Discovery of very-high-energy <i>γ</i>-ray emission from the
 vicinity   of PSR J1913+1011 with HESS

Aharonian, F.; Akhperjanian, A. G.; Bazer‐Bachi, A. R.; Behera, B.; Beilicke, M.; Benbow, W.; Berge, D.; Bernlöhr, K.; Boisson, C.; Bolz, O.; Borrel, V.; Braun, I.; Brion, E.; Brown, A. M.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Carrigan, S.; Chadwic, P.M.; Chounet, L.‐M.; Clapson, A. C.; Coignet, G.; Cornils, R.; Costamante, L.; Degrange, B.; Dickinson, H. J.; Djannati‐Ataï, A.; Domainko, W.; Drury, L. O’c.; Dubus, G.; Dyks, J.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Farnier, C.; Feinstein, F.; Fiaßon, A.; ̈orster, A. F; Fontaine, G.; Fukui, Y.; Funk, S.; Füßling, M.; Gallant, Y. A.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Hadjichristidis, C.; Hauser, D.; Hauser, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Holleran, M.; Hoppe, S.; Horns, D.; Jachołkowska, A.; Jager, O. C. de; Kendziorra, E.; Kerschhagg, M.; Khélifi, B.; Komin, Nu.; Kosack, K.; Lamanna, G.; Latham, I. J.; Gallou, R. Le; Lemière, A.; Lemoine‐Goumard, M.; Lenain, J.‐P.; Löhse, T.; Martin, Jean‐Michel; Martineau‐Huynh, O.; Marcowith, A.; Masterson, C.; Maurin, D.; McComb, T. J. L.; Moderski, R.; Moriguchi, Y.; Moulin, Emmanuel; Naurois, M. de; Nedbal, D.; Nolan, S. J.; Olive, J.-P.; Orford, K. J.; Osborne, J. L.; Ostrowski, M.; Panter, M.; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; ̈uhlhofer, G. P; Punch, M.; Ranchon, S.; Raubenheimer, Britt; Raue, M.; Rayner, S. M.; Reimer, O.; Renaud, M.; Ripken, J.; Rob, L.; Rolland, L.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Ruppel, J.; Sahakian, V.; Santangelo, A.; Saugé, L.; Schlenker, S.; Schlickeiser, R.; Schröder, R.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sol, H.; Spangler, D.; Stawarz,; Steenkamp, R.; Stegmann, C.; Superina, G.; Takeuchi, T. T.; Tam, P. H. T.; Tavernet, J.‐P.; Terrier, R.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Vialle, J. P.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Wagner, S. J.; Ward, M. J.

doi:10.1051/0004-6361:20078715

Cited by 24 publications

(19 citation statements)

References 28 publications

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“…Assuming the pulsar is at a distance of 8 kpc, the luminosity of the HESS source in the 1 to 10 TeV range is 4.8 × 10 34 erg s −1 . The association with the pulsar would imply conversion from rotational energy into non-thermal emission with efficiency 0.4%, comparable to those inferred for other VHE γ-ray sources associated with PWNe, i.e., HESS J1912+1011 (Aharonian et al 2008) or HESS J1718-385 (Aharonian et al 2007b). However, the pulsar distance and age limit the maximum extension of the nebula (see i.e.…”

Section: Hess J1023-575supporting

confidence: 70%

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Revisiting the Westerlund 2 field with the HESS telescope array

Abramowski¹,

Acero²,

Aharonian³

et al. 2010

A&A

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Aims. Previous observations with the HESS telescope array revealed the existence of extended very-high-energy (VHE; E > 100 GeV) γ-ray emission, HESS J1023-575, coincident with the young stellar cluster Westerlund 2. At the time of discovery, the origin of the observed emission was not unambiguously identified, and follow-up observations have been performed to further investigate the nature of this γ-ray source. Methods. The Carina region towards the open cluster Westerlund 2 has been re-observed, increasing the total exposure to 45.9 h. The combined dataset includes 33 h of new data and now permits a search for energy-dependent morphology and detailed spectroscopy. Results. A new, hard spectrum VHE γ-ray source, HESS J1026-582, was discovered with a statistical significance of 7σ. It is positionally coincident with the Fermi LAT pulsar PSR J1028-5819. The positional coincidence and radio/γ-ray characteristics of the LAT pulsar favors a scenario where the TeV emission originates from a pulsar wind nebula. The nature of HESS J1023-575 is discussed in light of the deep HESS observations and recent multi-wavelength discoveries, including the Fermi LAT pulsar PSR J1022-5746 and giant molecular clouds in the region. Despite the improved VHE dataset, a clear identification of the object responsible for the VHE emission from HESS J1023-575 is not yet possible, and contribution from the nearby high-energy pulsar and/or the open cluster remains a possibility.

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Section: Hess J1023-575supporting

confidence: 70%

“…Its large FoV and good off-axis sensitivity make HESS ideally suited for studies of extended sources and regions of the sky in which more than one γ-ray source could be present (see e.g. Aharonian et al 2008). The system works in a coincidence mode (e.g.…”

Section: Analysis and Resultsmentioning

confidence: 99%

Revisiting the Westerlund 2 field with the HESS telescope array

Abramowski¹,

Acero²,

Aharonian³

et al. 2010

A&A

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“…These are HESS J1857+026, formerly unidentified but for which a potential counterpart, PSR J1856+0245, has been recently discovered (Aharonian et al 2008a;Hessels et al 2008) the still unidentified HESS J1858+020 (Aharonian et al 2008a), and the PWN candidate HESS J1912+101 (Aharonian et al 2008d).…”

Section: Milagro Detectability -Neighbouring Hess Sourcesmentioning

confidence: 99%

Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Aharonian

Akhperjanian

Anton

et al. 2009

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Aims. Detection of a γ-ray source above 300 GeV is reported, confirming the unidentified source MGRO J1908+06, discovered by the Milagro collaboration at a median energy of 20 TeV. Methods. The source was observed during 27 h as part of the extension of the HESS Galactic plane survey to longitudes >30• . Results. HESS J1908+063 is detected at a significance level of 10.9σ with an integral flux above 1 TeV of (3.76 ± 0.29 stat ± 0.75 sys ) × 10 −12 ph cm −2 s −1 , and a spectral photon index Γ = 2.10 ± 0.07 stat ± 0.2 sys . The positions and fluxes of HESS J1908+063 and MGRO J1908+06 are in good agreement. Possible counterparts at other wavelengths and the origin of the γ-ray emission are discussed. The nearby unidentified GeV source, GRO J1908+0556 (GeV) which also remains unidentified and the new Fermi pulsar 0FGL J1907.5+0617, may be connected to the TeV source.

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“…A corrected version of Tables 2 and 3 of Di Palma et al (2017) is provided in Tables 2, 3, and 4 below. We also report, in Table 1, a corrected version of the Table 1 of Di Palma et al (2017) where we correct a flux that was wrongly reported and a reference (for source J1912+101 we refer now to Aharonian et al 2008b). …”

Section: Conversion Of γ-Ray Fluxes Into Neutrino Fluxesmentioning

confidence: 99%