Gonzalo Vilella Rojo
The J-PLUS survey was designed to carry out the photometric callibration of the J-PAS survey. To do that, it will observe ~8500 square degrees of the sky with a wide field camera (2.1 square degrees per exposure) and a set of 12 filters (7 median/narrowband and 5 broadband) that cover the optical wavelength range from 3200 to 10500 A.
Apart from the calibration purposes, J-PLUS allows us to do studies of galaxy evolution in the local Universe thanks to a narrowband filter (~150 A) centred at the Ha rest-frame emission wavelength. The survey strategy puts more time in this filter to reach AB mag of 22.6 at S/N=3. This will allow us to get a robust estimation of the Ha luminosity function up to z~0.015. Additionally, a similar filter is placed near the rest-frame emission wavelength of the [OII] doublet to work on similar purposes.
In this talk I will present the main characteristics of the J-PLUS survey. After that, I will explain how we extract the Ha+[NII] and the [OII] emissions. Finally, I will comment how we correct for dust extinction and [NII] contamination.
2015 October 22, 15:00
Observatório Astronómico de Lisboa (Seminar room)
Tapada da Ajuda, 1349-018 Lisboa