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Observation Date (UT) Observation Lat

Canonical Name:TeV J2032+4130
TeVCat Name:TeV J2032+415
Other Names:0FGL J2032.2+4122
MGRO J2031+41
2HWC J2031+415
VER J2032+414
MAGIC J2032+4127
PSR J2032+4127
MT91 213
2HWC J2031+415
Source Type:PWN
R.A.:20 31 33 (hh mm ss)
Dec.:+41 34 38 (dd mm ss)
Gal Long: 80.25 (deg)
Gal Lat: 1.20 (deg)
Distance: 1.8 kpc
Flux:0.03 (Crab Units)
Energy Threshold:1000 GeV
Spectral Index:2
Size (X):0.19 (deg)
Size (Y):0.08 (deg)
Discovery Date:2002-10
Discovered By: HEGRA
TeVCat SubCat:Default Catalog

Source Notes:

TeV J2032+4130 is co-located with PSR J2032+4127, and may be physically associated with it.

Source position and its uncertainty:
On 181018 the source position was updated from that of Aharonian et al. (2002)
to that of VERITAS and MAGIC Collaborations (2018).

From VERITAS and MAGIC Collaborations (2018):
- R.A. (J2000): 20h 31m 33s +/- 2s (stat) +/- 2s (syst)
- Dec. (J2000): +41d 34' 38'' +/- 36'' (stat) +/- 36'' (syst)
- R.A. (J2000): 20h 31m 39.7s +/- 2s (stat)
- Dec. (J2000): +41d 34' 23'' +/- 20'' (stat)
From Abdo et al. (2012):
- R.A. (J2000): 20h 28m 43.2s
- Dec. (J2000): +41d 18' 36"
From Bartoli et al. (2012):
- R.A. (J2000) 307.85deg = 20h 31m 24s
- Dec. (J2000): 41.75 deg = 41d 45' 00"
- No information on the uncertainty in the position is provided.
From Abdo et al. (2009):
- R.A. (J2000): 20h 31m 43s
- Dec. (J2000): 40d 40'
... +/- 0.3 deg (stat)
From Albert et al. (2008):
- R.A. (J2000): 20h 32m 20s +/- 11s(stat) +/- 11s(syst)
- Dec. (J2000): 41d 30' 36"0s +/- 1.2'(stat) +/- 1.8'(syst)
From Konopelko et al. (2007):
- R.A. (J2000): 20h 32m 27s +/- 21s(stat) +/- 32s(syst)
- Dec. (J2000): 41d 39' 17" +/- 5'(stat) +/- 6'(syst)
From Aharonian et al. (2005):
- R.A. (J2000): 20h 31m 57s +/- 6.2s(stat) +/- 13.7s(syst)
- Dec. (J2000): 41d 29' 56"8s +/- 1.1'(stat) +/- 1.0'(syst)
From Aharonian et al. (2002):
- R.A. (J2000): 20h 32m 07s +/- 9.2s(stat) +/- 2.2s(syst)
- Dec. (J2000): 41d 30' 30" +/- 2.0'(stat) +/- 0.4'(syst)

Source Extent:
On 181018 the source extent was updated from that of Aharonian et al. (2002)
to that of VERITAS and MAGIC Collaborations (2018).

From VERITAS and MAGIC Collaborations (2018):
- semi-major axis: 0.19deg +/- 0.02deg (stat) +/- 0.01deg (syst)
- semi-minor axis: 0.08deg +/- 0.01deg (stat) +/- 0.03deg (syst)
- angle: 41deg +/- 4deg (stat) +/- 1deg (syst) east of north
- semi-major axis: 0.125deg +/- 0.01deg (stat)
- semi-minor axis: 0.08deg +/- 0.01deg (stat)
- angle: 34deg +/- 2deg (stat) east of north
From Abdo et al. (2012):
- A fit of a two-dimensional Gaussian gives sigma = 1.8 deg (radius)
From Bartoli et al. (2012):
- radius: 0.2deg +0.4deg -0.2deg (=12' +24' -12')
From Abdo et al. (2009):
- spatial extent: 3.0 +/- 0.9 deg
"... much larger than the few-arcminute extent of TeV J2032+413
...There must be another source or sources contributing the Milagro excess."
From Albert et al. (2008):
- radius: 5.0' +/- 1.7(stat) +/- 0.6(sys) (= 0.08 +/- 0.03 deg)
From Konopelko et al. (2007):
- Based on the data reported here, the source seen with the Whipple
Observatory 10 m telescope is consistent with a pointlike gamma-ray
source. At the same time, given a 7.6' width of the PSF for the 10 m
Whipple collaboration telescope, we cannot distinguish between a point
source and a diffuse source with extent less than a 6'. Thus, the
Whipple source is consistent with HEGRA source in terms of its extension
From Aharonian et al. (2005):
- radius: 6.2' +/- 1.2'(stat) +/- 0.9'(syst) (= 0.10 +/- 0.02 deg)
From Aharonian et al. (2002):
- radius: 5.6' +/- 1.7'

