LMC N132D

Last updated
LMC N132D
XRISM Reveals Its First Look at X-ray Cosmos (SVS14492 - N132D LMC).jpg
Event type Supernova remnant   OOjs UI icon edit-ltr-progressive.svg
II
Constellation Dorado
Right ascension 05h 25m 1.4s
Declination -69° 38' 31.0"
Epoch J2000
Galactic coordinates Large Magellanic Cloud
Other designationsLMC N132D, SNR J052501-693842, IRAS 05240-6948
  Commons-logo.svg Related media on Commons
[ edit on Wikidata]

LMC N132D (also known as SNR J052501-693842) is a prominent supernova remnant (SNR) located in the Large Magellanic Cloud (LMC), a satellite galaxy of the Milky Way Galaxy, in the constellation of Dorado. It lies approximately 170,000 light-years (52,000 parsecs) away. It is one of the brightest and most studied oxygen-rich SNRs in the LMC, known for its complex morphology and high-energy emissions across multiple wavelengths. [1] [2] [3]

Contents

Observation

LMC N132D is a very high-energy (VHE) gamma-ray source, detected by the High Energy Stereoscopic System (H.E.S.S.) with an angular resolution of ~0.05 degrees. Its power-law spectrum extends beyond 8 TeV without a cutoff, unusual for a remnant of its age, making it a key target for studying particle acceleration in mature SNRs. [4] It is located near the center of the galaxy, 1.5 degrees west of the Tarantula Nebula . The nebula emits X-rays, and its material travels at a speed of 2000 km/s. [5] [6]

Significance

LMC N132D offers critical insights into core-collapse supernovae, shock interactions with the interstellar medium, and non-thermal processes in SNRs. Its oxygen-rich ejecta and association with molecular clouds provide clues about the progenitor star's environment and evolution. The remnant's gamma-ray emission challenges models of particle acceleration, as its mature age contrasts with its high-energy output. [7] [8]

References

  1. ↑ "Supernova Remnant LMC N132D - NASA Science". 2009-09-09. Retrieved 2025-09-20.
  2. ↑ information@eso.org. "Oxygen-Rich Supernova". www.esahubble.org. Retrieved 2025-09-20.
  3. ↑ "COS Spectrum of Supernova Remnant LMC N132D - NASA Science". 2009-09-09. Retrieved 2025-09-20.
  4. ↑ Abdalla, H.; Aharonian, F.; Benkhali, F. Ait; Angüner, E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Martins, V. Barbosa; Barnacka, A.; Barnard, M.; Batzofin, R.; Becherini, Y. (2021-11-01). "LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV". Astronomy & Astrophysics. 655: A7. arXiv: 2108.02015 . Bibcode:2021A&A...655A...7H. doi:10.1051/0004-6361/202141486. ISSN   0004-6361.
  5. ↑ "A Supernova Remnant in the Large Magellanic Cloud (SEDS HST Archive 79 of 135)". seds.lpl.arizona.edu. Archived from the original on 2008-01-02. Retrieved 2025-09-20.
  6. ↑ "N132D - IACHEC - MIT Wiki Service". wikis.mit.edu. Retrieved 2025-09-20.
  7. ↑ Vink, Jacco; Simoni, Rachel; Komin, Nukri; Prokhorov, Dmitry (2021-07-22), LMC N132D: a mature supernova remnant with a youthful gamma-ray spectrum, arXiv: 2107.10946 , Bibcode:2022icrc.confE.778V
  8. ↑ "Molecular Clouds and Supernova Remnants in the LMC". www.physics.rutgers.edu. Retrieved 2025-09-20.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.