The Italian LBT spectroscopic data reduction pipeline

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1 LBTO 2017 Users' Meeting The Italian LBT spectroscopic data reduction pipeline Alida Marchetti INAF-IASF Milano Firenze, June 20th-23rd

2 reduction pipeline SOME NUMBERS INAF nights 46 Effective observing INAF nights 33 Total number of completed masks MODS LUCI SEMI automatic reduction of all data as a service to the Italian community

3 reduction pipeline FLOW CHART MODS GENERIC CALIB Bias & Flat fields Bad pixels Bias prescan /over scan TARGET CALIBRATIONS Flat Field Arc frames Pixel2pixel Inverse correction Dispersion Solution Optical distortion correction Standard Sensitivity function Spectra location Bad Pixel Map SCIENCE Science Exposure bad pixels, cosmic rays and bias correction Optical distortion correction Science Exposures Wavelength calibration Bias 2D extraction Master Flat Master Lamp Sky subtraction Flux calibration table Flux calibration 1D extraction Combine exposures 1D extraction Data products

4 reduction pipeline FLOW CHART LUCI GENERIC CALIB Darks & Flat fields TARGET CALIBRATIONS Flat Field Darks Arc frames Pixel2pixel Inverse correction Dispersion Solution Optical distortion correction Dead/hot pixels Telluric Sensitivity function Telluric correction Spectra location Bad Pixel Map Master dark SCIENCE Science Exposure bad pixels, cosmic rays and dark correction Optical distortion correction Science Exposures Wavelength calibration 2D extraction Master Flat Master Lamp Sky subtraction Flux calibration table Flux calibration 1D extraction Combine exposures 1D extraction Data products

5 reduction pipeline TARGET CALIBRATIONS TRACING OF THE SPECTRAL DISPERSION + PIXEL-TO-PIXEL VARIATION CORRECTION (MASTERFLAT) MODS1 MODS1MOS MOS - first guess of the pixel-angstrom correspondence and of the location of spectra (2D polynomial fit) - tracing of the spectral dispersion through a set of matrices that follow optical distortions (slit by slit) -refinement through halogen lamps observations (spectroscopic FLATS)

6 reduction pipeline TARGET CALIBRATIONS TRACING OF THE SPECTRAL DISPERSION + PIXEL-TO-PIXEL VARIATION CORRECTION (MASTERFLAT) MODS1 MOS

7 reduction pipeline TARGET CALIBRATIONS TRACING OF THE SPECTRAL DISPERSION + PIXEL-TO-PIXEL VARIATION CORRECTION (MASTERFLAT) MODS1 MOS

8 reduction pipeline TARGET CALIBRATIONS TRACING OF THE SPECTRAL DISPERSION + PIXEL-TO-PIXEL VARIATION CORRECTION (MASTERFLAT) MODS1 LS

9 reduction pipeline TARGET CALIBRATIONS WAVELENGTH CALIBRATION (MASTERLAMP) LUCI1 LS - the first guesses of the Masterflat on line positions are refined through calibration arcs observations: the local polynomial describing the pixel-wavelength correspondence is adjusted on the basis of the arcs emission peaks. The procedure is iterated to find the better IDS solution

10 reduction pipeline TARGET CALIBRATIONS WAVELENGTH CALIBRATION (MASTERLAMP) LUCI1 LS ESEMPIO 1 VISUAL CHECK

11 reduction pipeline TARGET CALIBRATIONS WAVELENGTH CALIBRATION (MASTERLAMP) Mean accuracy (average 1 and 2 instruments) [Å]: ESEMPIO 1 VISUAL CHECK INSTRUMENT CONFIG. ACCURACY DISP. MODSR MODSB LUCI 200HK (HK) LUCI 200HK (zj) LUCI 210zjHK (J) LUCI 210zjHK (H) LUCI 150Ks (Ks)

12 reduction pipeline FLOW CHART MODS GENERIC CALIB Bias & Flat fields Bad pixels Bias prescan /over scan TARGET CALIBRATIONS Flat Field Arc frames Pixel2pixel Inverse correction Dispersion Solution Optical distortion correction Standard Sensitivity function Spectra location Bad Pixel Map SCIENCE Science Exposure bad pixels, cosmic rays and bias correction Optical distortion correction Science Exposures Wavelength calibration Bias 2D extraction Master Flat Master Lamp Sky subtraction Flux calibration table Flux calibration 1D extraction Combine exposures 1D extraction Data products

13 reduction pipeline SCIENCE INSTRUMENTAL EFFECTS AND COSMIC CORRECTION MODS2 LS ESEMPIO

14 reduction pipeline SCIENCE 2D SPECTRAL EXTRACTION LUCI2 LS ESEMPIO Linear wavelength