From The ARGO-YBJ Collaboration (2013):
- "the measured flux is also higher than that measured by IACTs, but
with a discrepancy of more than a factor 10."
From Abdo et al. (2012):
- Flux normalisation for a power law is 2.1 +0.6(stat) -0.6(stat) x10e-10 s-1 m-2 TeV-1 at 10TeV
- The overall flux is subject to a 30% syst. uncertainty
From Bartoli et al. (2012):
- 31% Crab at energies above 1 TeV
From Abdo et al. (2009):
- The flux quoted is 0.39 Crab when the flux at
35 TeV of 63.3e-17 /TeV /s /cm2 is compared with that
from the Crab (162.6e-17 /TeV /s /cm2)
also quoted at 35 TeV.
From Albert et al. (2008):
- 3% Crab
From Konopelko et al. (2007):
- 8% Crab
From Aharonian et al. (2005):
- 5% Crab
From Aharonian et al. (2002):
- 3% Crab

Spectral Information:
From Abdo et al. (2012):
- the preferred spectral fit is a power law
- Spectral index: 3.22 +0.23(stat) -0.18(stat) +/- 0.1(syst)
From Bartoli et al. (2012):
- Spectral index: 2.83 +/- 0.37
From Albert et al. (2008):
- Spectral index: 2.0 +/- 0.3(stat) +/- 0.2(syst)
From Konopelko et al. (2007):
- the signal does not have sufficient strength to
measure its gamma-ray spectrum adequately
From Aharonian et al. (2002):
- Spectral index: 1.9 +/- 0.3(stat) +/- 0.3(syst)

From Camilo et al. (2009):
- A distance of approximately 1.8 kpc is proposed.

Source Classification:
From Abeysekara et al. (2017):
- "Source 2HWC J2031+415 is associated with TeV J2031+4130, a PWN
first reported as unidentified in TeV by HEGRA (Aharonian et al. 2002).
Various IACTs have reported point-like or up to 0.2deg extended
emissions from the pulsar position, with consistent spectra
(Lang et al. 2004; Albert et al. 2008; Aliu et al. 2014). Milagro
and ARGO have reported extended emission compatible with the Cygnus
Cocoon, as mentioned above. The HAWC flux is more consistent with the
flux measured by Milagro and ARGO than the IACTs, in agreement with
possible additional emission components besides the PWN within the
From Linden et al. (2017):
- the authors propose that this object is a member of a new class of
TeV emitters - "extrended TeV halos"
- "Observations by HAWC and Milagro have detected bright and spatially
extended TeV gamma-ray sources surrounding the Geminga and Monogem
pulsars. We argue that these observations, along with a substantial
population of other extended TeV sources coincident with pulsar wind
nebulae, constitute a new morphological class of spatially extended
TeV halos."
140702: The source classification was updated from UNID to PWN due to
the analyses described below.
From Camilo et al. (2009):
- A PWN is proposed as the source class for this TeV emission.
- "PSR J2032+4127 is located within the 1sigma extent of TeV
J2032+4130, only 4' from its HEGRA centroid. We therefore propose its
PWN as the source of TeV J2032+4130. Further support for the
association of PSR J2032+4127 with TeV J2032+4130 comes from comparing
their properties with those of other TeV PWNe."
From Bednarek (2003):
- "We argue that gamma-ray sources observed in the direction of the
Cygnus OB2 association in the GeV and TeV energy range are due to a
pulsar that was created by a supernova a few tens of thousands of
years ago. The GeV emission is produced by a middle-aged pulsar, a
factor of 2 older than the Vela pulsar. The TeV emission is produced
by high-energy hadrons and/or leptons accelerated in pulsar wind

Seen by: HEGRA, Whipple, Crimea, Milagro, ARGO-YBJ, HAWC
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