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A study of Galactic Plane Planck Galactic cold clumps observed by SCOPE and the JCMT Plane Survey

Monthly Notices of the Royal Astronomical Society 2024年第4期530卷 5192-5208页

作者： Eden, D.J. Liu, Tie Moore, T.J.T. Di Francesco, J. Fuller, G. Kim, Kee-Tae Li, Di Liu, S.-Y. Plume, R. Tatematsu, Ken'ichi Thompson, M.A. Wu, Y. Bronfman, L. Butner, H.M. Currie, M.J. Garay, G. Goldsmith, P.F. Hirano, N. Johnstone, D. Juvela, M. Lai, S.-P. Lee, C.W. Mannfors, E.E. Olguin, F. Pattle, K. Park, Geumsook Polychroni, D. Rawlings, M. Rigby, A.J. Sanhueza, P. Traficante, A. Urquhart, J.S. Weferling, B. White, G.J. Yadav, R.K. Armagh Observatory and Planetarium College Hill ArmaghBT61 9DB United Kingdom Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Astrophysics Research Institute Liverpool John Moores University Liverpool Science Park iC2 146 Brownlow Hill LiverpoolL3 5RF United Kingdom NRC Herzberg Astronomy and Astrophysics 5071 West Saanich Rd VictoriaBCV9E 2E7 Canada Department of Physics and Astronomy University of Victoria VictoriaBCV8W 2Y2 Canada Jodrell Bank Centre for Astrophysics School of Physics and Astronomy The University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejon34055 Korea Republic of 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of NationalAstronomicalObservatories ChineseAcademyofSciences Beijing100012 China Key Laboratory of Radio Astronomy Chinese Academy of Science Nanjing210008 China Academia Sinica Institute of Astronomy and Astrophysics 11F of AS/NTU Astronomy – Mathematics Building No.1 Section 4 Roosevelt Rd Taipei10617 Taiwan Department of Physics and Astronomy University of Calgary 2500 University Drive NW CalgaryABT2N 1N4 Canada 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 Mitaka Tokyo181-8588 Japan School of Physics and Astronomy University of Leeds LeedsLS2 9JT United Kingdom Department of Astronomy Peking University Beijing100871 China Astronomy Department Universidad de Chile Casilla 36-D Santiago7591245 Chile Department of Physics and Astronomy James Madison University MSC 4502 901 Carrier Drive HarrisonburgVA22807 United States RAL Space STFC Rutherford Appleton Laboratory Chilton Didcot OxfordshireOX11 0QX United Kingdom East Asian Obser

We have investigated the physical properties of Planck Galactic Cold Clumps (PGCCs) located in the Galactic Plane, using the JCMT Plane Survey (JPS) and the SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE) survey. By utilizing a suite of molecular-line surveys, velocities, and distances were assigned to the compact sources within the PGCCs, placing them in a Galactic context. The properties of these compact sources show no large-scale variations with Galactic environment. Investigating the star-forming content of the sample, we find that the luminosity-to-mass ratio (L/M) is an order of magnitude lower than in other Galactic studies, indicating that these objects are hosting lower levels of star formation. Finally, by comparing ATLASGAL sources that are associated or are not associated with PGCCs, we find that those associated with PGCCs are typically colder, denser, and have a lower L/M ratio, hinting that PGCCs are a distinct population of Galactic Plane sources. © 2024 The Author(s).

关键词： Stars

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JASMINE: Near-Infrared Astrometry and Time Series Photometry science

