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2. Multilevel diffractive lens in the MWIR with extended depth-of-focus and wide field-of-view

Author

Teddy Cheung, Richard Espinola, Christopher Dunay, Marc Christophersen, Freddie Santiago, Nicole Brimhall, Syed Qadri, Tina Hayward, and Rajesh Menon

Abstract

Optics in the mid-wave-infra-red (MWIR) band are generally heavy, thick and expensive. Here, we demonstrate multi-level diffractive lenses; one designed using inverse design approaches and another using the conventional propagation phase (the Fresnel zone plate or FZP) with diameter = 25um and focal length = 25um operating at $\lambda=4\thinspace\mu$m. We fabricated the lenses by optical lithography and characterized their performance. We show that the inverse-designed MDL achieves larger depth-of-focus and better off-axis performance when compared to the the FZP at the expense of larger spot size and reduced focusing efficiencies. Both lenses are flat with thickness

Published
2023
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3. Multi-Messenger observations of the Fermi-LAT blazar 4FGL J0658.6+0636 consistent with an IceCube high-energy neutrino

Author

David R. Williams, Antoine Kouchner, K. A. Farrell, Alasdair E. Gent, V. V. Vassiliev, Fabian Schüssler, H. A. Peña-Herazo, Georgios Paraschos, R. Shang, D. S. Hanna, Q. Feng, John L. Quinn, D. Ribeiro, Daniel Nieto, A. Brill, Giacomo Bonnoli, M. Kertzman, Lucy Fortson, Yong Sheng, Olivier Hervet, T. B. Humensky, Francesco Massaro, S. O'Brien, Alessio Berti, M. J. Lang, donggeun tak, Teddy Cheung, Suvi Gezari, Joern Wilms, A. D. Falcone, P. T. Reynolds, Miguel Perez-Torres, Andrea Tramacere, Reshmi Mukherjee, G. M. Foote, Binita Hona, C. Giuri, Raniere de Menezes, P. Kaaret, I. Sadeh, Frank J. Masci, Emilio Fernandez-Garcia, W. Jin, Wystan Benbow, Uwe Bach, R. R. Prado, P. Moriarty, Jonas Heßdörfer, M. Pohl, Matthias Kadler, Steven Hämmerich, Gernot Maier, G. H. Sembroski, Andrea Gokus, R. A. Ong, M. Capasso, Ivan Agudo, Marcos Santander, C. E. McGrath, T. J. Williamson, A. J.R. Weinstein, E. Roache, A. Archer, Jorge Otero-Santos, Simone Garrappa, Alex Kraus, G. H. Gillanders, A. J. Castro-Tirado, Alexis Coleiro, Jodi Christiansen, Jamie Holder, K. Ragan, Meenakshi Rajagopal, A. N. Otte, Alessandro Paggi, K. Pfrang, Orel Gueta, Marcello Giroletti, Cristina Nanci, Javier Moldon, M. Nievas-Rosillo, Elisa Bernardini, C. Adams, Werner Colmar, Y. D. Hu, J. A. Ryan, Richard Walters, M. Lundy, Florian Eppel, Tobias Kleiner, R. Sanchez-Ramirez, J. H. Buckley, A. J. Chromey, Amy Furniss, Charlotte Ward, Konstancja Satalecka, E. Pueschel, Manel Errando, Sara Buson, S. Kumar, S. Patel, M. D. Caballero-Garcia, and Marco Ajello

Subjects
Physics, High energy, Astrophysics, Neutrino, Blazar, Fermi Gamma-ray Space Telescope
Published
2021
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4. Relativistic X‐ray jets at high redshift

Author

Doug B. Gobeille, Aneta Siemiginowska, G. Migliori, Diana M Worrall, John F. C. Wardle, Daniel A. Schwartz, Mark Birkinshaw, Herman L. Marshall, and Teddy Cheung

