![CALIFA: Summary I Calar Alto Legacy Integral Field Area survey. Survey of ~600 Galaxies in the Local Universe (0.0005<z<0.003), i.e., D<40Mpc. IFS using [email_address] Calar Alto. Mid-resolution (R~1000/2000) spectroscopic data between 3700-7000AA. Covering a 90% of the size of the galaxies.](https://image.slidesharecdn.com/integralfieldspectroscopy-110126080208-phpapp01/75/Integral-field-spectroscopy-27-2048.jpg)
![CALIFA: Summary I Calar Alto Legacy Integral Field Area survey. Survey of ~600 Galaxies in the Local Universe (0.0005<z<0.003), i.e., D<40Mpc. IFS using [email_address] Calar Alto. Mid-resolution (R~1000/2000) spectroscopic data between 3700-7000AA. Covering a 90% of the size of the galaxies.](https://crownmelresort.com/image.slidesharecdn.com/integralfieldspectroscopy-110126080208-phpapp01/75/Integral-field-spectroscopy-27-2048.jpg)
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Integral field spectroscopy
- 1. Integral Field SpectroscopyUniversidad de Almeria Viernes de Ciencia 14 January 2011 S.F.Sánchez (CAHA)
- 2. IFS or 3DSpectroscopy Is the spectroscopic technique that samples a quasi-continous area in the sky (FOV). The FOV is sampled by small aperture elements named spaxels, which correspond to pixels of an image. Light coming through each spaxel is transported to the entrance of an spectrograph. The image/plane and focal/plane are completely decoupled: Lot of software is required to reconstruct the orginal spatial shape at each wavelength.
- 3. Different kind ofspaxels. Is the spectroscopic technique that samples a quasi-continous area in the sky (FOV). The FOV is sampled by small aperture elements named spaxels, which correspond to pixels of an image. Light coming through each spaxel is transported to the entrance of an spectrograph. The image/plane and focal/plane are completely decoupled: Lot of software is required to reconstruct the orginal spatial shape at each wavelength.
- 4. How to sendthe light to the Spectrograph? Image Slicers: Light is “sliced” in small continous pseudo-slits: SINFONI, MUSE... Lensarrays: Continous lensarray is focused in separated apertures: SAURON, TIGER... Fiber-Bundles (+lensarrays): Lights is conducted by fibers: PMAS/PPAK, VIMOS, GMOS...
- 5. Fiber Feed IFStechnique
- 6. The Raw dataof FF IFUs
- 7. The Raw dataof FF IFUs
- 8. FF IFU: DataReduction (I) Continuum exposure used to find and trace the location of the spectra in the CCD. The FWHM of the spectra projected in the cross-dispersion axis determined. Gaussian extraction performed. Comparison Arc used to determine the distorsion correction and wavelength solution, latter applied to the data.
- 9. FF IFU: DataReduction (II) Sky-frames taken during the twilight used to correct for the differentical transmission fiber to fiber (wavelength dependent). Spectrophotometric calibration standard star exposure used to determine the flux calibration, applied to the science frames. Science (331), Sky (36) and calibration spectra (15) are separated in different frames, once reduced. Sky spectrum is derived for each frae (median+3sigma clipping of the 36 sky-spectra) and the subtracted to the data.
- 10. FF IFU: DataReduction (III) Re-arrange the dithered pointings in a single row-stacked spectra frame, plus the complementary Position Table. Mask the spectral pixel strongly affected by the vignetting. Interpolate the final Mosaic into a common grid datacube of 1”/pixel. When available, perform a flux recalibration based on broad-band photometry.
- 11. The Raw dataof FF IFUs
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- 14. Extraction: How toAdd flux?
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- 16. Extraction: The finalproduct
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- 20. Sky subtraction... If possible.
- 21. Where my spectracomes from?.
- 22. PMAS/PPAK: Dithering. 3position dither pattern per pointing. Complete spatial covering of the FOV. Increase of the spatial resolution. Fully implemented in R3D.
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- 24. Matching the pointings.The pointings overlap, in at least 11 spectra. The change in transparency is critical Accuracy of the telescope offsets is also critical.
- 25. Results: Orion (Sánchez et al. 2006)
- 26. Results: M74 (Sánchezet al. 2010)
- 27. CALIFA: Summary ICalar Alto Legacy Integral Field Area survey. Survey of ~600 Galaxies in the Local Universe (0.0005<z<0.003), i.e., D<40Mpc. IFS using [email_address] Calar Alto. Mid-resolution (R~1000/2000) spectroscopic data between 3700-7000AA. Covering a 90% of the size of the galaxies.
- 28. CALIFA: Summary IIProposed by 47 researchers from 5 countries: PI:S.F.Sánchez. co-PI: R.Kennicutt & A.Gil de Paz). It will consume ~200 dark nights in 3 years. Starting the 1 st of July 2010 (NOW!!!). Already on-going: Runs scheduled. ~40 galaxies already observed.
- 29. CALIFA: Science GoalsModel the resolved stellar population in galaxies of any kind and trace the star formation history. Determine the nature of the ionized gas and its chemical abundance gradients. Determine the 2D kinematic structure of galaxies in the local Universe.
- 30. CALIFA: Mother SampleProposal: 937 galaxies, diameter selected, at 0.005<z<0.03 from SDSS imaging survey, covering the full CM down to Mb<-18 mag. 572/937 have 2MASS data. 339/937 have IRAS data (24 with L FIR >10 10.5 L Sun ). 261/937 have FIRST data. All included in NYU (n sersic , scale-length). All included in the GalaxyZoo. 537/937 have SDSS spectra: 162 with few or no gas. 184 AGN candidates. 277 galaxies with SF ionization.
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- 32. CALIFA: Pilot Study.Work in process: Data reduced. Integrated and central spectra derived. Automatic analysis on the Integrated Spectra Performed. Gradients studied for a reduced sample. To be done: Fully automatic 2D analysis. Detail comparison with SDSS.
- 33. 3D Spectroscopy SummaryIFS is a common user technique (40% of the observations done with the 3.5m at CAHA, 80% of one of the UT/VLT). Many of proposed or new generations instruments are IFUs (MUSE, MEGARA). JWST will include an IFU. There is science that can only be done with IFUs. Any future astronomer should be prepared to use it.