arXiv

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arXiv 2023年

作者： Kawata, Daisuke Kawahara, Hajime Gouda, Naoteru Secrest, Nathan J. Kano, Ryouhei Kataza, Hirokazu Isobe, Naoki Ohsawa, Ryou Usui, Fumihiko Yamada, Yoshiyuki Graham, Alister W. Pettitt, Alex R. Asada, Hideki Baba, Junichi Bekki, Kenji Dorland, Bryan N. Fujii, Michiko Fukui, Akihiko Hattori, Kohei Hirano, Teruyuki Kamizuka, Takafumi Kashima, Shingo Kawanaka, Norita Kawashima, Yui Klioner, Sergei A. Kodama, Takanori Koshimoto, Naoki Kotani, Takayuki Kuzuhara, Masayuki Levine, Stephen E. Majewski, Steven R. Masuda, Kento Matsunaga, Noriyuki Miyakawa, Kohei Miyoshi, Makoko Morihana, Kumiko Nishi, Ryoichi Notsu, Yuta Omiya, Masashi Sanders, Jason Tanikawa, Ataru Tsujimoto, Masahiro Yano, Taihei Aizawa, Masataka Arimatsu, Ko Biermann, Michael Boehm, Celine Chiba, Masashi Debattista, Victor P. Gerhard, Ortwin Hirabayashi, Masayuki Hobbs, David Ikenoue, Bungo Izumiura, Hideyuki Jordi, Carme Kohara, Naoki Löffler, Wolfgang Luri, Xavier Mase, Ichiro Miglio, Andrea Mitsuda, Kazuhisa Newswander, Trent Nishiyama, Shogo Obuchi, Yoshiyuki Ootsubo, Takafumi Ouchi, Masami Ozaki, Masanobu Perryman, Michael Prusti, Timo Ramos, Pau Read, Justin I. Rich, R. Michael Schönrich, Ralph Shikauchi, Minori Shimizu, Risa Suematsu, Yoshinori Tada, Shotaro Takahashi, Aoi Tatekawa, Takayuki Tatsumi, Daisuke Tsujimoto, Takuji Tsuzuki, Toshihiro Urakawa, Seitaro Uraguchi, Fumihiro Utsunomiya, Shin Van Eylen, Vincent van Leeuwen, Floor Wada, Takehiko Walton, Nicholas A. National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Mullard Space Science Laboratory University College London Holmbury St. Mary Dorking SurreyRH5 6NT United Kingdom Institute of Space and Astronautical Science Japan Aerospace Exploration Agency 3-1-1 Yoshinodai Chuo-ku Kanagawa Sagamihara252-5210 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-1855 Japan U.S. Naval Observatory 3450 Massachusetts Ave NW WashingtonDC20392-5420 United States Department of Physics Kyoto University Kitashirakawa-oiwake-cho Sakyo-ku Kyoto606-8502 Japan Centre for Astrophysics and Supercomputing Swinburne University of Technology HawthornVIC3122 Australia Department of Physics and Astronomy California State University Sacramento 6000 J Street SacramentoCA95819-6041 United States Graduate School of Science and Technology Hirosaki University Aomori036-8561 Japan Graduate School of Science and Engineering Kagoshima University 1-21-35 Korimoto Kagoshima890-0065 Japan International Centre for Radio Astronomy Research The University of Western Australia 7 Fairway CrawleyWA6009 Australia Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Department of Earth and Planetary Science Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Institute of Statistical Mathematics 10-3 Midoricho Tachikawa Tokyo190-8562 Japan Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Institute of Astronomy Graduate School of Science The University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kitashirakawa-oiwake-cho Sakyo-ku Kyoto606-8502 Japan Cluster for Pioneering Research RIKEN 2-1 Hirosawa Saitama Wako351-0198 Japan Lohrmann Observ

Japan Astrometry Satellite Mission for INfrared Exploration (JASMINE) is a planned M-class science space mission by the Institute of space and Astronautical science, the Japan Aerospace Exploration Agency. JASMINE has two main science goals. One is the Galactic archaeology with Galactic Center Survey, which aims to reveal the Milky Way's central core structure and formation history from Gaia-level (∼25 µas) astrometry in the Near-Infrared (NIR) Hw-band (1.0-1.6 µm). The other is the Exoplanet Survey, which aims to discover transiting Earth-like exoplanets in the habitable zone from NIR time-series photometry of M dwarfs when the Galactic center is not accessible. We introduce the mission, review many science objectives, and present the instrument concept. JASMINE will be the first dedicated NIR astrometry space mission and provide precise astrometric information of the stars in the Galactic center, taking advantage of the significantly lower extinction in the NIR. The precise astrometry is obtained by taking many short-exposure images. Hence, the JASMINE Galactic center survey data will be valuable for studies of exoplanet transits, asteroseismology, variable stars and microlensing studies, including discovery of (intermediate mass) black holes. We highlight a swath of such potential science, and also describe synergies with other missions. © 2023, CC BY.

关键词： Time series

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The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST

arXiv

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arXiv 2024年

作者： Thao, Pa Chia Mann, Andrew W. Feinstein, Adina D. Gao, Peter Thorngren, Daniel Rotman, Yoav Welbanks, Luis Brown, Alexander Duvvuri, Girish M. France, Kevin Longo, Isabella Sandoval, Angeli Christian Schneider, P. Wilson, David J. Youngblood, Allison Vanderburg, Andrew Barber, Madyson G. Wood, Mackenna L. Batalha, Natasha E. Kraus, Adam L. Murray, Catriona Anne Newton, Elisabeth R. Rizzuto, Aaron Tofflemire, Benjamin M. Tsai, Shang-Min Bean, Jacob L. Berta-Thompson, Zachory K. Evans-Soma, Thomas M. Froning, Cynthia S. Kempton, Eliza M.-R. Miguel, Yamila Sebastian Pineda, J. Department of Physics and Astronomy The University of North Carolina at Chapel Hill Chapel HillNC27599 United States Laboratory for Atmospheric and Space Physics University of Colorado Boulder UCB 600 BoulderCO80309 United States Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Earth and Planets Laboratory Carnegie Institution for Science 5241 Broad Branch Road NW WashingtonDC20015 United States Department of Physics & Astronomy Johns Hopkins University BaltimoreMD United States School of Earth and Space Exploration Arizona State University TempeAZ85281 United States Center for Astrophysics and Space Astronomy University of Colorado 389 UCB BoulderCO80309 United States Department of Physics and Astronomy Vanderbilt University NashvilleTN37235 United States Department of Astrophysical and Planetary Sciences University of Colorado UCB 389 BoulderCO80309 United States Astrophysics Program The CUNY Graduate Center City University of New York New YorkNY10016 United States Exoplanets and Stellar Astrophysics Laboratory NASA Goddard Space Flight Center GreenbeltMD20771 United States Hamburger Sternwarte Gojenbergsweg 112 HamburgD-21029 Germany Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States MIT Kavli Institute for Astrophysics Space Research Massachusetts Institute of Technology CambridgeMA02139 United States NASA Ames Research Center Moffett FieldCA94035 United States Department of Astronomy The University of Texas at Austin AustinTX78712 United States Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO United States Department of Physics and Astronomy Dartmouth College HanoverNH03755 United States Mondo Level 26/2 Southbank Blvd SouthbankVIC3006 Australia Department of Earth and Planetary Sciences University of California RiversideCA United States