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Magnetic energy, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Compton scattering, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Lorentz factor, symbols.namesake, Astrophysical jet, Space and Planetary Science, 0103 physical sciences, symbols, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Microwave
Abstract

Powerful radio sources and quasars emit relativistic jets of plasma and magnetic fields that travel hundreds of kilo-parsecs, ultimately depositing energy into the intra- or inter-cluster medium. In the rest frame of the jet, the energy density of the cosmic microwave background is enhanced by the bulk Lorentz factor squared, and when this exceeds the magnetic energy density the primary loss mechanism of the relativistic electrons is via inverse Compton scattering. The microwave energy density is also enhanced by a factor (1+z)^4, which becomes important at large redshifts. We are using Chandra to survey a z>3 sub-sample of radio sources selected with 21 cm wavelength flux density > 70 mJy, and with a spectroscopic redshift. Out of the first 12 objects observed, there are two clear cases of the X-rays extending beyond the detectable radio jet., 6 pages, 4 figures. In proceedings of the IWARA 2018 conference, to be published in Astronomische Nachrichten

Published
2019
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5. A multi-band study of the remarkable jet in Quasar 4C+19.44

Author

Teddy Cheung, Aneta Siemiginowska, Svetlana G. Jorstad, Herman L. Marshall, Nicholas Lee, Diana M Worrall, Francesco Massaro, Lukasz Stawarz, Hermine Landt, Jonathan Gelbord, Daniel A. Schwartz, Yasunobu Uchiyama, C. Megan Urry, Eric S. Perlman, Alan P. Marscher, Daniel E. Harris, and Mark Birkinshaw

Subjects
Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Population, Cosmic microwave background, jets [galaxies], FOS: Physical sciences, active, galaxies: jets, quasars: individual (4C+19.44), radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, individual: 4C+19.44 [quasars], 01 natural sciences, [radiation mechanisms], 0103 physical sciences, Angular resolution, jets — galaxies, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Jet (fluid), education.field_of_study, Spectral index, non-thermal — quasars, 010308 nuclear & particles physics, Compton scattering, Quasar, non-thermal [radiation mechanisms], individual (4C+19.44) — galaxies, active [galaxies], Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present arc-second-resolution data in the radio, IR, optical and X-ray for 4C+19.44 (=PKS 1354+195), the longest and straightest quasar jet with deep X-ray observations. We report results from radio images with half to one arc-second angular resolution at three frequencies, plus HST and Spitzer data. The Chandra data allow us to measure the X-ray spectral index in 10 distinct regions along the 18 arcsec jet and compare with the radio index. The radio and X-ray spectral indices of the jet regions are consistent with a value of $\alpha =0.80$ throughout the jet, to within 2 sigma uncertainties. The X-ray jet structure to the south extends beyond the prominent radio jet and connects to the southern radio lobe, and there is extended X-ray emission in the direction of the unseen counter jet and coincident with the northern radio lobe. This jet is remarkable since its straight appearance over a large distance allows the geometry factors to be taken as fixed along the jet. Using the model of inverse Compton scattering of the cosmic microwave background (iC/CMB) by relativistic electrons, we find that the magnetic field strengths and Doppler factors are relatively constant along the jet. If instead the X-rays are synchrotron emission, they must arise from a population of electrons distinct from the particles producing the radio synchrotron spectrum., Comment: Accepted for ApJ

Published
2017
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7. High energy $\gamma$-ray emission from PSR B1259$-$63 during 2014 and 2010 periastron passages

Author

Caliandro, G. Andrea, Teddy Cheung, C. C., Li, Jian, Diego F. Torres, and Wood, Kent

