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UNIVERSIDAD COMPLUTENSE DE MADRID Grupo UCM de Astrofísica Instrumental y eXtragaláctica

PRESENTADO POR: Raffaella Anna Marino. COLABORADORES: A. Gil de Paz, S. Sánchez, J.C. Muñoz-Mateos, A. Castillo. UNIVERSIDAD COMPLUTENSE DE MADRID Grupo UCM de Astrofísica Instrumental y eXtragaláctica. CONTENT. THE AIM OF THIS WORK INTEGRAL FIELD SPECTROSCOPY PPAK

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UNIVERSIDAD COMPLUTENSE DE MADRID Grupo UCM de Astrofísica Instrumental y eXtragaláctica

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  1. PRESENTADO POR: Raffaella Anna Marino COLABORADORES: A. Gil de Paz, S. Sánchez, J.C. Muñoz-Mateos, A. Castillo UNIVERSIDAD COMPLUTENSE DE MADRID Grupo UCM de Astrofísica Instrumental y eXtragaláctica

  2. CONTENT • THE AIM OF THIS WORK • INTEGRAL FIELD SPECTROSCOPY • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSIONS • FUTURE PROJECTS 1/17 17/09/2010 IFS NGC5668

  3. THE AIM OF THIS WORK • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS • FORMATION AND EVOLUTION OF SPIRAL GALAXIES • ADVANTAGES OF INTEGRAL FIELD SPECTROSCOPY • DUST ATTENUATION CHEMICAL ABUNDANCE • HOW OLD ARE THE SPIRAL DISK? • HOW DID THEY CHEMICALLY EVOLVE? • ARE THEY GROWING INSIDE-OUT? Hα/Hβ BALMER DECREMENT KEWLEY & DOPITA RECIPE (2002)‏ 17/09/2010 IFS NGC5668 2/17

  4. INTEGRAL FIELD SPECTROSCOPY • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS • Simultaneous record of the spectral and spatial information in 2D • We obtain a cube fits for exposure • Efficiency and Homogeneity • NOW: • Image (+ filter): (x, y)@λ • Spectroscopy (long-slit): (x, λ) @ y fixed HOW TO REGISTER 3D INFO TO THE 2D DETECTOR? 3/17 17/09/2010 IFS NGC5668

  5. PPak-IFU Principle design focal reducer + hexagonal packed fiber-bundle Focal reducer lens F/10 to F/3.3, diam=50 mm Plate-scale 17’’.85 /mm Fiber configuration 331 object, 36 sky, 15 calibration PPak – FoV 74’’×64’’(hexagonal packed)‏ Spatial sampling 2.68” per fiber diameter Fiber pitch 3.5” fiber-to-fiber core diameter 150um Wavelength range 400–900 nm PPAK • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS 4/17 17/09/2010 IFS NGC5668

  6. NAME NGC 5668 MORPHOLOGICAL TYPE Sc(s) II-III/Sd RA(2000) 14h 33m 24.3s Dec(2000) +04°27'02" B MAGNITUDE R MAGNITUDE LB 12.13 ± 0.03 mag 11.28 ± 0.01 mag 2.7 ± 0.6 × 109 LΘ RADIAL VELOCITY(Hel.)‏ 1582 ± 5 km/s D (Galactocentric GSR)‏ 15.6 ± 1.5 Mpc INCLINATION 18° Position Angle (PA)‏ 145° MAJOR DIAMETER 3.3 arcmin MINOR DIAMETER 3.0 arcmin HELIOCENTRIC REDSHIFT 0.005277±0.000017 MTOT 5.7 × 1010 MΘ MTOT / LB 2.9 MΘ /LΘ,B THE CASE OF NGC5668 • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS SDSS 3,6 μm GALEX 8,0 μm E N 17/09/2010 IFS NGC5668 5/17

  7. OBSERVATIONAL PARAMETERS 22/06/2007 to 24/06/2007 Date of observation Telescope Calar Alto, 3.5m Focus Cassegrain Instrument PPAK OFF-AXIS FIBER BUNDLE IFU Fibre projected size 2.68’’ per fiber diam. 3.45’’ pitch Field Mosaic 6 pointings FOV = 3x2 arcmin2 OBSERVATIONS (1) • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS Pointing 2 Pointing 3 Pointing 7 Pointing 1 Pointing 4 Pointing 5 17/09/2010 IFS NGC5668 6/16

  8. IMAGE OBS.DATE TIME (UT)‏ # IMAGE AIRMASS texp (sec)‏ RA (deg)‏ Dec (deg)‏ NGC5668 p1 2007/06/22 20:59:21 3 1.207306 3x1000 218.5001 4.50243 21:36:47 NGC5668 p2 2007/06/22 22:13:53 4 1.38137 4x1000 218.5006 4.52086 23:12:31 NGC5668 p3 2007/06/22-23 23:33:44 3 1.75179 3x1000 218.4864 4.51397 00:11:08 NGC5668 p7 2007/06/23 21:00:15 3 1.211576 3x1000 218.5143 4.51076 21:37:41 NGC5668 p5 2007/06/23 22:15:29 3 1.362266 3x1000 218.5008 4.48774 22:52:55 NGC5668 p4 2007/06/23-24 23:28:42 3 1.743736 3x1000 218.4861 4.49738 00:06:07 OBSERVATIONS (2) • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS 7/17 17/09/2010 IFS NGC5668

