Detection of GeV Gamma-Rays from HESS J1534−571 and Multiwavelength Implications for the Origin of the Nonthermal Emission

Araya, Miguel

doi:10.3847/1538-4357/aa7261

Cited by 20 publications

(13 citation statements)

References 32 publications

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“…Independent of the MAXI J1535−571 discovery, the existence of the cavity (Figure 1) favours a core-collapse supernova explosion model for the SNR, like that required to create a BH. The cavity is also consistent with SNR distance estimates from radio brightness (12), X-ray absorption ( 14) and gamma-ray emission modeling (15). Given the strong case for a relation between the SNR and BH, we used the SNR shock evolution modelling age estimate of 8-24 kyr (12) as a guide to model the history of this unique association.…”

supporting

confidence: 53%

A supernova remnant associated with a nascent black hole low-mass X-ray binary

Maxted,

Ruiter,

Belczynski

et al. 2020

Preprint

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Energy released when the core of a high-mass star collapses into a black hole often powers an explosion that creates a supernova remnant. Black holes have limited windows of observability, and consequently are rarely identified in association with supernova remnants. Analysing multi-messenger data, we show that MAXI J1535−571 is the black hole produced in the stellar explosion that gave rise to the supernova remnant G323.7−1.0, making it the first case of an association between a black hole low-mass X-ray binary and a supernova remnant. Given this connection, we can infer from our modeling that the progenitor system was a close binary whose primary star had an initial mass of ∼23-35 solar masses with a companion star about 10 times less massive.

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supporting

confidence: 53%

A supernova remnant associated with a nascent black hole low-mass X-ray binary

Maxted,

Ruiter,

Belczynski

et al. 2020

Preprint

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“…Each CCD chip is placed on the focal plane of the X-Ray Telescope (XRT; Serlemitsos et al 2007 (Puehlhofer et al 2015). The cross point shows the brightness peak position of the GeV gamma-ray emission (Araya 2017).…”

Section: Observation and Data Reductionmentioning

confidence: 99%

Discovery of 6.4 keV line and soft X-ray emissions from G323.7−1.0 with Suzaku

Saji

Matsumoto

Nobukawa

et al. 2018

Publications of the Astronomical Society of Japan

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In this paper, the Suzaku X-ray data of the Galactic Supernova Remnant (SNR) candidate G323.7−1.0 are analyzed to search for X-ray emission. Spatially-extended enhancements in the 6.4 keV line and in soft X-rays are found inside or on the radio shell. The soft X-ray enhancement would be the hottest part of the shell-like X-ray emission along the radio shell.The 6.4 keV line enhancement is detected at a significance level of 4.1σ. The lower limit of the equivalent width (EW) is 1.2 keV. The energy centroid of the 6.4 keV line is 6.40 ± 0.04 keV, indicating that the iron is less ionized than the Ne-like state. If the 6.4 keV line originates from ionizing non-equilibrium thermal plasma, presence of iron-rich ejecta in a low-ionization state is required, which is disfavored by the relatively old age of the SNR. The 6.4 keV line enhancement would be due to K-shell ionization of iron atoms in a dense interstellar medium by high-energy particles. Since there is no irradiating X-ray source, the origin of the 6.4 keV line enhancement is not likely the photoionization. The large EW can only be explained by K-shell ionization due to cosmic-ray protons with an energy of ∼ 10 MeV, which might be generated by the shock acceleration in G323.7−1.0.

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“…results on HESS J1534−571, Araya (2017) has recently shown that a disk-like GeV counterpart to HESS J1534−571 can be extracted from Fermi-LAT data as well. The GeV source position and size are in good morphological agreement with G323.7−1.0 and HESS J1534−571.…”

Section: Gev Emission With Fermi-latmentioning

confidence: 94%

Search for new supernova remnant shells in the Galactic plane with H.E.S.S.

Puehlhofer¹,

Brun²,

Capasso³

et al. 2016

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

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A search for new supernova remnants (SNRs) has been conducted using TeV γ-ray data from the H.E.S.S. Galactic plane survey. As an identification criterion, shell morphologies that are characteristic for known resolved TeV SNRs have been used. Three new SNR candidates were identified in the H.E.S.S. data set with this method. Extensive multiwavelength searches for counterparts were conducted. A radio SNR candidate has been identified to be a counterpart to HESS J1534−571. The TeV source is therefore classified as a SNR. For the other two sources, HESS J1614−518 and HESS J1912+101, no identifying counterparts have been found, thus they remain SNR candidates for the time being. TeV-emitting SNRs are key objects in the context of identifying the accelerators of Galactic cosmic rays. The TeV emission of the relativistic particles in the new sources is examined in view of possible leptonic and hadronic emission scenarios, taking the current multiwavelength knowledge into account.

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Detection of GeV Gamma-Rays from HESS J1534−571 and Multiwavelength Implications for the Origin of the Nonthermal Emission

Cited by 20 publications

References 32 publications

A supernova remnant associated with a nascent black hole low-mass X-ray binary

A supernova remnant associated with a nascent black hole low-mass X-ray binary

Discovery of 6.4 keV line and soft X-ray emissions from G323.7−1.0 with Suzaku

Search for new supernova remnant shells in the Galactic plane with H.E.S.S.

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