| Canonical Name: | HESS J1708-410 |
| TeVCat Name: | TeV J1708-410 |
| Other Names: | |
| Source Type: | UNID |
| R.A.: | 17 08 24 (hh mm ss) |
| Dec.: | -41 05 24 (dd mm ss) |
| Gal Long: | 345.68 (deg) |
| Gal Lat: | -0.47 (deg) |
| Distance: | |
| Flux: | 0.04 (Crab Units) |
| Energy Threshold: | 200 GeV |
| Spectral Index: | 2.46 |
| Extended: | Yes |
| Size (X): | 0.06 (deg) |
| Size (Y): | 0.08 (deg) |
| Discovery Date: | 2006-01 |
| 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 J1708-410 |
| Source Class: | Unid |
| Identified Object: | None |
| R.A. (J2000): | 257.06 deg (17 08 13) |
| Dec. (J2000): | -41.08 deg (-41 04 44) |
| Positional uncertainty: | 0.020 deg |
| Spatial Model: | Gaussian |
| Size: | 0.064 +/- 0.006 deg |
| Spectral Model: | power law |
| Integral Flux > 1 TeV: | 6.52e-13 +/- 5.25e-14 cm-2 s-1 |
| Pivot Energy, E0: | 1.05 TeV |
| Diff. Flux at E0: | 8.88e-13 +/- 6.14e-14 cm-2 s-1 TeV-1 |
| Spectral Index: | 2.54 +/- 0.07 |
| HGPS Source Notes: | |
| | |
This is one of eleven HGPS sources that "do not have any associations with known physical objects, although some are associated
with HE gamma-ray sources."
"HESS J1708−410 has no compelling association, even though this source was the target of dedicated X-ray observations to look for associated emission
(Van Etten et al. 2009).
Given the brightness and relatively steep spectrum of this VHE source (index = 2.57 +/- 0.09), the absence of a counterpart at lower gamma-ray energies in the Fermi-LAT catalogs
is surprising and suggests the emission peaks in the hundreds of GeV range."
This source is one of the twelve source whose HGPS results differed from those published in previous publications.
- "The flux above 1 TeV of HESS J1708−410 is found to be smaller in the HGPS analysis than in Aharonian et al. (2008).
While the size of the source is similar in both cases,
the different approaches used in the HGPS analysis lead to different integration radii used to derive the source spectrum. The HGPS analysis uses an integration radius about
two times smaller than in the dedicated analysis, which explains the apparent discrepancy"
Source position and its uncertainty:
From
Aharonian et al. (2006):
- l: 345.672 +/- 0.013 (deg)
- b: -0.438 +/- 0.010 (deg)
- R.A. (deg): 257.06 (Convert to HMS: 17 08 14.4)
- Dec. (deg): -41.08 (Convert to HMS: -41 04 48)
From
Aharonian et al. (2008):
- RA: (J2000): 17 08 24
- Dec (J2000): -41 05 24
- The fit position has a statistical error of 0.05 deg
Source Extent:
From
Aharonian et al. (2006):
- radius: 0.054 +/- 0.012 deg
From
Aharonian et al. (2008):
- semi-major axis: 0.06 +/- 0.01 deg
- semi-minor axis: 0.08 +/- 0.01 deg
- angle: -20 +/- 23 deg
...measured counter-clk relative to RA axis
Source Classification:
-
Tibolla et al. (2011) suggest that this source is an ancient PWN
Seen by: H.E.S.S.
-
Ancient Pulsar Wind Nebulae as a natural explanation for unidentified gamma-ray sources
Kaufmann, S. and Tibolla, O., ArXiv e-prints p (2018) [LINK]
-
New developments in the ancient PulsarWind Nebulae scenario
Tibolla, O. et al., ArXiv e-prints p (2011) [LINK]
-
Ancient Pulsar Wind Nebulae in light of recent GeV and TeV observations
Tibolla, O. et al., ArXiv e-prints p (2011) [LINK]
-
A Multi-Wavelength Investigation of the Unidentified Gamma-Ray Source HESS J1708-410
Van Etten, A. et al., ArXiv e-prints p (2009) [LINK]
-
HESS very-high-energy gamma-ray sources without identified counterparts
Aharonian, F. et al., A&A 477 p353-363 (2008) [LINK]
-
The H.E.S.S. Survey of the Inner Galaxy in Very High Energy Gamma Rays
Aharonian, F. et al., ApJ 636 p777-797 (2006) [LINK]
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