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Optical Materials: X 2019年 2卷

作者： Fang, Y. Furniss, D. Jayasuriya, D. Parnell, H. Tang, Z.Q. Gibson, D. Bayya, S. Sanghera, J. Seddon, A.B. Benson, T.M. Mid-Infrared Photonics Group George Green Institute for Electromagnetics Research Faculty of Engineering University of Nottingham University Park NottinghamNG7 2RD United Kingdom Now Shenzhen Engineering Laboratory of Phosphorene and Optoelectronics Collaborative Innovation Center for Optoelectronic Science and Technology And Key Laboratory of Optoelectronic Devices and Systems of Ministry of Education and Guangdong Province Shenzhen University Shenzhen518060 China Now at ThorLabs 1 St. Thomas Place ElyCB7 4EX United Kingdom Rustat House 62 Clifton Rd CambridgeCB1 7EG United Kingdom Naval Research Laboratory WashingtonDC20375 United States

Chalcogenide glasses have attracted much attention for the realization of photonic components owing to their outstanding optical properties in the mid-infrared (MIR) region. However, relatively few refractive index dispersion data are presently available for these glasses at MIR wavelengths. This paper presents a mini review of methods we have both used and developed to determine the refractive indices and thermo-optic coefficients of chalcogenide glasses at MIR wavelengths, and is supported by new results. The mini review should be useful to both new and established researchers in the chalcogenide glass field and fields of MIR optics, fiber-optics and waveguides. Three groups of methods are distinguished: (1) spectroscopic ellipsometry, (2) prism-based methods, and (3) methods using Fourier transform infrared (FTIR) transmission data. The mini review is supported by a brief discussion of refractive index models. © 2019 The Author(s)

关键词： Refractive index

The DESI PRObabilistic value-added bright galaxy survey (PROVABGS) mock challenge

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arXiv 2022年

作者： Hahn, ChangHoon Kwon, K.J. Tojeiro, Rita Siudek, Malgorzata Canning, Rebecca E.A. Mezcua, Mar Tinker, Jeremy L. Brooks, David Doel, Peter Fanning, Kevin Gaztañaga, Enrique Kehoe, Robert Landriau, Martin Meisner, Aaron Moustakas, John Poppett, Claire Tarle, Gregory Weiner, Benjamin Zou, Hu Department Of Astrophysical Sciences Princeton University Peyton Hall PrincetonNJ08544 United States Astronomy Department University Of California At Berkeley BerkeleyCA94720 United States Department Of Physics University Of California Santa Barbara Santa BarbaraCA93106-9530 United States School Of Physics And Astronomy University Of St Andrews North Haugh St AndrewsKY16 9SS United Kingdom The Barcelona Institute Of Science And Technology Bellaterra Barcelona08193 Spain National Centre For Nuclear Research ul. Pasteura 7 Warsaw02-093 Poland Institute Of Cosmology & Gravitation University Of Portsmouth Dennis Sciama Building PortsmouthPO1 3FX United Kingdom Campus UAB Carrer de Can Magrans Barcelona08193 Spain C/ Gran Capità Barcelona08034 Spain Center For Cosmology And Particle Physics Department Of Physics New York University New York10003 United States Department Of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department Of Physics The Ohio State University 191 West Woodruff Avenue ColumbusOH43210 United States Institut De Cìencies De l'Espai IEEC-CSIC Campus UAB Carrer de Can Magrans s/n Bellaterra Barcelona08913 Spain Department Of Physics Southern Methodist University 3215 Daniel Avenue DallasTX75275 United States Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States NSF's National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Avenue TucsonAZ85719 United States Department Of Physics And Astronomy Siena College 515 Loudon Road LoudonvilleNY12211 United States Department Of Physics University Of Michigan Ann ArborMI48109 United States Department Of Physics University Of Arizona 1111 E. Fourth Street TucsonAZ85721 United States Key Laboratory Of Optical Astronomy National Astronomical Observatories Chinese Academy Of Sciences Beijing100012 China

