检索结果-内蒙古大学图书馆

arXiv 2021年

作者： Lokken, Martine Hložek, R. van Engelen, A. Madhavacheril, M. Baxter, E. DeRose, J. Doux, C. Pandey, S. Rykoff, E.S. Stein, G. To, C. Abbott, T.M.C. Adhikari, S. Aguena, M. Allam, S. Andrade-Oliveira, F. Annis, J. Battaglia, N. Bernstein, G.M. Bertin, E. Bond, J.R. Brooks, D. Calabrese, E. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Cawthon, R. Choi, A. Costanzi, M. Crocce, M. da Costa, L.N. da Silva Pereira, M.E. De Vicente, J. Desai, S. Dietrich, J.P. Doel, P. Dunkley, J. Everett, S. Evrard, A.E. Ferraro, S. Flaugher, B. Fosalba, P. Frieman, J. Gallardo, P.A. García-Bellido, J. Gaztanaga, E. Gerdes, D.W. Giannantonio, T. Gruen, D. Gruendl, R.A. Gschwend, J. Gutierrez, G. Hill, J.C. Hilton, M. Hincks, A.D. Hinton, S.R. Hollowood, D.L. Honscheid, K. Hoyle, B. Huang, Z. Hughes, J.P. Huterer, D. Jain, B. James, D.J. Jeltema, T. Kuehn, K. Lima, M. Maia, M.A.G. Marshall, J.L. McMahon, J. Melchior, P. Menanteau, F. Miquel, R. Mohr, J.J. Moodley, K. Morgan, R. Nati, F. Page, L. Ogando, R.L.C. Palmese, A. Paz-Chinchón, F. Plazas Malagón, A.A. Pieres, A. Romer, A.K. Rozo, E. Sanchez, E. Scarpine, V. Schillaci, A. Schubnell, M. Serrano, S. Sevilla-Noarbe, I. Sheldon, E. Shin, T. Sifón, C. Smith, M. Soares-Santos, M. Suchyta, E. Swanson, M.E.C. Tarle, G. Thomas, D. Tucker, D.L. Varga, T.N. Weller, J. Wechsler, R.H. Wilkinson, R.D. Wollack, E.J. Xu, Z. David A. Dunlap Department of Astronomy & Astrophysics University of Toronto 50 St. George St. TorontoONM5S 3H4 Canada Canadian Institute for Theoretical Astrophysics University of Toronto 60 St. George St. TorontoONM5S 3H4 Canada Dunlap Institute of Astronomy & Astrophysics 50 St. George St. TorontoONM5S 3H4 Canada School of Earth and Space Exploration Arizona State University TempeAZ85287 United States Perimeter Institute for Theoretical Physics 31 Caroline Street N WaterlooONN2L 2Y5 Canada Department of Physics and Astronomy University of Southern California Los AngelesCA90007 United States Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive HonoluluHI96822 United States Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Berkeley Center for Cosmological Physics 341 Campbell Hall University of California BerkeleyCA94720 United States Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States Cerro Tololo Inter-American Observatory NSF's National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Department of Astronomy and Astrophysics University of Chicago 5640 S. Ellis Ave. ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Department of Astronomy Cornell University IthacaNY14853 United States CNRS UMR 7095 Institut d'Astrophysique de Paris ParisF-75014 Fra

The cosmic web contains filamentary structure on a wide range of scales. On the largest scales, superclustering aligns multiple galaxy clusters along inter-cluster bridges, visible through their thermal Sunyaev-Zel'dovich signal in the Cosmic Microwave Background. We demonstrate a new, flexible method to analyze the hot gas signal from multi-scale extended structures. We use a Compton-y map from the Atacama Cosmology Telescope (ACT) stacked on redMaPPer cluster positions from the optical Dark Energy Survey (DES). Cutout images from the y map are oriented with large-scale structure information from DES galaxy data such that the superclustering signal is aligned before being overlaid. We find evidence for an extended quadrupole moment of the stacked y signal at the 3.5σ level, demonstrating that the large-scale thermal energy surrounding galaxy clusters is anisotropically distributed. We compare our ACT×DES results with the Buzzard simulations, finding broad agreement. Using simulations, we highlight the promise of this novel technique for constraining the evolution of anisotropic, non-Gaussian structure using future combinations of microwave and optical surveys. Copyright © 2021, The Authors. All rights reserved.

关键词： Telescopes

来源：评论

学校读者我要写书评

暂无评论

Euclid: Early Release Observations – A preview of the Euclid era through a galaxy cluster magnifying lens

