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arXiv 2022年

作者： Shim, Hyunjin Lee, Dongseob Kim, Yeonsik Scott, Douglas Serjeant, Stephen Ao, Yiping Barrufet, Laia Chapman, Scott C. Clements, David L. Conselice, Christopher J. Goto, Tomotsugu Greve, Thomas R. Hwang, Ho Seong Im, Myungshin Jeong, Woong-Seob Kim, Helen K. Kim, Minjin Kim, Seong Jin Kong, Albert K.H. Koprowski, MacIej P. Malkan, Matthew A. Michalowski, Michal J. Pearson, Chris Seo, Hyunjong Takagi, Toshinobu Toba, Yoshiki White, Glenn J. Woo, Jong-Hak Department of Earth Science Education Kyungpook National University Daegu41566 Korea Republic of Department of Astronomy and Atmospheric Sciences Kyungpook National University Daegu41566 Korea Republic of Department of Physics and Astronomy University of British Columbia Canada The Open University Milton KeynesMK7 6AA United Kingdom Purple Mountain Observatory Key Laboratory for Radio Astronomy Chinese Academy of Sciences Nanjing China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei China Geneva Observatory University of Geneva Versoix Switzerland Ral Space Stfc Rutherford Appleton Laboratory Oxfordshire DidcotOX11 0QX United Kingdom Department of Physics and Atmospheric Science Dalhouise University HalifaxNSB3H 4R2 Canada Imperial College London Blackett Lab. Prince Consort Road LondonSW7 2AZ United Kingdom Department of Physics and Astronomy University of Manchester United Kingdom Institute of Astronomy National Tsing Hua University 101 Section 2. Kuang-Fu Road Hsinchu30013 Taiwan Cosmic Dawn Center National Space Institute Dtu Space Technical University of Denmark Elektrovej 327 Kgs. LyngbyDK-2800 Denmark Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Astronomy Program Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Snu Astronomy Research Center Astronomy Program Department of Physics and Astronomy Seoul National University Korea Republic of Korea Astronomy and Space Science Institute Daejeon34055 Korea Republic of Department of Physics and Astronomy Ucla Los AngelesCA90095-1547 United States Institute of Astronomy Faculty of Physics Astronomy and Informatics Nicolaus Copernicus University Grudziadzka 5 Torun87-100 Poland Astronomical Observatory Institute Faculty of Physics Adam Mickiewicz University ul. Sloneczna 36 Poznan60-286 Poland Japan Scien

We present the multi-wavelength counterparts of 850-μm selected submillimetre sources over a 2-deg2field centred on the North Ecliptic Pole. In order to overcome the large beam size (15 arcsec) of the 850-μm images, deep optical to near-infrared (NIR) photometric data and arcsecond-resolution 20-cm images are used to identify counterparts of submillimetre sources. Among 647 sources, we identify 514 reliable counterparts for 449 sources (69 per cent in number), based either on probabilities of chance associations calculated from positional offsets or offsets combined with the optical-to-NIR colours. In the radio imaging, the fraction of 850-μm sources having multiple counterparts is 7 per cent. The photometric redshift, infrared luminosity, stellar mass, star-formation rate (SFR), and the AGN contribution to the total infrared luminosity of the identified counterparts are investigated through spectral energy distribution fitting. The SMGs are infrared-luminous galaxies at an average (z) = 2.5 with log10(LIR/Lo) = 11.5-13.5, with a mean stellar mass of log10(Mstar/Mo) = 10.90 and SFR of log10(SFR/Moyr-1) = 2.34. The SMGs show twice as large SFR as galaxies on the starforming main sequence, and about 40 per cent of the SMGs are classified as objects with bursty star formation. At z ≥ 4, the contribution of AGN luminosity to total luminosity for most SMGs is larger than 30 per cent. The FIR-to-radio correlation coefficient of SMGs is consistent with that of main-sequence galaxies at z ≅ 2. Copyright © 2022, The Authors. All rights reserved.