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

PSR B1259$-$63/SS 2883 is a $\gamma$-ray binary system composed of a radio pulsar in a long (1236.7 days) and elliptical ($e\sim0.87$) orbit around a Be star. In its 2010 periastron passage, multiwavelength emission from radio to TeV was observed, and an unexpected GeV flare was detected by the Fermi Large Area Telescope (LAT). Here we present the results of the LAT monitoring of PSR B1259$-$63 during its most recent 2014 periastron passage. We confirm that the GeV flare is recurrent within the orbit. The comparison of the 2014 and 2010 periastron passages shows overall similarities of flare durations, average flux levels, and spectra. In contrast, the detailed time evolutions of the two flares present interesting differences. Indeed, the light curves of the two flares show both a different structure and peak energy flux ($9.6 \pm1.8 \times 10^{-10}$ erg cm$^{-2}$ s$^{-1}$ and $7.1 \pm1.3 \times 10^{-10}$ erg cm$^{-2}$ s$^{-1}$, respectively in 2010 and 2014). While the tail of the 2010 flare the flux decayed exponentially, in 2014 it persisted at a high level. The interpretation of these differences as well as of the flare themselves is subject of debate., Comment: Conference proceeding. Swift: 10 Years of Discovery, 2-5 December 2014, La Sapienza University, Rome, Italy. 6 pages, 2 figures

Published
2015

8. JD6 - The Connection between Radio Properties and High Energy Emission in AGNs

Author

Teddy Cheung and Gabriele Giovannini

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio spectrum, Astrophysical jet, Orders of magnitude (time), Space and Planetary Science, Blazar, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

While observations in the radio band are providing essential information on the innermost structures of relativistic jets in active galactic nuclei (AGN), the recent detection by Fermi of gamma-ray emission from many hundreds of blazars shows that the maximum jet power is emitted at high energies. Multi-wavelength monitoring observations further allow variability studies of the AGN spectral energy distributions over 13 orders of magnitude in frequency. The Joint Discussion offered the possibility for a comprehensive discussion of advances in the observational domain and stimulated theoretical discussion about our current understanding of jet physics., Comment: 11 pages, 5 figures, Highlights of Astronomy, Vol. 16, in press

Published
2013
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9. All-sky Medium Energy Gamma-ray Observatory: Exploring the Extreme Multimessenger Universe