arXiv

引用

arXiv 2024年

作者： Atek, Hakim Gavazzi, R. Weaver, J.R. Diego, J.M. Schrabback, T. Hatch, N.A. Aghanim, N. Dole, H. Hartley, W.G. Taamoli, S. Congedo, G. Jimenez-Teja, Y. Cuillandre, J.-C. Bañados, E. Belladitta, S. Bowler, R.A.A. Franco, M. Jauzac, M. Mahler, G. Richard, J. Rocci, P.-F. Serjeant, S. Toft, S. Abriola, D. Bergamini, P. Biviano, A. Dimauro, P. Ezziati, M. Golden-Marx, J.B. Grillo, C. Hughes, A.C.N. Kang, Y. Kneib, J.-P. Lombardi, M. Mamon, G.A. McPartland, C.J.R. Meneghetti, M. Miyatake, H. Montes, M. Mortlock, D.J. Oesch, P.A. Okabe, N. Rosati, P. Taylor, A.N. Tarsitano, F. Weller, J. Kluge, M. Laureijs, R. Paltani, S. Saifollahi, T. Schirmer, M. Stone, C. Mora, A. Altieri, B. Amara, A. Andreon, S. Auricchio, N. Baldi, M. Balestra, A. Bardelli, S. Basset, A. Bender, R. Bodendorf, C. Bonino, D. Branchini, E. Brescia, M. Brinchmann, J. Camera, S. Candini, G.P. Capobianco, V. Carbone, C. Cardone, V.F. Carretero, J. Casas, S. Castander, F.J. Castellano, M. Cavuoti, S. Cimatti, A. Conselice, C.J. Conversi, L. Copin, Y. Corcione, L. Courbin, F. Courtois, H.M. Da Silva, A. Degaudenzi, H. Di Giorgio, A.M. Dinis, J. Douspis, M. Dubath, F. Dupac, X. Dusini, S. Ealet, A. Farina, M. Farrens, S. Ferriol, S. Fotopoulou, S. Frailis, M. Franceschi, E. Galeotta, S. Gillard, W. Gillis, B. Giocoli, C. Gómez-Alvarez, P. Grazian, A. Grupp, F. Guzzo, L. Hailey, M. Haugan, S.V.H. Hoar, J. Hoekstra, H. Holliman, M.S. Holmes, W. Hook, I. Hormuth, F. Hornstrup, A. Hudelot, P. Jahnke, K. Jhabvala, M. Keihänen, E. Kermiche, S. Kiessling, A. Kitching, T. Kohley, R. Kubik, B. Kuijken, K. Kümmel, M. Kunz, M. Kurki-Suonio, H. Lahav, O. Le Mignant, D. Ligori, S. Lilje, P.B. Lindholm, V. Lloro, I. Maino, D. Maiorano, E. Mansutti, O. Marggraf, O. Markovic, K. Martinet, N. Marulli, F. Massey, R. Maurogordato, S. McCracken, H.J. Mei, S. Mellier, Y. Merlin, E. Meylan, G. Moresco, M. Moscardini, L. Nakajima, R. Nichol, R.C. Institut d’Astrophysique de Paris UMR 7095 CNRS Sorbonne Université 98 bis boulevard Arago Paris75014 France Aix-Marseille Université CNRS CNES LAM Marseille France Department of Astronomy University of Massachusetts AmherstMA01003 United States Instituto de Física de Cantabria Edificio Juan Jordá Avenida de los Castros Santander39005 Spain Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstr. 25/8 Innsbruck6020 Austria School of Physics and Astronomy University of Nottingham University Park NottinghamNG7 2RD United Kingdom Université Paris-Saclay CNRS Institut d’astrophysique spatiale Orsay91405 France Department of Astronomy University of Geneva ch. d’Ecogia 16 Versoix1290 Switzerland Physics and Astronomy Department University of California 900 University Ave. RiversideCA92521 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía Granada18080 Spain Observatorio Nacional Rua General Jose Cristino 77-Bairro Imperial de Sao Cristovao Rio de Janeiro20921-400 Brazil Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-Yvette91191 France Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 Bologna40129 Italy Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom The University of Texas at Austin AustinTX78712 United States Department of Physics Centre for Extragalactic Astronomy Durham University South Road DH1 3LE United Kingdom Department of Physics Institute for Computational Cosmology Durham University South Road DH1 3LE United Kingdom Astrophysics Research Centre University of KwaZulu-Natal Westville Campus Durban4041 South Africa School of

We present the first analysis of the Euclid Early Release Observations (ERO) program that targets fields around two lensing clusters, Abell 2390 and Abell 2764. We use VIS and NISP imaging to produce photometric catalogs for a total of ∼ 500 000 objects. The imaging data reach a 5 σ typical depth in the range 25.1–25.4 AB in the NISP bands, and 27.1–27.3 AB in the VIS band. Using the Lyman-break method in combination with photometric redshifts, we search for high-redshift galaxies. We identify 30 Lyman-break galaxy (LBG) candidates at z > 6 and 139 extremely red sources (ERSs), most likely at lower redshift. The deeper VIS imaging compared to NISP means we can routinely identify high-redshift Lyman breaks of the order of 3 magnitudes, which reduces contamination by brown dwarf stars and low-redshift galaxies. The difficulty of spatially resolving most of these sources in 0′′ . 3 pix−1 imaging makes the distinction between galaxies and quasars more challenging. Spectroscopic followup campaigns of such bright sources will help constrain both the bright end of the ultraviolet galaxy luminosity function and the quasar luminosity function at z > 6, and constrain the physical nature of these objects. Additionally, we have performed a combined strong lensing and weak lensing analysis of A2390, and demonstrate how Euclid will contribute to better constraining the virial mass of galaxy clusters. From these data, we also identify optical and near-infrared counterparts of known z > 0.6 clusters, which exhibit strong lensing features, establishing the ability of Euclid to characterize high-redshift clusters. Finally, we provide a glimpse of Euclid’s ability to map the intracluster light out to larger radii than current facilities, enabling a better understanding of the cluster assembly history and mapping of the dark matter distribution. This initial dataset illustrates the diverse spectrum of legacy science that will be enabled by the Euclid survey. © 2024, CC BY.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

