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Observation Date (UT) Observation Lat

Canonical Name:2HWC J1955+285
TeVCat Name:TeV J1955+285
Other Names:SNR G065.1+00.6
3EG J1958+2909
PSR J1954+2836
3FGL J1954.2+2836
3HWC J1954+286
SNR G65.1+0.6
1LHAASO J1954+2836u
Source Type:UNID
R.A.:19 55 19.2 (hh mm ss)
Dec.:+28 35 24 (dd mm ss)
Gal Long: 65.35 (deg)
Gal Lat: 0.18 (deg)
Distance:
Flux: (Crab Units)
Energy Threshold: GeV
Spectral Index:2.4
Extended:No
Discovery Date:2017-02
Discovered By: HAWC
TeVCat SubCat:Default Catalog

Source Notes:

Source Position:

From Abeysekara et al. (2017):
- R.A. (J2000): 298.83 deg (= 19h 55m 19.2s)
- Dec. (J2000): +28.59 deg (= +28d 35' 24")
- the statistical uncertainty on the position is 0.14 deg
- the systematic uncertainty on the position is 0.1 deg

Source Extent:

From Abeysekara et al. (2017):
- "This source is found in the point search with a TS value of 25.4."

Spectral Properties:

From Abeysekara et al. (2017):
- spectral index: 2.40 +/- 0.24(stat) +/- 0.2(syst)

Source Association:

From Xing et al. (2022):
- "We carry out high-energy studies of the region of the Galactic TeV
source 3HWC J1954+286, whose location coincides with those of PSR
J1954+2836 and supernova remnant (SNR) G65.1+0.6. Analyzing the GeV
gamma-ray data obtained with the Large Area Telescope (LAT) onboard
the Fermi Gamma-ray Space Telescope, we are able to separate the
pulsar's emission from that of the region. Excess power-law-like
emission of a āˆ¼6 sigma significance level at the region is found, for
which we explain as arising from the SNR~G65.1+0.6. Given the
low-significance detection, either a hadronic or a leptonic model can
provide a fit to the power-law spectrum. Considering the properties of
the pulsar and the SNR, we discuss the possible origin of the TeV
source, and suggest that it is likely the TeV halo associated with the
pulsar."

From Abeysekara et al. (2018):
- "VERITAS sees a region of excess gamma-ray counts around 2HWC J1955+285.
The maximum pre-trial significance in this region is 3.5 sigma offset
by 0.35 deg from the position of the HAWC source. With the current
data set, it is unclear whether this is a weak source or simply a
statistical fluctuation."

From Abeysekara et al. (2017):
- "In this region, two sources are found nearby in the point source
search: 2HWC J1953+294 and 2HWC J1955+285, none of which has previous
TeV detection. 2HWC J1955+285, may be associated with the shell-type
supernova remnant SNR G065.1+00.6, located 0.5 deg away. The first
gamma-ray source in the region of SNR G065.1+00.6 was reported by the
COS-B satellite as 2CG 065+00 (Swanenburg et al. 1981), then confirmed
by the EGRET detection 3EG J1958+2909 (Hartman et al. 1999).
2HWC J1955+285 is near the energetic Fermi-LAT pulsar PSR J1954+2836 (0.2 deg
away, E-dot = 1.0Ɨ10e36 erg sāˆ’1, age = 69 kyr). Fermi-LAT also reported a
non observation of the SNR in Acero et al. (2016). Milagro reported a
4.3 sigma excess at this location (Abdo et al. 2009). MAGIC reported a non
detection and set a flux limit at 2ā€“3% of the Crab Nebula flux at
1 TeV (Aleksic et al. 2010)."

A PeVatron:

From Cao et al. (2024):
- This source is listed as being a UHE source in Table 2. This means
that it has a detection above 100 TeV at a significance level
corresponding to a test statistic of greater than 20.


Seen by: HAWC, LHAASO
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