The PRObabilistic Value-Added Bright Galaxy Survey (PROVABGS) catalog will provide measurements of galaxy properties, such as stellar mass (M∗), star formation rate (SFR), stellar metallicity (ZMW), and stellar age (tage;MW), for >10 million galaxies of the DESI Bright Galaxy Survey. Full posterior distributions of the galaxy properties will be inferred using state-of-the-art Bayesian spectral energy distribution (SED) mod- eling of DESI spectroscopy and Legacy Surveys photometry. In this work, we present the SED model, Bayesian inference framework, and methodology of PROVABGS. Furthermore, we apply the PROVABGS SED modeling on realistic synthetic DESI spectra and photometry, constructed using the L-Galaxies semi-analytic model. We compare the inferred galaxy properties to the true galaxy properties of the simulation using a hierarchical Bayesian framework to quantify accuracy and precision. Overall, we accurately infer the true M∗, SFR, ZMW, and tage;MWof the simulated galaxies. However, the priors on galaxy properties induced by the SED model have a significant impact on the posteriors. They impose a SFR>10-1Mo=yr lower bound on SFR, a ∼0.3 dex bias on log ZMWfor galaxies with low spectral signal-to-noise, and tage;MW © 2022, CC BY.

关键词： Galaxies

Terahertz Photon Detection: Sensitive Terahertz Detection and Imaging Driven by the Photothermoelectric Effect in Ultrashort-Channel Black Phosphorus Devices (Adv. Sci. 5/2020)

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Advanced science 2020年第5期7卷 2070029-2070029页

作者： Wanlong Guo Zhuo Dong Yijun Xu Changlong Liu Dacheng Wei Libo Zhang Xinyao Shi Cheng Guo Huang Xu Gang Chen Lin Wang Kai Zhang Xiaoshuang Chen Wei Lu State Key Laboratory of Infrared Physics Shanghai Institute of Technical Physics Chinese Academy of Sciences 500 Yu-Tian Road Shanghai 200083 China University of Chinese Academy of Sciences No. 19A Yuquan Road Beijing 100049 China School of Physical Science and Technology ShanghaiTech University Shanghai 201210 China CAS Key Laboratory of Nano-Bio Interface and Key Laboratory of Nanodevices and Applications i-Lab Suzhou Institute of Nano-Tech and Nano-Bionics (SINANO) Chinese Academy of Sciences Ruoshui Road 398 Suzhou Jiangsu 215123 China School of Nano Technology and Nano Bionics University of Science and Technology of China Jinzhai Road 96 Hefei Anhui 230026 China Zhejiang Lab Artificial Intelligence Town No.1818 Wenyixi Road Hangzhou 311100 China Institute of Molecular Materials and Devices Department of Material Sciences and Department of Macromolecular Sciences Fudan University Shanghai 200433 China

In article number https://***/10.1002/advs.201902699 , Lin Wang, Kai Zhang, Xiaoshuang Chen, and co‐workers boost the photothermoelectric effect (PTE) through ultrashort channel design via a titled‐angle evaporation technique. Such a detector exhibits tremendous field‐enhancement as well as high efficiency terahertz photon absorption across a broadband frequency range beyond the skin depth limit, introducing an avenue for deeply understanding the role of the PTE effect and its targeted applications for fast imaging.

关键词： black phosphorus imaging photothermoelectric effect terahertz detectors

SIMS Analysis of Impurity in HgCdTe Epilayers of infrared Focal Plane Array

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SIMS Analysis of Impurity in HgCdTe Epilayers of Infrared Fo...

第十九届国际电子封装技术会议(ICEPT 2018)

作者： Shaohua Yang Guoguang Lu Canxiong Lai Songmin Zhou Xi Wang Science and Technology on Reliability Physics and Application of Electronic Component Laboratory CEP Key Laboratory of Infrared Imaging Materials and Detectors Shanghai Institute of Technical Physics S

infrared Focal Plane Array(IRFPA)is a critical component for advanced infrared *** plays an important role in different applications including environmental monitoring,biomedicine,process control,science and *** get high performance IRFPA detectors,quality of HgCdTe epilayers is a critical *** this paper,we focus on the impurity in HgCdTe epilayers,which is closely related to the leakage current performance of IRFPA ***,the principle and characteristics of the Secondary Ion Mass Spectrometry(SIMS)are *** high sensitivity and all-elements detection ability make it an effective technology to study trace ***,the impurity elements and their distribution properties in HgCdTe epilayers are investigated by SIMS *** of Li,Na,K and Ca are found in ***,the source of the impurity is analysised based on the epitaxial growth process of HgCdTe *** impact of the impurity on device performance is also discussed.

