Back to Main Page
Observation Date (UT) Observation Lat

Canonical Name:SNR G292.2-00.5
TeVCat Name:TeV J1119-614
Other Names:HESS J1119-614, PSR J1119-6127
Source Type:PWN
R.A.:11 19 00 (hh mm ss)
Dec.:-61 24 00 (dd mm ss)
Gal Long: 292.10 (deg)
Gal Lat: -0.49 (deg)
Distance: 5 kpc
Flux:0.04 (Crab Units)
Energy Threshold:500 GeV
Spectral Index:2.2
Extended:Yes
Size (X):0.05 (deg)
Size (Y):0.05 (deg)
Discovery Date:2009-07
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 J1119-614
Source Class: Composite
Identified Object: PSR J1119-6127
R.A. (J2000): 169.77 deg (11 19 04)
Dec. (J2000): -61.45 deg (-61 27 07)
Positional uncertainty: 0.039 deg
Spatial Model: Gaussian
Size: 0.098 +/- 0.014 deg
Spectral Model: power law
Integral Flux > 1 TeV: 9.17e-13 +/- 9.45e-14 cm-2 s-1
Pivot Energy, E0: 1.27 TeV
Diff. Flux at E0: 7.96e-13 +/- 7.47e-14 cm-2 s-1 TeV-1
Spectral Index: 2.64 +/- 0.12
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 J1119.1−6127 (3FGL)
- J1119−6127 (PSR)
- G292.2−0.5 (COMP)
"We confirm the discovery of VHE gamma-ray emission from HESS J1119−614 and identify it as the composite SNR G292.2−0.5. We base the firm identification on the basis of spatial coincidence with the SNR and its associated PWN G292.15−0.54 and highly magnetized pulsar PSR J1119−6127. H.E.S.S. previously published (Djannati-Atai et al. 2009) preliminary source properties that are compatible with the HGPS results."

"A compact (size 6'' x 15''), nonthermal PWN has been detected in X-rays (Gonzalez & Safi-Harb 2003; Safi-Harb & Kumar 2008) and is considered a candidate PWN in HE gamma-rays (Acero et al. 2013). It is powered by the energetic pulsar PSR J1119−6127, with":
- spin-down luminosity Edot = 2.3 x 10e-36 erg s−1
- distance d = 8.4 ± 0.4 kpc (Caswell et al. 2004)
- braking index n = 2.684 ± 0.002 (Weltevrede et al. 2011)
- characteristic age Tc = 1.9 kyr
"The pulsar has been detected in radio (Camilo et al. 2000) and HE gamma rays (Parent et al. 2011; Acero et al. 2015, as 3FGL J1119.1−6127 in the latter) and is characterized by a relatively high surface B field (4.1 x 10e13 G)."

"Considering the luminosity of HESS J1119−614, L_gamma(1−10 TeV) = 2.4 x 10e34(d/8.4 kpc)^2 erg s−1, the apparent efficiency of converting the pulsar's rotational energy to gamma rays (1.1%), is compatible with the efficiencies (<∼10%) of other VHE sources that have been identified as PWNe (Kargaltsev et al. 2013)."

"The offset of the VHE emission from this young pulsar, where the X-ray PWN is located, is not statistically significant with respect to the uncertainty on the best-fit VHE centroid."

"The age of SNR G292.2−0.5 is in the range 4.2−7.1 kyr (Kumar et al. 2012). This can be reconciled with the characteristic age of the pulsar if the braking index n was much smaller than the current value until recently. This assumption is reasonable in light of recent evidence for erratic radio timing behavior from the pulsar (Weltevrede et al. 2011). The X-ray emission from the SNR is predominantly thermal and has an additional hard, nonthermal, X-ray component. This nonthermal emission is likely from the PWN, although an origin in the SNR reverse shock could not be ruled out (Kumar et al. 2012). The X-ray spectral measurements suggest the SNR is generally expanding in a low-density medium, appearing to disfavor a hadronic origin for the VHE gamma rays (Drury et al. 1994). However, there is also evidence for localized, high-density regions near the eastern SNR shell, including dark clouds and CO features (Kumar et al. 2012). We cannot confirm the claim by Kumar et al. (2012), based on preliminary H.E.S.S. results (Djannati-Atai et al. 2009), that no VHE emission is detected from the eastern SNR shell, as it is well within the VHE emission region in the HGPS analysis."

"In conclusion, while the identification with the composite SNR and PWN system is firm, it is not yet clear whether the VHE emission originates in the SNR shock, either leptonically, from the shell itself, or hadronically, from interactions with ambient media; the PWN; or some combination thereof."

Source position and its uncertainty:
From Djannati-Atai et al. (2009):
- coordinates are taken directly from the HESS name
- no information available on the positional uncertainty

Source Extent:
From Djannati-Atai et al. (2009):
- diameter: extended emission size ~0.1 deg
- uncertainty on size not quoted

Spectral Index:
From Djannati-Atai et al. (2009):
- spectal index is a lower limit (S.I. > 2.2)

Source Distance:
HESS: Nov. 2009 Source of the month
- "The distance to pulsar and shell were estimated to about
5 kpc, with very large uncertainty."

Source Association:
From Acero et al. (2013):
- Analysis of the LAT data from this source leads to its
classification as a PWN candidate
From HESS: Nov. 2009 Source of the month
- "The centroid of the emission is offset from the pulsar
in the West/South-West direction, overlapping with a region
of increased X-ray emission from the shell (top image),
which might be attributed to interaction of the supernova
shock with ambient material, or both. The origin of the TeV
emission is not yet uniquely identified; it could either be
attributed to an offset pulsar wind nebula as seen for many
pulsars, or to particles accelerated in the shell and interacting
with ambient gas."

Significance (provided here for sources Newly Announced Catalog):
From Djannati-Atai et al. (2009):
- 8.9 sigma

Seen by: H.E.S.S.
Want a reference added? Send a bibtex entry to the TeVCat Team