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Short vertical-wavelength gravity wave activities in the upper troposphere lower stratosphere observed with global navigation satellite system radio occultation under different QBO phases

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IOP Conference Series: Earth and Environmental science 2021年第1期893卷

作者： Firas Rasyad Tri Wahyu Hadi Noersomadi Earth Science Program Institut Teknologi Bandung Indonesia Atmospheric Science Research Group Faculty of Earth Science and Technology Institut Teknologi Bandung Indonesia Center of Atmospheric Science and Technology National Institute of Aeronautics and Space (LAPAN) Bandung Indonesia

Gravity Waves (GWs) are believed to play important role in the generation of the driving force of the stratospheric Quasi-Biennial Oscillation (QBO). Deep convection in the equatorial region can generate large amount of GW with short vertical wavelength (λz <1 km) but studies of these wave activities in the upper troposphere lower stratosphere (UTLS) region are still limited. Recent advances in Global Navigation Satellite System (GNSS) Radio Occultation (RO) retrieval techniques have made it possible to derive global temperature profile with vertical resolution of less than 1 km. In this research, activities of GW with λz from 0.5 to 3.5 km in the UTLS region of 20-27 km heights are identified by calculating the GW potential energy (Ep). Correlation between GW activities and QBO phases is examined using 50 hPa zonal wind as the QBO index. The results show that during both easterly and westerly QBO phases, the GW Ep value increases gradually with time and reaches its peak in the transition periods. This pattern is seen in Ep with all vertical wavelengths between 0.5-3.5 km but the percentage value of Ep for λz<1 km is higher during the transition from westerly to easterly QBO. The GW Ep values exhibit downward propagation with the QBO phase but there are also discernible upward propagations of GW activities below 24 km height and intersect those two bring large changes in QBO phases. Additionally, higher percentage of Ep with λz<1 km is also found to be associated with El Niño events.

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Elemental Characterization of Ambient Particulate Matter for a Globally Distributed Monitoring Network: Methodology and Implications

ACS ES&T air

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ACS ES&T air 2024年第4期1卷 283-293页

作者： Xuan Liu Jay R Turner Christopher R Oxford Jacob McNeill Brenna Walsh Emmie Le Roy Crystal L Weagle Emily Stone Haihui Zhu Wenyu Liu Zilin Wei Nicole P Hyslop Jason Giacomo Ann M Dillner Abdus Salam Al-Amin Hossen Zubayer Islam Ihab Abboud Clement Akoshile Omar Amador-Muñoz Nguyen Xuan Anh Araya Asfaw Rajasekhar Balasubramanian Rachel Ying-Wen Chang Craig Coburn Sagnik Dey David J Diner Jinlu Dong Tareq Farrah Paterne Gahungu Rebecca M Garland Michel Grutter de la Mora Sina Hasheminassab Juanette John Jhoon Kim Jong Sung Kim Kristy Langerman Pei-Chen Lee Puji Lestari Yang Liu Tesfaye Mamo Mathieu Martins Olga L Mayol-Bracero Mogesh Naidoo Sang Seo Park Yoav Schechner Robyn Schofield Sachchida N Tripathi Eli Windwer Ming-Tsang Wu Qiang Zhang Michael Brauer Yinon Rudich Randall V Martin Department of Energy Environmental & Chemical Engineering Washington University in St. Louis St. Louis Missouri 63130 United States. Air Quality Research Center University of California Davis Davis California 95616 United States. Department of Chemistry University of Dhaka Dhaka 1000 Bangladesh. Air Quality Research Division Environment and Climate Change Canada Toronto Ontario M3H 5T4 Canada. Department of Physics University of Ilorin Ilorin 240003 Nigeria. Instituto de Ciencias de la Atmósfera y Cambio Climático Universidad Nacional Autónoma de México Mexico City 04510 Mexico. Institute of Geophysics Vietnam Academy of Science and Technology Hanoi 11307 Vietnam. Institute of Geophysics and Space Science Addis Ababa University Addis Ababa 1176 Ethiopia. Department of Civil and Environmental Engineering National University of Singapore Singapore 117576 Singapore. Department of Physics and Atmospheric Science Dalhousie University Halifax Nova Scotia B3H 4R2 Canada. Department of Geography and Environment University of Lethbridge Lethbridge Alberta T1K 3M4 Canada. Centre for Atmospheric Sciences Indian Institute of Technology Delhi New Delhi 110016 India. Jet Propulsion Laboratory California Institute of Technology Pasadena California 91109 United States. School of Environment Tsinghua University Beijing 100084 People's Republic of China. Research Laboratories Khalifa University Abu Dhabi 127788 United Arab Emirates. Institute of Applied Statistics University of Burundi Bujumbura BP1550 Burundi. Council for Scientific and Industrial Research Pretoria 0001 South Africa. Unit for Environmental Sciences and Management North-West University Potchefstroom 2531 South Africa. Department of Geography Geo-Informatics and Meteorology University of Pretoria Pretoria 0002 South Africa. Department of Atmospheric Sciences Yonsei University Seoul 03722 Republic of Korea. Department of Community Health and Epidemiology Dalhousie University Halifax Nova Scotia B3