关键词： Secondary ion mass spectrometry (SIMS) Impurity HgCdTe liquid phase epitaxy (LPE)

cosmological insights into the early accretion of r-process-enhanced stars. I. acomprehensive chemo-dynamical analysis of lamost j1109+0754

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arXiv 2020年

作者： Mardini, Mohammad K. Placco, Vinicius M. Meiron, Yohai Ishchenko, Marina Avramov, Branislav Mazzarini, Matteo Berczik, Peter Sedda, Manuel Arca Beers, Timothy C. Frebel, Anna Taani, Ali Donnari, Martina Al-Wardat, Mashhoor A. Zhao, Gang Key Lab of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Institute of Space Sciences Shandong University Weihai264209 China NSF’s Optical-Infrared Astronomy Research Laboratory TucsonAZ85719 United States Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S3H4 Canada Main Astronomical Observatory National Academy of Sciences of Ukraine 27 Akademika Zabolotnoho St. Kyiv03143 Ukraine Astronomisches Rechen Institut - Zentrum für Astronomie der Universität Heidelberg Mönchhofstrasse 12-14 HeidelbergD-69120 Germany National Astronomical Observatories and Key Laboratory of Computational Astrophysics Chinese Academy of Sciences 20A Datun Rd. Chaoyang District Beijing100101 China Department of Physics University of Notre Dame Notre DameIN46556 United States United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Physics Department Faculty of Science Al-Balqa Applied University Jordan Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany Department of Applied Physics and Astronomy University of Sharjah Sharjah United Arab Emirates Sharjah Academy for Astronomy Space Sciences and Technology University of Sharjah Sharjah United Arab Emirates

This study presents a comprehensive chemo-dynamical analysis of LAMOST J1109+0754, a bright (V = 12.8), extremely metal-poor ([Fe/H] = −3.17) star, with a strong r-process enhancement ([Eu/Fe] = +0.94 ± 0.12). Our results are based on the 7-D measurements supplied by Gaia and the chemical composition derived from a high-resolution (R ∼ 110, 000), high signal-to-noise ratio (S/N ∼ 60) optical spectrum obtained by the 2.4 m Automated Planet Finder Telescope at Lick Observatory. We obtain chemical abundances of 31 elements (from lithium to thorium). The abundance ratios ([X/Fe]) of the light-elements (Z 6 30) suggest a massive Population III progenitor in the 13.4-29.5 M mass range. The heavy-element (30 Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

Electrical and optical property of annealed Te-doped GaSb

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Journal of Semiconductors 2017年第4期38卷 18-22页

作者： Jie Su Tong Liu Jingming Liu Jun Yang Guiying Shen Yongbiao Bai Zhiyuan Dong Fangfang Wang Youwen Zhao Key Laboratory of Semiconductor Materials Science Beijing Key Laboratory of Low Dimensional Semiconductor Materialsand DevicesInstitute of SemiconductorsChinese Academy of SciencesBeijing 100083China College of Materials Science and Opto-Electronic Technology University of Chinese Academy of SciencesBeijing 100049China Inner Mongolia Aerospace Honggang Machinery Corporation Limited Hohhot 010020China Key Laboratory of Infrared Imaging Materials and Detectors Shanghai Institute of Technical Physics Chinese Academy of SciencesShanghai 200083China

GaSb is the most suitable substrate in the epitaxial growth of mixed semiconductors of GaSb *** this work,Te-doped GaSb bulk crystals with different doping concentration have been annealed at 550℃ for100 h in ambient *** annealed samples have been studied by Hall effect measurement,infrared（IR）optical transmission,Glow discharge mass spectroscopy（GDMS） and photoluminescence（PL） *** annealing,Te-doped GaSb samples exhibit a decrease of carrier concentration and increase of mobility,along with an improvement of below gap IR *** acceptor related electrical compensation analysis suggests a formation of donor defect with deeper energy *** mechanism of the variation of the defect and its influence on the material properties are discussed.

