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1. The MegaMapper: A Stage-5 Spectroscopic Instrument Concept for the Study of Inflation and Dark Energy

Author

Schlegel, David J., Kollmeier, Juna A., Aldering, Greg, Bailey, Stephen, Baltay, Charles, Bebek, Christopher, BenZvi, Segev, Besuner, Robert, Blanc, Guillermo, Bolton, Adam S., Bonaca, Ana, Bouri, Mohamed, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, Crane, Jeffrey, Demina, Regina, DeRose, Joseph, Dey, Arjun, Doel, Peter, Fan, Xiaohui, Ferraro, Simone, Finkbeiner, Douglas, Font-Ribera, Andreu, Gontcho, Satya Gontcho A, Green, Daniel, Gutierrez, Gaston, Guy, Julien, Heetderks, Henry, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kremin, Anthony, Kronig, Luzius, Konidaris, Nick, Lahav, Ofer, Lampton, Michael L., Landriau, Martin, Lang, Dustin, Leauthaud, Alexie, Levi, Michael E., Liguori, Michele, Linder, Eric V., Magneville, Christophe, Martini, Paul, Mateo, Mario, McDonald, Patrick, Miller, Christopher J., Moustakas, John, Myers, Adam D., Mulchaey, John, Newman, Jeffrey A., Nugent, Peter E., Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Piro, Antonella Palmese Anthony L., Poppett, Claire, Prochaska, Jason X., Pullen, Anthony R., Rabinowitz, David, Raichoor, Anand, Ramirez, Solange, Rix, Hans-Walter, Ross, Ashley J., Samushia, Lado, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Shectman, Stephen A., Schlafly, Edward F., Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Slosar, Anže, Soares-Santos, Marcelle, Tarlé, Greg, Thompson, Ian, Valluri, Monica, Wechsler, Risa H., White, Martin, Wilson, Michael J., Yèche, Christophe, Zaritsky, Dennis, Zhou, Rongpu, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
High Energy Physics - Experiment (hep-ex), DESI, galaxy: redshift, target: density, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, Astrophysics - Instrumentation and Methods for Astrophysics, dark energy, Instrumentation and Methods for Astrophysics (astro-ph.IM), High Energy Physics - Experiment
Abstract

In this white paper, we present the MegaMapper concept. The MegaMapper is a proposed ground-based experiment to measure Inflation parameters and Dark Energy from galaxy redshifts at $2, Comment: Contributed White Paper to Snowmass 2021. arXiv admin note: substantial text overlap with arXiv:1907.11171. text overlap with arXiv:2209.03585