The characterization of young planets (⊕) planet, HIP 67522b, observed with JWST NIRSpec/G395H. To check for spot contamination, we obtain a simultaneous g-band transit with SOAR. The spectrum exhibits absorption features 30-50% deeper than the overall depth, far larger than expected from an equivalent mature planet, and suggests that HIP 67522 b's mass is ⊕ irrespective of cloud cover and stellar contamination. A Bayesian retrieval analysis returns a mass constraint of 13.8±1.0M⊕. This challenges the previous classification of HIP 67522b as a hot Jupiter and instead, positions it as a precursor to the more common sub-Neptunes. With a density of 3, HIP 67522 b is one of the lowest density planets known. We find strong absorption from H2O and CO2 (≥ 7σ), a modest detection of CO (3.5σ), and weak detections of H2S and SO2 ( 2σ). Comparisons with radiative-convective equilibrium models suggest supersolar atmospheric metallicities and solar-to-subsolar C/O ratios, with photochemistry further constraining the inferred atmospheric metallicity to 3×10 Solar due to the amplitude of the SO2 feature. These results point to the formation of HIP 67522b beyond the water snowline, where its envelope was polluted by icy pebbles and planetesimals. The planet is likely experiencing substantial mass loss (0.01-0.03 M⊕ Myr−1), sufficient for envelope destruction within a Gyr. This highlights the dramatic evolution occurring within the first 100 Myr of its existence. © 2024, CC BY.

关键词： Planets

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The SCUBA-2 Large eXtragalactic Survey: 850 μm map, catalogue and the bright-end number counts of the XMM-LSS field

arXiv

引用

arXiv 2023年

作者： Garratt, T.K. Geach, J.E. Tamura, Y. Coppin, K.E.K. Franco, M. Ao, Y. Chen, C.-C. Cheng, C. Clements, D.L. Dai, Y.S. Dannerbauer, H. Greve, T.R. Hatsukade, B. Hwang, H.S. Jiang, L. Kohno, K. Koprowski, M.P. Michalowski, M.J. Sawicki, M. Scott, D. Shim, H. Takeuchi, T.T. Wang, W.-H. Xue, Y.Q. Yang, C. Centre for Astrophysics Research University of Hertfordshire HatfieldAL10 9AB United Kingdom Division of Particle and Astrophysical Science Nagoya University Aichi Nagoya464-8602 Japan Purple Mountain Observatory Key Laboratory for Radio Astronomy Chinese Academy of Sciences 10 Yuanhua Road Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China Academia Sinica Institute of Astronomy and Astrophysics No. 1 Section 4 Roosevelt Road Taipei10617 Taiwan Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Imperial College London Blackett Lab Prince Consort Road LondonSW7 2AZ United Kingdom National Astronomical Observatories Chinese Academy of Sciences 20A Datun RoadChaoyang District Beijing100101 China Tenerife La LagunaE-38205 Spain Universidad de La Laguna Dpto. Astrofísica Tenerife La LagunaE-38206 Spain 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 Institute of Astronomy Graduate School of Science The University of Tokyo 2-21-1 Osawa Tokyo Mitaka181-0015 Japan 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 Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Kavli Institute for Astronomy and Astrophysics Peking University No. 5 Yiheyuan Road Haidian District Beijing100871 China 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 Poznań60-286 Poland Department of Astronomy and P

We present 850 μm imaging of the XMM-LSS field observed for 170 hours as part of the James Clerk Maxwell Telescope SCUBA-2 Large eXtragalactic Survey (S2LXS). S2LXS XMM-LSS maps an area of 9 deg2, reaching a moderate depth of 1σ 4 mJy beam−1. This is the largest contiguous area of extragalactic sky mapped by JCMT at 850 μm to date. The wide area of the S2LXS XMM-LSS survey allows us to probe the ultra-bright (S850μm & 15 mJy), yet rare submillimetre population. We present the S2LXS XMM-LSS catalogue, which comprises 40 sources detected at >5σ significance, with deboosted flux densities in the range of 7 mJy to 48 mJy. We robustly measure the bright-end of the 850 μm number counts at flux densities >7 mJy, reducing the Poisson errors compared to existing measurements. The S2LXS XMM-LSS observed number counts show the characteristic upturn at bright fluxes, expected to be motivated by local sources of submillimetre emission and high-redshift strongly lensed galaxies. We find that the observed 850 μm number counts are best reproduced by model predictions that include either strong lensing or source blending from a 15 arcsec beam, indicating that both may make an important contribution to the observed over-abundance of bright single dish 850 μm selected sources. We make the S2LXS XMM-LSS 850 μm map and >5σ catalogue presented here publicly available. Copyright © 2023, The Authors. All rights reserved.

