Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebula
In this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) γ-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1 σ (9.4 σ) above 25 TeV (100 TeV). The s...
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2025-04-01
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| description | In this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) γ-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1 σ (9.4 σ) above 25 TeV (100 TeV). The source energy spectrum extended up to 300 TeV, which was well fitted by a log-parabola function with N0 = (1.93 ± 0.23) × 10−16 TeV−1 cm−2 s−1, α = 2.14 ± 0.27, and β = 1.20 ± 0.41 at E0 = 30 TeV. The associated pulsar, PSR J1740+1000, resides at a high galactic latitude (Gb) and powers a bow-shock pulsar wind nebula (BSPWN) with an extended X-ray tail. The best-fit position of the γ-ray source appeared to be shifted by 0.2° with respect to the pulsar position. As (1) the currently identified pulsar halos do not demonstrate such offsets and (2) the centroid of the γ ray emission is approximately located at the extension of the X-ray tail, we speculate that the UHE γ-ray emission may originate from re-accelerated electron/positron pairs that are advected away in the bow-shock tail. |
| format | Article |
| id | doaj-art-b789e8d53e884674b9d1dcb0b8916ca3 |
| institution | DOAJ |
| issn | 2666-6758 |
| language | English |
| publishDate | 2025-04-01 |
| publisher | Elsevier |
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| series | The Innovation |
| spelling | doaj-art-b789e8d53e884674b9d1dcb0b8916ca32025-08-20T03:17:57ZengElsevierThe Innovation2666-67582025-04-016410080210.1016/j.xinn.2025.100802Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebulaIn this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) γ-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1 σ (9.4 σ) above 25 TeV (100 TeV). The source energy spectrum extended up to 300 TeV, which was well fitted by a log-parabola function with N0 = (1.93 ± 0.23) × 10−16 TeV−1 cm−2 s−1, α = 2.14 ± 0.27, and β = 1.20 ± 0.41 at E0 = 30 TeV. The associated pulsar, PSR J1740+1000, resides at a high galactic latitude (Gb) and powers a bow-shock pulsar wind nebula (BSPWN) with an extended X-ray tail. The best-fit position of the γ-ray source appeared to be shifted by 0.2° with respect to the pulsar position. As (1) the currently identified pulsar halos do not demonstrate such offsets and (2) the centroid of the γ ray emission is approximately located at the extension of the X-ray tail, we speculate that the UHE γ-ray emission may originate from re-accelerated electron/positron pairs that are advected away in the bow-shock tail.http://www.sciencedirect.com/science/article/pii/S2666675825000050LHAASOγ-ray astronomyBSPWN |
| spellingShingle | Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebula The Innovation LHAASO γ-ray astronomy BSPWN |
| title | Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebula |
| title_full | Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebula |
| title_fullStr | Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebula |
| title_full_unstemmed | Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebula |
| title_short | Ultra-high-energy γ-ray emission associated with the tail of a bow-shock pulsar wind nebula |
| title_sort | ultra high energy γ ray emission associated with the tail of a bow shock pulsar wind nebula |
| topic | LHAASO γ-ray astronomy BSPWN |
| url | http://www.sciencedirect.com/science/article/pii/S2666675825000050 |