# The rate of iPTF 14gqr like ultra-stripped supernovae and binary evolution leading to double neutron star formation

## TL;DR

This paper estimates the detection rates of ultra-stripped supernovae similar to iPTF 14gqr using various optical surveys and explores binary evolution pathways leading to double neutron star systems.

## Contribution

It provides the first population synthesis-based rate estimates for iPTF 14gqr-like USSNe and analyzes binary physics effects on DNS formation.

## Key findings

- iPTF, ZTF, and LSST can detect 1, 40, and 5 USSNe per year respectively.
- iPTF could observe about 4 USSNe over four years.
- Binary physics significantly influences DNS orbital parameters and formation channels.

## Abstract

Double neutron star (DNS) systems are produced from massive binaries. A supernova (SN) explosion of an extremely stripped star is expected to occur at the final stage of DNS formation. This type of SN is called ultra-stripped SN (USSN). A recent research reveals that a type Ic SN, iPTF 14gqr (SN 2014ft) has low ejecta mass ($\approx0.2~\mathrm{M}_\odot$) and its progenitor has a helium envelope with its mass $\sim0.01~\mathrm{M}_\odot$. Then this SN is interpreted as an USSN, and this is the first discovery of the USSN. Furthermore, the observation of iPTF 14gqr provides us with some information about its formation history. Here, we perform population synthesis calculations so as to estimate the detection rate of iPTF 14gqr like USSNe by optical transient surveys, intermediate Palomar Transient Factory (iPTF), Zwicky Transient Facility (ZTF), and Large Synoptic Survey Telescope (LSST). We find that iPTF, ZTF, and LSST can observe iPTF 14gqr like USSNe at the rates of 1, 40, and 5 $\mathrm{yr}^{-1}$, respectively. The iPTF may detect 4 iPTF 14gqr like USSNe during four years observation. Additionally, we investigate effects of some binary physics on the orbital parameters of DNS systems and formation channels.