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176 results on '"SUPERNOVA REMNANTS [ISM]"'

1. Properties of shocked dust grains in supernova remnants

Author

F D Priestley, H Chawner, M J Barlow, I De Looze, H L Gomez, and M Matsuura

Subjects
HERSCHEL, supernova remnants [ISM], FOS: Physical sciences, Astronomy and Astrophysics, ) dust, extinction [(ISM], evolution [ISM], Astrophysics - Astrophysics of Galaxies, CASSIOPEIA, Physics and Astronomy, GAS, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MHZ MASER EMISSION, DESTRUCTION
Abstract

Shockwaves driven by supernovae both destroy dust and reprocess the surviving grains, greatly affecting the resulting dust properties of the interstellar medium (ISM). While these processes have been extensively studied theoretically, observational constraints are limited. We use physically-motivated models of dust emission to fit the infrared (IR) spectral energy distributions of seven Galactic supernova remnants, allowing us to determine the distribution of dust mass between diffuse and dense gas phases, and between large and small grain sizes. We find that the dense ($\sim 10^3 \,{\rm cm}^{-3}$), relatively cool ($\sim 10^3 \, {\rm K}$) gas phase contains $>90\%$ of the dust mass, making the warm dust located in the X-ray emitting plasma ($\sim 1 \,{\rm cm}^{-3}$/$10^6 \, {\rm K}$) a negligible fraction of the total, despite dominating the mid-IR emission. The ratio of small ($\lesssim 10 \, {\rm nm}$) to large ($\gtrsim 0.1 \, {\rm μm}$) grains in the cold component is consistent with that in the ISM, and possibly even higher, whereas the hot phase is almost entirely devoid of small grains. This suggests that grain shattering, which processes large grains into smaller ones, is ineffective in the low-density gas, contrary to model predictions. Single-phase models of dust destruction in the ISM, which do not account for the existence of the cold swept-up material containing most of the dust mass, are likely to greatly overestimate the rate of dust destruction by supernovae., 13 pages, 12 figures. MNRAS accepted

Published
2022

2. Rectangular core-collapse supernova remnants: application to Puppis A

Author

D M-A Meyer, P F Velázquez, O Petruk, A Chiotellis, M Pohl, A Camps-Fariña, M Petrov, E M Reynoso, J C Toledo-Roy, E M Schneiter, A Castellanos-Ramírez, and A Esquivel

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants [ISM], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, massive [stars], MHD [methods], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), evolution [stars], ddc:520, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n = 1/cm3, T = 8000 K), an organised magnetic field of strength 7 microG has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper we show through 2.5D magneto-hydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 Mo star, that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15 to 20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetised, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A., Accepted at MNRAS

Published
2022
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3. Evidence for γ-ray emission from the remnant of Kepler's supernova based on deep H.E.S.S. observations

Author

Collaboration, H. E. S. S., Aharonian, F., Benkhali, F. Ait, Anguner, E. O., Ashkar, H., Backes, M., Martins, V. Barbosa, Batzofin, R., Becherini, Y., Berge, D., Bernloehr, K., Boettcher, M., Boisson, C., Bolmont, J., de Lavergne, M. de Bony, Breuhaus, M., Brose, R., Brun, F., Bulik, T., Bylund, T., Cangemi, F., Caroff, S., Casanova, S., Cerruti, M., Chand, T., Chen, A., Chibueze, O., Cotter, G., Cristofari, P., Mbarubucyeye, J. Damascene, Devin, J., Djannati-Atai, A., Dmytriiev, A., Egberts, K., Einecke, S., Ernenwein, J. -P., Feijen, K., Fiasson, A., de Clairfontaine, G. Fichet, Fontaine, G., Funk, S., Gabici, S., Gallant, Y. A., Ghafourizadeh, S., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J. F., Grondin, M. -H., Hoerbe, M., Hofmann, W., Holch, T. L., Holler, M., Horns, D., Huang, Zhiqiu, Jamrozy, M., Joshi, V., Jung-Richardt, I., Kasai, E., Katarzynski, K., Katz, U., Khelifi, B., Kluzniak, W., Komin, Nu., Kosack, K., Kostunin, D., Lemiere, A., Lemoine-Goumard, M., Lenain, J. -P., Leuschner, F., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Marti-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Meyer, M., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moulin, E., Muller, J., Nakashima, K., de Naurois, M., Nayerhoda, A., Niemiec, J., Noel, A. Priyana, O'Brien, P., Ohm, S., Olivera-Nieto, L., Wilhelmi, E. de Ona, Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Peron, G., Poireau, V., Prokhorov, D. A., Puehlhofer, G., Punch, M., Quirrenbach, A., Reichherzer, P., Reimer, A., Reimer, O., Renaud, M., Reville, B., Rieger, F., Rowell, G., Rudak, B., Ricarte, H. Rueda, Sahakian, V., Sailer, S., Salzmann, H., Sanchez, D. A., Santangelo, A., Sasaki, M., Schafer, J., Schussler, F., Schutte, H. M., Schwanke, U., Shapopi, J. N. S., Simoni, R., Sol, H., Specovius, A., Spencer, S., Stawarz, L., Steinmassl, S., Steppa, C., Sushch, I., Takahashi, T., Tanaka, T., Taylor, A. M., Terrier, R., Tsirou, M., Uchiyama, Y., Unbehaun, T., van Eldik, C., Veh, J., Vink, J., Voelk, H. J., Wagner, S. J., Werner, F., White, R., Wierzcholska, A., Wong, Yu Wun, Yusafzai, A., Zacharias, M., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zouari, S., Zywucka, N., H.E.S.S. Collaboration, 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 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), 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 Paris Cité (UPCité), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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 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 de Physique des Deux Infinis Bordeaux (LP2I - Bordeaux), Université de Bordeaux (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), H.E.S.S., High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, atmosphere [Cherenkov counter], energy spectrum, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov counter: atmosphere, GeV, VHE, GLAST, individual: Kepler [supernovae], emission [gamma ray], HESS, supernova, Astrophysics::Solar and Stellar Astrophysics, supernovae: individual: Kepler’s SN, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, supernova remnants [ISM], Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Astronomy and Astrophysics, gamma rays: general, gamma-rays: general, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], flux, supernovae: individual: Kepler, gamma ray: emission, Space and Planetary Science, HESS - Abteilung Hinton, ddc:520, high [energy], spectral, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays], statistical, general [gamma-rays], individual: Kepler’s SN [supernovae]
Abstract

Astronomy and astrophysics 662, A65 (2022). doi:10.1051/0004-6361/202243096, Observations with imaging atmospheric Cherenkov telescopes (IACTs) have enhanced our knowledge of nearby supernova (SN) remnants with ages younger than 500 yr by establishing Cassiopeia A and the remnant of Tycho’s SN as very-high-energy (VHE) γ-ray sources. The remnant of Kepler’s SN, which is the product of the most recent naked-eye SN in our Galaxy, is comparable in age to the other two, but is significantly more distant. If the γ-ray luminosities of the remnants of Tycho’s and Kepler’s SNe are similar, then the latter is expected to be one of the faintest γ-ray sources within reach of the current generation IACT arrays. Here we report evidence at a statistical level of 4.6σ for a VHE signal from the remnant of Kepler’s SN based on deep observations by the High Energy Stereoscopic System (H.E.S.S.) with an exposure of 152 h. The measured integral flux above an energy of 226 GeV is ∼0.3% of the flux of the Crab Nebula. The spectral energy distribution (SED) reveals a γ-ray emitting component connecting the VHE emission observed with H.E.S.S. to the emission observed at GeV energies with Fermi-LAT. The overall SED is similar to that of the remnant of Tycho’s SN, possibly indicating the same nonthermal emission processes acting in both these young remnants of thermonuclear SNe., Published by EDP Sciences, Les Ulis

Published
2022

4. Magneto-hydrodynamic simulations of young supernova remnants and their energy-conversion phase

Author

Salvatore Orlando, R Brose, T. Kuzyo, Oleh Petruk, M. Pohl, ITA, DEU, IRL, and UKR

Subjects
Shock wave, MHD, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), FOS: Physical sciences, Astrophysics, Kinetic energy, 01 natural sciences, 0103 physical sciences, Radiative transfer, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, supernova remnants [ISM], Astronomy and Astrophysics, shock waves, Polarization (waves), Magnetic field, Supernova, Space and Planetary Science, ddc:520, Magnetohydrodynamics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Monthly notices of the Royal Astronomical Society 505(1), 755 - 770 (2021). doi:10.1093/mnras/stab1319, Supernova remnants (SNRs) can be rich sources of information on the parent SN (supernova) explosion. Thus, investigating the transition from the phase of SN to that of SNR can be crucial to link these two phases of evolution. Here, we aim to study the early development of SNR in more detail, paying the major attention to the transition from the early expansion stage to the Sedov stage and the role played by magnetic field in this transition. To this end, spherical magnetohydrodynamic simulations of SNRs have been performed to study the evolution of magnetic field in young SNRs and explore a sequence of the SNR evolutionary stages in the pre-radiative epoch. Remnants of three supernova types are considered, namely, SNIa, SNIc, and SNIIP, that covers a wide space of parameters relevant for SNRs. Changes in global characteristics and development of spatial distributions are analysed. It is shown that the radial component of magnetic field rapidly drops downstream of the forward shock. Therefore, the radially aligned polarization patterns observed in few young SNRs cannot be reproduced in the 1D MHD simulations. The period SNR takes for the transition from the earliest ejecta-driven phase to the Sedov phase is long enough, with its distinctive physical features, headed by the energy conversion from mostly kinetic one to a fixed ratio between the thermal and kinetic components. This transition worth to be distinguished as a phase in SNR evolutionary scheme. The updated sequence of stages in SNR evolution could be the free expansion (of gas) – energy conversion – Sedov–Taylor – post-adiabatic – radiative., Published by Oxford Univ. Press, Oxford

Published
2021

5. A Galactic dust devil: far-infrared observations of the Tornado supernova remnant candidate

Author

Jeonghee Rho, Haley Louise Gomez, Mikako Matsuura, Loretta Dunne, I. De Looze, Alberto Noriega-Crespo, Andreas Papageorgiou, F. D. Priestley, H. Chawner, M. J. Barlow, A. D. P. Howard, Matthew Smith, and K. A. Marsh

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, RAYET STAR POPULATIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, MASS, 01 natural sciences, law.invention, Telescope, Far infrared, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, ISM [submillimetre], Supernova remnant, RADIO-CONTINUUM, 010303 astronomy & astrophysics, Stellar evolution, Dust devil, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, HI-GAL, 010308 nuclear & particles physics, supernova remnants [ISM], ISM [infrared], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, CATALOG, CASSIOPEIA, Astrophysics - Solar and Stellar Astrophysics, Physics and Astronomy, STELLAR EVOLUTION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DISCOVERY, Attenuation coefficient, ROTATION, Outflow, Astrophysics::Earth and Planetary Astrophysics, Tornado, Astrophysics - High Energy Astrophysical Phenomena, EMISSION
Abstract

We present complicated dust structures within multiple regions of the candidate supernova remnant (SNR) the `Tornado' (G357.7-0.1) using observations with Spitzer and Herschel. We use Point Process Mapping, PPMAP, to investigate the distribution of dust in the Tornado at a resolution of 8", compared to the native telescope beams of 5-36". We find complex dust structures at multiple temperatures within both the head and the tail of the Tornado, ranging from 15 to 60K. Cool dust in the head forms a shell, with some overlap with the radio emission, which envelopes warm dust at the X-ray peak. Akin to the terrestrial sandy whirlwinds known as `Dust Devils', we find a large mass of dust contained within the Tornado. We derive a total dust mass for the Tornado head of 16.7 solar masses, assuming a dust absorption coefficient of kappa_300 =0.56m^2 kg^1, which can be explained by interstellar material swept up by a SNR expanding in a dense region. The X-ray, infra-red, and radio emission from the Tornado head indicate that this is a SNR. The origin of the tail is more unclear, although we propose that there is an X-ray binary embedded in the SNR, the outflow from which drives into the SNR shell. This interaction forms the helical tail structure in a similar manner to that of the SNR W50 and microquasar SS433., 16 pages, 10 figures + 3 appendix figures. Accepted to be published in MNRAS

Published
2020

6. Spectral softening in core-collapse supernova remnant expanding inside wind-blown bubble

Author

Das, Samata, Brose, Robert, Meyer, Dominique, Pohl, Martin, Sushch, Iurii, and Plotko, Pavlo

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, supernova remnants [ISM], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, bubbles [ISM], cosmic rays, Space and Planetary Science, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, ISM: bubbles, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants
Abstract

Astronomy and astrophysics 661, A128 (2022). doi:10.1051/0004-6361/202142747, Context. Galactic cosmic rays (CRs) are widely assumed to arise from diffusive shock acceleration, specifically at shocks in supernova remnants (SNRs). These shocks expand in a complex environment, particularly in the core-collapse scenario as these SNRs evolve inside the wind-blown bubbles created by their progenitor stars. The CRs at core-collapse SNRs may carry spectral signatures of that complexity.Aims. We study particle acceleration in the core-collapse SNR of a progenitor with an initial mass of 60 M⊙ and realistic stellar evolution. The SNR shock interacts with discontinuities inside the wind-blown bubble and generates several transmitted and reflected shocks. We analyse their impact on particle spectra and the resulting emission from the remnant.Methods. To model the particle acceleration at the forward shock of a SNR expanding inside a wind bubble, we initially simulated the evolution of the pre-supernova circumstellar medium (CSM) by solving the hydrodynamic equations for the entire lifetime of the progenitor star. As the large-scale magnetic field, we considered parameterised circumstellar magnetic field with passive field transport. We then solved the hydrodynamic equations for the evolution of a SNR inside the pre-supernova CSM simultaneously with the transport equation for CRs in test-particle approximation and with the induction equation for the magnetohydrodynamics in 1D spherical symmetry.Results. The evolution of a core-collapse SNR inside a complex wind-blown bubble modifies the spectra of both the particles and their emission on account of several factors including density fluctuations, temperature variations, and the magnetic field configuration. We find softer particle spectra with spectral indices close to 2.5 during shock propagation inside the shocked wind, and this softness persists at later evolutionary stages. Further, our calculated total production spectrum released into the interstellar medium demonstrates spectral consistency at high energy (HE) with the injection spectrum of Galactic CRs, which is required in propagation models. The magnetic field structure effectively influences the emission morphology of SNRs as it governs the transportation of particles and the synchrotron emissivity. There is rarely a full correspondence of the intensity morphology in the radio, X-ray, and gamma-ray bands.Key words: ISM: supernova remnants / ISM: bubbles / cosmic rays★ Movie associated to Fig. B.1 is only available at https://www.aanda.org, Published by EDP Sciences, Les Ulis

Published
2022
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7. Radio observations of supernova remnant G1.9+0.3

Author

Quentin Roper, Michael G. Burton, Ain De Horta, Kieran J. Luken, Gavin Rowell, T. J. Galvin, Nicholas O Ralph, Natasha Hurley-Walker, Miroslav Filipovic, Graeme F Wong, Ray P. Norris, Denis Leahy, Lisa Harvey-Smith, N. Maxted, Dejan Urošević, I. Sushch, Catherine Braiding, Rebecca Blackwell, Roland Kothes, James R. Allison, and Robert Brose

Subjects
Expansion rate, FOS: Physical sciences, ISM [radio continuum], Astrophysics, 01 natural sciences, Radio spectrum, law.invention, Telescope, supernovae: general, law, 0103 physical sciences, ISM: individual objects: G1.9+0.3, Supernova remnant, 010303 astronomy & astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, individual objects: G1.9+0.3 [ISM], Spectral index, 010308 nuclear & particles physics, supernova remnants [ISM], Astronomy and Astrophysics, Continuum flux, Astrophysics - Astrophysics of Galaxies, radio continuum: ISM, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ddc:520, Astrophysics - High Energy Astrophysical Phenomena, general [supernovae]
Abstract

Monthly notices of the Royal Astronomical Society 492(2), 2606 - 2621 (2020). doi:10.1093/mnras/stz3439, We present 1–10 GHz radio continuum flux density, spectral index, polarization, and rotation measure (RM) images of the youngest known Galactic supernova remnant (SNR) G1.9+0.3, using observations from the Australia Telescope Compact Array. We have conducted an expansion study spanning eight epochs between 1984 and 2017, yielding results consistent with previous expansion studies of G1.9+0.3. We find a mean radio continuum expansion rate of (0.78 ± 0.09) per cent yr$^{−1}$ (or ∼8900 km s$^{−1}$ at an assumed distance of 8.5 kpc), although the expansion rate varies across the SNR perimetre. In the case of the most recent epoch between 2016 and 2017, we observe faster-than-expected expansion of the northern region. We find a global spectral index for G1.9+0.3 of −0.81 ± 0.02 (76 MHz–10 GHz). Towards the northern region, however, the radio spectrum is observed to steepen significantly (∼−1). Towards the two so-called (east and west) ‘ears’ of G1.9+0.3, we find very different RM values of 400–600 and 100–200 rad m$^2$, respectively. The fractional polarization of the radio continuum emission reaches (19 ± 2) per cent, consistent with other, slightly older, SNRs such as Cas A., Published by Oxford Univ. Press, Oxford

Published
2019

8. Characterizing mass, momentum, energy, and metal outflow rates of multiphase galactic winds in the FIRE-2 cosmological simulations

Author

Philip F. Hopkins, Daniel Anglés-Alcázar, John C. Forbes, Robert Feldmann, Zachary Hafen, Jonathan Stern, Rachel S. Somerville, Viraj Pandya, Drummond Fielding, Christopher C. Hayward, Norman Murray, Andrew Wetzel, Eliot Quataert, Greg L. Bryan, Chang-Goo Kim, Dušan Kereš, Claude André Faucher-Giguère, University of Zurich, and Pandya, Viraj

Subjects
530 Physics, Astrophysics::High Energy Astrophysical Phenomena, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Momentum, Gravitational potential, 1912 Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Physics, 010308 nuclear & particles physics, Star formation, jets and outflows [ISM], supernova remnants [ISM], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Stars, haloes [galaxies], 13. Climate action, Space and Planetary Science, 10231 Institute for Computational Science, Astrophysics of Galaxies (astro-ph.GA), hydrodynamics, 3103 Astronomy and Astrophysics, Outflow, Halo, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], Astronomical and Space Sciences
Abstract

We characterize mass, momentum, energy and metal outflow rates of multi-phase galactic winds in a suite of FIRE-2 cosmological "zoom-in" simulations from the Feedback in Realistic Environments (FIRE) project. We analyze simulations of low-mass dwarfs, intermediate-mass dwarfs, Milky Way-mass halos, and high-redshift massive halos. Consistent with previous work, we find that dwarfs eject about 100 times more gas from their interstellar medium (ISM) than they form in stars, while this mass "loading factor" drops below one in massive galaxies. Most of the mass is carried by the hot phase ($>10^5$ K) in massive halos and the warm phase ($10^3-10^5$ K) in dwarfs; cold outflows ($, Accepted to MNRAS with minor revisions, main body is 25 pages with 14 figures

Published
2021

9. Mapping the spectral index of Cassiopeia A: evidence for flattening from radio to infrared

Author

J. V. Hernández Santisteban, Jacco Vink, Domček, Ping Zhou, Tracey DeLaney, High Energy Astrophys. & Astropart. Phys (API, FNWI), FMG, and University of St Andrews. School of Physics and Astronomy

Subjects
Acceleration of particles, Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Flattening, 0103 physical sciences, Computer Science::Networking and Internet Architecture, QB Astronomy, 010306 general physics, 010303 astronomy & astrophysics, individual objects: Cassiopeia A [ISM], QC, Astrophysics::Galaxy Astrophysics, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, non-thermal [Radiation mechanisms], supernova remnants [ISM], Astronomy, DAS, Astronomy and Astrophysics, Cassiopeia A, QC Physics, 13. Climate action, Space and Planetary Science, Physics::Accelerator Physics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Synchrotron radiation from supernova remnants are caused by electrons accelerated through diffusive shock acceleration (DSA). The standard DSA theory predicts an electron spectral index of $p=2$, corresponding to a radio spectral index of $\alpha=-0.5$. An extension of DSA predicts that the accelerated particles changes the shock structure, resulting in a spectrum that is steeper than $p>2$ ($\alpha, Comment: 18 pages, 18 figures, accepted to MNRAS

Published
2021

10. High-resolution Hα imaging of the northern Galactic plane and the IGAPS image database

Author

A. A. Zijlstra, Paul J. Groot, S. Phillipps, Robert Greimel, J. Eislöffel, Richard Ashley, C. Fariña, M. J. Barlow, Rhys Morris, Janet E. Drew, Maria Monguió, Nicholas J. Wright, Antonio Mampaso, Tim Naylor, S. Scaringi, B. Stecklum, Mike Irwin, C. Roe, Quentin A. Parker, Laurence Sabin, A. Fernández-Martín, Geert Barentsen, Science and Technology Facilities Council (UK), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, National Aeronautics and Space Administration (US), and Netherlands Organization for Scientific Research

Subjects
HII regions, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Q1, law.invention, Astronomical databases: miscellaneous, law, QB460, Planetary nebulae: general, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Surface brightness, Supernova remnant, QB600, Astrophysics::Galaxy Astrophysics, QB, ISM: general, ISM: supernova remnants, Physics, Pixel, general [ISM], Newtonian telescope, supernova remnants [ISM], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galactic plane, Planetary nebula, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), miscellaneous [Astronomical databases], general [Planetary nebulae], Noise (radio), QB799
Abstract

Greimel, R., et al., The INT Galactic Plane Survey (IGAPS) is the merger of the optical photometric surveys IPHAS and UVEX based on data from the Isaac Newton Telescope (INT) obtained between 2003 and 2018. It captures the entire northern Galactic plane within the Galactic coordinate range |b|< 5° and 30° < ℓ < 215°. From the beginning, the incorporation of narrow-band Hα imaging has been a unique and distinctive feature of this effort. Alongside a focused discussion of the nature and application of the Hα data, we present the IGAPS world-accessible database of images for all five survey filters, i, r, g, URGO, and narrow-band Hα, observed on a pixel scale of 0.33 arcsec and at an effective (median) angular resolution of 1.1-1.3 arcsec. The background, noise, and sensitivity characteristics of the narrow-band Hα filter images are outlined. Typical noise levels in this band correspond to a surface brightness at full ∼1 arcsec resolution of around 2 × 10-16 erg cm-2 s-1 arcsec-2. Illustrative applications of the Hα data to planetary nebulae and Herbig-Haro objects are outlined and, as part of a discussion of the mosaicking technique, we present a very large background-subtracted narrow-band mosaic of the supernova remnant Simeis 147. Finally, we lay out a method that exploits the database via an automated selection of bright ionised diffuse interstellar emission targets for the coming generation of wide-field massive-multiplex spectrographs. Two examples of the diffuse Hα map output from this selection process are presented and compared with previously published data., RG benefitted from support via STFC grant ST/M001334/1 as a visitor to UCL. JED and MM acknowledge the support of research grants funded by the Science, Technology and Facilities Council of the UK (STFC, grants ST/M001008/1 and ST/J001333/1). MM was partially supported by the MINECO (Spanish Ministry of Economy) through grant ESP2016-80079-C2-1-R and RTI2018-095076-B-C21 (MINECO/FEDER, UE), and MDM-2014-0369 of ICCUB (Unidad de Excelencia ‘María de Maeztu’). AM acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant AYA2017-83383-P. PJG is partially supported by NRF-SARChI grant 111692 and acknowledges support from the Netherlands Organisation for Scientific Research (NWO), in contributing to the Isaac Newton Group of Telescopes and through grant 614.000.601. Aspects of the analysis presented have been carried out via TOPCAT and STILTS (Taylor 2006). This research has made use of both the SIMBAD database and the “Aladin sky atlas”, respectively operated and developed at CDS, Strasbourg, France. This research has also made use of the image manipulation software, MONTAGE. It is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration’s Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology.

