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1. Morphometry on the sphere: Cartesian and irreducible Minkowski tensors explained and implemented

Author

Caroline Collischon, Michael A. Klatt, Anthony J. Banday, Manami Sasaki, and Christoph Räth

Subjects
Astrophysics, QB460-466, Physics, QC1-999
Abstract

Abstract Minkowski tensors are comprehensive shape descriptors that robustly capture n-point information in complex random geometries and that have already been extensively applied in the Euclidean plane. Here, we devise a framework for Minkowski tensors on the sphere. We first advance the theory by introducing irreducible Minkowski tensors, which avoid the redundancies of previous representations. We, moreover, generalize Minkowski sky maps to the sphere. These maps are a concept of local anisotropy, which easily adjusts to masked data. We demonstrate the power of our new procedure by applying it to simulations and real data of the Cosmic Microwave Background, finding an anomalous region close to the well-known Cold Spot. The accompanying open-source software, litchi, used to generate these maps from data in the HEALPix-format is made publicly available to facilitate broader integration of Minkowski maps in other fields, such as fluid demixing, porous structures, or geosciences more generally.

Published
2024
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2. Morphological Evidence for the eROSITA Bubbles Being Giant and Distant Structures

Author

Teng Liu, Andrea Merloni, Jeremy Sanders, Gabriele Ponti, Andrew Strong, Michael C. H. Yeung, Nicola Locatelli, Peter Predehl, Xueying Zheng, Manami Sasaki, Michael Freyberg, Konrad Dennerl, Werner Becker, Kirpal Nandra, Martin Mayer, and Johannes Buchner

Subjects
Milky Way Galaxy, Interstellar clouds, Diffuse interstellar clouds, Shocks, X-ray surveys, Active galactic nuclei, Astrophysics, QB460-466
Abstract

There are two contradictory views of the eROSITA bubbles: either a 10 ^4 pc scale pair of giant bubbles blown by the Galactic center (GC), or a 10 ^2 pc scale local structure coincidentally located in the direction of GC. A key element of this controversy is the distance to the bubbles. Based on the 3D dust distribution in the Galactic plane, we found three isolated, distant (500–800 pc) clouds at intermediate Galactic latitudes. Their projected morphologies perfectly match the X-ray shadows on the defining features of the north eROSITA bubble, i.e., the North Polar Spur (NPS) and the Lotus Petal Cloud (LPC), indicating that both the NPS and LPC are distant, with a distance lower limit of nearly 1 kpc. In the X-ray-dark region between the NPS and LPC, we found a few polarized radio arcs and attributed them to the bubble’s shock front. These arcs match up perfectly with the outer border of the NPS and LPC and provide a way to define the bubble’s border. The border defined in this way can be well described by the line-of-sight tangent of a 3D skewed cup model rooted in the GC. We conclude that, instead of being two independent, distant features, the NPS and LPC compose a single, giant bubble, which therefore is most plausibly a 10 kpc scale bubble rooted at the GC.

Published
2024
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4. The ASKAP-EMU Early Science Project: 888 MHz radio continuum survey of the Large Magellanic Cloud

Author

Clara M Pennock, Jacco Th van Loon, Miroslav D Filipović, Heinz Andernach, Frank Haberl, Roland Kothes, Emil Lenc, Lawrence Rudnick, Sarah V White, Claudia Agliozzo, Sonia Antón, Ivan Bojičić, Dominik J Bomans, Jordan D Collier, Evan J Crawford, Andrew M Hopkins, Kanapathippillai Jeganathan, Patrick J Kavanagh, Bärbel S Koribalski, Denis Leahy, Pierre Maggi, Chandreyee Maitra, Josh Marvil, Michał J Michałowski, Ray P Norris, Joana M Oliveira, Jeffrey L Payne, Hidetoshi Sano, Manami Sasaki, Lister Staveley-Smith, and Eleni Vardoulaki

Published
2021
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5. EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3

Author

Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, and Branislav Vukotić

Subjects
Supernova remnants, Radio astronomy, Astronomy, QB1-991
Abstract

We present the serendipitous detection of a new Galactic supernova remnant (SNR), G288.8–6.3, using data from the Australian Square Kilometre Array Pathfinder (ASKAP) Evolutionary Map of the Universe (EMU) survey. Using multifrequency analysis, we confirm this object as an evolved Galactic SNR at high Galactic latitude with low radio surface brightness and typical SNR spectral index of α = − 0.41 ± 0.12. To determine the magnetic field strength in SNR G288.8–6.3, we present the first derivation of the equipartition formulae for SNRs with spectral indices α > − 0.5. The angular size is 1.°8 × 1.°6 (107.′6 × 98.′4), and we estimate that its intrinsic size is ∼40 pc, which implies a distance of ∼1.3 kpc and a position of ∼140 pc above the Galactic plane. This is one of the largest in angular size and closest Galactic SNRs. Given its low radio surface brightness, we suggest that it is about 13,000 yr old.

Published
2023
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10. Strong perturbation of a super-virial Magellanic circum-galactic medium

Author

Nicola Locatelli, Gabriele Ponti, Andrea Merloni, Xueying Zheng, Konrad Dennerl, Frank Haberl, Chandreyee Maitra, Jeremy Sanders, Manami Sasaki, and Franco Vazza

Abstract

Modern galaxy evolution theories predict a large fraction of ordinary matter to be distributed in the form of gas over the largest galactic scales, with most of the gas mass encompassing the peak and high tail of the overall temperature distribution1. Satellite galaxies however, may lose a large amount of this extended gas due to stripping and ram pressure generated by their in-fall onto a larger system2. The presence of highly ionized gas associated with the Small and Large Magellanic Clouds has been recently confirmed through indirect probes3,4. Using eROSITA/SRG data, in this work we show the first direct images of the X-ray emission from the hottest gas associated to the circum-galactic medium surrounding the Magellanic Clouds. We discover an extended hot gas phase at ~2.3×106 K. This temperature challenges the theoretical expectations from a virialized system5,6 implying that heating mechanisms are at play in the Magellanic Clouds circum-galactic medium. We also discover a strong perturbation that we identify as a cold front in the (Galactic) South direction of the Magellanic Clouds, morphologically connected to them both. The cold front -the first ever discovered at galactic scales (~10 kpc)- also appears to be coincident with enhanced polarization at radio frequencies, as well as with a tangential alignment of the magnetic field lines. The detected discontinuity in the properties of the gas surrounding the Magellanic Clouds is consistent with a gas reservoir being perturbed by the three-body interaction between the Magellanic Clouds and the Milky Way7,8. The Magellanic Clouds provide a unique laboratory for assessing the presence of a hot gas phase in in-falling satellite systems9. The detection of a still large reservoir of hot gas, together with the detection of a front connected with thermal heating and magnetic amplification corroborates and inform galaxy evolution theories10.

Published
2023
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13. Multi-Wavelength View of Supernova Remnants

Author

Manami Sasaki

Subjects
Engineering (General). Civil engineering (General), TA1-2040
Abstract

This contribution gives a very short overview on the emission of supernova remnants and the processes that are responsible for both the thermal and non-thermal origins of the emission, typically observed in radio, X-rays, and up to gamma-rays. We discuss in particular the case of the Galactic SNR CTB 109. As detailed X-ray studies combined with observations in radio have shown, CTB 109 is interacting with a giant molecular cloud complex. The interaction of the SNR shock with dense interstellar clouds is responsible for both the unusual semi-circular morphology of the SNR and the bright X-ray feature inside the SNR, and, as has been shown recently, seems also to play a major role in the production of gamma-rays.

Published
2014
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14. XMMU J050722.1−684758: discovery of a new Be X-ray binary pulsar likely associated with the supernova remnant MCSNR J0507−6847

Author

Miroslav Filipovic, P. Maggi, Andrzej Udalski, Patrick J. Kavanagh, Frank Haberl, George Vasilopoulos, Chandeyee Maitra, Manami Sasaki, Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Superbubble, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Binary pulsar, Neutron star, Pulsar, [SDU]Sciences of the Universe [physics], Space and Planetary Science, 0103 physical sciences, High mass, Astrophysics - High Energy Astrophysical Phenomena, Large Magellanic Cloud, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the discovery of a new high mass X-ray binary pulsar, XMMU J050722.1-684758, possibly associated with the supernova remnant MCSNR J0507-6847 in the Large Magellanic Cloud, using XMM-Newton X-ray observations. Pulsations with a periodicity of 570 s are discovered from the Be X-ray binary XMMU J050722.1-684758 confirming its nature as a HMXB pulsar. The HMXB is located near the geometric centre of the supernova remnant MCSNR J0507-6847 (0.9 arcmin from the centre) which supports the XRB-SNR association. The estimated age of the supernova remnant is 43-63 kyr which points to a middle aged to old supernova remnant. The large diameter of the supernova remnant combined with the lack of distinctive shell counterparts in optical and radio indicates that the SNR is expanding into the tenous environment of the superbubble N103. The estimated magnetic field strength of the neutron star is $B\gtrsim10^{14}$ G assuming a spin equilibrium condition which is expected from the estimated age of the parent remnant and assuming that the measured mass-accretion rate remained constant throughout., 12 pages, 13 figures, accepted for publication in MNRAS

Published
2021
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16. ALMA CO observations of a giant molecular cloud in M 33: Evidence for high-mass star formation triggered by cloud–cloud collisions

Author

Toshikazu Onishi, Rei Enokiya, Jonathan Knies, Manami Sasaki, Gavin Rowell, Kazuyuki Muraoka, N. Maxted, Shinji Fujita, Kisetsu Tsuge, Kengo Tachihara, Paul P. Plucinsky, Hidetoshi Sano, Mikito Kohno, Y. Yamane, Kazuki Tokuda, Miroslav Filipovic, and Yasuo Fukui

Subjects
Physics, 010504 meteorology & atmospheric sciences, Star formation, business.industry, Molecular cloud, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Cloud computing, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, High mass, Astrophysics::Solar and Stellar Astrophysics, business, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

We report the first evidence for high-mass star formation triggered by collisions of molecular clouds in M33. Using the Atacama Large Millimeter/submillimeter Array, we spatially resolved filamentary structures of giant molecular cloud 37 in M33 using $^{12}$CO($J$ = 2-1), $^{13}$CO($J$ = 2-1), and C$^{18}$O($J$ = 2-1) line emission at a spatial resolution of $\sim$2 pc. There are two individual molecular clouds with a systematic velocity difference of $\sim$6 km s$^{-1}$. Three continuum sources representing up to $\sim$10 high-mass stars with the spectral types of B0V-O7.5V are embedded within the densest parts of molecular clouds bright in the C$^{18}$O($J$ = 2-1) line emission. The two molecular clouds show a complementary spatial distribution with a spatial displacement of $\sim$6.2 pc, and show a V-shaped structure in the position-velocity diagram. These observational features traced by CO and its isotopes are consistent with those in high-mass star-forming regions created by cloud-cloud collisions in the Galactic and Magellanic Cloud HII regions. Our new finding in M33 indicates that the cloud-cloud collision is a promising process to trigger high-mass star formation in the Local Group., Comment: 13 pages, 10 figures, 1 table, accepted for publication in PASJ

Published
2020
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17. Detection of extended TeV emission around the Geminga pulsar with H.E.S.S

Author

Michael Punch, Christo Venter, Christian Stegmann, Stefan Wagner, Andreas Zech, Yasunobu Uchiyama, M. Hörbe, L. Mohrmann, Hassan Abdalla, Albert Seyffert, Michael Backes, Laenita Lorraine Oberholzer, Dieter Horns, K. Nakashima, Tim Holch, K. Bernloehr, Naomi Tsuji, Heinrich J. Völk, Regis Terrier, Carlo Romoli, Gerard Fontaine, Tadayuki Takahashi, M. Fuessling, Hester Schutte, S. Steinmassl, Samuel Timothy Spencer, Sami Caroff, Victor Doroshenko, Frank M. Rieger, Clemens Hoischen, A. A. Zdziarski, P. T. O'Brien, Markus Holler, Q. Remy, Felix Jankowsky, Hannah Dalgleish, German Hermann, Paul Morris, Anne Lemiere, E. Kasai, Louis Du Plessis, Johann van der Walt, Martin Tluczykont, Dan Parsons, Anna Barnacka, D. Malyshev, Nukri Komin, Tom Armstrong, Felix Aharonian, Gilles Maurin, J. F. Glicenstein, David Sanchez, Krzysztof Katarzynski, Victor Barbosa Martins, Ira Jung, C. Arcaro, Sebastian Panny, Gianluca Giavitto, Angel Noel, Bruno Khelifi, Alison Mitchell, Santiago Pita, Werner Hofmann, Gašper Kukec Mezek, Atreyee Sinha, Emma Ona-Wilhelmi, Jonathan Mackey, Carlo van Rensburg, Gerd Puehlhofer, Lei Sun, Laura Olivera-Nieto, Hambeleleni Ndiyavala, Floriane Cangemi, A. Yusafzai, C. Levy, Alexandre Marcowith, Felix Werner, Thomas Lohse, Hend Yassin, Anton Dmytriiev, Manuel Meyer, Arnaud Mares, Manami Sasaki, Mathieu Naurois, Catherine Boisson, Jhilik Majumdar, N. Zywucka, Sumari Hattingh, Takaaki Tanaka, Gavin Rowell, Hector Rueda Ricarte, Mathieu Bony, Oguzhan Anguener, C. Moore, Riaan Steenkamp, Richard White, Kirsty Feijen, Heike Prokoph, Thomas Bylund, Rowan Batzofin, Andreas Zmija, Dorit Glawion, Samuel Zouari, Tomasz Bulik, Robert Brose, Andrea Santangelo, Jacco Vink, Michal Ostrowski, Anna Luashvili, Jacques Muller, Malgorzata Curlo, Marion Spir-Jacob, M. Lemoine-Goumard, Lente Dreyer, David Huber, J.-P. Lenain, Matthieu Renaud, Amid Nayerhoda, Hugh Spackman, Michael Kreter, Justine Devin, Sabrina Casanova, Anu Kundu, Stefan Klepser, V. Sahakian, G. Peron, Alessandro Montanari, Garret Cotter, Vikas Joshi, Zhiqiu Huang, T. Chand, Lott Frans, D. A. Prokhorov, K. Kosack, Sylvia Zhu, P. J. Meintjes, David Berge, Yves Gallant, Lukasz Stawarz, Stefan Ohm, Halim Ashkar, Fabian Leuschner, Jason John Watson, Davit Zargaryan, Arache Djannati-Ataï, Johannes Schaefer, S. J. Fegan, Andreas Quirrenbach, Gaëtan Fichet de Clairfontaine, Axel Donath, A. W. Chen, Stefan Funk, Alicja Wierzcholska, Guillem Marti'i-Devesa, P. Reichherzer, V. Poireau, Jimmy N.S. Shapopi, Jaqueline Catalano, Stefano Gabici, Ramin Marx, M. Panter, Michael Zacharias, Jim Hinton, Jean-Pierre Ernenwein, U. Katz, G. Lamanna, R. Konno, Isak Delberth Davids, Fabian Schüssler, A. Fiasson, Sabrina Einecke, Iryna Lypova, S. Sailer, Dmitry Khangulyan, Charles Thorpe-Morgan, Roberta Zanin, Emmanuel Moulin, Andrew Taylor, B. Rudak, Kathrin Egberts, Johannes Veh, J. Bolmont, Faical Ait-Benkhali, Kleopas Shiningayamwe, Jacek Niemiec, G. Vasileiadis, Monica Barnard, Yvonne Becherini, Denys Malyshev, Maria Haupt, Olaf Reimer, Edna Ruiz Velasco, Lenka Tomankova, Sébastien Le Stum, Thomas Murach, Christopher van Eldik, Rafal Moderski, Mohanraj Senniappan, Francois Brun, P. Vincent, Heiko Salzmann, Andreas Specovius, Yu Wun Wong, Vincent Marandon, Hannes Thiersen, Vardan Baghmanyan, Celine Armand, Dmitriy Kostunin, L. Giunti, Brian van Soelen, Thomas Tavernier, Markus Boettcher, Michelle Tsirou, M.-H. Grondin, Rachel Simoni, Anita Reimer, Constantin Steppa, Ullrich Schwanke, Jean Damascene Mbarubucyeye, Wlodek Kluzniak, Brian Reville, Connor Duffy, James Davies, R. J. Tuffs, B. Bi, Mischa Breuhaus, Pauline Chambery, Marek Jamrozy, Helene Sol, Paolo Marchegiani, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and H.E.S.S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma rays, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, imaging, Astronomy, IACT, Cosmology, Tellurium compounds, Cherenkov counter, gamma ray: emission, Pulsar, HESS, Milagro, TeV, HESS - Abteilung Hinton, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, HAWC, Cosmic rays, Cherenkov radiation, pulsar
Abstract

Highly extended gamma-ray emission around the Geminga pulsar was discovered by Milagro and verified by HAWC. Despite many observations with Imaging Atmospheric Cherenkov Telescopes (IACTs), detection of gamma-ray emission on angular scales exceeding the IACT field-of-view has proven challenging. Recent developments in analysis techniques have enabled the detection of significant emission around Geminga in archival data with H.E.S.S.. In 2019, further data on the Geminga region were obtained with an adapted observation strategy. Following the announcement of the detection of significant TeV emission around Geminga in archival data, in this contribution we present the detection in an independent dataset. New analysis results will be presented, and emphasis given to the technical challenges involved in observations of highly extended gamma-ray emission with IACTs., PoS: Proceedings of Science, 395, ISSN:1824-8039, Proceedings of 37th International Cosmic Ray Conference

Published
2022

18. Searching for VHE gamma-ray emission associated with IceCube neutrino alerts using FACT, H.E.S.S., MAGIC, and VERITAS