关键词： Blending

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Simultaneous multicolour transit photometry of hot Jupiters HAT-P-19b, HAT-P-51b, HAT-P-55b, and HAT-P-65b

arXiv

引用

arXiv 2024年

作者： Kang, Huiyi Chen, Guo Pallé, Enric Murgas, Felipe García, Nestor Abreu de Leon, Jerome Enoc, Gareb Esparza-Borges, Emma Fukuda, Izuru Fukui, Akihiko Galán, Daniel Hayashi, Yuya Isogai, Keisuke Kagetani, Taiki Kawauchi, Kiyoe Korth, Judith Livingston, John H. Luque, Rafael Ma, Yuehua Madrigal-Aguado, Alberto Meni, Pedro Rodriguez, Pilar Montañes Mori, Mori Torres, Sara Muñoz Narita, Norio Orell-Miquel, Jaume Parviainen, Hannu Peláez-Torres, Alberto Stangret, Monika Tamura, Motohide Watanabe, Noriharu CAS Key Laboratory of planetary sciences Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China CAS Center for Excellence in Comparative Planetology Hefei230026 China Instituto de Astrofísica de Canarias Vía Láctea s/n Tenerife La Laguna38205 Spain Departamento de Astrofísica Universidad de La Laguna C/Padre Herrera Tenerife La Laguna38206 Spain Department of Multi-Disciplinary Sciences Graduate School of Arts and Sciences The University of Tokyo 3-8-1 Komaba Meguro Tokyo153-8902 Japan Komaba Institute for Science The University of Tokyo 3-8-1 Komaba Meguro Tokyo153-8902 Japan Okayama Observatory Kyoto University 3037-5 Honjo Kamogatacho Okayama Asakuchi719-0232 Japan Department of Physical Sciences Ritsumeikan University Shiga Kusatsu525-8577 Japan Lund Observatory Division of Astrophysics Department of Physics Lund University Box 43 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 Department of Astronomy & Astrophysics University of Chicago ChicagoIL60637 United States School of Architecture Universidad Europea de Canarias C/Inocencio Garcia 1 Tenerife La Orotava38300 Spain INAF - Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 Padova35122 Italy Department of Astronomy University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan

Accurate physical parameters of exoplanet systems are essential for further exploration of planetary internal structure, atmospheres, and formation history. We aim to use simultaneous multicolour transit photometry to improve the estimation of transit parameters, to search for transit timing variations (TTVs), and to establish which of our targets should be prioritised for follow-up transmission spectroscopy. We performed time series photometric observations of 12 transits for the hot Jupiters HAT-P-19b, HAT-P-51b, HAT-P-55b, and HAT-P-65b using the simultaneous four-colour camera MuSCAT2 on the Telescopio Carlos Sánchez. We collected 56 additional transit light curves from TESS photometry. To derive transit parameters, we modelled the MuSCAT2 light curves with Gaussian processes to account for correlated noise. To derive physical parameters, we performed EXOFASTv2 global fits to the available transit and radial velocity data sets, together with the Gaia DR3 parallax, isochrones, and spectral energy distributions. To assess the potential for atmospheric characterisation, we compared the multicolour transit depths with a flat line and a clear atmosphere model. We consistently refined the transit and physical parameters. We improved the orbital period and ephemeris estimates, and found no evidence for TTVs or orbital decay. The MuSCAT2 broadband transmission spectra of HAT-P-19b and HAT-P-65b are consistent with previously published low-resolution transmission spectra. We also found that, except for HAT-P-65b, the assumption of a planetary atmosphere can improve the fit to the MuSCAT2 data. In particular, we identified HAT-P-55b as a priority target among these four planets for further atmospheric studies using transmission spectroscopy. Copyright © 2024, The Authors. All rights reserved.