Published
2021

11. Revisiting the evolution of nonradiative supernova remnants: A hydrodynamical-informed parameterization of the shock positions

Author

Niccolò Bucciantini, B. Olmi, J. M. Martin, Diego F. Torres, Rino Bandiera, Ministerio de Ciencia, Innovación y Universidades (España), ITA, and ESP

Subjects
Physics, Shock wave, High Energy Astrophysical Phenomena (astro-ph.HE), numerical [Methods], Methods: numerical, supernova remnants [ISM], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Pulsar wind nebula, Shock waves, Supernova, Pulsar, Space and Planetary Science, Radiative transfer, Hydrodynamics, Astrophysics::Solar and Stellar Astrophysics, Ejecta, Supernova remnant, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants
Abstract

Understanding the evolution of a supernova remnant shell in time is fundamental. Such understanding is critical to build reliable models of the dynamics of the supernova remnant shell interaction with any pulsar wind nebula it might contain. Here, we perform a large study of the parameter space for the one-dimensional spherically symmetric evolution of a supernova remnant, accompanying it by analytical analysis. Assuming, as is usual, an ejecta density profile with a power-law core and an envelope, and a uniform ambient medium, we provide a set of highly-accurate approximations for the evolution of the main structural features of supernova remnants, such as the reverse and forward shocks and the contact discontinuity. We compare our results with previously adopted approximations, showing that existing simplified prescriptions can easily lead to large errors. In particular, in the context of pulsar wind nebulae modelling, an accurate description for the supernova remnant reverse shock is required. We also study in depth the self-similar solutions for the initial phase of evolution, when the reverse shock propagates through the envelope of the ejecta. Since these self-similar solutions are exact, but not fully analytical, we here provide highly-accurate approximations as well., Comment: 15 pages, 8 figures, 6 tables

Published
2021
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12. Non-thermal radio supernova remnants of exiled Wolf-Rayet stars

Author

D. M.-A. Meyer, Lidia M. Oskinova, M. Petrov, and Martin Pohl

Subjects
Shock wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Wolf–Rayet star, massive [stars], Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Ejecta, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants [ISM], Astronomy and Astrophysics, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], Astrophysics - Astrophysics of Galaxies, Magnetic field, Interstellar medium, stars: massive, Stars, Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ddc:520, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Monthly notices of the Royal Astronomical Society 502(4), 5340 - 5355 (2021). doi:10.1093/mnras/stab452, A signification fraction of Galactic massive stars (⁠|${\ge}8\, \rm M_{\odot }$|⁠) are ejected from their parent cluster and supersonically sail away through the interstellar medium (ISM). The winds of these fast-moving stars blow asymmetric bubbles thus creating a circumstellar environment in which stars eventually die with a supernova explosion. The morphology of the resulting remnant is largely governed by the circumstellar medium of the defunct progenitor star. In this paper, we present 2D magneto-hydrodynamical simulations investigating the effect of the ISM magnetic field on the shape of the supernova remnants of a |$35\, \mathrm{M}_{\odot }$| star evolving through a Wolf–Rayet phase and running with velocity 20 and |$40\, \rm km\, \rm s^{-1}$|⁠, respectively. A |$7\, \mu \rm G$| ambient magnetic field is sufficient to modify the properties of the expanding supernova shock front and in particular to prevent the formation of filamentary structures. Prior to the supernova explosion, the compressed magnetic field in the circumstellar medium stabilizes the wind/ISM contact discontinuity in the tail of the wind bubble. A consequence is a reduced mixing efficiency of ejecta and wind materials in the inner region of the remnant, where the supernova shock wave propagates. Radiative transfer calculations for synchrotron emission reveal that the non-thermal radio emission has characteristic features reflecting the asymmetry of exiled core-collapse supernova remnants from Wolf–Rayet progenitors. Our models are qualitatively consistent with the radio appearance of several remnants of high-mass progenitors, namely the bilateral G296.5+10.0 and the shell-type remnants CTB109 and Kes 17, respectively., Published by Oxford Univ. Press, Oxford

Published
2021

13. LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV

Author

Abdalla, H., Aharonian, F., Martins, V. Barbosa, Klepser, S., Kluźniak, W., Komin, Nu., Konno, R., Kosack, K., Kostunin, D., Kreter, M., Mezek, G. Kukec, Kundu, A., Lamanna, G., Barnacka, A., Stum, S. Le, Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leuschner, F., Levy, C., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Barnard, M., Majumdar, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Mares, A., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Batzofin, R., Meyer, M., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moore, C., Morris, P., Moulin, E., Muller, J., Murach, T., Becherini, Y., Nakashima, K., de Naurois, M., Nayerhoda, A., Ndiyavala, H., Niemiec, J., Oakes, L., Peyaud, B., Piel, Q., Noel, A. Priyana, O'Brien, P., Berge, D., Oberholzer, L., Odaka, H., Ohm, S., Olivera-Nieto, L., Wilhelmi, E. de Ona, Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Peron, G., Bernlöhr, K., Pita, S., Poireau, V., Prokhorov, D. A., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Rauth, R., Reichherzer, P., Bi, B., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Rinchiuso, L., Reville, B., Rieger, F., Romoli, C., Rowell, G., Rudak, B., Böttcher, M., Ricarte, H. Rueda, Ruiz-Velasco, E., Sahakian, V., Sailer, S., Salzmann, H., Sanchez, D. A., Santangelo, A., Sasaki, M., Scalici, M., Schäfer, J., Boisson, C., Schüssler, F., Schutte, H. M., Schwanke, U., Seglar-Arroyo, M., Senniappan, M., Seyffert, A. S., Shafi, N., Shapopi, J. N. S., Shiningayamwe, K., Simoni, R., Benkhali, F. Ait, Bolmont, J., Sinha, A., Sol, H., Specovius, A., Spencer, S., Spir-Jacob, M., Stawarz, L., Steenkamp, R., Stegmann, C., Steinmassl, S., Steppa, C., de Lavergne, M. de Bony, Sun, L., Takahashi, T., Tanaka, T., Tavernier, T., Taylor, A. M., Terrier, R., Thiersen, J. H. E., Thorpe-Morgan, C., Tiziani, D., Tluczykont, M., Breuhaus, M., Tomankova, L., Trichard, C., Tsirou, M., Tsuji, N., Tuffs, R., Uchiyama, Y., van der Walt, D. J., van Eldik, C., van Rensburg, C., van Soelen, B., Brose, R., Vasileiadis, G., Veh, J., Venter, C., Vincent, P., Vink, J., Völk, H. J., Wadiasingh, Z., Wagner, S. J., Watson, J., Werner, F., Brun, F., White, R., Wierzcholska, A., Wong, Yu Wun, Yassin, H., Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Brun, P., Zhu, S. J., Zmija, A., Zorn, J., Zouari, S., Żywucka, N., H. E. S. S. Collaboration, Bryan, M., Büchele, M., Bulik, T., Bylund, T., Angüner, E. O., Cangemi, F., Caroff, S., Carosi, A., Casanova, S., Catalano, J., Chambery, P., Chand, T., Chandra, S., Chen, A., Cotter, G., Arcaro, C., Curyło, M., Mbarubucyeye, J. Damascene, Davids, I. D., Davies, J., Deil, C., Devin, J., Dirson, L., Djannati-Atai, A., Dmytriiev, A., Donath, A., Armand, C., Doroshenko, V., Dreyer, L., Plessis, L. Du, Duffy, C., Dyks, J., Egberts, K., Eichhorn, F., Einecke, S., Emery, G., Ernenwein, J.-P., Armstrong, T., Fegan, S., Feijen, K., Fiasson, A., de Clairfontaine, G. Fichet, Fontaine, G., Lott, F., Füßling, M., Funk, S., Gabici, S., Gallant, Y. A., Ashkar, H., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J. F., Grondin, M.-H., Hattingh, S., Hahn, J., Haupt, M., Hermann, G., Hinton, J. A., Backes, M., Hofmann, W., Hoischen, C., Holch, T. L., Holler, M., Hörbe, M., Horns, D., Huang, Zhiqiu, Huber, D., Jamrozy, M., Jankowsky, D., Baghmanyan, V., Jankowsky, F., Jardin-Blicq, A., Joshi, V., Jung-Richardt, I., Kasai, E., Kastendieck, M. A., Katarzynski, K., Katz, U., Khangulyan, D., Khélifi, B., 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 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), 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, 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), H.E.S.S., Collaboration, H.E.S.S., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics, Spectral line, Luminosity, cosmic rays, High Energy Stereoscopic System, Large Magellanic Cloud, Supernova remnant, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Computer Science::Information Retrieval, supernova remnants [ISM], Astronomy and Astrophysics, gamma rays: general, Space and Planetary Science, Spectral energy distribution, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [gamma rays], Fermi Gamma-ray Space Telescope
Abstract

Astronomy and astrophysics 655, A7 (2021). doi:10.1051/0004-6361/202141486, Context. Supernova remnants (SNRs) are commonly thought to be the dominant sources of Galactic cosmic rays up to the knee of the cosmic-ray spectrum at a few PeV. Imaging Atmospheric Cherenkov Telescopes have revealed young SNRs as very-high-energy (VHE, >100 GeV) gamma-ray sources, but for only a few SNRs the hadronic cosmic-ray origin of their gamma-ray emission is indisputably established. In all these cases, the gamma-ray spectra exhibit a spectral cutoff at energies much below 100 TeV and thus do not reach the PeVatron regime.Aims. The aim of this work was to achieve a firm detection for the oxygen-rich SNR LMC N132D in the VHE gamma-ray domain with an extended set of data, and to clarify the spectral characteristics and the localization of the gamma-ray emission from this exceptionally powerful gamma-ray-emitting SNR.Methods. We analyzed 252 h of High Energy Stereoscopic System (H.E.S.S.) observations towards SNR N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 h of observations to the previously published data set to ensure a > 5σ detection. To broaden the gamma-ray spectral coverage required for modeling the spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was also included.Results. We unambiguously detect N132D at VHE with a significance of 5.7σ. We report the results of a detailed analysis of its spectrum and localization based on the extended H.E.S.S. data set. The joint analysis of the extended H.E.S.S and Fermi-LAT data results in a spectral energy distribution in the energy range from 1.7 GeV to 14.8 TeV, which suggests a high luminosity of N132D at GeV and TeV energies. We set a lower limit on a gamma-ray cutoff energy of 8 TeV with a confidence level of 95%. The new gamma-ray spectrum as well as multiwavelength observations of N132D when compared to physical models suggests a hadronic origin of the VHE gamma-ray emission.Conclusions. SNR N132D is a VHE gamma-ray source that shows a spectrum extending to the VHE domain without a spectral cutoff at a few TeV, unlike the younger oxygen-rich SNR Cassiopeia A. The gamma-ray emission is best explained by a dominant hadronic component formed by diffusive shock acceleration. The gamma-ray properties of N132D may be affected by an interaction with a nearby molecular cloud that partially lies inside the 95% confidence region of the source position.Key words: gamma rays: general / cosmic rays / ISM: supernova remnants, Published by EDP Sciences, Les Ulis

Published
2021

14. Planck intermediate results

Author

Adam, R, Ade, PAR, Aghanim, N, Arnaud, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartlett, JG, Bartolo, N, Battaner, E, Benabed, K, Benoit-Lévy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, J-F, Catalano, A, Challinor, A, Chamballu, A, Chary, R-R, Chiang, HC, Christensen, PR, Clements, DL, Colombi, S, Colombo, LPL, Combet, C, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Zotti, G, Delabrouille, J, Delouis, J-M, Désert, F-X, Dickinson, C, Diego, JM, Dolag, K, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dunkley, J, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Falgarone, E, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Héraud, Y, Gjerløw, E, González-Nuevo, J, Górski, KM, Gratton, S, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, FK, Hanson, D, Harrison, DL, Helou, G, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hivon, E, Hobson, M, Holmes, WA, Huffenberger, KM, Hurier, G, Jaffe, AH, Jaffe, TR, and Jewell, J

Subjects
statistics [galaxies], instruments [space vehicles], galaxies [submillimeter], cosmic background radiation, general [X-rays], Astrophysics::Solar and Stellar Astrophysics, clusters: general [galaxies], submillimeter, dark ages, general [radiation mechanisms], relativistic processes, astro-ph.HE, theory [cosmology], general [ISM], extinction, supernova remnants [ISM], Astrophysics::Instrumentation and Methods for Astrophysics, ISM [infrared], observations [cosmology], bubbles [ISM], ISM - dust, observations, clusters: intracluster medium [galaxies], active [galaxies], structure [galaxies], astro-ph.CO, reionization, Astrophysics::Earth and Planetary Astrophysics, dust, large-scale structure of Universe, star formation [galaxies], disk [Galaxy], clouds [ISM], local insterstellar matter, high-redshift [galaxies], Astronomical and Space Sciences, Astrophysics::High Energy Astrophysical Phenomena, astro-ph.GA, statistical [methods], first stars, individual: Messier 31 [galaxies], ISM [radio continuum], Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Affordable and Clean Energy, ISM [gamma rays], cosmic rays, surveys, weak [gravitational lensing], diffuse background [infrared], atomic data, data analysis [methods], reference systems, general [planets and satellites], cosmological parameters, ISM [submillimeter], general [infrared], general [Galaxy], evolution [galaxies], Astrophysics::Galaxy Astrophysics, nucleus [Galaxy], polarization, detectors [instrumentation], ISM [galaxies], turbulence, magnetic fields [ISM], clusters: individual: Virgo [galaxies], general [submillimeter], galaxies [radio continuum], diffuse radiation, astro-ph.EP, structure [ISM], magnetohydrodynamics, cosmology, catalogs, general [galaxies], astro-ph.IM
Abstract

The six parameters of the standard ΛCDM model have best-fit values derived from the Planck temperature power spectrum that are shifted somewhat from the best-fit values derived from WMAP data. These shifts are driven by features in the Planck temperature power spectrum at angular scales that had never before been measured to cosmic-variance level precision. We have investigated these shifts to determine whether they are within the range of expectation and to understand their origin in the data. Taking our parameter set to be the optical depth of the reionized intergalactic medium, the baryon density ωb, the matter density ωm, the angular size of the sound horizon the spectral index of the primordial power spectrum, ns, and Ase-2τ (where As is the amplitude of the primordial power spectrum), we have examined the change in best-fit values between a WMAP-like large angular-scale data set (with multipole moment < 800 in the Planck temperature power spectrum) and an all angular-scale data set (< 2500Planck temperature power spectrum), each with a prior on τ of 0.07 ± 0.02. We find that the shifts, in units of the 1σ expected dispersion for each parameter, are {value of 8.0. We find that this χ2 value is exceeded in 15% of our simulated data sets, and that a parameter deviates by more than 2.2σ in 9% of simulated data sets, meaning that the shifts are not unusually large. Comparing < 800 instead to > 800, or splitting at a different multipole, yields similar results. We examined the < 800 model residuals in the > 800 power spectrum data and find that the features there that drive these shifts are a set of oscillations across a broad range of angular scales. Although they partly appear similar to the effects of enhanced gravitational lensing, the shifts in ΛCDM parameters that arise in response to these features correspond to model spectrum changes that are predominantly due to non-lensing effects; the only exception is, which, at fixed Ase-2τ, affects the > 800 temperature power spectrum solely through the associated change in As and the impact of that on the lensing potential power spectrum. We also ask, "what is it about the power spectrum at < 800 that leads to somewhat different best-fit parameters than come from the full range?" We find that if we discard the data at < 30, where there is a roughly 2σ downward fluctuation in power relative to the model that best fits the full range, the < 800 best-fit parameters shift significantly towards the < 2500 best-fit parameters. In contrast, including < 30, this previously noted "low-deficit" drives ns up and impacts parameters correlated with ns, such as ωm and H0. As expected, the < 30 data have a much greater impact on the < 800 best fit than on the < 2500 best fit. So although the shifts are not very significant, we find that they can be understood through the combined effects of an oscillatory-like set of high-residuals and the deficit in low-power, excursions consistent with sample variance that happen to map onto changes in cosmological parameters. Finally, we examine agreement between PlanckTT data and two other CMB data sets, namely the Planck lensing reconstruction and the TT power spectrum measured by the South Pole Telescope, again finding a lack of convincing evidence of any significant deviations in parameters, suggesting that current CMB data sets give an internally consistent picture of the ΛCDM model.

Published
2020

15. Reverberation of pulsar wind nebulae (I): Impact of the medium properties and other parameters upon the extent of the compression

Author

Niccolò Bucciantini, Jonathan Martin, Rino Bandiera, B. Olmi, Diego F. Torres, Ministerio de Ciencia, Innovación y Universidades (España), and Istituto Nazionale di Astrofisica

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Reverberation, numerical [Methods], non-thermal [Radiation mechanisms], Methods: numerical, Radiation mechanisms: non-thermal, 010308 nuclear & particles physics, supernova remnants [ISM], Acoustics, Astrophysics::High Energy Astrophysical Phenomena, general [Pulsars], FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Pulsars: general, Pulsar, Space and Planetary Science, Compression (functional analysis), 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants
Abstract

The standard approach to the long-term evolution of pulsar wind nebulae (PWNe) is based on one-zone models treating the nebula as a uniform system. In particular for the late phase of evolved systems, many of the generally used prescriptions are based on educated guesses for which a proper assessment lacks. Using an advanced radiative code, we evaluate the systematic impact of various parameters, like the properties of the supernova ejecta, of the inner pulsar, as well of the ambient medium, upon the extent of the reverberation phase of PWNe. We investigate how different prescriptions shift the starting time of the reverberation phase, how this affects the amount of the compression, and how much of this can be ascribable to the radiation processes. Some critical aspects are the description of the reverse shock evolution, the efficiency by which at later times material from the ejecta accretes on to the swept-up shell around the PWN, and finally the density, velocity, and pressure profiles in the surrounding supernova remnant. We have explicitly treated the cases of the Crab Nebula, and of J1834.9-0846, taken to be representatives of the more and the less energetic pulsars, respectively. Especially for the latter object, the prediction of large compression factors is confirmed, even larger in the presence of radiative losses, also confirming our former prediction of periods of superefficiency during the reverberation phase of some PWNe., This work has been supported by grants PGC2018-095512-B-I00, SGR2017-1383, AYA2017-92402-EXP, 2017-14-H.O ASI-INAF and INAF MAINSTREAM

Published
2020

16. SNR G39.2-0.3, an hadronic cosmic rays accelerator

Author

I. Sushch, Y. Su, Emma de Oña Wilhelmi, Enrique Mestre, Robert Brose, Roberta Zanin, 24922986 - Sushch, Iurii, and Alexander von Humboldt Foundation

Subjects
heavy [nucleus], acceleration: efficiency, magnetic field: high, Infrared, Physics::Instrumentation and Detectors, Hadron, Astrophysics, p: acceleration, ISM: clouds, ISM [gammarays], clouds: ISM, high [magnetic field], ISM [Gamma-rays], individual objects: G39.2–0.3 [ISM], cloud, Astrophysics::Solar and Stellar Astrophysics, ISM: individual objects: G39.2–0.3, ISM [clouds], ISM: supernova remnants, energy spectrum [gamma ray], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, supernova remnants [ISM], shock waves, efficiency [acceleration], Magnetic field, gammarays: ISM, Wavelength, Supernova, gamma ray: emission, nucleus: heavy, cosmic radiation: galaxy, infrared, Spectral energy distribution, high [energy], Astrophysics - High Energy Astrophysical Phenomena, clouds [ISM], velocity, accelerator, target: density, Astrophysics::High Energy Astrophysical Phenomena, satellite, acceleration [p], FOS: Physical sciences, Cosmic ray, Radiation, gamma ray: energy spectrum, Computer Science::Digital Libraries, GLAST, Nuclear physics, Acceleration, emission [gamma ray], density [target], gas, supernova, individual objects: G39.2-0.3 [ISM], Astrophysics::Galaxy Astrophysics, gamma-rays: ISM, Astronomy and Astrophysics, Space and Planetary Science, ddc:520, galaxy [cosmic radiation], spectral, ISM: individual objects: G39.2-0.3
Abstract

arXiv:2007.04627v2, Recent results obtained with gamma-ray satellites have established supernova remnants as accelerators of GeV hadronic cosmic rays. In such processes, CRs accelerated in SNR shocks interact with particles from gas clouds in their surrounding. In particular, the rich medium in which core-collapse SNRs explode provides a large target density to boost hadronic gamma-rays. SNR G39.2–0.3 is one of the brightest SNR in infrared wavelengths, and its broad multiwavelength coverage allows a detailed modelling of its radiation from radio to high energies. We reanalysed the Fermi-LAT data on this region and compare it with new radio observations from the MWISP survey. The modelling of the spectral energy distribution from radio to GeV energies favours a hadronic origin of the gamma-ray emission and constrains the SNR magnetic field to be at least ∼100 µG. Despite the large magnetic field, the present acceleration of protons seems to be limited to ∼10 GeV, which points to a drastic slow down of the shock velocity due to the dense wall traced by the CO observations, surrounding the remnant. Further investigation of the gamma-ray spectral shape points to a dynamically old remnant subjected to severe escape of CRs and a decrease of acceleration efficiency. The low-energy peak of the gamma-ray spectrum also suggests that that the composition of accelerated particles might be enriched by heavy nuclei which is certainly expected for a core-collapse SNR. Alternatively, the contribution of the compressed pre-existing Galactic cosmic rays is discussed, which is, however, found to not likely be the dominant process for gamma-ray production., This research was supported by the Alexander von Humboldt Foundation.