The atacama cosmology telescope: Delensed power spectra and parameters

arXiv

引用

arXiv 2020年

作者： Han, Dongwon Sehgal, Neelima MacInnis, Amanda van Engelen, Alexander Sherwin, Blake D. Madhavacheril, Mathew S. Aiola, Simone Battaglia, Nicholas Beall, James A. Becker, Daniel T. Calabrese, Erminia Choi, Steve K. Darwish, Omar Denison, Edward V. Devlin, Mark J. Dunkley, Jo Ferraro, Simone Fox, Anna E. Hasselfield, Matthew Hill, J. Colin Hilton, Gene C. Hilton, Matt Hložek, Renée Hubmayr, Johannes Hughes, John P. Kosowsky, Arthur van Lanen, Jeff Louis, Thibaut Moodley, Kavilan Naess, Sigurd Namikawa, Toshiya Nati, Federico Nibarger, John P. Niemack, Michael D. Page, Lyman A. Partridge, Bruce Qu, Frank J. Schillaci, Alessandro Spergel, David N. Staggs, Suzanne Storer, Emilie Wollack, Edward J. Physics and Astronomy Department Stony Brook University Stony BrookNY11794 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States School of Earth and Space Exploration Arizona State University TempeAZ85287 United States Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road CambridgeCB3 0WA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 OHA United Kingdom Centre for the Universe Perimeter Institute for Theoretical Physics WaterlooONN2L 2Y5 Canada Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Astronomy Cornell University IthacaNY14853 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States School of Physics and Astronomy Cardiff University The Parade Cardiff WalesCF24 3AA United Kingdom Department of Physics Cornell University IthacaNY14853 United States Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Berkeley Center for Cosmological Physics Department of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory One Cyclotron Road BerkeleyCA94720 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics Columbia University New YorkNY10027 United States Astrophysics Research Centre School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa David A. Dunlap Department of Astronomy and

We present ΛCDM cosmological parameter constraints obtained from delensed microwave background power spectra. Lensing maps from a subset of DR4 data from the Atacama Cosmology Telescope (ACT) are used to undo the lensing effect in ACT spectra observed at 150 and 98 GHz. At 150 GHz, we remove the lensing distortion with an effective efficiency of 30% (TT), 30% (EE), 26% (TE) and 20% (BB);this results in detections of the delensing effect at 8.7σ (TT), 5.1σ (EE), 2.6σ (TE), and 2.4σ (BB) significance. The combination of 150 and 98 GHz TT, EE, and TE delensed spectra is well fit by a standard ΛCDM model. We also measure the shift in best-fit parameters when fitting delensed versus lensed spectra;while this shift does not inform our ability to measure cosmological parameters, it does provide a three-way consistency check among the lensing inferred from the best-fit parameters, the lensing in the CMB power spectrum, and the reconstructed lensing map. This shift is predicted to be zero when fitting with the correct model since both lensed and delensed spectra originate from the same region of sky. Fitting with a ΛCDM model and marginalizing over foregrounds, we find that the shift in cosmological parameters is consistent with zero. Our results show that gravitational lensing of the microwave background is internally consistent within the framework of the standard cosmological model. Copyright © 2020, The Authors. All rights reserved.

关键词： Power spectrum

来源：评论

学校读者我要写书评

暂无评论

Causes of blindness and vision impairment in 2020 and trends over 30 years, and prevalence of avoidable blindness in relation to VISION 2020: the Right to Sight: an analysis for the Global Burden of Disease Study (vol 2, pg 144, 2021)

引用

LANCET GLOBAL HEALTH 2021年第4期9卷 E408-E408页

作者： Steinmetz, Jaimie D. Vision and Eye Research Institute Anglia Ruskin University Cambridge United Kingdom Biomedical Informatics Seoul National University Hospital Seoul South Korea Institute for Health Metrics and Evaluation University of Washington Seattle WA United States Department of Health Metrics Sciences School of Medicine University of Washington Seattle WA United States Institute of Health Services Research Yonsei University Seoul South Korea Department of Ophthalmology University of Washington Seattle WA United States Department of Mathematics Imperial College London London United Kingdom WHO Collaborating Centre for Public Health Education and Training Imperial College London London United Kingdom Department of Primary Care and Public Health Imperial College London London United Kingdom School of Population and Global Health University of Melbourne Carlton VIC Australia School of Optometry and Vision Science UNSW Sydney NSW Australia Brien Holden Vision Institute Sydney Australia Department of Ophthalmology University of Adelaide Adelaide SA Australia Department of Parasitology and Mycology Jahrom University of Medical Sciences Jahrom Iran Department of Clinical Sciences University of Sharjah Sharjah United Arab Emirates Ophthalmic Research Center Shahid Beheshti University of Medical Sciences Tehran Iran Department of Ophthalmology Shahid Beheshti University of Medical Sciences Tehran Iran Research Institute for Endocrine Sciences Shahid Beheshti University of Medical Sciences Tehran Iran Ophthalmic Epidemiology Research Center Shahid Beheshti University of Medical Sciences Tehran Iran Health Services Management Department Qazvin University of Medical Sciences Qazvin Iran Department of Systems Populations and Leadership University of Michigan Ann Arbor MI United States Department of Medicine Sofia Ismail Memorial Medical Centre Bogura Bangladesh The Fred Hollows Foundation Sydney NSW Australia Berhan Public Health & Eye Care Consultancy Addis A

Hospital El Salvador: a novel paradigm of intensive care in response to COVID-19 in central America. Lancet Glob Health 2021;9: e241?42?In this Comment, the conflict of interest statement should have included the following: ?By virtue of their roles within a public hospital or the Ministry of Health, MB, LC, WH, and XS are government employees. The findings and conclusions in the Comment are only those of the authors.? This correction has been made as of Feb 26, 2021.

