2007A&A...473..883M


C.D.S. - SIMBAD4 rel 1.7 - 2020.06.05CEST00:06:16

2007A&A...473..883M - Astronomy and Astrophysics, volume 473, 883-889 (2007/10-3)

VLT observations of the central compact object in the Vela Jr. supernova remnant.

MIGNANI R.P., DE LUCA A., ZAGGIA S., SESTER D., PELLIZZONI A., MEREGHETTI S. and CARAVEO P.A.

Abstract (from CDS):

X-ray observations have unveiled the existence of enigmatic point-like sources at the center of young (a few kyrs) supernova remnants. These sources, known as central compact objects (CCOs), are thought to be neutron stars produced by the supernova explosion, although their X-ray phenomenology makes them markedly different from all other young neutron stars discovered to date. The aim of this work is to search for the optical/IR counterpart of the Vela Junior CCO and to understand the nature of the associated Hα nebula discovered by Pellizzoni et al. (2002A&A...393L..65P).We used deep optical (R-band) and IR (J,H,Ks-bands) observations recently performed by our group with the ESO VLT to obtain the first deep, high resolution images of the field to resolve the nebula structure and pinpoint a point-like source possibly associated with the neutron star.Our R-band image shows that the nebula's flux and structure are very similar to those of, the Hα one, suggesting that the nebula spectrum is dominated by pure Hα line emission. However, the nebula is not detected in our IR observations, which makes it impossible to to constrain its spectrum. A faint point-like object (J≥22.6, H∼21.6, Ks∼21.4 ) compatible with the neutron star's Chandra X-ray position is detected in our IR images (H and Ks) but not in the optical image (R>25.6), where it is buried by the nebula background. The nebula is most likely a bow-shock produced by the neutron star motion through the ISM or, alternatively, a photo-ionization nebula powered by UV radiation from a hot neutron star. A synchrotron nebula, powered by the relativistic particle wind from the neutron star, is the less likely interpretation because of its non-detection in the X-rays and the apparent lack of continuum emission. The candidate CCO counterpart could be the neutron star itself, a fallback disk left over from the supernova explosion, or a mid M-type star, or later, at a distance of 2kpc.

Abstract Copyright:

Journal keyword(s): stars: neutron - X-rays: individual: CXO J085201.4-461753 - ISM: supernova remnants

Status at CDS:  

Simbad objects: 16

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Number of rows : 16

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 J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 504 0
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5624 1
3 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4789 1
4 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5580 4
5 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 795 3
6 NAME Geminga Psr 06 33 54.153 +17 46 12.91           ~ 1089 0
7 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1107 2
8 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545           ~ 2046 1
9 Ve 7-27 Em* 08 51 59.6873349537 -46 18 07.268122029   14.87 13.88 14.59 12.96 ~ 46 1
10 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 399 2
11 2XMM J085201.4-461753 X 08 52 01.4 -46 17 53           ~ 36 1
12 HD 76060 * 08 52 02.4492422465 -46 17 19.841772188   7.79 7.88     B8IV/V 20 0
13 NAME Vela Z Rad 08 53 30 -45 35.0           ~ 28 0
14 SNR G295.5+09.7 SNR 12 09 40 -52 25.0           ~ 254 1
15 PKS 1613-50 Rad 16 17 33.000 -51 02 00.00           ~ 452 3
16 PSR J1959+2048 Psr 19 59 36.7480 +20 48 14.599   20.4       ~ 695 2

    Equat.    Gal    SGal    Ecl

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2020.06.05-00:06:16

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