Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

Berezhko, E. G.; Ksenofontov, L. T.; Völk, H. J.

doi:10.1088/0004-637x/732/1/58

Cited by 28 publications

(44 citation statements)

References 39 publications

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“…These are summarised in Table 6 under two assumptions for the photon index over 1-10 GeV. For SN1987A, our upper limit on the 1-10 GeV flux is not constraining when compared to the predictions made by Berezhko et al (2011); our limit is a factor of 3 above their predicted flux for 2010 and remains above the maximum flux predicted for 2030. For 30 Dor C, our upper limit is not constraining either when compared to the γ-ray emission models considered in Abramowski et al (2015); our limit is a factor of 6 above the most optimistic prediction of the hadronic model.…”

Section: Upper Limits On Selected Objectsmentioning

confidence: 76%

“…This is the case of superbubble 30 Doradus C (a rare superbubble with non-thermal emission, recently detected at TeV energies with H.E.S.S. ; see Abramowski et al 2015;Yamaguchi et al 2010), or SN 1987A (the closest supernova in modern times, predicted to be accelerating particles and to be increasingly shining in γ-rays; see Berezhko et al 2011). Another possible source of GeV emission was N 11, the second most active star-forming region of the LMC after 30 Doradus, and maybe an older version of it (Rosado et al 1996;Walborn & Parker 1992).…”

Section: Upper Limits On Selected Objectsmentioning

confidence: 98%

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Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

Ackermann¹,

Albert²,

Atwood³

et al. 2016

A&A

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Context. The nearby Large Magellanic Cloud (LMC) provides a rare opportunity of a spatially resolved view of an external star-forming galaxy in γ-rays. The LMC was detected at 0.1-100 GeV as an extended source with CGRO/EGRET and using early observations with the Fermi-LAT. The emission was found to correlate with massive star-forming regions and to be particularly bright towards 30 Doradus. Aims. Studies of the origin and transport of cosmic rays (CRs) in the Milky Way are frequently hampered by line-of-sight confusion and poor distance determination. The LMC offers a complementary way to address these questions by revealing whether and how the γ-ray emission is connected to specific objects, populations of objects, and structures in the galaxy. Methods. We revisited the γ-ray emission from the LMC using about 73 months of Fermi-LAT P7REP data in the 0.2-100 GeV range. We developed a complete spatial and spectral model of the LMC emission, for which we tested several approaches: a simple geometrical description, template-fitting, and a physically driven model for CR-induced interstellar emission. Results. In addition to identifying PSR J0540−6919 through its pulsations, we find two hard sources positionally coincident with plerion N 157B and supernova remnant N 132D, which were also detected at TeV energies with H.E.S.S. We detect an additional soft source that is currently unidentified. Extended emission dominates the total flux from the LMC. It consists of an extended component of about the size of the galaxy and additional emission from three to four regions with degree-scale sizes. If it is interpreted as CRs interacting with interstellar gas, the large-scale emission implies a large-scale population of ∼1-100 GeV CRs with a density of ∼30% of the local Galactic value. On top of that, the three to four small-scale emission regions would correspond to enhancements of the CR density by factors 2 to 6 or higher, possibly more energetic and younger populations of CRs compared to the large-scale population. An alternative explanation is that this is emission from an unresolved population of at least two dozen objects, such as pulsars and their nebulae or supernova remnants. This small-scale extended emission has a spatial distribution that does not clearly correlate with known components of the LMC, except for a possible relation to cavities and supergiant shells. Conclusions. The Fermi-LAT GeV observations allowed us to detect individual sources in the LMC. Three of the newly discovered sources are associated with rare and extreme objects. The 30 Doradus region is prominent in GeV γ-rays because PSR J0540−6919 and N 157B are strong emitters. The extended emission from the galaxy has an unexpected spatial distribution, and observations at higher energies and in radio may help to clarify its origin.