关键词： Surveys

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Feedback from protoclusters does not significantly change the kinematic properties of the embedded dense gas structures

arXiv

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arXiv 2023年

作者： Zhou, J.W. Dib, S. Wyrowski, F. Liu, T. Li, S.H. Sanhueza, P. Juvela, M. Xu, F.W. Liu, H.L. Baug, T. Peng, Y.P. Menten, K.M. Bronfman, L. Lee, C.W. Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany Max Planck Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Physics University of Helsinki P.O.Box 64 FI-00014 Finland Kavli Institute for Astronomy and Astrophysics Peking University Haidian District Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Department of Astronomy Yunnan University Kunming650091 China Department of Physics Faculty of Science Kunming University of Science and Technology Kunming650500 China National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Departamento de Astronomía Universidad de Chile Casilla 36-D Santiago Chile Satyendra Nath Bose National Centre for Basic Sciences BlockJD Sector-III Salt Lake Kolkata700 106 India Korea Astronomy and Space Science Institute 776 Daedeokdaero Yuseonggu Daejeon34055 Korea Republic of 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan

A total of 64 ATOMS sources at different evolutionary stages were selected to investigate the kinematics and dynamics of gas structures under feedback. We identified dense gas structures based on the integrated intensity map of H13CO+ J=1-0 emission, and then extracted the average spectra of all structures to investigate their velocity components and gas kinematics. For the scaling relations between velocity dispersion σ, effective radius R and column density N of all structures, σ − N ∗ R always has a stronger correlation compared to σ − N and σ − R. There are significant correlations between velocity dispersion and column density, which may imply that the velocity dispersion originates from gravitational collapse, also revealed by the velocity gradients. The measured velocity gradients for dense gas structures in early-stage sources and late-stage sources are comparable, indicating gravitational collapse through all evolutionary stages. Late-stage sources do not have large-scale hub-filament structures, but the embedded dense gas structures in late-stage sources show similar kinematic modes to those in early- and middle-stage sources. These results may be explained by the multi-scale hub-filament structures in the clouds. We quantitatively estimated the velocity dispersion generated by the outflows, inflows, ionized gas pressure and radiation pressure, and found that the ionized gas feedback is stronger than other feedback mechanisms. However, although feedback from Hii regions is the strongest, it does not significantly affect the physical properties of the embedded dense gas structures. Combining with the conclusions in Zhou et al. (2023a) on cloud-clump scales, we suggest that although feedback from cloud to core scales will break up the original cloud complex, the substructures of the original complex can be reorganized into new gravitationally governed configurations around new gravitational centers. This process is accompanied by structural destruction and g

关键词： Gases

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Multiwavelength Constraints on the Origin of a Nearby Repeating Fast Radio Burst Source in a Globular Cluster

arXiv

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arXiv 2023年

作者： Pearlman, Aaron B. Scholz, Paul Bethapudi, Suryarao Hessels, Jason W.T. Kaspi, Victoria M. Kirsten, Franz Nimmo, Kenzie Spitler, Laura G. Fonseca, Emmanuel Meyers, Bradley W. Stairs, Ingrid H. Tan, Chia Min Bhardwaj, Mohit Chatterjee, Shami Cook, Amanda M. Curtin, Alice P. Dong, Fengqiu Adam Eftekhari, Tarraneh Gaensler, B.M. Güver, Tolga Kaczmarek, Jane Leung, Calvin Masui, Kiyoshi W. Michilli, Daniele Prince, Thomas A. Sand, Ketan R. Shin, Kaitlyn Smith, Kendrick M. Tendulkar, Shriharsh P. Department of Physics McGill University MontréalQC Canada Trottier Space Institute McGill University MontréalQC Canada Division of Physics Mathematics and Astronomy California Institute of Technology PasadenaCA United States Dunlap Institute for Astronomy and Astrophysics University of Toronto TorontoON Canada Department of Physics and Astronomy York University TorontoON Canada Max-Planck-Institut für Radioastronomie Bonn Germany Anton Pannekoek Institute for Astronomy University of Amsterdam Amsterdam Netherlands ASTRON Netherlands Institute for Radio Astronomy Dwingeloo Netherlands Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala Sweden MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA United States Department of Physics and Astronomy West Virginia University MorgantownWV United States Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building MorgantownWV United States International Centre for Radio Astronomy Research Curtin University BentleyWA Australia Department of Physics and Astronomy University of British Columbia VancouverBC Canada McWilliams Center for Cosmology Department of Physics Carnegie Mellon University PittsburghPA United States Cornell Center for Astrophysics and Planetary Science Cornell University IthacaNY United States David A. Dunlap Department of Astronomy and Astrophysics University of Toronto TorontoON Canada Center for Interdisciplinary Exploration and Research in Astrophysics Department of Physics and Astronomy Northwestern University EvanstonIL United States Department of Astronomy and Astrophysics University of California Santa Cruz Santa CruzCA United States Department of Astronomy and Space Sciences Science Faculty Istanbul University Istanbul Turkey Istanbul University Observatory Research and Application Center Istanbul University Istanbul T

