Is Vela Jr. a young supernova remnant?

Katsuda, Satoru; Tsunemi, H.; Mori, Koji

doi:10.1016/j.asr.2009.01.004

Cited by 7 publications

(7 citation statements)

References 21 publications

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“…The uncertainty of this result is rather large, as can be seen when varying the properties of the explosion and of the SNR environment. A lower explosion energy closer to the canonical value of 10 51 erg or a higher density of the inter-cloud ISM delay the impact of the blast wave on the clouds significantly, and we would estimate a time of explosion about 2000 years earlier, consistent with the speculations by Katsuda et al (2009). Besides the geometry of the SNR, we can estimate the rate at which the X-ray bright front marking the interaction of the blast wave and the clouds expands.…”

Section: Discussionsupporting

confidence: 74%

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Hydrodynamic simulations of the interaction of supernova shock waves with a clumpy environment: the case of the RX J0852.0−4622 (Vela Jr) supernova remnant

Obergaulinger

Iyudin

Müller

et al. 2013

Monthly Notices of the Royal Astronomical Society

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Observations in all electromagnetic bands show that many supernova remnants (SNRs) have a very aspheric shape. This can be the result of asymmetries in the supernova explosion and of a clumpy circum-stellar medium. We study the generation of inhomogeneities and the mixing of elements due to these two sources in multi-dimensional hydrodynamic simulations of the propagation of a supernova blast wave into a cloudy environment. We model a specific SNR, VelaJr (RX J0852.0-4622). By comparing our results with recent observations, we can constrain the properties of the explosion. We find that a very energetic explosion of several 10 51 erg occurring roughly about 800 years ago as well as a supernova with an energy closer to the canonic value of 10 51 erg a few 1000 years ago are consistent with the shape and emission of the SNR.

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Section: Discussionsupporting

confidence: 74%

“…Age estimates for Vela Jr. range from ∼ 700 yrs (Iyudin et al 2005) up to a few 1000 yrs (Katsuda et al 2009). The question of the age of the SNR is closely linked to the determination of its distance, for which a similar range of values has been obtained.…”

Section: Introductionmentioning

confidence: 99%

Hydrodynamic simulations of the interaction of supernova shock waves with a clumpy environment: the case of the RX J0852.0−4622 (Vela Jr) supernova remnant

Obergaulinger

Iyudin

Müller

et al. 2013

Monthly Notices of the Royal Astronomical Society

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“…In this case, we could constrain the CXO J085201.4−461753 rotational energy loss from its spatial velocity and from the H α luminosity of the nebula (Chatterjee & Cordes 2002). We inferred the radial velocity V r from the assumed red-shift of the H α line, while we derived the transverse velocity V t from the CCO displacement from the SNR centre (≈5 ) which, for a distance of ∼1 kpc (Slane et al 2001) and for an age of ∼1000−3000 years (Katsuda et al 2009), implies a value of 500−1500 km s −1 . This corresponds to a spatial velocity V = 700−3000 km s −1 , large but not unheard of for a neutron star, as it is shown by the Guitar Nebula pulsar PSR B2224+65 (see, e.g.…”

Section: Discussionmentioning

confidence: 99%

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

Mignani¹,

Luca

2009

A&A

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Context. 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 H α band detected a nebula around CXO J085201.4−461753, 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 H α , 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. Aims. The aim of this work is to resolve the morphology of the H α nebula around the CCO to verify the proposed interpretations. Methods. 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 H α line. Results. Surprisingly enough, we did not detect the nebula in our WFPC2 image down to a 3σ flux limit of ∼3 × 10 −15 erg cm −2 s −1 . 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 H α filters. Conclusions. 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 H α line is redshifted by ∼10−60 Å due to the neutron star motion with a radial velocity 450 < ∼ V r < ∼ 2700 km s −1 . The other possibility is that the nebula is a knot of [NII] emission (λ = 6583.6 Å) unrelated to CXO J085201.4−461753 and possibly associated with the nearby star Wray 16-30. High-resolution spectroscopy observations will help to settle the nature of the nebula.

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“…The ∼10 arcsecond-scale errors associated with the SNR radius and the differing coverage of the 1999 and 2011 observations (see Figure 1) make the data unsuitable for expansion rate studies, particularly because previous X-ray expansion rate measurements (Katsuda et al 2009;Allen et al 2015) suggest that sub-arcsecond yr −1 precision is required for this purpose. Dec.…”

Section: Parametrising the Snr Shellmentioning

confidence: 99%

“…The 44 Ti detection was and remains controversial (Renaud et al 2006). More recent studies estimate ages of ∼1 to 3 kyr and 2.4 to 5.1 kyr (Katsuda et al 2009;Allen et al 2015, respectively), with distances of ∼700 pc (±200 pc). A new relevance for this object came to light when HESS observations at TeV energies (HESS J10852−463, Aharonian et al 2005Aharonian et al , 2007 H.E.S.S.…”

Section: Introductionmentioning

confidence: 99%

A Morphological Study of the Supernova Remnant Rx J0852.0–4622 (Vela Jr.)

Maxted

Filipović

Sano

et al. 2018

ApJ

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We conduct a multi-wavelength morphological study of the Galactic supernova remnant RX J0852.0-4622 (also known as Vela Jr., Vela Z and G266.2−1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela supernova remnant causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio continuum emission can be characterised by a 2-dimensional shell with a radius of 0.90±0.01 • (or 11.8±0.6 pc at an assumed distance of 750 pc) centred at (l,b)=(133.08 • ±0.01 • ,−46.34 • ± 0.01 • ) (or RA=8h 52m 19.2 s, Dec=−46 • 20 ′ 24.0 ′′ , J2000), consistent with X-ray and gamma-ray emission. Although [OIII] emission features are generally associated with the Vela SNR, one particular [OIII] emission feature, which we denote as "the Vela Claw", morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Towards the north-western edge of RX J0852.0-4622, we find a flattening of the radio spectral index towards another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and the ISM.

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Is Vela Jr. a young supernova remnant?

Cited by 7 publications

References 21 publications

Hydrodynamic simulations of the interaction of supernova shock waves with a clumpy environment: the case of the RX J0852.0−4622 (Vela Jr) supernova remnant

Hydrodynamic simulations of the interaction of supernova shock waves with a clumpy environment: the case of the RX J0852.0−4622 (Vela Jr) supernova remnant

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

A Morphological Study of the Supernova Remnant Rx J0852.0–4622 (Vela Jr.)

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