Published
2022

2. 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

3. KM3NeT/ARCA expectations in view of a novel multimessenger study of starburst galaxies

Author

Marinelli, A., Ambrosone, A., Ibnsalih, W. I., Miele, G., Migliozzi, P., Pisanti, O., Sharma, A., Ageron, M., Aiello, S., Albert, A., Alshamsi, M., Alves Garre, S., Aly, Z., Ameli, F., Andre, M., Androulakis, G., Anghinolfi, M., Anguita, M., Anton, G., Ardid, M., Ardid, S., Assal, W., Aublin, J., Bagatelas, C., Baret, B., Basegmez Du Pree, S., Bendahman, M., Benfenati, F., Berbee, E., Van Den Berg, A. M., Bertin, V., Beurthey, S., Van Beveren, V., Biagi, S., Billault, M., Bissinger, M., Boettcher, M., Bou Cabo, M., Boumaaza, J., Bouta, M., Boutonnet, C., Bouvet, G., Bouwhuis, M., Bozza, C., Branzas, H., Bruijn, R., Brunner, J., Bruno, R., Buis, E., Buompane, R., Busto, J., Caiffi, B., Caillat, L., Calvo, D., Campion, S., Capone, A., Carduner, H., Carretero, V., Castaldi, P., Celli, S., Cereseto, R., Chabab, M., Champion, C., Chau, N., Chen, A., Cherubini, S., Chiarella, V., Chiarusi, T., Circella, M., Cocimano, R., Coelho, J. A. B., Coleiro, A., Colomer Molla, M., Colonges, S., Coniglione, R., Cosquer, A., Coyle, P., Cresta, M., Creusot, A., Cruz, A., Cuttone, G., D'Amico, A., Dallier, R., De Martino, B., De Palma, M., Di Palma, I., Diaz, A. F., Diego-Tortosa, D., Distefano, C., Domi, A., Donzaud, C., Dornic, D., Dorr, M., Drouhin, D., Eberl, T., Eddyamoui, A., Van Eeden, T., Van Eijk, D., El Bojaddaini, I., Eljarrari, H., Elsaesser, D., Enzenhofer, A., Espinosa, V., Fermani, P., Ferrara, G., Filipovic, M. D., Filippini, F., Fransen, J., Fusco, L. A., Gajanana, D., Gal, T., Garcia Mendez, J., Garcia Soto, A., Garcon, E., Garufi, F., Gatius, C., Geisselbrecht, N., Gialanella, L., Giorgio, E., Gozzini, S. R., Gracia, R., Graf, K., Grella, G., Guderian, D., Guidi, C., Guillon, B., Gutierrez, M., Haefner, J., Hallmann, S., Hamdaoui, H., Van Haren, H., Heijboer, A., Hekalo, A., Hennig, L., Henry, S., Hernandez-Rey, J. J., Hofestadt, J., Huang, F., Idrissi Ibnsalih, W., Ilioni, A., Illuminati, G., James, C. W., Janezashvili, D., Jansweijer, P., De Jong, M., De Jong, P., Jung, B. J., Kadler, M., Kalaczynski, P., Kalekin, O., Katz, U. F., Kayzel, F., Keller, P., Khan Chowdhury, N. R., Kistauri, G., Van Der Knaap, F., Kooijman, P., Kouchner, A., Kreter, M., Kulikovskiy, V., Labalme, M., Lagier, P., Lahmann, R., Lamare, P., Lamoureux, M., Larosa, G., Lastoria, C., Laurence, J., Lazo, A., Le Breton, R., Le Guirriec, E., Le Stum, S., Lehaut, G., Leonardi, O., Leone, F., Leonora, E., Lerouvillois, C., Lesrel, J., Lessing, N., Levi, G., Lincetto, M., Lindsey Clark, M., Lipreau, T., Llorens Alvarez, C., Lonardo, A., Longhitano, F., Lopez-Coto, D., Lumb, N., Maderer, L., Majumdar, J., Manczak, J., Margiotta, A., Marini, A., Markou, C., Martin, L., Martinez-Mora, J. A., Martini, A., Marzaioli, F., Mastroianni, S., Melis, K. W., Migneco, E., Mijakowski, P., Miranda, L. S., Mollo, C. M., Mongelli, M., Moussa, A., Muller, R., Musico, P., Musumeci, M., Nauta, L., Navas, S., Nicolau, C. A., Nkosi, B., Fearraigh, B. O., O'Sullivan, M., Orlando, A., Ottonello, G., Ottonello, S., Palacios Gonzalez, J., Papalashvili, G., Papaleo, R., Pastore, C., Paun, A. M., Pavalas, G. E., Pellegrini, G., Pellegrino, C., Perrin-Terrin, M., Pestel, V., Piattelli, P., Pieterse, C., Poire, C., Popa, V., Pradier, T., Pratolongo, F., Probst, I., Puhlhofer, G., Pulvirenti, S., Quemener, G., Randazzo, N., Rapicavoli, A., Razzaque, S., Real, D., Reck, S., Riccobene, G., Rigalleau, L., Romanov, A., Rovelli, A., Royon, J., Salesa Greus, F., Samtleben, D. F. E., Sanchez Losa, A., Sanguineti, M., Santangelo, A., Santonocito, D., Sapienza, P., Schmelling, J., Schnabel, J., Schneider, M. F., Schumann, J., Schutte, H. M., Seneca, J., Sgura, I., Shanidze, R., Sinopoulou, A., Spisso, B., Spurio, M., Stavropoulos, D., Steijger, J., Stellacci, S. M., Taiuti, M., Tatone, F., Tayalati, Y., Tenllado, E., Tezier, D., Thakore, T., Theraube, S., Thiersen, H., Timmer, P., Tingay, S., Tsagkli, S., Tsourapis, V., Tzamariudaki, E., Tzanetatos, D., Valieri, C., Van Elewyck, V., Vasileiadis, G., Versari, F., Viola, S., Vivolo, D., De Wasseige, G., Wilms, J., Wojaczynski, R., De Wolf, E., Yousfi, T., Zavatarelli, S., Zegarelli, A., Zito, D., Zornoza, J. D., Zuniga, J., Zywucka, N., Research unit Astroparticle Physics, Marinelli, A., Ambrosone, A., Ibnsalih, W. I., Miele, G., Migliozzi, P., Pisanti, O., Sharma, A., Ageron, M., Aiello, S., Albert, A., Alshamsi, M., Alves Garre, S., Aly, Z., Ameli, F., Andre, M., Androulakis, G., Anghinolfi, M., Anguita, M., Anton, G., Ardid, M., Ardid, S., Assal, W., Aublin, J., Bagatelas, C., Baret, B., Basegmez Du Pree, S., Bendahman, M., Benfenati, F., Berbee, E., Van Den Berg, A. M., Bertin, V., Beurthey, S., Van Beveren, V., Biagi, S., Billault, M., Bissinger, M., Boettcher, M., Bou