The purple in this image is a false color indication of the x-rays detected by the Chandra X-Ray Observatory emanating from the edge of the supernova remnant due to a shockwave front. The center of the remnant is out of frame, off to the left.
RX J0852.0−4622 (also known as G266.2−1.2) is a supernova remnant. The remnant is located in the southern sky in the constellationVela ("sail"), and sits (in projection) inside the much larger and older Vela Supernova Remnant. For this reason, RX J0852.0−4622 is often referred to as Vela Junior (Vela Jr.).[1][2] There have been a minority of suggestions that the remnant may be a spurious identification of a complicated substructure within the larger and better studied Vela SNR, but most studies accept that G266.2−1.2 is a SNR in its own right. Indeed, its detection in the high energy Teraelectronvolt range by the High Energy Stereoscopic System in 2005 is strong confirmation of such.[3]
It was found in 1998 with an analysis of data from the ROSAT x-ray telescope.[4] Published simultaneously with its discovery was a claimed detection by the Compton Gamma Ray Observatory of a gamma ray spectral line of 44Ti which has a half-life of 60 years and therefore seemed to indicate a young provenance for the supernova, perhaps the youngest one yet discovered.[5] Later independent groups could not reproduce the detection, and so the consensus is that the identification of this line was likely spurious.[6] Since the age and distance are correlated, a young, nearby supernova like this has inspired some detective work to identify evidence that such a supernova may have been observed and recorded by groups of people,[7] and geochronologists have looked for evidence of a young supernova in tree ring[8] and ice core data,[9] but identification of claimed correlate signals have not been conclusively made.[2] The latest analyses of the remnant indicate an age of at least 2400 years (and possibly much older), a distance of no less than 500 parsecs, and a radial size of at least 8 parsecs.[2]
The central compact object (CCO) was discovered in 2001.[10] In the initial ChandraX-ray image and deeper images thereafter, no pulsations were detected from the compact remnant, which is believed to be the neutron star CXOU J085201.4-461753. A different pulsar was suggested as the remnant,[11] but its kinematics do not conform as well to the observed kinematics of the remnant shell.[2]