关键词： Te-doped GaSb annealing Hall effect measurement photoluminescence spectroscopy IR optical transmission

Long-Term Decline of the Mid-infrared Emission of Normal Galaxies: Dust Echo of Tidal Disruption Flare?

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arXiv 2018年

作者： Wang, Tinggui Yan, Lin Dou, Liming Jiang, Ning Sheng, Zhenfeng Yang, Chenwei CAS Key Laboratory for Research in Galaxies and Cosmology University of Science and Technology of China Hefei Anhui230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei Anhui230026 China Caltech Optical Observatories Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States Infrared Processing and Analysis Center California Institute of Technology PasadenaCA91125 United States Center for Astrophysics Guangzhou University Guangzhou510006 China Astronomy Science and Technology Research Laboratory Department of Education of Guangdong Province Guangzhou510006 China

We report the discovery of a sample of 19 low redshift (z ν) after subtracting host galaxies are in the range of a few 1042 to 1044 erg s−1 with a median of 5 × 1043 erg s−1 in the W2 band. The black hole masses distribute in a wide range with more than half in between 107 to 108 Mo, but significantly different from that of optical/UV selected TDEs. Furthermore, MIR luminosities are correlated with black hole masses, the stellar mass or luminosity of their host bulges. Most galaxies in the sample are red and luminous with an absolute magnitude of r between -20 to -23. We estimate the rate of event about 10−4 gal−1 yr−1 among luminous red galaxies. We discuss several possibilities for the variable infrared sources, and conclude that most likely, they are caused by short sporadic fueling to the supermassive black holes via either the instability of accretion flows or tidal disruption of stars. Copyright © 2018, The Authors. All rights reserved.

关键词： Black holes

GOODS-ALMA 2.0: Starbursts in the main sequence reveal compact star formation regulating galaxy evolution prequenching

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arXiv 2022年

作者： Gómez-Guijarro, Carlos Elbaz, D. Xiao, M. Kokorev, V.I. Magdis, G.E. Magnelli, B. Daddi, E. Valentino, F. Sargent, M.T. Dickinson, M. Béthermin, M. Franco, M. Pope, A. Kalita, B.S. Ciesla, L. Demarco, R. Inami, H. Rujopakarn, W. Shu, X. Wang, T. Zhou, L. Alexander, D.M. Bournaud, F. Chary, R. Ferguson, H.C. Finkelstein, S.L. Giavalisco, M. Iono, D. Juneau, S. Kartaltepe, J.S. Lagache, G. Le Floc'h, E. Leiton, R. Leroy, L. Lin, L. Motohara, K. Mullaney, J. Okumura, K. Pannella, M. Papovich, C. Treister, E. AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité Gif-sur-Yvette F-91191 France School of Astronomy and Space Science Nanjing University Nanjing210093 China Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen N DK-2200 Denmark DTU-Space Technical University of Denmark Elektrovej 327 Kgs. Lyngby DK-2800 Denmark Astronomy Centre Department of Physics and Astronomy University of Sussex BrightonBN1 9QH United Kingdom Hallerstrasse 6 BernCH-3012 Switzerland Community Science and Data Center NSF's NOIRLab 950 N. Cherry Ave. TucsonAZ85719 United States Aix Marseille Université CNRS LAM Laboratoire d'Astrophysique de Marseille Marseille France Centre for Astrophysics Research University of Hertfordshire HatfieldAL10 9AB United Kingdom Astronomy Department University of Massachusetts AmherstMA01003 United States Departamento de Astronomía Facultad de Ciencias Fsicas y Matemáticas Universidad de Concepción Concepción Chile Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Hiroshima Higashi-Hiroshima 739-8526 Japan Department of Physics Faculty of Science Chulalongkorn University 254 Phayathai Road Pathumwan Bangkok10330 Thailand Don Kaeo Mae Rim Chiang Mai50180 Thailand UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Department of Physics Anhui Normal University Anhui Wuhu241000 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education Nanjing210093 China Centre for Extragalactic Astronomy Department of Physics Durham University DurhamDH1 3LE United Kingdom Infrared Processing and Analysis Center MS314-6 California Institute of Technology PasadenaCA91125 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Astronomy The University of Texas at Austin AustinTX78712 United States National Astronomical Observatory of Jap