Global ground-level measurements of elements in ambient particulate matter (PM) can provide valuable information to understand the distribution of dust and trace elements, assess health impacts, and investigate emission sources. We use X-ray fluorescence spectroscopy to characterize the elemental composition of PM samples collected from 27 globally distributed sites in the Surface PARTiculate mAtter Network (SPARTAN) over 2019-2023. Consistent protocols are applied to collect all samples and analyze them at one central laboratory, which facilitates comparison across different sites. Multiple quality assurance measures are performed, including applying reference materials that resemble typical PM samples, acceptance testing, and routine quality control. Method detection limits and uncertainties are estimated. Concentrations of dust and trace element oxides (TEO) are determined from the elemental dataset. In addition to sites in arid regions, a moderately high mean dust concentration (6 μg/m) in PM is also found in Dhaka (Bangladesh) along with a high average TEO level (6 μg/m). High carcinogenic risk (>1 cancer case per 100000 adults) from airborne arsenic is observed in Dhaka (Bangladesh), Kanpur (India), and Hanoi (Vietnam). Industries of informal lead-acid battery and e-waste recycling as well as coal-fired brick kilns likely contribute to the elevated trace element concentrations found in Dhaka.

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Exploring disparities of teleconsultation readiness: A comparative analysis of healthcare facilities in Indonesia

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DIGITAL HEALTH 2024年 10卷

作者： Daniel Chriswinanto Adityo Nugroho Katherina Adisaputro Mitra Andini Sigilipoe Ida Ayu Triastuti Suryani Hutomo Ardhinta Bellano Septarda Aryososepti Yuwono Caraka Randi Yusuf Dedik Sulistiawan Balqis Gusbela Jason C Hsu Emily Chia-Yu Su Faculty of Medicine Universitas Kristen Duta Wacana Yogyakarta IndonesiaGraduate Institute of Biomedical Informatics College of Medical Science and Technology Taipei Medical University Taipei Faculty of Medicine Universitas Kristen Duta Wacana Yogyakarta Indonesia Faculty of Public Health Universitas Ahmad Dahlan Yogyakarta IndonesiaSchool of Public Health Taipei Medical University Taipei International PhD Program in Biotech and Healthcare Management College of Management Taipei Medical University Taipei International PhD Program in Biotech and Healthcare Management College of Management Taipei Medical University TaipeiClinical Data Center Office of Data Science Taipei Medical University TaipeiClinical Big Data Research Center Taipei Medical University Hospital TaipeiResearch Center of Health Care Industry Data Science College of Management Taipei Medical University Taipei Graduate Institute of Biomedical Informatics College of Medical Science and Technology Taipei Medical University TaipeiClinical Big Data Research Center Taipei Medical University Hospital TaipeiInstitute of Biomedical Informatics College of Medicine National Yang Ming Chiao Tung University Taipei