The precise origins of fast radio bursts (FRBs) remain unknown. Multiwavelength observations of nearby FRB sources can provide important insights into the enigmatic FRB phenomenon. Here, we present results from a sensitive, broadband X-ray and radio observational campaign of FRB 20200120E, the closest known extragalactic repeating FRB source (located 3.63 Mpc away in an ∼10-Gyr-old globular cluster). We place deep limits on the persistent and prompt X-ray emission from FRB 20200120E, which we use to constrain possible origins for the source. We compare our results with various classes of X-ray sources, transients, and FRB models. We find that FRB 20200120E is unlikely to be associated with ultraluminous X-ray bursts, magnetar-like giant flares, or an SGR 1935+2154-like intermediate flare. Although other types of bright magnetar-like intermediate flares and short X-ray bursts would have been detectable from FRB 20200120E during our observations, we cannot entirely rule them out as a class. We show that FRB 20200120E is unlikely to be powered by an ultraluminous X-ray source or a young extragalactic pulsar embedded in a Crab-like nebula. We also provide new constraints on the compatibility of FRB 20200120E with accretion-based FRB models involving X-ray binaries. These results highlight the power of multiwavelength observations of nearby FRBs for discriminating between FRB models. © 2023, CC BY.

关键词： X-ray astronomy

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Performance evaluation of the high-voltage CMOS active pixel sensor AstroPix for gamma-ray space telescopes

arXiv

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arXiv 2024年

作者： Suda, Yusuke Caputo, Regina Steinhebel, Amanda L. Striebig, Nicolas Jadhav, Manoj Fukazawa, Yasushi Hashizume, Masaki Kierans, Carolyn Leys, Richard Metcalfe, Jessica Negro, Michela Perić, Ivan Perkins, Jeremy S. Shin, Taylor Tajima, Hiroyasu Violette, Daniel Nakano, Norito Physics Program Graduate School of Advanced Science and Engineering Hiroshima University 1-3-1 Kagamiyama Higashihiroshima Hiroshima739-8526 Japan NASA Goddard Space Flight Center 8800 Greenbelt Rd GreenbeltMDMD 20771 United States 8800 Greenbelt Rd GreenbeltMDMD 20771 United States ASIC and Detector Laboratory Karlsruhe Institute of Technology Hermann-von-Helmholtz-Platz 1 Karlsruhe Baden-WürttembergD-76344 Germany Argonne National Laboratory 9700 S. Cass Avenue LemontILIL 60439 United States Department of Physics and Astronomy Louisiana State University 202 Nicholson Hall Baton RougeLALA 70803 United States University of California Santa Cruz 1156 High Street Santa CruzCACA 95064 United States Institute for Space–Earth Environmental Research Nagoya University Furo-cho Chikusa-ku Aichi Nagoya464-8601 Japan Kobayashi-Maskawa Institute for the Origin of Particles and the Universe Nagoya University Furo-cho Chikusa-ku Aichi Nagoya464-8602 Japan

AstroPix is a novel monolithic high-voltage CMOS active pixel sensor proposed for next generation medium-energy gamma-ray observatories like the All-sky Medium Energy Gamma-ray Observatory eXplorer (AMEGO-X). For AMEGO-X AstroPix must maintain a power consumption of less than 1.5 mW/cm2 while having a pixel pitch of up to 500 µm. We developed the second and third versions of AstroPix, namely AstroPix2 and AstroPix3. AstroPix2 and AstroPix3 exhibit power consumptions of 3.4 mW/cm2 and 4.1 mW/cm2, respectively. While AstroPix2 has a pixel pitch of 250 µm, AstroPix3 achieves the desired size for AMEGO-X with a pixel pitch of 500 µm. Performance evaluation of a single pixel in an AstroPix2 chip revealed a dynamic range from 13.9 keV to 59.5 keV, with the energy resolution meeting the AMEGO-X target value (60Co source. The chip was fully operational after irradiation although a decrease in gain by approximately 4% was observed. Copyright © 2024, The Authors. All rights reserved.

