Issue |
A&A
Volume 449, Number 1, April I 2006
|
|
---|---|---|
Page(s) | 243 - 250 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20054236 | |
Published online | 16 March 2006 |
The interior of the SNR RX J0852.0-4622 (Vela Jr) at radio wavelengths
1
Instituto de Astronomía y Física del Espacio (IAFE), CC 67, Suc. 28, 1428 Buenos Aires, Argentina e-mail: ereynoso@iafe.uba.ar
2
School of Physics, University of Sydney, NSW 2006, Australia
3
Australia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation, Post Office Box 76, Epping, NSW 1710, Australia
Received:
22
September
2005
Accepted:
23
November
2005
Aims.We observed the center of the supernova remnant Vela Jr in radio
continuum in order to search for a counterpart to the compact central X-ray
source CXOU J085201.4-461753, possibly a neutron star candidate which could be the remnant of
the supernova explosion.Methods.Observations were made with the Australia Telescope Compact Array at 13
and 20 cm. Spectral indices were obtained using flux density correlations
of the data which were spatially filtered to have the same coverage. A
multiwavelength search for counterparts to the compact central X-ray source
was made.Results.We compiled a new catalogue of 31 small diameter radio sources, including the
previously known source PMN J0853-4620, listing the integrated flux densities
at 20 cm and, for half of the sources, the flux densities at 13 cm with the
corresponding spectral indices. All sources are unresolved at the present
angular resolution except for Source 18, which is clearly elongated and lies
strikingly close to CXOU J085201.4-461753. Our observations show no evidence for the
existence of a pulsar wind driven nebula associated with the point X-ray
source. Furthermore, Source 18 has a thermal spectrum with index
(
), and appears to be the counterpart
of the optical source Wray 16-30. In spite of the absence of [O iii] emission
lines as reported in the literature, we find that this object could be
explained as a low emission planetary nebula belonging to the “butterfly”
morphological class.Conclusions.We conclude that if the radio source 18 is actually a planetary nebula, then
CXOU J085201.4-461753 is more likely to be related to it rather than to Vela Jr.
© ESO, 2006
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