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The ALMA-QUARKS Survey: II. the ACA 1.3 mm continuum source catalog and the assembly of dense gas in massive star-forming clumps

arXiv

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arXiv 2024年

作者： Xu, Fengwei Wang, Ke Liu, Tie Zhu, Lei Garay, Guido Liu, Xunchuan Goldsmith, Paul Zhang, Qizhou Sanhueza, Patricio Qin, Shengli He, Jinhua Juvela, Mika Tej, Anandmayee Liu, Hongli Li, Shanghuo Morii, Kaho Zhang, Siju Zhou, Jianwen Stutz, Amelia Evans, Neal J. Kee-Tae, Kim Liu, Shengyuan Mardones, Diego Li, Guangxing Bronfman, Leonardo Tatematsu, Kenichi Lee, Chang Won Lu, Xing Mai, Xiaofeng Jiao, Sihan Chibueze, James O. Su, Keyun Tóth, L. Viktor Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road 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 Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Tokyo Mitaka181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Tokyo Mitaka181-8588 Japan School of Physics and Astronomy Yunnan University Kunming650091 China Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Department of Physics University of Helsinki PO Box 64 HelsinkiFI-00014 Finland Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India Max Planck Institute for Astronomy Knigstuhl 17 HeidelbergD-69117 Germany Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany Departamento de Astronoma Universidad de Concepcion Casilla 160-C Concepción Chile 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 South-Western Institute for Astronomy

Leveraging the high resolution, sensitivity, and wide frequency coverage of the Atacama Large Millimeter/submillimeter Array (ALMA), the QUARKS survey, standing for 'Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures', is observing 139 massive star-forming clumps at ALMA Band 6 (λ ∼ 1.3 mm). This paper introduces the Atacama Compact Array (ACA) 7-m data of the QUARKS survey, describing the ACA observations and data reduction. Combining multi-wavelength data, we provide the first edition of QUARKS atlas, offering insights into the multiscale and multiphase interstellar medium (ISM) in high-mass star formation. The ACA 1.3 mm catalog includes 207 continuum sources that are called ACA sources. Their gas kinetic temperatures are estimated using three formaldehyde transitions with a non-LTE radiation transfer model, and the mass and density are derived from a dust emission model. The ACA sources are massive (16-84 percentile values of 6-160 M☉), gravity-dominated (M ∝ R1.1) fragments within massive clumps, with supersonic turbulence (M > 1) and embedded star-forming protoclusters. We find a linear correlation between the masses of the fragments and the massive clumps, with a ratio of 6% between the two. When considering the fragments as representative of dense gas, the ratio indicates a dense gas fraction (DGF) of 6%, although with a wide scatter ranging from 1% to 10%. If we consider the QUARKS massive clumps to be what is observed at various scales, then the size-independent DGF indicates a self-similar fragmentation or collapsing mode in protocluster formation. With the ACA data over four orders of magnitude of luminosity-to-mass ratio (L/M), we find that the DGF increases significantly with L/M, which indicates clump evolutionary stage. We observed a limited fragmentation at the subclump scale, which can be explained by dynamic global collapse process. © 2024, CC BY.

关键词： Kinematics

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The Future of Gamma-Ray Experiments in the MeV-EeV Range

arXiv

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arXiv 2022年

作者： Engel, Kristi Goodman, Jordan Huentemeyer, Petra Kierans, Carolyn Lewis, Tiffany R. Negro, Michela Santander, Marcos Williams, David A. University Of Maryland College Park College ParkMD20742 United States Physics Division Los Alamos National Laboratory Los AlamosNM87545 United States Michigan Technological University HoughtonMI49931 United States Astroparticle Physics Laboratory NASA Goddard Space Flight Center GreenbeltMD20771 United States NASA Postdoctoral Program University Of Maryland Baltimore County BaltimoreMD21250 United States Center For Research And Exploration In Space Science And Technology NASA/GSFC GreenbeltMD20771 United States University Of Alabama TuscaloosaAL35487 United States Santa Cruz Institute For Particle Physics Department Of Physics University Of California Santa Cruz Santa CruzCA95064 United States

