| Canonical Name: | CTA 1 |
| TeVCat Name: | TeV J0006+729 |
| Other Names: | SNR G119.5+10.2,
VER J0006+729,
1LHAASO J0007+7303u |
| Source Type: | PWN |
| R.A.: | 00 06 26 (hh mm ss) |
| Dec.: | +72 59 01.0 (dd mm ss) |
| Gal Long: | 119.60 (deg) |
| Gal Lat: | 10.40 (deg) |
| Distance: | 1.4 kpc |
| Flux: | 0.04 (Crab Units) |
| Energy Threshold: | 1000 GeV |
| Spectral Index: | 2.2 |
| Extended: | Yes |
| Size (X): | 0.30 (deg) |
| Size (Y): | 0.24 (deg) |
| Discovery Date: | 2011-10 |
| Discovered By: | VERITAS |
| TeVCat SubCat: | Default Catalog |
Source Notes:
Source Position:
From
LHAASO Collaboration (2024):
- For each of the energy ranges, the centroid is quoted for the
benchmark spatial model, the Gaussian profile:
E > 100 TeV:
- R.A. (J2000): 00 07 04.8 (1.77 deg)
- Dec. (J2000): +73 03 36 (73.06 deg)
- 95% statistical uncertainty: 0.08 deg
E: 8-100 TeV:
- R.A. (J2000): 00 06 38.8 (1.66 deg)
- Dec. (J2000): +73 04 48 (73.08 deg)
- 95% statistical uncertainty: 0.06 deg
From
Aliu et al. (2012):
- R.A. (J2000): 00h 06m 26s +/- 0.09 deg
- Dec. (J2000): +72d 59' 01.0" +/- 0.04deg
- Systematic uncertainty: 50"
Spectral Information:
From
LHAASO Collaboration (2024):
- "The energy spectrum is well described by a power-law with an exponential cutoff function:
... dN/dE= (42.4 +/- 4.1)(E/20 TeV)^-2.31 +/- 0.11 exp(-E/110 +/- 25 TeV) TeV−1 cm−2 s−1
in the energy range from 8 TeV to 300 TeV"
From
Aliu et al. (2012):
- Spectral index: 2.2 +/- 0.2(stat) +/- 0.3(syst)
Source Morphology:
From
LHAASO Collaboration (2024):
- "This source is well detected with significances of 21 sigma and 17
sigma at 8-100 TeV and >100 TeV, respectively. The corresponding
extensions are determined to be (0.23 +/-0.03) deg and (0.17 +/- 0.03) deg"
From
Aliu et al. (2012):
- semi-major axis: 0.30deg
- semi-minor axis: 0.24deg
Source Classification:
From
Martin et al. (2016):
- "We estimate the molecular mass around CTA 1 using data from Planck
and the Harvard CO survey. We observe that the molecular mass in the
vicinity of the complex is not enough to explain the TeV emission
observed by VERITAS, even under favorable assumptions for the
cosmic-ray acceleration properties of the supernova remnant. This
supports the idea that the TeV emission comes from the PWN. "
From
Acero et al. (2013):
- This LAT emission from this source below 10 GeV is likely from a
pulsar
Seen by: VERITAS
-
Deep view of Composite SNR CTA1 with LHAASO in gamma-rays up to 300 TeV
LHAASO Collaboration, arXiv e-prints parXiv:2409.09499 (2024) [LINK]
-
Possible GeV gamma-ray emission from the pulsar wind nebula in CTA 1
Zhou, Liancheng et al., MNRAS 529 p3593-3600 (2024) [LINK]
-
Molecular environment, reverberation, and radiation from the pulsar wind nebula in CTA 1
Martin, J. et al., ArXiv e-prints p (2016) [LINK]
-
Search for radio counterpart of the Fermi/VERITAS PWN candidate in the SNR CTA 1
Giacani, E. et al., ArXiv e-prints p (2014) [LINK]
-
Discovery of TeV Gamma-Ray Emission from CTA 1 by VERITAS
Aliu, E. et al., ApJ 764 p38 (2013) [LINK]
-
Constraints on the Galactic Population of TEV Pulsar Wind Nebulae Using Fermi Large Area Telescope Observations
Acero, F. et al., ArXiv e-prints p (2013) [LINK]
-
VERITAS observation of CTA1
Park, N. and VERITAS Collaboration, 1505 p354-357 (2012) [LINK]
-
Observations of SNR CTA 1 and the Cyg OB1 region with VERITAS
Aliu, E., ArXiv e-prints p (2011) [LINK]
-
VHE Observation of CTA 1 with VERITAS
McArthur, S. and for the VERITAS Collaboration, ArXiv e-prints p (2011) [LINK]
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