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Transactions on Electrical and Electronic Materials 2023年第1期25卷 120-120页

作者： Khan, Faiza Mubashir, Talha Ahmed, Kainat Mateen, Abdul Lee, Soonil Ahmed, Tauseef Department of Nanoscience and Technology Preston Institute of Nanoscience and Technology PINSAT Islamabad Pakistan Department of Applied Ecology and Biotechnology Inland Norway University of Applied Sciences Hamar Norway Interdisciplinary Program in Senior Human Ecology Changwon National University Gyeongnam Republic of Korea Department of Mineral Processing Engineering Pak-Austria Fachhochschule Institute of Applied Sciences & Technology Haripur Pakistan School of Materials Science and Engineering Changwon National University Gyeongnam Republic of Korea Department of Materials Science & Engineering Institute of Space Technology Islamabad Pakistan

Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b

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Astronomical Journal 2023年第6期166卷 223页

作者： A-Thano, Napaporn Awiphan, Supachai Jiang, Ing-Guey Kerins, Eamonn Priyadarshi, Akshay McDonald, Iain Joshi, Yogesh C. Chulikorn, Thansuda Hayes, Joshua J. C. Charles, Stephen Huang, Chung-Kai Rattanamala, Ronnakrit Yeh, Li-Chin Dhillon, Vik S Department of Physics Institute of Astronomy National Tsing-Hua University Hsinchu 30013 Taiwan National Astronomical Research Institute of Thail 260 Moo 4 Donkaew Mae Rim Chiang Mai 50180 Thailand Jodrell Bank Centre for Astrophysics University of Manchester Oxford Road Manchester M13 9PL United Kingdom Department of Physical Sciences The Open University Walton Hall Milton Keynes MK7 6AA United Kingdom Aryabhatta Research Institute of Observational Sciences (ARIES) Manora Peak Nainital 263001 India Department of Physics Faculty of Science Chulalongkorn University 254 Phayathai Road Pathumwan Bangkok 10330 Thailand Institute of Astronomy and Astrophysics Academia Sinica No.1 Sec. 4 Roosevelt Road Taipei 10617 Taiwan PhD Program in Astronomy Department of Physics and Materials Science Faculty of Science Chiang Mai University Chiang Mai 50200 Thailand Department of Physics and General Science Faculty of Science and Technology Nakhon Ratchasima Rajabhat University Nakhon Ratchasima 30000 Thailand Institute of Computational and Modeling Science National Tsing-Hua University Hsinchu 30013 Taiwan Department of Physics and Astronomy University of Sheffield Sheffield S3 7RH United Kingdom Instituto de Astrofísica de Canarias La Laguna Tenerife E-38205 Spain

We present a transit-timing variation (TTV) and planetary atmosphere analysis of the Neptune-mass planet HAT-P-26 b. We present a new set of 13 transit light curves from optical ground-based observations and combine them with light curves from the Wide Field Camera 3 on the Hubble space Telescope, the Transiting Exoplanet Survey Satellite, and previously published ground-based data. We refine the planetary parameters of HAT-P-26 b and undertake a TTV analysis using 33 transits obtained over seven years. The TTV analysis shows an amplitude signal of 1.98 ± 0.05 minutes, which could result from the presence of an additional ∼0.02 M _Jup planet at a 1:2 mean-motion resonance orbit. Using a combination of transit depths spanning optical to near-infrared wavelengths, we find that the atmosphere of HAT-P-26 b contains 2.4 − 1.6 + 2.9 % H₂O with a derived temperature of 590 − 50 + 60 K. © 2023. The Author(s). Published by the American Astronomical Society.

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Calibrating mg II-based black-hole mass estimators using low-to-high-luminosity active galactic nuclei

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arXiv 2020年

作者： Le, Huynh Anh N. Woo, Jong-Hak Xue, Yongquan Astronomy Program Department of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China

We present single-epoch black-hole mass (MBH) estimators based on the rest-frame ultraviolet (UV) Mg II 2798Å and optical Hβ 4861Å emission lines. To enlarge the luminosity range of active galactic nuclei (AGNs), we combine the 31 reverberation-mapped AGNs with relatively low luminosities from Bahk et al. (2019), 47 moderate-luminosity AGNs from Woo et al. (2018), and 425 high-luminosity AGNs from the Sloan Digital Sky Survey (SDSS). The combined sample has the monochromatic luminosity at 5100Å ranging logλL5100 ∼ 41.3−46.5 erg s−1, over the range of 5.5 BH BH estimators. By exploring the systematic discrepancy between the UV and optical MBH estimators as a function of AGN properties, we suggest to add correction term ∆M = -1.14 log(FWHMMgII/σMgII) + 0.33 in the UV mass estimator equation. We also find a ∼0.1 dex bias in the MBH estimation due to the difference of the spectral slope in the 2800-5200 Å range. Depending on the selection of MBH estimator based on either line dispersion or FWHM and either continuum or line luminosity, the derived UV mass estimators show >∼0.1 dex intrinsic scatter with respect to the fiducial Hβ based MBH Copyright © 2020, The Authors. All rights reserved.