Naturally occurring particle accelerators shine brightly throughout the universe, inviting us to discover fundamental laws and hone our theories if we look in their directions with the right detectors. Gamma-rays, the most energetic photons, carry information from the far reaches of extragalactic space with minimal interaction or loss of information. They bring messages about particle acceleration in environments so extreme they cannot be reproduced on earth for a closer look. Gamma-ray astrophysics is so complementary with collider work that particle physicists and astroparticle physicists are often one in the same. Gamma-ray instruments, especially the Fermi Gamma-ray space Telescope, have been pivotal in major multi-messenger discoveries over the past decade. There is presently a great deal of interest and scientific expertise available to push forward new technologies, to plan and build space- and ground-based gamma-ray facilities, and to build multimessenger networks with gamma rays at their core. It is therefore concerning that before the community comes together for planning exercises again, much of that infrastructure could be lost to a lack of long-term planning for support of gamma-ray astrophysics. Gamma-rays with energies from the MeV to the EeV band are therefore central to multiwavelength and multi-messenger studies to everything from astroparticle physics with compact objects, to dark matter studies with diffuse large scale structure. These science goals and the excitement of new discoveries have generated a wave of new gamma-ray facility proposals and programs. Since the legacy of existing facilities is well covered in many other places, this paper highlights new and proposed gamma-ray technologies and facilities that have each been designed to address specific needs in the measurement of extreme astrophysical sources that probe some of the most pressing questions in fundamental physics for the next decade. The proposed instrumentation would also add

关键词： Gamma rays

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SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). V. Confusion-limited Submillimeter Galaxy Number Counts at 450 µm and Data Release for the COSMOS Field

arXiv

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arXiv 2024年

作者： Gao, Zhen-Kai Lim, Chen-Fatt Wang, Wei-Hao Chen, Chian-Chou Smail, Ian Chapman, Scott C. Zheng, Xian Zhong Shim, Hyunjin Kodama, Tadayuki Ao, Yiping Chang, Siou-Yu Clements, David L. Dunlop, James S. Ho, Luis C. Hsu, Yun-Hsin Hwang, Chorng-Yuan Hwang, Ho Seong Koprowski, M.P. Scott, Douglas Serjeant, Stephen Toba, Yoshiki Urquhart, Sheona A. No. 1 Section 4 Roosevelt Rd. Taipei10617 Taiwan Graduate Institute of Astronomy National Central University 300 Zhongda Road Zhongli Taoyuan32001 Taiwan Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Department of Physics and Atmospheric Science Dalhousie University Halifax HalifaxNSB3H 3J5 Canada 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 Department of Earth Science Education Kyungpook National University 80 Daehak-ro Buk-gu Daegu41566 Korea Republic of Astronomical Institute Tohoku University 6-3 Aramaki Aoba Miyagi Sendai980-8578 Japan Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu30013 Taiwan Imperial College London Blackett Laboratory Prince Consort Road LondonSW7 2AZ United Kingdom SUPA Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Department of Philosophy National Taiwan University No. 1 Section 4 Roosevelt Rd. Taipei10617 Taiwan Astronomy Program Department of Physics and Astronomy 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 Institute of Astronomy Faculty of Physics Astronomy and Informatics Nicolaus Copernicus University Grudziadzka 5 Torun87-100 Poland Department of Physics and Astronomy University of British Columbia 6224 Agricultural Road VancouverBCV6T 1Z1 Canada School of Physical Sciences The Open University Milton KeynesMK7 6AA United Kingdom

