| Canonical Name: | LHAASO J1825-1326 |
| TeVCat Name: | TeV J1825-134 |
| Other Names: | HESS J1825-137
HESS J1826-130
2HWC J1825-134
PSR J1826-1334
PSR J1826-1256 |
| Source Type: | UNID |
| R.A.: | 18 25 48 (hh mm ss) |
| Dec.: | -13 27 00 (dd mm ss) |
| Gal Long: | 18.07 (deg) |
| Gal Lat: | -0.54 (deg) |
| Distance: | |
| Flux: | 3.57 (Crab Units) |
| Energy Threshold: | 100000 GeV |
| Spectral Index: | |
| Extended: | Yes |
| Size (X): | 0.00 (deg) |
| Size (Y): | 0.00 (deg) |
| Discovery Date: | 2021-05 |
| Discovered By: | LHAASO |
| TeVCat SubCat: | Default Catalog |
Source Notes:
Details of the source detection:
From
Cao et al. (2021):
- "At 100 TeV, the angular and energy resolutions are about 15–20 arcmin
and better than 20%, respectively, allowing adequate spectroscopic and
morphological studies."
- "The statistical significance of the detection above 100 TeV is calculated
using a 0.3deg extension template"
- "Crab Units (CU), flux of the Crab Nebula at 100 TeV; 1 CU = 6.1 x 10-17 photons TeV-1 cm-2 s-1)"
- Significance above 100 TeV: 16.4 sigma
- E_max (PeV): 0.42 +/- 0.16
- Differential photon flux at 100 TeV (CU): 3.57 +/- 0.52
- On-source events/Off-source events: 61/3.2
- Exposure (hr): 1149.3
Source Position:
From
Cao et al. (2021):
- R.A. (J2000): 276.45 = 18h 25m 48s
- Dec. (J2000): -13.45 = -13d 27m
Spectral Properties:
From
Cao et al. (2021):
- "For the three most significantly detected sources, LHAASO J1825-1326,
LHAASO J1908+0621 and LHAASO J2226+6057, we determine their SEDs."
- The authors show "the spectral energy distributions of three
luminous sources with fluxes exceeding 1 CU (at 100 TeV): LHAASO
J1825-1326, LHAASO J1908+0621 and LHAASO J2226+6057. Above 100 TeV,
the spectra of these sources are steep, characterized by a power-law
photon index of approx. 3. However, a closer look reveals that
between 10 TeV and 500 TeV, the spectra experience gradual
steepening with energy. To explore this tendency, the spectra were
fitted by the so-called log-parabola function dN/dE ∝ E-A(E), where
the local photon index A(E) = a + blogE (a and b are free
parameters) characterizes the slope of the tangent. For all three
spectra, the log-parabola fits are preferred over simple power-law
fits. The gradual steepening of multi-hundred-teraelectronvolt gamma
rays is partly due to the photon-photon absorption that occurs
during their interactions with the diffuse far-infrared and
microwave radiation fields."
- For LHAASO J1825-1326 the parameters of the fit are:
... a: 0.92
... b: 1.19
... A: 3.36
Possible Origin:
From
Cao et al. (2021):
- This list contains sources potentially at the origin of the LHAASO source, together with their class, their distance, age and luminosity
- PSR J1826-1334, Pulsar, Distance: 3.1 +/- 0.2 kpc, Age: 21.4 kyr, L_s: 2.8 x10e36
- PSR J1826-1256, Pulsar, Distance: 1.6 kpc, Age: 14.4 kyr, L_s: 3.6 x10e36
Potential TeV Counterparts:
From
Cao et al. (2021):
- This list contains "Nearby teraelectronvolt sources within 1deg of the centre of the LHAASO source"
-
HESS J1825-137
-
HESS J1826-130
-
2HWC J1825-134
Seen by: LHAASO
-
Constraints on Axion-like Particles from the Observation of Galactic Sources by LHAASO
Li, Jun et al., arXiv e-prints parXiv:2401.01829 (2024) [LINK]
-
The Eel Pulsar Wind Nebula: a PeVatron-Candidate Origin for HAWC J1826-128 and HESS J1826-130
Burgess, Daniel A. et al., arXiv e-prints parXiv:2204.03185 (2022) [LINK]
-
Ultrahigh-energy photons up to 1.4 petaelectronvolts from 12 gamma-ray Galactic sources
Cao, Z., Aharonian, F.A., An, Q., et al., Nature 594, pages 33–36 (2021) [LINK]
-
Strong constraints on Lorentz violation using new gamma-ray observations around PeV
Chen, Liang et al., arXiv e-prints parXiv:2105.07927 (2021) [LINK]
-
Constraints on Hadronic Contribution to LHAASO Sources with Neutrino Observations
Huang, Tian-Qi and Li, Zhuo, arXiv e-prints parXiv:2105.09851 (2021) [LINK]
-
Ultrahigh-energy photons from LHAASO as probes of Lorentz symmetry violations
Li, Chengyi and Ma, Bo-Qiang, arXiv e-prints parXiv:2105.07967 (2021) [LINK]
-
The Hunt for Pevatrons: The Case of Supernova Remnants
Cristofari, P., arXiv e-prints parXiv:2110.07956 (2021) [LINK]
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