| Canonical Name: | HESS J1026-582 |
| TeVCat Name: | TeV J1026-582 |
| Other Names: | 3EG J1027-5817
1FGL J1028.4-5810
PSR J1028-5819 |
| Source Type: | PWN |
| R.A.: | 10 26 38.4 (hh mm ss) |
| Dec.: | -58 12 00 (dd mm ss) |
| Gal Long: | 284.80 (deg) |
| Gal Lat: | -0.52 (deg) |
| Distance: | 2.3 kpc |
| Flux: | 0.03 (Crab Units) |
| Energy Threshold: | 800 GeV |
| Spectral Index: | 1.94 |
| Extended: | Yes |
| Size (X): | 0.14 (deg) |
| Size (Y): | 0.14 (deg) |
| Discovery Date: | 2011-01 |
| 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 J1026-582 |
| Source Class: | Unid |
| Identified Object: | None |
| R.A. (J2000): | 156.74 deg (10 26 57) |
| Dec. (J2000): | -58.23 deg (-58 13 31) |
| Positional uncertainty: | 0.075 deg |
| Spatial Model: | Gaussian |
| Size: | 0.130 +/- 0.039 deg |
| Spectral Model: | power law |
| Integral Flux > 1 TeV: | 6.63e-13 +/- 8.86e-14 cm-2 s-1 |
| Pivot Energy, E0: | 4.43 TeV |
| Diff. Flux at E0: | 3.64e-14 +/- 4.76e-15 cm-2 s-1 TeV-1 |
| Spectral Index: | 1.81 +/- 0.10 |
| HGPS Source Notes: | |
| | |
This source is listed as unidentified in the HGPS. Two 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":
- HESS J1026−582 G285.1−0.5 (PWN)
- J1028−5819 (PSR)
Source position and its uncertainty:
From
Abramowski et al. (2011):
- RA (J2000): 10 26 38.4 +/- 21.6s(stat) +/- 20s(syst)
- Dec (J2000): -58 12 00 +/- 1'48"(stat) +/- 20"(syst)
Source Extent:
From
Abramowski et al. (2011):
- 0.14 +/- 0.03 deg
Spectral Properties:
From
Abramowski et al. (2011):
- Spectral index: 1.94 +/- 0.20 (stat) +/- 0.2 (sys)
Source Association:
From
Acero et al. (2013):
- "No significant LAT emission coming from the location of the
H.E.S.S. excess is detected in our analysis. The very low TS value of
1.0 with an integrated flux less than 1.6 x 10e-10 ph cm−2 s−1 gives
little hope for a future detection by the LAT. The upper limits show
that a rising spectrum is needed in the LAT energy range. This
suggests an IC peak at energies higher than 100 GeV consistent with
Fermi-LAT observations of other PWNe. However, the lack of
multi-wavelength data (especially in radio and X-rays) prevents clear
identification of this source."
Seen by: H.E.S.S.
-
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]
-
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]
-
VLT and Suzaku observations of the Fermi pulsar PSR J1028-5819
Mignani, R.P. et al., A&A 543 pA130 (2012) [LINK]
-
Revisiting the Westerlund 2 field with the HESS telescope array
HESS Collaboration et al., A&A 525 pA46+ (2011) [LINK]
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the TeVCat Team
