OTELO survey: optimal emission-line flux determination with OSIRIS/GTC

TL;DR

The paper presents an optimized method for measuring emission-line fluxes in galaxies using OSIRIS/GTC tunable filters, enabling precise deblending of Hα and [NII] lines for better galaxy evolution insights.

Contribution

It identifies the optimal FWHM and sampling parameters for OSIRIS tunable filters to accurately deblend emission lines in galaxy surveys.

Findings

Optimal FWHM of 12 Å and sampling of 5 Å for red TFs.

Flux error below 20% for deblended Hα and [NII] lines.

Enables estimation of SFRs and metallicities from flux measurements.

Abstract

Emission-line galaxies are important targets for understanding the chemical evolution of galaxies in the universe. Deep, narrow-band imaging surveys allow to detect and study the flux and the equivalent widths (EW) of the emission line studied. The present work has been developed within the context of the OTELO project, an emission line survey using the Tunable Filters (TF) of OSIRIS, the first generation instrument on the GTC 10.4m telescope located in La Palma, Spain, that will observe through selected atmospheric windows relatively free of sky emission lines. With a total survey area of 0.1 square degrees distributed in different fields, reaching a 5 \sigma depth of 10^-18 erg/cm^2/s and detecting objects of EW < 0.3 A, OTELO will be the deepest emission line survey to date. As part of the OTELO preparatory activities, the objective of this study is to determine the best combination of sampling and full width at half maximum (FWHM) for the OSIRIS tunable filters for deblending H\alpha from [NII] lines by analyzing the flux errors obtained. We simulated the OTELO data by convolving a complete set of synthetic HII galaxies in EW with different widths of the OSIRIS TFs. We estimated relative flux errors of the recovered H\alpha and [NII]6583 lines. We found that, for the red TF, a FWHM of 12 A and a sampling of 5 A is an optimal combination that allow deblending H\alpha from the [NII]6583 line with a flux error lower than 20%. This combination will allow estimating SFRs and metallicities using the H\alpha flux and the N2 method, respectively.