A new study of the supernova remnant G344.7-0.1 located in the vicinity of the unidentified TeV source HESS J1702-420

Giacani, E.; Smith, Mike; Dubner, G.; Loiseau, N.

doi:10.1051/0004-6361/201116768

Cited by 35 publications

(60 citation statements)

References 33 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The sources 2FHLJ1703.4−4145 and 2FHLJ1745.1−3035 are the hardest sources (Γ < 1.3) among the six objects. 2FHLJ1703.4−4145 is spatially coincident with the bright radio emission observed from the western side of the shell of SNR G344.7−001, a nearby mid-aged shell-type (age ∼ 3000 years and 8′ diameter) SNR (Giacani et al 2011). Both the 2FHL source and the SNR are spatially coincident with the larger, elongated and unidentified HESSJ1702−420 (Aharonian et al 2008b).…”

Section: Comparison With the Hess Galactic Plane Surveymentioning

confidence: 59%

2fhl: The Second Catalog of Hard Fermi-Lat Sources

Ackermann¹,

Ajello²,

Atwood³

et al. 2016

ApJS

254

207

View full text Add to dashboard Cite

We present a catalog of sources detected above 50 GeV by the Fermi-Large Area Telescope (LAT) in 80 months of data. The newly delivered Pass8 event-level analysis allows the detection and characterization of sources in the 50 GeV-2 TeV energy range. In this energy band, Fermi-LAT has detected 360 sources, which constitute the second catalog of hard Fermi-LAT sources (2FHL). The improved angular resolution enables the precise localization of point sources (∼1 7 radius at 68% C.L.) and the detection and characterization of spatially extended sources. We find that 86% of the sources can be associated with counterparts at other wavelengths, of which the majority (75%) are active galactic nuclei and the rest (11%) are Galactic sources. Only 25% of the 2FHL sources have been previously detected by Cherenkov telescopes, implying that the 2FHL provides a reservoir of candidates to be followed up at very high energies. This work closes the energy gap between the observations performed at GeV energies by Fermi-LATon orbit and the observations performed at higher energies by Cherenkov telescopes from the ground.

show abstract

Section: Comparison With the Hess Galactic Plane Surveymentioning

confidence: 59%

2fhl: The Second Catalog of Hard Fermi-Lat Sources

Ackermann¹,

Ajello²,

Atwood³

et al. 2016

ApJS

254

207

View full text Add to dashboard Cite

show abstract

“…12). From a radio spectral study carried out in this region of the remnant using the Very Large Array (VLA, NRAO) and the Australia Telescope Compact Array (ATCA) data at 1.4 GHz and 5 GHz, Giacani et al (2011) determined a mean radio spectral index of α ∼ 0.3 for the nebula, a value compatible with those of radio PWNe. The combination of the emission in the three mentioned spectral ranges allowed the authors to rule out a PWN origin, concluding that the central bright radio feature is probably the result of strong shocks interacting with dense material.…”

Section: Comparison Of Radio Emission With Emission In Other Spectralmentioning

confidence: 91%

Radio emission from supernova remnants

Dubner

Giacani

2015

Astron Astrophys Rev

150

121

View full text Add to dashboard Cite

show abstract

“…The very large "darkness ratio" of γ-ray to X-ray luminosity (in the 1-30 TeV and 2-10 keV bands respectively) for this source of 156, makes this the darkest identified PWN to date (the darker HESS J1702-420, darkness ratio 1500, is now believed to be an SNR, Giacani et al 2011). This could imply a relatively old age for PSR J1301−6305.…”

Section: Distance To the Sourcementioning

confidence: 92%

Identification of HESS J1303−631 as a pulsar wind nebula throughγ-ray, X-ray, and radio observations

Abramowski¹,

Acero²,

Aharonian³

et al. 2012

A&A

View full text Add to dashboard Cite

Aims. The previously unidentified very high-energy (VHE; E > 100 GeV) γ-ray source HESS J1303−631, discovered in 2004, is re-examined including new data from the H.E.S.S. Cherenkov telescope array in order to identify this object. Archival data from the XMM-Newton X-ray satellite and from the PMN radio survey are also examined. Methods. Detailed morphological and spectral studies of VHE γ-ray emission as well as of the XMM-Newton X-ray data are performed. Radio data from the PMN survey are used as well to construct a leptonic model of the source. The γ-ray and X-ray spectra and radio upper limit are used to construct a one zone leptonic model of the spectral energy distribution (SED). Results. Significant energy-dependent morphology of the γ-ray source is detected with high-energy emission (E > 10 TeV) positionally coincident with the pulsar PSR J1301−6305 and lower energy emission (E < 2 TeV) extending ∼0.4• to the southeast of the pulsar. The spectrum of the VHE source can be described with a power-law with an exponential cut-off N 0 = (5.6 ± 0.5) × 10 −12 TeV −1 cm −2 s −1 , Γ = 1.5 ± 0.2) and E cut = (7.7 ± 2.2) TeV. The pulsar wind nebula (PWN) is also detected in X-rays, extending ∼2−3 from the pulsar position towards the center of the γ-ray emission region. A potential radio counterpart from the PMN survey is also discussed, showing a hint for a counterpart at the edge of the X-ray PWN trail and is taken as an upper limit in the SED. The extended X-ray PWN has an unabsorbed flux of F 2−10 keV ∼ 1.6and is detected at a significance of 6.5σ. The SED is well described by a one zone leptonic scenario which, with its associated caveats, predicts a very low average magnetic field for this source.Conclusions. Significant energy-dependent morphology of this source, as well as the identification of an associated X-ray PWN from XMM-Newton observations enable identification of the VHE source as an evolved PWN associated to the pulsar PSR J1301−6305. This identification is supported by the one zone leptonic model, which suggests that the energetics of the γ-ray and X-ray radiation are such that they may have a similar origin in the pulsar nebula. However, the large discrepancy in emission region sizes and the low level of synchrotron radiation suggest a multi-population leptonic nature. The low implied magnetic field suggests that the PWN has undergone significant expansion. This would explain the low level of synchrotron radiation and the difficulty in detecting counterparts at lower energies, the reason this source was originally classified as a "dark" VHE γ-ray source.

show abstract

A new study of the supernova remnant G344.7-0.1 located in the vicinity of the unidentified TeV source HESS J1702-420

Cited by 35 publications

References 33 publications

2fhl: The Second Catalog of Hard Fermi-Lat Sources

2fhl: The Second Catalog of Hard Fermi-Lat Sources

Radio emission from supernova remnants

Identification of HESS J1303−631 as a pulsar wind nebula throughγ-ray, X-ray, and radio observations

Contact Info

Product

Resources

About