| Canonical Name: | LHAASO J2018+3651 |
| TeVCat Name: | TeV J2019+368 |
| Other Names: | MGRO J2019+37
VER J2019+368
VER J2016+371
PSR J2021+3651
Sh 2-104 |
| Source Type: | UNID |
| R.A.: | 20 19 00 (hh mm ss) |
| Dec.: | +36 51 00 (dd mm ss) |
| Gal Long: | 74.98 (deg) |
| Gal Lat: | 0.45 (deg) |
| Distance: | |
| Flux: | 0.5 (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: 10.4 sigma
- E_max (PeV): 0.27 +/- 0.02
- Differential photon flux at 100 TeV (CU): 0.50 +/- 0.10
- On-source events/Off-source events: 42/6.3
- Exposure (hr): 2610.7.
Source Position:
From
Cao et al. (2021):
- R.A. (J2000): 304.75 = 20d 19m 00s
- Dec. (J2000): +36.85 = +36d 51m
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 J2021+3651, Pulsar, Distance: 1.8 +1.7 -1.4 kpc, Age: 17.2 kyr, L_s: 3.4 x10e36
- Sh 2-104, H-II / Young Molecular Cloud, Distance: 3.3 +/- 0.3 kpc / 4.0 +/- 0.5,
Potential TeV Counterparts:
From
Cao et al. (2021):
- This list contains "Nearby teraelectronvolt sources within 1deg of the centre of the LHAASO source"
-
MGRO J2019+37
-
VER J2019+368
-
VER J2016+371
Source Association:
From
Woo et al. (2023):
- "We studied the PeVatron nature of the pulsar wind nebula G75.2+0.1
("Dragonfly") as part of our NuSTAR observational campaign of
energetic PWNe. The Dragonfly is spatially coincident with LHAASO
J2018+3651 whose maximum photon energy is 0.27 PeV."
- "Our analysis of archival XMM data and 13 years of Fermi-LAT data
confirms the detection of an extended (~10') outer nebula in 2 − 6
keV (Index = 1.82 +/- 0.03 ) and non-detection of a GeV nebula,
respectively. "
- "The maximum injected particle energy of 1.4 PeV from our model
suggests that the Dragonfly is likely a PeVatron. Our model
prediction of the low magnetic field (2.7 micro G) in the outer
nebula and recent interaction with the host supernova remnant's
reverse shock (4 kyrs ago) align with common features of PeVatron
PWNe. The origin of its highly asymmetric morphology, pulsar proper
motion, PWN-SNR interaction, and source distance will require further
investigations in the future including a multi-wavelength study using
radio, X-ray, and gamma-ray observations."
Seen by: LHAASO
-
Hard X-ray observation and multiwavelength study of the PeVatron candidate pulsar wind nebula ``Dragonfly''
Woo, Jooyun et al., arXiv e-prints parXiv:2306.07347 (2023) [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 p33-36 (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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