Compact star formation appears to be generally common in dusty star-forming galaxies (SFGs). However, its role in the framework set by the scaling relations in galaxy evolution remains to be understood. In this work we follow up on the galaxy sample from the GOODS-ALMA 2.0 survey, an ALMA blind survey at 1.1 mm covering a continuous area of 72.42 arcmin2 using two array configurations. We derived physical properties, such as star formation rates, gas fractions, depletion timescales, and dust temperatures for the galaxy sample built from the survey. There exists a subset of galaxies that exhibit starburst-like short depletion timescales, but they are located within the scatter of the so-called main sequence of SFGs. These are dubbed starbursts in the main sequence and display the most compact star formation and they are characterized by the shortest depletion timescales, lowest gas fractions, and highest dust temperatures of the galaxy sample, compared to typical SFGs at the same stellar mass and redshift. They are also very massive, accounting for ∼ 60% of the most massive galaxies in the sample (log(M∗/M ) > 11.0). We find trends between the areas of the ongoing star formation regions and the derived physical properties for the sample, unveiling the role of compact star formation as a physical driver of these properties. Starbursts in the main sequence appear to be the extreme cases of these trends. We discuss possible scenarios of galaxy evolution to explain the results drawn from our galaxy sample. Our findings suggest that the star formation rate is sustained in SFGs by gas and star formation compression, keeping them within the main sequence even when their gas fractions are low and they are presumably on the way to quiescence. Copyright © 2022, The Authors. All rights reserved.

关键词： Galaxies

Blanco DECam bulge survey (BDBS) II: Project performance, data analysis, and early science results

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arXiv 2020年

作者： Johnson, Christian I Rich, R. Michael Young, Michael D Simion, Iulia T Clarkson, William I Pilachowski, Catherine A Michael, Scott Kunder, Andrea Koch, Andreas Vivas, A. Katherina Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy UCLA 430 Portola Plaza Box 951547 Los AngelesCA90095-1547 United States Indiana University University Information Technology Services CIB 2709 E 10th Street BloomingtonIN47401 United States Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory 80 Nandan Road Shanghai200030 China Department of Natural Sciences University of Michigan-Dearborn 4901 Evergreen Rd. DearbornMI48128 United States Indiana University Department of Astronomy SW319 727 E 3rd Street BloomingtonIN47405 United States Saint Martin’s University 5000 Abbey Way SE LaceyWA98503 United States Zentrum für Astronomie der Universität Heidelberg Astronomisches Rechen-Institut Mönchhofstr. 12 Heidelberg69120 Germany Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile

The Blanco DECam Bulge Survey (BDBS) imaged more than 200 square degrees of the Southern Galactic bulge using the ugrizY filters of the Dark Energy Camera, and produced point spread function photometry of approximately 250 million unique sources. In this paper, we present details regarding the construction and collation of survey catalogs, and also discuss the adopted calibration and dereddening procedures. Early science results are presented with a particular emphasis on the bulge metallicity distribution function and globular clusters. A key result is the strong correlation (σ ∼ 0.2 dex) between (u − i)o and [Fe/H] for bulge red clump giants. We utilized this relation to find that interior bulge fields may be well described by simple closed box enrichment models, but fields exterior to b ∼ −6◦ seem to require a secondary metal-poor component. Applying scaled versions of the closed box model to the outer bulge fields is shown to significantly reduce the strengths of any additional metal-poor components when compared to Gaussian mixture models. Additional results include: a confirmation that the u-band splits the sub-giant branch in M 22 as a function of metallicity, the detection of possible extra-tidal stars along the orbits of M 22 and FSR 1758, and additional evidence that NGC 6569 may have a small but discrete He spread, as evidenced by red clump luminosity variations in the reddest bands. We do not confirm previous claims that FSR 1758 is part of a larger extended structure. Copyright © 2020, The Authors. All rights reserved.

