Raffaella Anna Marino UNIVERSIDAD COMPLUTENSE DE MADRID Grupo

Raffaella Anna Marino UNIVERSIDAD COMPLUTENSE DE MADRID Grupo UCM de Astrofísica Instrumental y e. Xtragaláctica

THE AIM OF THIS WORK INTEGRAL FIELD SPECTROSCOPY PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS CONCLUSIONS FUTURE PROJECTS 08/05/2009 IFS NGC 5668 1/21

THE AIM OF THIS WORK IFS PPAK THE CASE OF NGC 5668 FORMATION AND EVOLUTION OF SPIRAL GALAXIES HOW OLD ARE THE SPIRAL DISK? HOW DID THEY CHEMICALLY EVOLVE? ARE THEY GROWING INSIDE-OUT? OBSERVATIONS ANALYSIS RESULTS CONCLUSION ADVANTAGES OF INTEGRAL FIELD SPECTROSCOPY FUTURE PROJECTS DUST ATTENUATION ELECTRON DENSITY CHEMICAL ABUNDANCE Hα/Hβ BALMER DECREMENT SII 6717/6731 RATIO KEWLEY & DOPITA RECIPE (2002) 08/05/2009 IFS NGC 5668 2/21

THE AIM OF THIS WORK IFS PPAK THE CASE OF NGC 5668 Simultaneous record of the spectral and spatial information in 2 D NOW: We obtain a cube fits for exposure → Image (+ filter): (x, y)@ Efficiency and (x, Homogeneity → Spectroscopy (long-slit): ) @ y fixed OBSERVATIONS ANALYSIS RESULTS CONCLUSION HOW TO REGISTER 3 D INFO TO THE 2 D DETECTOR? FUTURE PROJECTS 08/05/2009 IFS NGC 5668 3/21

THE AIM OF THIS WORK IFS FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS PPak-IFU CONCLUSION Principle design FUTURE PROJECTS Focal reducer Plate-scale Fiber configuration PPak – Fo. V Spatial sampling Fiber pitch Wavelength range 08/05/2009 focal reducer + hexagonal packed fiber-bundle lens F/10 to F/3. 3, diam=50 mm 17’’. 85 /mm 331 object, 36 sky, 15 calibration 74’’× 64’’(hexagonal packed) 2. 68” per fiber diameter 3. 5” fiber-to-fiber core diameter 150 um 400– 900 nm IFS NGC 5668 5/21

NAME THE AIM OF THIS WORK MORPHOLOGICAL TYPE RA(2000) IFS NGC 5668 Sa(s)d /Sc(s) II-III 14 h 33 m 24. 3 s Dec(2000) FIBERS +04° 27'02" B MAGNITUDE RPPAK LB 12. 13 ± 0. 03 mag 11. 28 ± 0. 01 mag 2. 7 ± 0. 6 × 109 LΘ THE CASE OF NGC 5668 RADIAL VELOCITY(Hel. ) 1582 ± 5 km/s DOBSERVATIONS (Galactocentric GSR) 21. 6 ± 1. 5 Mpc INCLINATION ANALYSIS 18° Position Angle (PA) 145° MAJOR RESULTS DIAMETER 3. 3 arcmin DIAMETER MINOR CONCLUSION 3. 0 arcmin HELIOCENTRIC REDSHIFT MFUTURE PROJECTS TOT MTOT /LB 0. 005277± 0. 000017 5. 7 × 1010 MΘ 2. 9 MΘ /LΘ, B E N 08/05/2009 IFS NGC 5668 6/21

