Molecular Clouds Associated with the Type Ia SNR N103B in the Large Magellanic Cloud

Abstract

N103B is a Type Ia supernova remnant (SNR) in the Large Magellanic Cloud (LMC). We carried out new 12 CO(J = 3-2) and 12 CO(J = 1-0) observations using ASTE and ALMA. We have confirmed the existence of a giant molecular cloud (GMC) at V LSR ∼245 km s −1 towards the southeast of the SNR using ASTE 12 CO(J = 3-2) data at an angular resolution of ∼25 ′′ (∼6 pc in the LMC). Using the ALMA 12 CO(J = 1-0) data, we have spatially resolved CO clouds along the southeastern edge of the SNR with an angular resolution of ∼1.8 ′′ (∼0.4 pc in the LMC). The molecular clouds show an expanding gas motion in the position-velocity diagram with an expansion velocity of ∼ 5 km s −1 . The spatial extent of the expanding shell is roughly similar to that of the SNR. We also find tiny molecular clumps in the directions of optical nebula knots. We present a possible scenario that N103B exploded in the wind-bubble formed by the accretion winds from the progenitor system, and is now interacting with the dense gas wall. This is consistent with a single-degenerate scenario.

Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9

“…This means that the expanding gas motion was possibly created by stellar winds or accretion winds from the progenitor system of the SNR (e.g. Sano et al 2017bSano et al , 2018Kuriki et al 2018), which gives alternative support for the physical association between the SNR shocks and the ISM. The minimum intensity spot corresponding to a geometric center of the expanding shell is l ∼ 159.…”

Chemical Abundances in Sgr A East: Evidence for a Type Iax Supernova Remnant

“…Another source of the winds could be strong accretion outflows from the progenitor WD binary system prior to the SN explosion (Hachisu et al 1996). Windblown molecular bubbles have been reported for Type Ia SNR Tycho (Zhou et al 2016;Chen et al 2017) and N103B (Sano et al 2018). Dense wind bubbles have also been found in Type Ia SNR candidates RCW 86 (Williams et al 2011)…”

Radio emission from interstellar shocks: Young type Ia supernova remnants and the case of N 103B in the Large Magellanic Cloud

“…. , 45 K km s −1 ), and indicate the potential molecular gas association found by Sano et al (2018). Four circles show regions containing optical nebula knots, as seen in the HST Hα emission (Li et al 2017) the Western hemisphere that is ∼ 3 times brighter than the Eastern hemisphere (Dickel and Milne 1995).…”

“…It is located close to a dense H II region (Chu and Kennicutt 1988), and only ∼ 40 pc from the young star cluster NGC 1850 (Li et al 2017). X-ray (Hughes et al 1995), CO (Sano et al 2018) and optical studies (Rest et al 2005(Rest et al , 2008 have shown that it is likely to be a type Ia SNR; Li et al (2017) observed a main sequence star that is likely to be the surviving companion. As shown in Fig.…”

“…The decisive signature of an SD explosion is the observation of the surviving companion star, because the merger of the two WDs in the DD scenario leaves no remnant star. Other signatures include a dense circumstellar medium (Douvion et al 2001;Blair et al 2007;Williams et al 2012), accretion winds from the progenitor system (Hachisu et al 1996;Sano et al 2018), and strong K-shell emission from Ni and Mn (Yamaguchi et al 2015). Detailed observations of type Ia SNRs, to reconstruct the scene of the explosion and pinpoint the likely location of a surviving companion (if it exists), are required to distinguish between the SN scenarios.…”