Author

Konstancja, Satalecka, Acciari, Victor A., Stefano, Ansoldi, Lucio Angelo Antonelli, Axel Arbet Engels, Manuel, Artero, Katsuaki, Asano, Dominik, Baack, Ana, Babic, Andr('(e))s, Baquero, Ulisses Barres de Almeida, Juan Abel Barrio, Ivana, Batkovi('(c)), Josefa Becerra Gonzalez, Wlodek, Bednarek, Lorenzo, Bellizzi, Elisa, Bernardini, Maria-Isabel, Bernardos, Alessio, Berti, Jürgen, Besenrieder, Wrijupan, Bhattacharyya, Ciro, Bigongiari, Adrian, Biland, Oscar, Blanch, Hendrik, Bökenkamp, Giacomo, Bonnoli, Zeljka, Bosnjak, Giovanni, Busetto, Roberto, Carosi, Giovanni, Ceribella, Matteo, Cerruti, Yating, Chai, Ashot, Chilingarian, Stefan, Cikota, Sidika Merve Colak, Eduardo, Colombo, Jose Luis Contreras, Juan, Cortina, Stefano, Covino, Giacomo D( extquotesingle)Amico, Valerio D( extquotesingle)Elia, Paolo Da Vela, Francesco, Dazzi, Alessandro De Angelis, Barbara De Lotto, Manuel, Delfino, Jordi, Delgado, Carlos Delgado Mendez, Davide, Depaoli, Federico Di Pierro, Leonardo Di Venere, Elia Do Souto Espi(~(n))eira, Dijana Dominis Prester, Alice, Donini, Daniela, Dorner, Michele, Doro, Dominik, Elsaesser, Vandad Fallah Ramazani, Alicia, Fattorini, Maria Victoria Fonseca, Lluis, Font, Christian, Fruck, Satoshi, Fukami, Yasushi, Fukazawa, Garc('(i))a L('(o))pez, Ramon J., Markus, Garczarczyk, Sargis, Gasparyan, Markus, Gaug, Giglietto, Nicola, Francesco, Giordano, Pawel, Gliwny, Nikola, Godinovic, David, Green, Jarred Gershon Green, Daniela, Hadasch, Alexander, Hahn, Lea, Heckmann, Javier, Herrera, John, Hoang, Dario, Hrupec, Moritz, Hütten, Tomohiro, Inada, Kazuma, Ishio, Yuki, Iwamura, Irene Jim('(e))nez Mart('(i))nez, Jenni, Jormanainen, L('(e))a, Jouvin, Marie, Karjalainen, Daniel, Kerszberg, Yukiho, Kobayashi, Hidetoshi, Kubo, Junko, Kushida, Alessandra, Lamastra, Damir, Lelas, Francesco, Leone, Elina, Lindfors, Lena, Linhoff, Saverio, Lombardi, Francesco, Longo, Ruben, Lopez-Coto, Marcos, L('(o))pez-Moya, Alicia, L('(o))pez-Oramas, Loporchio, Serena, Bernardo Machado de Oliveira Fraga, Camilla, Maggio, Pratik, Majumdar, Martin, Makariev, Manuela, Mallamaci, Galina, Maneva, Marina, Manganaro, Karl, Mannheim, Laura, Maraschi, Mos(`(e)), Mariotti, Manel, Martinez, Daniel, Mazin, Stefano, Menchiari, Simone, Mender, Sa( (s))a Mi('(c))anovi('(c)), Davide, Miceli, Tjark, Miener, Jose Miguel Miranda, Razmik, Mirzoyan, Edgar, Molina, Abelardo, Moralejo, Daniel, Morcuende, Victoria, Moreno, Elena, Moretti, Takeshi, Nakamori, Lara, Nava, Vitaly, Neustroev, Cosimo, Nigro, Kari, Nilsson, Kyoshi, Nishijima, Koji, Noda, Seiya, Nozaki, Yoshiki, Ohtani, Tomohiko, Oka, Jorge, Otero-Santos, Simona, Paiano, Michele, Palatiello, David, Paneque, Riccardo, Paoletti, Paredes, Josep M., Lovro, Pavleti('(c)), Pablo, Pe(~(n))il, Massimo, Persic, Marine, Pihet, Pier Giorgio Prada Moroni, Elisa, Prandini, Chaitanya, Priyadarshi, Ivica, Puljak, Wolfgang, Rhode, Marc, Rib('(o)), Javier, Rico, Chiara, Righi, Andrea, Rugliancich, Narek, Sahakyan, Takayuki, Saito, Shunsuke, Sakurai, Francesco Gabriele Saturni, Bernd, Schleicher, Kevin, Schmidt, Thomas, Schweizer, Julian, Sitarek, Iva, ( (S))nidari('(c)), Dorota, Sobczy('(n))ska, Alessia, Spolon, Antonio, Stamerra, Jelena Stri( (s))kovi('(c)), Derek, Strom, Marcel, Strzys, Yusuke, Suda, Tihomir, Suri('(c)), Mitsunari, Takahashi, Ryuji, Takeishi, Fabrizio, Tavecchio, Petar, Temnikov, Tomislav, Terzic, Masahiro, Teshima, Luca, Tosti, Stefano, Truzzi, Antonio, Tutone, Santiago, Ubach, Juliane van Scherpenberg, Gaia, Vanzo, Monica VAZQUEZ ACOSTA, Sofia, Ventura, Vassil, Verguilov, Carlo Francesco Vigorito, Vincenzo, Vitale, Ievgen, Vovk, Martin, Will, Carolin, Wunderlich, Tokonatsu, Yamamoto, Darko, Zari('(c)), Matteo, Balbo, Thomas, Bretz, Jens, Buss, Laura, Eisenberger, Dorothee, Hildebrand, Roman, Iotov, Adelina, Kalenski, Dominik, Neise, Maximilian, Noethe, Aleksander, Paravac, Vitalii, Sliusar, Roland, Walter, Rasha, Abbasi, Markus, Ackermann, Jenni, Adams, Juanan, Aguilar, Ahlers, M., Maryon, Ahrens, Cyril Martin Alispach, Antonio Augusto Alves Junior, Najia Moureen Binte Amin, Rui, An, Karen, Andeen, Tyler, Anderson, Gisela, Anton, Carlos, Arguelles, Yosuke, Ashida, Spencer, Axani, Xinhua, Bai, Aswathi Balagopal, V., Anastasia Maria Barbano, Barwick, S. W., Benjamin, Bastian, Vedant, Basu, Sebastian, Baur, Bay, R. C., Beatty, J. J., Becker, K. -H., Julia Becker Tjus, Chiara, Bellenghi, Segev, Benzvi, Berley, D., Besson, D. Z., Gary, Binder, Daniel, Bindig, Blaufuss, E., Summer, Blot, Matthias, Boddenberg, Federico, Bontempo, Jurgen, Borowka, Boser, S., Olga, Botner, Jakob, Bottcher, Etienne, Bourbeau, Federica, Bradascio, Braun, J., Stephanie, Bron, Jannes, Brostean-Kaiser, Sally-Ann, Browne, Alexander, Burgman, Ryan, Burley, Raffaela, Busse, Michael, Campana, Erin, Carnie-Bronca, Chujie, Chen, Dmitry, Chirkin, Koun, Choi, Bryanlee, Clark, Kenneth, Clark, Lew, Classen, Alan, Coleman, Gabriel, Collin, Conrad, J. M., Paul, Coppin, Pablo, Correa, Cowen, D. F., Cross, R., Christian, Dappen, Pranav, Dave, Catherine DE CLERCQ, James, Delaunay, Hans, Dembinski, Kunal, Deoskar, Sam De Ridder, Abhishek, Desai, Paolo, Desiati, Krijn de Vries, Gwenhaël de Wasseige, Meike De With, Tyce, Deyoung, Sukeerthi, Dharani, Alejandro, Diaz, Juan Carlos Diaz-Velez, Markus, Dittmer, Hrvoje, Dujmovic, Matt, Dunkman, Michael, Duvernois, Emily, Dvorak, Thomas, Ehrhardt, Philipp, Eller, Ralph, Engel, Hannah, Erpenbeck, John, Evans, Evenson, P. A., Kwok Lung Fan, Fazely, A. R., Sebastian, Fiedlschuster, Aaron, Fienberg, Kirill, Filimonov, Chad, Finley, Leander, Fischer, Derek, B Fox, Anna, Franckowiak, Elizabeth, Friedman, Alexander, Fritz, Philipp, Furst, Gaisser, T. K., Jay, Gallagher, Erik, Ganster, Alfonso, Garcia, Simone, Garrappa, Gerhardt, L., Ava, Ghadimi, Christian, Glaser, Theo, Glauch, Thorsten, Glusenkamp, Goldschmidt, A., Javier, Gonzalez, Sreetama, Goswami, Darren, Grant, Timoth('(e))e, Gr('(e))goire, Spencer, Griswold, Mehmet, Gunduz, Christoph, Günther, Christian, Haack, Allan, Hallgren, Halliday, R., Halve, L., Halzen, F., Martin Ha Minh, Kael, Hanson, John, Hardin, Harnisch, Alexander A., Andreas, Haungs, Simon, Hauser, Dustin, Hebecker, Helbing, K., Felix, Henningsen, Hettinger, Emma C., Stephanie, Hickford, Joshua, Hignight, Colton, Hill, Hill, G. C., Kara, Hoffman, Ruth, Hoffmann, Tobias, Hoinka, Benjamin, Hokanson-Fasig, Hoshina, K., Feifei, Huang, Matthias, Huber, Thomas, Huber, Klas, Hultqvist, Mirco, Hunnefeld, Raamis, Hussain, Seongjin, In, Nad(`(e))ge, Iovine, Aya, Ishihara, Matti, Jansson, George, Japaridze, Minjin, Jeong, Ben, Jones, Donghwa, Kang, Woosik, Kang, Xinyue, Kang, Alexander, Kappes, David, Kappesser, Timo, Karg, Martina, Karl, Karle, A., Katz, U., Kauer, M., Moritz, Kellermann, Kelley, J. L., Ali, Kheirandish, Ken( extquotesingle)ichi Kin, Thomas, Kintscher, Joanna, Kiryluk, Spencer, Klein, Ramesh, Koirala, Hermann, Kolanoski, Tomas, Kontrimas, Lutz, Kopke, Claudio, Kopper, Sandro, Kopper, Koskinen, D. J., Paras, Koundal, Michael, Kovacevich, Marek, Kowalski, Tetiana, Kozynets, Emma, Kun, Naoko, Kurahashi, Neha, Lad, Cristina Lagunas Gualda, Justin, Lanfranchi, Michael, J Larson, Frederik Hermann Lauber, Jeffrey, Lazar, Jiwoong, Lee, Kayla, Leonard, Agnieszka, Leszczy('(n))ska, Yijia, Li, Massimiliano, Lincetto, Qinrui, Liu, Maria, Liubarska, Elisa, Lohfink, Cristian Jesus Lozano Mariscal, Lu, Lu, Francesco, Lucarelli, Andrew, Ludwig, William, Luszczak, Yang, Lyu, Wing Yan Ma, James, Madsen, Kendall, Mahn, Yuya, Makino, Sarah, Mancina, Ioana Codrina Maris, Maruyama, Reina H., Mase, K., Thomas, Mcelroy, Frank, Mcnally, James Vincent Mead, Meagher, K., Andres, Medina, Maximilian, Meier, Stephan, Meighen-Berger, Jessie, Micallef, Daniela, Mockler, Teresa, Montaruli, Roger, Moore, Morse, R., Marjon, Moulai, Richard, Naab, Ryo, Nagai, Uwe, Naumann, Jannis, Necker, Le Viet Nguyen, Hans, Niederhausen, Mehr, Nisa, Sarah, Nowicki, Dave, Nygren, Anna Obertacke Pollmann, Marie, Oehler, Olivas, A., Erin O( extquotesingle)Sullivan, Hershal, Pandya, Daria, Pankova, Nahee, Park, Grant, Parker, Ek Narayan Paudel, Larissa, Paul, Carlos Perez de los Heros, Lilly, Peters, Saskia, Philippen, Damian, Pieloth, Sarah, Pieper, Martin, Pittermann, Pizzuto, A., Plum, M., Yuiry, Popovych, Alessio, Porcelli, Maria Prado Rodriguez, Buford Price, P., Brandom, Pries, Gerald, Przybylski, Christoph, Raab, Amirreza, Raissi, Mohamed, Rameez, Rawlins, K., Immacolata Carmen Rea, Abdul, Rehman, Ren('(e)), Reimann, Giovanni, Renzi, Elisa, Resconi, Simeon, Reusch, Mike, Richman, Benedikt, Riedel, Ella, Roberts, Sally, Robertson, Gerrit, Roellinghoff, Martin, Rongen, Carsten, Rott, Tim, Ruhe, Dirk, Ryckbosch, Devyn Rysewyk Cantu, Ibrahim, Safa, Julian, Saffer, Sebastian Sanchez Herrera, Alexander, Sandrock, Joakim, Sandroos, Marcos, Santander, Subir, Sarkar, Sourav, Sarkar, Maximilian Karl Scharf, Merlin, Schaufel, Harald, Schieler, Sebastian, Schindler, Schlunder, P., Torsten, Schmidt, Austin, Schneider, Judith, Schneider, Schröder, Frank G., Lisa Johanna Schumacher, Georg, Schwefer, Steve, Sclafani, Seckel, D., Surujhdeo, Seunarine, Ankur, Sharma, Shefali, Shefali, Manuel, Silva, Barbara, Skrzypek, Ben, Smithers, Robert, Snihur, Jan, Soedingrekso, Dennis, Soldin, Christian, Spannfellner, Glenn, Spiczak, Christian, Spiering, Juliana, Stachurska, Michael, Stamatikos, Stanev, T., Robert, Stein, Joeran, Stettner, Steuer, A., Stezelberger, T., Timo, Sturwald, Thomas, Stuttard, Sullivan, G. W., Taboada, I., Frederik, Tenholt, Samvel, Ter-Antonyan, Tilav, S., Franziska, Tischbein, Kirsten, Tollefson, Christoph, Tönnis, Simona, Toscano, Delia, Tosi, Alexander, Trettin, Maria, Tselengidou, Chunfai, Tung, Andrea, Turcati, Roxanne, Turcotte, Colin, Turley, Jean Pierre Twagirayezu, Bunheng, Ty, Martin Unland Elorrieta, Nora, Valtonen-Mattila, Justin, Vandenbroucke, Nick van Eijndhoven, David, Vannerom, Jakob van Santen, Stef, Verpoest, Matthias, Vraeghe, Walck, C., Timothyblake, Watson, Chris, Weaver, Philip, Weigel, Andreas, Weindl, Matthew, Weiss, Jan, Weldert, Chris, Wendt, Johannes, Werthebach, Mark, Weyrauch, Nathan, Whitehorn, Wiebusch, C. H., Dawn, Williams, Martin, Wolf, Kurt, Woschnagg, Gerrit, Wrede, Johan, Wulff, Xianwu, Xu, Yiqian, Xu, Juan Pablo Yanez, Yoshida, S., Shiqi, Yu, Tianlu, Yuan, Zelong, Zhang, Weidong, Jin, Hassan, Abdalla, Felix, Aharonian, Faical, Ait-Benkhali, Oguzhan, Anguener, Cornelia, Arcaro, Celine, Armand, Tom, Armstrong, Halim, Ashkar, Michael, Backes, Vardan, Baghmanyan, Victor Barbosa Martins, Anna, Barnacka, Monica, Barnard, Rowan, Batzofin, Yvonne, Becherini, David, Berge, Konrad, Bernlöhr, Baiyang, Bi, Markus, Boettcher, Catherine, Boisson, Julien, Bolmont, Mathieu de Bony, Mischa, Breuhaus, Robert, Brose, Francois, Brun, Tomasz, Bulik, Thomas, Bylund, Floriane, Cangemi, Sami, Caroff, Sabrina, Casanova, Jaqueline, Catalano, Pauline, Chambery, Tej Bahadur Chand, Andrew, Chen, Garret, Cotter, Malgorzata, Curlo, Jean Damascene Mbarubucyeye, Isak Delberth Davids, James, Davies, Justine, Devin, Arache, Djannati-Ataï, Anton, Dmytriiev, Axel, Donath, Victor, Doroshenko, Lente, Dreyer, Louis Du Plessis, Connor, Duffy, Kathrin, Egberts, Sabrina, Einecke, Gabriel, Emery, Jean-Pierre, Ernenwein, Steven, Fegan, Kirsty, Feijen, Armand, Fiasson, Gaëtan Fichet de Clairfontaine, Gerard, Fontaine, Lott, Frans, Matthias, Fuessling, Stefan, Funk, Stefano, Gabici, Yves, Gallant, Shahede, Ghafourizade, Gianluca, Giavitto, Luca, Giunti, Dorit, Glawion, Jean-Francois, Glicenstein, Marie-H('(e))l(`(e))ne, Grondin, Sumari, Hattingh, Maria, Haupt, German, Hermann, Jim, Hinton, Werner, Hofmann, Clemens, Hoischen, Tim, Holch, Markus, Holler, Dieter, Horns, Zhiqiu, Huang, David, Huber, Mario, Hörbe, Marek, Jamrozy, Felix, Jankowsky, Vikas, Joshi, Ira, Jung, Eli, Kasai, Krzysztof, Katarzynski, Ul(`(i)), Katz, Dmitry, Khangulyan, Bruno, Khelifi, Stefan, Klepser, Wlodek, Kluzniak, Nukri, Komin, Ruslan, Konno, Karl, Kosack, Dmitriy, Kostunin, Michael, Kreter, Ga( (s))per Kukec Mezek, Anu, Kundu, Giovanni, Lamanna, S('(e))bastien Le Stum, Anne, Lemiere, Marianne, Lemoine-Goumard, Jean-Philippe, Lenain, Fabian, Leuschner, Christelle, Levy, Thomas, Lohse, Anna, Luashvili, Iryna, Lypova, Jonathan, Mackey, Jhilik, Majumdar, Denys, Malyshev, Dmitry, Malyshev, Vincent, Marandon, Paolo, Marchegiani, Alexandre, Marcowith, Arnaud, Mares, Guillem Marti( extquotesingle)i-Devesa, Ramin, Marx, Gilles, Maurin, Pieter, Meintjes, Manuel, Meyer, Alison, Mitchell, Rafal, Moderski, Lars, Mohrmann, Alessandro, Montanari, Chris, Moore, Paul, Morris, Emmanuel, Moulin, Jacques, Muller, Thomas, Murach, Kaori, Nakashima, Mathieu Naurois (de), Amid, Nayerhoda, Hambeleleni, Ndiyavala, Jacek, Niemiec, Angel, Noel, Paul O( extquotesingle)Brien, Laenita Lorraine Oberholzer, Stefan, Ohm, Laura, Olivera-Nieto, Emma Ona-Wilhelmi (de), Michal, Ostrowski, Sebastian, Panny, Michael, Panter, Dan, Parsons, Giada, Peron, Santiago, Pita, Vincent, Poireau, Dmitry, Prokhorov, Heike, Prokoph, Gerd, Puehlhofer, Michael, Punch, Andreas, Quirrenbach, Patrick, Reichherzer, Anita, Reimer, Olaf, Reimer, Quentin, Remy, Matthieu, Renaud, Brian, Reville, Frank, Rieger, Carlo, Romoli, Gavin, Rowell, Bronislaw, Rudak, Hector Rueda Ricarte, Edna Ruiz Velasco, Vardan, Sahakian, Simon, Sailer, Heiko, Salzmann, David, Sanchez, Andrea, Santangelo, Manami, Sasaki, Johannes, Schaefer, Hester, Schutte, Ullrich, Schwanke, Fabian, Schüssler, Mohanraj, Senniappan, Albert, Seyffert, Shapopi, Jimmy N. S., Kleopas, Shiningayamwe, Rachel, Simoni, Atreyee, Sinha, Helene, Sol, Hugh, Spackman, Andreas, Specovius, Samuel Timothy Spencer, Marion, Spir-Jacob, Lukasz, Stawarz, Riaan, Steenkamp, Christian, Stegmann, Simon, Steinmassl, Constantin, Steppa, Lei, Sun, Tadayuki, Takahashi, Takaaki, Tanaka, Thomas, Tavernier, Andrew, Taylor, Regis, Terrier, Hannes, Thiersen, Charles, Thorpe-Morgan, Martin, Tluczykont, Lenka, Tomankova, Michelle, Tsirou, Naomi, Tsuji, Richard, Tuffs, Yasunobu, Uchiyama, Johann van der Walt, Christopher van Eldik, Carlo van Rensburg, Brian van Soelen, George, Vasileiadis, Johannes, Veh, Christo, Venter, Pascal, Vincent, Jacco, Vink, Völk, Heinrich J., Stefan, Wagner, Jason John Watson, Felix, Werner, Richard, White, Alicja, Wierzcholska, Yu Wun Wong, Hend, Yassin, Anke, Yusafzai, Michael, Zacharias, Roberta, Zanin, Davit, Zargaryan, Andrzej, Zdziarski, Andreas, Zech, Sylvia, Zhu, Andreas, Zmija, Samuel, Zouari, Natalia, Zywucka, The FACT Collaboration, The H.E.S.S. Collaboration, The IceCube Collaboration, The MAGIC Collaboration, The VERITAS Collaboration, and Współautorami artykułu są członkowie Magic Collaboration, IceCube Collaboration, FACT Collaboration, H.E.S.S. Collaboration, VERITAS Collaboration w liczbie 808