关键词： Luminance

The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). X. Hot Gas Reveals Deeply Embedded Star Formation

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Astrophysical Journal 2024年第2期963卷 163-163页

作者： Izumi, Natsuko Sanhueza, Patricio Koch, Patrick M. Lu, Xing Li, Shanghuo Sabatini, Giovanni Olguin, Fernando A. Zhang, Qizhou Nakamura, Fumitaka Tatematsu, Ken’ichi Morii, Kaho Sakai, Takeshi Tafoya, Daniel Institute of Astronomy and Astrophysics Academia Sinica No. 1 Section 2 Roosevelt Road Taipei 10617 Taiwan National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai 200030 China Max Planck Institute for Astronomy Konigstuhl 17 Heidelberg D-69117 Germany INAF Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze I-50125 Italy Institute of Astronomy National Tsing Hua University Hsinchu 30013 Taiwan Center for Astrophysics Harvard & Smithsonian 60 Garden Street Cambridge 02138 MA United States Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan Graduate School of Informatics and Engineering The University of Electro-Communications Chofu Tokyo 182-8585 Japan Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala SE-439 92 Sweden

Massive infrared dark clouds (IRDCs) are considered to host the earliest stages of high-mass star formation. In particular, 70 μm dark IRDCs are the colder and more quiescent clouds. At a scale of about 5000 au using formaldehyde (H₂CO) emission, we investigate the kinetic temperature of dense cores in 12 IRDCs obtained from the pilot Atacama Large Millimeter/submillimeter Array Survey of 70 μm dark High-mass clumps in Early Stages (ASHES). Compared to the 1.3 mm dust continuum and other molecular lines, such as C¹⁸O and deuterated species, we find that H₂CO is mainly sensitive to low-velocity outflow components rather than to quiescent gas expected in the early phases of star formation. The kinetic temperatures of these components range from 26 to 300 K. The Mach number reaches about 15 with an average value of about 4, suggesting that the velocity distribution of gas traced by H₂CO is significantly influenced by a supersonic nonthermal component. In addition, we detect warm line emission from HC₃N and OCS in 14 protostellar cores, which requires high excitation temperatures (E _u/k ∼ 100 K). These results show that some of the embedded cores in the ASHES fields are in an advanced evolutionary stage, previously unexpected for 70 μm dark IRDCs. © 2024. The Author(s). Published by the American Astronomical Society.

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Unprecedented anti-inflammatory biscembranoids with 3-hydroperoxy-3-methylcyclohex-1-ene moiety isolated from aquaculture Sarcophyton trocheliophorum

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Aquaculture Reports 2023年 33卷

作者： Peng, Bo-Rong Nguyen, Ngoc Bao An Chen, Lo-Yun El-Shazly, Mohamed Hwang, Tsong-Long Su, Jui-Hsin Lai, Kuei-Hung Graduate Institute of Pharmacognosy College of Pharmacy Taipei Medical University Taipei 11031 Taiwan PhD Program in Clinical Drug Development of Herbal Medicine College of Pharmacy Taipei Medical University Taipei 11031 Taiwan Department of Pharmacognosy Faculty of Pharmacy Ain-Shams University Organization of African Unity Street Cairo Abassia 11566 Egypt Research Center for Chinese Herbal Medicine College of Human Ecology Chang Gung University of Science and Technology Taoyuan 33303 Taiwan Graduate Institute of Health Industry Technology College of Human Ecology Chang Gung University of Science and Technology Taoyuan 33303 Taiwan Department of Anaesthesiology Chang Gung Memorial Hospital Taoyuan 33305 Taiwan Graduate Institute of Natural Products College of Medicine Chang Gung University Taoyuan 33302 Taiwan Department of Chemical Engineering Ming Chi University of Technology New Taipei City 24301 Taiwan National Museum of Marine Biology & Aquarium Pingtung 94450 Taiwan Department of Marine Biotechnology and Resources National Sun Yat-sen University Kaohsiung 80424 Taiwan Traditional Herbal Medicine Research Center Taipei Medical University Hospital Taipei 11031 Taiwan

