| Canonical Name: | LHA 120-N 157B |
| TeVCat Name: | TeV J0537-691 |
| Other Names: | HESS J0537-691
PSR J0537-6910 |
| Source Type: | PWN |
| R.A.: | 05 37 44 (hh mm ss) |
| Dec.: | -69 09 57 (dd mm ss) |
| Gal Long: | 279.55 (deg) |
| Gal Lat: | -31.75 (deg) |
| Distance: | 50 kpc |
| Flux: | 0.02 (Crab Units) |
| Energy Threshold: | 600 GeV |
| Spectral Index: | 2.8 |
| Extended: | Yes |
| Size (X): | 0.01 (deg) |
| Size (Y): | 0.01 (deg) |
| Discovery Date: | 2012-01 |
| Discovered By: | H.E.S.S. |
| TeVCat SubCat: | Default Catalog |
Source Notes:
Source Location:
From
HESS Collaboration (2012):
- R.A. (J2000): 05h 37m 44s +/- 11"(stat)
- Dec. (J2000): 69d 09' 57" +/- 11"(stat)
- systematic uncertainty of 20" on each axis
From
Komin et al. (2012):
- R.A. (J2000): 05h 37m 44s +/- 2s(stat)
- Dec. (J2000): 69d 09' 57" +/- 11"(stat)
Spectral Information:
From
H.E.S.S. Collaboration (2015):
- Spectral index: 2.8 +/- 0.1(stat) +/ 0.3(syst)
From
HESS Collaboration (2012):
- Spectral index: 2.8 +/- 0.2(stat) +/- 0.3(syst)
From
Komin et al. (2012):
- Spectral index: 2.7 +/- 0.2(stat) +/- 0.3(syst)
Source Extent:
From
H.E.S.S. Collaboration (2015):
- "The diameter of N 157B of 100" is of the order of the
H.E.S.S. angular resolution."
- the radius has been entered as 0.014deg (=50")
Source Association:
From
Ferdman et al. (2017):
- "Rotating with a spin period of 16 ms, PSR J0537-6910 is the fastest
spinning and most energetic young pulsar known. It also displays the
most glitch activity of any known pulsar. We have found 42 glitches
over the data span, corresponding to a glitch rate of 3.2 yr-1, with
an overall glitch activity rate of 8.8 e10-7 yr-1."
From
HESS Collaboration (2012):
- This is the first detection of an extragalactic PWN at these
energies. It is associated with PSR J0537-6910, which is the pulsar
with the highest known spin-down luminosity.
From
Komin et al. (2012):
- This source is in the LMC and is likely associated with PSR J0537-6910.
Distance:
From
H.E.S.S. Collaboration (2015):
- the distance to the Large Magellenic Cloud, where this PWN
lies, is approximately 50 kpc
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]
-
High-energy gamma-ray detection of supernova remnants in the Large Magellanic Cloud
Campana, R. et al., MNRAS 515 p1676-1689 (2022) [LINK]
-
Spatially Resolved Chandra Spectroscopy of the Large Magellanic Cloud Supernova Remnant N132D
Sharda, Piyush et al., arXiv e-prints parXiv:2004.07366 (2020) [LINK]
-
Search for Point-Like Sources in the Large Magellanic Cloud
Komin, N. et al., 36th International Cosmic Ray Conference (ICRC2019) 36 p716 (2019) [LINK]
-
The glitches and rotational history of the highly energetic young pulsar PSR J0537-6910
Ferdman, R.D. et al., ArXiv e-prints p (2017) [LINK]
-
X-ray/GeV emissions from Crab-like pulsars in LMC
Takata, J. and Cheng, K.S., ArXiv e-prints p (2016) [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]
-
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]
-
H.E.S.S. observations of the Large Magellanic Cloud
Komin, N. et al., ArXiv e-prints p (2012) [LINK]
-
Discovery of gamma-ray emission from the extragalactic pulsar wind nebula N 157B with H.E.S.S.
H.E.S.S. Collaboration et al., A&A 545 pL2 (2012) [LINK]
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