

作者： Das, Swagat R. Merello, Manuel Bronfman, Leonardo Liu, Tie Garay, Guido Stutz, Amelia Mardones, Diego Zhou, Jian-Wen Sanhueza, Patricio Liu, Hong-Li Vázquez-Semadeni, Enrique Gómez, Gilberto C. Palau, Aina Tej, Anandmayee Xu, Feng-Wei Baug, Tapas Dewangan, Lokesh K. He, Jinhua Zhu, Lei Li, Shanghuo Juvela, Mika Saha, Anindya Issac, Namitha Hwang, Jihye Nazeer, Hafiz Toth, L. Viktor Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Departamento de Astronomía Universidad de Concepción Av. Esteban Iturra s/n Distrito Universitario 160-C Chile Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan School of Physics and Astronomy Yunnan University Kunming650091 China Instituto de Radioastronomía y Astrofísica Universidad Nacional Autónoma de México Apdo. Postal 3-72 Michoacán Morelia58089 Mexico Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China S. N. Bose National Centre for Basic Sciences Block-JD Sector-III Salt Lake City Kolkata700106 India Physical Research Laboratory Navrangpura Ahmedabad380 009 India Yunnan Observatories Chinese Academy of Sciences 396 Yang-fangwang Guandu District Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Max Planck Institute of Astronoy Königstuhl 17 Heidelberg69117 Germany SOFIA Science Centre USRA NASA Ames Research Centre MS-12 N232 Moffett FieldCA94035 United States Department of Physics University of Helsinki PO Box 64 HelsinkiFI-00014 Finland Korea Astronomy and Space Science Institute 776 Daedeokdaero Yuseong-gu Daejeon34055 Korea Republic of Institute of Physics and Astronomy Eotvos Lorand University Pazmany Peter setany 1/A BudapestH-1117 Hungary

Hub-filament systems are considered as natural sites for high-mass star formation. Kinematic analysis of the surroundings of hub-filaments is essential to better understand high-mass star formation within such systems. In this work, we present a detailed study of the massive Galactic protocluster IRAS 15394−5358, using continuum and molecular line data from the ALMA Three-millimeter Observations of Massive Star-forming Regions (ATOMS) survey. The 3 mm dust continuum map reveals the fragmentation of the massive (M = 843 M☉) clump into six cores. The core C-1A is the largest (radius = 0.04 pc), the most massive (M = 157 M☉), and lies within the dense central region, along with two smaller cores (M = 7 and 3 M☉). The fragmentation process is consistent with the thermal Jeans fragmentation mechanism and virial analysis shows that all the cores have small virial parameter values (αvir 13CO+ shows that the massive clump is associated with a hub-filament system, where the central hub is linked with four filaments. A sharp velocity gradient is observed towards the hub, suggesting a global collapse where the filaments are actively feeding the hub. We discuss the role of global collapse and the possible driving mechanisms for the massive star formation activity in the protocluster. Copyright © 2024, The Authors. All rights reserved.

关键词： Kinematics

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TOI-2015 b: A sub-Neptune in strong gravitational interaction with an outer non-transiting planet

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Astronomy and Astrophysics 2025年 695卷