关键词：

来源：评论

学校读者我要写书评

暂无评论

The LOFAR Two-metre Sky Survey V. Second data release

arXiv

引用

arXiv 2022年

作者： Shimwell, Timothy W. Hardcastle, M.J. Tasse, C. Best, P.N. Röttgering, H.J.A. Williams, W.L. Botteon, A. Drabent, A. Mechev, A. Shulevski, A. van Weeren, R.J. Bester, L. Brüggen, M. Brunetti, G. Callingham, J.R. Chyzy, K.T. Conway, J.E. Dijkema, T.J. Duncan, K. de Gasperin, F. Hale, C.L. Haverkorn, M. Hugo, B. Jackson, N. Mevius, M. Miley, G.K. Morabito, L.K. Morganti, R. Offringa, A. Oonk, J.B.R. Rafferty, D. Sabater, J. Smith, D.J.B. Schwarz, D.J. Smirnov, O. O’Sullivan, S.P. Vedantham, H. White, G.J. Albert, J.G. Alegre, L. Asabere, B. Bacon, D.J. Bonafede, A. Bonnassieux, E. Brienza, M. Bilicki, M. Bonato, M. Calistro Rivera, G. Cassano, R. Cochrane, R. Croston, J.H. Cuciti, V. Dallacasa, D. Danezi, A. Dettmar, R.J. Di Gennaro, G. Edler, H.W. Enßlin, T.A. Emig, K.L. Franzen, T.M.O. García-Vergara, C. Grange, Y.G. Gürkan, G. Hajduk, M. Heald, G. Heesen, V. Hoang, D.N. Hoeft, M. Horellou, C. Iacobelli, M. Jamrozy, M. Jelić, V. Kondapally, R. Kukreti, P. Kunert-Bajraszewska, M. Magliocchetti, M. Mahatma, V. Malek, K. Mandal, S. Massaro, F. Meyer-Zhao, Z. Mingo, B. Mostert, R.I.J. Nair, D.G. Nakoneczny, S.J. Nikiel-Wroczynski, B. Orrú, E. Pajdosz-Smierciak, U. Pasini, T. Prandoni, I. van Piggelen, H.E. Rajpurohit, K. Retana-Montenegro, E. Riseley, C.J. Rowlinson, A. Saxena, A. Schrijvers, C. Sweijen, F. Siewert, T.M. Timmerman, R. Vaccari, M. Vink, J. West, J.L. Wolowska, A. Zhang, X. Zheng, J. ASTRON The Netherlands Institute for Radio Astronomy Oude Hoogeveensedijk 4 Dwingeloo 7991 PD Netherlands Leiden Observatory Leiden University PO Box 9513 LeidenNL-2300 RA Netherlands Centre for Astrophysics Research School of Physics Astronomy and Mathematics University of Hertfordshire College Lane Hatfield AL10 9AB United Kingdom GEPI Observatoire de Paris Université PSL CNRS 5 Place Jules Janssen Meudon 92190 France Department of Physics & Electronics Rhodes University PO Box 94 Grahamstown 6140 South Africa School of Physics and Astronomy Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Thüringer Landessternwarte Sternwarte 5 Tautenburg D-07778 Germany 2 Fir Street Black River Business Park Observatory Cape Town South Africa Hamburger Sternwarte University of Hamburg Gojenbergsweg 112 Hamburg21029 Germany INAF Istituto di Radioastronomia via P. Gobetti 101 Bologna40129 Italy Astronomical Observatory Jagiellonian University ul. Orla 171 Kraków30-244 Poland Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala439 92 Sweden Department of Astrophysics IMAPP Radboud University Nijmegen P.O. Box 9010 Nijmegen6500 GL Netherlands Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy School of Natural Sciences University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Centre for Extragalactic Astronomy Department of Physics Durham University DurhamDH1 3LE United Kingdom Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands SURF P.O.Box 94613 AmsterdamNL-1090 GP Netherlands Fakultät für Physik Universität Bielefeld Postfach 100131 Bielefeld33501 Germany School of Physical Sciences and Centre for Astrophysics & R

In this data release from the ongoing LOw-Frequency ARray (LOFAR) Two-metre Sky Survey (LoTSS) we present 120-168 MHz images covering 27% of the northern sky. Our coverage is split into two regions centred at approximately 12h45m +44◦30′ and 1h00m +28◦00′ and spanning 4178 and 1457 square degrees respectively. The images were derived from 3,451 hrs (7.6 PB) of LOFAR High Band Antenna data which were corrected for the direction-independent instrumental properties as well as direction-dependent ionospheric distortions during extensive, but fully automated, data processing. A catalogue of 4,396,228 radio sources is derived from our total intensity (Stokes I) maps, where the majority of these have never been detected at radio wavelengths before. At 6″ resolution, our full bandwidth Stokes I continuum maps with a central frequency of 144 MHz have: a median rms sensitivity of 83 µJy/beam;a flux density scale accuracy of approximately 10%;an astrometric accuracy of 0.2″;and we estimate the point-source completeness to be 90% at a peak brightness of 0.8 mJy/beam. By creating three 16 MHz bandwidth images across the band we are able to measure the in-band spectral index of many sources, albeit with an error on the derived spectral index of > ±0.2 which is a consequence of our flux-density scale accuracy and small fractional bandwidth. Our circular polarisation (Stokes V) 20″ resolution 120-168 MHz continuum images have a median rms sensitivity of 95 µJy/beam, and we estimate a Stokes I to Stokes V leakage of 0.056%. Our linear polarisation (Stokes Q and Stokes U) image cubes consist of 480 × 97.6 kHz wide planes and have a median rms sensitivity per plane of 10.8 mJy/beam at 4′ and 2.2 mJy/beam at 20″;we estimate the Stokes I to Stokes Q/U leakage to be approximately 0.2%. Here we characterise and publicly release our Stokes I, Q, U and V images in addition to the calibrated uv-data to facilitate the thorough scientific exploitation of this unique dataset. Copyright © 2022,