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Point source, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, IACT, Astrophysics, law.invention, High Energy Physics - Experiment, Telescope, High Energy Physics - Experiment (hep-ex), law, HESS - Abteilung Hinton, ddc:530, High Energy Physics::Experiment, MAGIC (telescope), Neutrino, Blazar, Astrophysics - High Energy Astrophysical Phenomena, Cherenkov radiation
Abstract

The realtime follow-up of neutrino events is a promising approach to search for astrophysical neutrino sources. It has so far provided compelling evidence for a neutrino point source: the flaring gamma-ray blazar TXS 0506+056 observed in coincidence with the high-energy neutrino IceCube-170922A detected by IceCube. The detection of very-high-energy gamma rays (VHE, $\mathrm{E} > 100\,\mathrm{GeV}$) from this source helped establish the coincidence and constrained the modeling of the blazar emission at the time of the IceCube event. The four major imaging atmospheric Cherenkov telescope arrays (IACTs) - FACT, H.E.S.S., MAGIC, and VERITAS - operate an active follow-up program of target-of-opportunity observations of neutrino alerts sent by IceCube. This program has two main components. One are the observations of known gamma-ray sources around which a cluster of candidate neutrino events has been identified by IceCube (Gamma-ray Follow-Up, GFU). Second one is the follow-up of single high-energy neutrino candidate events of potential astrophysical origin such as IceCube-170922A. GFU has been recently upgraded by IceCube in collaboration with the IACT groups. We present here recent results from the IACT follow-up programs of IceCube neutrino alerts and a description of the upgraded IceCube GFU system., Presented at the 37th International Cosmic Ray Conference (ICRC 2021). See arXiv:2107.06966 for all IceCube contributions. See arXiv:2108.05257 for all H.E.S.S. contributions

Published
2022

19. SRG/eROSITA and XMM-Newton observations of Vela Jr

Author

Francesco Camilloni, Werner Becker, Peter Predehl, Konrad Dennerl, Michael Freyberg, Martin G. F. Mayer, and Manami Sasaki

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Vela supernova remnant complex is a region containing at least three supernova remnants: Vela, Puppis A, and Vela Jr. With the launch of the spectro-imaging X-ray telescope eROSITA on board the Spectrum Roentgen Gamma (SRG) mission, it became possible to observe the one degree wide Vela Jr in its entirety. Although several previous pointed Chandra and XMM-Newton observations are available, it is only the second time after the ROSAT all-sky survey that the whole remnant was observed in X-rays with homogeneous sensitivity. Vela Jr is one of the few remnants emitting in the TeV band, making it an important object in shock acceleration studies. However, the age and distance determination using X-ray emission is largely hampered by the presence of the Vela SNR along the same line. With the eROSITA data set our aim is to characterize the emission of Vela Jr and distinguish it from Vela emission, and also to characterize the spectral emission of the inner remnant. We processed the eROSITA data dividing the whole remnant into seven different regions. In addition, images of the whole remnant were employed to pinpoint the position of the geometric center and constrain the proper motion of the CCO. We also employed archival XMM-Newton pointed observations of the NW rim to determine the cutoff energy of the electrons and the expansion velocity. We find the magnetic field can vary between 2 $\mu$G and 16 $\mu$G in the NW rim. We also find that the remnant spectrum is uniformly featureless in most regions, except for two inner regions where an extra thermal model component improves the fit. We obtain new coordinates for the geometric remnant center, resulting in a separation of only 35.2 $\pm$ 15.8" from the position of the CCO. As a result, we reinforce the association between the CCO and a proposed faint optical/IR counterpart., Comment: Accepted for publication in A&A

Published
2023
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21. Limits on primordial black hole evaporation from H.E.S.S. observations

Author

Hannah Dalgleish, Michael Punch, Samuel Timothy Spencer, Stefan Ohm, Stefan Klepser, M. Fuessling, Constantin Steppa, Markus Holler, Q. Remy, Felix Jankowsky, Alessandro Montanari, Stefano Gabici, Felix Aharonian, Dan Parsons, S. Steinmassl, Sami Caroff, Gianluca Giavitto, Sumari Hattingh, Takaaki Tanaka, Ramin Marx, M. Panter, Laura Olivera-Nieto, A. Yusafzai, M.-H. Grondin, U. Katz, N. Zywucka, Alison Mitchell, Krzysztof Katarzynski, Catherine Boisson, J. Bolmont, Victor Barbosa Martins, Ullrich Schwanke, P. T. O'Brien, Jhilik Majumdar, Markus Boettcher, Faical Ait-Benkhali, Dieter Horns, C. Arcaro, Floriane Cangemi, V. Poireau, Jimmy N.S. Shapopi, Jean Damascene Mbarubucyeye, Wlodek Kluzniak, Clemens Hoischen, A. A. Zdziarski, Carlo van Rensburg, Albert Seyffert, Justine Devin, Gavin Rowell, G. Vasileiadis, Johann van der Walt, V. Sahakian, K. Nakashima, Sébastien Le Stum, Denys Malyshev, Regis Terrier, Mathieu Bony, Oguzhan Anguener, Tadayuki Takahashi, Victor Doroshenko, L. Giunti, E. Kasai, Vikas Joshi, Carlo Romoli, Yves Gallant, Frank M. Rieger, Atreyee Sinha, Kirsty Feijen, K. Bernloehr, Samuel Zouari, Andreas Zmija, Christian Stegmann, Michal Ostrowski, Stefan Wagner, J.-P. Lenain, Christo Venter, Hugh Spackman, S. J. Fegan, Andreas Zech, Jason John Watson, Heinrich J. Völk, Jean-Pierre Ernenwein, M. Lemoine-Goumard, Yasunobu Uchiyama, Matthieu Renaud, Mohanraj Senniappan, L. Mohrmann, Lukasz Stawarz, Anton Dmytriiev, German Hermann, Paul Morris, Johannes Veh, Brian Reville, Connor Duffy, James Davies, Stefan Funk, Alicja Wierzcholska, Michelle Tsirou, Michael Kreter, Anne Lemiere, Rachel Simoni, Andreas Quirrenbach, Manami Sasaki, R. J. Tuffs, B. Bi, Guillem Marti'i-Devesa, Jacek Niemiec, M. Hörbe, Andreas Specovius, Andrea Santangelo, Mischa Breuhaus, Pauline Chambery, Olaf Reimer, Michael Zacharias, Emma Ona-Wilhelmi, Martin Tluczykont, Yu Wun Wong, Robert Brose, Michael Backes, Francois Brun, Thomas Lohse, Marek Jamrozy, Jaqueline Catalano, T. Chand, Thomas Murach, Arache Djannati-Ataï, P. Reichherzer, Gašper Kukec Mezek, P. Vincent, Anita Reimer, Laenita Lorraine Oberholzer, Nukri Komin, G. Lamanna, Helene Sol, R. Konno, Monica Barnard, Anna Barnacka, Heiko Salzmann, G. Peron, Vincent Marandon, Hannes Thiersen, Andrew Taylor, Garret Cotter, Tim Holch, Dmitriy Kostunin, Hend Yassin, Isak Delberth Davids, Manuel Meyer, A. Fiasson, Tom Armstrong, Celine Armand, Johannes Schaefer, Roberta Zanin, Zhiqiu Huang, Paolo Marchegiani, Vardan Baghmanyan, Naomi Tsuji, Mathieu Naurois, D. A. Prokhorov, K. Kosack, Gerard Fontaine, Brian van Soelen, David Sanchez, Santiago Pita, Werner Hofmann, Hester Schutte, Hambeleleni Ndiyavala, Gilles Maurin, J. F. Glicenstein, Thomas Tavernier, Kleopas Shiningayamwe, Bruno Khelifi, Edna Ruiz Velasco, Lenka Tomankova, Sabrina Einecke, Iryna Lypova, Yvonne Becherini, Hassan Abdalla, C. Levy, Sylvia Zhu, P. J. Meintjes, David Berge, Richard White, Jacco Vink, Heike Prokoph, Marion Spir-Jacob, David Huber, Amid Nayerhoda, Maria Haupt, Sabrina Casanova, Halim Ashkar, Fabian Leuschner, B. Rudak, Kathrin Egberts, Christopher van Eldik, Rafal Moderski, Anna Luashvili, Lott Frans, Jim Hinton, S. Sailer, Dmitry Khangulyan, Charles Thorpe-Morgan, Angel Noel, Jonathan Mackey, C. Moore, Dorit Glawion, Davit Zargaryan, Tomasz Bulik, Malgorzata Curlo, Lente Dreyer, Gaëtan Fichet de Clairfontaine, Axel Donath, A. W. Chen, Riaan Steenkamp, Fabian Schüssler, Emmanuel Moulin, Thomas Bylund, Rowan Batzofin, Jacques Muller, Hector Rueda Ricarte, Louis Du Plessis, Anu Kundu, D. Malyshev, Ira Jung, Sebastian Panny, Gerd Puehlhofer, Lei Sun, Alexandre Marcowith, Felix Werner, and Arnaud Mares

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Gravitational collapse, Evaporation, Order (ring theory), Primordial black hole, Astrophysics, Radiation, Universe, media_common, Hawking radiation
Abstract

Primordial Black Holes are expected to be formed in the early Universe by the gravitational collapse of overdense regions, among other mechanisms. They are also expected to loose their mass over time by the Hawking radiation process. As the rates of this radiation increase with temperature, the PBH evaporation should result in a violent explosion. The current upper limits on explosion rates are on the order of 10$^{4}$ − 10$^{5}$pc$^{-3}$yr$^{-1}$. In this contribution we'll present the results of a search for TeV γ-ray burst within timescale of few seconds, using nearly 5000 hours of H.E.S.S. data. The search algorithm and statistical estimation strategy will be presented as well as cosmological implications of this measurement.

Published
2022

22. Detection of new Extreme BL Lac objects with H.E.S.S. and Swift XRT

Author

Angel Priyana Noel, Hassan Abdalla, Felix Aharonian, Faical Ait-Benkhali, Oguzhan Anguener, Cornelia Arcaro, Celine Armand, Tom Armstrong, Halim Ashkar, Michael Backes, Vardan Baghmanyan, Victor Barbosa Martins, Anna Barnacka, Monica Barnard, Rowan William Batzofin, Yvonne Becherini, David Berge, Konrad Bernloehr, Baiyang Bi, Markus Böttcher, Catherine Boisson, Julien Bolmont, Mathieu Bony (de), Mischa Breuhaus, Robert Brose, Francois Brun, Tomasz Bulik, Thomas Bylund, Floriane Cangemi, Sami Caroff, Sabrina Casanova, Jaqueline Catalano, Pauline Chambery, Tej Bahadur Chand, Andrew Chen, Garret Cotter, Malgorzata Curlo, Hannah Dalgleish, Jean Damascene Mbarubucyeye, Isak Delberth Davids, James Davies, Justine Devin, Arache Djannati-Ataï, Anton Dmytriev, Axel Donath, Victor Doroshenko, Lente Dreyer, Louis Du Plessis, Connor Duffy, Kathrin Egberts, Sabrina Einecke, Jean-Pierre ERNENWEIN, Steven Fegan, Kirsty Feijen, Armand Fiasson, Gaëtan Fichet de Clairfontaine, Gerard Fontaine, Lott Frans, Matthias Fuessling, Stefan Funk, Stefano Gabici, Yves Gallant, Gianluca Giavitto, Luca Giunti, Dorit Glawion, Jean-Francois Glicenstein, Marie-Hélène Grondin, Sumari Hattingh, Maria Haupt, German HERMANN, Jim Hinton, Werner Hofmann, Clemens Hoischen, Tim Holch, Markus Holler, Dieter Horns, Zhi-Qiu Huang, David Huber, Mario Hörbe, Marek Jamrozy, Felix Jankowsky, Vikas Joshi, Ira JUNG, Eli Kasai, Krzysztof Katarzynski, Ulì Katz, Dmitry Khangulyan, Bruno Khelifi, Stefan Klepser, Wlodek Kluzniak, Nukri Komin, Ruslan Konno, Karl Kosack, Dmitriy Kostunin, Michael Kreter, Gašper Kukec Mezek, Anu Kundu, Giovanni Lamanna, Sebastien Le Stum, Anne Lemiere, Marianne Lemoine-Goumard, Jean-Philippe Lenain, Fabian Leuschner, Christelle Levy, Thomas Lohse, Anna Luashvili, Iryna Lypova, Jonathan Mackey, Jhilik Majumdar, Denys Malyshev, Dmitry Malyshev, Vincent Marandon, Paolo Marchegiani, Alexandre Marcowith, Arnaud Mares, Guillem Martí-Devesa, Ramin Marx, Gilles Maurin, Pieter Meintjes, Manuel Meyer, Alison Mitchell, Rafal Moderski, Lars Mohrmann, Alessandro Montanari, Chris Moore, Paul Morris, Emmanuel Moulin, Jacques Muller, Thomas Murach, Kaori Nakashima, Mathieu Naurois (de), Amid Nayerhoda, Hambeleleni Davids, Jacek Niemiec, Paul O'Brien, Laenita Lorraine Oberholzer, Stefan Ohm, Laura Olivera-Nieto, Emma Ona-Wilhelmi (de), Michal Ostrowski, Sebastian Panny, Michael Panter, Dan Parsons, Giada Peron, Santiago Pita, Vincent Poireau, Dmitry A Prokhorov, Heike Prokoph, Gerd PUEHLHOFER, Michael Punch, Andreas Quirrenbach, Patrick Reichherzer, Anita Reimer, Olaf Reimer, Quentin Remy, Matthieu Renaud, Brian Reville, Frank Rieger, Carlo Romoli, Gavin P Rowell, Bronislaw Rudak, Hector Rueda Ricarte, Edna Ruiz Velasco, Vardan Sahakian, Simon Sailer, Heiko Salzmann, David Sanchez, Andrea Santangelo, Manami Sasaki, Johannes Schaefer, Hester Schutte, Ullrich Schwanke, Fabian Schüssler, Mohanraj Senniappan, Albert Seyffert, Jimmy N.S. Shapopi, Kleopas Shiningayamwe, Rachel Simoni, Atreyee Sinha, Helene Sol, Hugh Spackman, Andreas Specovius, Samuel Timothy Spencer, Marion Spir-Jacob, Lukasz Stawarz, Riaan Steenkamp, Christian Stegmann, Simon Steinmassl, Constantin Steppa, Lei Sun, Tadayuki Takahashi, Takaaki Tanaka, Thomas Tavernier, Andrew Taylor, Regis Terrier, Hannes Thiersen, Charles Thorpe-Morgan, Martin Tluczykont, Lenka Tomankova, Michelle Tsirou, Naomi Tsuji, Richard Tuffs, Yasunobu Uchiyama, Johann van der Walt, Christopher van Eldik, Carlo van Rensburg, Brian van Soelen, George Vasileiadis, Johannes Veh, Christo Venter, Pascal Vincent, Jacco Vink, Heinrich J. Völk, Stefan Wagner, Jason John Watson, Felix Werner, Richard White, Alicja Wierzcholska, Yu Wun Wong, Hend Mahmoud Yassin, Anke Yusafzai, Michael Zacharias, Roberta Zanin, Davit Zargaryan, Andrzej Zdziarski, Andreas Zech, Sylvia Zhu, Andreas Zmija, Samuel Zouari, Natalia Żywucka, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), H.E.S.S., and Fermi-LAT

Subjects
accelerator, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, gamma ray: absorption, VHE, law.invention, blazar, X-ray, particle: acceleration, law, HESS, synchrotron, Radiative transfer, TeV, High Energy Stereoscopic System, 10. No inequality, Absorption (electromagnetic radiation), Blazar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), energy: high, redshift, Redshift, Synchrotron, Particle acceleration, spectral, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Extreme high synchrotron peaked blazars (EHBLs) are amongst the most powerful accelerators found in nature. Usually the synchrotron peak frequency of an EHBL is above $10^{17}\,$Hz, i.e., lies in the range of medium to hard X-rays making them ideal sources to study particle acceleration and radiative processes. EHBL objects are commonly observed at energies beyond several TeV, making them also powerful probes of gamma-ray absorption in the intergalactic medium. During the last decade, several attempts have been made to increase the number of EHBL detected at TeV energies and probe their spectral characteristics. Here we report new detections of EHBLs in the TeV energy regime, each at a redshift of less than 0.2, by the High Energy Stereoscopic System (H.E.S.S.). Also, we report on X-ray observations of these EHBLs candidates with Swift XRT. In conjunction with the very high energy observations, this allows us to probe the radiation mechanisms and the underlying particle acceleration processes., Proceedings of the 37th International Cosmic Ray Conference (ICRC 2021)