Author

Julie McEnery, Alexander van der Horst, Alberto Dominguez, Alexander Moiseev, Alexandre Marcowith, Alice Harding, Amy Lien, Andrea Giuliani, Andrew Inglis, Stefano Ansoldi, Antonio Stamerra, Antonios Manousakis, Andy Strong, Cosimo Bambi, Barbara Patricelli, Matthew Baring, Juan Abel Barrio, Denis Bastieri, Brian Fields, John Beacom, Volker Beckmann, Wlodek Bednarek, Bindu Rani, Steven Boggs, Aleksey Bolotnikov, Brad Cenko, S., Jim Buckley, Brian Grefenstette, Michelle Hui, Carlotta Pittori, Chanda Prescod-Weinstein, Chris Shrader, Christian Gouiffes, Carolyn Kierans, Colleen Wilson-Hodge, Ammando, Filippo D., Daniel Castro, Daniel Kocveski, Dario Gasparrini, David Thompson, David Williams, Alessandro De Angelis, Denis Bernard, Seth Digel, Daniel Morcuende, Eric Charles, Elisabetta Bissaldi, Elizabeth Hays, Elizabeth Ferrara, Enrico Bozzo, Eric Grove, Eric Wulf, Eugenio Bottacini, Ezio Caroli, Fabian Kislat, Foteini Oikonomou, Francesco Giordano, Francesco Longo, Chris Fryer, Yasushi Fukazawa, Markos Georganopoulos, Georgia De Nolfo, Giacomo Vianello, Gottfried Kanbach, George Younes, Harsha Blumer, Dieter Hartmann, Margarita Hernanz, Hiromitsu Takahashi, Hui Li, Ivan Agudo, Igor Moskalenko, Inga Stumke, Isabelle Grenier, Jacob Smith, James Rodi, Jeremy Perkins, Joseph Gelfand, Jamie Holder, Jurgen Knodlseder, Joachim Kopp, Jean-Philippe Lenain, José-Manuel Álvarez, Jessica Metcalfe, John Krizmanic, Stephen, John B., Jack Hewitt, John Mitchell, Pat Harding, John Tomsick, Judith Racusin, Justin Finke, Oleg Kargaltsev, Klimenko, Alexei V., Henric Krawczynski, Karl Smith, Hidetoshi Kubo, Leonardo Di Venere, Lea Marcotulli, Jan Lommler, Lucas Parker, Luca Baldini, Luca Foffano, Luca Zampieri, Luigi Tibaldo, Maria Petropoulou, Marco Ajello, Manuel Meyer, Marcos López, Marc McConnell, Markus Boettcher, Martina Cardillo, Manel Martinez, Matthew Kerr, Nicola Mazziotta, M., Mattia Di Mauro, Matthew Wood, Eileen Meyer, Michael Briggs, Michaël De Becker, Michael Lovellette, Michele Doro, Sanchez-Conde, Miguel A., Michael Moss, Tsunefumi Mizuno, Marc Ribó, Kazuhiro Nakazawa, Naoko Kurahashi Neilson, Natalia Auricchio, Nicola Omodei, Uwe Oberlack, Masanori Ohno, Elena Orlando, Nepomuk Otte, Paolo Coppi, Peter Bloser, Haocheng Zhang, Philippe Laurent, Martin Pohl, Elisa Prandini, Peter Shawhan, Regina Caputo, Riccardo Campana, Riccardo Rando, Richard Woolf, Robert Johnson, Roberto Mignani, Roland Walter, Roopesh Ojha, Rui Curado da Silva, Stefano Dietrich, Stefan Funk, Silvia Zane, Sonia Anton, Sara Buson, Sara Cutini, Pablo Saz Parkinson, Richard Schirato, Sean Griffin, Kaufmann, S., Lukasz Stawarz, Stefano Ciprini, Stefano Del Sordo, Sam Jones, Sylvain Guiriec, Hiro Tajima, Teddy Cheung, Lih-Sin The, Tonia Venters, Troy Porter, Tim Linden, Ulisses Barres, Paliya, Vaidehi S., Vladimir Bozhilov, Tom Vestrand, Vincent Tatischeff, Wenlei Chen, Xilu Wang, Yasuyuki Tanaka, Lucas Uhm, Bing Zhang, Stephan Zimmer, Andreas Zoglauer, Zorawar Wadiasingh, NASA Goddard Space Flight Center (GSFC), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Clemson University, Centros de Laseres Pulsados, Universidade de Aveiro, Istituto Nazionale di Fisica Nucleare [Pisa] (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Fudan University [Shanghai], Rice University [Houston], Centro Brasileiro de Pesquisas Físicas (CBPF), Ministério da Ciência e Tecnologia, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), Istituto Nazionale di Fisica Nucleare, sezione di Bari (INFN, sezione di Bari), Los Alamos National Laboratory (LANL), West Virginia University [Morgantown], North-West University [South Aftrica] (NWU), University of California [San Diego] (UC San Diego), University of California (UC), Brookhaven National Laboratory [Upton, NY] (BNL), UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY)-U.S. Department of Energy [Washington] (DOE), Софийски университет = Sofia University, Université de Genève = University of Geneva (UNIGE), University of Alabama in Huntsville (UAH), Washington University in Saint Louis (WUSTL), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, SLAC National Accelerator Laboratory (SLAC), Stanford University, Naval Research Laboratory (NRL), Agenzia Spaziale Italiana (ASI), Yale University [New Haven], Universidade de Coimbra [Coimbra], ASI Science Data Center (ASDC), Italian Space Agency, Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Université de Liège, CNR Institute of Atmospheric Sciences and Climate (ISAC), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), University of Illinois System, Hiroshima University, Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), New York University [New York] (NYU), NYU System (NYU), University of Maryland [Baltimore