We present confusion-limited SCUBA-2 450-µm observations in the COSMOS-CANDELS region as part of the JCMT Large program, SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). Our maps at 450 and 850 µm cover an area of 450 arcmin2. We achieved instrumental noise levels of σ450 = 0.59 mJy beam−1 and σ850 = 0.09 mJy beam−1 in the deepest area of each map. The corresponding confusion noise levels are estimated to be 0.65 and 0.36 mJy beam−1. Above the 4 (3.5) σ threshold, we detected 360 (479) sources at 450 µm and 237 (314) sources at 850 µm. We derive the deepest blank-field number counts at 450 µm, covering the flux-density range of 2 to 43 mJy. These are in agreement with other SCUBA-2 blank-field and lensing-cluster observations, but are lower than various model counts. We compare the counts with those in other fields and find that the field-to-field variance observed at 450 µm at the R = 6′ scale is consistent with Poisson noise, so there is no evidence of strong 2-D clustering at this scale. Additionally, we derive the integrated surface brightness at 450 µm down to 2.1 mJy to be (Equation presented) Jy deg−2, contributing to (41±4)% of the 450-µm extragalactic background light (EBL) measured by COBE and Planck. Our results suggest that the 450-µm EBL may be fully resolved at (Equation presented) mJy, which extremely deep lensing-cluster observations and next-generation submillimeter instruments with large aperture sizes may be able to achieve. © 2024, CC BY.

关键词： Galaxies

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The transit timing and atmosphere of hot jupiter HAT-P-37b

arXiv

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arXiv 2021年

作者： A-Thano, Napaporn Jiang, Ing-Guey Awiphan, Supachai Rattanamala, Ronnakrit Su, Li-Hsin Hengpiya, Torik Sariya, Devesh P. Yeh, Li-Chin Shlyapnikov, A.A. Gorbachev, Mark A. Rublevski, Alexey N. Mannaday, Vineet Kumar Thakur, Parijat Sahu, D.K. Mkrtichian, David Griv, Evgeny Department of Physics and Institute of Astronomy National Tsing-Hua University Hsinchu30013 Taiwan National Astronomical Research Institute of Thailand 260 Moo 4 Donkaew Mae Rim Chiang Mai50180 Thailand PhD Program in Astronomy Department of Physics and Materials Science Faculty of Science Chiang Mai University Chiang Mai50200 Thailand Department of Physics and General Science Faculty of Science and Technology Nakhon Ratchasima Rajabhat University Nakhon Ratchasima30000 Thailand Regional Observatory for the Public Songkhla 79/4 Moo 4 Khao Roop Chang Muang District Songkhla90000 Thailand Institute of Computational and Modeling Science National Tsing-Hua University Hsinchu30013 Taiwan Crimean Astrophysical Observatory 298409 Nauchny Crimea 495009 India Indian Institute of Astrophysics Bangalore560034 India Department of Physics Ben-Gurion University Beer-Sheva84105 Israel

The transit timing variation (TTV) and transmission spectroscopy analyses of the planet HAT-P-37b, which is a hot Jupiter orbiting an G-type star, were performed. Nine new transit light curves are obtained and analysed together with 21 published light curves from the literature. The updated physical parameters of HAT-P-37b are presented. The TTV analyses show a possibility that the system has an additional planet which induced the TTVs amplitude signal of 1.74 ± 0.17 minutes. If the body is located near the 1:2 mean motion resonance orbit, the sinusoidal TTV signal could be caused by the gravitational interaction of a sub-Earth mass planet with mass of 0.06 MO. From the analysis of an upper mass limit for the second planet, the Saturn mass planet with orbital period less than 6 days is excluded. The broad-band transmission spectra of HAT-P-37b favours a cloudy atmospheric model with an outlier spectrum in B-filter. Copyright © 2021, The Authors. All rights reserved.