关键词： CMOS integrated circuits

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TOI-3493 b: A planet with a Neptune-like density transiting a bright G0-type star

arXiv

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arXiv 2025年

作者： Chaturvedi, P. Goffo, E. Gandolfi, D. Persson, C.M. Hatzes, A.P. Nowak, G. Bonfanti, A. Bieryla, A. Cochran, W.D. Collins, K.A. Fajardo-Acosta, S.B. Howell, S.B. Jenkins, J.M. Korth, J. Livingston, J. Pallé, E. Quinn, S.N. Schwarz, R.P. Seager, S. Shporer, A. Stassun, K.G. Striegel, S. Van Eylen, V. Watkins, C.N. Winn, J.N. Ziegler, C. Thüringer Landessternwarte Tautenburg Sternwarte 5 Tautenburg07778 Germany Department of Astronomy and Astrophysics Tata Institute of Fundamental Research Mumbai400005 India Dipartimento di Fisica Università degli Studi di Torino via Pietro Giuria 1 TorinoI-10125 Italy Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala43992 Sweden Institute of Astronomy Faculty of Physics Astronomy and Informatics Nicolaus Copernicus University Grudziądzka 5 Toruń87-100 Poland Space Research Institute Austrian Academy of Sciences Schmiedlstrasse 6 GrazA-8042 Austria Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States McDonald Observatory The University of Texas AustinTX United States Center for Planetary Systems Habitability The University of Texas AustinTX United States Caltech IPAC Mail Code 100-22 PasadenaCA91125 United States NASA Ames Research Center Moffett Field CA94035 United States Lund Observatory Division of Astrophysics Department of Physics Lund University Box 118 Lund22100 Sweden 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 Calle Vía Láctea s/n Tenerife La Laguna38205 Spain Tenerife La Laguna38206 Spain Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Department of Earth Atmospheric and Planetary Sciences Massachusetts Institute of Technology CambridgeMA02139 United States Department of Aeronautics and Astronautics MIT 77 Massachusetts Avenue CambridgeMA02139 United States Department of Physics and Astronomy Vanderbilt University NashvilleTN37235 United States SETI Institute Mountain ViewCA94043 U

We report the discovery of TOI-3493 b, a sub-Neptune-sized planet on an 8.15-d orbit transiting the bright (V=9.3) G0 star HD 119355 (aka TIC 203377303) initially identified by NASA’s TESS space mission. With the aim of confirming the planetary nature of the transit signal detected by TESS and determining the mass of the planet, we performed an intensive Doppler campaign with the HARPS spectrograph, collecting radial velocity measurements. We found that TOI-3493 b lies in a nearly circular orbit and has a mass of 9.0 ± 1.2 M and a radius of 3.22 ± 0.08 R, implying a bulk density of 1.47+0.23-0.22g cm−3, consistent with a composition comprising a small solid core surrounded by a thick H/He-dominated atmosphere. © 2025, CC BY.

