Poster abstract details
NEFER, a High Resolution Fabry-Perot Spectrometer
Abstract
NEFER (Nuevo Espectrómetro Fabry-Perot de Extrema Resolución) is a 3D instrument aimed to implement a high
resolution spectrometry for velocity determinations of extended stellar objects, with R up to 15,000. The instrument
conceived as a high resolution Fabry-Perot (F-P) spectrometer will be hosted in OSIRIS, the tunable imager/spectrograph of the 10.4 m GTC telescope. NEFER implementation does not require any hardware changes to the host instrument except substituting the tunable filter with a high resolution F-P (NEFER), using another set of narrow band interference filters and a calibration software package for data acquisition an reduction. In this way, instead of obtaining direct narrowband images, we get a data cube interference frame by scanning the F-P at selected steps, from which we can study the kinematics of the observed region. High level requirements for this instrument specify that it will take advantage of the host instrument field of view (FOV) of 8.5 x 8.7 arcmins and the spatial resolution determined by the detector pixel size (0.125 arcsec,) and the seeing of the telescope. Other high level requirements specify two spectral ranges: 6300 to 7000 and 8000 to 9000 Angstroms with a effective Finesse of at least 23 in the two ranges.
resolution spectrometry for velocity determinations of extended stellar objects, with R up to 15,000. The instrument
conceived as a high resolution Fabry-Perot (F-P) spectrometer will be hosted in OSIRIS, the tunable imager/spectrograph of the 10.4 m GTC telescope. NEFER implementation does not require any hardware changes to the host instrument except substituting the tunable filter with a high resolution F-P (NEFER), using another set of narrow band interference filters and a calibration software package for data acquisition an reduction. In this way, instead of obtaining direct narrowband images, we get a data cube interference frame by scanning the F-P at selected steps, from which we can study the kinematics of the observed region. High level requirements for this instrument specify that it will take advantage of the host instrument field of view (FOV) of 8.5 x 8.7 arcmins and the spatial resolution determined by the detector pixel size (0.125 arcsec,) and the seeing of the telescope. Other high level requirements specify two spectral ranges: 6300 to 7000 and 8000 to 9000 Angstroms with a effective Finesse of at least 23 in the two ranges.