| Canonical Name: | 30 Dor C |
| TeVCat Name: | TeV J0535-692 |
| Other Names: | |
| Source Type: | Superbubble |
| R.A.: | 05 35 55 (hh mm ss) |
| Dec.: | -69 11 10 (dd mm ss) |
| Gal Long: | 279.60 (deg) |
| Gal Lat: | -31.91 (deg) |
| Distance: | 50 kpc |
| Flux: | (Crab Units) |
| Energy Threshold: | GeV |
| Spectral Index: | 2.6 |
| Extended: | No |
| Discovery Date: | 2014-10 |
| Discovered By: | H.E.S.S. |
| TeVCat SubCat: | Default Catalog |
Source Notes:
From
H.E.S.S. Collaboration (2015):
- "(the detection) coincides with the superbubble 30 Dor C, the first
such source detected in VHE gamma rays"
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.
Positional Information:
150128: The position was updated from the
SIMBAD one.
From
H.E.S.S. Collaboration (2015):
- R.A. (J2000): 05 35 55 +/- 5s
- Dec. (J2000): -69 11 10 +/- 20"
Spectral Information:
From
H.E.S.S. Collaboration (2015):
- spectral index: 2.6 +/- 0.2(stat) +/- 0.3(syst)
Distance:
From
H.E.S.S. Collaboration (2015):
- the distance to the Large Magellenic Cloud, where this superbubble
lies, is approximately 50 kpc
Source properties:
From
Kavanagh et al. (2018):
- "The 30 Dor C superbubble is unique for its synchrotron X-ray shell,
as well as being the first superbubble to be detected in TeV gamma
rays, though the dominant TeV emission mechanism, i.e., leptonic or
hadronic, is still unclear. We aim to use new Chandra observations of
30 Dor C to resolve the synchrotron shell in unprecedented detail and
to estimate the magnetic field in the postshock region, a key
discriminator between TeV gamma-ray emission mechanisms."
- "The average postshock B-field determined around the X-ray
synchrotron shell of 30 Dor C suggests the leptonic scenario as the
dominant emission mechanism for the TeV gamma-rays."
Seen by: H.E.S.S.
-
Associated molecular and atomic clouds with X-ray shell of superbubble 30 Doradus C in the LMC
Yamane, Y. et al., arXiv e-prints parXiv:2106.09916 (2021) [LINK]
-
Massive stars in the Tarantula Nebula: A Rosetta Stone for Extragalactic Supergiant HII Regions
Crowther, Paul, arXiv e-prints parXiv:1911.02047 (2019) [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]
-
Constraining cosmic ray acceleration in young star clusters using multi-wavelength observations
Gupta, S. et al., ArXiv e-prints p (2018) [LINK]
-
Magnetic field estimates from the X-ray synchrotron emitting rims of the 30 Dor C superbubble and the implications for the nature of 30 Dor C's TeV emission
Kavanagh, P.J. et al., ArXiv e-prints p (2018) [LINK]
-
Evidence of Particle Acceleration in the Superbubble 30 Doradus C with NuSTAR
Lopez, L.A. et al., ArXiv e-prints p (2018) [LINK]
-
Deep view of the Large Magellanic Cloud with six years of Fermi-LAT observations
Ackermann, M. et al., A&A 586 pA71 (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]
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