Cabo, M., Boumaaza, J., Bouta, M., Boutonnet, C., Bouvet, G., Bouwhuis, M., Bozza, C., Branzas, H., Bruijn, R., Brunner, J., Bruno, R., Buis, E., Buompane, R., Busto, J., Caiffi, B., Caillat, L., Calvo, D., Campion, S., Capone, A., Carduner, H., Carretero, V., Castaldi, P., Celli, S., Cereseto, R., Chabab, M., Champion, C., Chau, N., Chen, A., Cherubini, S., Chiarella, V., Chiarusi, T., Circella, M., Cocimano, R., Coelho, J. A. B., Coleiro, A., Colomer Molla, M., Colonges, S., Coniglione, R., Cosquer, A., Coyle, P., Cresta, M., Creusot, A., Cruz, A., Cuttone, G., D'Amico, A., Dallier, R., De Martino, B., De Palma, M., Di Palma, I., Diaz, A. F., Diego-Tortosa, D., Distefano, C., Domi, A., Donzaud, C., Dornic, D., Dorr, M., Drouhin, D., Eberl, T., Eddyamoui, A., Van Eeden, T., Van Eijk, D., El Bojaddaini, I., Eljarrari, H., Elsaesser, D., Enzenhofer, A., Espinosa, V., Fermani, P., Ferrara, G., Filipovic, M. D., Filippini, F., Fransen, J., Fusco, L. A., Gajanana, D., Gal, T., Garcia Mendez, J., Garcia Soto, A., Garcon, E., Garufi, F., Gatius, C., Geisselbrecht, N., Gialanella, L., Giorgio, E., Gozzini, S. R., Gracia, R., Graf, K., Grella, G., Guderian, D., Guidi, C., Guillon, B., Gutierrez, M., Haefner, J., Hallmann, S., Hamdaoui, H., Van Haren, H., Heijboer, A., Hekalo, A., Hennig, L., Henry, S., Hernandez-Rey, J. J., Hofestadt, J., Huang, F., Idrissi Ibnsalih, W., Ilioni, A., Illuminati, G., James, C. W., Janezashvili, D., Jansweijer, P., De Jong, M., De Jong, P., Jung, B. J., Kadler, M., Kalaczynski, P., Kalekin, O., Katz, U. F., Kayzel, F., Keller, P., Khan Chowdhury, N. R., Kistauri, G., Van Der Knaap, F., Kooijman, P., Kouchner, A., Kreter, M., Kulikovskiy, V., Labalme, M., Lagier, P., Lahmann, R., Lamare, P., Lamoureux, M., Larosa, G., Lastoria, C., Laurence, J., Lazo, A., Le Breton, R., Le Guirriec, E., Le Stum, S., Lehaut, G., Leonardi, O., Leone, F., Leonora, E., Lerouvillois, C., Lesrel, J., Lessing, N., Levi, G., Lincetto, M., Lindsey Clark, M., Lipreau, T., Llorens Alvarez, C., Lonardo, A., Longhitano, F., Lopez-Coto, D., Lumb, N., Maderer, L., Majumdar, J., Manczak, J., Margiotta, A., Marini, A., Markou, C., Martin, L., Martinez-Mora, J. A., Martini, A., Marzaioli, F., Mastroianni, S., Melis, K. W., Migneco, E., Mijakowski, P., Miranda, L. S., Mollo, C. M., Mongelli, M., Moussa, A., Muller, R., Musico, P., Musumeci, M., Nauta, L., Navas, S., Nicolau, C. A., Nkosi, B., Fearraigh, B. O., O'Sullivan, M., Orlando, A., Ottonello, G., Ottonello, S., Palacios Gonzalez, J., Papalashvili, G., Papaleo, R., Pastore, C., Paun, A. M., Pavalas, G. E., Pellegrini, G., Pellegrino, C., Perrin-Terrin, M., Pestel, V., Piattelli, P., Pieterse, C., Poire, C., Popa, V., Pradier, T., Pratolongo, F., Probst, I., Puhlhofer, G., Pulvirenti, S., Quemener, G., Randazzo, N., Rapicavoli, A., Razzaque, S., Real, D., Reck, S., Riccobene, G., Rigalleau, L., Romanov, A., Rovelli, A., Royon, J., Salesa Greus, F., Samtleben, D. F. E., Sanchez Losa, A., Sanguineti, M., Santangelo, A., Santonocito, D., Sapienza, P., Schmelling, J., Schnabel, J., Schneider, M. F., Schumann, J., Schutte, H. M., Seneca, J., Sgura, I., Shanidze, R., Sinopoulou, A., Spisso, B., Spurio, M., Stavropoulos, D., Steijger, J., Stellacci, S. M., Taiuti, M., Tatone, F., Tayalati, Y., Tenllado, E., Tezier, D., Thakore, T., Theraube, S., Thiersen, H., Timmer, P., Tingay, S., Tsagkli, S., Tsourapis, V., Tzamariudaki, E., Tzanetatos, D., Valieri, C., Van Elewyck, V., Vasileiadis, G., Versari, F., Viola, S., Vivolo, D., De Wasseige, G., Wilms, J., Wojaczynski, R., De Wolf, E., Yousfi, T., Zavatarelli, S., Zegarelli, A., Zito, D., Zornoza, J. D., Zuniga, J., Zywucka, N., 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 Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Groupe de Recherche en Physique des Hautes Energies (GRPHE), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-IUT de Colmar, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), 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 de physique subatomique et des technologies associées (SUBATECH), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), 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), KM3NeT, Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut Universitaire de Technologie de Colmar, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), neutrino: energy: high, Astrophysics::High Energy Astrophysical Phenomena, target: density, FOS: Physical sciences, Particle detectors, Astrophysics::Cosmology and Extragalactic Astrophysics, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], density: high, KM3NeT, particle source, Instrumentation, Astrophysics::Galaxy Astrophysics, Mathematical Physics, High Energy Astrophysical Phenomena (astro-ph.HE), mass: solar, Cherenkov detectors, central region, Simulation methods and programs, star: formation, acceleration, sensitivity, messenger, gas: target, cosmic radiation, High Energy Physics::Experiment, galaxy, Particle detector, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Cherenkov detector
Abstract