关键词： Surveys

来源：评论

学校读者我要写书评

暂无评论

The Atacama Cosmology Telescope: A catalog of > 4000 Sunyaev-Zel'dovich galaxy clusters

arXiv

引用

arXiv 2020年

作者： Hilton, Matthew Sifón, C. Naess, S. Madhavacheril, M. Oguri, M. Rozo, E. Rykoff, E. Abbott, T.M.C. Adhikari, S. Aguena, M. Aiola, S. Allam, S. Amodeo, S. Amon, A. Annis, J. Ansarinejad, B. Aros-Bunster, C. Austermann, J.E. Avila, S. Bacon, D. Battaglia, N. Beall, J.A. Becker, D.T. Bernstein, G.M. Bertin, E. Bhandarkar, T. Bhargava, S. Bond, J.R. Brooks, D. Burke, D.L. Calabrese, E. Carretero, J. Choi, S.K. Choi, A. Conselice, C. da Costa, L.N. Costanzi, M. Crichton, D. Crowley, K.T. Dünner, R. Denison, E.V. Devlin, M.J. Dicker, S.R. Diehl, H.T. Dietrich, J.P. Doel, P. Duff, S.M. Duivenvoorden, A.J. Dunkley, J. Everett, S. Ferraro, S. Ferrero, I. Ferté, A. Flaugher, B. Frieman, J. Gallardo, P.A. García-Bellido, J. Gaztanaga, E. Gerdes, D.W. Giles, P. Golec, J.E. Gralla, M.B. Grandis, S. Gruen, D. Gruendl, R.A. Gschwend, J. Gutierrez, G. Han, D. Hartley, W.G. Hasselfield, M. Hill, J.C. Hilton, G.C. Hincks, A.D. Hinton, S.R. Ho, S.-P.P. Honscheid, K. Hoyle, B. Hubmayr, J. Huffenberger, K.M. Hughes, J.P. Jaelani, A.T. Jain, B. James, D.J. Jeltema, T. Kent, S. Carrasco Kind, M. Knowles, K. Koopman, B.J. Kuehn, K. Lahav, O. Lima, M. Lin, Y.-T. Lokken, M. Loubser, S.I. MacCrann, N. Maia, M.A.G. Marriage, T.A. Martin, J. McMahon, J. Melchior, P. Menanteau, F. Miquel, R. Miyatake, H. Moodley, K. Morgan, R. Mroczkowski, T. Nati, F. Newburgh, L.B. Niemack, M.D. Nishizawa, A.J. Ogando, R.L.C. Orlowski-Scherer, J. Page, L.A. Palmese, A. Partridge, B. Paz-Chinchón, F. Phakathi, P. Plazas, A.A. Robertson, N.C. Romer, A.K. Carnero Rosell, A. Salatino, M. Sanchez, E. Schaan, E. Schillaci, A. Sehgal, N. Serrano, S. Shin, T. Simon, S.M. Smith, M. Soares-Santos, M. Spergel, D.N. Staggs, S.T. Storer, E.R. Suchyta, E. Swanson, M.E.C. Tarle, G. Thomas, D. To, C. Trac, H. Ullom, J.N. Vale, L.R. van Lanen, J. Vavagiakis, E.M. de Vicente, J. Wilkinson, R.D. Wollack, E.J. Xu, Z. Zhang, Y. Astrophysics Research Centre University of KwaZulu-Natal Westville Campus Durban4041 South Africa School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Instituto de Física Pontificia Universidad Católica de Valparaíso Casilla Valparaíso4059 Chile Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Centre for the Universe Perimeter Institute for Theoretical Physics WaterlooONN2L 2Y5 Canada Research Center for the Early Universe University of Tokyo Tokyo113-0033 Japan Department of Physics University of Tokyo Tokyo113-0033 Japan University of Tokyo Chiba277-8582 Japan Department of Physics University of Arizona TucsonAZ85721 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Cerro Tololo Inter-American Observatory NSF's National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States Departamento de Física Matemática Instituto de Física Universidade de São Paulo CP 66318 São Paulo SP05314-970 Brazil Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Astronomy Cornell University IthacaNY14853 United States Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Quantum Sensors Group NIST 325 Broadway BoulderCO80305 United States Instituto de Fisica Teorica UAM CSIC Universidad Autonoma de Madrid Madrid28049 Spain Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Department of Physics and Astronomy University of Pennsylvania Ph

We present a catalog of 4195 optically confirmed Sunyaev-Zel'dovich (SZ) selected galaxy clusters detected with signal-to-noise > 4 in 13,211 deg2 of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multi-frequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008-2018, and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ-signal vs. mass scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M500c > 3.8 × 1014 M☉, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio > 5 in maps filtered at an angular scale of 2.40. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ-signal mass-scaling relation, such as the Dark Energy Survey (4566 deg2), the Hyper Suprime-Cam Subaru Strategic Program (469 deg2), and the Kilo Degree Survey (825 deg2). We highlight some noteworthy objects in the sample, including potentially projected systems;clusters with strong lensing features;clusters with active central galaxies or star formation;and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses, and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr. Copyright © 2020, The Authors. All rights reserved.

