| Canonical Name: | Kookaburra (Rabbit) |
| TeVCat Name: | TeV J1418-609 |
| Other Names: | G313.3+0.1,
HESS J1418-609
PSR J1418-6058 |
| Source Type: | PWN |
| R.A.: | 14 18 04 (hh mm ss) |
| Dec.: | -60 58 31 (dd mm ss) |
| Gal Long: | 313.25 (deg) |
| Gal Lat: | 0.15 (deg) |
| Distance: | 5.6 kpc |
| Flux: | 0.06 (Crab Units) |
| Energy Threshold: | 300 GeV |
| Spectral Index: | 2.26 |
| Extended: | Yes |
| Size (X): | 0.08 (deg) |
| Size (Y): | 0.06 (deg) |
| Discovery Date: | 2006-09 |
| Discovered By: | H.E.S.S. |
| TeVCat SubCat: | Default Catalog |
Source Notes:
| H.E.S.S. Galactic Plane Survey (HGPS, 2018): |
| A selection of information for each of the 78 sources in the HGPS is provided in TeVCat. For full details, visit the HGPS website. |
| Name: | HESS J1418-609 |
| Source Class: | PWN |
| Identified Object: | PSR J1418-6058 |
| R.A. (J2000): | 214.50 deg (14 18 00) |
| Dec. (J2000): | -60.99 deg (-60 59 09) |
| Positional uncertainty: | 0.026 deg |
| Spatial Model: | Gaussian |
| Size: | 0.108 +/- 0.011 deg |
| Spectral Model: | power law |
| Integral Flux > 1 TeV: | 2.69e-12 +/- 1.53e-13 cm-2 s-1 |
| Pivot Energy, E0: | 1.87 TeV |
| Diff. Flux at E0: | 8.27e-13 +/- 4.64e-14 cm-2 s-1 TeV-1 |
| Spectral Index: | 2.26 +/- 0.05 |
| HGPS Source Notes: | |
| | |
This is one of the 31 firmly-identified objects among the HGPS sources. Three possible associations are listed in Table A.9. "This is a
list of astronomical objects, extracted from catalogs of plausible counterparts, which are are found to be spatially coincident with the HGPS source":
- 3FGL J1418.6−6058 (3FGL)
- G313.3+0.1 (PWN)
- J1418−6058 (PSR)
Source position and its uncertainty:
From
Aharonian et al. (2006):
- RA (J2000): 14h 18m 04s +/- 7s
- Dec (J2000): -60d 58m 31s +/- 35"
Source Extent:
From
Aharonian et al. (2006):
- semi-major axis: 4.9' +/- 1.5' (= 0.082 +/- 0.025 deg)
- semi-major axis: 2.7' +/- 0.7' (= 0.045 +/- 0.012 deg)
- angle: 46.2 +/- 20.4 deg
... major axis, North to East
Source Association:
From
Jaegeun et al. (2023):
- "The extended hard X-ray and TeV emission, associated respectively
with synchrotron radiation and inverse Compton scattering by
relativistic electrons, suggests that particles are accelerated to
very high energies (>=500 TeV), indicating that the Rabbit PWN is a
Galactic PeVatron candidate."
From
Acero et al. (2013):
- This LAT emission from this source below 10 GeV is likely from a
pulsar
Seen by: H.E.S.S.
-
A broadband X-ray study of the Rabbit pulsar wind nebula powered by PSR J1418-6058
Park, Jaegeun et al., arXiv e-prints parXiv:2302.03277 (2023) [LINK]
-
Search for PeV Gamma-Ray Emission from the Southern Hemisphere with 5 Yr of Data from the IceCube Observatory
Aartsen, M.G. et al., ApJ 891 p9 (2020) [LINK]
-
Connecting the ISM to TeV PWNe and PWN candidates
Voisin, F.J. et al., pasa 36 pe014 (2019) [LINK]
-
Dense molecular gas at 12 mm towards Galactic TeV gamma-ray sources
de Wilt, P. et al., MNRAS 468 p2093-2113 (2017) [LINK]
-
Constraints on the Galactic Population of TEV Pulsar Wind Nebulae Using Fermi Large Area Telescope Observations
Acero, F. et al., ArXiv e-prints p (2013) [LINK]
-
X-ray investigation of the diffuse emission around plausible gamma-ray emitting pulsar wind nebulae in Kookaburra region
Kishishita, T. et al., ArXiv e-prints p (2012) [LINK]
-
Discovery of the two ''wings'' of the Kookaburra complex in VHE Gamma-rays with HESS
Aharonian, F. et al., A&A 456 p245-251 (2006) [LINK]
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