Published
2022
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23. H.E.S.S. ToO program on nearby core-collapse Supernovae : search for very-high energy γ-ray emission towards the SN candidate AT2019krl in M74

Author

German Hermann, Paul Morris, Tadayuki Takahashi, Victor Doroshenko, Ramin Marx, Marek Jamrozy, E. Kasai, Jean-Pierre Ernenwein, Helene Sol, M. Panter, Denys Malyshev, U. Katz, Stefan Klepser, Alessandro Montanari, Markus Boettcher, Jacek Niemiec, Johannes Veh, Olaf Reimer, Regis Terrier, Robert Brose, M.-H. Grondin, Paolo Marchegiani, Matthieu Renaud, Stefan Ohm, Faical Ait-Benkhali, Thomas Murach, Carlo Romoli, Frank M. Rieger, Constantin Steppa, T. Chand, Laura Olivera-Nieto, Mohanraj Senniappan, G. Peron, Stefano Gabici, A. Yusafzai, Garret Cotter, Zhiqiu Huang, D. A. Prokhorov, K. Kosack, Ullrich Schwanke, Johannes Schaefer, Sébastien Le Stum, Jean Damascene Mbarubucyeye, Wlodek Kluzniak, Arache Djannati-Ataï, Hannah Dalgleish, P. Reichherzer, Santiago Pita, Justine Devin, Hambeleleni Ndiyavala, Martin Tluczykont, Maria Haupt, J. Bolmont, G. Lamanna, M. Hörbe, Albert Seyffert, Isak Delberth Davids, A. Fiasson, Rachel Simoni, Roberta Zanin, P. T. O'Brien, Samuel Timothy Spencer, Brian Reville, Connor Duffy, C. Levy, James Davies, Dmitriy Kostunin, Gašper Kukec Mezek, Michal Ostrowski, Michael Backes, R. J. Tuffs, B. Bi, J.-P. Lenain, Jaqueline Catalano, Hugh Spackman, Dan Parsons, Halim Ashkar, Fabian Leuschner, Atreyee Sinha, Mathieu Bony, Oguzhan Anguener, S. J. Fegan, Brian van Soelen, N. Zywucka, Mischa Breuhaus, Pauline Chambery, Anton Dmytriiev, Laenita Lorraine Oberholzer, K. Nakashima, Christo Venter, Hend Yassin, Tim Holch, Kirsty Feijen, M. Fuessling, R. Konno, Manami Sasaki, Anna Barnacka, Markus Holler, Q. Remy, Felix Jankowsky, Manuel Meyer, Francois Brun, Andrew Taylor, Vikas Joshi, K. Bernloehr, P. Vincent, Anita Reimer, Krzysztof Katarzynski, Naomi Tsuji, Stefan Funk, Andrea Santangelo, Alicja Wierzcholska, Mathieu Naurois, Thomas Tavernier, Catherine Boisson, Floriane Cangemi, Gerard Fontaine, Anne Lemiere, Felix Aharonian, B. Rudak, V. Poireau, Kathrin Egberts, Jimmy N.S. Shapopi, S. Steinmassl, Sami Caroff, Heiko Salzmann, Hester Schutte, Jhilik Majumdar, Heinrich J. Völk, Andreas Specovius, Lukasz Stawarz, G. Vasileiadis, Richard White, Victor Barbosa Martins, Andreas Zmija, Jacco Vink, M. Lemoine-Goumard, Yu Wun Wong, Alison Mitchell, Jason John Watson, Celine Armand, David Huber, Andreas Quirrenbach, Sabrina Casanova, Emma Ona-Wilhelmi, Michael Kreter, Vincent Marandon, Hannes Thiersen, Guillem Marti'i-Devesa, Nukri Komin, Tom Armstrong, L. Giunti, Vardan Baghmanyan, Michael Zacharias, Christian Stegmann, Thomas Lohse, Stefan Wagner, Andreas Zech, Yasunobu Uchiyama, L. Mohrmann, Carlo van Rensburg, C. Arcaro, Christopher van Eldik, Samuel Zouari, Rafal Moderski, V. Sahakian, David Sanchez, Gavin Rowell, Michelle Tsirou, Yves Gallant, Kleopas Shiningayamwe, Werner Hofmann, Sabrina Einecke, Edna Ruiz Velasco, Iryna Lypova, Yvonne Becherini, Lenka Tomankova, Heike Prokoph, Monica Barnard, Marion Spir-Jacob, Amid Nayerhoda, Gilles Maurin, J. F. Glicenstein, Sylvia Zhu, P. J. Meintjes, David Berge, Bruno Khelifi, Jim Hinton, S. Sailer, Dmitry Khangulyan, Charles Thorpe-Morgan, Hassan Abdalla, Davit Zargaryan, Gaëtan Fichet de Clairfontaine, Axel Donath, A. W. Chen, Fabian Schüssler, Emmanuel Moulin, Gianluca Giavitto, Ira Jung, Sebastian Panny, Louis Du Plessis, Sumari Hattingh, Gerd Puehlhofer, Lei Sun, Thomas Bylund, Rowan Batzofin, Takaaki Tanaka, Alexandre Marcowith, Felix Werner, Jacques Muller, Anna Luashvili, Stuart Ryder, Lott Frans, Arnaud Mares, Hector Rueda Ricarte, Angel Noel, Jonathan Mackey, C. Moore, Dorit Glawion, D. Malyshev, Tomasz Bulik, Riaan Steenkamp, Malgorzata Curlo, Lente Dreyer, Anu Kundu, Michael Punch, Dieter Horns, Clemens Hoischen, A. A. Zdziarski, and Johann van der Walt

Subjects
Core (optical fiber), Physics, Supernova, High energy, Gamma ray, Collapse (topology), Astrophysics
Abstract

While the youngest known supernova remnants (SNRs), such as Cassiopeia A (Cas A), have been proven to be able to accelerate cosmic rays (CRs) only up to ∼ 10$^{14}$ eV at their present evolutionary stages, recent studies have shown that particle energies larger than a few PeV (10$^{15}$ eV) could be reached during the early stages of a core-collapse Supernova (cc-SN), when the high-velocity forward shock expands into the dense circumstellar medium (CSM) shaped by the stellar progenitor wind. Such environments, in particular the type IIn SNe whose progenitors may exhibit mass loss rates as high as 10$^{-2}$ M$_{\bigodot}$ yr$^{-1}$, could thus lead to γ-ray emission from $\pi ^{0}$ decay in hadronic interactions, potentially detectable with current Cherenkov telescopes at very-high energies. Such a detection would provide direct evidence for efficient acceleration of CR protons/nuclei in supernovae, and hence new insights on the long-standing issue of the origin of Galactic Cosmic Rays. In that context, the High Energy Stereoscopic System (H.E.S.S.) has been carrying out a Target of Opportunity program since 2016 to search for such an early very-high-energy γ-ray emission towards nearby core-collapse supernovae and supernova candidates (up to ∼ 10 Mpc), within a few weeks after discovery. After giving an overview of this H.E.S.S. Target of Opportunity program, we present the results obtained from the July 2019 observations towards the transient AT2019krl, originally classified as a type IIn supernova, which occurred in the galaxy M74 at ∼ 9.8 Mpc. Although its nature still remains unclear, the derived H.E.S.S. constraints on this transient are placed in the general context of the expected VHE γ-ray emission from core-collapse supernovae.

Published
2022

24. A global view of shocked plasma in the supernova remnant Puppis A provided by SRG/eROSITA

Author

Martin G. F. Mayer, Werner Becker, Peter Predehl, Manami Sasaki, and Michael Freyberg

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Context. Puppis A is a medium-age supernova remnant (SNR), which is visible as a very bright extended X-ray source. While numerous studies have investigated individual features of the SNR, at this time, no comprehensive study of the entirety of its X-ray emission exists. Aims. Using field-scan data acquired by the SRG/eROSITA telescope during its calibration and performance verification phase, we aim to investigate the physical conditions of shocked plasma and the distribution of elements throughout Puppis A. Methods. Using broad- and narrow-band imaging, we investigate the large-scale distribution of absorption and plasma temperature as well as typical emission lines. This approach is complemented by spatially resolved spectral analysis of the shocked plasma in Puppis A, for which we divide the SNR into around 700 distinct regions, resulting in maps of key physical quantities over its extent. Results. We find a strong peak of foreground absorption in the southwest quadrant, which in conjunction with high temperatures at the northeast rim creates the well-known strip of hard emission crossing Puppis A. Furthermore, using the observed distribution of ionization ages, we attempt to reconstruct the age of the shock in the individual regions. We find a quite recent shock interaction for the prominent northeast filament and ejecta knot, as well as for the outer edge of the bright eastern knot. Finally, elemental abundance maps reveal only a single clear enhancement of the plasma with ejecta material, consistent with a previously identified region, and no obvious ejecta enrichment in the remainder of the SNR. Within this region, we confirm the spatial separation of silicon-rich ejecta from those dominated by lighter elements., 20+5 pages, 10+5 figures; Accepted by A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission; Abstract abridged

Published
2021

25. Tracking down the origin of superbubbles and supergiant shells in the Magellanic Clouds with Minkowski tensor analysis

Author

Klaus Mecke, Manami Sasaki, Caroline Collischon, Sean D. Points, and Michael A. Klatt

Subjects
Physics, Star formation, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Supernova, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Emission spectrum, Small Magellanic Cloud, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

We develop an automatic bubble-recognition routine based on Minkowski functionals (MF) and tensors (MT) to detect bubble-like interstellar structures in optical emission line images. Minkowski functionals and MT are powerful mathematical tools for parameterizing the shapes of bodies. Using the papaya2-library, we created maps of the desired MF or MT of structures at a given window size. We used maps of the irreducible MT $\psi_2$, which is sensitive to elongation, to find filamentary regions in H$\alpha$, [SII], and [OIII] images of the Magellanic Cloud Emission Line Survey (MCELS). Using the phase of $\psi_2$, we were able to draw lines perpendicular to each filament and thus obtain line-density maps. This allowed us to find the center of a bubble-like structure and to detect structures at different window sizes. The detected bubbles in all bands are spatially correlated to the distribution of massive stars, showing that we indeed detect interstellar bubbles without large spatial bias. Eighteen out of 59 supernova remnants in the Large Magellanic Cloud (LMC) and 13 out of 20 superbubbles are detected in at least one wavelength. The lack of detection is mostly due to surrounding emission that disturbs the detection, a too small size, or the lack of a (circular) counterpart in our emission line images. In line-density maps at larger scales, maxima can be found in regions with high star formation in the past, often inside supergiant shells (SGS). In SGS LMC 2, there is a maximum west of the shell where a collision of large gas clouds is thought to have occurred. In the Small Magellanic Cloud (SMC), bubble detection is impaired by the more complex projected structure of the galaxy. Line maps at large scales show large filaments in the SMC in a north-south direction, especially in the [SII] image. The origin of these filaments is unknown., Comment: 19 pages, 27 figures. Accepted for publication in Astronomy & Astrophysics

Published
2021

26. Is PKS 0625-354 another variable TeV active galactic nucleus?

Author

Halim Ashkar, Fabian Leuschner, Gilles Maurin, Riaan Steenkamp, J. F. Glicenstein, Heike Prokoph, Bruno Khelifi, Floriane Cangemi, Michael Punch, Gianluca Giavitto, Anna Luashvili, Lott Frans, Sumari Hattingh, Martin Tluczykont, Marek Jamrozy, Sabrina Einecke, Takaaki Tanaka, Iryna Lypova, Marion Spir-Jacob, Yvonne Becherini, Helene Sol, Rachel Simoni, Davit Zargaryan, Hannah Dalgleish, Jim Hinton, Gašper Kukec Mezek, Gaëtan Fichet de Clairfontaine, Axel Donath, A. W. Chen, S. Sailer, Dmitry Khangulyan, Charles Thorpe-Morgan, Andreas Zmija, Amid Nayerhoda, M. Lemoine-Goumard, Stefan Klepser, Alessandro Montanari, C. Arcaro, S. J. Fegan, Anu Kundu, B. Rudak, T. Chand, Hend Yassin, Michael Kreter, Paolo Marchegiani, Tadayuki Takahashi, Dmitriy Kostunin, Mathieu Bony, Oguzhan Anguener, Fabian Schüssler, Manuel Meyer, Markus Boettcher, Gavin Rowell, Kathrin Egberts, Maria Haupt, Victor Doroshenko, Emmanuel Moulin, Ira Jung, Brian van Soelen, Sebastian Panny, Mathieu Naurois, E. Kasai, Kirsty Feijen, Samuel Timothy Spencer, Dieter Horns, Vikas Joshi, Thomas Tavernier, Johannes Schaefer, Gerd Puehlhofer, Lei Sun, Constantin Steppa, Jacek Niemiec, Hassan Abdalla, Albert Seyffert, Olaf Reimer, Christian Stegmann, Stefan Wagner, Andreas Zech, Alexandre Marcowith, Regis Terrier, Felix Werner, Yasunobu Uchiyama, K. Nakashima, K. Bernloehr, Carlo Romoli, Hector Rueda Ricarte, Lukasz Stawarz, Frank M. Rieger, Thomas Murach, Kleopas Shiningayamwe, Clemens Hoischen, A. A. Zdziarski, Christopher van Eldik, N. Zywucka, Jaqueline Catalano, L. Mohrmann, Monica Barnard, Rafal Moderski, Heinrich J. Völk, Arnaud Mares, Ullrich Schwanke, Stefan Ohm, Thomas Bylund, Rowan Batzofin, Anita Reimer, Andreas Quirrenbach, Edna Ruiz Velasco, Johann van der Walt, Jhilik Majumdar, Guillem Marti'i-Devesa, R. Konno, Jacques Muller, Dan Parsons, Jean Damascene Mbarubucyeye, Wlodek Kluzniak, Lenka Tomankova, Stefano Gabici, Andrew Taylor, Michael Zacharias, Christo Venter, Sylvia Zhu, P. J. Meintjes, David Berge, M. Hörbe, Michael Backes, Robert Brose, V. Poireau, Jimmy N.S. Shapopi, V. Sahakian, Krzysztof Katarzynski, Brian Reville, Connor Duffy, Laenita Lorraine Oberholzer, Tim Holch, Anton Dmytriiev, M. Fuessling, Manami Sasaki, G. Vasileiadis, Catherine Boisson, Arache Djannati-Ataï, P. Reichherzer, J. Bolmont, Jason John Watson, D. Malyshev, Andrea Santangelo, Naomi Tsuji, Matthieu Renaud, Denys Malyshev, Isak Delberth Davids, G. Lamanna, James Davies, A. Fiasson, Roberta Zanin, Yves Gallant, S. Steinmassl, Sami Caroff, R. J. Tuffs, Gerard Fontaine, B. Bi, Santiago Pita, Hambeleleni Ndiyavala, Hester Schutte, Justine Devin, Mohanraj Senniappan, C. Levy, Mischa Breuhaus, Pauline Chambery, Andreas Specovius, Jean-Pierre Ernenwein, Yu Wun Wong, Johannes Veh, Vincent Marandon, Hannes Thiersen, Vardan Baghmanyan, Markus Holler, Q. Remy, Felix Jankowsky, Richard White, Felix Aharonian, Jacco Vink, Alison Mitchell, David Huber, Sabrina Casanova, Louis Du Plessis, Angel Noel, Jonathan Mackey, Anna Barnacka, C. Moore, Victor Barbosa Martins, Dorit Glawion, Carlo van Rensburg, Anne Lemiere, Tomasz Bulik, Malgorzata Curlo, Emma Ona-Wilhelmi, Samuel Zouari, Thomas Lohse, Lente Dreyer, Michal Ostrowski, J.-P. Lenain, Hugh Spackman, Stefan Funk, Alicja Wierzcholska, Ramin Marx, M. Panter, U. Katz, Faical Ait-Benkhali, G. Peron, Garret Cotter, Sébastien Le Stum, Zhiqiu Huang, D. A. Prokhorov, K. Kosack, P. T. O'Brien, Atreyee Sinha, Laura Olivera-Nieto, A. Yusafzai, Nukri Komin, Tom Armstrong, David Sanchez, Werner Hofmann, L. Giunti, Michelle Tsirou, Francois Brun, P. Vincent, Heiko Salzmann, Celine Armand, M.-H. Grondin, German Hermann, and Paul Morris

Subjects
Physics, Brightness, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Viewing angle, Variable (computer science), symbols.namesake, symbols, Spectral energy distribution, Blazar, Doppler effect, Astrophysics::Galaxy Astrophysics
Abstract

The majority of the active galactic nuclei (AGN) detected at very-high-energies above 100 GeV belong to the class of blazars with a small angle between the jet-axis and the line-of-sight. Only about 10 percent of the gamma-ray AGN are objects with a larger viewing angle resulting in a smaller Doppler boosting of the emission. Originally, it was believed that gamma-ray emission can only be observed from blazars and those are variable in its brightness. Instead, the last years have shown that non-blazar active galaxies also show a fascinating variability behaviour which provide important new insights into the physical processes responsible for the gamma-ray production and especially for flaring events. Here, we report on the observation of gamma-ray variability of the active galaxy PKS 0625−354 detected with the H.E.S.S. telescopes in November 2018. The classification of PKS 0625−354 is a still matter of debate. The H.E.S.S. measurements were performed as part of a flux observing program and showed in the first night of the observation a detection of the object with > 5σ. A denser observation campaign followed for the next nine nights resulting in a decrease of the gamma-ray flux. Those observations were accompanied with Swift in the X-ray and UV/optical band allowing for the reconstruction of a multi-band broad-band spectral energy distribution. We will discuss the implications of the gamma-ray variability of the object.

