| Canonical Name: | LMC N132D |
| TeVCat Name: | TeV J0525-696 |
| Other Names: | SNR J052501-693842 |
| Source Type: | SNR/Molec. Cloud |
| R.A.: | 05 24 47 (hh mm ss) |
| Dec.: | -69 38 50 (dd mm ss) |
| Gal Long: | 280.32 (deg) |
| Gal Lat: | -32.81 (deg) |
| Distance: | 50 kpc |
| Flux: | (Crab Units) |
| Energy Threshold: | GeV |
| Spectral Index: | 2.4 |
| Extended: | No |
| Discovery Date: | 2014-10 |
| Discovered By: | H.E.S.S. |
| TeVCat SubCat: | Default Catalog |
Source Notes:
This detection was announced at the
Fermi Symposium by
Komin et al. (2014):
- "H.E.S.S., with its superior angular resolution of about 0.05
degrees, can separate individual sources in the LMC. In this talk we
will present the result of 210 h observations with the H.E.S.S.
telescopes. Besides the already known PWN N 157B, these observations
establish significant VHE gamma-ray emission from the superbubble
30 Dor C and show evidence for emission from the supernova remnant (SNR) N 132D.
From
H.E.S.S. Collaboration (2015):
- "Along with the clear detection of N 157B and 30 Dor C, evidence for
VHE gamma-ray emission is observed from the prominent SNR N 132D. The
emission peaks at a significance of about 5 SD above a background that
is estimated from a ring around each sky bin. At the nominal position
of the SNR, 43 gamma rays with a statistical significance of 4.7 SD
are recorded."
From
Lemoine-Goumard (2015):
- this is one of the oldest VHE gamma-ray emitting SNRs
Positional Information:
On 210805, the positional information in TeVCat was updated from that given in
SIMBAD
to that given in
H.E.S.S. Collaboration (2021).
From
H.E.S.S. Collaboration (2021):
- R.A. (J2000): 05h 24m 47s +/- 6.9s (stat)
- Dec. (J2000): -69d 38' 50'' +/- 29'' (stat)
- "The uncertainty of the telescope pointing leads to a systematic
error of ∼20'' per axis."
The position is taken from
SIMBAD:
- R.A. (J2000): 05h 25m 02.20d
- Dec. (J2000): -69d 38' 39.0''
Source Extent:
From
H.E.S.S. Collaboration (2021):
There is no evidence for this source being extended:
- "As there is no evidence for an extension, a point source assumption
was used by fitting the two-dimensional Gaussian profile with a width
of 0.005deg."
Distance:
From
H.E.S.S. Collaboration (2015):
- the distance to the Large Magellenic Cloud, where this SNR/
Molecular Cloud lies, is approximately 50 kpc
Spectral Information:
From
H.E.S.S. Collaboration (2021):
"The joint analysis of the extended H.E.S.S and Fermi-LAT data results
in a spectral energy distribution in the energy range from 1.7 GeV to
14.8 TeV, which suggests a high luminosity of N132D at GeV and TeV
energies. We set a lower limit on a gamma-ray cutoff energy of 8 TeV
with a confidence level of 95%."
- "The H.E.S.S. spectrum is well fit with a single power law":
... dN/dE = F0 × (E0/1TeV)−A) with
... A: 2.3 ± 0.2
... F0: 1.31 +/- 0.43 x 10e-13 TeV-1 cm-2 s-1
- "Systematic errors on the spectrum parameters are estimated to be +/- 0.3 for 1,
and +/- 30% for F0. These systematic uncertainties arise because the data set
spans 13 years and the LMC is mostly observed during the rainy season, leading
to significant variations in atmospheric conditions (
Abramowski et al., 2012)."
From
H.E.S.S. Collaboration (2015):
- Spectral index: 2.4 +/- 0.3(stat) +/- 0.3(syst)
Origin of the Gamma-ray Emission:
From
H.E.S.S. Collaboration (2021):
- "The new gamma-ray spectrum as well as multiwavelength observations of
N132D when compared to physical models suggests a hadronic origin of
the VHE gamma-ray emission"
- "SNR N132D is a VHE gamma-ray source that shows a spectrum extending
to the VHE domain without a spectral cutoff at a few TeV, unlike the
younger oxygen-rich SNR Cassiopeia A."
- "The gamma-ray emission is best explained by a dominant hadronic
component formed by diffusive shock acceleration."
- "The gamma-ray properties of N132D may be affected by an interaction
with a nearby molecular cloud that partially lies inside the 95%
confidence region of the source position."
Seen by: H.E.S.S.
-
Search for gamma-ray emission from SNRs in the Large Magellanic Cloud: a new cluster analysis at energies above 4 GeV
Tramacere, Andrea et al., arXiv e-prints parXiv:2503.20351 (2025) [LINK]
-
Evidence for Charge Exchange Emission in Supernova Remnant N132D from XRISM/Resolve Observations
Gu, Liyi et al., arXiv e-prints parXiv:2504.03223 (2025) [LINK]
-
Measurement of the Forward Shock Velocities of the Supernova Remnant N132D Based on the Thermal X-Ray Emission
Okada, Yoshizumi et al., ApJ 982 p190 (2025) [LINK]
-
XMM-Newton Observations of the High Temperature Plasma in the Large Magellanic Cloud Supernova Remnant N132D
Foster, Adam R. et al., arXiv e-prints parXiv:2504.19964 (2025) [LINK]
-
Infrared Ejecta and Cold Dust in the Young Supernova Remnant N132D
Rho, Jeonghee et al., arXiv e-prints parXiv:2303.04966 (2023) [LINK]
-
High-energy gamma-ray detection of supernova remnants in the Large Magellanic Cloud
Campana, R. et al., MNRAS 515 p1676-1689 (2022) [LINK]
-
LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV
H.E.S.S. Collaboration et al., arXiv e-prints parXiv:2108.02015 (2021) [LINK]
-
Three-Dimensional Kinematic Reconstruction of the Optically-Emitting, High-Velocity, Oxygen-Rich Ejecta of Supernova Remnant N132D
Law, Charles J. et al., arXiv e-prints parXiv:2004.00016 (2020) [LINK]
-
Plasma Diagnostics of the Supernova Remnant N132D using Deep XMM-Newton Observations with the Reflection Grating Spectrometer
Suzuki, Hitomi et al., ApJ 900 p39 (2020) [LINK]
-
ALMA CO Observations of Gamma-Ray Supernova Remnant N132D in the Large Magellanic Cloud:
Possible Evidence for Shocked Molecular Clouds Illuminated by Cosmic-Ray Protons
Sano, H. et al., arXiv e-prints parXiv:2007.07900 (2020) [LINK]
-
Search for Point-Like Sources in the Large Magellanic Cloud
Komin, N. et al., International Cosmic Ray Conference, 36 p716 (2019) [LINK]
-
Shocked Interstellar clouds and dust grain destruction in the LMC Supernova Remnant N132D
Dopita, M.A. et al., ArXiv e-prints p (2018) [LINK]
-
A deep view of the Large Magellanic Cloud with 6 years of Fermi-LAT observations
The Fermi-LAT Collaboration, ArXiv e-prints p (2015) [LINK]
-
The exceptionally powerful TeV gamma-ray emitters in the Large Magellanic Cloud
H.E.S.S. Collaboration, Science (2015), 347, 6220, p406-412 [LINK]
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