Recent advancements in the discovery of natural products have made significant progress in rapidly identifying known compounds from complex extracts using advanced spectroscopic technologies. Among these methods, one powerful approach called MS/MS molecular networking (MN) organizes chemical similarity based on MS/MS fragmentation data, serving as a valuable complement to traditional dereplication strategies. In our ongoing research focused on lead discovery from a sustainable medicinal source, an aquaculture soft coral Sarcophyton trocheliophorum, the MN profiling approach revealed the chemical diversity of biscembranoid analogs. By analyzing the MN pattern, biscembranoid derivatives with unique MS/MS fragments were prioritized for further investigation. Two novel biscembranoids, sarcotroxide A (1) and B (2), were successfully obtained through targeted isolation. These novel biscembranes contained an unprecedented 3-hydroperoxy-3-methylcyclohex-1-ene moiety compared with all biscembranoid analogs. The chemical structures of the two new biscembranoids were confirmed through spectroscopic analyses and in silico calculations. Their anti-inflammatory properties were assessed against the generation of superoxide anion (O₂^•−) and elastase release in activated human neutrophils. Sarcotroxides A (1) and B (2) exhibited anti-inflammatory activity by inhibiting O₂^•− accumulation (with 43.67% and 61.62% inhibition) and elastase release (with 38.21% and 61.62% inhibition) at 10 µM. These findings validated the potential of these biscembranoids from the cultured S. trocheliophorum as promising candidates for the future development of anti-inflammatory agents specifically designed to target neutrophils. © 2023 The Authors

关键词： Anti-inflammation Aquaculture soft coral Biscembranoid Neutrophil Sarcophyton trocheliophorum

The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). XI. Statistical Study of Early Fragmentation

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Astrophysical Journal 2024年第2期966卷 171-171页

作者： Morii, Kaho Sanhueza, Patricio Zhang, Qizhou Nakamura, Fumitaka Li, Shanghuo Sabatini, Giovanni Olguin, Fernando A. Beuther, Henrik Tafoya, Daniel Izumi, Natsuko Tatematsu, Ken’ichi Sakai, Takeshi Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Center for Astrophysics Harvard & Smithsonian 60 Garden Street Cambridge 02138 MA United States Max Planck Institute for Astronomy Königstuhl 17 Heidelberg D-69117 Germany INAF-Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze I-50125 Italy Institute of Astronomy National Tsing Hua University Hsinchu 30013 Taiwan Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala 439 92 Sweden Academia Sinica Institute of Astronomy and Astrophysics 11F of AS/NTU Astronomy-Mathematics Building No.1 Section 4 Roosevelt Road Taipei 10617 Taiwan Graduate School of Informatics and Engineering The University of Electro-Communications Chofu Tokyo 182-8585 Japan

Fragmentation during the early stages of high-mass star formation is crucial for understanding the formation of high-mass clusters. We investigated fragmentation within 39 high-mass star-forming clumps as part of the Atacama Large Millimeter/submillimeter Array Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES) survey. Considering projection effects, we have estimated core separations for 839 cores identified from the continuum emission and found mean values between 0.08 and 0.32 pc within each clump. We find compatibility of the observed core separations and masses with the thermal Jeans length and mass, respectively. We also present subclump structures revealed by the 7 m array continuum emission. Comparison of the Jeans parameters using clump and subclump densities with the separation and masses of gravitationally bound cores suggests that they can be explained by clump fragmentation, implying the simultaneous formation of subclumps and cores within rather than a step-by-step hierarchical fragmentation. The number of cores in each clump positively correlates with the clump surface density and the number expected from the thermal Jeans fragmentation. We also find that the higher the fraction of protostellar cores, the larger the dynamic range of the core mass, implying that the cores are growing in mass as the clump evolves. The ASHES sample exhibits various fragmentation patterns: aligned, scattered, clustered, and subclustered. Using the Q -parameter, which can help distinguish between centrally condensed and subclustered spatial core distributions, we finally find that in the early evolutionary stages of high-mass star formation, cores tend to follow a subclustered distribution. © 2024. The Author(s). Published by the American Astronomical Society.

