Looking for molecular gas associated with the pulsar wind nebula 3C 58

Abstract

El remanente de supernova 3C 58, ubicado en el Brazo de Perseo a una distancia de 2.0 ± 0.3 kpc, es una nebulosa de viento alimentada por el púlsar PSR J0205+6449. Este remanente ha sido detectado en radio, rayos X, y rayos γ. Utilizando datos del ¹²CO(1-0) del Canadian Galactic Plane Survey, se identificó una estructura de gas molecular proyectada en dirección al remanente, que posee una distancia cinemática de 0.6+0.3 kpc. Debido a los movimientos no circulares del gas en esta región de la Galaxia, que ponen en duda el método cinemático para acotar distancias, no puede descartarse una asociación entre 3C 58 y dicha estructura. Se usarán nuevas observaciones moleculares para buscar evidencia de gas chocado por el remanente y determinar si existe una asociación física con el gas molecular. Los resultados de este estudio futuro se publicarán oportunamente.

The supernova remnant 3C 58, located in the Perseus Arm at a distance 2.0+0.3 kpc, is a wind nebula powered by the pulsar PSR J0205+6449. This remnant has been detected in various wavelengths, including radio, X-rays, and γ-rays. Using data of the ¹²CO(1-0) emission from the Canadian Galactic Plane Survey, I identified a structure of molecular gas projected onto 3C 58, which has a kinematic distance of 0.6 ± 0.3 kpc. Based on the non circular motions of the gas in this part of the Galaxy, which question the reliability of the kinematic method to obtain distances, I cannot discard the association between 3C 58 and the molecular structure. I will look for shocked gas using new molecular line observations to establish whether 3C 58 is physically associated with the molecular gas. This study will be conducted in the future and the results will be published anywhere.