关键词： Surveys

来源：评论

学校读者我要写书评

暂无评论

The atacama cosmology telescope: weighing distant clusters with the most ancient light

arXiv

引用

arXiv 2020年

作者： Madhavacheril, Mathew S. Sifón, Cristóbal Battaglia, Nicholas Aiola, Simone Amodeo, Stefania Austermann, Jason E. Beall, James A. Becker, Daniel T. Bond, J. Richard Calabrese, Erminia Choi, Steve K. Denison, Edward V. Devlin, Mark J. Dicker, Simon R. Duff, Shannon M. Duivenvoorden, Adriaan J. Dunkley, Jo Dünner, Rolando Ferraro, Simone Gallardo, Patricio A. Guan, Yilun Han, Dongwon Hill, J. Colin Hilton, Gene C. Hilton, Matt Hubmayr, Johannes Huffenberger, Kevin M. Hughes, John P. Koopman, Brian J. Kosowsky, Arthur van Lanen, Jeff Lee, Eunseong Louis, Thibaut MacInnis, Amanda McMahon, Jeffrey Moodley, Kavilan Naess, Sigurd Namikawa, Toshiya Nati, Federico Newburgh, Laura Niemack, Michael D. Page, Lyman A. Partridge, Bruce Qu, Frank J. Robertson, Naomi C. Salatino, Maria Schaan, Emmanuel Schillaci, Alessandro Schmitt, Benjamin L. Sehgal, Neelima Sherwin, Blake D. Simon, Sara M. Spergel, David N. Staggs, Suzanne Storer, Emilie R. Ullom, Joel N. Vale, Leila R. van Engelen, Alexander Vavagiakis, Eve M. Wollack, Edward J. Xu, Zhilei Centre for the Universe Perimeter Institute WaterlooONN2L 2Y5 Canada Instituto de Física Pontificia Universidad Católica de Valparaíso CasillaValparaíso4059 Chile Department of Astronomy Cornell University IthacaNY14853 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Canadian Institute for Theoretical Astrophysics University of Toronto 60 St. George Street TorontoONM5S 3H8 Canada School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Department of Physics Cornell University IthacaNY14853 United States Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Instituto de Astrofísica Centro de Astro-Ingeniería Facultad de Física Pontificia Universidad Católica de Chile Av. Vicuña Mackenna 4860 SantiagoMacul7820436 Chile Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics and Astronomy University of Pittsburgh PittsburghPA15260 United States Physics and Astronomy Department Stony Brook University Stony BrookNY11794 United States Department of Physics Columbia University 550 West 120th Street New YorkNY10027 United States Astrophysics Research Centre University of KwaZulu-Natal Westville Campus Durban4041 South Africa School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Department of Physics Florida State University TallahasseeFL32306 United States Department of Physics and Astronomy Rutgers University 136 Frelinghuysen Road PiscatawayNJ08854-

We use gravitational lensing of the cosmic microwave background (CMB) to measure the mass of the most distant blindly-selected sample of galaxy clusters on which a lensing measurement has been performed to date. In CMB data from the the Atacama Cosmology Telescope (ACT) and the Planck satellite, we detect the stacked lensing effect from 677 near-infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS), which have a mean redshift of hzi = 1.08. There are no current optical weak lensing measurements of clusters that match the distance and average mass of this sample. We detect the lensing signal with a significance of 4.2σ. We model the signal with a halo model framework to find the mean mass of the population from which these clusters are drawn. Assuming that the clusters follow Navarro-Frenk-White density profiles, we infer a mean mass of hM500ci = (1.7 ± 0.4) × 1014 M. We consider systematic uncertainties from cluster redshift errors, centering errors, and the shape of the NFW profile. These are all smaller than 30% of our reported uncertainty. This work highlights the potential of CMB lensing to enable cosmological constraints from the abundance of distant clusters populating ever larger volumes of the observable Universe, beyond the capabilities of optical weak lensing measurements. Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