Published
2020

17. Stochastic re-acceleration and magnetic-field damping in Tycho ’s supernova remnant

Author

Vikram V. Dwarkadas, I. Telezhinsky, Martin Pohl, and A. Wilhelm

Subjects
Shock wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, ISM: individual objects: Tycho’s SNR, 01 natural sciences, Momentum, Acceleration, cosmic rays, 0103 physical sciences, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, ISM: supernova remnants, acceleration of particles, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Computer Science::Information Retrieval, supernova remnants [ISM], Astronomy and Astrophysics, shock waves, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], individual objects: Tycho’s SNR [ISM], Shock (mechanics), Supernova, Space and Planetary Science, ddc:520, Induction equation, Astrophysics - High Energy Astrophysical Phenomena, Event (particle physics)
Abstract

Astronomy and astrophysics 639, A124 (2020). doi:10.1051/0004-6361/201936079, Context. Tycho’s supernova remnant (SNR) is associated with the historical supernova (SN) event SN 1572 of Type Ia. The explosion occurred in a relatively clean environment, and was visually observed, providing an age estimate. This SNR therefore represents an ideal astrophysical test-bed for the study of cosmic-ray acceleration and related phenomena. A number of studies suggest that shock acceleration with particle feedback and very efficient magnetic-field amplification combined with Alfvénic drift are needed to explain the rather soft radio spectrum and the narrow rims observed in X-rays.Aims. We show that the broadband spectrum of Tycho’s SNR can alternatively be well explained when accounting for stochastic acceleration as a secondary process. The re-acceleration of particles in the turbulent region immediately downstream of the shock should be efficient enough to impact particle spectra over several decades in energy. The so-called Alfvénic drift and particle feedback on the shock structure are not required in this scenario. Additionally, we investigate whether synchrotron losses or magnetic-field damping play a more profound role in the formation of the non-thermal filaments.Methods. We solved the full particle transport equation in test-particle mode using hydrodynamic simulations of the SNR plasma flow. The background magnetic field was either computed from the induction equation or follows analytic profiles, depending on the model considered. Fast-mode waves in the downstream region provide the diffusion of particles in momentum space.Results. We show that the broadband spectrum of Tycho can be well explained if magnetic-field damping and stochastic re-acceleration of particles are taken into account. Although not as efficient as standard diffusive shock acceleration, stochastic acceleration leaves its imprint on the particle spectra, which is especially notable in the emission at radio wavelengths. We find a lower limit for the post-shock magnetic-field strength ∼330 μG, implying efficient amplification even for the magnetic-field damping scenario. Magnetic-field damping is necessary for the formation of the filaments in the radio range, while the X-ray filaments are shaped by both the synchrotron losses and magnetic-field damping., Published by EDP Sciences, Les Ulis

Published
2020

18. Exploiting morphological data from Pulsar Wind Nebulae via a spatiotemporal leptonic transport code

Author

Christo Venter, A. S. Seyffert, Alice K. Harding, C. van Rensburg, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, and 20126999 - Seyffert, Albertus Stefanus

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, general [Gamma-rays], non-thermal [Radiation mechanisms], numerical [Methods], Astrophysics::High Energy Astrophysical Phenomena, supernova remnants [ISM], FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, law.invention, Telescope, Pulsar, Space and Planetary Science, law, Test statistic, Spectral energy distribution, Surface brightness, Astrophysics - High Energy Astrophysical Phenomena, Cherenkov radiation
Abstract

The next era of ground-based Cherenkov telescope development will see a great increase in both quantity and quality of $\gamma$-ray morphological data. This initiated the development of a spatio-temporal leptonic transport code to model pulsar wind nebulae. We present results from this code that predicts the evolution of the leptonic particle spectrum and radiation at different radii in a spherically-symmetric source. We simultaneously fit the overall broadband spectral energy distribution, the surface brightness profile and the X-ray photon index vs.\ radius for PWN 3C~58, PWN G21.5$-$0.9 and PWN G0.9+0.1. Such concurrent fitting of disparate data sets is non-trivial and we thus investigate the utility of different goodness-of-fit statistics, specifically the traditional $\chi^2$ test statistic and a newly developed scaled-flux-normalised test statistic to obtain best-fit parameters. We find reasonable fits to the spatial and spectral data of all three sources, but note some remaining degeneracies that will have to be broken by future observations., Comment: 13 Pages, 13 Figures. 4 Tables

Published
2020

19. Studying the nature of the unidentified gamma-ray source HESS J1841−055 with the MAGIC telescopes

Author

A Acciari, V, Ansoldi, S, A Antonelli, L, Arbet , A, Engels, Asano, K, Baack, D, Babić, A, Banerjee, B, Baquero, A, Barresundefined, U, deundefined, Almeida, A Barrio, J, Becerraundefined, J, González, Bednarek, W, Bellizzi, L, Bernardini, E, Bernardos, M, Berti, A, Besenrieder, J, Bhattacharyya, W, Bigongiari, C, Biland, A, Blanch, O, Bonnoli, G, Bošnjak, Ž, Busetto, G, Carosi, R, Ceribella, G, Cerruti, M, Chai, Y, Chilingarian, A, Cikota, S, M Colak, S, Colombo, E, L Contreras, J, Cortina, J, Covino, S, D’Amico, G, D’Elia, V, Daundefined, P, Vela, Dazzi, F, Deundefined, A, Angelis, Deundefined, B, Lotto, Delfino, M, Delgado, J, Delgadoundefined, C, Mendez, Depaoli, D, Diundefined, T, Girolamo, Diundefined, F, Pierro, Diundefined, L, Venere, Doundefined, E, Soutoundefined, Espiñeira, Dominisundefined, D, Prester, Donini, A, Dorner, D, Doro, M, Elsaesser, D, Fallahundefined, V, Ramazani, Fattorini, A, Ferrara, G, Foffano, L, V Fonseca, M, Font, L, Fruck, C, Fukami, S, J Garcíaundefined, R, López, Garczarczyk, M, Gasparyan, S, Gaug, M, Giglietto, N, Giordano, F, Gliwny, P, Godinović, N, Green, D, Hadasch, D, Hahn, A, Heckmann, L, Herrera, J, Hoang, J, Hrupec, D, Hütten, M, Inada, T, Inoue, S, Ishio, K, Iwamura, Y, Jouvin, L, Kajiwara, Y, Karjalainen, M, Kerszberg, D, Kobayashi, Y, Kubo, H, Kushida, J, Lamastra, A, Lelas, D, Leone, F, Lindfors, E, Lombardi, S, Longo, F, López, M, López-Coto, R, López-Oramas, A, Loporchio, S, Machadoundefined, B, deundefined, Oliveiraundefined, Fraga, Maggio, C, Majumdar, P, Makariev, M, Mallamaci, M, Maneva, G, Manganaro, M, Mannheim, K, Maraschi, L, Mariotti, M, Martínez, M, Mazin, D, Mender, S, Mićanović, S, Miceli, D, Miener, T, Minev, M, M Miranda, J, Mirzoyan, R, Molina, E, Moralejo, A, Morcuende, D, Moreno, V, Moretti, E, Munar-Adrover, P, Neustroev, V, Nigro, C, Nilsson, K, Ninci, D, Nishijima, K, Noda, K, Nozaki, S, Ohtani, Y, Oka, T, Otero-Santos, J, Palatiello, M, Paneque, D, Paoletti, R, M Paredes, J, Pavletić, L, Peñil, P, Perennes, C, Persic, M, G Pradaundefined, P, Moroni, Prandini, E, Priyadarshi, C, Puljak, I, Rhode, W, Ribó, M, Rico, J, Righi, C, Rugliancich, A, Saha, L, Sahakyan, N, Saito, T, Sakurai, S, Satalecka, K, Schleicher, B, Schmidt, K, Schweizer, T, Sitarek, J, Šnidarić, I, Sobczynska, D, Spolon, A, Stamerra, A, Strom, D, Strzys, M, Suda, Y, Surić, T, Takahashi, M, Tavecchio, F, Temnikov, P, Terzić, T, Teshima, M, Torres-Albà, N, Tosti, L, Truzzi, S, vanundefined, J, Scherpenberg, Vanzo, G, Vazquezundefined, M, Acosta, Ventura, S, Verguilov, V, F Vigorito, C, Vitale, V, Vovk, I, Will, M, Zarić, D, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Japan Society for the Promotion of Science, German Research Foundation, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Asano, K., Baack, D., Babic, A., Banerjee, B., Baquero, A., Barres De Almeida, U., Barrio, J. A., Becerra Gonzalez, J., Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bosnjak, Z., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Amico, G., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., Di Girolamo, T., Di Pierro, F., Di Venere, L., Do Souto Espineira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., Garcia Lopez, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinovic, N., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., Hutten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Lopez-Coto, R., Lopez-Oramas, A., Loporchio, S., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Mazin, D., Mender, S., Micanovic, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletic, L., Penil, P., Perennes, C., Persic, M., Prada Moroni, P. G., Prandini, E., Priyadarshi, C., Puljak, I., Rhode, W., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Snidaric, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Suric, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Tosti, L., Truzzi, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., and Zaric, D.

Subjects
gamma-rays: stars, ISM: individual objects: HESS J1841−055, ISM: supernova remnants, radiation mechanisms: non-thermal, pulsars: general, Hadron, pi, Astrophysics, individual objects: HESS J1841−055 [ISM], 4/3, 01 natural sciences, general [pulsars], HESS, cloud, MAGIC (telescope), 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, supernova remnants [ISM], ISM: individual objects: HESS J1841-055, Astrophysics - High Energy Astrophysical Phenomena, Gamma ray, Bremsstrahlung, model: hadronic, non-thermal [radiation mechanisms], Supernova remnant [ISM], gamma ray: emission, curvature, Spectral energy distribution, Electrónica, Electricidad, ISM: Individual objects: HESS J1841-055, Astrophysics::High Energy Astrophysical Phenomena, Star [gamma-rays], energy spectrum, FOS: Physical sciences, Curvature, bremsstrahlung, GeneralLiterature_MISCELLANEOUS, GLAST, stars [gamma-rays], energy dependence, gamma-rays: Stars, ISM: Supernova remnants, pulsars: General, radiation mechanisms: Non-thermal, Pion, emission [gamma ray], 0103 physical sciences, 010308 nuclear & particles physics, Molecular cloud, ComputingMilieux_PERSONALCOMPUTING, Astronomy and Astrophysics, MAGIC, Individual objects: HESS J1841-055 [ISM], Space and Planetary Science, ddc:520, spectral, High Energy Physics::Experiment, hadronic [model]
Abstract

MAGIC Collaboration: et al., We investigate the physical nature and origin of the gamma-ray emission from the extended source HESS J1841−055 observed at TeV and GeV energies. We observed HESS J1841−055 at TeV energies for a total effective time of 43 h with the MAGIC telescopes, in 2012 and 2013. Additionally, we analysed the GeV counterpart making use of about 10 yr of Fermi-LAT data. Using both Fermi-LAT and MAGIC, we study both the spectral and energy-dependent morphology of the source for almost four decades of energy. The origin of the gamma-ray emission from this region is investigated using multiwaveband information on sources present in this region, suggested to be associated with this unidentified gamma-ray source. We find that the extended emission at GeV–TeV energies is best described by more than one source model. We also perform the first energy-dependent analysis of the HESS J1841−055 region at GeV–TeV. We find that the emission at lower energies comes from a diffuse or extended component, while the major contribution of gamma rays above 1 TeV arises from the southern part of the source. Moreover, we find that a significant curvature is present in the combined observed spectrum of MAGIC and Fermi-LAT. The first multiwavelength spectral energy distribution of this unidentified source shows that the emission at GeV–TeV energies can be well explained with both leptonic and hadronic models. For the leptonic scenario, bremsstrahlung is the dominant emission compared to inverse Compton. On the other hand, for the hadronic model, gamma-ray resulting from the decay of neutral pions (π0) can explain the observed spectrum. The presence of dense molecular clouds overlapping with HESS J1841−055 makes both bremsstrahlung and π0-decay processes the dominant emission mechanisms for the source., The financial support by the German BMBF and MPG; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, and FPA2017-90566-REDC); the Indian Department of Atomic Energy; and the Japanese JSPS and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia ‘Severo Ochoa’ SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia ‘Maria de Maeztu’ MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ.

Published
2020
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20. MAGIC very large zenith angle observations of the Crab Nebula up to 100 TeV

Author

Acciari, V. A. (V. A.), Ansoldi, S. (S.), Antonelli, L. A. (L. A.), Engels, A. A. (A. Arbet), Baack, D. (D.), Babic, A. (A.), Banerjee, B. (B.), Barres de Almeida, U. (U.), Barrio, J. A. (J. A.), Becerra Gonzalez, J. (J.), Bednarek, W. (W.), Bellizzi, L. (L.), Bernardini, E. (E.), Berti, A. (A.), Besenrieder, J. (J.), Bhattacharyya, W. (W.), Bigongiari, C. (C.), Biland, A. (A.), Blanch, O. (O.), Bonnoli, G. (G.), Bosnjak, Z. (Z.), Busetto, G. (G.), Carosi, A. (A.), Carosi, R. (R.), Ceribella, G. (G.), Chai, Y. (Y.), Chilingaryan, A. (A.), Cikota, S. (S.), Colak, S. M. (S. M.), Colin, U. (U.), Colombo, E. (E.), Contreras, J. L. (J. L.), Cortina, J. (J.), Covino, S. (S.), D'Amico, G. (G.), D'Elia, V. (V), Da Vela, P. (P.), Dazzi, F. (F.), De Angelis, A. (A.), De Lotto, B. (B.), Delfino, M. (M.), Delgado, J. (J.), Depaoli, D. (D.), Di Pierro, F. (F.), Di Venere, L. (L.), Do Souto Espineira, E. (E.), Prester, D. D. (D. Dominis), Donini, A. (A.), Dorner, D. (D.), Doro, M. (M.), Elsaesser, D. (D.), Ramazani, V. F. (V. Fallah), Fattorini, A. (A.), Fernandez-Barral, A. (A.), Ferrara, G. (G.), Fidalgo, D. (D.), Foffano, L. (L.), Fonseca, M. V. (M., V), Font, L. (L.), Fruck, C. (C.), Fukami, S. (S.), Gallozzi, S. (S.), Garcia Lopez, R. J. (R. J.), Garczarczyk, M. (M.), Gasparyan, S. (S.), Gaug, M. (M.), Giglietto, N. (N.), Giordano, F. (F.), Godinovic, N. (N.), Green, D. (D.), Guberman, D. (D.), Hadasch, D. (D.), Hahn, A. (A.), Herrera, J. (J.), Hoang, J. (J.), Hrupec, D. (D.), Huetten, M. (M.), Inada, T. (T.), Inoue, S. (S.), Ishio, K. (K.), Iwamura, Y. (Y.), Jouvin, L. (L.), Kerszberg, D. (D.), Kubo, H. (H.), Kushida, J. (J.), Lamastra, A. (A.), Lelas, D. (D.), Leone, F. (F.), Lindfors, E. (E.), Lombardi, S. (S.), Longo, F. (F.), Lopez, M. (M.), Lopez-Coto, R. (R.), Lopez-Oramas, A. (A.), Loporchio, S. (S.), Machado de Oliveira Fraga, B. (B.), Maggio, C. (C.), Majumdar, P. (P.), Makariev, M. (M.), Mallamaci, M. (M.), Maneva, G. (G.), Manganaro, M. (M.), Mannheim, K. (K.), Maraschi, L. (L.), Mariotti, M. (M.), Martinez, M. (M.), Masuda, S. (S.), Mazin, D. (D.), Micanovic, S. (S.), Miceli, D. (D.), Minev, M. (M.), Miranda, J. M. (J. M.), Mirzoyan, R. (R.), Molina, E. (E.), Moralejo, A. (A.), Morcuende, D. (D.), Moreno, V. (V), Moretti, E. (E.), Munar-Adrover, P. (P.), Neustroev, V. (V), Nigro, C. (C.), Nilsson, K. (K.), Ninci, D. (D.), Nishijima, K. (K.), Noda, K. (K.), Nogues, L. (L.), Noethe, M. (M.), Nozaki, S. (S.), Paiano, S. (S.), Palacio, J. (J.), Palatiello, M. (M.), Paneque, D. (D.), Paoletti, R. (R.), Paredes, J. M. (J. M.), Penil, P. (P.), Peresano, M. (M.), Persic, M. (M.), Moroni, P. G. (P. G. Prada), Prandini, E. (E.), Puljak, I. (I), Rhode, W. (W.), Ribo, M. (M.), Rico, J. (J.), Righi, C. (C.), Rugliancich, A. (A.), Saha, L. (L.), Sahakyan, N. (N.), Saito, T. (T.), Sakurai, S. (S.), Satalecka, K. (K.), Schmidt, K. (K.), Schweizer, T. (T.), Sitarek, J. (J.), Snidaric, I. (I), Sobczynska, D. (D.), Somero, A. (A.), Stamerra, A. (A.), Strom, D. (D.), Strzys, M. (M.), Suda, Y. (Y.), Suric, T. (T.), Takahashi, M. (M.), Tavecchio, F. (F.), Temnikov, P. (P.), Terzic, T. (T.), Teshima, M. (M.), Torres-Alba, N. (N.), Tosti, L. (L.), Tsujimoto, S. (S.), Vagelli, V. (V.), van Scherpenberg, J. (J.), Vanzo, G. (G.), Vazquez Acosta, M. (M.), Vigorito, C. F. (C. F.), Vitale, V. (V.), Vovk, I. (I), Will, M. (M.), and Zaric, D. (D.)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, supernova remnants [ISM], Astrophysics::Instrumentation and Methods for Astrophysics, observational [methods], general [gamma rays]
Abstract

Aims: We measure the Crab Nebula γ-ray spectral energy distribution in the ~100 TeV energy domain and test the validity of existing leptonic emission models at these high energies. Methods: We used the novel very large zenith angle observations with the MAGIC telescope system to increase the collection area above 10 TeV. We also developed an auxiliary procedure of monitoring atmospheric transmission in order to assure proper calibration of the accumulated data. This employs recording optical images of the stellar field next to the source position, which provides a better than 10% accuracy for the transmission measurements. Results: We demonstrate that MAGIC very large zenith angle observations yield a collection area larger than a square kilometer. In only ~ 56 h of observations, we detect the γ-ray emission from the Crab Nebula up to 100 TeV, thus providing the highest energy measurement of this source to date with Imaging Atmospheric Cherenkov Telescopes. Comparing accumulated and archival MAGIC and Fermi/LAT data with some of the existing emission models, we find that none of them provides an accurate description of the 1 GeV to 100 TeV γ-ray signal.

Published
2020

21. A complete catalogue of dusty supernova remnants in the Galactic plane

Author

Phil Cigan, Haley Louise Gomez, K. A. Marsh, Mikako Matsuura, Alberto Noriega-Crespo, I. De Looze, Matthew Smith, Jeonghee Rho, M. J. Barlow, Andreas Papageorgiou, Loretta Dunne, and H. Chawner

Subjects
Astrophysics, Compact star, MOLECULAR CLOUD, 01 natural sciences, Pulsar, 0103 physical sciences, INFRARED SURVEY, ISM [submillimetre], TRIGGERED STAR-FORMATION, Ejecta, Large Magellanic Cloud, XMM-NEWTON OBSERVATIONS, RADIO-CONTINUUM, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, supernova remnants [ISM], Molecular cloud, MAGNETIC-FIELD, ISM [infrared], Astronomy and Astrophysics, Galactic plane, HOST GALAXIES, Stars, Supernova, Physics and Astronomy, 13. Climate action, Space and Planetary Science, X-RAY, MHZ MASER EMISSION, LARGE-MAGELLANIC-CLOUD
Abstract

We search for far-infrared (FIR) counterparts of known supernova remnants (SNRs) in the Galactic plane (360° in longitude and $b = \pm \, 1^{\circ }$) at 70–500 μm with Herschel. We detect dust signatures in 39 SNRs out of 190, made up of 13 core-collapse supernovae (CCSNe), including 4 Pulsar Wind Nebulae (PWNe), and 2 Type Ia SNe. A further 24 FIR detected SNRs have unknown types. We confirm the FIR detection of ejecta dust within G350.1−0.3, adding to the known sample of ∼ 10 SNRs containing ejecta dust. We discover dust features at the location of a radio core at the centre of G351.2+0.1, indicating FIR emission coincident with a possible Crab-like compact object, with dust temperature and mass of Td = 45.8 K and Md = 0.18 M⊙, similar to the PWN G54.1+0.3. We show that the detection rate is higher among young SNRs. We produce dust temperature maps of 11 SNRs and mass maps of those with distance estimates, finding dust at temperatures $15\, \lesssim \, T_d\, \lesssim \, 40$ K. If the dust is heated by shock interactions the shocked gas must be relatively cool and/or have a low density to explain the observed low grain temperatures.