关键词： Photometry

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The Astrometric Animation of Water Masers towards the Mira Variable BX Cam

arXiv

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arXiv 2022年

作者： Xu, Shuangjing Imai, Hiroshi Yun, Youngjoo Zhang, Bo Rioja, María J. Dodson, Richard Cho, Se-Hyung Kim, Jaeheon Cui, Lang Sobolev, Andrey M. Chibueze, James O. Kim, Dong-Jin Amada, Kei Nakashima, Jun-Ichi Orosz, Gabor Oyadomari, Miyako Oh, Sejin Yonekura, Yoshinori Sun, Yan Mai, Xiaofeng Zhang, Jingdong Wen, Shiming Jung, Taehyun Korea Astronomy and Space Science Institute 776 Daedeok-daero Yuseong-gu Daejeon34055 Korea Republic of Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Graduate School of Science and Engineering Kagoshima University 1-21-35 Korimoto Kagoshima890-0065 Japan Amanogawa Galaxy Astronomy Research Center Graduate School of Science and Engineering Kagoshima University 1-21-35 Korimoto Kagoshima890-0065 Japan Center for General Education Institute for Comprehensive Education Kagoshima University 1-21-30 Korimoto Kagoshima890-0065 Japan ICRAR M468 The University of Western Australia 35 Stirling Hwy CrawleyWA6009 Australia CSIRO Astronomy and Space Science PO Box 1130 BentleyWA6102 Australia Alfonso XII 3 y 5 Madrid28014 Spain Astronomy program Department of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of Republic of Korea Korea Astronomy and Space Science Institute Yuseonggu Daejeon34055 Korea Republic of Xinjiang Astronomical Observatory Chinese Academy of Sciences 150 Science 1-Street Urumqi830011 China Ural Federal University 19 Mira Street Ekaterinburg620002 Russia Centre for Space Research North-West University Potchefstroom2520 South Africa Department of Physics and Astronomy Faculty of Physical Sciences University of Nigeria Carver Building 1 University Road Nsukka Nigeria Massachusetts Institute of Technology Haystack Observatory 99 Millstone Road WestfordMA01886 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany School of Physics and Astronomy Sun Yat-sen University 2 Daxue Road Tangjia Guangdong Province Zhuhai China Joint Institute for VLBI ERIC Oude Hoogeveensedijk 4 Dwingeloo7991PD Netherlands Center for Astronomy Ibaraki University 2-1-1 Bunkyo Ibaraki Mito310-8512 Japan Yuquan Rd. Shijingshan Beijing100049 China

We report VLBI monitoring observations of the 22 GHz water (H2O) masers around the Mira variable BX Cam, which were carried out as a part of the EAVN Synthesis of Stellar Maser Animations (ESTEMA) project. Data of 37 epochs in total were obtained from 2018 May to 2021 June with a time interval of 3–4 weeks, spanning approximately three stellar pulsation periods (P =∼440 d). In particular, the dual-beam system equipped on the VERA stations was used to measure the kinematics and parallaxes of the H2O maser features. The measured parallax, π = 1.79 ± 0.08 mas, is consistent with Gaia EDR3 and previously measured VLBI parallaxes within a 1-σ error level. The position of the central star was estimated, based on both the Gaia EDR3 data and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser distribution imaged with the KVN. The three-dimensional H2O maser kinematics indicates that the circumstellar envelope is expanding at a velocity of 13 ± 4 km s−1, while there are asymmetries in both the spatial and velocity distributions of the maser features. Furthermore, the H2O maser animation achieved by our dense monitoring program manifests the propagation of shock waves in the circumstellar envelope of BX Cam. © 2022, CC BY.

关键词： Stars

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Input optics systems of the KAGRA detector during O3GK (vol 2023, 023F01, 2023)

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PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS 2023年第5期2023卷