Euclid: Early Release Observations The intracluster light of Abell 2390

引用

Astronomy and Astrophysics 2025年第1期698卷

作者： Ellien, A. Montes, M. Ahad, S.L. Dimauro, P. Golden-Marx, J.B. Jimenez-Teja, Y. Durret, F. Bellhouse, C. Diego, J.M. Bamford, S.P. Gonzalez, A.H. Hatch, N.A. Kluge, M. Ragusa, R. Slezak, E. Cuillandre, J.-C. Gavazzi, R. Dole, H. Mahler, G. Congedo, G. Saifollahi, T. Aghanim, N. Altieri, B. Amara, A. Andreon, S. Auricchio, N. Baccigalupi, C. Baldi, M. Balestra, A. Bardelli, S. Basset, A. Battaglia, P. Biviano, A. Bonchi, A. Bonino, D. Branchini, E. Brescia, M. Brinchmann, J. Caillat, A. Camera, S. Capobianco, V. Carbone, C. Cardone, V.F. Carretero, J. Casas, S. Castellano, M. Castignani, G. Cavuoti, S. Cimatti, A. Colodro-Conde, C. Conselice, C.J. Conversi, L. Copin, Y. Courbin, F. Courtois, H.M. Cropper, M. Silva, A. Da Degaudenzi, H. De Lucia, G. Giorgio, A.M. Di Dinis, J. Dubath, F. Duncan, C.A.J. Dupac, X. Dusini, S. Farina, M. Faustini, F. Ferriol, S. Fotopoulou, S. Frailis, M. Franceschi, E. Galeotta, S. George, K. Gillis, B. Giocoli, C. Gómez-Alvarez, P. Grazian, A. Grupp, F. Guzzo, L. Haugan, S.V.H. Hoar, J. Hoekstra, H. Holmes, W. Hormuth, F. Hornstrup, A. Hudelot, P. Jahnke, K. Jhabvala, M. Joachimi, B. Keihänen, E. Kermiche, S. Kiessling, A. Kubik, B. Kuijken, K. Kümmel, M. Kunz, M. Kurki-Suonio, H. Laureijs, R. Le Mignant, D. Ligori, S. Lilje, P.B. Lindholm, V. Lloro, I. Mainetti, G. Maino, D. Maiorano, E. Mansutti, O. Marcin, S. Marggraf, O. Markovic, K. Martinelli, M. Martinet, N. Marulli, F. Massey, R. Maurogordato, S. Medinaceli, E. Mei, S. Melchior, M. Mellier, Y. Meneghetti, M. Merlin, E. Meylan, G. Mora, A. Moresco, M. Moscardini, L. Nakajima, R. Neissner, C. Nichol, R.C. Niemi, S.-M. Nightingale, J.W. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Percival, W.J. Pettorino, V. Pires, S. Polenta, G. Poncet, M. Popa, L.A. Pozzetti, L. Raison, F. Rebolo, R. Renzi, A. Rhodes, J. Riccio, G. Romelli, E. Roncarelli, M. Rossetti, E. Saglia, R. Sakr, Z. Sapone, D. Sartoris, B. Scaramella, R. Schirmer, M. Schneider, P. Schrabback, T. Secroun, A. Sefusatti, E. Seidel, G. Seiffert, M. Serrano, S. Sirignano OCA P.H.C Boulevard de l’Observatoire CS 34229 Nice Cedex 4 06304 France Institute of Space Sciences (ICE CSIC) Campus UAB Carrer de Can Magrans s/n Barcelona 08193 Spain Instituto de Astrofísica de Canarias Vía Láctea Tenerife La Laguna 38205 Spain Universidad de La Laguna Departamento de Astrofísica Tenerife La Laguna 38206 Spain Waterloo Centre for Astrophysics University of Waterloo Waterloo N2L 3G1 ON Canada Department of Physics and Astronomy University of Waterloo Waterloo N2L 3G1 ON Canada INAF-Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone 00078 Italy Observatorio Nacional Rua General Jose Cristino 77-Bairro Imperial de Sao Cristovao Rio de Janeiro 20921-400 Brazil School of Physics and Astronomy University of Nottingham University Park Nottingham NG7 2RD United Kingdom Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía Granada 18080 Spain Institut d’Astrophysique de Paris 98bis Boulevard Arago Paris 75014 France Instituto de Física de Cantabria Edificio Juan Jordá Avenida de los Castros Santander 39005 Spain Department of Astronomy University of Florida Bryant Space Science Center Gainesville 32611 FL United States Max Planck Institute for Extraterrestrial Physics Giessenbachstr. 1 Garching 85748 Germany INAF-Osservatorio Astronomico di Capodimonte Via Moiariello 16 Napoli 80131 Italy Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Laboratoire Lagrange Bd de l’Observatoire CS 34229 Nice cedex 4 06304 France Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-Yvette 91191 France Aix-Marseille Université CNRS CNES LAM Marseille France Institut d’Astrophysique de Paris UMR 7095 CNRS Sorbonne Université 98 bis boulevard Arago Paris 75014 France Université Paris-Saclay CNRS Institut d’astrophysique spatiale Orsay 91405 France STAR Institute Quartier Agora – Allée du six Août Liège B-4000 Belgium Department of Physics Centre for Extragal

Intracluster light (ICL) provides a record of the dynamical interactions undergone by clusters, giving clues on cluster formation and evolution. Here, we analyse the properties of ICL in the massive cluster Abell 2390 at redshift z = 0.228. Our analysis is based on the deep images obtained by the Euclid mission as part of the Early Release Observations in the near-infrared (Y_E, J_E, H_E bands), using the NISP instrument in a 0.75 deg² field. We subtracted a point–spread function (PSF) model and removed the Galactic cirrus contribution in each band after modelling it with the DAWIS software. We then applied three methods to detect, characterise, and model the ICL and the brightest cluster galaxy (BCG): the CICLE 2D multi-galaxy fitting;the DAWIS wavelet-based multiscale software;and a mask-based 1D profile fitting. We detect ICL out to 600 kpc. The ICL fractions derived by our three methods range between 18% and 36% (average of 24%), while the BCG+ICL fractions are between 21% and 41% (average of 29%), depending on the band and method. A galaxy density map based on 219 selected cluster members shows a strong cluster substructure to the south-east and a smaller feature to the north-west. Ellipticals dominate the cluster’s central region, with a centroid offset from the BCG by about 70 kpc and distribution following that of the ICL, while spirals do not trace the entire ICL but rather substructures. The comparison of the BCG+ICL, mass from gravitational lensing, and X-ray maps show that the BCG+ICL is the best tracer of substructures in the cluster. Based on colours, the ICL (out to about 400 kpc) seems to be built by the accretion of small systems (M ∼ 10^9.5 M ), or from stars coming from the outskirts of Milky Way-type galaxies (M ∼ 10¹⁰ M ). Though Abell 2390 does not seem to be undergoing a merger, it is not yet fully relaxed, since it has accreted two groups that have not fully merged with the cluster

关键词： galaxies: clusters: general galaxies: clusters: individual: Abell 2390 galaxies: clusters: intracluster medium