关键词： Astrophysics

The HASHTAG project: The first submillimeter images of the andromeda galaxy from the ground

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arXiv 2021年

作者： Smith, Matthew W.L. Eales, Stephen A. Williams, Thomas G. Lee, Bumhyun Li, Zongnan Barmby, Pauline Bureau, Martin Chapman, Scott Cho, Brian S. Chung, Aeree Chung, Eun Jung Chung, Hui-Hsuan Clark, Christopher J.R. Clements, David L. Davis, Timothy A. De Looze, Ilse Eden, David J. Athikkat-Eknath, Gayathri Ford, George P. Gao, Yu Gear, Walter Gomez, Haley L. de Grijs, Richard He, Jinhua Ho, Luis C. Hughes, Thomas M. Jiao, Sihan Li, Zhiyuan Kemper, Francisca Kirchschlager, Florian Koch, Eric W. Kong, Albert K.H. Lee, Chien-Hsiu Lin, En-Tzu Mairs, Steve Michalowski, Michal J. Pattle, Kate Peng, Yingjie Ragan, Sarah E. Rawlings, Mark G. Rigopoulou, Dimitra Saintonge, Amelie Schruba, Andreas Tang, Xindi Wang, Junfeng Whitworth, Anthony P. Wilson, Christine D. Yim, Kijeong Zhu, Ming School of Physics & Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy Yonsei University 50 Yonsei-ro Seodaemun-gu Seoul03722 Korea Republic of School of Astronomy and Space Science Nanjing University Nanjing210023 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Nanjing210023 China Department of Physics & Astronomy Institute for Earth & Space Exploration University of Western Ontario 1151 Richmond Street LondonON Canada Sub-Department of Astrophysics Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Dalhousie University HalifaxNS Canada Department of Physics and Astronomy Seoul National University Gwanak-gu Seoul08826 Korea Republic of Department of Astronomy Yonsei University 50 Yonsei-ro Seodaemun-gu Seoul03722 Korea Republic of Department of Astronomy and Space Science Chungnam National University 99 Daehak-ro Yuseong-gu Daejeon34134 Korea Republic of Institute of Astronomy National Tsing Hua University Hsinchu30013 Taiwan Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Astrophysics Group Physics Department Blackett Laboratory Imperial College London Prince Consort Road LondonSW7 2AZ United Kingdom Sterrenkundig Observatorium Ghent University Krijgslaan 281 - S9 GhentB-9000 Belgium Department of Physics and Astronomy University College London LondonWC1E 6BT United Kingdom Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Department of Astronomy Xiamen University Fujian Xiamen361005 China Purple Mountain Observatory Key Laboratory for Radio Astronomy Chinese Academy of Sciences 10 Yuanhua Road N

Observing nearby galaxies with submillimeter telescopes on the ground has two major challenges. First, the brightness is significantly reduced at long submillimeter wavelengths compared to the brightness at the peak of the dust emission. Second, it is necessary to use a high-pass spatial filter to remove atmospheric noise on large angular scales, which has the unwelcome by-product of also removing the galaxy's large-scale structure. We have developed a technique for producing high-resolution submillimeter images of galaxies of large angular size by using the telescope on the ground to determine the small-scale structure (the large Fourier components) and a space telescope (Herschel or Planck) to determine the large-scale structure (the small Fourier components). Using this technique, we are carrying out the HARP and SCUBA-2 High Resolution Terahertz Andromeda Galaxy Survey (HASHTAG), an international Large Program on the James Clerk Maxwell Telescope, with one aim being to produce the first high-fidelity high-resolution submillimeter images of Andromeda. In this paper, we describe the survey, the method we have developed for combining the space-based and ground-based data, and present the first HASHTAG images of Andromeda at 450 and 850 µm. We also have created a method to predict the CO(J=3-2) line flux across M 31, which contaminates the 850 µm band. We find that while normally the contamination is below our sensitivity limit, the contamination can be significant (up to 28%) in a few of the brightest regions of the 10 kpc ring. We therefore also provide images with the predicted line emission removed. © 2021, CC BY.

关键词： Surveys