Published
2020
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22. MAGIC very large zenith angle observations of the Crab Nebula up to 100 TeV

Author

David Paneque, A. Biland, T. Schweizer, D. Ninci, Elina Lindfors, J. Besenrieder, D. Guberman, Masahiro Teshima, Chiara Righi, Daniel Mazin, A. De Angelis, J. Becerra González, A. Berti, S. Ansoldi, N. Godinović, S. Fukami, B. Machado de Oliveira Fraga, L. Bellizzi, Giacomo Bonnoli, D. Dominis Prester, K. Mannheim, N. Torres-Albà, J. Palacio, J. van Scherpenberg, P. Da Vela, A. Babić, D. Elsaesser, M. Ribó, D. Morcuende, P. Peñil, F. Leone, I. Šnidarić, A. Rugliancich, Marina Manganaro, V. Moreno, Dario Hrupec, Antonio Stamerra, P. G. Prada Moroni, G. Ceribella, Massimo Persic, Stefano Covino, Konstancja Satalecka, V. Fallah Ramazani, L. Nogués, P. Majumdar, Jose Carlos Herrera, Michele Doro, M. A. Lopez, G. Maneva, Elisa Prandini, D. Miceli, D. Fidalgo, Julian Sitarek, M. Mariotti, S. Cikota, M. I. Martínez, Razmik Mirzoyan, L. Saha, A. Chilingaryan, W. Rhode, G. Vanzo, M. Strzys, J. M. Paredes, Kyoshi Nishijima, U. Barres de Almeida, U. Colin, David A. Green, D. Hadasch, E. Do Souto Espiñeira, Tomislav Terzić, Ciro Bigongiari, D. Dorner, L. A. Antonelli, Petar Temnikov, M. Mallamaci, M. Minev, W. Bhattacharyya, Christian Fruck, S. Lombardi, D. Zarić, Jordi Delgado, John Hoang, Elisa Bernardini, G. Busetto, Y. Suda, Jose Luis Contreras, Dorota Sobczyńska, C. Maggio, Juan Cortina, R. López-Coto, Saša Mićanović, T. Surić, D. Lelas, Fabrizio Tavecchio, Y. Chai, Seiya Nozaki, S. Gasparyan, A. Lamastra, Eduardo Colombo, Ll. Font, S. M. Colak, D. Strom, J. Kushida, V. Vagelli, M. V. Fonseca, Auni Somero, M. Peresano, Kevin Schmidt, A. Arbet Engels, F. Di Pierro, M. Palatiello, Vitaly Neustroev, Luca Tosti, Juan Abel Barrio, M. Takahashi, I. Puljak, Narek Sahakyan, Carlo Vigorito, Laura Maraschi, Francesco Dazzi, Riccardo Paoletti, Markus Gaug, M. Vazquez Acosta, Nicola Giglietto, Valerio D'Elia, M. Delfino, A. López-Oramas, P. Munar-Adrover, G. Ferrara, Susumu Inoue, Abelardo Moralejo, E. Moretti, D. Depaoli, C. Nigro, V. A. Acciari, M. Makariev, Dominik Baack, R. J. García López, Luca Foffano, Francesco Giordano, Kari Nilsson, J. Rico, H. Kubo, Daniel Kerszberg, M. Will, Ž. Bošnjak, L. Jouvin, S. Loporchio, Simona Paiano, K. Noda, Jose Miguel Miranda, Edgar Molina, T. Saito, L. Di Venere, M. Hütten, B. Banerjee, Shunsuke Sakurai, Vincenzo Vitale, Ievgen Vovk, A. Hahn, Y. Iwamura, Markus Garczarczyk, Kazuma Ishio, B. De Lotto, W. Bednarek, Francesco Longo, Oscar Blanch, A. Fattorini, Roberto Carosi, Tomohiro Inada, A. Donini, Federal Ministry of Education and Research (Germany), Istituto Nazionale di Fisica Nucleare, Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Department of Atomic Energy (India), Ministry of Education, Youth and Science (Bulgaria), Academy of Finland, Universidad de Barcelona, Croatian Science Foundation, University of Rijeka, Ministério da Ciência, Tecnologia e Inovação (Brasil), Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Baack, D., Babic, A., Banerjee, B., Barres De Almeida, U., Barrio, J. A., Becerra Gonzalez, J., Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bosnjak, Z., Busetto, G., Carosi, R., Ceribella, G., Chai, Y., Chilingaryan, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espineira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., Garcia Lopez, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Godinovic, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Hutten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kerszberg, D., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Lopez-Coto, R., Lopez-Oramas, A., Loporchio, S., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Mazin, D., Micanovic, S., Miceli, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Nozaki, S., Paiano, S., Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Penil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Rhode, W., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schmidt, K., Schweizer, T., Sitarek, J., Snidaric, I., Sobczynska, D., Somero, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Suric, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Tosti, L., Vagelli, V., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., and Zaric, D.

Subjects
Gamma rays: general, ISM: supernova remnants, Methods: observational, Astronomy, gamma rays general, methods observational, ISM supernova remnants, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, model [emission], generalI [Gamma rays], Astrophysics, 01 natural sciences, Raigs gamma, optical, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supernoves, supernova remnants [ISM], Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Supernovae, Gamma rays: generalI, high [energy], Spectral energy distribution, Física nuclear, Astrophysics::High Energy Astrophysical Phenomena, general [Gamma rays], FOS: Physical sciences, SM: supernova remnants, monitoring [atmosphere], emission [gamma ray], 0103 physical sciences, Calibration, observational [Methods], 14. Life underwater, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Zenith, Computer Science::Information Retrieval, Gamma rays, Astronomy and Astrophysics, calibration, supernova remnants [SM], MAGIC, Cherenkov counter, Crab Nebula, Space and Planetary Science, ddc:520, spectral, supernova remnant [ISM], Energy (signal processing), Fermi Gamma-ray Space Telescope
Abstract

Aims. We measure the Crab Nebula γ-ray spectral energy distribution in the ~100 TeV energy domain and test the validity of existing leptonic emission models at these high energies. Methods. We used the novel very large zenith angle observations with the MAGIC telescope system to increase the collection area above 10 TeV. We also developed an auxiliary procedure of monitoring atmospheric transmission in order to assure proper calibration of the accumulated data. This employs recording optical images of the stellar field next to the source position, which provides a better than 10% accuracy for the transmission measurements. Results. We demonstrate that MAGIC very large zenith angle observations yield a collection area larger than a square kilometer. In only ~ 56 h of observations, we detect the γ-ray emission from the Crab Nebula up to 100 TeV, thus providing the highest energy measurement of this source to date with Imaging Atmospheric Cherenkov Telescopes. Comparing accumulated and archival MAGIC and Fermi/LAT data with some of the existing emission models, we find that none of them provides an accurate description of the 1 GeV to 100 TeV γ-ray signal., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy, the Japanese JSPS and MEXT, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. This research has made use of the CTA instrument response functions provided by the CTA Consortium and Observatory, see http://www.cta-observatory.org/science/cta-performance/ (version prod3b-v1) for more details.

Published
2020

23. E0102-VR: Exploring the scientific potential of Virtual Reality for observational astrophysics

Author

Frédéric P. A. Vogt, Enrico Baracaglia, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), European Southern Observatory - ESO (GERMANY), and European Southern Observatory (Santiago, Chile)

Subjects
010308 nuclear & particles physics, Computer science, supernova remnants [ISM], Entertainment industry, Astronomy and Astrophysics, individual objects [ISM], 1E 0102.2-7219, neutron [Stars], Astrophysics, Virtual reality, 01 natural sciences, Field (computer science), Computer Science Applications, Visualization, Autre, Space and Planetary Science, 0103 physical sciences, Observational study, miscellaneous [Methods], 010303 astronomy & astrophysics
Abstract

Virtual Reality (VR) technology has been subject to a rapid democratization in recent years, driven in large by the entertainment industry, and epitomized by the emergence of consumer-grade, plug-and-play, room-scale VR devices. To explore the scientific potential of this technology for the field of observational astrophysics, we have created an experimental VR application: E0102-VR. The specific scientific goal of this application is to facilitate the characterization of the 3D structure of the oxygen-rich ejecta in the young supernova remnant 1E 0102.2-7219 in the Small Magellanic Cloud. Using E0102-VR, we measure the physical size of two large cavities in the system, including a (7.0 ± 0.5) pc-long funnel structure on the far-side of the remnant. The E0102-VR application, albeit experimental, demonstrates the benefits of using human depth perception for a rapid and accurate characterization of complex 3D structures. Given the implementation costs (time-wise) of a dedicated VR application like E0102-VR, we conclude that the future of VR for scientific purposes in astrophysics most likely resides in the development of a robust, generic application dedicated to the exploration and visualization of 3D observational datasets, akin to a “ds9-VR”.

Published
2020

24. Deciphering the nature of the pulsar wind nebula CTB 87 with XMM–Newton

Author

A. MacMaster, Roland Kothes, B. Olmi, Elena Amato, Niccolò Bucciantini, Samar Safi-Harb, Zaven Arzoumanian, Benson Guest, National Research Council of Canada, Canada Research Chairs, University of Manitoba, Istituto Nazionale di Astrofisica, and National Aeronautics and Space Administration (US)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, individual (CTB 87 CXOU J201609.2+371110) [ISM], 010504 meteorology & atmospheric sciences, supernova remnants [ISM], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: individual (CTB 87 CXOU J201609.2+371110), 01 natural sciences, Pulsar wind nebula, Scholarship, Space and Planetary Science, 0103 physical sciences, Natural science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, ISM: supernova remnants
Abstract

CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU~J201609.2+371110, was first resolved with \textit{Chandra} and is surrounded by a compact and a more extended X-ray nebula. Here we use a deep {\textit{XMM-Newton}} observation to examine the morphology and evolutionary stage of the PWN and to search for thermal emission expected from a supernova shell or reverse shock interaction with supernova ejecta. We do not find evidence of thermal X-ray emission from the SNR and place an upper limit on the electron density of 0.05~cm$^{-3}$ for a plasma temperature $kT\sim 0.8$ keV. The morphology and spectral properties are consistent with a $\sim$20~kyr-old relic PWN expanding into a stellar wind-blown bubble. We also present the first X-ray spectral index map from the PWN and show that we can reproduce its morphology by means of 2D axisymmetric relativistic hydrodynamical simulations., 9 pages, 10 figures. Accepted for publication in MNRAS

Published
2019

25. Cosmic-ray acceleration and escape from post-adiabatic Supernova remnants

Author

Taras Kuzyo, Iurii Sushch, Robert Brose, Oleh Petruk, Martin Pohl, and 24922986 - Sushch, Iurii

Subjects
Acceleration of particles, magnetic [turbulence], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, feedback, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, power spectrum, 01 natural sciences, time dependence [acceleration], 010305 fluids & plasmas, Luminosity, thermal [plasma], X-ray, Pion, emission [gamma ray], 0103 physical sciences, supernova, propagation, ISM [Gamma rays], spectrum [cosmic radiation], structure, decay [pi], 010303 astronomy & astrophysics, Cosmic rays, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, emission [radio wave], supernova remnants [ISM], scattering, diffusion, Gamma ray, Astronomy and Astrophysics, rotation [symmetry], Interstellar medium, Turbulence, Supernova, Space and Planetary Science, flow, hydrodynamics, ddc:520, acceleration [cosmic radiation], low [density], galaxy, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Supernova remnants are known to accelerate cosmic rays on account of their non-thermal emission of radio waves, X-rays, and gamma rays. Although there are many models for the acceleration of cosmic rays in Supernova remnants, the escape of cosmic rays from these sources is yet understudied. We use our time-dependent acceleration code RATPaC to study the acceleration of cosmic rays and their escape in post-adiabatic Supernova remnants and calculate the subsequent gamma-ray emission from inverse-Compton scattering and Pion decay. We performed spherically symmetric 1-D simulations in which we simultaneously solve the transport equations for CRs, magnetic turbulence, and the hydrodynamical flow of the thermal plasma in a volume large enough to keep all CRs in the simulation. The transport equations for cosmic-rays and magnetic turbulence are coupled via the cosmic-ray gradient and the spatial diffusion coefficient of the cosmic rays, while the cosmic-ray feedback onto the shock structure can be ignored. Our simulations span 100kyrs, thus covering the remnants evolution until the beginning of the post-adiabatic phase. At later stages of the evolution cosmic rays over a wide range of energy can reside outside of the remnant, creating spectra that are softer than predicted by standard DSA and feature breaks in the 10-100 GeV-range. The total spectrum of cosmic rays released into the interstellar medium has a spectral index of s~2.4 above roughly 10 GeV which is close to that required by Galactic propagation models. We further find the gamma-ray luminosity to peak around an age of 4,000 years for inverse-Compton-dominated high-energy emission. Remnants expanding in low-density media emit generally more inverse-Compton radiation matching the fact that the brightest known supernova remnants - RCW86, Vela Jr, HESSJ1731-347 and RXJ1713.7-3946 - are all expanding in low density environments., 12 pages, 13 figures, accepted by A&A

Published
2019

26. Study of supernova remnants with H.E.S.S. and analysis of prototype data of the FlashCam Cherenkov Camera

Author

Capasso, Massimo and Santangelo, Andrea (Prof. Dott.)

Subjects
Morphology, Astroteilchen Physik, Very high energy gamma rays, Astrophysics::High Energy Astrophysical Phenomena, supernova remnants [ISM], VHE Gammastrahlen, Astrophysics::Cosmology and Extragalactic Astrophysics, Supernovaüberrest, Astroparticle Physics, Supernovaüberreste [ISM], Kosmischen Strahlung, Cosmic rays, Morphologie, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, ISM: Supernovaüberreste
Abstract

This thesis will present the results of two data analysis projects conducted in the framework of the H.E.S.S. (High Energy Stereoscopic System) Collaboration. H.E.S.S. is a system of five Cherenkov telescopes located in Namibia, which detect VHE (Very High Energy) γ-rays from Galactic and Extragalactic sources. Both of the presented projects focus on Galactic supernova remnants (SNRs), which are among the astrophysical objects known to emit VHE γ -rays. Supernova remnants are the remains of a star exploding into a so-called supernova. More precisely, due to the explosion, the outer layers of the pre-supernova star are ejected at high velocity and particles are accelerated by the shock wave up to very high energies, hundreds of times higher than those reached at the Large Hadron Collider (LHC), currently the most powerful particle accelerator on Earth. One of the key reasons why SNRs are of particular interest in the astrophysics community is that they are believed to be responsible for the production and acceleration of the bulk of Galactic Cosmic Rays (CRs) (hydrogen and helium nuclei and heavier particles). In this context, VHE γ-rays produced by the interaction of the supernova ejecta with the ambient medium provide a clean tracer to probe this hypothesis, though a definite answer on the topic is yet to be found. Given these premises, this work is structured as follows: Chapter 1 will provide an introduction on VHE γ-ray astronomy. The driving idea is to try and follow a sequence of questions. How does the sky actually look in VHE γ-rays? How are the latter produced? Where do they come from, i.e., which are the astrophysical sources that produce them? How can we detect them? Chapter 2 focuses on the search for new supernova remnants in our Galaxy with the H.E.S.S. experiment. In the energy range covered with H.E.S.S., the only way to identify new supernova remnant candidates is by their shell-like appearance. The idea of this work was then to scan the H.E.S.S. dataset looking for shell-like structures and see if they could be confirmed as supernova remnants. This morphological search criterion is not new in the astrophysics community; however, it was the first time, to our knowledge, in which it was successfully applied to VHE γ-ray data. The search led to the identification of three new significant shell structures; one of them could be confirmed as supernova remnant. Chapter 3 presents a second analysis project involving the study of a supernova remnant and of its surroundings. As mentioned above, VHE γ-rays can be produced in the interaction between CRs accelerated at a supernova remnant shock-front and the ambient medium (consisting of both atomic and molecular gas). Therefore, if the VHE γ-ray emission from a supernova remnant or from its neighborhood is found to be coincident with known dense gas regions, this shows that such a process is likely taking place. Having this in mind, a correlation study between the VHE γ-ray and gas emission from the supernova remnant HESS J1731−347 region was carried out. The physical implications of the outcome of this study are then discussed. Finally, a glance at the future. The Astronomy and Astrophysics Institute of the University of Tübingen is currently contributing to the development of the next-generation ground-based VHE γ-ray telescopes, the Cherenkov Telescope Array (CTA). One of the projects concerns the realization of the focal plane instrument for one of the telescope types foreseen by CTA. In this context, an analysis of prototype data was performed. This thesis concludes with an overview of the main results obtained so far (Chapter 4)., In dieser Dissertation werden die Ergebnisse von zwei Datenanalyse-Projekten vorgestellt, die im Rahmen der H.E.S.S. (High Energy Stereoscopic System) Kollaboration durchgeführt wurden. H.E.S.S. ist ein System aus fünf Cherenkov-Teleskopen in Namibia, die VHE (Very High Energy) Gammastrahlung aus galaktischen und extragalaktischen Quellen detektieren. Beide vorgestellten Projekte konzentrieren sich auf galaktische Supernovaüberreste (Supernova remnants, SNRs), astrophysikalische Objekte, von denen bekannt ist, dass sie VHE Gammastrahlung ausstrahlen. Supernovaüberreste sind die Überbleibsel eines Sterns, der als Supernova explodiert ist. Durch die Explosion wurden die äußeren Schichten des Prä-Supernova-Sterns mit hoher Geschwindigkeit ausgestoßen, und durch die Shockwelle wurden Teilchen auf sehr hohe Energien beschleunigt; die erreichten Energien sind hundertfach höher als beim Large Hadron Collider (LHC), dem stärksten von Menschen gebauten Teilchenbeschleuniger der Erde. SNRs sind besonders interessant, weil sie wahrscheinlich für die Produktion und Beschleunigung der Kosmischen Strahlung (Wasserstoff- und Heliumkerne sowie schwerere Teilchen) verantwortlich sind. In diesem Zusammenhang bietet VHE-Gammastrahlung, durch die Wechselwirkung der ausgestoßenen Materie mit dem Umgebungsmedium erzeugt wird, eine Möglichkeit, um diese Hypothese zu untersuchen, wobei eine eindeutige Antwort auf das Thema noch nicht gefunden werden konnte. Die vorliegende Arbeit ist wie folgt strukturiert: Kapitel 1 enthält eine Einführung in die VHE Gammastrahlen-Astronomie. Diese orientiert sich dabei an den folgenden Fragen: Wie sieht der Himmel im Bereich der VHE-Gammastrahlung aus? Wie wird diese produziert? Woher kommt sie, d.h. aus welchen astrophysikalischen Quellen stammt sie? Wie können wir sie detektieren? Kapitel 2 beschäftigt sich mit der Suche nach neuen Supernovaüberresten in unserer Galaxie mit dem H.E.S.S. Experiment. Im Energiebereich, der mit H.E.S.S. abgedeckt wird, ist der einzige Weg um neue Supernovaüberrestkandidaten zu identifizieren, ihr ringförmiges Aussehen. Die Idee dieser Arbeit ist deswegen, den H.E.S.S. Datensatz zu untersuchen, um ringförmige Strukturen zu finden, und sehen, ob sie als Supernovaüberreste klassifiziert werden könnten. Dieses morphologische Suchkriterium ist in der astrophysikalischen Gemeinschaft nicht neu; es war jedoch unseres Wissens das erste Mal, dass es erfolgreich auf VHE-Gammastrahlung-Daten angewendet wurde. Die Suche führte zur Identifizierung von drei neuen signifikanten Strukturen; eine konnte als Supernovaüberrest bestätigt werden. In Kapitel 3 wird ein zweites Datenanalyse-Projekt vorgestellt, bei dem ein Supernovaüberrest und seine Umgebung untersucht werden. Wie oben erwähnt, könnte VHE-Gammastrahlung in der Wechselwirkung zwischen CRs, die an der Shockwelle eines Supernovaüberrests beschleunigt werden, und dem Umgebungsmedium (bestehend aus atomarem und molekularem Gas) erzeugt werden. Wenn sich herausstellt, dass die VHE-Gammastrahlung eines Supernovaüberrests oder seiner Umgebung mit bekannten Regionen mit dichtem Gas zusammenfällt, zeigt dies, dass wahrscheinlich ein solcher Prozess stattfindet. Vor diesem Hintergrund wurde eine Korrelationsstudie zwischen der VHE-Gammastrahlung und der Gasemission aus dem Supernovaüberrest HESS J1731-347 durchgeführt. Anschließend werden die Implikationen des Ergebnisses dieser Studie diskutiert. Zum Schluss noch ein Blick in die Zukunft. Das Institut für Astronomie und Astrophysik der Universität Tübingen leistet derzeit einen Beitrag zur Entwicklung der bodengestützten Gammateleskope der nächsten Generation, des Cherenkov Telescope Array (CTA). Eines der Projekte betrifft die Realisierung des Fokalinstruments für einen der von CTA vorgese- henen Teleskoptypen. In diesem Zusammenhang wurde eine Analyse von Prototypdaten durchgeführt. Diese Arbeit schließt mit einem Überblick über die wichtigsten bisher erzielten Ergebnisse (Kapitel 4).