Published
2021
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27. Search for dark matter annihilation towards the inner Milky Way halo with the H.E.S.S. Inner Galaxy Survey

Author

Clemens Hoischen, A. A. Zdziarski, Robert Brose, Johann van der Walt, Halim Ashkar, Fabian Leuschner, Stefan Ohm, L. Giunti, Albert Seyffert, Davit Zargaryan, Stefan Klepser, Alessandro Montanari, K. Nakashima, Gaëtan Fichet de Clairfontaine, Sabrina Einecke, Axel Donath, A. W. Chen, Iryna Lypova, K. Bernloehr, Heinrich J. Völk, Yvonne Becherini, Stefano Gabici, Michelle Tsirou, Anna Luashvili, Vikas Joshi, J. Bolmont, Fabian Schüssler, M.-H. Grondin, Emmanuel Moulin, Andreas Specovius, Kleopas Shiningayamwe, Anne Lemiere, B. Rudak, Lott Frans, Michael Punch, Edna Ruiz Velasco, Sylvia Zhu, P. J. Meintjes, David Berge, Michael Backes, Matthieu Renaud, German Hermann, Paul Morris, Kathrin Egberts, Constantin Steppa, Tadayuki Takahashi, Laenita Lorraine Oberholzer, Tim Holch, Lukasz Stawarz, Louis Du Plessis, Naomi Tsuji, V. Poireau, Jimmy N.S. Shapopi, Victor Doroshenko, Yu Wun Wong, Emma Ona-Wilhelmi, Riaan Steenkamp, E. Kasai, G. Lamanna, Ullrich Schwanke, Gerard Fontaine, Jim Hinton, Victor Barbosa Martins, Thomas Lohse, Frank M. Rieger, Hester Schutte, Carlo van Rensburg, Francois Brun, P. Vincent, Heiko Salzmann, Mathieu Bony, Oguzhan Anguener, Kirsty Feijen, S. Sailer, Dmitry Khangulyan, Charles Thorpe-Morgan, Ramin Marx, Dmitriy Kostunin, M. Panter, U. Katz, Jean Damascene Mbarubucyeye, Wlodek Kluzniak, Jaqueline Catalano, R. Konno, Hector Rueda Ricarte, T. Chand, Samuel Zouari, P. T. O'Brien, M. Hörbe, Celine Armand, Andreas Quirrenbach, Guillem Marti'i-Devesa, Faical Ait-Benkhali, Andrew Taylor, G. Vasileiadis, Vincent Marandon, Brian van Soelen, Marek Jamrozy, Hannes Thiersen, Dieter Horns, Hassan Abdalla, Thomas Bylund, Rowan Batzofin, Sébastien Le Stum, Thomas Tavernier, Gilles Maurin, Floriane Cangemi, Helene Sol, Christian Stegmann, Jacques Muller, Vardan Baghmanyan, Johannes Schaefer, J. F. Glicenstein, Anu Kundu, Stefan Wagner, Andreas Zech, Yasunobu Uchiyama, Monica Barnard, L. Mohrmann, Arache Djannati-Ataï, C. Levy, Atreyee Sinha, Bruno Khelifi, Michal Ostrowski, J.-P. Lenain, Hugh Spackman, Michael Zacharias, Regis Terrier, Hannah Dalgleish, P. Reichherzer, Andreas Zmija, Gianluca Giavitto, Jacek Niemiec, M. Lemoine-Goumard, Paolo Marchegiani, Markus Holler, Carlo Romoli, Isak Delberth Davids, Stefan Funk, Alicja Wierzcholska, Olaf Reimer, Q. Remy, Felix Jankowsky, Michael Kreter, Anna Barnacka, Brian Reville, Connor Duffy, A. Fiasson, Roberta Zanin, Thomas Murach, Heike Prokoph, James Davies, Sumari Hattingh, Felix Aharonian, Richard White, Angel Noel, M. Fuessling, R. J. Tuffs, B. Bi, Christo Venter, Takaaki Tanaka, D. Malyshev, Jonathan Mackey, Jacco Vink, Ira Jung, Sebastian Panny, Alison Mitchell, Anita Reimer, David Huber, Sabrina Casanova, Marion Spir-Jacob, Mischa Breuhaus, Pauline Chambery, Gerd Puehlhofer, C. Arcaro, C. Moore, Jhilik Majumdar, Lei Sun, Santiago Pita, Hambeleleni Ndiyavala, S. Steinmassl, Sami Caroff, Anton Dmytriiev, Dorit Glawion, G. Peron, Garret Cotter, Alexandre Marcowith, Felix Werner, Amid Nayerhoda, Manami Sasaki, Tomasz Bulik, Zhiqiu Huang, Malgorzata Curlo, Maria Haupt, Andrea Santangelo, Arnaud Mares, Lente Dreyer, D. A. Prokhorov, K. Kosack, V. Sahakian, Gavin Rowell, Jean-Pierre Ernenwein, N. Zywucka, Denys Malyshev, Markus Boettcher, Yves Gallant, Christopher van Eldik, Rafal Moderski, Johannes Veh, Samuel Timothy Spencer, Mohanraj Senniappan, Rachel Simoni, Dan Parsons, Krzysztof Katarzynski, Catherine Boisson, Justine Devin, Lenka Tomankova, Martin Tluczykont, Gašper Kukec Mezek, Hend Yassin, Manuel Meyer, Mathieu Naurois, Jason John Watson, S. J. Fegan, Nukri Komin, Tom Armstrong, David Sanchez, Werner Hofmann, Laura Olivera-Nieto, and A. Yusafzai

Subjects
Physics, Annihilation, WIMP, Milky Way, Weakly interacting massive particles, media_common.quotation_subject, Dark matter, Astrophysics::Cosmology and Extragalactic Astrophysics, Halo, Astrophysics, Galaxy, Universe, media_common
Abstract

The presence of dark matter (DM) is suggested by a wealth of astrophysical and cosmological measurements. However, its underlying nature is yet unknown. Among the most promising candidates are weakly interacting massive particles (WIMPs): particles with mass and coupling strength at the electroweak scale and thermally produced in the early universe have a present relic density consistent with that observed today. WIMP self-annihilation would produce Standard Model particles including gamma-rays, which have been long-time recognized as a prime messenger to indirectly detect dark matter signals. The centre of the Milky Way is predicted as the brightest source of DM annihilations. The H.E.S.S. collaboration is currently performing a survey of the inner region of the Milky Way, the Inner Galaxy Survey (IGS), intended to achieve the best sensitivity to faint and diffuse emissions in a region of several degrees around the Galactic Centre. We analyzed 2014-2020 observations taken with the five-telescope array to search for a DM annihilation signal. With the current dataset of about 550 hours, we found no significant excess and therefore derived strong constraints on the velocity-weighted annihilation cross-section. TeV thermal WIMPs can be probed in different annihilation channels.

Published
2021
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28. SN 1987A : Tracing the flux decline and spectral evolution through a comparison of SRG/eROSITA and XMM-Newton observations

Author

Frank Haberl, Chandreyee Maitra, Michael Freyberg, P. Maggi, Konrad Dennerl, Manami Sasaki, Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Time evolution, Equatorial ring, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Shock (mechanics), Supernova, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Supergiant, Ejecta, Supernova remnant, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

SN 1987A is the closest observed supernova in the last four centuries and provides a unique opportunity to witness the birth and evolution of a supernova remnant. The source has been monitored by XMM Newton EPIC-pn from 2007--2020. SRG/eROSITA also observed the source during its commissioning phase and the first light in Sept. and Oct. 2019. We investigated the spectral and flux evolution of SN 1987A in X-rays over the last fourteen years up to Nov. 2020 using XMM-Newton and eROSITA observations. We performed a detailed spectral analysis using a three-component plane-parallel shock model and analysed and modelled the EPIC-pn monitoring and eROSITA observations in a consistent manner. This paper reports a complete and most up to date flux evolution of SN 1987A in the soft (0.5-2 keV) and hard (3-10 keV) X-ray band. The flux in the soft band flattened around 9424 d and then displayed a turnover between 10142-10493 d after which it showed a continued decline. Around the same time, a break in the hard-band flux time evolution slope was detected. This implies that the blast wave has now passed beyond the dense structures of the equatorial ring and is expanding further into more tenuous circumstellar medium. The temporal evolution of the normalizations of the three shock components match well the results of hydrodynamical simulations predicting a blue supergiant progenitor scenario. The trend at recent epochs indicate that the emission caused by the forward shock after leaving the equatorial ring and by the reverse shock in the ejecta is becoming more dominant now. The elemental abundances in the hot plasma component are significantly higher than those in the `cooler' one, indicating its origin from the reverse shock propagating into the ejecta., 11 pages, 7 figures, 7 tables, Accepted in A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission

Published
2021

29. The eROSITA Final Equatorial-Depth Survey (eFEDS): Presenting The Demographics of X-ray Emission From Normal Galaxies

Author

Ann Hornschemeier, Hermann Brunner, Andrea Merloni, Manami Sasaki, Andrea Santangelo, Frank Haberl, Mara Salvato, Konstantinos Kovlakas, Chandreyee Maitra, N. Vulic, Kirpal Nandra, E. Kyritsis, Jörn Wilms, Andy Ptak, A. Bogdan, Georg Lamer, Andreas Zezas, Tom Dwelly, Tong Liu, and A. Basu-Zych

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Demographics, United States Naval Observatory, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Infrared Processing and Analysis Center, Space and Planetary Science, Observatory, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Space research, National laboratory, Data archive, Web site
Abstract

The $\it{eROSITA}$ Final Equatorial Depth Survey (eFEDS), completed during the calibration and performance verification phase of the $\it{eROSITA}$ instrument on $\it{Spectrum\, Roentgen\, Gamma}$, delivers data at and beyond the final depth of the four-year $\it{eROSITA}$ all-sky survey (eRASS:8), $f_{0.5-2\,\text{ keV}}$ = $1.1\times10^{-14}$ erg s$^{-1}$ cm$^{2}$, over 140 deg$^{2}$. It provides the first view of normal galaxy X-ray emission from X-ray binaries (XRBs) and the hot interstellar medium at the full depth of eRASS:8. We use the Heraklion Extragalactic Catalogue (HECATE) of galaxies to correlate with eFEDS X-ray sources and identify 94 X-ray detected normal galaxies. We classify galaxies as star-forming, early-type, composite, and AGN using SDSS and 6dF optical spectroscopy. The eFEDS field harbours 37 normal galaxies: 36 late-type (star-forming) galaxies and 1 early-type galaxy. There are 1.9 times as many normal galaxies as predicted by scaling relations via SIXTE simulations, with an overabundance of late-type galaxies and a dearth of early-type galaxies. Dwarf galaxies with high specific star formation rate (SFR) have elevated L$_{\text{X}}$/SFR when compared with specific SFR and metallicity, indicating an increase in XRB emission due to low-metallicity. We expect that eRASS:8 will detect 12,500 normal galaxies, the majority of which will be star-forming, with the caveat that there are unclassified sources in eFEDS and galaxy catalogue incompleteness issues that could increase the actual number of detected galaxies over these current estimates. eFEDS observations detected a rare population of galaxies -- the metal-poor dwarf starbursts -- that do not follow known scaling relations. eRASS is expected to discover significant numbers of these high-redshift analogues, which are important for studying the heating of the intergalactic medium at high-redshift., Comment: 17 pages, 10 figures, 3 tables. Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission

Published
2021
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31. The eROSITA X-ray telescope on SRG

Author

Robert Andritschke, Christian Schmid, Joern Wilms, T. Mernik, Josef Eder, C. Tenzer, Mara Salvato, Lothar Strüder, Lars Tiedemann, Michael Freyberg, V. Arefiev, E. Churazov, V. Babyshkin, Esra Bulbul, Benjamin Mican, H. Scheuerle, Axel Schwope, Hermann Brunner, D. Coutinho, Georg Lamer, Jan Robrade, Miriam E. Ramos-Ceja, Heinrich Bräuninger, Elmar Pfeffermann, Kirpal Nandra, Peter Friedrich, Marcella Brusa, Tanja Eraerds, Joachim Trümper, I. Lomakin, I. Lapshov, Antonis Georgakakis, Joseph J. Mohr, W. Kink, A. Gueguen, Thomas H. Reiprich, Vadim Burwitz, Daniel Pietschner, Frank Haberl, N. Clerc, Jonas Reiffers, Ian M. Stewart, O. Batanov, Chandreyee Maitra, Katharina Borm, M. Buntov, V. Nazarov, Th. Boller, Alexis Finoguenov, Sebastian Müller, Emanuele Perinati, Matthias Steinmetz, A. Shirshakov, S. Friedrich, Valeri Yaroshenko, F. Korotkov, Peter Predehl, Andreas von Kienlin, P. Weber, Valentin Emberger, M. N. Pavlinsky, Florian Pacaud, W. Bornemann, Thomas Dauser, Marcus Brüggen, Norbert Meidinger, Gisela Hartner, Konrad Dennerl, A. V. Bogomolov, O. Hälker, P. Gureev, B. Menz, Wolfgang Burkert, Jeremy S. Sanders, Werner Becker, Andrea Merloni, Rashid Sunyaev, Long Ji, V. Voron, S. Granato, Maria Fürmetz, Manami Sasaki, Andrea Santangelo, Hans Böhringer, Guenther Hasinger, Arne Rau, Victor Doroshenko, H. Huber, Ingo Kreykenbohm, Tie Liu, Marat Gilfanov, Christoph Grossberger, Jürgen H. M. M. Schmitt, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Predehl P., Andritschke R., Arefiev V., Babyshkin V., Batanov O., Becker W., Boehringer H., Bogomolov A., Boller T., Borm K., Bornemann W., Br'auninger H., Br'uggen M., Brunner H., Brusa M., Bulbul E., Buntov M., Burwitz V., Burkert W., Clerc N., Churazov E., Coutinho D., Dauser T., Dennerl K., Doroshenko V., Eder J., Emberger V., Eraerds T., Finoguenov A., Freyberg M., Friedrich P., Friedrich S., Fuermetz M., Georgakakis A., Gilfanov M., Granato S., Grossberger C., Gueguen A., Gureev P., Haberl F., Haelker O., Hartner G., Hasinger G., Huber H., Ji L., Kienlin A., v., Kink W., Korotkov F., Kreykenbohm I., Lamer G., Lomakin I., Lapshov I., Liu T., Maitra C., Meidinger N., Menz B., Merloni A., Mernik T., Mican B., Mohr J., M'uller S., Nandra K., Nazarov V., Pacaud F., Pavlinsky M., Perinati E., Pfeffermann E., Pietschner D., Ramos-Ceja M.,~E., Rau A., Reiffers J., Reiprich T.,~H., Robrade J., Salvato M., Sanders J., Santangelo A., Sasaki M., Scheuerle H., Schmid C., Schmitt J., Schwope A., Shirshakov A., Steinmetz M., Stewart I., Strueder L., Sunyaev R., Tenzer C., Tiedemann L., Truemper J., Voron V., Weber P., Wilms J., Yaroshenko V., Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
X-rays general, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, X-ray telescope, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, 7. Clean energy, law.invention, Telescope, space vehicles: instruments, X-rays: general, surveys, dark energy, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, law, 0103 physical sciences, ROSAT, Dark energy, Space vehicles instruments, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Celestial sphere, Galaxy, Redshift, Space and Planetary Science, Sky, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the primary instrument on the Spectrum-Roentgen-Gamma (SRG) mission, which was successfully launched on July 13, 2019, from the Baikonour cosmodrome. After the commissioning of the instrument and a subsequent calibration and performance verification phase, eROSITA started a survey of the entire sky on December 13, 2019. By the end of 2023, eight complete scans of the celestial sphere will have been performed, each lasting six months. At the end of this program, the eROSITA all-sky survey in the soft X-ray band (0.2--2.3\,keV) will be about 25 times more sensitive than the ROSAT All-Sky Survey, while in the hard band (2.3--8\,keV) it will provide the first ever true imaging survey of the sky. The eROSITA design driving science is the detection of large samples of galaxy clusters up to redshifts $z>1$ in order to study the large-scale structure of the universe and test cosmological models including Dark Energy. In addition, eROSITA is expected to yield a sample of a few million AGNs, including obscured objects, revolutionizing our view of the evolution of supermassive black holes. The survey will also provide new insights into a wide range of astrophysical phenomena, including X-ray binaries, active stars, and diffuse emission within the Galaxy. Results from early observations, some of which are presented here, confirm that the performance of the instrument is able to fulfil its scientific promise. With this paper, we aim to give a concise description of the instrument, its performance as measured on ground, its operation in space, and also the first results from in-orbit measurements., 16 pages, 19 figures, accepted by Astronomy & Astrophysics

Published
2021
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32. GALACTIC AND EXTRAGALACTIC SUPERNOVA REMNANTS AS SITES OF PARTICLE ACCELERATION

Author

Manami Sasaki

Subjects
Engineering (General). Civil engineering (General), TA1-2040
Abstract

Supernova remnants, owing to their strong shock waves, are likely sources of Galactic cosmic rays. Studies of supernova remnants in X-rays and gamma rays provide us with new insights into the acceleration of particles to high energies. This paper reviews the basic physics of supernova remnant shocks and associated particle acceleration and radiation processes. In addition, the study of supernova remnant populations in nearby galaxies and the implications for Galactic cosmic ray distribution are discussed.