作者： Akutsu, T. Ando, M. Arai, K. Arai, Y. Araki, S. Araya, A. Aritomi, N. Asada, H. Aso, Y. Bae, S. Bae, Y. Baiotti, L. Bajpai, R. Barton, M. A. Cannon, K. Cao, Z. Capocasa, E. Chan, M. Chen, C. Chen, K. Chen, Y. Chiang, C-I Chu, H. Chu, Y-K Eguchi, S. Enomoto, Y. Flaminio, R. Fujii, Y. Fujikawa, Y. Fukunaga, M. Fukushima, M. Furuhata, T. Gao, D. Ge, G-G Ha, S. Hagiwara, A. Haino, S. Han, W-B Hasegawa, K. Hattori, K. Hayakawa, H. Hayama, K. Himemoto, Y. Hiranuma, Y. Hirata, N. Hirose, E. Hong, Z. Hsieh, B-H Huang, G-Z Huang, H-Y Huang, P. Huang, Y-C Huang, Y-J Hui, D. C. Y. Ide, S. Ikenoue, B. Imam, S. Inayoshi, K. Inoue, Y. Ioka, K. Ito, K. Itoh, Y. Izumi, K. Jeon, C. Jin, H-B Jung, K. Jung, P. Kaihotsu, K. Kajita, T. Kakizaki, M. Kamiizumi, M. Kanbara, S. Kanda, N. Kang, G. Kataoka, Y. Kawaguchi, K. Kawai, N. Kawasaki, T. Kim, C. Kim, J. Kim, J. C. Kim, Ws Kim, Y-M Kimura, N. Kita, N. Kitazawa, H. Kojima, Y. Kokeyama, K. Komori, K. Kong, A. K. H. Kotake, K. Kozakai, C. Kozu, R. Kumar, R. Kume, J. Kuo, C. Kuo, H-S Kuromiya, Y. Kuroyanagi, S. Kusayanagi, K. Kwak, K. Lee, H. K. Lee, H. W. Lee, R. Leonardi, M. Li, K. L. Lin, L. C-C Lin, C-Y Lin, F-K Lin, F-L Lin, H. L. Liu, G. C. Luo, L-W Majorana, E. Marchio, M. Michimura, Y. Mio, N. Miyakawa, O. Miyamoto, A. Miyazaki, Y. Miyo, K. Miyoki, S. Mori, Y. Morisaki, S. Moriwaki, Y. Nagano, K. Nagano, S. Nakamura, K. Nakano, H. Nakano, M. Nakashima, R. Nakayama, Y. Narikawa, T. Naticchioni, L. Negishi, R. Quynh, L. Nguyen Ni, W-T Nishizawa, A. Nozaki, S. Obuchi, Y. Ogaki, W. Oh, J. J. Oh, S. H. Ohashi, M. Ohishi, N. Ohkawa, M. Ohta, H. Okutani, Y. Okutomi, K. Oohara, K. Ooi, C. Oshino, S. Otabe, S. Pan, K-C Pang, H. Parisi, A. Park, J. Arellano, F. E. Pena Pinto, I. Sago, N. Saito, S. Saito, Y. Sakai, K. Sakai, Y. Sakuno, Y. Sato, S. Sato, T. Sawada, T. Sekiguchi, T. Sekiguchi, Y. Shao, L. Shibagaki, S. Shimizu, R. Shimoda, T. Shimode, K. Shinkai, H. Shishido, T. Shoda, A. Somiya, K. Son, E. J. Sotani, H. Sugimoto, R. Suresh, J. Suzuki, T. Suzuki, T. Tagoshi, H. Takahashi, H Gravitational Wave Science Project National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Department of Physics The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan Research Center for the Early Universe The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan Institute for Cosmic Ray Research KAGRA Observatory The University of Tokyo 5-1-5 Kashiwa-no-Ha Kashiwa City Chiba 277-8582 Japan Accelerator Laboratory High Energy Accelerator Research Organization (KEK) 1-1 Oho Tsukuba City Ibaraki 305-0801 Japan Earthquake Research Institute The University of Tokyo 1-1-1 Yayoi Bunkyo-ku Tokyo 113-0032 Japan Department of Mathematics and Physics Graduate School of Science and Technology Hirosaki University 3 Bunkyo-cho Hirosaki Aomori 036-8561 Japan Kamioka Branch National Astronomical Observatory of Japan 238 Higashi-Mozumi Kamioka-cho Hida City Gifu 506-1205 Japan The Graduate University for Advanced Studies (SOKENDAI) 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Korea Institute of Science and Technology Information 245 Daehak-ro Yuseong-gu Daejeon 34141 Republic of Korea National Institute for Mathematical Sciences 70 Yuseong-daero 1689 Beon-gil Yuseong-gu Daejeon 34047 Republic of Korea International College Osaka University 1-1 Machikaneyama-cho Toyonaka City Osaka 560-0043 Japan School of High Energy Accelerator Science The Graduate University for Advanced Studies (SOKENDAI) 1-1 Oho Tsukuba City Ibaraki 305-0801 Japan Department of Astronomy Beijing Normal University Xinjiekouwai Street 19 Haidian District Beijing 100875 China Department of Applied Physics Fukuoka University 8-19-1 Nanakuma Jonan Fukuoka City Fukuoka 814-0180 Japan Department of Physics Tamkang University No. 151 Yingzhuan Road Danshui Dist. New Taipei City 25137 Taiwan Department of Physics

KAGRA, the underground and cryogenic gravitational-wave detector, was operated for its solo observation from February 25 to March 10, 2020, and its first joint observation with the GEO 600 detector from April 7 to April 21, 2020 (O3GK). This study presents an overview of the input optics systems of the KAGRA detector, which consist of various optical systems, such as a laser source, its intensity and frequency stabilization systems, modulators, a Faraday isolator, mode-matching telescopes, and a high-power beam dump. These optics were successfully delivered to the KAGRA interferometer and operated stably during the observations. The laser frequency noise was observed to limit the detector sensitivity above a few kilohertz, whereas the laser intensity did not significantly limit the detector sensitivity.

