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Title: Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Abstract

We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX J1713.7−3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very high energy (VHE) gamma rays. Special attention is paid to exploring possible spatial (anti)correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H i emission. We present a series of simulated images of RX J1713.7−3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the nonthermal X-ray emission observed by XMM-Newton , whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H i observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (i.e., hadronic versus leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to achieve various proposed scientific goals by observing this important cosmic particle accelerator.

Authors:
 [1]; ;  [2];  [3];  [4];  [5];  [6]; ;  [7];  [8];  [9];  [10];  [11];  [12];  [13];  [14];  [15];
+ Show Author Affiliations
  1. CEA/IRFU/SAp, CEA Saclay, Bat 709, Orme des Merisiers, F-91191 Gif-sur-Yvette (France)
  2. Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, I-50125 Firenze (Italy)
  3. LUTH and GEPI, Observatoire de Paris, CNRS, PSL Research University, 5 place Jules Janssen, F-92190, Meudon (France)
  4. INAF—Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040, Monteporzio Catone (Italy)
  5. INFN Sezione di Napoli, Via Cintia, ed. G, I-80126 Napoli (Italy)
  6. Department of Physics and Centre for Advanced Instrumentation, Durham University, South Road, Durham DH1 3LE (United Kingdom)
  7. Grupo de Altas Energías, Universidad Complutense de Madrid., Av Complutense s/n, E-28040 Madrid (Spain)
  8. Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashi-wanoha, Kashiwa, Chiba 277-8582 (Japan)
  9. School of Physics, University of New South Wales, Sydney NSW 2052 (Australia)
  10. University of Namibia, Department of Physics, 340 Mandume Ndemufayo Ave., Pioneerspark Windhoek (Namibia)
  11. School of Physics and Astronomy, Monash University, Melbourne, Victoria 3800 (Australia)
  12. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904 1098 XH Amsterdam (Netherlands)
  13. Department of Physics, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan)
  14. Riken, Institute of Physical and Chemical Research, 2-1 Hirosawa, Wako, Saitama, 351-0198 (Japan)
  15. Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02180 (United States)
Publication Date:
OSTI Identifier:
22663628
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 840; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCELERATORS; CARBON; CARBON MONOXIDE; CHERENKOV COUNTERS; COSMIC RADIATION; ELECTRONS; EMISSION; GAMMA RADIATION; PROTONS; RELATIVISTIC RANGE; SIMULATION; SPATIAL DISTRIBUTION; SPECTRA; SUPERNOVA REMNANTS; TELESCOPES; WAVELENGTHS; X RADIATION

Citation Formats

Acero, F., Aloisio, R., Amato, E., Amans, J., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Barrio, J. A., Asano, K., Ashley, M., Backes, M., Balazs, C., Balzer, A., Bamba, A., Barkov, M., Benbow, W., Bernlöhr, K., E-mail: sano@a.phys.nagoya-u.ac.jp, E-mail: nakamori@sci.kj.yamagata-u.ac.jp, and others, and. Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA6D67.
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Acero, F., Aloisio, R., Amato, E., Amans, J., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Barrio, J. A., Asano, K., Ashley, M., Backes, M., Balazs, C., Balzer, A., Bamba, A., Barkov, M., Benbow, W., Bernlöhr, K., E-mail: sano@a.phys.nagoya-u.ac.jp, E-mail: nakamori@sci.kj.yamagata-u.ac.jp, & others, and. Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946. United States. https://doi.org/10.3847/1538-4357/AA6D67
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Acero, F., Aloisio, R., Amato, E., Amans, J., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Barrio, J. A., Asano, K., Ashley, M., Backes, M., Balazs, C., Balzer, A., Bamba, A., Barkov, M., Benbow, W., Bernlöhr, K., E-mail: sano@a.phys.nagoya-u.ac.jp, E-mail: nakamori@sci.kj.yamagata-u.ac.jp, and others, and. 2017. "Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946". United States. https://doi.org/10.3847/1538-4357/AA6D67.
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@article{osti_22663628,
title = {Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946},
author = {Acero, F. and Aloisio, R. and Amato, E. and Amans, J. and Antonelli, L. A. and Aramo, C. and Armstrong, T. and Arqueros, F. and Barrio, J. A. and Asano, K. and Ashley, M. and Backes, M. and Balazs, C. and Balzer, A. and Bamba, A. and Barkov, M. and Benbow, W. and Bernlöhr, K., E-mail: sano@a.phys.nagoya-u.ac.jp, E-mail: nakamori@sci.kj.yamagata-u.ac.jp and others, and},
abstractNote = {We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX J1713.7−3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very high energy (VHE) gamma rays. Special attention is paid to exploring possible spatial (anti)correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H i emission. We present a series of simulated images of RX J1713.7−3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the nonthermal X-ray emission observed by XMM-Newton , whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H i observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (i.e., hadronic versus leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to achieve various proposed scientific goals by observing this important cosmic particle accelerator.},
doi = {10.3847/1538-4357/AA6D67},
url = {https://www.osti.gov/biblio/22663628}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 840,
place = {United States},
year = {Wed May 10 00:00:00 EDT 2017},
month = {Wed May 10 00:00:00 EDT 2017}
}
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Journal Article:
https://doi.org/10.3847/1538-4357/AA6D67
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