关键词： Planets

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Tract Integrity Predicts Neurological Outcomes in Neonatal Hypoxic-Ischemic Encephalopathy

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Pediatrics & Neonatology 2025年

作者： Pei-Ling Tsai Yu-Chun Lo Yi-Shan Tsai Yea-Shwu Hwang Ting-Chun Lin Yao-Wen Liang Chen-En Huang Fu-Chun Hsu Yi-Fang Tu You-Yin Chen Institute of Allied Health Sciences College of Medicine National Cheng Kung University Tainan Taiwan PhD Program in Medical Neuroscience College of Medical Science and Technology Taipei Medical University Taipei Taiwan Department of Medical Imaging National Cheng Kung University Hospital College of Medicine National Cheng Kung University Tainan Taiwan Department of Occupational Therapy College of Medicine National Cheng Kung University Tainan Taiwan Department of Biomedical Engineering National Yang Ming Chiao Tung University Taipei Taiwan College of Medicine National Yang Ming Chiao Tung University Taipei Taiwan Department of Pediatrics National Cheng Kung University Hospital College of Medicine National Cheng Kung University Tainan Taiwan Institute of Clinical Medicine College of Medicine National Cheng Kung University Tainan Taiwan Medical Device Innovation and Translation Center National Yang Ming Chiao Tung University Taipei Taiwan

Objective Early prognostication in infants with neonatal hypoxic-ischemic encephalopathy (HIE) is crucial for follow-up management. Alternations of microstructural integrity of neural fiber tracts in large-scale neural networks might predict neurological outcomes. Methods All consecutively-admitted patients with neonatal HIE from 2016 to 2020 were enrolled. Diffusion tensor imaging (DTI) tractography was performed at 4–7 days of age. Neurodevelopmental outcomes at 24 months of age were assessed with Bayley Scales of Infant Development, 3rd edition. Results A total of 62 HIE infants were enrolled, and 53 of these underwent DTI. Fractional anisotropy (FA) and mean diffusivity (MD) were measured to indicate the microstructural integrity of tracts, including the arcuate fasciculus, uncinate fasciculus, inferior fronto-occipital fasciculus, corticospinal tract (CST), and optic radiations (OR). Lower FA values of target tracts were associated with lower developmental scores at 24 months of age, particularly in the CST and OR (all P ≤ 0.003). The prognostic accuracy of FA values in CST surpassed that in the region of thalamus/basal ganglia (area under curves 0.839, 95% CI: 0.728–0.950 vs. 0.755, 95% CI: 0.583–0.928). Furthermore, the correlation between FA values in target tracts and developmental scores was most significant in infants with HIE stage III and this was not affected by therapeutic hypothermia. Conclusion Tract integrity in the CST and OR detected by DTI provides valuable insights for early prognostication in infants with HIE, regardless of therapeutic hypothermia.

关键词： neonatal hypoxic-ischemic encephalopathy diffusion tensor imaging tractography corticospinal tract optic radiations neurodevelopmental outcome

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Silica nanocone array as a template for fabricating a plasmon induced hot electron photodetector

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Photonics Research 2019年第3期7卷 294-299页

作者： ZHIQIANG YANG KANG DU FANFAN LU YANG PANG SHIJIA HUA XUETAO GAN WENDING ZHANG SOO JIN CHUA TING MEI Key Laboratory of Space Applied Physics and Chemistry Ministry of Education and Shaanxi Key Laboratory of Optical Information TechnologySchool of Science Northwestern Polytechnical University Department of Electrical and Computer Engineering National University of Singapore LEES Program Singapore-MIT Alliance for Research & Technology (SMART)

Plasmon induced hot electrons have attracted a great deal of interest as a novel route for photodetection and lightenergy harvesting. Herein, we report a hot electron photodetector in which a large array of nanocones deposited sequentially with aluminum, titanium dioxide, and gold films can be integrated functionally with nanophotonics and microelectronics. The device exhibits a strong photoelectric response at around 620 nm with a responsivity of 180 μA/W under short-circuit conditions with a significant increase under 1 V reverse bias to 360 μA/W. The increase in responsivity and a red shift in the peak value with increasing bias voltage indicate that the bias causes an increase in the hot electron tunneling effect. Our approach will be advantageous for the implementation of the proposed architecture on a vast variety of integrated optoelectronic devices.