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The ALCHEMI atlas: principal component analysis reveals starburst evolution in NGC 253

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arXiv 2024年

作者： Harada, Nanase Meier, David S. Martín, Sergio Muller, Sebastien Sakamoto, Kazushi Saito, Toshiki Gorski, Mark D. Henkel, Christian Tanaka, Kunihiko Mangum, Jeffrey G. Aalto, Susanne Aladro, Rebeca Bouvier, Mathilde Colzi, Laura Emig, Kimberly L. Herrero-Illana, Rubén Huang, Ko-Yun Kohno, Kotaro König, Sabine Nakanishi, Kouichiro Nishimura, Yuri Takano, Shuro Rivilla, Víctor M. Viti, Serena Watanabe, Yoshimasa van der Werf, Paul P. Yoshimura, Yuki National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Institute of Astronomy and Astrophysics Academia Sinica 11F of AS/NTU Astronomy-Mathematics Building No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-1855 Japan New Mexico Institute of Mining and Technology 801 Leroy Place SocorroNM87801 United States National Radio Astronomy Observatory PO Box O 1003 Lopezville Road SocorroNM87801 United States European Southern Observatory Alonso de Córdova 3107 Vitacura Santiago763-0355 Chile Joint ALMA Observatory Alonso de Córdova 3107 Vitacura Santiago763-0355 Chile Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory OnsalaSE-439 92 Sweden Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany Astronomy Department Faculty of Science King Abdulaziz University P. O. Box 80203 Jeddah21589 Saudi Arabia Department of Physics Faculty of Science and Technology Keio University 3-14-1 Hiyoshi Kanagawa Yokohama223-8522 Japan National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903-2475 United States Department of Space Earth and Environment Chalmers University of Technology GöteborgSE-412 96 Sweden Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands CSIC-INTA Ctra. de Ajalvir Km. 4 Torrejón de Ardoz Madrid28850 Spain Campus UAB Carrer de Magrans BarcelonaE-08193 Spain Institute of Astronomy Graduate School of Science The University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan Department of Astronomy The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan ALMA Project National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Physic

Molecular lines are powerful diagnostics of the physical and chemical properties of the interstellar medium (ISM). These ISM properties, which affect future star formation, are expected to differ in starburst galaxies from those of more quiescent galaxies. We investigate the ISM properties in the central molecular zone of the nearby starburst galaxy NGC 253 using the ultra-wide millimeter spectral scan survey from the ALMA Large program ALCHEMI. We present an atlas of velocity-integrated images at a 1′′. 6 resolution of 148 unblended transitions from 44 species, including the first extragalactic detection of HCNH+ and the first interferometric images of C3H+, NO, HCS+. We conduct a principal component analysis (PCA) on these images to extract correlated chemical species and to identify key groups of diagnostic transitions. To the best of our knowledge, our dataset is currently the largest astronomical set of molecular lines to which PCA has been applied. The PCA can categorize transitions coming from different physical components in NGC 253 such as i) young starburst tracers characterized by high-excitation transitions of HC3N and complex organic molecules (COMs) versus tracers of on-going star formation (radio recombination lines) and high-excitation transitions of CCH and CN tracing PDRs, ii) tracers of cloud-collision-induced shocks (low-excitation transitions of CH3OH, HNCO, HOCO+, and OCS) versus shocks from star-formation-induced outflows (high-excitation transitions of SiO), as well as iii) outflows showing emission from HOC+, CCH, H3O+, CO isotopologues, HCN, HCO+, CS, and CN. Our findings show these intensities vary with galactic dynamics, star formation activities, and stellar feedback. © 2024, CC BY.

关键词： Principal component analysis

The ALMA Survey of 70 µm Dark High-mass Clumps in Early Stages (ASHES). X: Hot Gas Reveals Deeply Embedded Star Formation

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arXiv 2023年

作者： Izumi, Natsuko Sanhueza, Patricio Koch, Patrick M. Lu, Xing Li, Shanghuo Sabatini, Giovanni Olguin, Fernando A. Zhang, Qizhou Nakamura, Fumitaka Tatematsu, Ken'ichi Morii, Kaho Sakai, Takeshi Tafoya, Daniel Institute of Astronomy and Astrophysics Academia Sinica No. 1 Section 4 Roosevelt Road Taipei10617 Taiwan 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 Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Max Planck Institute for Astronomy Konigstuhl 17 HeidelbergD-69117 Germany INAF Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 FirenzeI-50125 Italy Institute of Astronomy National Tsing Hua University Hsinchu30013 Taiwan Center for Astrophysics |Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Astronomy Graduate School of Science The University of Tokyo Bunkyo-ku Tokyo113-0033 Japan Graduate School of Informatics and Engineering The University of Electro-Communications Chofu Tokyo182-8585 Japan Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory OnsalaSE-439 92 Sweden

