| Canonical Name: | 1ES 0033+595 |
| TeVCat Name: | TeV J0035+598 |
| Other Names: | |
| Source Type: | HBL |
| R.A.: | 00 35 16.8 (hh mm ss) |
| Dec.: | +59 47 24.0 (dd mm ss) |
| Gal Long: | 120.90 (deg) |
| Gal Lat: | -3.02 (deg) |
| Distance: | z=0.467 |
| Flux: | 0.015 (Crab Units) |
| Energy Threshold: | 150 GeV |
| Spectral Index: | 3.8 |
| Extended: | No |
| Discovery Date: | 2011-10 |
| Discovered By: | MAGIC |
| TeVCat SubCat: | Default Catalog |
Source Notes:
141028: This source was moved to the Default Catalog.
Positional Information:
From
Aleksic et al. (2014):
- The position was updated to this one on 141029:
- R.A. (J2000): 00 35 16.8
- Dec. (J2000): +59 47 24.0
- "The fitted position of the signal is RA: 0.588 +/- 0.002 h and
DEC: 59.79 +/- 0.02 deg (J2000.0), which, when taking into account the
weakness and steepness of the source and the systematic uncertainty in
the pointing position of the MAGIC stereo system, is consistent with
the catalog cordinates reported in
Giommi et al. (2002)"
From
Mariotti (2011):
- R.A. (J2000): 00:35:52.63
- Dec. (J2000): 59:50:04.56
- very close to
SIMBAD position
- no uncertainty quoted on the position
Spectral Information:
From
Aleksic et al. (2014):
- spectral index: 3.8 +/- 0.7(stat) +/- 0.3(syst)
- for an energy range between 125 GeV and 500 GeV
Distance:
The redshift was updated from unknown to z = 0.467 on 170119 (see details below)
From
Paiano et al. (2016):
"We found an emission feature at 5468 Ang of EW = 0.4 A. This feature
is detected in all three individual spectra and therefore we consider
it a secure detection. If identified as [OII] 3727 Ang emission, a
tentative redshift of z = 0.467 can be provided."
From
Aleksic et al. (2014):
- using the method of
Prandini et al. (2010), "a value of
z = 0.58 +/- 0.12 is obtained which corresponds to an upper limit on the redshift."
- "An estimate of the likely redshift can be obtained using the
inverse formula of
Prandini et al. (2010), resulting in
z = 0.34 +/- 0.08 +/- 0.05, where the first error (0.08) was
calculated based on the uncertainties in photon indices of the source
spectra measured by MAGIC and Fermi LAT, while the second error (0.05)
is the method uncertainty, which comes from the spread in the results
after applying the method to known redshift sources.
Seen by: MAGIC
-
Long-term optical monitoring of TeV emitting blazars. I. Data analysis
Nilsson, K. et al., A&A 620 pA185 (2018) [LINK]
-
On the redshift of TeV BL Lac objects
Paiano, S. et al., ArXiv e-prints p (2017) [LINK]
-
Discovery of very high energy gamma-ray emission from the blazar 1ES 0033+595 by the MAGIC telescopes
Aleksic, J. et al., ArXiv e-prints p (2014) [LINK]
-
Discovery of the long hunted blazar 1ES 0033+595 by the MAGIC telescopes
Uellenbeck, M. et al., 1505 p494-497 (2012) [LINK]
-
VHE detection of the blazar 1ES 0033+595 by MAGIC
Mariotti, M., The Astronomer's Telegram 3719 p1-+ (2011) [LINK]
-
The BeppoSAX View of Extreme BL Lacs
Costamante, L. et al., p21 (2002) [LINK]
-
Extreme synchrotron BL Lac objects. Stretching the blazar sequence
Costamante, L. et al., A&A 371 p512-526 (2001) [LINK]
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