关键词： Silica nanocone array plasmon induced hot electron photodetector

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JOYS+: mid-infrared detection of gas-phase SO2 emission in a low-mass protostar The case of NGC 1333 IRAS2A: hot core or accretion shock

arXiv

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arXiv 2023年

作者： Van Gelder, Martijn Ressler, M.E. van Dishoeck, E.F. Nazari, P. Tabone, B. Black, J.H. Tychoniec, L. Francis, L. Barsony, M. Beuther, H. Caratti o Garatti, A. Chen, Y. Gieser, C. le Gouellec, V.J.M. Kavanagh, P.J. Klaassen, P.D. Lew, B.W.P. Linnartz, H. Majumdar, L. Perotti, G. Rocha, W.R.M. Leiden Observatory Leiden University PO Box 9513 Leiden2300RA Netherlands Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Giessenbachstrasse 1 Garching85748 Germany Université Paris-Saclay CNRS Institut d’Astrophysique Spatiale Orsay91405 France Chalmers University of Technology Department of Space Earth and Environment Onsala Space Observatory Onsala439 92 Sweden European Southern Observatory Karl-Schwarzschild-Strasse 2 Garching bei Mnchen 85748 Germany SETI Institute 189 Bernardo Avenue 2nd Floor Mountain ViewCA94043 United States Max Planck Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany INAF-Osservatorio Astronomico di Capodimonte Salita Moiariello 16 Napoli80131 Italy NASA Ames Research Center Space Science and Astrobiology Division M.S. 245-6 Moffett FieldCA94035 United States NASA Postdoctoral Program Fellow United States Department of Experimental Physics Maynooth University Maynooth Co Kildare Ireland UK Astronomy Technology Centre Royal Observatory Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom Bay Area Environmental Research Institute NASA Ames Research Center Moffett FieldCA94035 United States Laboratory for Astrophysics Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands School of Earth and Planetary Sciences National Institute of Science Education and Research Odisha Jatni752050 India Homi Bhabha National Institute Training School Complex Anushaktinagar Mumbai400094 India

Context. The Mid-InfraRed Instrument (MIRI) on the James Webb space Telescope (JWST) has sharpened our infrared eyes toward the star formation process. Due to its unprecedented spatial and spectral resolution and sensitivity in the mid-infrared, JWST/MIRI can see through highly extincted protostellar envelopes and probe the warm inner regions. An abundant molecule in these warm inner regions is SO2, which is a common tracer of both outflow and accretion shocks as well as hot core chemistry. Aims. This paper presents the first mid-infrared detection of gaseous SO2 emission in an embedded low-mass protostellar system rich in complex molecules and aims to determine the physical origin of the SO2 emission. Methods. JWST/MIRI observations taken with the Medium Resolution Spectrometer (MRS) of the low-mass protostellar binary NGC 1333 IRAS2A are presented from the JWST Observations of Young protoStars (JOYS+) program, revealing emission from the SO2 ν3 asymmetric stretching mode at 7.35 µm. Using simple slab models and assuming local thermodynamic equilibrium (LTE), the rotational temperature and total number of SO2 molecules are derived. The results are compared to those derived from high-angular resolution SO2 data on the same scales (∼ 50 − 100 au) obtained with the Atacama Large Millimeter/submillimeter Array (ALMA). Results. The SO2 emission from the ν3 band is predominantly located on ∼ 50 − 100 au scales around the MIR continuum peak of the main component of the binary, IRAS2A1. A rotational temperature of 92±8 K is derived from the ν3 lines. This is in good agreement with the rotational temperature derived from pure rotational lines in the vibrational ground state (i.e., ν=0) with ALMA (104 ± 5 K) which are extended over similar scales. However, the emission of the ν3 lines in the MIRI-MRS spectrum is not in LTE given that the total number of molecules predicted by a LTE model is found to be a factor 2 × 104 higher than what is derived for the ν = 0 state from the

关键词： Ground state

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