PHotometry Assisted Spectral Extraction (PHASE) and identification of SNLS supernovae

TL;DR

This paper introduces advanced spectral extraction and identification methods for supernovae that leverage photometric data, enabling more accurate separation of supernova and host galaxy signals and improving type and redshift determination accuracy.

Contribution

The paper presents novel extraction and identification techniques that utilize photometric information and spectral modeling to enhance supernova spectral analysis within the SNLS.

Findings

Achieved ~70% successful supernova-host separation in spectra.

Enabled secure supernova type and redshift determination in ~80% of cases.

Demonstrated improved performance over standard spectral extraction methods.

Abstract

Aim: We present new extraction and identification techniques for supernova (SN) spectra developed within the Supernova Legacy Survey (SNLS) collaboration. Method: The new spectral extraction method takes full advantage of photometric information from the Canada-France-Hawai telescope (CFHT) discovery and reference images by tracing the exact position of the supernova and the host signals on the spectrogram. When present, the host spatial profile is measured on deep multi-band reference images and is used to model the host contribution to the full (supernova + host) signal. The supernova is modelled as a Gaussian function of width equal to the seeing. A chi-square minimisation provides the flux of each component in each pixel of the 2D spectrogram. For a host-supernova separation greater than <~ 1 pixel, the two components are recovered separately and we do not use a spectral template in contrast to more standard analyses. This new procedure permits a clean extraction of the supernova separately from the host in about 70% of the 3rd year ESO/VLT spectra of the SNLS. A new supernova identification method is also proposed. It uses the SALT2 spectrophotometric template to combine the photometric and spectral data. A galaxy template is allowed for spectra for which a separate extraction of the supernova and the host was not possible. Result: These new techniques have been tested against more standard extraction and identification procedures. They permit a secure type and redshift determination in about 80% of cases. The present paper illustrates their performances on a few sample spectra.