Raffaella Anna Marino UNIVERSIDAD COMPLUTENSE DE MADRID Grupo UCM de Astrofísica Instrumental y eXtragaláctica

1/21 08/05/2009 IFS NGC5668  THE AIM OF THIS WORK  INTEGRAL FIELD SPECTROSCOPY  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSIONS  FUTURE PROJECTS

2/21 08/05/2009 IFS NGC5668 FORMATION AND EVOLUTION OF SPIRAL GALAXIES ADVANTAGES OF INTEGRAL FIELD SPECTROSCOPY DUST ATTENUATION ELECTRON DENSITY CHEMICAL ABUNDANCE  HOW OLD ARE THE SPIRAL DISK?  HOW DID THEY CHEMICALLY EVOLVE?  ARE THEY GROWING INSIDE-OUT? Hα/Hβ BALMER DECREMENT SII 6717/6731 RATIO KEWLEY & DOPITA RECIPE (2002)‏  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS

08/05/2009 IFS NGC5668 3/21  THE AIM OF THIS WORK  IFS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS HOW TO REGISTER 3D INFO TO THE 2D DETECTOR? NOW: →  Image (+ filter): (x, →  Spectroscopy (long-slit): (x, y fixed  Simultaneous record of the spectral and spatial information in 2D  We obtain a cube fits for exposure  Efficiency and Homogeneity

08/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTSPPak-IFU Principle design focal reducer + hexagonal packed fiber-bundle Focal reducer lens F/10 to F/3.3, diam=50 mm Plate-scale17’’.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 5/21

08/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS E NNAMENGC 5668 MORPHOLOGICAL TYPE Sa(s)d /Sc(s) II-III RA(2000)14h 33m 24.3s 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)‏ 21.6 ± 1.5 Mpc INCLINATION 18 ° Position Angle (PA)‏ 145 ° MAJOR DIAMETER 3.3 arcmin MINOR DIAMETER 3.0 arcmin HELIOCENTRIC REDSHIFT ± M TOT 5.7 × M Θ M TOT / L B 2.9 M Θ /L Θ,B 6/21

08/05/2009 IFS NGC5668 7/21  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS → SCHULMAN ET AL. (1994): with Arecibo telescope detected HVC and 8 HRVR. → SCHULMAN ET AL. (1997): derived SFR from L FIR = (5.8±1.2)×10 9 L Θ and from L Hα = 1.0±0.3 ×10 8 L Θ → NAKANO ET AL.(2004): discovered a possible SN (SN2004G), Already discovered SN1952G, SN1954B BARBON ET AL.(1989), NGC5668 is known as a SNe FACTORY. → GANDA ET AL.(2006): measured the gas distribution, stellar cinematics with SAURON, and found a ring-like structure. NGC5668 is part of several surveys: → NGC5668 is part of several surveys: § Pahre et al.(2004), “Mid-Infrared Galaxy Morphology along the Hubble Sequence” with IRAC, Spitzer. § Medium – Deep Imaging Survey, GALEX. 3,6 μ m 8,0 μ m GALEX

08/05/2009 IFS NGC56688/21  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS OBSERVATIONAL PARAMETERS Date of observation 22/06/2007 to 24/06/2007 TelescopeCalar Alto, 3.5m FocusCassegrain Instrument PPAK OFF-AXIS FIBER BUNDLE IFU Fibre projected size 2.68’’ per fiber diam. 3.45’’ pitch Field Mosaic 6 pointings FOV = 3x2 arcmin 2

9/21 08/05/2009 IFS NGC5668IMAGE OBS. DATE TIME(UT)‏ # IMAGE AIRMASS t exp (sec)‏ RA (deg)‏ Dec(deg)‏ NGC5668 p1 2007/06/22 20:59: x :36:47 NGC5668 p2 2007/06/22 22:13: x :12:31 NGC5668 p3 2007/06/ :33: x :11:08 NGC5668 p7 2007/06/23 21:00: x :37:41 NGC5668 p5 2007/06/23 22:15: x :52:55 NGC5668 p4 2007/06/ :28: x :06:07  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS

08/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS 10/21

08/05/2009 IFS NGC566811/21  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS

08/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS → IDENTIFY BAD FIBERS ( Field stars or Cross Talk affected)‏ → REMOVE SKYLINES → SUBTRACT CONTINUUM EMISSION (by using a polinomial order of 3)‏ → 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 H  )‏ 12/21LINE λ in Å LINE [OII]3727,3[OIII]5006,8 HδHδ 4101,7[NII]6548,1 HγHγ 4340,5HαHα 6562,8 [OIII]4363,0[NII]6583,6 HH 4861,3[SII]6717,0 [OIII]4958,9[SII]6731,3

 THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS → ENDED UP WITH 17 CONCENTRIC ANNULI SPECTRA. → ANALYSIS WITH IDL SCRIPT Acm_fit WE FIND THE UNDERLYING STELLAR POPULATION BY VARY 4 PARAMETERS. →FIND THE BEST MODEL IN THE TWO STELLAR LIBRARIES: Bruzal & Charlot (2003) AND MILES = Medium resolution INT Library of Empirical Spectra (Sánchez-Blázquez et al. 2006). → WE USE Charlot & Fall (2000) EXTINCTION LAW FOR STAR FORMING GALAXIES. 08/05/2009 IFS NGC566813/21

14/2108/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS → TOTAL IR (TIR) TO UV LUMINOSITY RATIO METHOD (Buat 1992; Xu & Buat 1995; Meurer et al. 1995, 1999) IS THE MOST RELIABLE ESTIMATOR OF THE DUST ATTENUATION → WE USED THE TECHNIQUES DEVELOPED BY Muñoz- Mateos et al. (2009, in preparation), THE CARDELLI EXTINCTION CURVE AND THE AVERAGE VALUE FOR R V = 3.1 (Cardelli et al. 1989)‏ → SO WE OBTAINED A V AND A Hb, (which can then be compared with the A Hb values derived from the analysis of the Balmer emission-line ratios).

15/21 08/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  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 (Gil de Paz et al. 2007). →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 VALUE UNTIL 25”, BUT FURTHER FOLLOW HII REGIONS

16/2108/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS N e -, IS ONE OF THE KEY PHYSICAL PARAMETERS NEEDED TO CHARACTERISE A GASEOUS NEBULA. THE DENSITY ESTIMATORS ARE BASED ON MEASUREMENTS OF A SINGLE EMISSION-LINE RATIO SENSITIVE. WE MAKE USE OF THE [SII]λ6716/λ6731 LINE RATIO, McCall et al. (1984). WE USE GARNETT (1992) RELATION, T [SII] ~ T [NII], (T [NII] can be estimated from the R 23 line ratio) AND WE CONSIDER A DIFFERENCE OF 3000 K BETWEEN THE [SII] AND [NII] EMITTING ZONES.

17/2113/03/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS → WE FIND A MEAN VALUE FOR n e OF 200 cm -3 IN AGREEMENT WITH OSTERBROCK (1989).

18/2113/03/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS WE UTILIZED KEWLEY & DOPITA RECIPE We use this logical flow diagram for determining abundance and ionization parameter using optical emission-line diagnostics.

19/21 08/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS → INWARDS OF THE OPTICAL EDGE O/H RATIO FOLLOW THE RADIAL GRADIENT. → CHANGE BETWEEN 8.15 ≤ 12 + log(O/H) ≤ 8.7. → GRADIENT VALUE OF dex/kpc LOWER RESPECT Zaritsky et al.(1994). →THERE’S A DISCONTINUITY NEAR THE OPTICAL EDGE OF THE DISK (Bresolin et al. 2009).

20/2108/05/2009 IFS NGC5668  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS IN ORDERTO 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 ELECTRON DENSITY OXYGEN ABUNDANCE GENERAL TREND =1 mag n e = 200 cm -3 GRADIENT VALUE = dex/kpc

 THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS 08/05/2009 IFS NGC566821/21 → CONSIDER SOME SPECTRAL INDICES THAT SUFFER FROM WEAKER AGE-EXTINCION-Z DEGENERACIES → PART OF A SAMPLE OF A DOZEN GALAXIES OBSERVED WITH VIMOS (VLT) AND PPAK (IFU data)‏ → CALIFA’s SURVEY: Calar Alto Large Integral Field- Spectroscopy Astronomical Survey → HGRS : Herschel Galaxy Reference Survey; Boselli et al. 2006

08/05/2009 IFS NGC5668 1/4 Bundle fibers x y Data cube Fibers  THE AIM OF THIS WORK  IFS  FIBERS  PPAK  THE CASE OF NGC5668  OBSERVATIONS  ANALYSIS  RESULTS  CONCLUSION  FUTURE PROJECTS Transform the geometry 2D of the object in 1D Fibers 2D -> 1D Grating elements 1D -> 2D Pseudo Slit Grating

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 08/05/2009 IFS NGC5668 2/4

08/05/2009 IFS NGC5668 3/4

08/05/2009 IFS NGC5668 4/4