SINFONI data reduction using the ESO pipeline

Instrument design and its impact on the data (I) integral field spectrometer using mirrors brickwall pattern

Instrument design and its impact on the data (II) Near-infrared: strong sky background -> ON - OFF observing strategy

Instrument design and its impact on the data (III) Rectangular spatial pixels. Smooth, round PSF with sqare pixels only with many (or suitably offset) dithered positions

Data Retrieval Data delivery from ESO archive for one’s own run Obtaining archival data

The pipeline: esorex and gasgano pipeline offers two modes of data reduction: command line via esorex, or GUI driven using gasgano

Association/tagging Pipeline requires classification of data. Manual for esorex in input file, automatic in gasgano We will therefore use gasgano, but command line mode has advantages for example for large amounts of data to be reduced in a similar way, checking impact of parameter change, etc.

The science project The nuclear star-forming ring in NGC 613 (Boeker et al., 2008) Optimally applies the advantages of the instument: Line image and spectral analysis

The science project II Band: H+K Scale: 0.25”/pix (8”x8”) observations in 3 different nights proper ON/OFF pairs, 4 pairs/OB DIT=300s, NDIT=1 telluric standards from calibration plan

Data reduction: Dark input: Dark frames, 3 or more per DIT output: master dark and bad pixel map

Data reduction: Linearity input: Flat frames with different DITs output: master dark and non-linear pixel map

Data reduction: Flat input: Flat frames (ON/OFF) output: master Flat

Data reduction: Arc input: Arc frames (ON/OFF) output: Wavelength table

Data reduction: Distortion input: NS-Frames (75 typically) output: Distortion coefficients

Data reduction: Jitter input: Science Frames output: Sky subtracted Science data cube

Visualization: QFitsView Display the data cube, extract planes and spectra, do telluric correction, etc.