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EMPRESS. X. Spatially resolved mass-metallicity relation in extremely metal-poor galaxies: Evidence of episodic star-formation fueled by a metal-poor gas infall

arXiv

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arXiv 2024年

作者： Nakajima, Kimihiko Ouchi, Masami Isobe, Yuki Xu, Yi Ozaki, Shinobu Nagao, Tohru Inoue, Akio K. Rauch, Michael Kusakabe, Haruka Onodera, Masato Nishigaki, Moka Ono, Yoshiaki Sugahara, Yuma Hattori, Takashi Hirai, Yutaka Hashimoto, Takuya Kim, Ji Hoon Moriya, Takashi J. Yanagisawa, Hiroto Aoyama, Shohei Fujimoto, Seiji Fukushima, Hajime Fukushima, Keita Harikane, Yuichi Hatano, Shun Hayashi, Kohei Ishigaki, Tsuyoshi Kawasaki, Masahiro Kojima, Takashi Komiyama, Yutaka Koyama, Shuhei Koyama, Yusei Lee, Chien-Hsiu Matsumoto, Akinori Mawatari, Ken Motohara, Kentaro Murai, Kai Nagamine, Kentaro Nakane, Minami Saito, Tomoki Sasaki, Rin Shibuya, Takatoshi Suzuki, Akihiro Takeuchi, Tsutomu T. Umeda, Hiroya Umemura, Masayuki Watanabe, Kuria Yabe, Kiyoto Yajima, Hidenobu Zhang, Yechi National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan Osawa 2-21-1 Mitaka Tokyo181-8588 Japan University of Tokyo Chiba Kashiwa277-8583 Japan Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Cavendish Laboratory University of Cambridge 19 JJ Thomson Avenue CambridgeCB3 0HE United Kingdom Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Department of Physics Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Research Center for Space and Cosmic Evolution Ehime University Bunkyo-cho 2-5 Ehime Matsuyama790-8577 Japan Department of Physics School of Advanced Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Observatoire de Genève Université de Genève 51 Chemin de Pégase Versoix1290 Switzerland 650 North Aohoku Place HiloHI96720 United States Department of Physics and Astronomy University of Notre Dame 225 Nieuwland Science Hall Notre DameIN46556 United States Astronomical Institute Tohoku University 6-3 Aoba Aramaki Aoba-ku Miyagi Sendai980-8578 Japan Division of Physics Faculty of Pure and Applied Sciences University of Tsukuba Ibaraki Tsukuba305-8571 Japan Faculty of Pure and Applied Sciences University of Tsukuba Ibaraki Tsukuba305-8571 Japan Astronomy Program Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Cent

Using the Subaru/FOCAS IFU capability, we examine the spatially resolved relationships between gas-phase metallicity, stellar mass, and star-formation rate surface densities (Σ★ and ΣSFR, respectively) in extremely metal-poor galaxies (EMPGs) in the local universe. Our analysis includes 24 EMPGs, comprising 9,177 spaxels, which span a unique parameter space of local metallicity (12 + log(O/H) 6.9 to 7.9) and stellar mass surface density (Σ★ ∼ 105 to 107 Mo kpc−2), extending beyond the range of existing large integral-field spectroscopic surveys. Through spatially resolved emission line diagnostics based on the [N ii] BPT-diagram, we verify the absence of evolved active galactic nuclei in these EMPGs. Our findings reveal that, while the resolved mass-metallicity relation exhibits significant scatter in the low-mass regime, this scatter is closely correlated with local star-formation surface density. Specifically, metallicity decreases as ΣSFR increases for a given Σ★. Notably, half of the EMPGs show a distinct metal-poor horizontal branch on the resolved mass-metallicity relation. This feature typically appears at the peak clump with the highest Σ★ and ΣSFR and is surrounded by a relatively metal-enriched ambient region. These findings support a scenario in which metal-poor gas infall fuels episodic star formation in EMPGs, consistent with the kinematic properties observed in these systems. In addition, we identify four EMPGs with exceptionally low central metallicities (12 + log(O/H) 7.2), which display only a metal-poor clump without a surrounding metal-rich region. This suggests that such ultra-low metallicity EMPGs, at less than a few percent of the solar metallicity, may serve as valuable analogs for galaxies in the early stages of galaxy evolution. Copyright © 2024, The Authors. All rights reserved.

关键词： Spectroscopic analysis

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Development of an advanced SiPM camera for the Large Size Telescope of the Cherenkov Telescope Array Observatory 37

Development of an advanced SiPM camera for the Large Size Te...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Bellato, M. Bergnoli, A. Bernasconi, E. Biland, A. Charbon, E. Corti, D. Gascón, D. Gómez, S. Ziȩtara, K. 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. AQUA EPFL Neuchâtel Switzerland ETH Zurich Institute for Particle Physics Otto-Stern-Weg 5 Zurich8093 Switzerland Astronomical Observatory Jagiellonian University ul. Orla 171 Kraków30-244 Poland Institute for Cosmic Ray Research University of Tokyo Japan Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Martí i Franquès 1 Barcelona08028 Spain Instituto de Astrofísica de Andalucía CSIC Spain INAF Osservatorio Astronomico di Roma Italy INFN Sezione di Napoli Italy Aix Marseille Univ CNRS IN2P3 CPPM Marseille France Barcelona Institute of Science and Technology Spain 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 EMFTEL department IPARCOS Universidad Complutense de Madrid Spain INAF Osservatorio di Astrofisica e Scienza dello spazio di Bologna Centro Brasileiro de Pesquisas Físicas Brazil INFN Sezione di Padova 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 Germany Department of Physics TU Dortmund University Germany Saha Institute of Nuclear Physics India INFN Sezione di Trieste Università degli Studi di Udine Italy INFN Sezione di Catania Italy University of Geneva Département de Physique Nucléaire et Corpusculaire 24 Quai Ernest Ansermet GenèveCH-1211 Switzerland Palacky University Olomouc Faculty of Science Czech Republic CIEMAT Port d’Informació Científica INFN Sezione di Torino via P. Giuria 1 Torino10125 Italy Dipartimento di Fisica Universitá degli Studi di Torino via P. Giuria 1 Torino10125 Italy INFN Sezione di Bari Università di Bari University of Rijeka Department of Physics Institute for Theoretical Physics and Astrophysics Universitä

