| Canonical Name: | HESS J1458-608 |
| TeVCat Name: | TeV J1459-608 |
| Other Names: | PSR J1459-6053 |
| Source Type: | PWN |
| R.A.: | 14 59 39 (hh mm ss) |
| Dec.: | -60 46 49 (dd mm ss) |
| Gal Long: | 317.95 (deg) |
| Gal Lat: | -1.70 (deg) |
| Distance: | |
| Flux: | 0.06 (Crab Units) |
| Energy Threshold: | 1000 GeV |
| Spectral Index: | 1.81 |
| Extended: | Yes |
| Size (X): | 0.37 (deg) |
| Size (Y): | 0.37 (deg) |
| Discovery Date: | 2012-04 |
| 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 J1458-608 |
| Source Class: | Unid |
| Identified Object: | None |
| R.A. (J2000): | 224.91 deg (14 59 39) |
| Dec. (J2000): | -60.78 deg (-60 46 49) |
| Positional uncertainty: | 0.107 deg |
| Spatial Model: | Gaussian |
| Size: | 0.373 +/- 0.031 deg |
| Spectral Model: | power law |
| Integral Flux > 1 TeV: | 1.40e-12 +/- 3.45e-13 cm-2 s-1 |
| Pivot Energy, E0: | 4.43 TeV |
| Diff. Flux at E0: | 7.71e-14 +/- 1.87e-14 cm-2 s-1 TeV-1 |
| Spectral Index: | 1.81 +/- 0.14 |
| HGPS Source Notes: | |
| | |
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":
- J1459−6053 (PSR)
- 3FGL J1459.4−6053 (3FGL)
- 3FGL J1456.7−6046 (3FGL)
"VHE gamma-ray emission from the new source HESS J1458−608 is associated with the pulsar PSR J1459−6053 and can likely be identified as a heretofore
undetected PWN, on the basis of a spatial coincidence with an energetic pulsar and the absence of other plausible MWL counterparts. Preliminary VHE
morphological and spectral properties were first announced by de los Reyes et al. (2012). The updated morphological properties from the HGPS catalog
differ from those preliminary ones, which had underestimated the extent of the large, complex emission region (0.37deg +/- 0.03deg vs. 0.17deg +/- 0.07deg;
both morphological models 2D symmetric Gaussian), likely due to the irregular shape of the emission. Previously there was a hint for additional structure,
possibly a second source hidden in the tail of a dominant source, but this remains statistically insignificant in the HGPS analysis with respect to a
single-source Gaussian morphology. Also of note, the best-fit centroid of the VHE emission is now located closer to the gamma-ray pulsar (0.11deg vs.
0.16deg offset), bolstering the scenario in which the VHE emission is interpreted as a PWN powered by the pulsar. As expected for such changes in
0morphological properties, the HGPS spectral results also differ from the previously derived preliminary values."
"The pulsar PSR J1459−6053 (also 3FGL J1459.4−6053) is a relatively old (Tc = 65 kyr) but still very energetic HE gamma-ray pulsar with a spin-down
luminosity 9.1 x 10e35 erg s−1 and unknown distance (d < 22 kpc) (Abdo et al. 2013). As noted above, it is offset 0.11deg from the VHE centroid, which
is consistent with offsets observed in other PSR and VHE PWN systems (e.g., Kargaltsev et al. 2013). The putative PWN has not been detected in X-rays
potentially because of the age of the system (Ray et al. 2011) or HE gamma-rays
(Acero et al. 2013). The new VHE spectrum (E > 0.46 TeV) is consistent
with the 31–316 GeV Fermi-LAT upper limits. However, the conclusion, made by Acero et al. (2013), that the peak of the PWN’s inverse Compton emission
is located in this energy range has to be revised as the peak can now only be inferred to be at higher energies."
"Apart from the HE gamma-ray pulsar, there is a second HE source (3FGL J1456.7−6046) in the FoV. However, it is unclear if it is related to the PSR and
PWN scenario, since it exhibits a highly curved, log-parabolic spectrum typical of blazars and a TS that fluctuates strongly with the choice of diffuse
model or analysis method (Acero et al. 2015)."
Source Discovery:
- This detection appears in the proceedings of the 2011 ICRC
de los Reyes et al. (2012)
- This detection is mentioned in
Gast el al. (2012)
- It was also mentioned in July 2012 at the
Gamma 2012 meeting in
Heidelberg by Stegmann (presentation).
