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

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

2/1717/09/2010 IFS NGC5668 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 ? H α /H β BALMER DECREMENT KEWLEY & DOPITA RECIPE (2002) ‏  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS THE AIM OF THIS WORK

17/09/2010 IFS NGC5668 3/17 HOW TO REGISTER 3D INFO TO THE 2D DETECTOR? NOW:  Image (+ filter): (x,  Spectroscopy (long-slit): (x, y fixed INTEGRAL FIELD SPECTROSCOPY  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  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

17/09/2010 IFS NGC5668  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS 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 4/17

 THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS NAMENGC 5668 MORPHOLOGICAL TYPESc(s) II-III/Sd RA(2000)14 h 33 m 24.3 s Dec(2000) +04 ° 27'02" B MAGNITUDE R MAGNITUDE L B ± 0.03 mag ± 0.01 mag 2.7 ± 0.6 × 10 9 L Θ ‏ RADIAL VELOCITY(Hel.)‏1582 ± 5 km/s D (Galactocentric GSR)‏15.6 ± 1.5 Mpc INCLINATION 18 ° ‏ Position Angle (PA)‏ 145 ° MAJOR DIAMETER3.3 arcmin MINOR DIAMETER3.0 arcmin HELIOCENTRIC REDSHIFT ± M TOT 5.7 × M Θ M TOT / L B 2.9 M Θ /L Θ, B 17/09/2010 IFS NGC5668 E N 5/17 THE CASE OF NGC 5668 SDSS GALEX 8,0 μ m 3,6 μ m

17/09/2010 IFS NGC56686/16 OBSERVATIONAL PARAMETERS Date of observation 22/06/2007 to 24/06/2007 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  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS OBSERVATIONS (1) Pointing 5 Pointing 1 Pointing 2 Pointing 7 Pointing 3 Pointing 4

7/17 17/09/2010 IFS NGC5668 IMAGEOBS. DATE TIME (UT)‏ # IMAGE AIRMAS S texp (sec)‏ RA (deg)‏ Dec (deg)‏ NGC5668 p1 2007/06/2220:59: x :36:47 NGC5668 p2 2007/06/2222:13: x :12:31 NGC5668 p3 2007/06/ :33: x :11:08 NGC5668 p7 2007/06/2321:00: x :37:41 NGC5668 p5 2007/06/2322:15: x :52:55 NGC5668 p4 2007/06/ :28: x :06:07 OBSERVATIONS (2)  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS

17/09/2010 IFS NGC5668 8/17  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS ANALYSIS: H II REGIONS (1)

17/09/2010 IFS NGC5668 9/17  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS ANALYSIS: ANNULI (1)

10/17 17/09/2010 IFS NGC5668 → 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 NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS ANALYSIS: H II REGIONS (2)

→ 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. 17/09/2010 IFS NGC5668  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS ANALYSIS: IDL 11/17

12/17 17/09/2010 IFS NGC5668 ANALYSIS

13/17 17/09/2010 IFS NGC5668 ~ → 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 = 0.44 x E(B-V) GAS.  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS RESULTS: DUST ATTENUATION

14/1717/09/2010 IFS NGC5668 → INWARDS OF THE OPTICAL EDGE O/H RATIO FOLLOW THE UNIVERSAL RADIAL GRADIENT. → RANGE VALUE 8.15 ≤ 12 + log(O/H) ≤ 8.7; R BREAK = 36 “ (260 kpc). → OF ± dex/kpc ( ± dex/ " ) IN AGREEMENT Zaritsky et al.(1994). → THERE’S A DISCONTINUITY NEAR THE OPTICAL EDGE OF THE DISK (Bresolin et al. 2009).  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS RESULTS: CHEMICAL ABUNDANCE

15/1717/09/2010 IFS NGC5668 RESULTS

15/1717/09/2010 IFS NGC5668 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 = dex/kpc  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS CONCLUSION

17/09/2010 IFS NGC566816/17 → 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 → CALIFA’s SURVEY: Calar Alto Legacy Integral Field-Spectroscopy Astronomical Survey.  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC 5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS FUTURE PROJECTS

Bundle fibers Fibers Transform the geometry 2D of the object in 1D Fibers 2D -> 1D Grating elements 1D -> 2D Pseudo Slit Grating  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS x y Data cube

R3D (Sanchez 2006) ‏ PRE-REDUCTION = Master Bias ( Bias subtraction and Cosmic ray rejection ) ‏ IDENTIFICATION OF SPECTRA POSITION ON THE DETECTOR = Dome Flat EXTRACTION OF EACH INDIVIDUAL SPECTRUM CROSS TALK DISTORSION CORRECTION OF THE EXTRACTED SPECTRA FIBER FLAT FLUX CALIBRATION SKY SUBTRACTION MOSAIC AND DITHER RECONSTRUCTION IFS NGC5668 2/4

IFS NGC5668 3/4

IFS NGC5668 4/4