Detecting the signatures of helium in type Iax supernovae.

摘要: Recent studies have argued that the progenitor system of type Iax supernovae must consist a carbon-oxygen white dwarf accreting from helium star companion. Based on existing explosion models invoking pure deflagration dwarfs, we investigate likelihood producing spectral features due to in supernovae. From this scenario, select those ejecta and $^{56}$Ni masses are broadly consistent with estimated for (0.014 - 0.478~$M_{\odot}$ $\sim0.003$ 0.183~$M_{\odot}$, respectively). To end, present series varying luminosities ($-18.4 \lesssim M_{\rm{V}} -14.5$~mag) abundances accounting up $\sim$36\% mass, covering range epochs beginning few days before B$-$band maximum approximately two weeks after maximum. We find best opportunity detecting \ion{He}{i} is at near-infrared wavelengths, post-maximum spectra fainter members class. show optical spectrum SN~2007J potentially large content (a 10$^{-2}~M_{\odot}$), but argue current accretion material stripping companion struggle produce compatible scenarios. also presence all objects spectra. SNe~2005hk, 2012Z, 2015H contain either no or their constrained much lower values ($\lesssim$10$^{-3}~M_{\odot}$). Our results demonstrate differences among supernovae, perhaps pointing different channels. Either an outlier terms its system, it not true member supernova