Published
2019

27. Discovery of a Pulsar-powered Bow Shock Nebula in the Small Magellanic Cloud Supernova Remnant DEMS5

Author

Roland Kothes, Thomas G. Pannuti, Kieran J. Luken, V. Velović, Andrew O'Brien, P. Maggi, Ray P. Norris, R. Z. E. Alsaberi, Nicholas F. H Tothill, Sebastián Gurovich, N. Maxted, Hidetoshi Sano, T. J. Galvin, Luke M Bozzetto, Dejan Urošević, Patrick J. Kavanagh, Natasha Hurley-Walker, B. Q. For, Miroslav Filipovic, H. Dénes, Evan J Crawford, Graeme F Wong, Yasuo Fukui, Thomas H. Jarrett, Manami Sasaki, D. Onić, Ivan S. Bojičić, Miranda Yew, Shi Dai, Lister Staveley-Smith, Naomi McClure-Griffiths, Gavin Rowell, P. Manjolović, Frank Haberl, Chandreyee Maitra, 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
Astrophysics::High Energy Astrophysical Phenomena, GENERAL [RADIATION MECHANISMS], FOS: Physical sciences, purl.org/becyt/ford/1.7 [https], radiation mechanisms: general, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, purl.org/becyt/ford/1 [https], ISM: individual objects: DEM S5, Pulsar, MAGELLANIC CLOUDS, 0103 physical sciences, Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, SUPERNOVA REMNANTS [ISM], Bow shock (aerodynamics), Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Nebula, ISM. [RADIO CONTINUUM], 010308 nuclear & particles physics, Astronomy and Astrophysics, radio continuum: ISM, 13. Climate action, Space and Planetary Science, INDIVIDUAL OBJECTS: DEMS5 [ISM], Small Magellanic Cloud, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report the discovery of a new Small Magellanic Cloud Pulsar Wind Nebula (PWN) at the edge of the Supernova Remnant (SNR)-DEM S5. The pulsar powered object has a cometary morphology similar to the Galactic PWN analogs PSR B1951+32 and 'the mouse'. It is travelling supersonically through the interstellar medium. We estimate the Pulsar kick velocity to be in the range of 700-2000 km/s for an age between 28-10 kyr. The radio spectral index for this SNR PWN pulsar system is flat (-0.29 $\pm$ 0.01) consistent with other similar objects. We infer that the putative pulsar has a radio spectral index of -1.8, which is typical for Galactic pulsars. We searched for dispersion measures (DMs) up to 1000 cm/pc^3 but found no convincing candidates with a S/N greater than 8. We produce a polarisation map for this PWN at 5500 MHz and find a mean fractional polarisation of P $\sim 23$ percent. The X-ray power-law spectrum (Gamma $\sim 2$) is indicative of non-thermal synchrotron emission as is expected from PWN-pulsar system. Finally, we detect DEM S5 in Infrared (IR) bands. Our IR photometric measurements strongly indicate the presence of shocked gas which is expected for SNRs. However, it is unusual to detect such IR emission in a SNR with a supersonic bow-shock PWN. We also find a low-velocity HI cloud of $\sim 107$ km/s which is possibly interacting with DEM S5. SNR DEM S5 is the first confirmed detection of a pulsar-powered bow shock nebula found outside the Galaxy., 20 pages, 15 figures, accepted for publication in MNRAS

Published
2019

28. Radio Emission from Interstellar Shocks: Young Type Ia Supernova Remnants and the Case of N 103B in the Large Magellanic Cloud

Author

T. J. Galvin, Nicholas O Ralph, Nicholas F. H Tothill, Sebastián Gurovich, R. Z. E. Alsaberi, Hidetoshi Sano, P. Maggi, Miroslav Filipovic, Frank Haberl, Graeme F Wong, Manami Sasaki, Luke A. Barnes, Yasuo Fukui, P. Manojlovic, Gavin Rowell, Luke M Bozzetto, Dejan Urošević, Evan J Crawford, N. Maxted, D. Onić, Patrick J. Kavanagh, B. Q. For, 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
Astrophysics::High Energy Astrophysical Phenomena, purl.org/becyt/ford/1.7 [https], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, GENERAL [SUPERNOVAE], law.invention, purl.org/becyt/ford/1 [https], Telescope, law, 0103 physical sciences, SUPERNOVA REMNANTS [ISM], Large Magellanic Cloud, 010303 astronomy & astrophysics, Equipartition theorem, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, Astronomy and Astrophysics, Galaxy, Interstellar medium, Supernova, Space and Planetary Science, [SDU]Sciences of the Universe [physics], INDIVIDUAL OBJECTS: N 103B [ISM], ISM [RADIO CONTINUUM], Astrophysics - High Energy Astrophysical Phenomena
Abstract

We investigate young type Ia supernova remnants (SNRs) in our Galaxy and neighbouring galaxies in order to understand their properties and early stage of their evolution. Here we present a radio continuum study based on new and archival data from the Australia Telescope Compact Array (ATCA) towards N 103B, a young (≤1000 yrs) spectroscopically confirmed type Ia SNR in the Large Magellanic Cloud (LMC) and proposed to have originated from a single degenerate (SD) progenitor. The radio morphology of this SNR is asymmetrical with two bright regions towards the north-west and south-west of the central location as defined by radio emission. N 103B identified features include: a radio spectral index of − 0.75 ± 0.01 (consistent with other young type Ia SNRs in the Galaxy); a bulk SNR expansion rate as in X-rays; morphology and polarised electrical field vector measurements where we note radial polarisation peak towards the north-west of the remnant at both 5500 and 9000 MHz. The spectrum is concave-up and the most likely reason is the non-linear diffusive shock acceleration (NLDSA) effects or presence of two different populations of ultra-relativistic electrons. We also note unpolarised clumps near the south-west region which is in agreement with this above scenario. We derive a typical magnetic field strength for N 103B of 16.4 μG for an average rotation measurement of 200radm−2. However, we estimate the equipartition field to be of the order of ∼235 μG with an estimated minimum energy of Emin=6.3×1048erg. The close (∼ 0.5 ∘) proximity of N 103B to the LMC mid-plane indicates that an early encounter with dense interstellar medium may have set an important constrain on SNR evolution. Finally, we compare features of N 103B to six other young type Ia SNRs in the LMC and Galaxy, with a range of proposed degeneracy scenarios to highlight potential differences due to a different models. We suggest that the single degenerate scenario might point to morphologically asymmetric type Ia supernova explosions. Fil: Alsaberi, Rami Z. E.. University of Western Sydney; Australia Fil: Barnes, L. A.. University of Western Sydney; Australia Fil: Filipovic, Miroslav. University of Western Sydney; Australia Fil: Maxted, Nigel. University of Western Sydney; Australia. University of New South Wales; Australia Fil: Sano, H.. Nagoya University; Japón Fil: Rowell, Gavin. University of Adelaide; Australia Fil: Bozzetto, L. M.. University of Western Sydney; Australia Fil: Gurovich, Sebastian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina Fil: Urošević, D.. Univerzitet U Beogradu; Serbia Fil: Onić, D.. Univerzitet U Beogradu; Serbia Fil: For, B. Q.. University of Western Australia; Australia. ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions; Australia Fil: Manojlović, P.. University of Western Sydney; Australia. CSIRO Astronomy and Space Sciences; Australia Fil: Wong, G.. University of Western Sydney; Australia. CSIRO Astronomy and Space Sciences; Australia Fil: Galvin, T. J.. Curtin University. International Centre for Radio Astronomy Research; Australia. University of Western Sydney; Australia. CSIRO Astronomy and Space Sciences; Australia Fil: Kavanagh, P.. Dublin Institute for Advanced Studies; Irlanda Fil: Ralph, N. O.. University of Western Sydney; Australia Fil: Crawford, Evan. University of Western Sydney; Australia Fil: Sasaki, Manami. Universitat Erlangen-Nuremberg; Alemania Fil: Haberl, Frank. Institut Max Planck Fuer Gesellschaft. Max Planck Institute For Extraterrestrial Physics; Alemania Fil: Maggi, P.. Université de Strasbourg; Francia. Centre National de la Recherche Scientifique; Francia Fil: Tothill, N. F. H.. University of Western Sydney; Australia Fil: Fukui, Y.. University of Adelaide; Australia

Published
2019
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29. The dust content of the Crab Nebula

Author

I. De Looze, F. D. Priestley, A. Bevan, M. J. Barlow, Mikako Matsuura, Haley Louise Gomez, Michael Bietenholz, Rino Bandiera, H. Chawner, Roger Wesson, ITA, GBR, BEL, CAN, and ZAF

Subjects
Astrophysics::High Energy Astrophysical Phenomena, MAGNETOHYDRODYNAMIC SIMULATIONS, Extinction (astronomy), individual: Crab Nebula [supernovae], Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar, INTERSTELLAR SILICATE MINERALOGY, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, SPACE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cosmic dust, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, 010308 nuclear & particles physics, supernova remnants [ISM], Astronomy and Astrophysics, non-thermal [radiation mechanisms], Astrophysics - Astrophysics of Galaxies, Galaxy, EVOLUTION, Supernova, SPITZER, CASSIOPEIA, Crab Nebula, Physics and Astronomy, Space and Planetary Science, SUPERNOVA REMNANT, Astrophysics of Galaxies (astro-ph.GA), MULTIBAND IMAGING PHOTOMETER, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, PULSAR-WIND NEBULAE, ABSOLUTE CALIBRATION
Abstract

We have modelled the near-infrared to radio images of the Crab Nebula with a Bayesian SED model to simultaneously fit its synchrotron, interstellar and supernova dust emission. We infer an interstellar dust extinction map with an average $A_{\text{V}}$=1.08$\pm$0.38 mag, consistent with a small contribution (, Comment: 33 pages, 17 figures, Manuscript accepted for publication in MNRAS. Accepted on 31/05/2019. Deposited on 31/05/2019

Published
2019

30. Dust masses and grain size distributions of a sample of Galactic pulsar wind nebulae

Author

I. De Looze, F. D. Priestley, H. Chawner, and M. J. Barlow

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, individual objects: Crab Nebula [ISM], 01 natural sciences, Power law, Luminosity, Pulsar, EARLY UNIVERSE, INTERSTELLAR SILICATE MINERALOGY, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, STAR, 010308 nuclear & particles physics, extinction, supernova remnants [ISM], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, EVOLUTION, CRAB-NEBULA, Stars, CASSIOPEIA, EJECTA, Crab Nebula, Physics and Astronomy, Space and Planetary Science, SUPERNOVA REMNANT, DISCOVERY, Astrophysics of Galaxies (astro-ph.GA), dust, Astrophysics::Earth and Planetary Astrophysics, EMISSION
Abstract

We calculate dust spectral energy distributions (SEDs) for a range of grain sizes and compositions, using physical properties appropriate for five pulsar wind nebulae (PWNe) from which dust emission associated with the ejecta has been detected. By fitting the observed dust SED with our models, with the number of grains of different sizes as the free parameters, we are able to determine the grain size distribution and total dust mass in each PWN. We find that all five PWNe require large ($\ge 0.1 \, {\rm \mu m}$) grains to make up the majority of the dust mass, with strong evidence for the presence of micron-sized or larger grains. Only two PWNe contain non-negligible quantities of small ($, Comment: 13 pages, 10 figures. MNRAS accepted 04/12/19

Published
2019
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31. 2FHL J0826.1–4500: Discovery of a Possible Shock–Cloud Interaction on the Western Edge of the Vela Supernova Remnant

Author

Daniel Castro, Marco Ajello, Jordan Eagle, Stefano Marchesi, Laura Duvidovich, Luigi Tibaldo, 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), Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)

Subjects
Shock wave, 010504 meteorology & atmospheric sciences, Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, Astrophysics, 7. Clean energy, 01 natural sciences, Spectral line, law.invention, Telescope, cosmic rays, law, 0103 physical sciences, SUPERNOVA REMNANTS [ISM], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, ISM: supernova remnants, Physics, Vela Supernova Remnant, Astronomy and Astrophysics, COSMIC RAYS, shock waves, Particle acceleration, Astronomía, radiation mechanisms: thermal, Space and Planetary Science, Spectral energy distribution, SHOCK WAVES, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], THERMAL [RADIATION MECHANISMS], CIENCIAS NATURALES Y EXACTAS, Fermi Gamma-ray Space Telescope
Abstract

We report on the investigation of a very high-energy, Galactic γ-ray source recently discovered at >50 GeV using the Large Area Telescope on board Fermi. This object, 2FHL J0826.1-4500, displays one of the hardest >50 GeV spectra (photon index Γγ ∼ 1.6) in the 2FHL catalog, and a follow-up observation with XMM-Newton has uncovered diffuse, soft thermal emission at the position of the γ-ray source. A detailed analysis of the available multi-wavelength data shows that this source is located on the western edge of the Vela supernova remnant (SNR): the observations and the modeling of the spectral energy distribution support a scenario where this γ-ray source is the byproduct of the interaction between the SNR shock and a neutral hydrogen cloud. If confirmed, this shock-cloud interaction would make 2FHL J0826.1-4500 a promising candidate for efficient particle acceleration. Fil: Eagle, J.. Clemson University; Estados Unidos Fil: Marchesini Serres, Magdalena. Clemson University; Estados Unidos Fil: Castro, D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Ajello, M.. Clemson University; Estados Unidos Fil: Duvidovich, Laura Patricia. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Tibaldo, L.. Observatoire Midi Pyrnes; Francia

Published
2019

32. The mass, location and heating of the dust in the Cassiopeia : a supernova remnant

Author

I. De Looze, F. D. Priestley, and M. J. Barlow

Subjects
GRAINS, Infrared, Astrophysics::High Energy Astrophysical Phenomena, INFRARED-EMISSION, Extinction (astronomy), individual: Cassiopeia A [supernovae], FOS: Physical sciences, Synchrotron radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, INTERSTELLAR SILICATE MINERALOGY, 0103 physical sciences, Thermal, Astrophysics::Solar and Stellar Astrophysics, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 3-DIMENSIONAL STRUCTURE, Physics, EXPLOSION, 010308 nuclear & particles physics, extinction, supernova remnants [ISM], TEMPERATURE-FLUCTUATIONS, X-RAY KNOTS, CONSTRAINTS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Cassiopeia A, Physics and Astronomy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Particle, Astrophysics::Earth and Planetary Astrophysics, dust, A SUPERNOVA
Abstract

We model the thermal dust emission from dust grains heated by synchrotron radiation and by particle collisions, under conditions appropriate for four different shocked and unshocked gas components of the Cassiopeia A (Cas A) supernova remnant (SNR). By fitting the resulting spectral energy distributions (SEDs) to the observed SNR dust fluxes, we determine the required mass of dust in each component. We find the observed SED can be reproduced by $\sim 0.6 \, {\rm M_\odot}$ of silicate grains, the majority of which is in the unshocked ejecta and heated by the synchrotron radiation field. Warmer dust, located in the X-ray emitting reverse shock and blastwave regions, contribute to the shorter wavelength infrared emission but make only a small fraction of the total dust mass. Carbon grains can at most make up $\sim 25 \%$ of the total dust mass. Combined with estimates for the gas masses, we obtain dust-to-gas mass ratios for each component, which suggest that the condensation efficiency in the ejecta is high, and that dust in the shocked ejecta clumps is well protected from destruction by sputtering in the reverse shock., Accepted by MNRAS, 14 pages, 6 figures. Author accepted manuscript. Accepted on 05/02/2019. Deposited on 05/02/2019

Published
2019

33. The optical and NIR spectrum of the Crab pulsar with X-shooter

Author

Jonatan Selsing, P. M. Vreeswijk, Peter Lundqvist, Jesper Sollerman, and Anders Nyholm

Subjects
Physics, Nebula, Spectral index, Very Large Telescope, Absorption spectroscopy, Crab Pulsar, supernova remnants [ISM], Astronomy, Astronomy and Astrophysics, Astrophysics, general [pulsars], 01 natural sciences, neutron [stars], Pulsar, Space and Planetary Science, 0103 physical sciences, individual: Crab pulsar [pulsars], lines and bands [ISM], Emission spectrum, 010306 general physics, 010303 astronomy & astrophysics, Spectrograph
Abstract

Context. Pulsars are well studied all over the electromagnetic spectrum, and the Crab pulsar may be the most studied object in the sky. Nevertheless, a high-quality optical to near-infrared (NIR) spectrum of the Crab or any other pulsar has not been published to date. Aims. Obtaining a properly flux-calibrated spectrum enables us to measure the spectral index of the pulsar emission, without many of the caveats from previous studies. This was the main aim of this project, but in addition we could also detect absorption and emission features from the pulsar and nebula over an unprecedentedly wide wavelength range. Methods. A spectrum was obtained with the X-shooter spectrograph on the Very Large Telescope. Special care was given to the flux-calibration of these data. Results. A high signal-to-noise spectrum of the Crab pulsar was obtained from 300 nm to 2400 nm. The spectral index fit to this spectrum is flat with αν = 0.16 ± 0.07. For the emission lines we measured a maximum velocity of ∼1600 km s−1, whereas the absorption lines from the material between us and the pulsar is unresolved at the ∼50 km s−1 resolution. A number of diffuse interstellar bands and a few NIR emission lines that have previously not been reported from the Crab are highlighted.

Published
2019

34. Discovery of TeV γ-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC

Author

R. J. García López, P G Prada Moroni, C. Arcaro, M. Vazquez Acosta, Masahiro Teshima, Elina Lindfors, Nikola Godinovic, Victoria Moreno, Daniel Mazin, Saverio Lombardi, A. Fernández-Barral, Chiara Righi, Pratik Majumdar, M. V. Fonseca, L. Nogués, Cosimo Nigro, M. Nievas Rosillo, Lluis Font, D. Dorner, A. Lamastra, M. Minev, R. Zanin, P. Temnikov, D. Elsaesser, J. Palacio, J. M. Paredes, Antonio Stamerra, Marcel Strzys, V. D'Elia, Martin Will, Stefano Covino, D. Zarić, Adrian Biland, D.F. Torres, Dario Hrupec, R. Paoletti, Wrijupan Bhattacharyya, B. Banerjee, A. Fattorini, Marc Ribó, S. Ansoldi, P. Giammaria, M. A. Lopez, Karl Mannheim, P. Bangale, Junko Kushida, J. Delgado, J. Rico, Kyoshi Nishijima, Tomoki Saito, Giovanni Ceribella, Satoshi Masuda, John Hoang, U. Barres de Almeida, Arka Chatterjee, Tarek M. Hassan, Hidetoshi Kubo, S. Paiano, Aaron Dominguez, F. Di Pierro, D. Kuveždić, Jürgen Besenrieder, Alexander Hahn, D. Hadasch, A. Rugliancich, Marina Manganaro, Fabrizio Tavecchio, M. I. Martínez, D. Fidalgo, Juan Abel Barrio, J. Becerra González, J. E. Ward, Damir Lelas, Francesco Longo, I. Snidaric, Sidika Merve Colak, G. Ferrara, E. Colombo, Sabrina Einecke, M. Delfino, Lab Saha, D. Dominis Prester, Alessio Berti, Ievgen Vovk, Louis Antonelli, A. Arbet Engels, S. Gallozzi, Gaia Vanzo, P. Cumani, Konstancja Satalecka, A. De Angelis, D. Ninci, Michele Doro, Dorota Sobczyńska, Martin Makariev, Ana Babić, Oscar Blanch, R. Mirzoyan, Vitaly Neustroev, W. Bednarek, T. Schweizer, Jose Luis Contreras, Christian Fruck, Julian Sitarek, Juan Cortina, J. Herrera, V. Fallah Ramazani, G. Bonnoli, David Paneque, M. Mariotti, Koji Noda, A. López-Oramas, Ivica Puljak, D. Guberman, Elisa Bernardini, G. Pedaletti, G. Maneva, D. Baack, M. Persic, P. Colin, V. A. Acciari, P. Da Vela, L. Foffano, L. Maraschi, Tomislav Terzić, Kari Nilsson, Yuki Iwamura, Susumu Inoue, J. R. Garcia, Camilla Maggio, Kazuma Ishio, E. de Oña Wilhelmi, A. Niedzwiecki, Elisa Prandini, Rodolfo Carosi, M. Peresano, N. Torres-Albà, Jose Miguel Miranda, D. Galindo, Francesco Leone, T. Surić, Shimpei Tsujimoto, Abelardo Moralejo, E. Moretti, Edgar Molina, B. De Lotto, Markus Gaug, Ciro Bigongiari, M. Garczarczyk, W. Rhode, Francesco Dazzi, A. Somero, Pablo Peñil, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., De Almeida, U Barre, Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., De Oña Wilhelmi, E., Torres, D. F., and Zanin, R.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, cloud [ISM], ISM:supernova remnants, acceleration of particles, ISM: clouds, cosmic rays, ISM: supernova remnants, gamma-rays: general, astro-ph.HE, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy and Astrophysics, Space and Planetary Science, 01 natural sciences, Spectral line, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, acceleration of particle, cosmic ray, Cherenkov radiation, Physics, Spectral index, 010308 nuclear & particles physics, supernova remnants [ISM], Spectral density, Astronomy and Astrophysic, acceleration of particles, cosmic rays, ISM:supernova remnants, ISM: clouds, gamma-rays: general, Acceleration of particles, cosmic rays, gamma-rays: general, ISM: clouds, ISM: supernova remnants, Supernova, 13. Climate action, ddc:520, supernova remnant [ISM], Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, clouds [ISM], general [gamma-rays], Radio wave
Abstract

SNR G24.7+0.6 is a 9.5 kyrs radio and $\gamma$-ray supernova remnant evolving in a dense medium. In the GeV regime, SNR G24.7+0.6 (3FHL\,J1834.1--0706e/FGES\,J1834.1--0706) shows a hard spectral index ($\Gamma$$\sim$2) up to $200$\,GeV, which makes it a good candidate to be observed with Cherenkov telescopes such as MAGIC. We observed the field of view of \snr\ with the MAGIC telescopes for a total of 31 hours. We detect very high energy $\gamma$-ray emission from an extended source located 0.34\degr\ away from the center of the radio SNR. The new source, named \mgc\ is detected up to 5\,TeV, and its spectrum is well-represented by a power-law function with spectral index of $2.74 \pm 0.08$. The complexity of the region makes the identification of the origin of the very-high energy emission difficult, however the spectral agreement with the LAT source and overlapping position at less than 1.5$\sigma$ point to a common origin. We analysed 8 years of \fermi-LAT data to extend the spectrum of the source down to 60\,MeV. \fermi-LAT and MAGIC spectra overlap within errors and the global broad band spectrum is described by a power-law with exponential cutoff at $1.9\pm0.5$\,TeV. The detected $\gamma$-ray emission can be interpreted as the results of proton-proton interaction between the supernova and the CO-rich surrounding., Comment: accepted for publication by MNRAS

Published
2019

35. 3D MHD modeling of the expanding remnant of SN 1987A : role of magnetic field and non-thermal radio emission

Author

Marco Miceli, Shigehiro Nagataki, Petar Mimica, Fabrizio Bocchino, Shiu-Hang Lee, Miguel-Ángel Aloy, Giovanni Peres, Massimiliano Guarrasi, Masaomi Ono, Salvatore Orlando, Oleh Petruk, ITA, ESP, JPN, POL, UKR, Orlando, S., Miceli, M., Petruk, O., Ono, M., Nagataki, S., Aloy, M.A., Mimica, P., Lee, S.-H., Bocchino, F., Peres, G., and Guarrasi, M.