Starburst galaxies (SBGs) and more in general starforming galaxies represent a class of galaxies with a high star formation rate (up to 100 solar masses/year). Despite their low luminosity, they can 19 be considered as guaranteed "factories" of high energy neutrinos, being "reservoirs" of accelerated 20 cosmic rays and hosting a high density target gas in the central region. In this contribution 21 we present a novel multimessenger study of these sources and the possibility of observing their 22 neutrino signals with the KM3NeT/ARCA telescope. The differential sensitivity for different SBG 23 scenarios is reported considering track-like neutrino events in the 100 GeV-100 PeV energy range., Presented at the 9th Very Large Volume Neutrino Telescope Workshop (VLVnT 2021), Prepared for submission to JINST

Published
2021

4. Disentangling hadronic from leptonic emission in the composite SNR G326.3$-$1.8

Author

Jean Ballet, J. Devin, J. Schmid, Fabio Acero, 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 AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
lepton, Astrophysics::High Energy Astrophysical Phenomena, target: density, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Pulsar wind nebula, GLAST, gamma rays: ISM, cosmic rays, Pulsar, 0103 physical sciences, supernova, cloud, Angular resolution, composite, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, acceleration of particles, ISM: supernova remnants, pulsar, supernova remnants, Astroparticle physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, Computer Science::Information Retrieval, gamma-rays: observations, Astronomy and Astrophysics, shock waves, Supernova, Automatic Keywords, angular resolution, astroparticle physics, gamma ray, 13. Climate action, Space and Planetary Science, spectral, hadron, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Lepton
Abstract

Context. G326.3−1.8 (also known as MSH 15−56) has been detected in radio as middle-aged composite supernova remnant (SNR) consisting of an SNR shell and a pulsar wind nebula (PWN) that has been crushed by the SNR reverse shock. Previous γ-ray studies of SNR G326.3−1.8 revealed bright and extended emission with uncertain origin. Understanding the nature of the γ-ray emission allows probing the population of high-energy particles (leptons or hadrons), but can be challenging for sources of small angular extent. Aims. With the recent Fermi Large Area Telescope data release Pass 8, which provides increased acceptance and angular resolution, we investigate the morphology of this SNR to disentangle the PWN from the SNR contribution. In particular, we take advantage of the new possibility to filter events based on their angular reconstruction quality. Methods. We performed a morphological and spectral analysis from 300 MeV to 300 GeV. We used the reconstructed events with the best angular resolution (PSF3 event type) to separately investigate the PWN and the SNR emissions, which is crucial to accurately determine the spectral properties of G326.3−1.8 and understand its nature. Results. The centroid of the γ-ray emission evolves with energy and is spatially coincident with the radio PWN at high energies (E > 3 GeV). The morphological analysis reveals that a model considering two contributions from the SNR and the PWN reproduces the γ-ray data better than a single-component model. The associated spectral analysis using power laws shows two distinct spectral features, a softer spectrum for the remnant (Γ = 2.17 ± 0.06) and a harder spectrum for the PWN (Γ = 1.79 ± 0.12), consistent with hadronic and leptonic origin for the SNR and the PWN, respectively. Focusing on the SNR spectrum, we use one-zone models to derive some physical properties, and we find in particular, that the emission is best explained with a hadronic scenario in which the high target density is provided by radiative shocks in H I clouds struck by the SNR.

Published
2018

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