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

Mignani, Roberto; Luca, A. De

doi:10.1051/0004-6361/200913028

Cited by 5 publications

(14 citation statements)

References 16 publications

(24 reference statements)

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“…Interestingly, the Vela Jr. CCO features an optical nebulosity detected in the R band with the VLT and also detected in the H α line, which has been interpreted as either a bow-shock, produced by the neutron star motion in the ISM, or a photo-ionisation nebula (Mignani et al 2007b,d). However, new HST observations (Mignani et al 2009e) apparently contradict the latter scenario. For the CCO in RCW 103, often suspected to be in a binary system because of its transient X-ray emission and its 6 hours periodicity, a candidate counterpart was proposed (Pavlov et al 2004) For the RRATs, a search for bursting optical emission from J1819−1458 was carried out by Dhillon et al (2006) but with negative results.…”

Section: Central Compact Objects (Ccos)mentioning

confidence: 99%

Optical, ultraviolet, and infrared observations of isolated neutron stars

Mignani¹

2011

Advances in Space Research

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Forty years passed since the optical identification of the first isolated neutron star (INS), the Crab pulsar. 25 INSs have been now identified in the optical (O), near-ultraviolet (nUV), or near-infrared (nIR), hereafter UVOIR, including rotation-powered pulsars (RPPs), magnetars, and X-ray-dim INSs (XDINSs), while deep investigations have been carried out for compact central objects (CCOs), Rotating RAdio transients (RRATs), and high-magnetic field radio pulsars (HBRPs). In this review I describe the status of UVOIR observations of INSs, their emission properties, and I present the results from recent observations.

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Section: Central Compact Objects (Ccos)mentioning

confidence: 99%

Optical, ultraviolet, and infrared observations of isolated neutron stars

Mignani¹

2011

Advances in Space Research

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“…evidence of X-ray pulsations (Becker et al 2006) or of a known radio pulsar at this location. 3 The object does lie in or near a 6 arcsec-diameter optically-emitting nebula (Pellizzoni et al 2002;Mignani et al 2007), at least on the plane of the sky, but it is not clear that the detected optical (Hα or [NII]) source and the X-ray source are the same object (Mignani et al 2009).…”

Section: Introductionmentioning

confidence: 99%

ON THE EXPANSION RATE, AGE, AND DISTANCE OF THE SUPERNOVA REMNANT G266.2–1.2 (Vela Jr.)

Allen

Chow

DeLaney

et al. 2014

ApJ

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An analysis of Chandra ACIS data for two relatively bright and narrow portions of the northwestern rim of G266.2−1.2 (a.k.a. RX J0852.0-4622 or Vela Jr.) reveal evidence of a radial displacement of 2.40 ± 0.56 arcsec between 2003 and 2008. The corresponding expansion rate (0.42±0.10 arcsec yr −1 or 13.6±4.2% kyr −1 ) is about half the rate reported for an analysis of XMM-Newton data from a similar, but not identical, portion of the rim over a similar, but not identical, time interval (0.84±0.23 arcsec yr −1 , Katsuda et al. 2008a). If the Chandra rate is representative of the remnant as a whole, then the results of a hydrodynamic analysis suggest that G266.2−1.2 is between 2.4 and 5.1 kyr old if it is expanding into a uniform ambient medium (whether or not it was produced by a Type Ia or Type II event). If the remnant is expanding into the material shed by a steady stellar wind, then the age could be as much as 50% higher. The Chandra expansion rate and a requirement that the shock speed be greater than or equal to 1000 km s −1 yields a lower limit on the distance of 0.5 kpc. An analysis of previously-published distance estimates and constraints suggests G266.2−1.2 is no further than 1.0 kpc. This range of distances is consistent with the distance to the nearer of two groups of material in the Vela Molecular Ridge (0.7 ± 0.2 kpc, Liseau et al. 1992) and to the Vel OB1 association (0.8 kpc, Eggen 1982).Subject headings: ISM: individual objects (G266.2−1.2) -ISM: supernova remnants -shock waves -X-rays: individual (G266.2−1.2)

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“…In the Hα band (Fig.2b) the nebula is more clearly resolved against Star Z than in the UKST image, with a clear maximum of emission at the centre of symmetry. This seems to indicate that the two objects are detached and, thus, that the nebula cannot be an unipolar gas outflow from Star Z (see also, Mignani et al 2009b). We qualitatively compared the Omegacam image of the nebula (May 11 2015) with the UKST (November 9 1999) Hα image of Pellizzoni et al (2002) to look for possible long-term variations in morphology and/or surface brightness associated with the displacement of the hypothetical bow-shock as CXO J085201.4−461753 moves in the ISM.The comparison is shown in Fig.…”

Section: Multi-band Imagingmentioning

confidence: 95%

“…Furthermore, the Omegacam observations provide the highest spatial resolution Hα images of the nebula and of the complex of bright arc-like structures observed 30 -40 West of CXO J085201.4−461753 ( Fig.2a) obtained so far. Indeed, the former is not detected in the HST images of Mignani et al (2009b) whereas the latter falls only marginally in the WFPC2 mosaiced image. These structures are seen through the NB 659 filter but not through the broad-band ones, 10 The nebula was indeed detected in the R band only thanks to the longer integration (5200 s) and the larger collecting area of the VLT (Mignani et al 2007).…”

Section: Multi-band Imagingmentioning

confidence: 96%

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The nature of the infrared counterpart and of the optical nebula associated with the Central Compact Object in Vela Jr.

Mignani

Luca

Zharikov

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The X-ray source CXO J085201.4−461753 in the few kyr-old Vela Jr. supernova remnant (G266.2-1.2) belongs to the peculiar class of isolated neutron stars dubbed "Central Compact Objects" (CCOs). At variance with the other CCOs, which are only detected in the X-rays, CXO J085201.4−461753 has been possibly detected also at other wavelengths. In particular, a candidate near-infrared counterpart (H = 21.6 ±0.1) was detected by the Very Large Telescope (VLT) in addition to a 6 -wide nebula detected in Hα, interpreted as a velocitydriven bow-shock. Here, we present new near-infrared and optical VLT observations of the candidate counterpart to CXO J085201.4−461753 and its nebula to confirm the proposed associations. Moreover, we used archival Chandra observations to measure for the first time the CXO J085201.4−461753 proper motion. The comparison between the two sets of nearinfrared VLT images, taken 10.56 year apart, do not show evidence of proper motion for the candidate counterpart to CXO J085201.4−461753, expected from its 4 offset from the SNR geometrical centre, with a 3σ upper limit of ∼ 10 mas yr −1 . This is much smaller than the expected proper motion of ∼50-100 mas yr −1 , which, in turn, is below the 3σ upper limit of ∼ 300 mas yr −1 that we obtained with Chandra. At the same time, VLT spectroscopy resolved the nebula optical emission, which is dominated by the NII doublet at 6548 and 6584 A and not by Hα. To summarise, we conclude that the proposed near-infrared counterpart is likely unassociated with CXO J085201.4−461753 and that the nebula is not a velocity-driven bow-shock.

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

Cited by 5 publications

References 16 publications

Optical, ultraviolet, and infrared observations of isolated neutron stars

Optical, ultraviolet, and infrared observations of isolated neutron stars

ON THE EXPANSION RATE, AGE, AND DISTANCE OF THE SUPERNOVA REMNANT G266.2–1.2 (Vela Jr.)

The nature of the infrared counterpart and of the optical nebula associated with the Central Compact Object in Vela Jr.

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