Subjects
Shock wave, H II region, Magnetohydrodynamics (MHD), shock wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Field strength, ISM [radio continuum], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, magnetohydrodynamics (MHD), Radio spectrum, individual: SN 1987A [supernovae], 0103 physical sciences, ISM [X-rays], 010303 astronomy & astrophysics, Blast wave, ISM: supernova remnant, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nebula, supernovae: individual: SN 1987A, 010308 nuclear & particles physics, supernova remnants [ISM], Astronomy and Astrophysics, shock waves, X-rays: ISM, Magnetic field, radio continuum: ISM, Space and Planetary Science, Magnetohydrodynamics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Aims. We investigate the role played by a pre-supernova (SN) ambient magnetic field on the dynamics of the expanding remnant of SN 1987A and the origin and evolution of the radio emission from the remnant, in particular, during the interaction of the blast wave with the nebula surrounding the SN. Methods. We model the evolution of SN 1987A from the breakout of the shock wave at the stellar surface to the expansion of its remnant through the surrounding nebula by 3D MHD simulations. The model considers the radiative cooling, the deviations from equilibrium of ionization, the deviation from temperature-equilibration between electrons and ions, and a plausible configuration of the pre-SN ambient magnetic field. From the simulations, we synthesize both thermal X-ray and non-thermal radio emission and compare the model results with observations. Results. The presence of an ambient magnetic field reduces the erosion and fragmentation of the dense equatorial ring after the impact of the SN blast wave. As a result, the ring survives the passage of the blast, at least, during the time covered by the simulations (40 years). Our model is able to reproduce the morphology and lightcurves of SN 1987A in both X-ray and radio bands. The model reproduces the observed radio emission if the flux originating from the reverse shock is heavily suppressed. In this case, the radio emission originates mostly from the forward shock traveling through the H II region. Possible mechanisms for the suppression of emission from the reverse shock are investigated. We find that synchrotron self-absorption and free-free absorption have negligible effects on the emission during the interaction with the nebula. We suggest that the emission from the reverse shock at radio frequencies might be limited by highly magnetized ejecta., 15 pages, 9 Figures, accepted for publication on A&A, high quality figures will be available on the published paper

Published
2019

36. X-ray emitting structures in the Vela SNR: ejecta anisotropies and progenitor stellar wind residuals

Author

Manami Sasaki, Vincenzo Sapienza, Fabrizio Bocchino, E. Greco, Federico García, Jorge Ariel Combi, Giovanni Peres, Marco Miceli, Salvatore Orlando, ITA, DEU, ARG, NLD, Astronomy, Sapienza V., Miceli M., Peres G., Bocchino F., Orlando S., Greco E., Combi J.A., Garcia F., and Sasaki M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics, ISM [X-RAYS], Photon energy, Vela, 01 natural sciences, purl.org/becyt/ford/1 [https], Protein filament, Settore FIS/05 - Astronomia E Astrofisica, 0103 physical sciences, ROSAT, Astrophysics::Solar and Stellar Astrophysics, SUPERNOVA REMNANTS [ISM], Ejecta, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Vela Supernova Remnant, 010308 nuclear & particles physics, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], X-rays: ISM, Supernova, ISM: individual objects: Vela SNR, Space and Planetary Science, INDIVIDUAL OBJECTS: VELA SNR [ISM], Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Vela supernova remnant (SNR) shows several ejecta fragments protruding beyond the forward shock (shrapnel). Recent studies have revealed high Si abundance in two shrapnel (A and G), located in opposite directions with respect to the SNR center. This suggests the possible existence of a Si-rich jet-counterjet structure. We analyzed an XMM-Newton observation of a bright clump, behind shrapnel G, which lies along the direction connecting A and G. The aim is to study the physical and chemical properties of this clump to ascertain whether it is part of this putative jet-like structure. We produced background-corrected and adaptively-smoothed count-rate images and median photon energy maps, and performed a spatially resolved spectral analysis. We identified two structures with different physical properties. The first one is remarkably elongated along the direction connecting A and G. Its X-ray spectrum is much softer than that of the other two shrapnel, to the point of hindering the determination of the Si abundance, however its physical and chemical properties are consistent with those of shrapnel A and G. The second structure, running along the southeast-northwest direction, has a higher temperature and appears like a thin filament. By analyzing the ROSAT data, we have found that this filament is part of a very large and coherent structure that we identified in the western rim of the shell. We obtained a thorough description of the tail of Shrapnel G. In addition we discovered a coherent and very extended feature that we interpret as a signature of an earlier interaction of the remnant with the stellar wind of its progenitor star. The peculiar Ne/O ratio we found in the wind residual may be suggestive of a Wolf-Rayet progenitor for Vela SNR, though further analysis is required to address this point., 10 pages, 13 figures, Accepted to A&A

Published
2021

37. Unidentified γ-ray emission towards the SNR Kes 41 revisited

Author

L. Supan, Michael G. Burton, G. Castelletti, and A.D. Supanitsky

Subjects
Physics, 010308 nuclear & particles physics, Computer Science::Information Retrieval, Astrophysics::High Energy Astrophysical Phenomena, ISM [GAMMA RAYS], INDIVIDUAL OBJECTS: KES 41 [ISM], Ciencias Físicas, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Astrophysics, 01 natural sciences, purl.org/becyt/ford/1 [https], Astronomía, Space and Planetary Science, 0103 physical sciences, SUPERNOVA REMNANTS [ISM], 010303 astronomy & astrophysics, Humanities, Astrophysics::Galaxy Astrophysics, CIENCIAS NATURALES Y EXACTAS
Abstract

Kes 41 is one of the Galactic supernova remnants (SNRs) that are proposed to be physically linked to γ-ray emission at GeV energies. The nature of the γ-ray photons has been explained, but inconclusively, as hadronic collisions of particles accelerated at the SNR blast wave with target protons in an adjacent molecular clump. We performed an analysis of Fermi-Large Area Telescope (LAT) data of about nine years to assess the origin of the γ-ray emission. To investigate this matter, we also used spectral modelling constraints from the physical properties of the interstellar medium towards the γ-ray emitting region along with a revised radio continuum spectrum of Kes 41 (α =-0.54 ± 0.10, Sνα). We demonstrate that the γ-ray fluxes in the GeV range can be explained through bremsstrahlung emission from electrons interacting with the surrounding medium. We also considered a model in which the emission is produced by pion decay after hadronic collisions, and confirm that this mechanism cannot be excluded. Fil: Supán, Jorge Leonardo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Castelletti, Gabriela Marta. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Supanitsky, Alberto Daniel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Burton, M.G.. University of New South Wales. Faculty of Science; Australia

Published
2018

38. Chandrasekhar and sub-Chandrasekhar models for the x-ray emission of type Ia Supernova remnants. I. Bulk properties

Author

Shigehiro Nagataki, Adam R. Foster, Anthony L. Piro, Daniel J. Patnaude, Katie Auchettl, Héctor Martínez-Rodríguez, Shiu-Hang Lee, Carles Badenes, Eduardo Bravo, Sangwook Park, Hiroya Yamaguchi, Patrick Slane, and Universitat Politècnica de Catalunya. Departament de Física

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, atomic data, Astrophysics::Solar and Stellar Astrophysics, ISM [X-rays], Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Chandrasekhar limit, Atomic data, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Supernoves, White dwarf, Astronomy and Astrophysics, Radius, X-rays: ISM, Interstellar medium, Supernova, Supernovae, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], hydrodynamics, Hydrodynamics, Supernova remnants [ISM], Astrophysics - High Energy Astrophysical Phenomena
Abstract

Type Ia supernovae originate from the explosion of carbon-oxygen white dwarfs in binary systems, but the exact nature of their progenitors remains elusive. The bulk properties of Type Ia supernova remnants, such as the radius and the centroid energy of the Fe K$\alpha$ blend in the X-ray spectrum, are determined by the properties of the supernova ejecta and the ambient medium. We model the interaction between Chandrasekhar and sub-Chandrasekhar models for Type Ia supernova ejecta and a range of uniform ambient medium densities in one dimension up to an age of 5000 years. We generate synthetic X-ray spectra from these supernova remnant models and compare their bulk properties at different expansion ages with X-ray observations from \textit{Chandra} and \textit{Suzaku}. We find that our models can successfully reproduce the bulk properties of most observed remnants, suggesting that Type Ia SN progenitors do not modify their surroundings significantly on scales of a few pc. Ambient medium density and expansion age are the main contributors to the diversity of the bulk properties in our models. Chandrasekhar and sub-Chandrasekhar progenitors make similar predictions for the bulk remnant properties, but detailed fits to X-ray spectra have the power to discriminate explosion energetics and progenitor scenarios., Comment: 22 pages, 14 figures, published in the ApJ

Published
2018

39. New perspectives on the supernova remnant Puppis A based on a radio polarization study

Author

Silvina Cichowolski, Estela Marta Reynoso, and Pablo F. Velázquez

Subjects
POLARIZATION, Astrophysics::High Energy Astrophysical Phenomena, Ciencias Físicas, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, purl.org/becyt/ford/1 [https], 0103 physical sciences, Puppis A, SUPERNOVA REMNANTS [ISM], Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, INDIVIDUAL OBJECTS: PUPPIS A [ISM], Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], MAGNETIC FIELDS, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Astronomía, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS
Abstract

We present a polarization study towards the supernova remnant (SNR) Puppis A based on original observations performed with the Australia Telescope Compact Array (ATCA). Based on the analysis of a feature detected outside the SNR shell (called `the tail' throughout the paper), it was possible to disentangle the emission with origin in Puppis A itself from that coming from the foreground Vela SNR. We found a very low polarization fraction, of about 3 percent on average. The upper limit of the magnetic field component parallel to the line of sight is estimated to be B$_\parallel \sim$ 20 $\mu$G. The statistical behavior of the magnetic vectors shows two preferential directions, almost perpendicular to each other, which are approximately aligned with the flat edges of Puppis A. A third, narrow peak oriented perpendicular to the Galactic plane suggests the existence of an interstellar magnetic field locally aligned in this direction. There is evidence that the magnetic vectors along the shell are aligned with the shock front direction. The low polarization fraction and the statistical behavior of the magnetic vectors are compatible with a scenario where the SNR evolves inside a stellar wind bubble with a box-like morphology, produced by the interaction of the different stellar winds, one of them magnetized, launched by the SN progenitor. This scenario can furthermore explain the morphology of Puppis A, rendering little support to the previously accepted picture which involved strong density gradients to explain the flat, eastern edge of the shell., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2018

40. Low-frequency radio absorption in Cassiopeia A

Author

M. Arias, J. Vink, F. de Gasperin, P. Salas, J. B. R. Oonk, R. J. van Weeren, A. S. van Amesfoort, J. Anderson, R. Beck, M. E. Bell, M. J. Bentum, P. Best, R. Blaauw, F. Breitling, J. W. Broderick, W. N. Brouw, M. Brüggen, H. R. Butcher, B. Ciardi, E. de Geus, A. Deller, P. C. G. van Dijk, S. Duscha, J. Eislöffel, M. A. Garrett, J. M. Grießmeier, A. W. Gunst, M. P. van Haarlem, G. Heald, J. Hessels, J. Hörandel, H. A. Holties, A. J. van der Horst, M. Iacobelli, E. Juette, A. Krankowski, J. van Leeuwen, G. Mann, D. McKay-Bukowski, J. P. McKean, H. Mulder, A. Nelles, E. Orru, H. Paas, M. Pandey-Pommier, V. N. Pandey, R. Pekal, R. Pizzo, A. G. Polatidis, W. Reich, H. J. A. Röttgering, H. Rothkaehl, D. J. Schwarz, O. Smirnov, M. Soida, M. Steinmetz, M. Tagger, S. Thoudam, M. C. Toribio, C. Vocks, M. H. D. van der Wiel, R. A. M. J. Wijers, O. Wucknitz, P. Zarka, P. Zucca, API (FNWI), High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), LOFAR, Astronomy, Astronomical Institute Anton Pannekoek, University of Amsterdam, SRON Netherlands Institute for Space Research (SRON), Leiden Observatory, Netherlands Institute for Radio Astronomy (ASTRON), GeoForschungsZentrum (GFZ), Max-Planck-Institut für Astronomie (MPIA), University of Technology Sydney, 15 Broadway, Ultimo, NSW 2007, Australia, University of Edinburgh, Leibniz-Institut für Astrophysik Potsdam (IAP), University of Hamburg, Gojenbergsweg 112, 21029, Hamburg, Germany, Mount Stromlo Observatory, Australian National University, Max-Planck-Institut für Astrophysik (MPA), Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Thüringer Landessternwarte, Tautenburg Observatory, JBCA School of Physics and Astronomy, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), CSIRO Astronomy and Space Science, Department of Astrophysics, Radboud University Nijmegen, PO Box 9010, 6500 GL, Nijmegen, The Netherlands, George Washington University, Astronomisches Institut der Ruhr-Universitat Bochum, Universitaetsstrasse 150, 44780, Bochum, Germany, University of Warmia and Mazury [Olsztyn], Department of Physics and Technology, University of Tromso, Tromso, Norway, Department of Physics and Astronomy, University of Missouri, Center for Information Technology, University of Groningen (CIT), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Poznan University of Technology, Space Research Center, Polish Academy of Sciences (Torun), Universität Bielefeld = Bielefeld University, Department of Physics and Electronics, Rhodes University, Astronomical Observatory, Jagiellonian University, Department of Physics and Electrical Engineering, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Electromagnetics, Center for Wireless Technology Eindhoven, EM for Radio Science Lab, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
TI-44, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, radio continuum: general, Astrophysics, 7. Clean energy, 01 natural sciences, supernova remnants / radiation mechanisms: general / radio continuum, Astrophysics::Solar and Stellar Astrophysics, individual, Ejecta, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, SUPERNOVA REMNANT CASSIOPEIA, general [radiation mechanisms], ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, ABSOLUTE SPECTRUM, supernova remnants [ISM], Radius, Supernova, EJECTA, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, general [radio continuum], Astrophysics - High Energy Astrophysical Phenomena, Cas A / ISM, individual: Cas A [supernovae], supernovae, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, radiation mechanisms: general, LARGE ARRAY, Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, Astronomy & Astrophysics, ACCELERATION, Radio spectrum, VDP::Matematikk og Naturvitenskap: 400::Fysikk: 430::Astrofysikk, astronomi: 438, 0103 physical sciences, 3-DIMENSIONAL STRUCTURE, Astrophysics::Galaxy Astrophysics, EXPLOSION, 010308 nuclear & particles physics, Astronomy and Astrophysics, LOFAR, Cassiopeia A, VDP::Mathematics and natural science: 400::Physics: 430::Astrophysics, astronomy: 438, supernovae: individual: Cas A, 13. Climate action, Space and Planetary Science, general, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CAS-A
Abstract

Cassiopeia A is one of the best-studied supernova remnants. Its shocked ejecta emits brightly in radio and X-rays. Its unshocked ejecta can be studied through infrared emission, the radio-active decay of $^{44}$Ti, and low frequency free-free absorption due to cold gas internal to the shell. Free-free absorption is affected by the mass, geometry, temperature, and ionisation conditions in the absorbing gas. Observations at the lowest radio frequencies constrain a combination of these properties. We use LOFAR LBA observations at 30-77 MHz and L-band VLA observations to compare $u-v$-matched images with a common resolution of 17". We simultaneously fit, per pixel, for the emission measure and the ratio of the emission from the unabsorbed front of the shell versus the absorbed back of the shell. We explore the effects that low temperatures and a high degree of clumping can have on the derived physical properties, such as mass and density. We also compile published radio flux measurements, fit for the absorption processes that occur in the radio band, and consider how they affect the secular decline of the source. We find a mass in the unshocked ejecta of $M = 2.95 \pm {0.48} \,M_{\odot}$ for an assumed gas temperature of $T=100$ K. This estimate is reduced for colder gas temperatures and if the ejecta are clumped. We measure the reverse shock to have a radius of $114$" $\pm $6". We also find that a decrease in the amount of mass in the unshocked ejecta (as more and more material meets the reverse shock and heats up) cannot account for the observed low frequency behaviour of the secular decline rate. To reconcile our low frequency absorption measurements with models that predict little mass in the unshocked ejecta we need the ejecta to be very clumped, or the temperature in the cold gas to be low ($\sim10$ K). Both conditions can jointly contribute to the high absorption., Accepted for publication in A&A v2: including the DOI, language edits

Published
2018

41. Population study of Galactic supernova remnants at very high γ-ray energies with H.E.S.S

Author

Christo Venter, H. Iwasaki, Gilles Maurin, Q. Piel, J. F. Glicenstein, J. Becker Tjus, A. Zech, M. Büchele, Julien Lefaucheur, Nachiketa Chakraborty, R. Liu, C. Mariaud, L. O'c. Drury, A.M. Taylor, C. Perennes, T. Garrigoux, Riaan Steenkamp, Ruben Lopez-Coto, Pierre Brun, M. Lemoine-Goumard, A. Wörnlein, P.-O. Petrucci, H. Ndiyavala, G. Lamanna, S. J. Fegan, A. Djannati-Ataï, N. W. Pekeur, P. Wagner, Alison Mitchell, Dieter Horns, Jean-Pierre Ernenwein, Zorawar Wadiasingh, B. Condon, I. Shilon, M. Seglar-Arroyo, Jan Conrad, Marco Padovani, Clemens Hoischen, A. A. Zdziarski, Frank M. Rieger, Johannes Veh, D. Gottschall, D. A. Sanchez, J. Hawkes, Anne Lemiere, Gavin Rowell, M. Bryan, R. C. G. Chaves, E. O. Angüner, Reinhard Schlickeiser, D. Zaborov, D. Jankowsky, Monica Barnard, A. S. Seyffert, Axel Donath, R. de los Reyes, A. W. Chen, M. Tluczykont, D. Fernandez, V. Poireau, Cameron B Rulten, C. Romoli, K. Morå, F. Gaté, Felix Spanier, I. Jung-Richardt, Manuel Meyer, H. Abdalla, Christian Stegmann, I. Oya, Stefan Wagner, Yasunobu Uchiyama, D. Wouters, M. A. Kastendieck, G. Vasileiadis, Nu. Komin, Jim Hinton, Y. A. Gallant, Fabian Schüssler, Matteo Cerruti, Stefan Ohm, Markus Holler, Felix Jankowsky, J. Decock, M. Mayer, S. Pita, Dmitry Khangulyan, Dorit Glawion, E. Moulin, Tomasz Bulik, S. Nakashima, J. Zorn, Robert Wagner, Thomas Lohse, L. Mohrmann, Felix Aharonian, L. Dirson, C. Farnier, Ramin Marx, E. Leser, M. Panter, U. Katz, Stefano Gabici, J. Dyks, C. van Rensburg, Werner Hofmann, G. Emery, Samar Safi-Harb, Thomas Vuillaume, B. Khélifi, S. Saito, Justine Devin, M. Lorentz, S. Bonnefoy, Constantin Steppa, M. Füßling, S. Eschbach, Jacek Niemiec, G. Hermann, Regis Terrier, Stefan Klepser, A. Balzer, Heinrich J. Völk, M. Mohamed, Olaf Reimer, P. P. Krüger, F. Voisin, D. Klochkov, Alexandre Marcowith, D.A. Prokhorov, M. Renaud, F. Zefi, D. Kerszberg, Rachel Simoni, Helen Poon, M. Jingo, R. D. Parsons, D. J. van der Walt, L. Oakes, J. Bolmont, I. Sushch, A. Ivascenko, R. Blackwell, S. Colafrancesco, Michael Backes, H. Prokoph, Masanori Arakawa, Gianluca Giavitto, V. Marandon, K. Dutson, Thomas Murach, Joachim Hahn, J. Lau, M. Settimo, Andreas Quirrenbach, Sami Caroff, Włodek Kluźniak, M. Capasso, S. Krakau, V. Sahakian, P. Bordas, Michael Zacharias, F. Niederwanger, J. P. Lees, H. Odaka, Tim Holch, S. Raab, A. Abramowski, G. Heinzelmann, N. Maxted, Krzysztof Katarzynski, A. Jacholkowska, Naomi Tsuji, Tanya Edwards, K. Kosack, Konrad Bernlöhr, Jacco Vink, Catherine Boisson, L. Tibaldo, D. Berge, Christoph Deil, Sabrina Casanova, Gerard Fontaine, G. Pelletier, B. Peyaud, Ullrich Schwanke, G. Pühlhofer, Johan Bregeon, J.-P. Tavernet, Kleopas Shiningayamwe, R. J. White, A. Reimer, A. Viana, Domenico Tiziani, D. Malyshev, Łukasz Stawarz, S. Bernhard, B. van Soelen, Michal Ostrowski, B. Rudak, J.-P. Lenain, F. Ait Benkhali, P. T. O'Brien, M. V. Fernandes, Manami Sasaki, S. Schwemmer, Andrea Santangelo, Gilles Henri, C. van Eldik, Stefan Funk, Alicja Wierzcholska, Marek Jamrozy, Helene Sol, B. Giebels, R. J. Tuffs, L. Jouvin, Iryna Lypova, Yvonne Becherini, K. Egberts, J. Chevalier, R. Rauth, Thomas Tavernier, N. Shafi, Natalia Żywucka, M. de Naurois, Ruizhi Yang, Tadayuki Takahashi, A. Schulz, Isak Delberth Davids, A. Fiasson, Roberta Zanin, P. Willmann, C. Trichard, P. J. Meintjes, A. Ziegler, H. Laffon, M. Arrieta, P. deWilt, J. King, Marion Spir-Jacob, Maria Haupt, Michelle Tsirou, L. Rinchiuso, Rafal Moderski, A. Carosi, Francois Brun, P. Vincent, M.-H. Grondin, Markus Böttcher, M. Katsuragawa, Pierre-Henri Aubert, M. Kraus, Michael Punch, Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), 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 de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Particules de Montpellier ( LUPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ), Centre d'Etudes Nucléaires de Bordeaux Gradignan ( CENBG ), 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 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 ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), 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 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 de la Recherche Scientifique ( CNRS ), HESS, 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)-Université Paris Diderot - Paris 7 (UPD7)-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 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), 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), 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), 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 Paris Cité (UPCité), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-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 Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), 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), 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), 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)-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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), 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), 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 de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), 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), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)