THE AIM OF THIS WORK → SCHULMAN ET AL. (1994): with Arecibo telescope detected HVC and 8 HRVR. IFS FIBERS PPAK 3, 6 μm THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS 8, 0 μm CONCLUSION FUTURE PROJECTS GALEX → SCHULMAN ET AL. (1997): derived SFR from LFIR = (5. 8± 1. 2)× 109 LΘ and from LHα = 1. 0± 0. 3 × 108 LΘ → NAKANO ET AL. (2004): discovered a possible SN (SN 2004 G), Already discovered SN 1952 G, SN 1954 B BARBON ET AL. (1989), NGC 5668 is known as a SNe FACTORY. → GANDA ET AL. (2006): measured the gas distribution, stellar cinematics with SAURON, and found a ring-like structure. → NGC 5668 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. 08/05/2009 IFS NGC 5668 7/21

THE AIM OF THIS WORK IFS FIBERS PPAK OBSERVATIONAL PARAMETERS THE CASE OF NGC 5668 Date of observation 22/06/2007 to 24/06/2007 Telescope Calar Alto, 3. 5 m 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 = 3 x 2 arcmin 2 OBSERVATIONS ANALYSIS RESULTS CONCLUSION FUTURE PROJECTS 08/05/2009 IFS NGC 5668 8/21

THE AIM OF THIS WORK IMAGE OBS. DATE NGC 5668 p 1 2007/06/22 NGC 5668 p 2 2007/06/22 NGC 5668 p 3 2007/06/22 -23 NGC 5668 p 7 2007/06/23 RESULTS NGC 5668 p 5 2007/06/23 CONCLUSION NGC 5668 p 4 2007/06/23 -24 IFS FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS TIME (UT) 20: 59: 21 21: 36: 47 22: 13: 53 23: 12: 31 23: 33: 44 00: 11: 08 21: 00: 15 21: 37: 41 22: 15: 29 22: 55 23: 28: 42 00: 06: 07 # IMAGE AIRMASS texp (sec) RA (deg) Dec (deg) 3 1. 207306 3 x 1000 218. 5001 4. 50243 4 1. 38137 4 x 1000 218. 5006 4. 52086 3 1. 75179 3 x 1000 218. 4864 4. 51397 3 1. 211576 3 x 1000 218. 5143 4. 51076 3 1. 362266 3 x 1000 218. 5008 4. 48774 3 1. 743736 3 x 1000 218. 4861 4. 49738 FUTURE PROJECTS 08/05/2009 IFS NGC 5668 9/21

THE AIM OF THIS WORK IFS FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS CONCLUSION FUTURE PROJECTS 08/05/2009 IFS NGC 5668 10/21

THE AIM OF THIS WORK IFS FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS CONCLUSION FUTURE PROJECTS 08/05/2009 IFS NGC 5668 11/21

THE AIM OF THIS WORK → IDENTIFY BAD FIBERS ( Field stars or Cross Talk affected) IFS FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS → REMOVE SKYLINES → SUBTRACT CONTINUUM EMISSION (by using a polinomial order of 3) → SELECTION OF WAVELENGTH RANGE (λλ 3700 – 6997 Å) RESULTS CONCLUSION FUTURE PROJECTS 08/05/2009 → CORRECT FROM THE CONTINUUM STELLAR ABSORPTION (by using respectively concentric annuli values, 1. 7 Å for Hα and 2 Å for H ) λ in Å LINE IFS NGC 5668 [OII] 3727, 3 [OIII] 5006, 8 Hδ 4101, 7 [NII] 6548, 1 Hγ 4340, 5 Hα 6562, 8 [OIII] 4363, 0 [NII] 6583, 6 H 4861, 3 [SII] 6717, 0 [OIII] 4958, 9 [SII] 6731, 3 12/21

THE AIM OF THIS WORK → ENDED UP WITH 17 CONCENTRIC ANNULI SPECTRA. IFS → ANALYSIS WITH IDL SCRIPT Acm_fit WE FIND THE UNDERLYING STELLAR POPULATION BY VARY 4 PARAMETERS. FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS CONCLUSION →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. FUTURE PROJECTS 08/05/2009 IFS NGC 5668 13/21

