| Canonical Name: | Vela Pulsar |
| TeVCat Name: | TeV J0835-453 |
| Other Names: | PSR B0833-45 |
| Source Type: | PSR |
| R.A.: | 08 35 20.7 (hh mm ss) |
| Dec.: | -45 10 35.2 (dd mm ss) |
| Gal Long: | 263.55 (deg) |
| Gal Lat: | -2.79 (deg) |
| Distance: | 0.29 kpc |
| Flux: | (Crab Units) |
| Energy Threshold: | 40 GeV |
| Spectral Index: | |
| Extended: | No |
| Discovery Date: | 2014-06 |
| Discovered By: | H.E.S.S. |
| TeVCat SubCat: | Default Catalog |
Source Notes:
This source was moved from the "Newly Announced" to the "Default"
catalogue on 180704 - see
H.E.S.S. Collaboration (2018).
This detection was announced at APP14/TeVPA and is available
here
Press release from 03 July 2014
here
Source Position:
The source position is taken from
SIMBAD who provide
Fey et al. (2004)
as the positional reference:
- R.A. (J2000): 08 35 20.7
- Dec. (J2000): -45 10 35.2
General Information:
From
H.E.S.S. Collaboration (2018):
- "At a period of 89 ms, the light curve of the pulsar exhibits two
peaks, labeled P1 and P2, separated by 0.43 in phase and connected by
a bridge emission, labeled P3."
Spectral Information:
From
H.E.S.S. Collaboration (2018):
- "A pulsed gamma-ray signal at a significance level of more than 15
sigma is detected from the P2 peak of the Vela pulsar light curve."
- "Of a total of 15835 events, more than 6000 lie at an energy below
20 GeV, implying a significant overlap between H.E.S.S. II-CT5 and the
Fermi-LAT."
- "While the investigation of the pulsar light curve with the LAT
confirms characteristics previously known up to 20 GeV, in the tens of
GeV energy range, CT5 data show a change in the pulse morphology of
P2, i.e., an extreme sharpening of its trailing edge, together with
the possible onset of a new component at 3.4 sigma significance
level."
- "Using both instruments data, it is however shown that the spectrum of P2 in
the 10-100 GeV has a pronounced curvature, i.e. a confirmation of the
sub-exponential cutoff form found at lower energies with the LAT."
- "... converging indications are found from both CT5 and LAT data for
the emergence of a hard component above 50 GeV in the leading wing
(LW2) of P2, which possibly extends beyond 100 GeV."
- "The fit of a power law to the overall data set above 20 GeV results
in:"
- Spectral index: 4.06 +/- 0.16 (stat)
- Normalisation: 30.6 +/- 1.9 (stat) at reference energy of 25 GeV
- Decorrelation energy: 21.5 GeV
- "The systematic uncertainties on normalization is -20% / +25% and on
index -0.2 / +0.3"
A TeV Halo?
From
Sudoh et al. (2019):
- "An intriguing edge case is the Vela pulsar (11 kyr, 280 pc). Vela
does not appear to produce a bright TeV halo (compared to the
luminosity expected if the formation efficiency is Geminga-like).
However, Vela does have dim, spatially-extended emission detected in
radio and GeV-TeV gamma-ray observations (
Abdo et al. 2010,
Abramowski et al. 2012,
Grondin et al. 2013,
Tibaldo et al. 2018).
This has historically been interpreted as a class of “relic PWN†that
are left behind after the interaction of the expanding PWN and the SNR
reverse shock, and which are powered by old electrons accumulated
since the birth of the pulsar (
Blondin et al. 2001,
de Jager et al. 2008,
Hinton et al. 2011,
Slane et al. 2018). Interestingly, the size of
this extended emission is ∼10 pc, comparable to that of observed TeV
halos. Thus, Vela could be interpreted as a transition case, where
inefficient TeV halos first form. Further TeV observations around
∼1–10 kyr pulsars are needed to study the properties of young
systems."
Seen by: H.E.S.S.