County] (UMBC), University of Maryland System, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), California Institute of Technology (CALTECH), 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), The George Washington University (GW), University of North Florida [Jacksonville] (UNF), University of Delaware [Newark], NASA Marshall Space Flight Center (MSFC), University of California [Santa Cruz] (UC Santa Cruz), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Universidad Autónoma de Chiapas, University of New Hampshire (UNH), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Kyoto University, Drexel University, 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), Stockholm University, Università degli studi di Trieste = University of Trieste, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Argonne National Laboratory [Lemont] (ANL), Nagoya University, European Southern Observatory (ESO), US Naval Observatory (US NAVAL OBSERVATORY), US Naval Observatory, Deutsches Elektronen-Synchrotron [Hamburg] (DESY), Princeton University, Universitat de Barcelona, Universitat de Barcelona (UB), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), University of Maryland [College Park], Uniwersytet Jagielloński w Krakowie = Jagiellonian University (UJ), Max-Planck-Institut für Extraterrestrische Physik (MPE), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), University College of London [London] (UCL), University of Nevada [Las Vegas] (WGU Nevada), Purdue University [West Lafayette], Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), University of California, U.S. Department of Energy [Washington] (DOE)-UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), University of Sofia, Université de Genève (UNIGE), Smithsonian Institution-Harvard University [Cambridge], Consiglio Nazionale delle Ricerche (CNR), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of California [Santa Cruz] (UCSC), 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), Kyoto University [Kyoto], 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)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Trieste, 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), University of California [Berkeley], Complutense University of Madrid (UCM), National Institute for Nuclear Physics (INFN), Brookhaven National Laboratory [Upton] (BNL), Stony Brook University [SUNY] (SBU), Harvard University [Cambridge]-Smithsonian Institution, Stanford Linear Accelerator Center (SLAC), Stanford University [Stanford], Istituto di Radioastronomia (IRA), Friedrich-Alexander Universitaet Erlangen-Nuernberg, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM PS1), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Univ. Paris-Sud, Commissariat à l'Énergie Atomique et aux Énergies Alternatives (CEA) - Grenoble, George Washington University (GW), University of North Florida, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-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), Universitat Autònoma de Barcelona [Barcelona] (UAB), and Jagiellonian University [Krakow] (UJ)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The All-sky Medium Energy Gamma-ray Observatory (AMEGO) is a probe class mission concept that will provide essential contributions to multimessenger astrophysics in the late 2020s and beyond. AMEGO combines high sensitivity in the 200 keV to 10 GeV energy range with a wide field of view, good spectral resolution, and polarization sensitivity. Therefore, AMEGO is key in the study of multimessenger astrophysical objects that have unique signatures in the gamma-ray regime, such as neutron star mergers, supernovae, and flaring active galactic nuclei. The order-of-magnitude improvement compared to previous MeV missions also enables discoveries of a wide range of phenomena whose energy output peaks in the relatively unexplored medium-energy gamma-ray band., Comment: Astro2020 APC White Paper Updated to make small change to author list in metadata

10. Nova Mon 2012 resolved as a double radio source

Author

Stewart Eyres, Nirupam Roy, Laura Chomiuk, Thomas Nelson, Bode, M. F., Brien, T. O., Jun Yang, Zsolt Paragi, Teddy Cheung, Rupen, Michael P., Taylor, Gregory B., Sokoloski, J. L., Koji Mukai, Jennifer Weston, and Mioduszewski, Amy J.

Subjects
Nova, Radio astronomy
Abstract

Nova Mon 2012 was first reported as a gamma-ray transient, subsequently associated with an optical nova and detected in the radio and X-ray/UV. Following the dramatic brightening at high radio frequencies, on September 18 we obtained e-VLBI radio observations of Nova Mon 2012 at 5.0 GHz using eight telescopes of the European VLBI Network (EVN), providing resolution of 6x8 milli-arcseconds.

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