作者： Barkaoui, K. Korth, J. Gaidos, E. Agol, E. Parviainen, H. Pozuelos, F.J. Palle, E. Narita, N. Grimm, S. Brady, M. Bean, J.L. Morello, G. Rackham, B.V. Burgasser, A.J. Van Grootel, V. Rojas-Ayala, B. Seifahrt, A. Marfil, E. Passegger, V.M. Stalport, M. Gillon, M. Collins, K.A. Shporer, A. Giacalone, S. Yalçinkaya, S. Ducrot, E. Timmermans, M. Triaud, A.H.M.J. De Wit, J. Soubkiou, A. Watkins, C.N. Aganze, C. Alonso, R. Amado, P.J. Basant, R. Baştürk, Ö. Benkhaldoun, Z. Burdanov, A. Calatayud-Borras, Y. Chouqar, J. Conti, D.M. Collins, K.I. Davoudi, F. Delrez, L. Dressing, C.D. De Leon, J. Dévora-Pajares, M. Demory, B.O. Dransfield, G. Esparza-Borges, E. Fernández-Rodriguez, G. Fukuda, I. Fukui, A. Gallardo, P.P.M. Garcia, L. Garcia, N.A. Ghachoui, M. Geraldía-González, S. Gómez Maqueo Chew, Y. González-Rodríguez, J. Günther, M.N. Hayashi, Y. Horne, K. Hooton, M.J. Hsu, C.C. Ikuta, K. Isogai, K. Jehin, E. Jenkins, J.M. Kawauchi, K. Kagetani, T. Kawai, Y. Kasper, D. Kielkopf, J.F. Klagyivik, P. Lacedelli, G. Latham, D.W. Libotte, F. Luque, R. Livingston, J.H. Mancini, L. Massey, B. Mori, M. Muñoz Torres, S. Murgas, F. Niraula, P. Orell-Miquel, J. Rapetti, David Rebolo-López, R. Ricker, G. Papini, R. Pedersen, P.P. Peláez-Torres, A. Pérez-Prieto, J.A. Poultourtzidis, E. Rodriguez, P.M. Queloz, D. Savel, A.B. Schanche, N. Sánchez-Benavente, M. Sibbald, L. Sefako, R. Sohy, S. Sota, A. Schwarz, R.P. Seager, S. Sebastian, D. Southworth, J. Stangret, M. Stefánsson, G. Stürmer, J. Srdoc, G. Thompson, S.J. Terada, Y. Vanderspek, R. Wang, G. Watanabe, N. Wilkin, F.P. Winn, J. Wells, R.D. Ziegler, C. Zúñiga-Fernández, S. Astrobiology Research Unit Université de Liège Allée du 6 Août 19C Liège4000 Belgium Department of Earth Atmospheric and Planetary Science Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Calle Vía Láctea s/n Tenerife La Laguna38200 Spain Lund Observatory Division of Astrophysics Department of Physics Lund University Box 118 Lund22100 Sweden Department of Earth Sciences University of Hawaii at Manoa 1680 East-West Rd HonoluluHI96822 United States Institute for Astrophysics University of Vienna Türkenschanzstrasse 17 Vienna1180 Austria Department of Astronomy and Astrobiology Program University of Washington Box 351580 SeattleWA98195 United States NExSS Virtual Planetary Laboratory University of Washington Box 351580 SeattleWA98195 United States Tenerife La LagunaE-38206 Spain Glorieta de la Astronomía s/n Granada18008 Spain INAF-Palermo Astronomical Observatory Piazza del Parlamento 1 Palermo90134 Italy Komaba Institute for Science University of Tokyo 3-8-1 Komaba Tokyo Meguro153-8902 Japan Astrobiology Center 2-21-1 Osawa Tokyo Mitaka181-8588 Japan Research Institute for Advanced Computer Science Universities Space Research Association WashingtonDC20024 United States Institute for Particle Physics and Astrophysics ETH Zürich OttoStern-Weg 5 Zürich8093 Switzerland Department of Astrophysics University of Zürich Winterthurerstrasse 190 Zürich8057 Switzerland Department of Astronomy & Astrophysics University of Chicago ChicagoIL United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Institute Université de Liège Allée du 6 Août 19C LiègeB-4000 Belgium Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica Chile Gemini Observatory/NSF NOIRLab 670 N. A'ohoku Place HiloHI96720 United States Departamento de Ingeniería Topográfica y Cartografía E.

TOI-2015 is a known exoplanetary system around an M4 dwarf star, consisting of a transiting sub-Neptune planet in a 3.35-day orbital period, TOI-2015 b, accompanied by a non-transiting companion, TOI-2015 c. High-precision radial-velocity measurements were taken with the MAROON-X spectrograph, and high-precision photometric data were collected, primarily using the SPECULOOS, MUSCAT, TRAPPIST and LCOGT networks. We collected 63 transit light curves and 49 different transit epochs for TOI-2015 b. We recharacterized the target star by combining optical spectra obtained by the MAROON-X, Shane/KAST and IRTF/SpeX spectrographs, Bayesian model averaging (BMA) and spectral energy distribution (SED) analysis. The TOI-2015 host star is a K = 10.3 mag M4-type dwarf with a subsolar metallicity of [Fe/H] =-0.31 ± 0.16, and an effective temperature of Teff ≈ 3200 K. Our photodynamical analysis of the system strongly favors the 5:3 mean-motion resonance and in this scenario the planet b (TOI-2015 b) has an orbital period of Pb = 3.34 days, a mass of Mp = 9.02-0.36+0.32M⊕, and a radius of Rp = 3.309-0.011+0.013R⊕, resulting in a density of ρp = 0.25 ± 0.01 ρ⊕ = 1.40 ± 0.06 g cm-3;this is indicative of a Neptune-like composition. Its transits exhibit large (> 1 hr) timing variations characteristic of an outer perturber in the system. We performed a global analysis of the high-resolution radial-velocity measurements, the photometric data, and the TTVs, and inferred that TOI-2015 hosts a second planet, TOI-2015 c, in a non-transiting configuration. Our analysis places it near a 5:3 resonance with an orbital period of Pc = 5.583 days and a mass of Mp = 8.91-0.40+0.38M⊕. The dynamical configuration of TOI-2015 b and TOI-2015 c can be used to constrain the system's planetary formation and migration history. Based on the mass-radius composition models, TOI-2015 b is a water-rich or rocky planet with a hydrogen-helium envelope. Moreover, TOI-2015 b has a high transmission-spectroscopic met

关键词： Velocity measurement

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