Silicon photomultipliers (SiPMs) have become the baseline choice for cameras of the small-sized telescopes (SSTs) of the Cherenkov Telescope Array (CTA). On the other hand, SiPMs are relatively new to the field and covering large surfaces and operating at high data rates still are challenges to outperform photomultipliers (PMTs). The higher sensitivity in the near infra-red and longer signals compared to PMTs result in higher night sky background rate for SiPMs. However, the robustness of the SiPMs represents a unique opportunity to ensure long-term operation with low maintenance and better duty cycle than PMTs. The proposed camera for large size telescopes will feature 0.05◦ pixels, low power and fast front-end electronics and a fully digital readout. In this work, we present the status of dedicated simulations and data analysis for the performance estimation. The design features and the different strategies identified, so far, to tackle the demanding requirements and the improved performance are described. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Photomultipliers

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Monitoring the pointing of the prototype LST-1 using star reconstruction in the Cherenkov camera 37

Monitoring the pointing of the prototype LST-1 using star re...

引用

37th International Cosmic Ray Conference, ICRC 2021

作者： Foffano, L. Carosi, A. Dalchenko, M. Heller, M. Della Volpe, D. Montaruli, T. 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. Cassol, F. Cerruti, M. Chai, Y. Cheng, K. Chikawa, M. Chytka, L. Contreras, J.L. Cortina, J. Costantini, H. De Angelis, A. de Bony de Lavergne, M. Deleglise, G. Delgado, C. Delgado Mengual, J. 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. 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. 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. Monteiro, I. Moralejo, A. Morcuende, D. Moretti, E. Morselli, A. Mrakovcic, K. Murase, K. Nagai, A. Nakamori, T. Nickel, L. University of Geneva Département de Physique Nucléaire et Corpusculaire quai Ernest Ansermet 24 Geneva Switzerland Institute for Cosmic Ray Research University of Tokyo 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 INAF - Osservatorio Astronomico di Roma Italy INFN Sezione di Napoli Italy Aix Marseille Univ CNRS IN2P3 CPPM France The Barcelona Institute of Science and Technology Spain 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 EMFTEL Department IPARCOS Universidad Complutense de Madrid Spain INAF - Osservatorio di Astrofisica e Scienza dello spazio di Bologna Italy Centro Brasileiro de Pesquisas Físicas Brazil INFN Sezione di Padova Università degli Studi di Padova Italy Instituto de Astrofísica de Canarias Departamento de Astrofísica Universidad de La Laguna Spain Max-Planck-Institut für Physik Germany Department of Physics TU Dortmund University Germany Saha Institute of Nuclear Physics India INFN Sezione di Trieste Università degli Studi di Udine Italy INFN Sezione di Catania Italy Italy Palacky University Olomouc Faculty of Science Czech Republic CIEMAT Spain Port d'Informació Científica Spain INFN Sezione di Torino 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 Bari Italy Faculty of Physics and Applied Informatics University of Lodz Poland University of Split FESB Croatia Department of Physics Yamagata Univ

The first Large-Sized Telescope (LST-1) proposed for the forthcoming Cherenkov Telescope Array (CTA) has started to operate in 2019 in La Palma. The large structure of LST-1 - with a 23 m mirror dish diameter - imposes a strict control of its deformations that could affect the pointing accuracy and its overall performance. According to CTA specifications that are conceived to resolve e.g. the fine structure of galactic sources, the LST post-calibration pointing accuracy should be better than 14 arcseconds. To fulfill this requirement, the telescope pointing precision is monitored with two dedicated CCD cameras located at the dish center. The analysis of their images allows us to disentangle different systematic deformations of the structure. In this work, we investigate a complementary approach that offers the possibility to monitor the pointing of the telescope during the acquisition of sky data. After properly cleaning the events from the Cherenkov showers, the reconstructed positions of the stars imaged in the camera field of view are compared to their nominal expected positions in catalogues. This provides a direct measurement of the telescope pointing, that can be used to cross-check the other methods and as a real-time monitoring of the optical properties of the telescope and of the pointing corrections applied by the bending models. Additionally, this method benefits from not relying on specific hardware or dedicated observations. In this contribution we will illustrate this analysis and show results based on simulations of LST-1. © 2022 Sissa Medialab Srl. All rights reserved.

关键词： Stars

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