The Square Kilometre Array (SKA)

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A spectroscopic, photometric, polarimetric, and radio study of the eclipsing polar UZ Fornacis: the first simultaneous SALT and MeerKAT observations

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 492:3 (2020) 4298-4312

Authors:

ZN Khangale, SB Potter, PA Woudt, DAH Buckley, AN Semena, EJ Kotze, DN Groenewald, DM Hewitt, ML Pretorius, RP Fender, P Groot, S Bloemen, M Klein-Wolt, E Körding, R Le Poole, VA McBride, L Townsend, K Paterson, DLA Pieterse, P Vreeswijk
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The Karl G. Jansky very large array sky survey (VLASS). Science case and survey design

Publications of the Astronomical Society of the Pacific 132:1009 (2020)

Authors:

M Lacy, SA Baum, CJ Chandler, S Chatterjee, TE Clarke, S Deustua, J English, J Farnes, BM Gaensler, N Gugliucci, G Hallinan, BR Kent, A Kimball, CJ Law, TJW Lazio, J Marvil, SA Mao, D Medlin, K Mooley, EJ Murphy, S Myers, R Osten, GT Richards, E Rosolowsky, L Rudnick, F Schinzel, GR Sivakoff, LO Sjouwerman, R Taylor, RL White, J Wrobel, H Andernach, AJ Beasley, E Berger, S Bhatnager, M Birkinshaw, GC Bower, WN Brandt, S Brown, S Burke-Spolaor, BJ Butler, J Comerford, PB Demorest, H Fu, S Giacintucci, K Golap, T Güth, CA Hales, R Hiriart, J Hodge

Abstract:

© 2020. The Astronomical Society of the Pacific. The Very Large Array Sky Survey (VLASS) is a synoptic, all-sky radio sky survey with a unique combination of high angular resolution (≈2.″5), sensitivity (a 1σ goal of 70 μJy/beam in the coadded data), full linear Stokes polarimetry, time domain coverage, and wide bandwidth (2–4 GHz). The first observations began in 2017 September, and observing for the survey will finish in 2024. VLASS will use approximately 5500 hr of time on the Karl G. Jansky Very Large Array (VLA) to cover the whole sky visible to the VLA (decl. > −40°), a total of 33 885 deg2. The data will be taken in three epochs to allow the discovery of variable and transient radio sources. The survey is designed to engage radio astronomy experts, multi-wavelength astronomers, and citizen scientists alike. By utilizing an “on the fly” interferometry mode, the observing overheads are much reduced compared to a conventional pointed survey. In this paper, we present the science case and observational strategy for the survey, and also results from early survey observations.
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Detection of very-high-energy γ-ray emission from the colliding wind binary η Car with H.E.S.S.

Astronomy & Astrophysics EDP Sciences 635 (2020) a167

Authors:

H Abdalla, R Adam, F Aharonian, F Ait Benkhali, EO Angüner, M Arakawa, C Arcaro, C Armand, T Armstrong, H Ashkar, M Backes, V Barbosa Martins, M Barnard, Y Becherini, D Berge, K Bernlöhr, R Blackwell, M Böttcher, C Boisson, J Bolmont, S Bonnefoy, J Bregeon, M Breuhaus, F Brun, P Brun, M Bryan, M Büchele, T Bulik, T Bylund, S Caroff, A Carosi, S Casanova, M Cerruti, T Chand, S Chandra, A Chen, S Colafrancesco, G Cotter, M Curyło, ID Davids, J Davies, C Deil, J Devin, P deWilt, L Dirson, A Djannati-Ataï, A Dmytriiev, A Donath, V Doroshenko, J Dyks, K Egberts, F Eichhorn, G Emery, J-P Ernenwein, S Eschbach, K Feijen, S Fegan, A Fiasson, G Fontaine, S Funk, M Füßling, S Gabici, YA Gallant, F Gaté, G Giavitto, L Giunti, D Glawion, JF Glicenstein, D Gottschall, M-H Grondin, J Hahn, M Haupt, G Heinzelmann, G Henri, G Hermann, JA Hinton, W Hofmann, C Hoischen, TL Holch, M Holler, M Hörbe, D Horns, D Huber, H Iwasaki, M Jamrozy, D Jankowsky, F Jankowsky, A Jardin-Blicq, V Joshi, I Jung-Richardt, MA Kastendieck, K Katarzyński, M Katsuragawa, U Katz, D Khangulyan, B Khélifi, J King, S Klepser, W Kluźniak, Nu Komin, K Kosack, D Kostunin, M Kreter, G Lamanna, A Lemière, M Lemoine-Goumard, J-P Lenain, E Leser, C Levy, T Lohse, I Lypova, J Mackey, J Majumdar, D Malyshev, D Malyshev, V Marandon, P Marchegiani, A Marcowith, A Mares, G Martí-Devesa, R Marx, G Maurin, PJ Meintjes, R Moderski, M Mohamed, L Mohrmann, C Moore, P Morris, E Moulin, J Muller, T Murach, S Nakashima, K Nakashima, M de Naurois, H Ndiyavala, F Niederwanger, J Niemiec, L Oakes, P O’Brien, H Odaka, S Ohm, E de Ona Wilhelmi, M Ostrowski, M Panter, RD Parsons, C Perennes, P-O Petrucci, B Peyaud, Q Piel, S Pita, V Poireau, A Priyana Noel, DA Prokhorov, H Prokoph, G Pühlhofer, M Punch, A Quirrenbach, S Raab, R Rauth, A Reimer, O Reimer, Q Remy, M Renaud, F Rieger, L Rinchiuso, C Romoli, G Rowell, B Rudak, E Ruiz-Velasco, V Sahakian, S Sailer, S Saito, DA Sanchez, A Santangelo, M Sasaki, M Scalici, R Schlickeiser, F Schüssler, A Schulz, HM Schutte, U Schwanke, S Schwemmer, M Seglar-Arroyo, M Senniappan, AS Seyffert, N Shafi, K Shiningayamwe, R Simoni, A Sinha, H Sol, A Specovius, S Spencer, M Spir-Jacob, Ł Stawarz, R Steenkamp, C Stegmann, C Steppa, T Takahashi, T Tavernier, AM Taylor, R Terrier, D Tiziani, M Tluczykont, L Tomankova, C Trichard, M Tsirou, N Tsuji, R Tuffs, Y Uchiyama, DJ van der Walt, C van Eldik, C van Rensburg, B van Soelen, G Vasileiadis, J Veh, C Venter, P Vincent, J Vink, HJ Völk, T Vuillaume, Z Wadiasingh, SJ Wagner, J Watson, F Werner, R White, A Wierzcholska, R Yang, H Yoneda, M Zacharias, R Zanin, AA Zdziarski, A Zech, J Zorn, N Żywucka
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MAGIC very large zenith angle observations of the Crab Nebula up to 100 TeV

Astronomy & Astrophysics EDP Sciences 635 (2020) a158

Authors:

VA Acciari, S Ansoldi, LA Antonelli, A Arbet Engels, D Baack, A Babić, B Banerjee, U Barres de Almeida, JA Barrio, J Becerra González, W Bednarek, L Bellizzi, E Bernardini, A Berti, J Besenrieder, W Bhattacharyya, C Bigongiari, A Biland, O Blanch, G Bonnoli, Ž Bošnjak, G Busetto, R Carosi, G Ceribella, Y Chai, A Chilingaryan, S Cikota, SM Colak, U Colin, E Colombo, JL Contreras, J Cortina, S Covino, V D’Elia, P Da Vela, F Dazzi, A De Angelis, B De Lotto, M Delfino, J Delgado, D Depaoli, F Di Pierro, L Di Venere, E Do Souto Espiñeira, D Dominis Prester, A Donini, D Dorner, M Doro, D Elsaesser, V Fallah Ramazani, A Fattorini, G Ferrara, D Fidalgo, L Foffano, MV Fonseca, L Font, C Fruck, S Fukami, RJ García López, M Garczarczyk, S Gasparyan, M Gaug, N Giglietto, F Giordano, N Godinović, D Green, D Guberman, D Hadasch, A Hahn, J Herrera, J Hoang, D Hrupec, M Hütten, T Inada, S Inoue, K Ishio, Y Iwamura, L Jouvin, D Kerszberg, H Kubo, J Kushida, A Lamastra, D Lelas, F Leone, E Lindfors, S Lombardi, F Longo, M López, R López-Coto, A López-Oramas, S Loporchio, B Machado de Oliveira Fraga, C Maggio, P Majumdar, M Makariev, M Mallamaci, G Maneva, M Manganaro, K Mannheim, L Maraschi, M Mariotti, M Martínez, D Mazin, S Mićanović, D Miceli, M Minev, JM Miranda, R Mirzoyan, E Molina, A Moralejo, D Morcuende, V Moreno, E Moretti, P Munar-Adrover, V Neustroev, C Nigro, K Nilsson, D Ninci, K Nishijima, K Noda, L Nogués, S Nozaki, S Paiano, J Palacio, M Palatiello, D Paneque, R Paoletti, JM Paredes, P Peñil, M Peresano, M Persic, PG Prada Moroni, E Prandini, I Puljak, W Rhode, M Ribó, J Rico, C Righi, A Rugliancich, L Saha, N Sahakyan, T Saito, S Sakurai, K Satalecka, K Schmidt, T Schweizer, J Sitarek, I Šnidarić, D Sobczynska, A Somero, A Stamerra, D Strom, M Strzys, Y Suda, T Surić, M Takahashi, F Tavecchio, P Temnikov, T Terzić, M Teshima, N Torres-Albà, L Tosti, V Vagelli, J van Scherpenberg, G Vanzo, M Vazquez Acosta, CF Vigorito, V Vitale, I Vovk, M Will, D Zarić
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The Thousand-Pulsar-Array programme on MeerKAT - I. Science objectives and first results

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Oxford University Press (OUP) 493:3 (2020) 3608-3615

Authors:

Simon Johnston, A Karastergiou, Mj Keith, X Song, P Weltevrede, F Abbate, M Bailes, S Buchner, F Camilo, M Geyer, B Hugo, A Jameson, M Kramer, A Parthasarathy, Dj Reardon, A Ridolfi, M Serylak, Rm Shannon, R Spiewak, W van Straten, V Venkatraman Krishnan, F Jankowski, Bw Meyers, L Oswald, B Posselt, C Sobey, A Szary, J van Leeuwen

Abstract:

© 2020 The Author(s). We report here on initial results from the Thousand-Pulsar-Array (TPA) programme, part of the Large Survey Project 'MeerTime' on the MeerKAT telescope. The interferometer is used in the tied-array mode in the band from 856 to 1712 MHz, and the wide band coupled with the large collecting area and low receiver temperature make it an excellent telescope for the study of radio pulsars. The TPA is a 5 year project, which aims at to observing (a) more than 1000 pulsars to obtain high-fidelity pulse profiles, (b) some 500 of these pulsars over multiple epochs, and (c) long sequences of single-pulse trains from several hundred pulsars. The scientific outcomes from the programme will include the determination of pulsar geometries, the location of the radio emission within the pulsarmagnetosphere, the connection between the magnetosphere and the crust and core of the star, tighter constraints on the nature of the radio emission itself, as well as interstellar medium studies. First, results presented here include updated dispersion measures, 26 pulsars with Faraday rotation measures derived for the first time, and a description of interesting emission phenomena observed thus far.
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