2009A&A...508..779M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST11:53:53

2009A&A...508..779M - Astronomy and Astrophysics, volume 508, 779-782 (2009/12-3)

HST observations of the nebula around the central compact object in the Vela Jr. supernova remnant.

MIGNANI R.P., DE LUCA A. and PELLIZZONI A.

Abstract (from CDS):

A handful of young (a few thousand years) supernova remnants (SNRs) host point-like X-ray sources, dubbed central compact objects (CCOs), which are thought to be radio-silent isolated neutron stars formed by the supernova explosion. So far, no CCO has been firmly detected at other wavelengths. However, ground-based observation in the Hα band detected a nebula around CXOJ085201.4-461753, the CCO in the Vela Jr. SNR. The nebula has also been detected in deep R-band observations performed with the Very Large Telescope (VLT). Interestingly, both its extension and its flux in the R band are consistent with those measured in Hα, suggesting that the nebula spectrum is dominated by line emission, possibly produced by a velocity-driven bow-shock in the interstellar medium (ISM) or by its photo-ionisation from the neutron star. The aim of this work is to resolve the morphology of the Hα nebula around the CCO to verify the proposed interpretations. We performed high-resolution imaging observations of the nebula with the Wide Field Planetary Camera 2 (WFPC2) of the Hubble Space Telescope (HST) through the 656N filter, almost exactly centred on the rest wavelength of the Hα line. Surprisingly enough, we did not detect the nebula in our WFPC2 image down to a 3σ flux limit of ∼3x10–15erg/cm2/s. This limit is a factor of 10 fainter than the nebula flux measured in the discovery ground-based observations which were, however, performed with redder and broader Hα filters. The non-detection of the nebula in the narrower and bluer WFPC2 656N filter suggests that the peak of the emission might actually be at longer wavelengths. One possibility, compatible with the bow-shock scenario only, is that the Hα line is red-shifted by ∼10-60Å due to the neutron star motion with a radial velocity 450≲Vr≲2700km/s. The other possibility is that the nebula is a knot of [NII] emission (λ= 6583.6Å) unrelated to CXOJ085201.4-461753 and possibly associated with the nearby star Wray 16-30. High-resolution spectroscopy observations will help to settle the nature of the nebula.

Abstract Copyright:

Journal keyword(s): stars: neutron - ISM: supernova remnants - ISM: clouds

Simbad objects: 11

goto Full paper

goto View the reference in ADS

Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 PSR J0821-4300 Psr 08 21 58.2 -43 00 22           ~ 113 2
2 NAME Pup A SNR 08 24 07 -42 59.8           ~ 517 1
3 Ve 7-27 Em* 08 51 59.6873349537 -46 18 07.268122029   14.87 13.88 14.59 12.96 ~ 46 1
4 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 400 2
5 2XMM J085201.4-461753 X 08 52 01.4 -46 17 53           ~ 37 1
6 HD 76060 * 08 52 02.4492422465 -46 17 19.841772188   7.79 7.88     B8IV/V 20 0
7 SNR G295.5+09.7 SNR 12 09 40 -52 25.0           ~ 255 1
8 PSR J1210-5226 Psr 12 10 00.88 -52 26 28.4           ~ 202 1
9 SNR G033.6+00.1 SNR 18 52 29.000 +00 38 42.00           ~ 239 1
10 PSR J1852+0040 Psr 18 52 38.49 +00 40 19.8           ~ 72 1
11 PSR B2223+65 Psr 22 25 52.36 +65 35 33.8           ~ 287 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2009A&A...508..779M and select 'bookmark this link' or equivalent in the popup menu


2020.07.12-11:53:53

© Université de Strasbourg/CNRS

    • Contact