来源：评论

学校读者我要写书评

暂无评论

The Atacama Cosmology Telescope: A CMB lensing mass map over 2100 square degrees of sky and its cross-correlation with BOSS-CMASS galaxies

arXiv

引用

arXiv 2020年

作者： Darwish, Omar Madhavacheril, Mathew S. Sherwin, Blake D. Aiola, Simone Battaglia, Nicholas Beall, James A. Becker, Daniel T. Bond, J. Richard Calabrese, Erminia Choi, Steve Devlin, Mark J. Dunkley, Jo Dünner, Rolando Ferraro, Simone Fox, Anna E. Gallardo, Patricio A. Guan, Yilun Halpern, Mark Han, Dongwon Hasselfield, Matthew Hill, J. Colin Hilton, Gene C. Hilton, Matt Hincks, Adam D. Ho, Shuay-Pwu Patty Hubmayr, J. Hughes, John P. Koopman, Brian J. Kosowsky, Arthur van Lanen, J. Louis, Thibaut Lungu, Marius MacInnis, Amanda Maurin, Loïc McMahon, Jeffrey Moodley, Kavilan Naess, Sigurd Namikawa, Toshiya Newburgh, Laura Nibarger, John P. Niemack, Micheal D. Page, Lyman A. Partridge, Bruce Qu, Frank J. Robertson, Naomi Schmitt, Benjamin Sehgal, Neelima Sifón, Cristóbal Spergel, David N. Staggs, Suzanne Storer, Emilie van Engelen, Alexander Wollack, Edward J. Center for Theoretical Cosmology DAMTP University of Cambridge CB3 0WA United Kingdom Centre for the Universe Perimeter Institute WaterlooONN2L 2Y5 Canada Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics Columbia University 550 West 120th Street New YorkNY10027 United States Department of Physics and Astronomy Haverford College HaverfordPA19041 United States Physics and Astronomy Department Stony Brook University Stony BrookNY11794 United States NASA/Goddard Space Flight Center GreenbeltMD20771 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States School of Natural Sciences Institute for Advanced Study PrincetonNJ08540 United States Institute of Astronomy Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 OHA United Kingdom NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics and Astronomy University of Pittsburgh PittsburghPA15260 United States Université Paris-Saclay CNRS/IN2P3 IJCLab Orsay91405 France School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Université Paris-Saclay CNRS Institut d’astrophysique spatiale Orsay91405 France Department of Physics Cornell University IthacaNY14853 United States Department of Astronomy Cornell University IthacaNY14853 Un

We construct cosmic microwave background lensing mass maps using data from the 2014 and 2015 seasons of observations with the Atacama Cosmology Telescope (ACT). These maps cover 2100 square degrees of sky and overlap with a wide variety of optical surveys. The maps are signal dominated on large scales and have fidelity such that their correlation with the cosmic infrared background is clearly visible by eye. We also create lensing maps with thermal Sunyaev-Zel’dovich contamination removed using a novel cleaning procedure that only slightly degrades the lensing signal-to-noise ratio. The cross-spectrum between the cleaned lensing map and the BOSS CMASS galaxy sample is detected at 10-σ significance, with an amplitude of A = 1.02±0.10 relative to the Planck best-fit LCDM cosmological model with fiducial linear galaxy bias. Our measurement lays the foundation for lensing cross-correlation science with current ACT data and beyond. Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

Guidelines for Developing Successful Short Advanced Courses in Systems Medicine and Systems Biology (vol 5, pg 168, 2017)

引用

CELL SYSTEMS 2017年第6期5卷 654-654页

作者： Gomez-Cabrero, David Marabita, Francesco Tarazona, Sonia Cano, Isaac Roca, Josep Conesa, Ana Sabatier, Philippe Tegner, Jesper Unit of Computational Medicine Department of Medicine Karolinska Institutet 171 77 Stockholm Sweden Center for Molecular Medicine Karolinska Institutet 171 77 Stockholm Sweden Unit of Clinical Epidemiology Department of Medicine Karolinska University Hospital L8 17176 Stockholm Sweden Science for Life Laboratory 17121 Solna Sweden Mucosal and Salivary Biology Division King’s College London Dental Institute London SE1 9RT UK Centro de Investigacion Principe Felipe 46012 Valencia Spain Department of Applied Statistics Operations Research and Quality Universitat Politècnica de València Camí de Vera 46022 Valencia Spain Hospital Clinic de Barcelona Institut d’Investigacions Biomèdiques August Pi i Sunyer (IDIBAPS) Universitat de Barcelona 08007 Barcelona Spain Center for Biomedical Network Research in Respiratory Diseases (CIBERES) 28029 Madrid Spain Microbiology and Cell Science Department Institute for Food and Agricultural Sciences University of Florida Gainesville FL 32603 USA TIMC-IMAG Laboratory UMR 5525 Centre National de la Recherche Scientifique Vetagro Sup Université Grenoble-Alpes 38400 Saint-Martin-d'Hères France Biological and Environmental Sciences and Engineering Division (BESE) Computer Electrical and Mathematical Sciences and Engineering Division (CEMSE) King Abdullah University of Science and Technology (KAUST) Thuwal 23955–6900 Kingdom of Saudi Arabia

Systems medicine and systems biology have inherent educational challenges. These have largely been addressed either by providing new masters programs or by redesigning undergraduate programs. In contrast, short courses can respond to a different need: they can provide condensed updates for professionals across academia, the clinic, and industry. These courses have received less attention. Here, we share our experiences in developing and providing such courses to current and future leaders in systems biology and systems medicine. We present guidelines for how to reproduce our courses, and we offer suggestions for how to select students who will nurture an interdisciplinary learning environment and thrive there.

关键词：

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：