Subjects
electron, Milky Way, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Hochenergie-Astrophysik Theorie - Abteilung Hofmann, Infrarot-Astrophysik - Abteilung Hofmann, Cosmic ray, magnetic field, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, 7. Clean energy, 01 natural sciences, Luminosity, HESS, 0103 physical sciences, supernova, ddc:530, luminosity, flux: upper limit, cosmic radiation: acceleration, 010303 astronomy & astrophysics, HESS - Abteilung Hofmann, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, Astroparticle physics, Physics, radio wave, density, energy: high, cosmic radiation: spectrum, 010308 nuclear & particles physics, supernova remnants [ISM], Molecular cloud, shell model, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma rays: general, Galactic plane, Supernova, gamma ray: VHE, Space and Planetary Science, cosmic radiation: galaxy, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [gamma rays]
Abstract

著者人数: H.E.S.S. Collaboration 253名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 桂川, 美穂; 中島, 真也; 小高, 裕和; 高橋, 忠幸), Number of authors: H.E.S.S. Collaboration 253 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Katsuragawa, Miho; Nakashima, Shinya; Odaka, Hirokazu; Takahashi, Tadayuki), Accepted: 2018-02-08, 資料番号: SA1170368000

Published
2018

42. The supernova remnant W49B as seen with H.E.S.S. and Fermi-LAT

Author

M. Jingo, Ullrich Schwanke, I. Jung-Richardt, Markus Holler, Victor Zabalza, A. G. Akhperjanian, Michael Punch, Felix Jankowsky, I. Shilon, K. Dutson, D. Jankowsky, Felix Spanier, N. Shafi, Natalia Żywucka, T. Garrigoux, M. de Naurois, Christian Stegmann, Stefan Wagner, Yasunobu Uchiyama, J. Dyks, Mateusz Janiak, Felix Aharonian, H. Laffon, S. Eschbach, F. Spies, Ruizhi Yang, Marco Padovani, L. Mohrmann, C. van Rensburg, Thomas Tavernier, F. Niederwanger, A. Marcowith, C. Mariaud, Dieter Horns, Clemens Hoischen, A. A. Zdziarski, M. Lorentz, A. Schulz, Christoph Deil, T. Jogler, Gavin Rowell, M. Bryan, D. Zaborov, R. de los Reyes, P. Bordas, Nachiketa Chakraborty, Jacco Vink, Sabrina Casanova, R. Liu, C. Romoli, David Salek, E. Moulin, Tomasz Bulik, G. Lamanna, A. Fiasson, Christo Venter, Daniel Kerszberg, Ruben Lopez-Coto, M. Lemoine-Goumard, J. Lau, A. Jacholkowska, P. Willmann, Francois Brun, M. Chrétien, R. Moderski, A. Zech, B. Condon, Riaan Steenkamp, P. Wagner, M. Mayer, David Sánchez, Jacek Niemiec, Maria Haupt, Olaf Reimer, J. Becker Tjus, Thomas Murach, J. Chevalier, J. Hawkes, Krzysztof Katarzynski, Gilles Fontaine, Frank M. Rieger, Denis Wouters, Julien Lefaucheur, J. Bregeon, P.-O. Petrucci, Guillaume Dubus, L. O'c. Drury, Matteo Cerruti, F. Krayzel, R. Chalme-Calvet, Reinhard Schlickeiser, A. S. Seyffert, W. Kluźniak, D. Klochkov, M.-H. Grondin, N. W. Pekeur, Markus Böttcher, F. Zefi, Alison Mitchell, Zorawar Wadiasingh, D.A. Prokhorov, Michal Ostrowski, R. C. G. Chaves, J.-P. Lenain, Stefan Ohm, K. Morå, R. Blackwell, E. O. Angüner, Werner Hofmann, J. Decock, Pierre-Henri Aubert, S. Pita, J. Jeffrey Carr, Monica Barnard, L. Dirson, S. Öttl, F. Voisin, G. Heinzelmann, S. Colafrancesco, Stefano Gabici, Regis Terrier, Jan Conrad, N. Maxted, Aion Viana, C. Perennes, Nu. Komin, K. Egberts, M. Kraus, B. Peyaud, G. Pelletier, M. Kieffer, P. deWilt, A. Wörnlein, H. Odaka, Andrew M. Taylor, Stefan Funk, Alicja Wierzcholska, Ramin Marx, M. Panter, J. King, F. Ait Benkhali, Manami Sasaki, U. Katz, S. Schwemmer, R. J. Tuffs, S. J. Fegan, A. Djannati-Ataï, Andrea Santangelo, L. Tibaldo, M. Füßling, F. Schüssler, A. Balzer, R. J. White, Marek Jamrozy, Helene Sol, Domenico Tiziani, C. Trichard, I. D. Davids, Olivier Hervet, C. B. Rulten, P. J. Meintjes, Mariangela Settimo, Pierre Brun, Y. Cui, Rachel Simoni, Helen Poon, Joachim Hahn, M. Capasso, A. Ziegler, S. Krakau, V. Sahakian, C. Boisson, C. Farnier, M. Gajdus, E. Leser, Jean-Pierre Ernenwein, G. Cologna, Daniela Hadasch, B. Khélifi, G. Hermann, Johannes Veh, V. Lefranc, Heinrich J. Völk, M. Renaud, S. Bernhard, B. van Soelen, B. Rudak, M. Tluczykont, B. Degrange, H. Abdalla, M. A. Kastendieck, D. Gottschall, Anne Lemiere, Stefan Klepser, G. Vasileiadis, A. Ivascenko, Gilles Maurin, Y. A. Gallant, Łukasz Stawarz, Andreas Quirrenbach, Robert Wagner, Thomas Lohse, Justine Devin, Michael Zacharias, Léa Jouvin, T. Andersson, D. Kolitzus, M. Arrieta, Pascal Vincent, T. Vuillaume, Heike Prokoph, A. Förster, K. Stycz, J. F. Glicenstein, D. J. van der Walt, L. Oakes, J. Bolmont, I. Sushch, Axel Donath, A. W. Chen, Gilles Henri, Q. Piel, R. D. Parsons, F. Stinzing, B. Giebels, Junichiro Katsuta, Gianluca Giavitto, I. Oya, Tanya Edwards, S. Rosier-Lees, G. Spengler, Jim Hinton, M. Mohamed, Michael Backes, W. Domainko, J. P. Lees, S. Raab, A. Abramowski, P. P. Krüger, V. Marandon, D. Berge, Arti Goyal, J.-P. Tavernet, Iryna Lypova, Yvonne Becherini, P. T. O'Brien, Manuel Meyer, M. V. Fernandes, Peter Eger, C. van Eldik, K. Kosack, Konrad Bernlöhr, G. Pühlhofer, A. Reimer, Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), API Other Research (FNWI), ATLAS (IHEF, IoP, FNWI), Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), 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 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), Laboratoire Univers et Particules de Montpellier (LUPM), 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), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre de Physique des Particules de Marseille (CPPM), 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 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), AstroParticule et Cosmologie (APC (UMR_7164)), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 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), HESS, 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)-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), 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), Laboratoire d'Annecy de Physique des Particules (LAPP), 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), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-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 Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (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 de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), 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), and 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

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Hochenergie-Astrophysik Theorie - Abteilung Hofmann, Infrarot-Astrophysik - Abteilung Hofmann, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, 0103 physical sciences, Binary star, ddc:530, Supernova remnant, 010303 astronomy & astrophysics, HESS - Abteilung Hofmann, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Astroparticle physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Computer Science::Information Retrieval, supernova remnants [ISM], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Institut für Physik und Astronomie, Astronomy and Astrophysics, Supernova, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], ddc:520, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays], clouds [ISM], Fermi Gamma-ray Space Telescope
Abstract

The supernova remnant (SNR) W49B originated from a core-collapse supernova that occurred between one and four thousand years ago, and subsequently evolved into a mixed-morphology remnant, which is interacting with molecular clouds (MC). $\gamma$-ray observations of SNR/MC associations are a powerful tool to constrain the origin of Galactic cosmic-rays, as they can probe the acceleration of hadrons through their interaction with the surrounding medium and subsequent emission of non-thermal photons. The detection of a $\gamma$-ray source coincident with W49B at very high energies (VHE; E > 100 GeV) with the H.E.S.S. Cherenkov telescopes is reported together with a study of the source with 5 years of Fermi-LAT high energy $\gamma$-ray (0.06 - 300 GeV) data. The smoothly-connected combined source spectrum, measured from 60 MeV to multi-TeV energies, shows two significant spectral breaks at $304\pm20$ MeV and $8.4_{-2.5}^{+2.2}$ GeV, the latter being constrained by the joint fit from the two instruments. The detected spectral features are similar to those observed in several other SNR/MC associations and are found to be indicative of $\gamma$-ray emission produced through neutral-pion decay., Comment: 10 pages, 6 figures. Accepted for publication in A&A

Published
2018

43. Detailed spectral and morphological analysis of the shell type supernova remnant RCW 86

Author

C.-C. Lu, F. Schüssler, Felix Spanier, M. V. Fernandes, Gilles Henri, Jacco Vink, M. Mayer, F. Krayzel, M. Ostrowski, Sabrina Casanova, N. Chakraborty, E. Birsin, Thomas Tavernier, Werner Hofmann, Peter Eger, C. van Eldik, M. de Naurois, Mateusz Janiak, Ruizhi Yang, Guillaume Dubus, A. Marcowith, P. Espigat, Nu. Komin, Michael Punch, S. Häffner, Rachel Simoni, Helen Poon, A. Lopatin, N. Zywucka, F. Stinzing, B. Giebels, Tanya Edwards, Marek Jamrozy, M. Zacharia, Isak Delberth Davids, Daniel Kerszberg, A. Fiasson, G. Pelletier, K. Dutson, F. Spies, S. J. Wagner, P. Willmann, S. Rosier-Lees, M. Mohamed, Michal Dyrda, T. Vuillaume, Jacek Niemiec, Stefan Ohm, S. Pita, I. Jung-Richardt, M. Lemoine-Goumard, Helene Sol, Olaf Reimer, S. Bernhard, C. Mariaud, M. Kieffer, B. van Soelen, P. Wagner, F. Ait Benkhali, T. Bulik, B. Rudak, K. Stycz, Reinhard Schlickeiser, Yuzhu Cui, S. Schwemmer, Stefano Gabici, B. Degrange, Andrea Santangelo, Christoph Deil, J. Hawkes, V. Marandon, Frank M. Rieger, J. F. Glicenstein, A. Wörnlein, Victor Zabalza, Thomas Murach, U. Menzler, M. Füßling, André Schulz, Jim Hinton, R. Chalme-Calvet, C. Romoli, S. J. Fegan, A. Djannati-Ataï, Markus Holler, Arti Goyal, Michael Backes, Regis Terrier, Felix Jankowsky, J.-P. Lenain, J. Dyks, Joachim Hahn, A. Ivascenko, G. Spengler, Francois Brun, M. Chrétien, V. Lefranc, Olivier Hervet, Denis Wouters, Dieter Horns, R. J. Tuffs, H. Prokoph, Clemens Hoischen, A. A. Zdziarski, C. B. Rulten, Öttl, G. Heinzelmann, D. Fernandez, K. Kosack, F. Voisin, Konrad Bernlöhr, D. Berge, G. Lamanna, Yvonne Becherini, K. Egberts, Petter Hofverberg, Felix Aharonian, R. D. Parsons, G. Pühlhofer, S. Colafrancesco, Pierre Brun, Jan Conrad, J. Bolmont, M. A. Kastendieck, D.A. Prokhorov, J.L. Van der Walt, I. Sushch, C. Couturier, D. Klochkov, Andrew M. Taylor, C. Farnier, Andreas Hillert, J. Becker Tjus, J. Jeffrey Carr, W. Domainko, Gerard Fontaine, Ignasi Reichardt, R. Blackwell, F. Feinstein, J. Bregeon, M. Paz Arribas, Gianluca Giavitto, M. Gajdus, A. Reimer, H. Laffon, Alison Mitchell, Markus Böttcher, Alicja Wierzcholska, T. Garrigoux, K. Valerius, Daniela Hadasch, B. Khélifi, G. Hermann, P.-O. Petrucci, M. Grudzińska, Jean-Pierre Ernenwein, R. C. G. Chaves, E. O. Angüner, L. O'c. Drury, F. Zefi, H. Odaka, N. W. Pekeur, Johannes Veh, A. Balzer, D. Kolitzus, P. deWilt, Lukasz Stawarz, A. Förster, G. Vasileiadis, S. Raab, A. G. Akhperjanian, A. Abramowski, S. Klepser, Aion Viana, Ramin Marx, J.-P. Tavernet, M. Panter, U. Katz, U. Schwanke, M. Tluczykont, B. Opitz, N. Maxted, K. Moraa, S. Krakau, L. B. Oakes, Y. A. Gallant, Christo Venter, Christian Stegmann, Andreas Quirrenbach, V. Sahakian, P.P. Krüger, Riaan Steenkamp, Misao Sasaki, M. Lorentz, R. Moderski, A. Zech, Axel Donath, A. W. Chen, Pascal Vincent, David Sánchez, M.-H. Grondin, J. Lau, Julien Lefaucheur, A. S. Seyffert, J. Chevalier, Krzysztof Katarzynski, C. Boisson, D. Gottschall, Anne Lemiere, C. Trichard, David Salek, E. Moulin, R. Lui, P. J. Meintjes, Matthias Weidinger, B. Condon, A. Jacholkowska, Manuel Meyer, Robert Wagner, B. Peyaud, R. White, Thomas Lohse, W. Kluzniak, Gavin Rowell, M. Bryan, D. Zaborov, R. de los Reyes, Gilles Maurin, G. Cologna, Heinrich J. Völk, M. Renaud, P. Bordas, Igor Oya, 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)-Université Paris Diderot - Paris 7 (UPD7)-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), 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, HESS, 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 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), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), API Other Research (FNWI), and ATLAS (IHEF, IoP, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), Kinetic energy, 01 natural sciences, cosmic rays, 0103 physical sciences, ddc:530, Sensitivity (control systems), 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, Spectral index, supernova remnants [ISM], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Institut für Physik und Astronomie, Astronomy and Astrophysics, Supernova, Space and Planetary Science, astroparticle physics, ddc:520, Spectral energy distribution, Production (computer science), general [gamma rays]
Abstract

Aim. We aim for an understanding of the morphological and spectral properties of the supernova remnant RCW 86 and for insights into the production mechanism leading to the RCW 86 very high-energy γ-ray emission.Methods. We analyzed High Energy Spectroscopic System (H.E.S.S.) data that had increased sensitivity compared to the observations presented in the RCW 86 H.E.S.S. discovery publication. Studies of the morphological correlation between the 0.5–1 keV X-ray band, the 2–5 keV X-ray band, radio, and γ-ray emissions have been performed as well as broadband modeling of the spectral energy distribution with two different emission models.Results. We present the first conclusive evidence that the TeV γ-ray emission region is shell-like based on our morphological studies. The comparison with 2–5 keV X-ray data reveals a correlation with the 0.4–50 TeV γ-ray emission. The spectrum of RCW 86 is best described by a power law with an exponential cutoff at Ecut = (3.5 ± 1.2stat) TeV and a spectral index of Γ ≈ 1.6 ± 0.2. A static leptonic one-zone model adequately describes the measured spectral energy distribution of RCW 86, with the resultant total kinetic energy of the electrons above 1 GeV being equivalent to ~0.1% of the initial kinetic energy of a Type Ia supernova explosion (1051 erg). When using a hadronic model, a magnetic field of B ≈ 100 μG is needed to represent the measured data. Although this is comparable to formerly published estimates, a standard E−2 spectrum for the proton distribution cannot describe the γ-ray data. Instead, a spectral index of Γp ≈ 1.7 would be required, which implies that ∼7 × 1049/ncm−3 has been transferred into high-energy protons with the effective density ncm−3 = n/1 cm−3. This is about 10% of the kinetic energy of a typical Type Ia supernova under the assumption of a density of 1 cm−3.

Published
2018

44. Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sato, T, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, AstroParticule et Cosmologie (APC (UMR_7164)), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, 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), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), 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)-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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], observational [methods], FOS: Physical sciences, Astrophysics, 01 natural sciences, individual objects (N 132 D) [ISM], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Spectral resolution, 010306 general physics, Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Line (formation), ISM: supernova remnants, instrumentation: spectrographs, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants [ISM], individual (N 132 D) [X-rays], Astronomy and Astrophysics, X-rays: individual (N 132 D), Redshift, Interstellar medium, Supernova, ISM: individual object (N 132 D), 13. Climate action, Space and Planetary Science, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], spectrographs [instrumentation]
Abstract

著者人数: Hitomi Collaboration 193名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 193 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-12-06, 資料番号: SA1170341000

Published
2018

45. Hitomi X-ray observation of the pulsar wind nebula G21.5$−$0.9

Author

Tsuneyoshi Kamae, Chris Done, Takeshi Nakamori, Hirofumi Noda, Philippe Laurent, Gregory V. Brown, Masahiro Tsujimoto, Luigi C. Gallo, Andrea Goldwurm, Akio Hoshino, Edward M. Cackett, Makoto Tashiro, Yoichi Yatsu, Kazutaka Yamaoka, Makoto Yamauchi, Makoto Sawada, Esra Bulbul, Yasuo Tanaka, Katsuji Koyama, Hiromitsu Takahashi, Kazuhisa Mitsuda, Tsunefumi Mizuno, Jon M. Miller, Takashi Okajima, Katsuhiro Hayashi, Yang Soong, Daisuke Yonetoku, Peter J. Serlemtsos, Yoshitaka Ishisaki, Hans A. Krimm, Akihiro Furuzawa, Olivier Limousin, Shiu-Hang Lee, Takao Kitaguchi, Laura Brenneman, Hideki Uchiyama, Samar Safi-Harb, Koji Mukai, Poshak Gandhi, Yasushi Fukazawa, Abderahmen Zoghbi, Ann Hornschemeier, Marc Audard, Hiroki Akamatsu, Andrew Szymkowiak, D. Lumb, Koji Mori, Hiroshi Tsunemi, Kazuhiro Nakazawa, Jan-Willem den Herder, Robert Petre, Shinya Saito, Aya Kubota, Takayuki Hayashi, Shinya Nakashima, Carlo Ferrigno, Eric D. Miller, Shin'ichiro Uno, Masachika Iwai, Dan McCammon, Takao Nakagawa, Irina Zhuravleva, Satoshi Sugita, Naomi Ota, Nozomu Nakaniwa, Ikuyuki Mitsuishi, Richard L. Kelley, Missagh Mehdipour, Motohide Kokubun, Dan R. Wilkins, Tadayuki Takahashi, Marshall W. Bautz, Francesco Tombesi, Jelle Kaastra, Katja Pottschmidt, Shunji Kitamoto, Masanobu Ozaki, Yuzuru Tawara, Margherita Giustini, Ken Ebisawa, Ryo Iizuka, Greg Madejski, Takeshi Go Tsuru, Shin Mineshige, Toshiki Sato, Liyi Gu, Hiroyasu Tajima, Aya Bamba, Roger Blandford, Yuichi Terashima, C. Megan Urry, Richard F. Mushotzky, Peter Kretschmar, Kosuke Sato, Knox S. Long, Steven W. Allen, Hideyuki Mori, Hiroyuki Uchida, Yoshihiro Ueda, Kyoko Matsushita, Nobuyuki Kawai, Brian J. Williams, Hiroshi Murakami, Tetsu Kitayama, Randall K. Smith, Hiroshi Tomida, Norbert Schartel, Toru Tamagawa, Łukasz Stawarz, Rie Sato, Hiroya Yamaguchi, Hisamitsu Awaki, Takaaki Tanaka, Frits Paerels, Tadayasu Dotani, Yasuharu Sugawara, Ciro Pinto, Paolo Coppi, Kiyoshi Hayashida, Frederick S. Porter, Matteo Guainazzi, Isamu Hatsukade, Toru Sasaki, Megan E. Eckart, Takaya Ohashi, Yasunobu Uchiyama, Kouichi Hagino, Yuichiro Ezoe, Megumi Shidatsu, Kumi Ishikawa, Takayuki Tamura, Stéphane Paltani, Hideyo Kunieda, Eugenio Ursino, Adam R. Foster, Ryuichi Fujimoto, Caroline A. Kilbourne, Yoh Takei, Yoshito Haba, Noriko Y. Yamasaki, Elisa Costantini, Shin'ichiro Takeda, Takayoshi Kohmura, Maria Chernyakova, Shin Watanabe, Aurora Simionescu, Hiroshi Nakajima, Satoru Katsuda, Magnus Axelsson, Meng P. Chiao, Jelle de Plaa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Yohko Tsuboi, Norbert Werner, Andrew C. Fabian, Kazuo Makishima, Fumie Akimoto, Jun Kataoka, Brian R. McNamara, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Shu Koyama, Masayoshi Nobukawa, Tahir Yaqoob, Hironori Matsumoto, Yoshitomo Maeda, Cor P. de Vries, Benson Guest, Masanori Ohno, Christopher S. Reynolds, Hirokazu Odaka, Michael Loewenstein, Kenji Hamaguchi, Ilana M. Harrus, Manabu Ishida, Yoshiyuki Inoue, Yukikatsu Terada, Hiroaki Murakami, Timothy R. Kallman, Takuya Miyazawa, Shinya Yamada, Kazuhiro Sakai, Felix Aharonian, Junko S. Hiraga, Hiromi Seta, Teruaki Enoto, John P. Hughes, Daniel Maier, Hajime Inoue, Lorella Angelini, Maurice A. Leutenegger, Kumiko K. Nobukawa, Goro Sato, Shutaro Ueda, AstroParticule et Cosmologie (APC (UMR_7164)), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, 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), 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), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Photon, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, pulsars: individual (PSRJ1833-1034), 01 natural sciences, Pulsar wind nebula, Power law, Spectral line, 010309 optics, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectrometer, supernova remnants [ISM], individual (PSR J1833-1034) [pulsars], Astronomy and Astrophysics, ISM: individual objects (G21.5-0.9), Space and Planetary Science, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, individual objects (G21.5-0.9) [ISM], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: 196名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子; 佐藤, 寿紀; 中庭, 望), Number of authors: Hitomi Collaboration 197 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Hayashi, Tasuku; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.; Sato, Toshiki; Nakaniwa, Nozomu), Accepted: 2018-02-14, 資料番号: SA1180104000