Published
2013
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33. The young massive stellar cluster Westerlund 1 in gamma rays as seen with H.E.S.S

Author

Lars Mohrmann, Hassan Abdalla, Felix Aharonian, Faical Ait-Benkhali, Oguzhan Anguener, Cornelia Arcaro, Celine Armand, Tom Armstrong, Halim Ashkar, Michael Backes, Vardan Baghmanyan, Victor Barbosa Martins, Anna Barnacka, Monica Barnard, Rowan William Batzofin, Yvonne Becherini, David Berge, Konrad Bernloehr, Baiyang Bi, Markus Böttcher, Catherine Boisson, Julien Bolmont, Mathieu Bony (de), Mischa Breuhaus, Robert Brose, Francois Brun, Tomasz Bulik, Thomas Bylund, Floriane Cangemi, Sami Caroff, Sabrina Casanova, Jaqueline Catalano, Pauline Chambery, Tej Bahadur Chand, Andrew Chen, Garret Cotter, Malgorzata Curlo, Hannah Dalgleish, Jean Damascene Mbarubucyeye, Isak Delberth Davids, James Davies, Justine Devin, Arache Djannati-Ataï, Anton Dmytriev, Axel Donath, Victor Doroshenko, Lente Dreyer, Louis Du Plessis, Connor Duffy, Kathrin Egberts, Sabrina Einecke, Jean-Pierre ERNENWEIN, Steven Fegan, Kirsty Feijen, Armand Fiasson, Gaëtan Fichet de Clairfontaine, Gerard Fontaine, Lott Frans, Matthias Fuessling, Stefan Funk, Stefano Gabici, Yves Gallant, Gianluca Giavitto, Luca Giunti, Dorit Glawion, Jean-Francois Glicenstein, Marie-Hélène Grondin, Sumari Hattingh, Maria Haupt, German HERMANN, Jim Hinton, Werner Hofmann, Clemens Hoischen, Tim Holch, Markus Holler, Dieter Horns, Zhi-Qiu Huang, David Huber, Mario Hörbe, Marek Jamrozy, Felix Jankowsky, Vikas Joshi, Ira JUNG, Eli Kasai, Krzysztof Katarzynski, Ulì Katz, Dmitry Khangulyan, Bruno Khelifi, Stefan Klepser, Wlodek Kluzniak, Nukri Komin, Ruslan Konno, Karl Kosack, Dmitriy Kostunin, Michael Kreter, Gašper Kukec Mezek, Anu Kundu, Giovanni Lamanna, Sebastien Le Stum, Anne Lemiere, Marianne Lemoine-Goumard, Jean-Philippe Lenain, Fabian Leuschner, Christelle Levy, Thomas Lohse, Anna Luashvili, Iryna Lypova, Jonathan Mackey, Jhilik Majumdar, Denys Malyshev, Dmitry Malyshev, Vincent Marandon, Paolo Marchegiani, Alexandre Marcowith, Arnaud Mares, Guillem Martí-Devesa, Ramin Marx, Gilles Maurin, Pieter Meintjes, Manuel Meyer, Alison Mitchell, Rafal Moderski, Alessandro Montanari, Chris Moore, Paul Morris, Emmanuel Moulin, Jacques Muller, Thomas Murach, Kaori Nakashima, Mathieu Naurois (de), Amid Nayerhoda, Hambeleleni Davids, Jacek Niemiec, Angel Noel, Paul O'Brien, Laenita Lorraine Oberholzer, Stefan Ohm, Laura Olivera-Nieto, Emma Ona-Wilhelmi (de), Michal Ostrowski, Sebastian Panny, Michael Panter, Dan Parsons, Giada Peron, Santiago Pita, Vincent Poireau, Dmitry A Prokhorov, Heike Prokoph, Gerd PUEHLHOFER, Michael Punch, Andreas Quirrenbach, Romed Rauth, Patrick Reichherzer, Anita Reimer, Olaf Reimer, Quentin Remy, Matthieu Renaud, Brian Reville, Frank Rieger, Carlo Romoli, Gavin P Rowell, Bronislaw Rudak, Hector Rueda Ricarte, Edna Ruiz Velasco, Vardan Sahakian, Simon Sailer, Heiko Salzmann, David Sanchez, Andrea Santangelo, Manami Sasaki, Johannes Schaefer, Hester Schutte, Ullrich Schwanke, Fabian Schüssler, Mohanraj Senniappan, Albert Seyffert, Jimmy N.S. Shapopi, Kleopas Shiningayamwe, Rachel Simoni, Atreyee Sinha, Helene Sol, Hugh Spackman, Andreas Specovius, Samuel Timothy Spencer, Marion Spir-Jacob, Lukasz Stawarz, Riaan Steenkamp, Christian Stegmann, Simon Steinmassl, Constantin Steppa, Lei Sun, Tadayuki Takahashi, Takaaki Tanaka, Thomas Tavernier, Andrew Taylor, Regis Terrier, Hannes Thiersen, Charles Thorpe-Morgan, Martin Tluczykont, Lenka Tomankova, Michelle Tsirou, Naomi Tsuji, Richard Tuffs, Yasunobu Uchiyama, Johann van der Walt, Christopher van Eldik, Carlo van Rensburg, Brian van Soelen, George Vasileiadis, Johannes Veh, Christo Venter, Pascal Vincent, Jacco Vink, Heinrich J. Völk, Stefan Wagner, Jason John Watson, Felix Werner, Richard White, Alicja Wierzcholska, Yu Wun Wong, Hend Mahmoud Yassin, Anke Yusafzai, Michael Zacharias, Roberta Zanin, Davit Zargaryan, Andrzej Zdziarski, Andreas Zech, Sylvia Zhu, Andreas Zmija, Samuel Zouari, Natalia Żywucka, Naurois , Mathieu, Ona-Wilhelmi , Emma, and Bony , Mathieu

Subjects
Physics, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Hadron, Gamma ray, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Likelihood analysis, Energy spectrum, Cluster (physics), ddc:530, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

37th International Cosmic Ray Conference, ICRC 2021, Berlin, online, Germany, 12 Jul 2021 - 23 Jul 2021; Proceedings of Science / International School for Advanced Studies (ICRC2021), 789 (2021). doi:10.22323/1.395.0789, Massive stellar clusters have recently been hypothesised as candidates for the acceleration of hadronic cosmic rays up to PeV energies. Previously, the H.E.S.S. Collaboration has reported about very extended $\gamma$-ray emission around Westerlund 1, a massive young stellar cluster in the Milky Way. In this contribution we present an updated analysis that employs a new analysis technique and is based on a much larger data set, allowing us to constrain better the morphology and the energy spectrum of the emission. The analysis technique used is a three-dimensional likelihood analysis, which is especially well suited for largely extended sources. The origin of the $\gamma$-ray emission will be discussed in light of multi-wavelength observations., Published by SISSA, Trieste

Published
2021
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34. First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA

Author

Frank Haberl, Lister Staveley-Smith, Miroslav Filipovic, Chandreyee Maitra, Jonathan Knies, Manami Sasaki, Michael Freyberg, Sean D Points, Konrad Dennerl, Jürgen Kerp, Andrei M. Bykov, and Bärbel S. Koribalski

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Stellar population, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Superbubble, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, Interstellar medium, Stars, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics
Abstract

In the first months after the launch in July 2019, eROSITA onboard Spektr-RG (SRG) performed long-exposure observations in the regions around SN 1987A and SNR N132D in the Large Magellanic Cloud (LMC). We analyse the distribution and the spectrum of the diffuse X-ray emission in the observed fields to determine the physical properties of the hot phase of the interstellar medium (ISM). The eROSITA data are complemented by newly derived column density maps for the Milky Way and the LMC, 888 MHz radio continuum map from the Australian Square Kilometer Array Pathfinder (ASKAP), and optical images of the Magellanic Cloud Emission Line Survey (MCELS). We detect significant emission from thermal plasma with kT=0.2 keV in all the regions. There is also an additional higher-temperature emission component from a plasma with kT = 0.7 keV. In addition, non-thermal X-ray emission is significantly detected in the superbubble 30 Dor C. The absorbing column density NH in the LMC derived from the analysis of the X-ray spectra taken with eROSITA is consistent with the NH obtained from the emission of the cold medium over the entire area. Neon abundance is enhanced in the regions in and around 30 Dor and SN 1987A, indicating that the ISM has been chemically enriched by the young stellar population. Emission from the stellar cluster RMC 136 and the Wolf-Rayet stars RMC 139 and RMC 140 is best modelled with a high-temperature (kT>1 keV) non-equilibrium ionisation plasma emission and a non-thermal component with a photon index of {\Gamma} =1.3. In addition, the optical SNR candidate J0529-7004 is also detected with eROSITA and we thus confirm the source as an SNR., Comment: Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission

Published
2021
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35. Deep observations of Kepler's SNR with H.E.S.S

Author

Jason John Watson, Kleopas Shiningayamwe, Edna Ruiz Velasco, Lenka Tomankova, Martin Tluczykont, Gašper Kukec Mezek, Hend Yassin, Manuel Meyer, Mathieu Naurois, Anton Dmytriiev, Manami Sasaki, Riaan Steenkamp, Andrea Santangelo, T. Chand, Gilles Maurin, J. F. Glicenstein, Jhilik Majumdar, Johannes Schaefer, Christian Stegmann, Stefan Wagner, Andreas Zech, Yasunobu Uchiyama, Bruno Khelifi, Anu Kundu, Hector Rueda Ricarte, Davit Zargaryan, Jacek Niemiec, L. Mohrmann, Arache Djannati-Ataï, Albert Seyffert, V. Sahakian, Anna Barnacka, P. Reichherzer, Gaëtan Fichet de Clairfontaine, Axel Donath, A. W. Chen, Ira Jung, Olaf Reimer, G. Peron, Christo Venter, Garret Cotter, Sebastian Panny, K. Nakashima, K. Bernloehr, Isak Delberth Davids, Victor Barbosa Martins, A. Fiasson, Roberta Zanin, Yves Gallant, Fabian Schüssler, Michael Backes, Heinrich J. Völk, Gerd Puehlhofer, Lei Sun, Thomas Murach, Jean-Pierre Ernenwein, Emmanuel Moulin, G. Lamanna, V. Poireau, Jimmy N.S. Shapopi, Alexandre Marcowith, Felix Werner, Laenita Lorraine Oberholzer, Tim Holch, Naomi Tsuji, Carlo van Rensburg, Zhiqiu Huang, D. A. Prokhorov, K. Kosack, Tadayuki Takahashi, Markus Holler, Q. Remy, Felix Jankowsky, Victor Doroshenko, Felix Aharonian, Johannes Veh, Gerard Fontaine, E. Kasai, G. Vasileiadis, M.-H. Grondin, Anne Lemiere, Floriane Cangemi, Arnaud Mares, Samuel Zouari, Denys Malyshev, Alison Mitchell, Samuel Timothy Spencer, Hester Schutte, Stefan Klepser, Andreas Specovius, Alessandro Montanari, Andreas Zmija, Clemens Hoischen, A. A. Zdziarski, M. Lemoine-Goumard, Emma Ona-Wilhelmi, Yu Wun Wong, Stefan Ohm, Dan Parsons, Johann van der Walt, Vikas Joshi, Brian Reville, Connor Duffy, Michael Kreter, Gianluca Giavitto, D. Malyshev, Thomas Lohse, Mohanraj Senniappan, James Davies, Vincent Marandon, Hannes Thiersen, R. J. Tuffs, Hannah Dalgleish, Vardan Baghmanyan, P. T. O'Brien, Stefano Gabici, Thomas Bylund, Krzysztof Katarzynski, Michal Ostrowski, B. Bi, J.-P. Lenain, Catherine Boisson, Hugh Spackman, Michael Punch, Lukasz Stawarz, Sumari Hattingh, Monica Barnard, Jaqueline Catalano, Takaaki Tanaka, Rowan Batzofin, Mischa Breuhaus, Pauline Chambery, Stefan Funk, Alicja Wierzcholska, R. Konno, Ramin Marx, M. Panter, Anna Luashvili, Justine Devin, J. Bolmont, U. Katz, Francois Brun, Richard White, Jacques Muller, Andrew Taylor, P. Vincent, N. Zywucka, Andreas Quirrenbach, Laura Olivera-Nieto, A. Yusafzai, Dieter Horns, Guillem Marti'i-Devesa, Hassan Abdalla, Heiko Salzmann, Jacco Vink, Mathieu Bony, Oguzhan Anguener, Michael Zacharias, Celine Armand, Atreyee Sinha, Marek Jamrozy, Kirsty Feijen, Faical Ait-Benkhali, Lott Frans, Robert Brose, Santiago Pita, Hambeleleni Ndiyavala, L. Giunti, David Huber, German Hermann, Paul Morris, M. Hörbe, Helene Sol, Sabrina Casanova, Jim Hinton, S. Sailer, Dmitry Khangulyan, Charles Thorpe-Morgan, Sébastien Le Stum, Paolo Marchegiani, Michelle Tsirou, Constantin Steppa, Halim Ashkar, Fabian Leuschner, Ullrich Schwanke, C. Arcaro, Jean Damascene Mbarubucyeye, Wlodek Kluzniak, Gavin Rowell, Regis Terrier, B. Rudak, Carlo Romoli, Kathrin Egberts, Nukri Komin, Tom Armstrong, Frank M. Rieger, Matthieu Renaud, M. Fuessling, David Sanchez, Heike Prokoph, C. Levy, S. Steinmassl, Sami Caroff, Werner Hofmann, Marion Spir-Jacob, S. J. Fegan, Amid Nayerhoda, Sylvia Zhu, P. J. Meintjes, David Berge, Maria Haupt, Christopher van Eldik, Rafal Moderski, Dmitriy Kostunin, Brian van Soelen, Thomas Tavernier, Markus Boettcher, Sabrina Einecke, Iryna Lypova, Anita Reimer, Yvonne Becherini, Rachel Simoni, Angel Noel, Jonathan Mackey, C. Moore, Dorit Glawion, Tomasz Bulik, Malgorzata Curlo, Lente Dreyer, Louis Du Plessis, Naurois , Mathieu, Ona-Wilhelmi , Emma, and Bony , Mathieu

Subjects
Astrophysics::High Energy Astrophysical Phenomena, atmosphere [Cherenkov counter], VHE [gamma ray], IACT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov counter: atmosphere, Kepler, HESS, supernova, Astrophysics::Solar and Stellar Astrophysics, ddc:530, High Energy Stereoscopic System, cosmic radiation: acceleration, Supernova remnant, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Physics, energy: high, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Galaxy, Cassiopeia A, Supernova, gamma ray: VHE, high [energy], acceleration [cosmic radiation], galaxy
Abstract

37th International Cosmic Ray Conference, ICRC 2021, Berlin, online, Germany, 12 Jul 2021 - 23 Jul 2021; Proceedings of Science / International School for Advanced Studies (ICRC2021), 805 (2021). doi:10.22323/1.395.0805, Kepler���s supernova remnant (SNR) which is produced by the most recent naked-eye supernova in our Galaxy is one of the best studied SNRs, but its gamma-ray detection has eluded us so far. Observations with modern imaging atmospheric Cherenkov telescopes (IACT) have enlarged the knowledge about nearby SNRs with ages younger than 500 years by establishing Cassiopeia A and Tycho���s SNRs as very high energy (VHE) gamma-ray sources and setting a lower limit on the distance to Kepler���s SNR. This SNR is significantly more distant than the other two and expected to be one of the faintest gamma-ray sources within reach of the IACT arrays of this generation. We report strong evidence for a VHE signal from Kepler���s SNR based on deep observations of the High Energy Stereoscopic System (H.E.S.S.) with an exposure of 152 hours, including 122 hours accumulated in 2017-2020. We further discuss implications of this result for cosmic-ray acceleration in young SNRs., Published by SISSA, Trieste

Published
2021
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36. Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission

Author

Ludovic Montier, Baptiste Mot, Paolo de Bernardis, Bruno Maffei, Giampaolo Pisano, Fabio Columbro, Jon E. Gudmundsson, Sophie Henrot-Versillé, Luca Lamagna, Joshua Montgomery, Thomas Prouvé, Megan Russell, Giorgio Savini, Samantha Stever, Keith L. Thompson, Masahiro Tsujimoto, Carole Tucker, Benjamin Westbrook, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, Ranajoy Banerji, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Masashi Hazumi, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Gianluca Morgante, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Gianluca Polenta, Davide Poletti, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), LiteBIRD, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Lystrup, Makenzie, Montier, L, Mot, B, de Bernardis, P, Maffei, B, Pisano, G, Columbro, F, Gudmundsson, J, Henrot-Versillé, S, Lamagna, L, Montgomery, J, Prouvé, T, Russell, M, Savini, G, Stever, S, Thompson, K, Tsujimoto, M, Tucker, C, Westbrook, B, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Morgante, G, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)

Subjects
cosmological model, experimental methods, detector: satellite, Cosmic microwave background, cosmic background radiation: polarization, detector: noise, magnetic field, 02 engineering and technology, LiteBIRD, cosmic microwave background, polarization measurements, space telescopes, 7. Clean energy, 01 natural sciences, law.invention, law, detector: calibration, media_common, Physics, conductivity: thermal, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, Polarization (waves), inflation: model, experimental equipment, B-mode, cosmic radiation, cryogenics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, cosmic background radiation: detector, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, LiteBIRD, Polarization measurements, Space telescopes, Astrophysics::Cosmology and Extragalactic Astrophysics, bolometer: superconductivity, frequency: high, Radio spectrum, tensor scalar: ratio, 010309 optics, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: angular resolution, Astrophysics::Galaxy Astrophysics, Gravitational wave, synchrotron radiation, gravitational radiation: primordial, Astronomy, Physics::History of Physics, optics, detector: sensitivity, 13. Climate action, Sky, Satellite, temperature: stability, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy. European collaborators acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement Nos. 772253, 819478, and 849169). The European Space Agency (ESA) has led a Concurrent Design Facility study, focused on the MHFT and Sub-Kelvin coolers, and funded Technology Research Programmes for “Large radii Half-Wave Plate (HWP) development” (contract number: 4000123266/18/NL/AF) and for the ‘Development of Large Anti-Reflection Coated Lenses for Passive (Sub)Millimeter-Wave Science Instruments” (contract number: 4000128517/19/NL/AS).

Published
2020
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37. LiteBIRD: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization

Author

Masashi Hazumi, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, R. Banjeri, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Paolo de Bernardis, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Fabio Columbro, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Jon E. Gudmundsson, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Sophie Henrot-Versillé, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Luca Lamagna, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Bruno Maffei, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Joshua Montgomery, Ludovic Montier, Gianluca Morgante, Baptiste Mot, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Fabio Noviello, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Giampaolo Pisano, Gianluca Polenta, Davide Poletti, Thomas Prouvé, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Megan Russell, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Giorgio Savini, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Samantha Stever, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Keith L. Thompson, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Masahiro Tsujimoto, Carole Tucker, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Benjamin Westbrook, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Lystrup, Makenzie, Hazumi, M, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banjeri, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Noviello, F, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, and Zonca, A

Subjects
cosmological model, experimental methods, detector: satellite, Physics beyond the Standard Model, Cosmic microwave background, LiteBIRD, cosmic inflation, cosmic microwave background, B-mode polarization, primordial gravi- tational waves, quantum gravity, space telescope, cosmic background radiation: polarization, detector: noise, 02 engineering and technology, 7. Clean energy, 01 natural sciences, expansion: multipole, Cosmology, General Relativity and Quantum Cosmology, B-mode: primordial, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), general relativity, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], B-mode polarization, media_common, Physics, new physics, quantum mechanics, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, BICEP, inflation: model, High Energy Physics - Phenomenology, error: statistical, experimental equipment, cryogenics, power spectrum: angular dependence, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], readout, Astrophysics::Earth and Planetary Astrophysics, dust, control system, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, cosmic inflation, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, primordial gravi- tational waves, Cosmic background radiation, space telescope, Lagrangian point, FOS: Physical sciences, LiteBIRD, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, polarization: sensitivity, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ionization, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic background radiation: power spectrum, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Inflation (cosmology), synchrotron radiation, primordial gravitational waves, gravitational radiation: primordial, Astronomy, calibration, Physics::History of Physics, recombination, detector: sensitivity, angular resolution, Sky, quantum gravity, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Satellite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], experimental results
Abstract

Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA’s H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 µK-arcmin with a typical angular resolution of 0.5◦ at 100 GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy.

