Abstract
We present an analysis of the impact of spiral density waves (DWs) on the radial and surface density distributions of supernovae (SNe) in host galaxies with different arm classes. We use a well-defined sample of 269 relatively nearby, low-inclination, morphologically non-disturbed and unbarred Sa-Sc galaxies from the Sloan Digital Sky Survey, hosting 333 SNe. Only for core-collapse (CC) SNe, a significant difference appears when comparing their R25-normalized radial distributions in long-armed grand-design (LGD) versus non-GD (NGD) hosts, with that in LGD galaxies being marginally inconsistent with an exponential profile, while SNe Ia exhibit exponential surface density profiles regardless of the arm class. Using a smaller sample of LGD galaxies with estimated corotation radii (Rc), we show that the Rc-normalized surface density distribution of CC SNe indicates a dip at corotation. Although not statistically significant, the high CC SNe surface density just inside and outside corotation may be the sign of triggered massive star formation by the DWs. Our results may, if confirmed with larger samples, support the large-scale shock scenario induced by spiral DWs in LGD galaxies, which predicts a higher star formation efficiency around the shock fronts, avoiding the corotation region.
Highlights
The spiral arm structure of star-forming disc galaxies was explained in the framework of density wave (DW) theory by the pioneering work of Lin & Shu (1964)
We see that the radial distribution of CC SNe in NGD subsample is concentrated to the centre of galaxies with a relatively narrow peak and fast decline in the outer disc
In this study, using a well-defined and homogeneous sample of SN host galaxies from the coverage of Sloan Digital Sky Survey (SDSS) Data Release 13 (DR13), we analyse the radial and surface density distributions of Type Ia and CC SNe in host galaxies with different arm classes (ACs) to find the possible impact of spiral DWs as triggers for star formation
Summary
The spiral arm structure of star-forming disc galaxies was explained in the framework of density wave (DW) theory by the pioneering work of Lin & Shu (1964). The simulations by Sellwood (2011) manifest short-lived patterns In another example, using a multiband analysis for some GD galaxies, Foyle et al (2010) found that there is no shock trigger, and that the spiral arms just reorganize the material from the disc out of which stars form (see Grosbøl & Dottori 2012).
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
