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Observation Date (UT) Observation Lat

Canonical Name:SNR G106.3+02.7
TeVCat Name:TeV J2227+608
Other Names:VER J2227+608
HAWC 2227+610
Source Type:Shell
R.A.:22 27 59 (hh mm ss)
Dec.:+60 52 37 (dd mm ss)
Gal Long: 106.35 (deg)
Gal Lat: 2.71 (deg)
Distance: 0.8 kpc
Flux:0.05 (Crab Units)
Energy Threshold:1000 GeV
Spectral Index:2.29
Size (X):0.27 (deg)
Size (Y):0.18 (deg)
Discovery Date:2009-07
Discovered By: VERITAS
Green's Catalog:Link
TeVCat SubCat:Default Catalog

Source Notes:

Source position and its uncertainty:
From Acciari et al. (2009):
- R.A. (J2000): 22h 27m 59s +/- 0.07 deg (stat)
- Dec. (J2000): 60d 52' 37" +/- 0.04 deg (stat)
- there is an additional combined systematic uncertainty of 0.07deg

Source Extent:
From Acciari et al. (2009):
- semi-major axis: 0.27 +/- 0.05 deg
- semi-minor axis: 0.18 +/- 0.03 deg
- angle: 22 deg east of north

Spectral Index:
From Acciari et al. (2009):
- 2.29 +/- 0.33(stat) +/- 0.30(syst)

Source Association:

From Cao et al. (2021):
- SNR G106.3+02.7 / VER J2227+608 / HAWC 2227+610 may be associated with LHAASO J2226+6057

From Fujita et al. (2021):
- "We report a discovery of diffuse X-ray emission around the
supernova remnant (SNR) G106.3+2.7, which is associated with VER
J2227+608 and HAWC J2227+610 and is known as a candidate for a PeV
cosmic ray accelerator (PeVatron)."
- "We analyze observational data of Suzaku around the SNR and the
adjacent pulsar PSR J2229+6114."
- "We find diffuse X-ray emission that is represented by either
thermal or non-thermal one."
- "The intensity of the diffuse emission increases toward PSR
J2229+6114 in the same way as radio emission, and it is in contrast
with gamma-ray emission concentrated on a molecular cloud. The X-ray
photon index does not change with the distance from the pulsar and it
indicates that radiative cooling is ineffective and particle diffusion
is not extremely slow. The X-ray and radio emissions seem to be of
leptonic origin and the parent electrons may originate from the pulsar
or its wind nebula. The gamma-ray emission appears to be of hadronic
origin because of its spacial distribution. The parent protons may be
tightly confined in the cloud separately from the diffusing

From Xin et al. (2019):
- "We report the detection of GeV gamma-ray emission from the
very-high-energy (VHE) gamma-ray source VER J2227+608 associated with
the “tail” region of SNR G106.3+2.7. The GeV gamma-ray emission is
extended and spatially coincident with molecular clouds traced by CO
emission. The broadband GeV to TeV emission of VER J2227+608 can be
well fitted by a single power-law function with an index of 1.90 +/- 0.04,
without obvious indication of spectral cutoff toward high energies"
- The authors propose that a hadronic model could describe the gamma-ray emission
and: "suggest that VER J2227+608 may be powered by the PWN instead of
shocks of the SNR."

From Acciari et al. (2009):
- Could be associated with PSR J2229+6114 (Boomerang)

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