15 reduction pipeline SCIENCE SKY SUBTRACTION Background is removed slit by slit in every single exposure LUCI MODS Local estimation along spatial direction through: Davies sky subtraction¹ (to minimize OH residuals) + - median -median - polynomial fit order 1 -polynomial fit order 1 - polynomial fit order 2 -polynomial fit order 2

16 reduction pipeline SCIENCE SKY SUBTRACTION MODS1 MOS Background is removed slit by slit in every single exposure

17 reduction pipeline SCIENCE SKY SUBTRACTION MODS1 MOS

18 reduction pipeline SCIENCE SKY SUBTRACTION Background is removed slit by slit in every single exposure LUCI MODS Local estimation along spatial direction through: Davies sky subtraction¹ (to minimize OH residuals) + - median -median - polynomial fit order 1 -polynomial fit order 1 - polynomial fit order 2 -polynomial fit order 2 1. Porting (C code) of Davies R. and Cresci, G. algorithm implementation Davies 2007: MNRAS, 375, 1099

19 reduction pipeline SCIENCE SKY SUBTRACTION LUCI1 LS

20 reduction pipeline SCIENCE SKY SUBTRACTION LUCI1 LS

21 reduction pipeline FLOW CHART LUCI GENERIC CALIB Darks & Flat fields TARGET CALIBRATIONS Flat Field Darks Arc frames Pixel2pixel Inverse correction Dispersion Solution Optical distortion correction Dead/hot pixels Telluric Sensitivity function Telluric correction Spectra location Bad Pixel Map Master dark SCIENCE Science Exposure bad pixels, cosmic rays and dark correction Optical distortion correction Science Exposures Wavelength calibration 2D extraction Master Flat Master Lamp Sky subtraction Flux calibration table Flux calibration 1D extraction Combine exposures 1D extraction Data products

22 reduction pipeline SCIENCE 2D COMBINATION pipeline combines 2D spectra according to the frame offsets: - script values - on image pipeline determination

23 reduction pipeline SCIENCE FINAL EXTRACTION The identification of objects is performed for each slit: MODS1 LS - the slit is collapsed along the spatial direction - a slit profile is created - a sigma clipping is applied to the profile - Horne extraction is performed to extract 1D spectra

24 reduction pipeline SCIENCE FINAL EXTRACTION The identification of objects is performed for each slit: MODS1 LS - the slit is collapsed along the spatial direction - a slit profile is created - a sigma clipping is applied to the profile - Horne extraction is performed to extract 1D spectra

25 reduction pipeline SCIENCE FINAL EXTRACTION The identification of objects is performed for each slit: MODS1 LS - the slit is collapsed along the spatial direction - a slit profile is created - a sigma clipping is applied to the profile - Horne extraction is performed to extract 1D spectra

26 reduction pipeline SCIENCE FLUX CALIBRATION Correction for the sensitivity response of the instrument MODS LUCI Standard star: Telluric star: - the observed spectrum of a standard star is compared to the tabulated spectrum - characteristics retrieved from Hipparcos catalog - choose corresponding Pickle template and rescale it - this spectrum is used a tabulated one

27 reduction pipeline SCIENCE FLUX CALIBRATION Flux Flux Sensitivity MODS1 Wavelength[Å] Wavelength[Å]

28 reduction pipeline SCIENCE FLUX CALIBRATION - BINOCULAR MODE Before combination, the EXR2D are flux calibrated

29 reduction pipeline DATA PRODUCTS DISTRIBUTED DATA - cleaned, sky subtracted, wavelength calibrated and 2D combined extracted spectrum (EXR2D) (also flux calibrated upon request, or in case of MODS/LUCI 1-2 combination) - clean, sky subtracted, wavelength and flux calibrated 1D combined extracted spectrum (EXR1D)

30 reduction pipeline SOME INFOS REDUCTION DIFFICULTIES Stability of keywords in the files header Many different possible grism configurations (LUCI) Absence of a bright object to help determining the real offsets with precision Shifts between science frames and calibration frames (both flats-arcs and telluric/standard frames)

31 reduction pipeline SOME INFOS LUC1 MOS REDUCTION DIFFICULTIES Absence of the OBJECT keyword in the files header (LUCI, now solved) Many different possible grism configurations (LUCI) Absence of a bright object to help determining the real offsets with precision Shifts between science frames and calibration frames (both flats-arcs and telluric/standard frames)

32 reduction pipeline SOME INFOS Average reduction time MIN: LS Mono 4 exposures ~2 HOURS Num of expos Num of slits Binocularity MAX: MOS Bino 100 exposures ~2 DAYS

33 reduction pipeline THE END THANK YOU

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