Published
2020
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38. eROSITA calibration and performance verification phase: High-mass X-ray binaries in the Magellanic Clouds

Author

Konrad Dennerl, Konstantin Postnov, Manami Sasaki, Michael Freyberg, Victor Doroshenko, X. Dai, N. I. Shakura, Andrzej Udalski, Stefania Carpano, Frank Haberl, and Chandreyee Maitra

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), Phase (waves), FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Light curve, Luminosity, Pulsar, Space and Planetary Science, Small Magellanic Cloud, Astrophysics - High Energy Astrophysical Phenomena, Large Magellanic Cloud
Abstract

During its performance verification phase, the soft X-ray instrument eROSITA aboard the Spektrum-Roentgen-Gamma(SRG) spacecraft observed large regions in the Magellanic Clouds, where almost 40 known high-mass X-ray binaries (HMXBs, including candidates) are located. We looked for new HMXBs in the eROSITA data, searched for pulsations in HMXB candidates and investigated the long-term behaviour of the full sample using archival X-ray and optical data. For sources sufficiently bright, a detailed spectral and temporal analysis of their eROSITA data was performed. A source detection analysis of the eROSITA images in different energy bands provided count rates and upper limits for the remaining sources. We report the discovery of a new Be/X-ray binary in the Large Magellanic Cloud. The transient SRGEt J052829.5-690345 was detected with a 0.2-8.0 keV luminosity of ~10^35 erg/s and exhibits a hard X-ray spectrum, typical for this class of HMXBs. The OGLE I-band light curve of the V~15.7 mag counterpart shows large variations by up to 0.75 mag, which occur quasi periodically with ~511 days. The eROSITA observations of the Small Magellanic Cloud covered 16 Be/X-ray binary pulsars, five of them were bright enough to accurately determine their current pulse period. The pulse periods for SXP 726 and SXP 1323 measured from eROSITA data are ~800 s and ~1006 s, respectively, far away from their discovery periods. Including archival XMM-Newton observations we update the spin-period history of the two long-period pulsars which show nearly linear trends in their period evolution since more than 15 years. The corresponding average spin-down rate for SXP 726 is 4.3 s/yr while SXP 1323 shows spin-up with a rate of -23.2 s/yr. We discuss the spin evolution of the two pulsars in the framework of quasi-spherical accretion., 21 pages, 28 figures, accepted for publication in Astronomy & Astrophysics, First science highlights from SRG/eROSITA

Published
2022
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39. eROSITA study of the globular cluster 47 Tucanae

Author

Sara Saeedi, Teng Liu, Jonathan Knies, Manami Sasaki, Werner Becker, Esra Bulbul, Konrad Dennerl, Michael Freyberg, Roman Laktionov, and Andrea Merloni

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

Aims. We present the results of the analysis of five observations of the globular clutser 47 Tucanae (47 Tuc) with the extended Roentgen Survey with an Imaging Telescope Array (eROSITA) on board the Spektrum-Roentgen-Gamma (Spektr-RG, SRG). We study the X-ray population in the field of one of the most massive globular clusters in our Milky Way. We focused on the classification of point-like sources in the field of 47 Tuc. The unresolved dense core of 47 Tuc (1.7 radius) and also sources that show extended emission are excluded from this study. Methods. We applied different methods of X-ray spectral and timing analysis together with multi-wavelength studies to classify the X-rays sources in the field of 47 Tuc. Results. We detected 888 point-like sources in the energy range of 0.2–5.0 keV. We identified 126 background active galactic nuclei and 25 foreground stars. One of the foreground stars is classified as a variable M dwarf. We also classified 14 X-ray sources as members of 47 Tuc, including one symbiotic star, two quiescent low-mass X-ray binaries, and four cataclysmic variables. There are also five X-ray sources that can either be a cataclysmic variable or a contact binary, and also one X-ray source can be an active binary (type RS CVn). We identified one X-ray binary that belongs to the Small Magellanic Cloud. Moreover, we calculated the X-ray luminosity function of 47 Tuc. No significant population that seems to belong to the globular cluster is observed in the energy range of 0.5–2.0 keV using eROSITA observations.

Published
2022
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40. An intermediate-velocity H <scp>i</scp> cloud falling to the galactic disk; Possible evidence for low-metallicity H <scp>i</scp> gas originating outside the galactic disk

Author

Yasuo Fukui, Hiroaki Yamamoto, Masako Koga, Robin L. Shelton, Ryuji Okamoto, Manami Sasaki, Takahiro Hayakawa, Kengo Tachihara, and Shohei Maruyama

Subjects
Galactic halo, Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Disc, Falling (sensation), Astrophysics - Astrophysics of Galaxies
Abstract

We found that an intermediate velocity cloud (IVC) IVC 86-36 in HI 21 cm emission shows a head-tail distribution toward the Galactic plane with marked parallel filamentary streamers, which is extended over 40 degrees in the sky. The distance of IVC 86-36 is constrained to be less than ~3 kpc from absorption of a background star as determined from opticalspectroscopy. There is a bridge feature in velocity between the IVC and the local ISM with velocity separation of ~50 km s-1, which may indicate dynamical interaction of the IVC with the disk. If the interaction is correct, the distance estimate d of the IVC ranges from 200 pc to 3 kpc, and the mass of the IVC head is estimated to be 7X103(d/1kpc)2Msol. The IVC shares similar properties to the Smith cloud located at 12 kpc, including the head-tail distribution, streamers, and bridge feature, while the mass of the IVC is less than ~0.1 of the Smith cloud. A comparison between the Hi and the Planck/IRAS dust emission indicates that the dust emission of IVC 86-36 is not detectable in spite of its HI column density of 2X10^20 cm-2, indicating low metalicity of IVC 86-36 by a factor of ~< 0.2 as compared with the solar neighbor. We conclude that IVC 86-38 is an infalling cloud which likely originated in the low-metallicity environment of the Galactic halo or the Magellanic system., Accepted for publication in PASJ

Published
2018
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41. An X-ray expansion and proper motion study of the Magellanic Cloud Supernova Remnant J0509–6731 with the Chandra X-ray observatory

Author

Hidetoshi Sano, Manami Sasaki, Frank Haberl, Laurence A. F. Park, Patrick J. Kavanagh, Thomas G. Pannuti, K. Fujii, Miroslav Filipovic, Y. Yamane, Quentin Roper, Satoshi Yoshiike, Glenn E. Allen, Yasuo Fukui, and Ivo R. Seitenzahl

Subjects
Physics, Proper motion, Space and Planetary Science, Observatory, 0103 physical sciences, X-ray, Astronomy and Astrophysics, Astrophysics, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, 01 natural sciences
Abstract

MS acknowledges support by the Deutsche Forschungsgemeinschaft through the research grant SA 2131/4-1 and the Heisenberg professor grant SA 2131/5-1.

Published
2018
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42. XMM–Newton study of the supersoft symbiotic system Draco C1

Author

Manami Sasaki, Sara Saeedi, and Lorenzo Ducci

Subjects
Physics, biology, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, biology.organism_classification, 010303 astronomy & astrophysics, 01 natural sciences, Draco (genus)
Published
2017
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43. X-ray observations of Galactic H.E.S.S. sources: An update

Author

Manami Sasaki, M. Capasso, P. Bordas, D. Gottschall, Peter Eger, and G. Pühlhofer

Subjects
Physics, Supernova, 010308 nuclear & particles physics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Small class, 0103 physical sciences, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences
Abstract

X-ray diagnostics of TeV (teraelectronvolt) sources continues to be an important tool to identify the nature of newly detected sources as well as to pinpoint the physics processes that are at work in these highly energetic objects. This paper gives a review of recent studies that have been performed on TeV sources with H.E.S.S. and XMM-Newton and also other X-ray facilities. Here, we mainly focus on the galactic object types γ-ray binaries and supernova remnants (SNRs). γ-ray binaries form a small class of objects whose identification and study is challenging because of the sometimes very long orbital periods that need to be established from data. Particular emphasis is given to SNR studies, including recently identified SNRs such as HESS J1731−347 and HESS J1534−571, as well as a revisit of RX J1713.7−3946.

Published
2017
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44. Detection of large-scale X-ray bubbles in the Milky Way halo

Author

Gabriele Ponti, Andrei M. Bykov, Kirpal Nandra, Sergey V. Sazonov, Frank Haberl, Chandreyee Maitra, M. N. Pavlinsky, E. Churazov, V. Nazarov, Manami Sasaki, Michael Freyberg, Rashid Sunyaev, N. Eismont, Nikolai Chugai, Andrea Merloni, Jörn Wilms, R. A. Burenin, Hermann Brunner, Jeremy S. Sanders, I. Khabibullin, Andrew W. Strong, A. M. Cherepashchuk, Marat Gilfanov, Victor Doroshenko, Werner Becker, P. S. Medvedev, Roman Krivonos, and Peter Predehl

Subjects
media_common.quotation_subject, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Galactic halo, law, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, 010308 nuclear & particles physics, Star formation, Galactic plane, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Sky, Astrophysics of Galaxies (astro-ph.GA), Halo, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The halo of the Milky Way provides a laboratory to study the properties of the shocked hot gas that is predicted by models of galaxy formation. There is observational evidence of energy injection into the halo from past activity in the nucleus of the Milky Way; however, the origin of this energy (star formation or supermassive-black-hole activity) is uncertain, and the causal connection between nuclear structures and large-scale features has not been established unequivocally. Here we report soft-X-ray-emitting bubbles that extend approximately 14 kiloparsecs above and below the Galactic centre and include a structure in the southern sky analogous to the North Polar Spur. The sharp boundaries of these bubbles trace collisionless and non-radiative shocks, and corroborate the idea that the bubbles are not a remnant of a local supernova but part of a vast Galaxy-scale structure closely related to features seen in gamma-rays. Large energy injections from the Galactic centre are the most likely cause of both the {\gamma}-ray and X-ray bubbles. The latter have an estimated energy of around 10$^{56}$ erg, which is sufficient to perturb the structure, energy content and chemical enrichment of the circumgalactic medium of the Milky Way., Comment: Author's version. 17 pages, 5 figures, Published in Nature 2020, Vol 588

Published
2020
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45. Supernova remnants in nearby galaxies

Author

Manami Sasaki

Subjects
Physics, Thesaurus (information retrieval), Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Local Group, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Naturwissenschaftliche Fakultät, Galaxy, Supernova, Space and Planetary Science, ddc:520, Astrophysics::Galaxy Astrophysics
Abstract

Supernova remnants (SNRs) are the aftermath of stellar explosions, which inject large amounts of energy into the interstellar medium (ISM), carving out new structures and transferring kinetic energy to the ISM. They also act as recycling centers, which return elements processed in stars to the ISM, and cosmic particle accelerators. The evolution of SNRs can be best studied in soft X‐ray line and continuum emission, since they mainly consist of very hot plasma (106–107 K). While it is difficult to observe these soft X‐ray sources in our own Galaxy due to absorption by matter in the Galactic plane, the Magellanic Clouds as well as the nearby spiral galaxies M 31 and M 33 are ideal targets to study both particular SNRs in detail and the SNR population in a galaxy as a whole. Various studies of SNRs in the Local Group galaxies have been carried out with XMM‐Newton or Chandra since the launch of the mission, and in the coming years the new X‐ray all‐sky survey performed with eROSITA will provide us with more complete data of SNRs in the nearby Universe to low flux limits.

Published
2020
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46. H.E.S.S. and Fermi-LAT observations of PSR B1259-63/LS 2883 during its 2014 and 2017 periastron passages

Author

Lars Mohrmann, J. Dyks, M. Zacharias, C. Armand, D. Tiziani, V. Poireau, F. Ait Benkhali, M. Panter, Manami Sasaki, V. Barbosa Martins, I. Jung-Richardt, G. Heinzelmann, J. Bolmont, G. Emery, S. Schwemmer, Andrea Santangelo, Michael Punch, M. Spir-Jacob, Stefano Gabici, K. Shiningayamwe, J.-P. Ernenwein, Simon Sailer, T. Chand, Jhilik Majumdar, Felix Aharonian, Michael Kreter, M. Böttcher, R. C. G. Chaves, E. O. Angüner, M. Büchele, C. Perennes, André Schulz, Ruizhi Yang, Stefan Ohm, Dieter Horns, C. Levy, Michelle Tsirou, J. Devin, C. Stegmann, Nu. Komin, E. Leser, S. J. Fegan, S. Pita, J.-P. Lenain, A. Carosi, N. Shafi, E. Moulin, G. Henri, P. T. O'Brien, F. Gaté, T. Vuillaume, J. Hahn, Reinhard Schlickeiser, M. Füßling, Dmitry Khangulyan, H. Abdalla, G. Vasileiadis, Werner Hofmann, Gerd Pühlhofer, M. Arakawa, German Hermann, S. Chandra, C. Trichard, M. Holler, A. Reimer, Yves Gallant, Regis Terrier, F. Schüssler, Dmitriy Kostunin, H.M. Schutte, Jonathan Mackey, J. Veh, Quentin Piel, D. A. Sanchez, G. Lamanna, E. de Ona Wilhelmi, R. Rauth, Naomi Tsuji, L. Dirson, Carlo Romoli, Marianne Lemoine-Goumard, M. Barnard, C. Moore, J. Muller, L. Oakes, Marie-Hélène Grondin, R. Zanin, H. Yoneda, Tomasz Bulik, Alison Mitchell, T. Bylund, Zorawar Wadiasingh, S. Klepser, Axel Donath, A. W. Chen, Michal Ostrowski, Andrzej A. Zdziarski, T. Lohse, J. Zorn, Catherine Boisson, Ullrich Schwanke, H. Iwasaki, Andrew M. Taylor, M. Curyło, Armelle Jardin-Blicq, I. D. Davids, Stefan Funk, D. J. van der Walt, Matteo Cerruti, Daniel Huber, Stefan Wagner, Yasunobu Uchiyama, S. Saito, C. van Rensburg, S. Raab, Kirsty Feijen, Shinya Nakashima, Atreyee Sinha, A. Djannati-Ataï, N. Żywucka, R. Steenkamp, H. Sol, P. Brun, Michael Backes, A. Fiasson, Richard J. Tuffs, G. Martí-Devesa, Vincent Marandon, Tim Holch, T. Takahashi, Gianluca Giavitto, R. Blackwell, E. Ruiz-Velasco, P.-O. Petrucci, K. Bernlöhr, Yvonne Becherini, Marek Jamrozy, Gerard Fontaine, B. Khélifi, D. A. Prokhorov, S. Eschbach, Q. Remy, B. Peyaud, B. van Soelen, Andreas Zech, Christo Venter, Włodek Kluźniak, D. Glawion, R. Moderski, J. Hinton, Christoph Deil, Mohanraj Senniappan, Karl Kosack, M.A. Kastendieck, S. Bonnefoy, Mischa Breuhaus, Pol Bordas, Frank M. Rieger, D. Gottschall, C. van Eldik, Mahmoud Mohamed, Felix Jankowsky, Clemens Hoischen, Igor Oya, S. Colafrancesco, J. F. Glicenstein, V. Sahakian, I. Lypova, Łukasz Stawarz, C. Mariaud, Uli Katz, A. Specovius, P. J. Meintjes, Francois Brun, P. Vincent, M. Haupt, Heinrich J. Völk, Jacek Niemiec, A. Lemière, Olaf Reimer, B. Rudak, H. Ndiyavala, Thomas Murach, D. Jankowsky, M. Tluczykont, Andreas Quirrenbach, Kathrin Egberts, S. Caroff, G. Maurin, Ramin Marx, Hirokazu Odaka, A.S. Seyffert, Monica Seglar-Arroyo, F. Niederwanger, Alicja Wierzcholska, Gavin Rowell, Jacco Vink, David Berge, M. Bryan, Sabrina Casanova, R. D. Parsons, A. Priyana Noel, Matthieu Renaud, M. Katsuragawa, L. Giunti, Heike Prokoph, P. deWilt, K. Katarzyński, J. King, T. Tavernier, A. Dmytriiev, C. Arcaro, R. Adam, C. Steppa, Victor Doroshenko, H. Ashkar, M. de Naurois, Alexandre Marcowith, L. Rinchiuso, Rachel Simoni, Arnaud Mares, Johan Bregeon, R. J. White, D. Malyshev, 26598973 - Abdalla, Hassan, 30588766 - Arcaro, Cornelia, 28644743 - Backes, Michael, 20574266 - Barnard, Monica, 24420530 - Böttcher, Markus, 30366755 - Chand, Tej B., 31125417 - Chandra, Sunil, 33379009 - Kreter, Michael, 26403366 - Ndiyavala, Hambeleleni, 22799133 - Schutte, Hester M., 20126999 - Seyffert, Albertus Stefanus, 10060499 - Van der Walt, Diederick Johannes, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 29092086 - Zacharias, Michael, 34208968 - Zywucka-Hejzner, Natalia, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, H.E.S.S., Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), Gravitation and Astroparticle Physics Amsterdam, University of Namibia, Federal Ministry of Education and Research (Germany), Max Planck Society, German Research Foundation, Helmholtz Association, Alexander von Humboldt Foundation, Ministre de l'Enseignement Supérieur, de la Recherche et de l'Innovation (France), Centre National de la Recherche Scientifique (France), Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), Science and Technology Facilities Council (UK), Knut and Alice Wallenberg Foundation, National Science Centre (Poland), Department of Science and Technology (South Africa), National Research Foundation (South Africa), National Commission on Research Science and Technology (Namibia), Federal Ministry of Education, Science and Research (Austria), Japan Society for the Promotion of Science, University of Amsterdam, H.E.S.S. Collaboration, Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)

Subjects
Shock wavesγ-rays: general, VHE [gamma ray], Flux, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, star, HESS, flux [gamma ray], Astrophysics::Solar and Stellar Astrophysics, gamma ray: flux, neutron star, 010303 astronomy & astrophysics, orbit, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, photon, shock waves, modulation, gamma ray: emission, binary [gamma ray], binaries: general, astroparticle physics, slope, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, asymmetry, signature, Astrophysics::High Energy Astrophysical Phenomena, Population, general [Pulsars], FOS: Physical sciences, Orbital eccentricity, Astrophysics::Cosmology and Extragalactic Astrophysics, GLAST, energy dependence, Shock waves, Pulsar, emission [gamma ray], pulsars: general, 0103 physical sciences, general [γ-Rays], education, Astrophysics::Galaxy Astrophysics, non-thermal [Radiation mechanisms], γ-rays: general, general [Binaries], 010308 nuclear & particles physics, gamma ray: binary, Astronomy and Astrophysics, radiation mechanisms: non-thermal, crossing, Light curve, Neutron star, gamma ray: VHE, Space and Planetary Science, HESS - Abteilung Hinton, ddc:520, Astroparticle physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