关键词： Earth atmosphere

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GLOBAL OCEANS

引用

BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY 2022年第8期103卷 S149-S191页

作者： Johnson, G. C. Lumpkin, R. NOAA/OAR Pacific Marine Environmental Laboratory Seattle Washington NOAA/OAR Atlantic Oceanographic and Meteorological Laboratory Miami Florida NOAA/NESDIS National Centers for Environmental Information Silver Spring Maryland NASA Goddard Space Flight Center Greenbelt Maryland and Morgan State University Baltimore Maryland College of Marine Science University of South Florida St. Petersburg Florida International Center for Climate and Environment Sciences Institute of Atmospheric Physics Chinese Academy of Sciences Beijing Department of Earth Environmental and Planetary Sciences Brown University Providence Rhode Island National Oceanography Centre NASA Goddard Space Flight Center Greenbelt Maryland School of Earth and Atmospheric Sciences Georgia Institute of Technology Atlanta NASA Goddard Space Flight Center Greenbelt Maryland and Science Systems and Application Inc. Lanham Maryland Science Systems and Applications Inc. Hampton Virginia Scripps Institution of Oceanography University of California San Diego La Jolla California Jet Propulsion Laboratory California Institute of Technology Pasadena California Met Office Hadley Centre Exeter Australian Antarctic Program Partnership Institute for Marine and Antarctic Studies and Australian Research Council Centre of Excellence for Climate Extremes University of Tasmania Hobart Tasmania NOAA/NWS NCEP Climate Prediction Center College Park Maryland NOAA/NESDIS National Centers for Environmental Information Asheville North Carolina National Oceanography Centre Liverpool Rosenstiel School of Marine and Atmospheric Science University of Miami Miami Florida Japan Meteorological Agency Tokyo Cooperative Institute for Marine and Atmospheric Studies University of Miami and NOAA/OAR Atlantic Oceanographic and Meteorological Laboratory Miami Florida currently at Direction Générale de l’Armement Ingénierie des projets Paris NOAA/NWS NCWCP Laboratory for Satellite Altimetry College Park Maryland Cooperative Institute

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The ALMA-QUARKS survey: – I. Survey description and data reduction

arXiv

引用

arXiv 2023年

作者： Liu, Xunchuan Liu, Tie Zhu, Lei Garay, Guido Liu, Hong-Li Goldsmith, Paul Evans, Neal Kim, Kee-Tae Liu, Sheng-Yuan Xu, Fengwei Lu, Xing Tej, Anandmayee Mai, Xiaofeng Bronfman, Leonardo Li, Shanghuo Mardones, Diego Stutz, Amelia Tatematsu, Kenichi Wang, Ke Zhang, Qizhou Qin, Sheng-Li Zhou, Jianwen Luo, Qiuyi Zhang, Siju Cheng, Yu He, Jinhua Gu, Qilao Li, Ziyang Zhang, Zhenying Zhang, Suinan Saha, Anindya Dewangan, Lokesh Sanhueza, Patricio Shen, Zhiqiang Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile School of Physics and Astronomy Yunnan University Kunming650091 China Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Department of Astronomy The University of Texas AustinTX78712-1205 United States Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Institute of Astronomy and Astrophysics Academia Sinica Roosevelt Road Taipei10617 Taiwan 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 Max Planck Institute for Astronomy Königstuhl 17 HeidelbergD-69117 Germany Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Nobeyama Radio Observatory National Astronomical Observatory of Japan National Institutes of Natural Sciences 462-2 Nobeyama Minamimaki Minamisaku Nagano384-1305 Japan Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53125 Germany School of Astronomy and Space Sciences University of Chinese Academy of Sciences Beijing100049 China National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China Physical Research Laboratory Navrangpura Ahmedabad380 009 India GUAS Astronomical Science Program SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan

This paper presents an overview of the QUARKS survey, which stands for ‘Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures’. The QUARKS survey is observing 139 massive clumps covered by 156 pointings at ALMA Band 6 (λ ∼ 1.3 mm). In conjunction with data obtained from the ALMA-ATOMS survey at Band 3 (λ ∼ 3 mm), QUARKS aims to carry out an unbiased statistical investigation of massive star formation process within protoclusters down to a scale of 1000 au. This overview paper describes the observations and data reduction of the QUARKS survey, and gives a first look at an exemplar source, the mini-starburst Sgr B2(M). The wide-bandwidth (7.5 GHz) and high-angular-resolution (∼ 0.3′′) observations of the QUARKS survey allow to resolve much more compact cores than could be done by the ATOMS survey, and to detect previously unrevealed fainter filamentary structures. The spectral windows cover transitions of species including CO, SO, N2D+, SiO, H30α, H2CO, CH3CN and many other complex organic molecules, tracing gas components with different temperatures and spatial extents. QUARKS aims to deepen our understanding of several scientific topics of massive star formation, such as the mass transport within protoclusters by (hub-)filamentary structures, the existence of massive starless cores, the physical and chemical properties of dense cores within protoclusters, and the feedback from already formed high-mass young protostars. Copyright © 2023, The Authors. All rights reserved.