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Section: Upper Limits On Selected Objectsmentioning

confidence: 76%

Section: Upper Limits On Selected Objectsmentioning

confidence: 98%

Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

Ackermann¹,

Albert²,

Atwood³

et al. 2016

A&A

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“…Last but not least, the unique object SN 1987A is, despite theoretical prediction (e.g. [115]), not detected, which constrains the theoretical framework of particle acceleration in very young SNRs. For first time individual, stellar-like, cosmic-ray accelerators are identified in an external galaxy.…”

Section: Powerful Stellar-like Emitters In the Lmcmentioning

confidence: 78%

The Very High Energy Sky from ~ 20 GeV to Hundreds of TeV - Selected Highlights

Naurois

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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After nearly a decade of operation, the three major arrays of atmospheric Cherenkov telescopes have revolutionized our view of the Very High Energy Universe, unveiling more than 100 sources of various types. MAGIC, consisting of two 17 m diameter telescopes on the Canary island of La Palma, and VERITAS, with four 12 m telescopes installed in southern Arizona, USA, have primarily explored the extragalactic sky, where the majority of the sources are active galactic nuclei (AGN), with γ-ray emission originating in their relativistic jets. In July 2014 MAGIC discovered the most distant source of very high energy γ rays, the gravitationally lensed blazar S3 0218 residing at the redshift of z = 0.944. The flat spectrum radio quasar PKS 1441+25 (z = 0.939), observed by MAGIC & VERITAS in 2015, showed a strong flaring activity over a time span of several weeks. Rapid variability from various BL Lacertae objects, down to minute timescales, has been observed by the three experiments, and measurement of their high-energy spectra allows the level of extragalactic background light to be constrained. Since the commissioning of the fifth, large (28 m diameter) telescope in December 2012, H.E.S.S.-II is the only array operating telescopes of different sizes together ("hybrid array "). The largest Cerenkov telescope ever built, CT5, provides an energy threshold of ∼ 20 GeV. With its broad energy range, H.E.S.S. explored the Galactic Plane with unprecedented sensitivity. The legacy release of the H.E.S.S. Galactic Plane Survey, consisting of 2800 hours of observations of the Galactic disk, reveals major new results. This is the first high-resolution (∼ 0.1 deg) sensitive (∼ 2% Crab Nebula point-source sensitivity) survey of the Milky Way in VHE γ rays. The Milky Way harbors a large variety of high energy sources of various types. In recent years, deep observations of several key Galactic regions of utmost importance for this field have been conducted by the three experiments. Among them are the Galactic Center region and its halo (particularly relevant for dark matter searches), the Cygnus region and its mysterious Milagro sources, the Crab Nebula and pulsar (surprisingly showing pulsed emission up to above 1 TeV), the iconic γ-ray supernova remnant RX J1713.7-3946 and other SNRs such as Tycho, the Vela pulsar and several binary systems such as LS 5039, PSR B1259-63, HESS J0632+057 and LS I +61 • 303. Joint observations on several of these objects proved to be the most efficient way to understand their nature. A deep observation of the Large Magellanic Cloud revealed, for the first time, spectacular and powerful accelerators of stellar origin outside our own galaxy. Highlights of these observations with H.E.S.S., MAGIC and VERITAS have been presented and discussed at the conference.

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“…The present work is a critical re-examination and extension of the studies by Berezhko & Ksenofontov (2000, 2006 and Berezhko et al (2011)(referred to as BKV11 in the following) concerning the properties of the nonthermal emission of SN 1987A. As in those previous investigations, our framework is a nonlinear kinetic theory of cosmic-ray (CR) acceleration in SN remnants (SNRs).…”

Section: Introductionmentioning

confidence: 89%

Re-Examination of the Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

Berezhko

Ksenofontov

Völk

2015

ApJ

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A nonlinear kinetic theory, combining cosmic-ray (CR) acceleration in supernova remnants (SNRs) with their gas dynamics, is used to re-examine the nonthermal properties of the remnant of SN 1987A for an extended evolutionary period of 5-50 yr. This spherically symmetric model is approximately applied to the different features of the SNR which consist of (i) a blue supergiant wind and bubble, and (ii) of the swept-up red supergiant (RSG) wind structures in the form of an H II region, an equatorial ring (ER), and an hourglass region. The RSG wind involves a mass loss rate that decreases significantly with elevation above and below the equatorial plane. The model adapts recent threedimensional hydrodynamical simulations by Potter et al. in 2014 that use a significantly smaller ionized mass of the ER than assumed in the earlier studies by the present authors. The SNR shock recently swept up the ER, which is the densest region in the immediate circumstellar environment. Therefore, the expected gamma-ray energy flux density at TeV energies in the current epoch has already reached its maximal value of ∼ 10 −13 erg cm −2 s −1 . This flux should decrease by a factor of about two over the next 10 years. Subject headings: acceleration of particles -ISM: individual objects (SN 1987A) -ISM: supernova remnants -X-rays: individual (SN 1987A) -gamma rays: ISM

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Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

Cited by 28 publications

References 39 publications

Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

The Very High Energy Sky from ~ 20 GeV to Hundreds of TeV - Selected Highlights

Re-Examination of the Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

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