[Context] PSR B1259–63/LS 2883 is a gamma-ray binary system consisting of a pulsar in an eccentric orbit around a bright Oe stellar-type companion star that features a dense circumstellar disc. The bright broad-band emission observed at phases close to periastron offers a unique opportunity to study particle acceleration and radiation processes in binary systems. Observations at gamma-ray energies constrain these processes through variability and spectral characterisation studies., [Aims] The high- and very-high-energy (HE, VHE) gamma-ray emission from PSR B1259–63/LS 2883 around the times of its periastron passage are characterised, in particular, at the time of the HE gamma-ray flares reported to have occurred in 2011, 2014, and 2017. Short-term and average emission characteristics of PSR B1259–63/LS 2883 are determined. Super-orbital variability is searched for in order to investigate possible cycle-to-cycle VHE flux changes due to different properties of the companion star’s circumstellar disc and/or the conditions under which the HE gamma-ray flares develop., [Methods] Spectra and light curves were derived from observations conducted with the H.E.S.S-II array in 2014 and 2017. Phase-folded light curves are compared with the results obtained in 2004, 2007, and 2011. Fermi-LAT observations from 2010/11, 2014, and 2017 are analysed., [Results] A local double-peak profile with asymmetric peaks in the VHE light curve is measured, with a flux minimum at the time of periastron tp and two peaks coinciding with the times at which the neutron star crosses the companion’s circumstellar disc (~tp ± 16 d). A high VHE gamma-ray flux is also observed at the times of the HE gamma-ray flares (~tp + 30 d) and at phases before the first disc crossing (~tp − 35 d). The spectral energy range now extends to below 200 GeV and up to ~45 TeV., [Conclusions] PSR B1259–63/LS 2883 displays periodic flux variability at VHE gamma-rays without clear signatures of super-orbital modulation in the time span covered by the monitoring of the source with the H.E.S.S. telescopes. This flux variability is most probably caused by the changing environmental conditions, particularly at times close to periastron passage at which the neutron star is thought to cross the circumstellar disc of the companion star twice. In contrast, the photon index remains unchanged within uncertainties for about 200 d around periastron. At HE gamma-rays, PSR B1259–63/LS 2883 has now been detected also before and after periastron, close to the disc crossing times. Repetitive flares with distinct variability patterns are detected in this energy range. Such outbursts are not observed at VHEs, although a relatively high emission level is measured. The spectra obtained in both energy regimes displays a similar slope, although a common physical origin either in terms of a related particle population, emission mechanism, or emitter location is ruled out., The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat a l’Énergie atomique et aux Énergies alternatives (CEA), the U.K. Science and Technology Facilities Council (STFC), the Knut and Alice Wallenberg Foundation, the National Science Centre, Poland grant no. 2016/22/M/ST9/00382, the South African Department of Science and Technology and National Research Foundation, the University of Namibia, the National Commission on Research, Science & Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science and by the University of Amsterdam. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen and in Namibia in the construction and operation of the equipment. This work benefitted from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation.

Published
2020
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47. Resolving the Crab pulsar wind nebula at teraelectronvolt energies

Author

Natalia Żywucka, M. de Naurois, T. Chand, Frank M. Rieger, J. Bolmont, S. Colafrancesco, Ruizhi Yang, W. Kluźniak, S. Eschbach, Jim Hinton, R. Simoni, Dmitry Khangulyan, Christopher J. Moore, G. Fontaine, M. Büchele, D. A. Sanchez, T. Tavernier, L. Mohrmann, Denys Malyshev, J. Veh, S. Klepser, B. Khélifi, H. M. Schutte, C. Perennes, D. Glawion, Christoph Deil, Mohanraj Senniappan, A.A. Zdziarski, A. Djannati-Ataï, Y.A. Gallant, Gavin Rowell, Stefan Funk, T. Takahashi, Gianluca Giavitto, Axel Donath, A. W. Chen, M. Bryan, J. Dyks, D. Zaborov, I. Oya, G. Heinzelmann, K. Shiningayamwe, T. Lohse, Yvonne Becherini, M. Renaud, H. Iwasaki, M. Holler, J.-P. Ernenwein, P. Vincent, R. D. Parsons, G. Emery, H. Odaka, Christo Venter, D. Huber, M. Arakawa, D. Berge, M. Capasso, Matteo Cerruti, Nachiketa Chakraborty, F. Niederwanger, A. Marcowith, A. Zech, E. Leser, Jacco Vink, R. Rauth, Sabrina Casanova, C. Arcaro, I. Jung-Richardt, T. Vuillaume, G. Hermann, D. Gottschall, Werner Hofmann, Regis Terrier, J. Becker Tjus, A. Schulz, Carlo Romoli, M. Panter, M. Seglar-Arroyo, H. Ndiyavala, B. van Soelen, Felix Aharonian, M. Haupt, Lukasz Stawarz, Michael Punch, V. Doroshenko, M. Spir-Jacob, R. Tuffs, R. C. G. Chaves, E. O. Angüner, A. Priyana Noel, L. O'c. Drury, S. Saito, J.F. Glicenstein, D. J. van der Walt, S. Raab, Andreas Quirrenbach, C. Steppa, J.-P. Lenain, N. Shafi, K. Egberts, Robert Wagner, K. Kosack, J. Hahn, Reinhard Schlickeiser, M. Tsirou, G. Vasileiadis, M. Kraus, S. Chandra, S. Nakashima, G. Martí-Devesa, M. Katsuragawa, Ruben Lopez-Coto, M.-H. Grondin, M. Böttcher, R. Blackwell, E. Ruiz-Velasco, L. Dirson, Stefan Ohm, Léa Jouvin, S. Pita, F. Schüssler, P. deWilt, J. King, F. Voisin, Julien Lefaucheur, A. Dmytriiev, R. Moderski, S. Gabici, A. Fiasson, J. Lau, L. Oakes, I.D. Davids, Alison Mitchell, L. Rinchiuso, P.J. Meintjes, Heike Prokoph, Zorawar Wadiasingh, R. J. White, S. Fegan, Dieter Horns, V. Poireau, Monica Barnard, P.-O. Petrucci, H. Abdalla, D. Jankowsky, Q. Piel, C. Stegmann, Nu. Komin, Marek Jamrozy, Catherine Boisson, Helene Sol, Pierre Brun, A.S. Seyffert, A. Carosi, M. Füßling, M.A. Kastendieck, S. Bonnefoy, N. Tsuji, F. Gaté, J. Devin, G. Henri, D. A. Prokhorov, D. Tiziani, C. Hoischen, Ullrich Schwanke, A. Specovius, R. Steenkamp, A. Reimer, J. Bregeon, Francois Brun, B. Condon, Michael Backes, H. Yoneda, Tim Holch, M. Tluczykont, E. Moulin, Tomasz Bulik, T. Bylund, A. Jacholkowska, S. Caroff, Celine Armand, F. Jankowsky, Stefan Wagner, Yasunobu Uchiyama, C. van Rensburg, M. Zacharias, C. Trichard, F. Ait Benkhali, Manami Sasaki, S. Schwemmer, Andrea Santangelo, A. Ziegler, G. Maurin, A. Wierzcholska, C. Mariaud, Jacek Niemiec, Olaf Reimer, Thomas Murach, A. Lemière, M. Lemoine-Goumard, I. Shilon, Heinrich J. Völk, R. Marx, P. Bordas, I. Lypova, G. Lamanna, J. Zorn, U. Katz, J.-P. Tavernet, B. Rudak, V. Marandon, K. Katarzyński, A.M. Taylor, V. Sahakian, M. Mohamed, M. Ostrowski, Konrad Bernlöhr, B. Peyaud, G. Pühlhofer, R. Zanin, P. T. O'Brien, Atreyee Sinha, C. van Eldik, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, H.E.S.S., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), European Commission, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Armagh Observatory, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), Gravitation and Astroparticle Physics Amsterdam, 26598973 - Abdalla, Hassan, 30588766 - Arcaro, Cornelia, 28644743 - Backes, Michael, 20574266 - Barnard, Monica, 24420530 - Böttcher, Markus, 30366755 - Chand, Tej B., 31125417 - Chandra, Sunil, 26403366 - Ndiyavala, Hambeleleni, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 22799133 - Schutte, Hester M., 20126999 - Seyffert, Albertus Stefanus, 29092086 - Zacharias, Michael, and Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Electromagnetic spectrum, electron: relativistic, magnetic field, Astrophysics, positron: energy, 01 natural sciences, 7. Clean energy, Pulsar wind nebula, particle: acceleration, Raigs gamma, Astrophysics::Solar and Stellar Astrophysics, HESS - Abteilung Hofmann, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], Nebula, radio wave, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 4. Education, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], photon, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, High-energy astrophysics, Particle astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Camps magnètics, accelerator, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, gap, X-ray, energy loss: rotation, Pulsar, 0103 physical sciences, synchrotron, Astrophysics::Galaxy Astrophysics, gamma ray: energy, 0105 earth and related environmental sciences, Crab Pulsar, Gamma rays, Astronomy and Astrophysics, Crab Nebula, electromagnetic, gamma ray: VHE, [SDU]Sciences of the Universe [physics], Magnetic fields, ddc:520, Physics::Accelerator Physics
Abstract

arXiv:1909.09494v2, H.E.S.S. Collaboration: et al., The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat à l’énergie atomique et aux énergies alternatives (CEA), the UK Science and Technology Facilities Council (STFC), the Knut and Alice Wallenberg Foundation, the National Science Centre, Poland (grant number 2016/22/M/ST9/00382), the South African Department of Science and Technology and the National Research Foundation, the University of Namibia, the National Commission on Research, Science and Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science and the University of Amsterdam. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen and Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation. R.C.G.C. was funded by EU FP7 Marie Curie (grant agreement number PIEF-GA-2012-332350).

Published
2020
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48. The supernova remnant population of the Small Magellanic Cloud

Author

Jean Ballet, Patrick J. Kavanagh, Milorad Stupar, Frank Haberl, Chandreyee Maitra, P. Maggi, Branislav Vukotić, Miroslav Filipovic, Manami Sasaki, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Western Sydney University, Astronomical Observatory Belgrade (AOB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), School of Cosmic Physics [Dublin], Dublin Institute for Advanced Studies (DIAS), Dr. Karl-Remeis-Sternwarte, Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU)-Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), School of Science and Health [Western Sydney University], Western Sydney University (UWS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM: abundances, supernovae: general, 0103 physical sciences, Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, education, Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, X-rays: ISM, Interstellar medium, Supernova, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Small Magellanic Cloud, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Aims: We present a comprehensive study of the supernova remnant (SNR) population of the Small Magellanic Cloud (SMC). We measure multiwavelength properties of the SMC SNRs and compare them to those of the Large Magellanic Cloud (LMC) population. Methods: This study combines the large dataset of XMM-Newton observations of the SMC, archival and recent radio continuum observations, an optical line emission survey, and new optical spectroscopic observations. We can thus build a complete and clean sample of 19 confirmed and 4 candidate SNRs. The homogeneous X-ray spectral analysis allows to search for SN ejecta and Fe K line emission, and to measure interstellar medium (ISM) abundances. We estimate the ratio of core-collapse to type Ia supernova rates of the SMC based on the X-ray properties and the local stellar environment of each SNR. Results : After the removal of unconfirmed or misclassified objects, and the addition of two newly confirmed SNRs based on multi-wavelength features, we present a final list of 21 confirmed SNRs and 2 candidates. While no Fe K line is detected even for the brightest and youngest SNR, we find X-ray evidence of SN ejecta in 11 SNRs. We estimate a ratio of 4.7$_{-1.9} ^{+0.6}$ core-collapse supernova to every type Ia SN, three times higher than in the LMC. The difference can be ascribed to the absence of the enhanced star formation episode in the SMC, which occurred in the LMC 0.5-1.5 Gyr ago. The hot-gas abundances of O, Ne, Mg, and Fe are 0.1-0.2 times solar. Their ratios with respect to SMC stellar abundances reflect the effects of dust depletion and partial dust destruction in SNR shocks. We find evidence that the ambient medium probed by SMC SNRs is less disturbed and less dense on average than in the LMC, consistent with the different morphologies of the two galaxies., Comment: Submitted to Astronomy & Astrophysics. 29 pages, 8 figures, 5 tables; 3 additional tables and 9 figures in Appendices

Published
2019
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49. Deep XMM-Newton observations of the northern disk of M31 II: Tracing the hot interstellar medium

Author

Manami Sasaki, Despina Hatzidimitriou, Miguel A. de Avillez, Patrick J. Kavanagh, Kirill Sokolovsky, Martin Henze, Frank Haberl, Miroslav Filipovic, Sara Saeedi, Benjamin F. Williams, Paul P. Plucinsky, Dieter Breitschwerdt, Timothy J Galvin, Federal Ministry of Science, Research and Economy (Germany), German Centre for Air and Space Travel, German Research Foundation, National Science Foundation (US), National Aeronautics and Space Administration (US), and California Institute of Technology

Subjects
HII regions, ISM: structure, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, ISM [Galaxies], 0103 physical sciences, ISM [X-rays], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Computer Science::Information Retrieval, Astronomy and Astrophysics, Grand design spiral galaxy, Astrophysics - Astrophysics of Galaxies, X-rays: ISM, Galaxy, bubbles [ISM], Andromeda, Interstellar medium, Galaxies: ISM, Supernova, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, structure [ISM], ISM: bubbles, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Aims: We use new deep XMM-Newton observations of the northern disk of M 31 to trace the hot interstellar medium (ISM) in unprecedented detail and to characterise the physical properties of the X-ray emitting plasmas. Methods: We used all XMM-Newton data up to and including our new observations to produce the most detailed image yet of the hot ISM plasma in a grand design spiral galaxy such as our own. We compared the X-ray morphology to multi-wavelength studies in the literature to set it in the context of the multi-phase ISM. We performed spectral analyses on the extended emission using our new observations as they offer sufficient depth and count statistics to constrain the plasma properties. Data from the Panchromatic Hubble Andromeda Treasury were used to estimate the energy injected by massive stars and their supernovae. We compared these results to the hot gas properties. Results: The brightest emission regions were found to be correlated with populations of massive stars, notably in the 10 kpc star-forming ring. The plasma temperatures in the ring regions are ~0.2 keV up to ~0.6 keV. We suggest this emission is hot ISM heated in massive stellar clusters and superbubbles. We derived X-ray luminosities, densities, and pressures for the gas in each region. We also found large extended emission filling low density gaps in the dust morphology of the northern disk, notably between the 5 kpc and 10 kpc star-forming rings. We propose that the hot gas was heated and expelled into the gaps by the populations of massive stars in the rings. Conclusions. It is clear that the massive stellar populations are responsible for heating the ISM to X-ray emitting temperatures, filling their surroundings, and possibly driving the hot gas into the low density regions. Overall, the morphology and spectra of the hot gas in the northern disk of M 31 is similar to other galaxy disks., 23 pages, 14 figures, accepted for publication in Astronomy & Astrophysics

Published
2019

50. The ASKAP EMU early science project: radio continuum survey of the Small Magellanic Cloud

Author

Manami Sasaki, T. D. Joseph, H. Leverenz, J. Th. van Loon, Ray P. Norris, P. Manojlovic, Andrew O'Brien, Hidetoshi Sano, F. Cavallaro, T. J. Galvin, M. Stupar, Michał J. Michałowski, J. Marvil, Grazia Maria Gloria Umana, Frank Haberl, Kevin Grieve, Anna D. Kapińska, Chandreyee Maitra, Jordan D. Collier, R. Z. E. Alsaberi, Roland Kothes, N. Maxted, Nicholas F. H Tothill, P. Maggi, Miranda Yew, E. L. Alexander, Roberto Soria, You-Hua Chu, Craig S. Anderson, Yasuo Fukui, Gavin Rowell, Simone Riggi, Denis Leahy, Ivan S. Bojičić, Miroslav Filipovic, Graeme F Wong, Eleni Vardoulaki, Luke A. Barnes, Di Li, Corrado Trigilio, Luke M Bozzetto, Dejan Urošević, Patrick J. Kavanagh, Baerbel Koribalski, Kisetsu Tsuge, Filomena Bufano, H. Dénes, Joana M. Oliveira, V. Velovic, Lawrence Rudnick, A. Ingallinera, Nick Seymour, Evan J Crawford, J. D. Bunton, Heinz Andernach, Clara M. Pennock, Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Radio galaxy, Point source, astro-ph.GA, Population, FOS: Physical sciences, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Magellanic Clouds, Supernova remnant, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, catalogues, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Planetary nebula, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Small Magellanic Cloud, Molonglo Observatory Synthesis Telescope, QB799
Abstract

We present two new radio continuum images from the Australian Square Kilometre Array Pathfinder (ASKAP) survey in the direction of the Small Magellanic Cloud (SMC). These images are part of the Evolutionary Map of the Universe (EMU) Early Science Project (ESP) survey of the Small and Large Magellanic Clouds. The two new source lists produced from these images contain radio continuum sources observed at 960 MHz (4489 sources) and 1320 MHz (5954 sources) with a bandwidth of 192 MHz and beam sizes of 30.0"x30.0" and 16.3"x15.1", respectively. The median Root Mean Squared (RMS) noise values are 186$\mu$Jy beam$^{-1}$ (960 MHz) and 165$\mu$Jy beam$^{-1}$ (1320 MHz). To create point source catalogues, we use these two source lists, together with the previously published Molonglo Observatory Synthesis Telescope (MOST) and the Australia Telescope Compact Array (ATCA) point source catalogues to estimate spectral indices for the whole population of radio point sources found in the survey region. Combining our ASKAP catalogues with these radio continuum surveys, we found 7736 point-like sources in common over an area of 30 deg$^2$. In addition, we report the detection of two new, low surface brightness supernova remnant candidates in the SMC. The high sensitivity of the new ASKAP ESP survey also enabled us to detect the bright end of the SMC planetary nebula sample, with 22 out of 102 optically known planetary nebulae showing point-like radio continuum emission. Lastly, we present several morphologically interesting background radio galaxies., Comment: 18 pages, 23 figues, 9 tables, Accepted for publication in the Monthly Notices of the Royal Astronomical Society

Published
2019
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