关键词： Data reduction

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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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Elemental abundances of 44 very metal-poor stars determined from Subaru/IRD near-infrared spectra

arXiv

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arXiv 2025年

作者： Aoki, Wako Beers, Timothy C. Honda, Satoshi Matsuno, Tadafumi Placco, Vinicius M. Yoon, Jinmi Kuzuhara, Masayuki Harakawa, Hiroki Hirano, Teruyuki Kotani, Takayuki Kurokawa, Takashi Nishikawa, Jun Omiya, Masashi Tamura, Motohide Vievard, Sébastien National Astronomical Observatory 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Physics and Astronomy JINA Center for the Evolution of the Elements University of Notre Dame Notre DameIN46556 United States Nishi-Harima Astronomical Observatory Center for Astronomy University of Hyogo 407-2 Nishigaichi Sayo-cho Hyogo Sayo679-5313 Japan Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Mönchhofstraße 12–14 Heidelberg69120 Germany NSF NOIRLab 950 N. Cherry Ave. TucsonAZ85719 United States Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United States Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Subaru Telescope 650 N. Aohoku Place HiloHI96720 United States Institute of Engineering Tokyo University of Agriculture and Technology 2-24-16 Nakacho Koganei Tokyo184-8588 Japan Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan

关键词： Supernovae

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The magnetic field in quiescent star-forming filament G16.96+0.27

arXiv

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arXiv 2024年

作者： Gu, Qi-Lao Liu, Tie Shen, Zhi-Qiang Jiao, Sihan Montillaud, Julien Juvela, Mika Lu, Xing Lee, Chang Won Liu, Junhao Li, Pak Shing Liu, Xunchuan Johnstone, Doug Kwon, Woojin Kim, Kee-Tae Tatematsu, Ken’ichi Sanhueza, Patricio Ristorcelli, Isabelle Koch, Patrick Zhang, Qizhou Pattle, Kate Hirano, Naomi Alina, Dana Di Francesco, James Shanghai Astronomical Observatory Chinese Academy of Sciences No.80 Nandan Road Xuhui Shanghai200030 China National Astronomical Observatories Chinese Academy of Sciences A20 Datun Road Chaoyang Beijing100101 China Université de Franche-Comté CNRS Institut UTINAM OSU THETA BesançonF-25000 France Department of Physics University of Helsinki PO box 64 FI-00014 Finland Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of University of Science and Technology 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of National Astronomical Observatory of Japan 2-21-1 Osawa Tokyo Mitaka181-8588 Japan NRC Herzberg Astronomy and Astrophysics 5071 West Saanich Rd VictoriaBCV9E 2E7 Canada Department of Physics and Astronomy University of Victoria VictoriaBCV8P 5C2 Canada Department of Earth Science Education Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of The Center for Educational Research Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Nobeyama Radio Observatory National Astronomical Observatory of Japan National Institutes of Natural Sciences Nobeyama Minamimaki Minamisaku Nagano384-1305 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Tokyo Mitaka181-8588 Japan IRAP Université de Toulouse CNRS 9 avenue du Colonel Roche BP 44346 Toulouse31028 Cedex 4 France Academia Sinica Institute of Astronomy and Astrophysics No. 1 Section 4 Roosevelt Road Taipei10617 Taiwan Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Physics School of Science and Technology Nazarbayev University Astana010000 Kazakhs

We present 850 µm thermal dust polarization observations with a resolution of 14.4′′(∼ 0.13 pc) towards an infrared dark cloud G16.96+0.27 using JCMT/POL-2. The average magnetic field orientation, which roughly agrees with the larger-scale magnetic field orientation traced by the Planck 353 GHz data, is approximately perpendicular to the filament structure. The estimated plane-of-sky magnetic field strength is ∼ 96 µG and ∼ 60 µG using two variants of the Davis-Chandrasekhar-Fermi methods. We calculate the virial and magnetic critical parameters to evaluate the relative importance of gravity, the magnetic field, and turbulence. The magnetic field and turbulence are both weaker than gravity, but magnetic fields and turbulence together are equal to gravity, suggesting that G16.96+0.27 is in a quasi-equilibrium state. The cloud-magnetic-field alignment is found to have a trend moving away from perpendicularity in the dense regions, which may serve as a tracer of potential fragmentation in such quiescent filaments. © 2024, CC BY.

关键词： Stars

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