Massive infrared dark clouds (IRDCs) are considered to host the earliest stages of high-mass star formation. In particular, 70 µm dark IRDCs are the colder and more quiescent clouds. At a scale of about 5000 au using formaldehyde (H2CO) emission, we investigate the kinetic temperature of dense cores in 12 IRDCs obtained from the pilot ALMA Survey of 70 µm dark High-mass clumps in Early Stages (ASHES). Compared to 1.3 mm dust continuum and other molecular lines, such as C18O and deuterated species, we find that H2CO is mainly sensitive to low-velocity outflow components rather than to quiescent gas expected in the early phases of star formation. The kinetic temperatures of these components range from 26 to 300 K. The Mach number reaches about 15 with an average value of about 4, suggesting that the velocity distribution of gas traced by H2CO is significantly influenced by a supersonic non-thermal component. In addition, we detect warm line emission from HC3N and OCS in 14 protostellar cores, which requires high excitation temperatures (Eu/k ∼ 100 K). These results show that some of the embedded cores in the ASHES fields are in an advanced evolutionary stage, previously unexpected for 70 µm dark IRDCs. Copyright © 2023, The Authors. All rights reserved.

关键词： Giant stars

Toward next generation solar coronagraph: Diagnostic coronagraph experiment

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arXiv 2020年

作者： Cho, K.-S. Yang, H. Lee, J.-O. Bong, S.-C. Kim, J. Choi, S. Park, J.-Y. Cho, K.-H. Baek, J.-H. Kim, Y.-H. Park, Y.-D. Korea Astronomy and Space Science Institute Daejeon305-348 Korea Republic of University of Science and Technology Daejeon305-330 Korea Republic of Astronomy Program Department of Physics and Astronomy Seoul National University Seoul151-747 Korea Republic of

Korea Astronomy and space science Institute (KASI) has been developing a next-generation coronagraph (NGC) in cooperation with NASA to measure the coronal electron density, temperature, and speed simultaneously using four different filters around 400 nm. KASI organized an expedition team to demonstrate the coronagraph measurement scheme and the instrumental technology through the 2017 total solar eclipse (TSE) across the USA. The observation site was in Jackson Hole, Wyoming, USA. We built an eclipse observation system, so-called Diagnostic Coronal Experiment (DICE), which is composed of two identical telescopes to improve a signal to noise ratio. The observation was conducted with 4 wavelengths and 3 linear polarization directions according to the planned schedule in a limited total eclipse time of about 140 seconds. Polarization information of corona from the data was successfully obtained but we were not able to obtain global information of coronal electron temperature and speed in the corona due to a low signal-to-noise ratio of the optical system and a strong emission from the prominence located in the western limb. In this study, we report the development of DICE and observation results from the eclipse expedition. TSE observation and analysis by using our own developed instrument gave an important lesson that a coronagraph should be carefully designed to achieve the scientific purpose of this study. And it was a very useful experience in the way for the success of follow-up NASA-KASI joint missions called the Balloon-borne Investigation of the Temperature and Speed of Electrons in the Corona (BITSE) and COronal Diagnostic EXperiment (CODEX). Copyright © 2020, The Authors. All rights reserved.

关键词： NASA

Simulations of torus reverberation mapping experiments with spherex

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arXiv 2021年

作者： Kim, Minjin Jeong, Woong-Seob Yang, Yujin Son, Jiwon Ho, Luis C. Woo, Jong-Hak Im, Myungshin Byun, Woowon Department of Astronomy and Atmospheric Sciences College of Natural Sciences Kyungpook National University Daegu41566 Korea Republic of Korea Astronomy and Space Science Institute Daejeon34055 Korea Republic of University of Science and Technology Daejeon34113 Korea Republic of Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Astronomy Program Department of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of SNU Astronomy Research Center Seoul National University Seoul08826 Korea Republic of

Reverberation mapping (RM) is an efficient method to investigate the physical sizes of the broad line region (BLR) and dusty torus in an active galactic nucleus (AGN). The Spectro-Photometer for the History of the Universe, Epoch of Reionization and Ices Explorer (SPHEREx) mission will provide multi-epoch spectroscopic data at optical and near-infrared wavelengths. These data can be used for RM experiments for bright AGNs. We present results of a feasibility test using SPHEREx data in the SPHEREx deep regions for the torus RM measurements. We investigate the physical properties of bright AGNs in the SPHEREx deep field. Based on this information, we compute the efficiency of detecting torus time lags in simulated light curves. We demonstrate that, in combination with the complementary optical data with a depth of ∼ 20 mag in B-band, lags of ≤ 750 days for tori can be measured for more than ∼ 200 bright AGNs. If high signal-to-noise ratio photometric data with a depth of ∼ 21-22 mag are available, RM measurements can be applied for up to ∼900 objects. When complemented by well-designed early optical observations, SPHEREx can provide a unique dataset for studies of the physical properties of dusty tori in bright AGNs. © 2021, CC BY-SA.

关键词： Galaxies