Source position and its uncertainty:
The position was updated on 191023 from that given in
de los Reyes et al. (2012) to that
given in
H.E.S.S. Collaboration (2018).
From
H.E.S.S. Collaboration (2018):
- R.A. (J2000): 14 59 39
- Dec. (J2000): -60 46 49
- Positional uncertainty: 0.107 deg
From
de los Reyes et al. (2012):
- R.A. (J2000): 14 58 09.6 +/- 7s
- Dec. (J2000): -60 52 38 +/- 4"
Source Association:
From
Devin et al. (2021):
- "We present a multiwavelength approach to constrain the origin of
the emission from unidentified H.E.S.S. Galactic Plane Survey
sources."
- "The method is applied on two unidentified sources, namely
HESS J1427-608 and HESS J1458-608, for which the multiwavelength
constraints favor the pulsar wind nebula (PWN) scenario."
- "We model their broadband nonthermal spectra in a leptonic scenario
with a magnetic field B <= 10 microG, which is consistent with that
obtained from ancient PWNe. We place both sources within the context
of the TeV PWN population to estimate the spin-down power and the
characteristic age of the putative pulsar."
From
Acero et al. (2013):
- "In our work HESS J1458-608 was not significantly detected above
10GeV. The observed marginal emission comes from the energy bin
between 10 and 31 GeV. Subtracting the pulsar’s contribution does not
change the SED. This comes from the fact that the spectrum of the
pulsar in the 2FGL catalog above 10 GeV is negligible compared to the
SED. The upper limits computed in the energy bins between 31 and
316GeV, where no pulsar emission is expected, show that a change in
the slope of the spectrum is needed between the H.E.S.S. and the LAT
component. This is consistent with an IC peak above 100GeV in the
range observed for the PWNe detected with the Fermi-LAT. However, the
H.E.S.S. spectrum of HESS J1458−608 differs from other PWNe, since it
seems to show a hardening at high energy."
From
de los Reyes et al. (2012):
- suggests the Fermi pulsar PSR J1459-60 as the counterpart
- it is located within the extended emission at 9.6' from the source
best-fit position
- the best fit position locates HESS J1458-608 at ~0.16deg west of the
Fermi pulsar position
From
Gast el al. (2012):
- it is listed as a PWN candidate
Spectral Information:
The index was updated on 191023 from that given in
de los Reyes et al. (2012) to that
given in
H.E.S.S. Collaboration (2018).
From
H.E.S.S. Collaboration (2018):
- spectral index: 1.81 +/- 0.14
From
de los Reyes et al. (2012):
- spectral index: 2.8 +/- 0.2
Source Extent:
The extent was updated on 191023 from that given in
de los Reyes et al. (2012) to that
given in
H.E.S.S. Collaboration (2018).
From
H.E.S.S. Collaboration (2018):
- The updated morphological properties from the HGPS catalog differ
from those preliminary ones (
de los Reyes et al. (2012)), which had
underestimated the extent of the large, complex emission region
(0.37deg +/- 0.03deg vs. 0.17deg +/- 0.07deg; both morphological
models 2D symmetric Gaussian), likely due to the irregular shape of
the emission. Previously there was a hint for additional structure,
possibly a second source hidden in the tail of a dominant source, but
this remains statistically insignificant in the HGPS analysis with
respect to a single-source Gaussian morphology.
From
de los Reyes et al. (2012):
- the 1 sigma extension of the fitted Gaussian is 0.17 +/- 0.07 deg
Seen by: H.E.S.S.
-
Multiwavelength constraints on the unidentified Galactic TeV sources HESS J1427-608, HESS J1458-608, and new VHE gamma-ray source candidates
Devin, Justine et al., arXiv e-prints parXiv:2101.07775 (2021) [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]
-
The H.E.S.S. Galactic plane survey
H.E.S.S. Collaboration et al., A&A 612 pA1 (2018) [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]
-
Exploring the Galaxy at TeV energies: Latest results from the H.E.S.S. Galactic Plane Survey
Gast, H. et al., ArXiv e-prints p (2012) [LINK]
-
A newly discovered VHE gamma-ray PWN candidate around PSR J1459-60
de los Reyes, R. et al., ArXiv e-prints p (2012) [LINK]
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