Published
2018

46. A Catalogue of Galactic Supernova Remnants in the far-infrared: revealing ejecta dust in pulsar wind nebulae

Author

Haley Louise Gomez, Alberto Noriega-Crespo, Phil Cigan, Jeonghee Rho, M. J. Barlow, Loretta Dunne, Mikako Matsuura, I. De Looze, H. Chawner, and Kenneth A. Marsh

Subjects
stars, Infrared, Astrophysics::High Energy Astrophysical Phenomena, MILLISECOND PULSAR, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, X-RAY-EMISSION, EARLY UNIVERSE, Far infrared, Pulsar, 0103 physical sciences, Emissivity, ISM [submillimetre], Ejecta, RADIO-CONTINUUM, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, HI-GAL, SUBMILLIMETER LUMINOSITY, 010308 nuclear & particles physics, supernova remnants [ISM], ISM [infrared], Astronomy and Astrophysics, PLANE, Galactic plane, Astrophysics - Astrophysics of Galaxies, CASSIOPEIA, Stars, Supernova, Physics and Astronomy, 13. Climate action, Space and Planetary Science, DISCOVERY, Astrophysics of Galaxies (astro-ph.GA), YOUNG
Abstract

We search for far-infrared (FIR) counterparts of known supernova remnants (SNRs) in the Galactic plane (10 deg, Comment: 33 pages and 39 figures. Accepted in MNRAS. Appendix figures are available here: https://github.com/hanchawn/Arxiv (includes full catalogue of Herschel images from this sample)

Published
2018
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47. Deep XMM-Newton observations of the northern disc of M31. I. Source catalogue

Author

B. F. Williams, Manami Sasaki, A. Karampelas, Frank Haberl, Dieter Breitschwerdt, Sara Saeedi, P. J. Kavanagh, Despina Hatzidimitriou, M. A. de Avillez, Kirill Sokolovsky, Paul P. Plucinsky, Martin Henze, Miroslav Filipovic, T. J. Galvin, and Knox S. Long

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Flux, Binary number, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, ISM [X-rays], 010303 astronomy & astrophysics, individual: M31 [galaxies], Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nebula, 010308 nuclear & particles physics, supernova remnants [ISM], Spectral properties, Astronomy and Astrophysics, Andromeda, Supernova, Stars, Space and Planetary Science, binaries [X-rays], Astrophysics - High Energy Astrophysical Phenomena
Abstract

We carried out new observations of two fields in the northern ring of M31 with XMM-Newton with two exposures of 100 ks each and obtained a complete list of X-ray sources down to a sensitivity limit of ~7 x 10^34 erg s^-1 (0.5 - 2.0 keV). The major objective of the observing programme was the study of the hot phase of the ISM in M31. The analysis of the diffuse emission and the study of the ISM is presented in a separate paper. We analysed the spectral properties of all detected sources using hardness ratios and spectra if the statistics were high enough. We also checked for variability. We cross-correlated the source list with the source catalogue of a new survey of the northern disc of M31 carried out with Chandra and Hubble (Panchromatic Hubble Andromeda Treasury, PHAT) as well as with other existing catalogues. We detected a total of 389 sources, including 43 foreground stars and candidates and 50 background sources. Based on the comparison to the Chandra/PHAT survey, we classify 24 hard X-ray sources as new candidates for X-ray binaries (XRBs). In total, we identified 34 XRBs and candidates and 18 supernova remnants (SNRs) and candidates. Three of the four brightest SNRs show emission mainly below 2 keV, consistent with shocked ISM. The spectra of two of them also require an additional component with a higher temperature. The SNR [SPH11] 1535 has a harder spectrum and might suggest that there is a pulsar-wind nebula inside the SNR. We find five new sources showing clear time variability. We also studied the spectral properties of the transient source SWIFT J004420.1+413702, which shows significant variation in flux over a period of seven months (June 2015 to January 2016) and associated change in absorption. Based on the likely optical counterpart detected in the Chandra/PHAT survey, the source is classified as a low-mass X-ray binary., Comment: Accepted for publication in A&A

Published
2018
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48. H.E.S.S. observations of RX J1713.7-3946 with improved angular and spectral resolution; evidence for gamma-ray emission extending beyond the X-ray emitting shell

Author

Collaboration, H., Abdalla, H., Abramowski, A., Aharonian, F., Ait Benkhali, F., Angüner, E., Arakawa, M., Arrieta, M., Aubert, P., Backes, M., Balzer, A., Barnard, M., Becherini, Y., Becker Tjus, J., Berge, D., Bernhard, S., Bernloehr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., Bordas Coma, P., Bregeon, J., Brun, F., Brun, P., Bryan, M., Büchele, M., Bulik, T., Capasso, M., Carrigan, S., Caro, S., Carosi, A., Casanova, S., Cerruti, M., Chakraborty, N., Chaves, R., Chen, A., Chevalier, J., Colafrancesco, S., Condon, B., Conrad, J., Davids, I., Decock, J., Deil, C., Devin, J., deWilt, P., Dirson, L., Djannati-Ataï, A., Domainko, W., Donath, A., Drury, L., Dutson, K., Dyks, J., Edwards, T., Egberts, K., Eger, P., Emery, G., Ernenwein, J., Eschbach, S., Farnier, C., Fegan, S., Fernandes, M., Fiasson, A., Fontaine, G., Förster, A., Funk, S., Füßling, M., Gabici, S., Gallant, Y., Garrigoux, T., Gast, H., Gaté, F., Giavitto, G., Giebels, B., Glawion, D., Glicenstein, J., Gottschall, D., Grondin, M., Hahn, J., Haupt, M., Hawkes, J., Heinzelmann, G., Henri, G., Hermann, G., Hinton, J., Hofmann, W., Hoischen, C., Holch, T., Holler, M., Horns, D., Ivascenko, A., Iwasaki, H., Jacholkowska, A., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jingo, M., Jouvin, L., Jung-Richardt, I., Kastendieck, M., Katarzynski, K., Katsuragawa, M., Katz, U., Kerszberg, D., Khangulyan, D., Khélifi, B., King, J., Klepser, S., Klochkov, D., Klúzniak, W., Komin, N., Kosack, K., Krakau, S., Kraus, M., Krüger, P., Lamanna, G., Lau, J., Lees, J., Lefaucheur, J., Lemière, A., Lemoine-Goumard, M., Lenain, J., Leser, E., Lohse, T., Lorentz, M., Liu, R., López-Coto, R., Lypova, I., Marandon, V., Malyshev, D., Marcowith, A., Mariaud, C., Marx, R., Maurin, G., Maxted, N., Mayer, M., Meintjes, P., Meyer, M., Mitchell, A., Moderski, R., Mohamed, M., Mohrmann, L., Morå, K., Moulin, E., Murach, T., Nakashima, S., de Naurois, M., Ndiyavala, H., Niederwanger, F., Niemiec, J., Oakes, L., O’Brien, P., Odaka, H., Ohm, S., Ostrowski, M., Oya, I., Padovani, M., Panter, M., Parsons, R., Paz Arribas, M., Pekeur, N., Pelletier, G., Perennes, C., Petrucci, P., Peyaud, B., Piel, Q., Pita, S., Poireau, V., Poon, H., Prokhorov, D., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Rauth, R., Reimer, A., Reimer, O., Renaud, M., de los Reyes, R., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Rulten, C., Safi-Harb, S., Sahakian, V., Saito, S., Sanchez, D., Santangelo, A., Sasaki, M., Schandri, M., Schlickeiser, R., Schüssler, F., Schulz, A., Schwanke, U., Schwemmer, S., Seglar-Arroyo, M., Settimo, M., ert, A., Shafi, N., Shilon, I., Shiningayamwe, K., Simoni, R., Sol, H., Spanier, F., Spir-Jacob, M., Stawarz, Ł., Steenkamp, R., Stegmann, C., Steppa, C., Sushch, I., Takahashi, T., Tavernet, J., Tavernier, T., Taylor, A., Terrier, R., Tibaldo, L., Tiziani, D., Tluczykont, M., Trichard, C., Tsirou, M., Tsuji, N., Tuffs, R., Uchiyama, Y., van der Walt, D., van Eldik, C., van Rensburg, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Viana, A., Vincent, P., Vink, J., Voisin, F., Voelk, H., Vuillaume, T., Wadiasingh, Z., Wagner, S., Wagner, P., Wagner, R., White, R., Wierzcholska, A., Willmann, P., Wörnlein, A., Wouters, D., Yang, R., Zaborov, D., Zacharias, M., Zanin, R., Zdziarski, A., Zech, A., Zefi, F., Ziegler, A., Zorn, J., Zywucka, N., Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), 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 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), Laboratoire Univers et Particules de Montpellier (LUPM), 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), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), 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), 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), AstroParticule et Cosmologie (APC (UMR_7164)), 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), 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)-Centre National de la Recherche Scientifique (CNRS), HESS, Laboratoire d'Annecy de Physique des Particules (LAPP), 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), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), 26598973 - Abdalla, Hassan, 20574266 - Barnard, Monica, 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 26909995 - Garrigoux, Tania, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 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 (UB)-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)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), API Other Research (FNWI), and ATLAS (IHEF, IoP, FNWI)

Subjects
emission [X-ray], [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, VHE [gamma ray], Hochenergie-Astrophysik Theorie - Abteilung Hofmann, Infrarot-Astrophysik - Abteilung Hofmann, energy spectrum, brightness, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, Acceleration, cosmic rays, emission [gamma ray], HESS, supernova, 0103 physical sciences, surface, Angular resolution, Surface brightness, Spectral resolution, HESS - Abteilung Hofmann, 010303 astronomy & astrophysics, ISM: supernova remnants, acceleration of particles, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, supernova remnants [ISM], Gamma ray, resolution, astroparticle physic, Astronomy and Astrophysics, gamma rays: general, acceleration, sensitivity, charged particle, doubling, Charged particle, Supernova, angular resolution, Space and Planetary Science, ddc:520, spectral, Astroparticle physics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [gamma rays]
Abstract

著者人数: H.E.S.S. Collaboration 256名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 高橋, 忠幸), Number of authors: H.E.S.S. Collaboration 256 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Takahashi, Tadayuki), Accepted: 2016-12-18, 資料番号: SA1170361000

Published
2018
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49. The population of TeV pulsar wind nebulae in the H.E.S.S. Galactic Plane Survey

Author

Collaboration, H., Abdalla, H., Abramowski, A., Aharonian, F., Ait Benkhali, F., Angüner, E., Arakawa, M., Arrieta, M., Aubert, P., Backes, M., Balzer, A., Barnard, M., Becherini, Y., Becker Tjus, J., Berge, D., Bernhard, S., Bernloehr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., Bordas Coma, P., Bregeon, J., Brun, F., Brun, P., Bryan, M., Büchele, M., Bulik, T., Capasso, M., Carrigan, S., Caro, S., Carosi, A., Casanova, S., Cerruti, M., Chakraborty, N., Chaves, R., Chen, A., Chevalier, J., Colafrancesco, S., Condon, B., Conrad, J., Davids, I., Decock, J., Deil, C., Devin, J., deWilt, P., Dirson, L., Djannati-Ataï, A., Domainko, W., Donath, A., Drury, L., Dutson, K., Dyks, J., Edwards, T., Egberts, K., Eger, P., Emery, G., Ernenwein, J., Eschbach, S., Farnier, C., Fegan, S., Fernandes, M., Fiasson, A., Fontaine, G., Förster, A., Funk, S., Füßling, M., Gabici, S., Gallant, Y., Garrigoux, T., Gast, H., Gaté, F., Giavitto, G., Giebels, B., Glawion, D., Glicenstein, J., Gottschall, D., Grondin, M., Hahn, J., Haupt, M., Hawkes, J., Heinzelmann, G., Henri, G., Hermann, G., Hinton, J., Hofmann, W., Hoischen, C., Holch, T., Holler, M., Horns, D., Ivascenko, A., Iwasaki, H., Jacholkowska, A., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jingo, M., Jouvin, L., Jung-Richardt, I., Kastendieck, M., Katarzynski, K., Katsuragawa, M., Katz, U., Kerszberg, D., Khangulyan, D., Khélifi, B., King, J., Klepser, S., Klochkov, D., Klúzniak, W., Komin, N., Kosack, K., Krakau, S., Kraus, M., Krüger, P., Lamanna, G., Lau, J., Lees, J., Lefaucheur, J., Lemière, A., Lemoine-Goumard, M., Lenain, J., Leser, E., Lohse, T., Lorentz, M., Liu, R., López-Coto, R., Lypova, I., Marandon, V., Malyshev, D., Marcowith, A., Mariaud, C., Marx, R., Maurin, G., Maxted, N., Mayer, M., Meintjes, P., Meyer, M., Mitchell, A., Moderski, R., Mohamed, M., Mohrmann, L., Morå, K., Moulin, E., Murach, T., Nakashima, S., de Naurois, M., Ndiyavala, H., Niederwanger, F., Niemiec, J., Oakes, L., O’Brien, P., Odaka, H., Ohm, S., Ostrowski, M., Oya, I., Padovani, M., Panter, M., Parsons, R., Paz Arribas, M., Pekeur, N., Pelletier, G., Perennes, C., Petrucci, P., Peyaud, B., Piel, Q., Pita, S., Poireau, V., Poon, H., Prokhorov, D., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Rauth, R., Reimer, A., Reimer, O., Renaud, M., de los Reyes, R., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Rulten, C., Safi-Harb, S., Sahakian, V., Saito, S., Sanchez, D., Santangelo, A., Sasaki, M., Schandri, M., Schlickeiser, R., Schüssler, F., Schulz, A., Schwanke, U., Schwemmer, S., Seglar-Arroyo, M., Settimo, M., ert, A., Shafi, N., Shilon, I., Shiningayamwe, K., Simoni, R., Sol, H., Spanier, F., Spir-Jacob, M., Stawarz, Ł., Steenkamp, R., Stegmann, C., Steppa, C., Sushch, I., Takahashi, T., Tavernet, J., Tavernier, T., Taylor, A., Terrier, R., Tibaldo, L., Tiziani, D., Tluczykont, M., Trichard, C., Tsirou, M., Tsuji, N., Tuffs, R., Uchiyama, Y., van der Walt, D., van Eldik, C., van Rensburg, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Viana, A., Vincent, P., Vink, J., Voisin, F., Voelk, H., Vuillaume, T., Wadiasingh, Z., Wagner, S., Wagner, P., Wagner, R., White, R., Wierzcholska, A., Willmann, P., Wörnlein, A., Wouters, D., Yang, R., Zaborov, D., Zacharias, M., Zanin, R., Zdziarski, A., Zech, A., Zefi, F., Ziegler, A., Zorn, J., Zywucka, N., 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 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), Laboratoire Univers et Particules de Montpellier (LUPM), 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), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), 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), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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), 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 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 Diderot - Paris 7 (UPD7), HESS, 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 (UB)-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)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), 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), 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 de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), API Other Research (FNWI), and ATLAS (IHEF, IoP, FNWI)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Proper motion, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Population, Hochenergie-Astrophysik Theorie - Abteilung Hofmann, Infrarot-Astrophysik - Abteilung Hofmann, FOS: Physical sciences, Astrophysics, 01 natural sciences, Pulsar wind nebula, general [pulsars], Pulsar, surveys, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, ddc:530, Surface brightness, education, 010303 astronomy & astrophysics, HESS - Abteilung Hofmann, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Nebula, 010308 nuclear & particles physics, Computer Science::Information Retrieval, supernova remnants [ISM], Institut für Physik und Astronomie, Astronomy and Astrophysics, Galactic plane, 13. Climate action, Space and Planetary Science, ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays], catalogs
Abstract

The nine-year H.E.S.S. Galactic Plane Survey (HGPS) yielded the most uniform observation scan of the inner Milky Way in the TeV gamma-ray band to date. The sky maps and source catalogue of the HGPS allow for a systematic study of the population of TeV pulsar wind nebulae found throughout the last decade. To investigate the nature and evolution of pulsar wind nebulae, for the first time we also present several upper limits for regions around pulsars without a detected TeV wind nebula. Our data exhibit a correlation of TeV surface brightness with pulsar spin-down power $\dot{E}$. This seems to be caused both by an increase of extension with decreasing $\dot{E}$, and hence with time, compatible with a power law $R_\mathrm{PWN}(\dot{E}) \sim \dot{E}^{-0.65 \pm 0.20}$, and by a mild decrease of TeV gamma-ray luminosity with decreasing $\dot{E}$, compatible with $L_{1-10\,\mathrm{TeV}} \sim \dot{E}^{0.59 \pm 0.21}$. We also find that the offsets of pulsars with respect to the wind nebula centres with ages around 10 kyr are frequently larger than can be plausibly explained by pulsar proper motion and could be due to an asymmetric environment. In the present data, it seems that a large pulsar offset is correlated with a high apparent TeV efficiency $L_{1-10\,\mathrm{TeV}}/\dot{E}$. In addition to 14 HGPS sources considered as firmly identified pulsar wind nebulae and 5 additional pulsar wind nebulae taken from literature, we find 10 HGPS sources that form likely TeV pulsar wind nebula candidates. Using a model that subsumes the present common understanding of the very high-energy radiative evolution of pulsar wind nebulae, we find that the trends and variations of the TeV observables and limits can be reproduced to a good level, drawing a consistent picture of present-day TeV data and theory., Comment: 28 pages, 12 figures, 8 tables. Accepted for publication in A&A

Published
2018

50. A decade of ejecta dust formation in the Type IIn SN 2005ip

Author

I. De Looze, A. Bevan, Roger Wesson, Kelsie Krafton, Geoffrey C. Clayton, Jennifer E. Andrews, Mikako Matsuura, M. J. Barlow, and Dan Milisavljevic

Subjects
GRAINS, media_common.quotation_subject, statistical [methods], Monte Carlo method, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, Methods statistical, CORE-COLLAPSE SUPERNOVAE, EARLY UNIVERSE, 0103 physical sciences, Radiative transfer, MASSES, Ejecta, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Line (formation), media_common, Physics, 010308 nuclear & particles physics, supernova remnants [ISM], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Universe, GALAXY, CASSIOPEIA, Supernova, Astrophysics - Solar and Stellar Astrophysics, Physics and Astronomy, radiative transfer, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), individual: SN 2005ip [supernovae], REMNANT, EMISSION, general [supernovae]
Abstract

In order to understand the contribution of core-collapse supernovae to the dust budget of the early universe, it is important to understand not only the mass of dust that can form in core-collapse supernovae but also the location and rate of dust formation. SN 2005ip is of particular interest since dust has been inferred to have formed in both the ejecta and the post-shock region behind the radiative reverse shock. We have collated eight optical archival spectra that span the lifetime of SN 2005ip and we additionally present a new X-shooter optical-near-IR spectrum of SN 2005ip at 4075d post-discovery. Using the Monte Carlo line transfer code DAMOCLES, we have modelled the blueshifted broad and intermediate width H$\alpha$, H$\beta$ and He I lines from 48d to 4075d post-discovery using an ejecta dust model. We find that dust in the ejecta can account for the asymmetries observed in the broad and intermediate width H$\alpha$, H$\beta$ and He I line profiles at all epochs and that it is not necessary to invoke post-shock dust formation to explain the blueshifting observed in the intermediate width post-shock lines. Using a Bayesian approach, we have determined the evolution of the ejecta dust mass in SN 2005ip over 10 years presuming an ejecta dust model, with an increasing dust mass from ~10$^{-8}$ M$_{\odot}$ at 48d to a current dust mass of $\sim$0.1 M$_{\odot}$., Comment: Accepted by MNRAS, 17 pages, 11 figures. Author accepted manuscript. Accepted on 04/03/19. Deposited on 07/03/19

Published
2018
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