Issue |
A&A
Volume 497, Number 1, April I 2009
|
|
---|---|---|
Page(s) | 167 - 176 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/200811385 | |
Published online | 18 February 2009 |
Observational and theoretical constraints for an Hα-halo around the Crab nebula *,**
1
Department of Astronomy, AlbaNova University Center, Stockholm University, 106 91 Stockholm, Sweden e-mail: anestis@astro.su.se
2
Isaac Newton Group of Telescopes, Calle Alvarez Abreu 68 2, 38700 Santa Cruz de La Palma, Spain
3
Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
Received:
20
November
2008
Accepted:
5
February
2009
Aims. We searched for a fast moving Hα shell around the Crab nebula. Such a shell could account for this supernova remnant's missing mass, and carry enough kinetic energy to make SN 1054 a normal type II event.
Methods. Deep Hα images were obtained with WFI at the 2.2 m MPG/ESO telescope and with MOSCA at the 2.56 m NOT. The data are compared with theoretical expectations derived from shell models with ballistic gas motion, constant temperature, constant degree of ionisation, and a power law for the density profile.
Results. We reach a surface brightness limit of 5 10-8 erg s-1 cm-2 sr-1. A halo is detected,
but at a much higher surface brightness than our models of recombination
emission and dust scattering predict. Only collisional excitation of
Lyβ with partial de-excitation to Hα could explain such
amplitudes. We show that the halo seen is caused by PSF scattering and thus not
related to a real shell. We also investigated the feasibility of a
spectroscopic detection of high-velocity Hα gas towards the centre of
the Crab nebula. Modelling the emission spectra shows that such gas
easily evades detection in the complex spectral environment of the
Hα-line.
Conclusions. PSF scattering significantly contaminates our data, preventing a detection of
the predicted fast shell. A real halo with observed peak flux of about
2 10-7 erg s-1 cm-2 sr-1 could still be accomodated within our error bars, but our
models predict a factor 4 lower surface brightness. Eight meters class telescopes
could detect such fluxes unambiguously, provided that a sufficiently
accurate PSF model is available. Finally, we note that PSF scattering also
affects other research areas where faint haloes are searched for around
bright and extended targets.
Key words: ISM: supernova remnants / stars: supernovae: individual: SN1054
© ESO, 2009
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.