Figure 1. Model predictions of the shock-heated emission light curves at 50 Mpc, overlayed on the best-fit early light curve of SN 2015F (Im et al. 2015b) that is fitted to the data after ~ 1 day after the explosion and shifted to 50 Mpc (the solid black line). The best-fit early light curve of SN 2015F represents a typical SN Ia light curve due to radioactive decay. The dashed lines are for Rabinak & Waxman (2011) for a CC SN, and the dotted lines are for Kasen (2010) due to the shock-heated emission from a companion star in SN Ia. The shock-heated emission from SN Ia is expected to be anisotropic, and can be fainter by 2.5 mag. The case plotted here is for the most optimal viewing angle.
Figure 2. MNUV (AB) versus distance (Mpc) of IMSNG galaxies (red squares), plotted over galaxies from Bai et al. (2015) (gray circles). The area within the black dashed line denotes the region where we selected IMSNG galaxies.
Figure 3. The locations of the telescopes used by IMSNG. The background world map is taken from http://trip8.co.
Figure 4. The occurrence of SNe per year per galaxy (SN rate) as a function of FUV (blue) or NUV (red) magnitudes for galaxies within 50 Mpc. The rates were examined over the period of 2006-2016.
Figure 5. The emergence of SN 2017gax (SN Ib/Ic) in NGC 1672 which is caught by SNUCAM-II on LSGT (Im et al. 2015b; Choi & Im 2017), one of the IMSNG telescopes (Im et al. 2017a). Each image shows a stack of three 180 sec exposure frames in r-band, and the green circle with a ra-dius of 20:000 indicates the location of the SN. This example demonstrates that the high cadence IMSNG observation can catch the early optical light curves of SNe. The UT date of the observation is also indicated in each image.
Figure 6. (Left) A single exposure (60 seconds) R-band image near NGC 895 galaxy. A part of NGC 895 is visible on the left. (Right) A stacked R-band image (2.37 hours) of the same eld. The data taken from 2013 to 2016 were used. A low SB satellite galaxy candidate is marked as a large, thick arrow. Merging features are visible in the deep image for a galaxy on the top and noted with small arrows.
Table 1 IMSNG target galaxies
Table 2 The current list of telescopes in the IMSNG network
Table 3 SNe and other transients in IMSNG galaxies (2014-2018)