THE AIM OF THIS WORK IFS → 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 FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS → WE USED THE TECHNIQUES DEVELOPED BY Muñoz. Mateos et al. (2009, in preparation) , THE CARDELLI EXTINCTION CURVE AND THE AVERAGE VALUE FOR RV= 3. 1 (Cardelli et al. 1989) CONCLUSION FUTURE PROJECTS 08/05/2009 → SO WE OBTAINED AV AND AHb, (which can then be compared with the AHb values derived from the analysis of the Balmer emission -line ratios). IFS NGC 5668 14/21

THE AIM OF THIS WORK IFS FIBERS PPAK THE CASE OF NGC 5668 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 08/05/2009 IFS NGC 5668 15/21

THE AIM OF THIS WORK IFS Ne-, IS ONE OF THE KEY PHYSICAL PARAMETERS NEEDED TO CHARACTERISE A GASEOUS NEBULA. FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS THE DENSITY ESTIMATORS ARE BASED ON MEASUREMENTS OF A SINGLE EMISSION-LINE RATIO SENSITIVE. WE MAKE USE OF THE [SII]λ 6716/λ 6731 LINE RATIO, Mc. Call et al. (1984). CONCLUSION FUTURE PROJECTS 08/05/2009 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. IFS NGC 5668 16/21

THE AIM OF THIS WORK IFS FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS CONCLUSION FUTURE PROJECTS → WE FIND A MEAN VALUE FOR ne OF 200 cm-3 IN AGREEMENT WITH OSTERBROCK (1989). 13/03/2009 IFS NGC 5668 17/21

THE AIM OF THIS WORK IFS WE UTILIZED KEWLEY & DOPITA RECIPE FIBERS PPAK THE CASE OF NGC 5668 We use this logical flow diagram for determining abundance and ionization parameter using optical emission-line diagnostics. OBSERVATIONS ANALYSIS RESULTS CONCLUSION FUTURE PROJECTS 13/03/2009 IFS NGC 5668 18/21

THE AIM OF THIS WORK IFS FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS → INWARDS OF THE OPTICAL EDGE O/H RATIO FOLLOW THE RADIAL GRADIENT. → CHANGE BETWEEN 8. 15 ≤ 12 + log(O/H) ≤ 8. 7. RESULTS CONCLUSION FUTURE PROJECTS → GRADIENT VALUE OF -0. 007 dex/kpc LOWER RESPECT Zaritsky et al. (1994). →THERE’S A DISCONTINUITY NEAR THE OPTICAL EDGE OF THE DISK (Bresolin et al. 2009). 08/05/2009 IFS NGC 5668 19/21

THE AIM OF THIS WORK IFS IN ORDERTO IMPROVE OUR KNOWLEDGE OF SPIRAL DISK WE HAVE OBTAINED A FULL 2 -D SPECTRAL CUBE MOSAIC OF THE NEARBY SPIRAL GALAXY NGC 5668. FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS WE EXTRACTED ANALYZED THE SPECTRA OF HII REGIONS AND CONCENTRIC ANNULI. RESULTS CONCLUSION FUTURE PROJECTS 08/05/2009 WE OBTAINED MAPS FOR GENERAL TREND =1 mag DUST ATTENUATION ne = 200 cm-3 ELECTRON DENSITY OXYGEN ABUNDANCE GRADIENT VALUE = -0. 007 dex/kpc IFS NGC 5668 20/21

THE AIM OF THIS WORK → CONSIDER SOME SPECTRAL INDICES THAT SUFFER FROM WEAKER AGE-EXTINCION-Z DEGENERACIES IFS → PART OF A SAMPLE OF A DOZEN GALAXIES OBSERVED WITH VIMOS (VLT) AND PPAK (IFU data) FIBERS PPAK THE CASE OF NGC 5668 OBSERVATIONS ANALYSIS RESULTS CONCLUSION → CALIFA’s SURVEY: Calar Alto Large Integral Field. Spectroscopy Astronomical Survey → HGRS : Herschel Galaxy Reference Survey; Boselli et al. 2006 FUTURE PROJECTS 08/05/2009 IFS NGC 5668 21/21