  9. ANALYSIS: HII REGIONS (1) • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS 8/17 17/09/2010 IFS NGC5668

  10. ANALYSIS: ANNULI (1) • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS 9/17 17/09/2010 IFS NGC5668

  11. ANALYSIS: HII REGIONS (2) • IDENTIFY BAD FIBERS(Field stars or Cross Talk affected)‏ • REMOVE SKYLINES • SUBTRACT CONTINUUM EMISSION(by using a polynomial order of 3 and 3Å of EW in Hß absortion derived from the fit to the ring spectra)‏ • SELECTION OF WAVELENGTH RANGE(λλ 3700 – 6997 Å)‏ • CORRECT FROM THE CONTINUUM STELLAR ABSORPTION(by using respectively concentric annuli values, 1.7 Å for Hα and 2 Å for Hβ)‏ • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS 10/17 17/09/2010 IFS NGC5668

  12. ANALYSIS: IDL • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS • ENDED UP WITH 17 CONCENTRIC ANNULI SPECTRA. • ANALYSIS WITH IDL SCRIPT fit_poblaciones WE FIND THE UNDERLYING STELLAR POPULATION BY VARY 4 PARAMETERS. • FIND THE BEST MODEL IN THE TWO STELLAR LIBRARIES: Bruzual & Charlot (2003) AND MILES (Sánchez-Blázquez et al. 2006). • WE USE Charlot & Fall (2000) EXTINCTION LAW FOR STAR FORMING GALAXIES. 11/17 17/09/2010 IFS NGC5668

  13. ANALYSIS 12/17 17/09/2010 IFS NGC5668

  14. RESULTS: DUST ATTENUATION • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS • THE GENERAL TREND HAS A MEAN VALUE OF ~1 mag, IN AGREEMENT WITH OTHER WORKS. • INCREASE IN THE OUTER REGION, WORSE S/N RATIO (the errors are much larger)‏. • GAS ATTENUATION APPEARS LARGER THAN THE CONTINUUM ATTENUATION. • GOOD AGREEMENT WITH IDL VALUES AND E(B-V)CONTINUUM= 0.44x E(B-V)GAS. 13/17 17/09/2010 IFS NGC5668

  15. RESULTS: CHEMICAL ABUNDANCE • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS • INWARDS OF THE OPTICAL EDGE O/H RATIO FOLLOW THE UNIVERSAL RADIAL GRADIENT. • RANGE VALUE 8.15 ≤ 12 + log(O/H) ≤ 8.7; RBREAK = 36“ (260 kpc). • <GRADIENT VALUE> OF -0.0346 ± 0.0074 dex/kpc (-0.0042 ± 0.0009 dex/") IN AGREEMENT Zaritsky et al.(1994). • THERE’S A DISCONTINUITY NEAR THE OPTICAL EDGE OF THE DISK (Bresolin et al. 2009). 17/09/2010 IFS NGC5668 14/17

  16. RESULTS 17/09/2010 IFS NGC5668 15/17

  17. CONCLUSION • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS IN ORDER TO IMPROVE OUR KNOWLEDGE OF SPIRAL DISK WE HAVE OBTAINED A FULL 2-D SPECTRAL CUBE MOSAIC OF THE NEARBY SPIRAL GALAXY NGC5668. WE EXTRACTED AND ANALYZED THE SPECTRA OF HII REGIONS AND CONCENTRIC ANNULI. WE OBTAINED MAPS FOR DUST ATTENUATION OXYGEN ABUNDANCE GENERAL TREND =1.14 mag GRADIENT VALUE = -0.0345 dex/kpc 17/09/2010 IFS NGC5668 15/17

  18. FUTURE PROJECTS • STELLAR POPULATION USING EITHER SPECTRAL INDEX OR FULL SPECTRAL FITTING IN THE CONTEXT OF SPECTRO-PHOTOMETRIC MODELS OF GALAXY DISKS. • PART OF A SAMPLE OF A DOZEN GALAXIES OBSERVED WITH VIMOS (VLT) AND PPAK (IFU data)‏ from HGRS Herschel Galaxy Reference Survey; Boselli et al. 2006. • CALIFA’s SURVEY: Calar Alto Legacy Integral Field-Spectroscopy Astronomical Survey. • THE AIM OF THIS WORK • IFS • PPAK • THE CASE OF NGC5668 • OBSERVATIONS • ANALYSIS • RESULTS • CONCLUSION • FUTURE PROJECTS 17/09/2010 IFS NGC5668 16/17

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