-
The Energy-dependent Gamma-Ray Light Curves and Spectra of the Vela Pulsar in the Dissipative Magnetospheres
Cao, Gang and Yang, Xiongbang, ApJ 962 p184 (2024) [LINK]
-
Absorption Line Observations of H3+ and CO in Sight Lines Toward the Vela and W28 Supernova Remnants
Indriolo, Nick, arXiv e-prints parXiv:2303.13689 (2023) [LINK]
-
Analysing the Time Period of the Vela pulsar
Goswami, Shreyan et al., Bulgarian Astronomical Journal 37 p108 (2022) [LINK]
-
Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit
Xie, Fei et al., Nature 612 p658-660 (2022) [LINK]
-
Probing the High-energy gamma-ray Emission Mechanism in the Vela Pulsar via Phase-resolved Spectral and Energy-dependent Light Curve Modeling
Barnard, Monica et al., arXiv e-prints parXiv:2111.03405 (2021) [LINK]
-
The Progenitor of the Vela Pulsar
Kochanek, C.S., arXiv e-prints parXiv:2110.11369 (2021) [LINK]
-
Very-High-Energy Emission From Pulsars
Harding, Alice K. et al., arXiv e-prints parXiv:2110.09412 (2021) [LINK]
-
Modelling pulsar emission in the high-energy and very-high-energy regimes
Barnard, M., arXiv e-prints parXiv:2103.10486 (2021) [LINK]
-
Measurement of High Energy Gamma Rays from 200 MeV to 1 TeV with the Alpha Magnetic Spectrometer on the International Space Station
Beischer, Bastian, arXiv e-prints parXiv:2007.08392 (2020) [LINK]
-
High-energy neutrinos from cosmic ray interactions in the Local Bubble
Bouyahiaoui, M. et al., arXiv e-prints parXiv:2001.00768 (2020) [LINK]
-
Rotationally-driven VHE emission from the Vela pulsar
Osmanov, Z. and Rieger, F.M., arXiv e-prints p (2019) [LINK]
-
On the Gamma-ray Nebula of Vela Pulsar. II. the Soft Spectrum of the Extended Radio Nebula
Bao, Yiwei and Chen, Yang, arXiv e-prints parXiv:1907.02038 (2019) [LINK]
-
On the Gamma-Ray Nebula of Vela Pulsar. I. Very Slow Diffusion of Energetic Electrons within the TeV Nebula
Bao, Yiwei et al., ApJ 877 p54 (2019) [LINK]
-
Multi-TeV Emission From the Vela Pulsar
Harding, A.K. et al., ArXiv e-prints p (2018) [LINK]
-
Timing analysis and pulse profile of the Vela pulsar in the optical band from Iqueye observations
Spolon, A. et al., ArXiv e-prints p (2018) [LINK]
-
First Ground-based Measurement of Sub-20 GeV to 100 GeV gamma-rays from the Vela Pulsar with H.E.S.S. II
H.E.S.S. Collaboration et al., ArXiv e-prints p (2018) [LINK]
-
High-energy Emission Properties of Pulsars
Venter, C. et al., ArXiv e-prints p (2018) [LINK]
-
High energy tails of pulsar gamma-ray emission
Richards, G. and Lyutikov, M., ArXiv e-prints p (2018) [LINK]
-
Modelling energy-dependent pulsar light curves
Venter, C. et al., ArXiv e-prints p (2017) [LINK]
-
The modeling of the Vela pulsar pulses - from optical to hard gamma-ray energy
Rudak, B. and Dyks, J., ArXiv e-prints p (2017) [LINK]
-
The Effect of an Offset Polar Cap Dipolar Magnetic Field on the Modeling of the Vela Pulsar's Gamma-Ray Light Curves
Barnard, M. et al., ApJ 832 p107 (2016) [LINK]
-
Very-high energy emission from pulsars
Breed, M. et al., ArXiv e-prints p (2016) [LINK]
-
Modeling of the gamma-ray pulsed spectra of Geminga, Crab, and Vela with synchro-curvature radiation
Vigano, D. and Torres, D.F., ArXiv e-prints p (2015) [LINK]
-
Very high energy emission as a probe of relativistic magnetic reconnection in pulsar winds
Mochol, I. and Petri, J., ArXiv e-prints p (2015) [LINK]
-
Fermi-LAT Detection of Pulsed Gamma-rays Above 50 GeV from the Vela Pulsar
Leung, G.C.K. et al., ArXiv e-prints p (2014) [LINK]
-
The Second Extension of the International Celestial Reference Frame: ICRF-EXT.1
Fey, A.L. et al., AJ 127 p3587-3608 (2004) [LINK]
-
Phase-resolved Studies of the High-Energy Gamma-Ray Emission from the Crab, Geminga, and VELA Pulsars
Fierro, J.M. et al., ApJ 494 p734-746 (1998) [LINK]
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