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Magpop Midterm Review Node OAMP-LAM, Marseille

Magpop Midterm Review Node OAMP-LAM, Marseille. Coordinator: V. Buat E.R.: Jakob Walcher S. Arnouts 1 , S. Boissier, A. Boselli, D. Burgarella, J. Iglesias-Paramo 2 & L. Tresse. 1: also at CFHT 2: also at IAA, Granada, Spain. Summary of the activities.

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Magpop Midterm Review Node OAMP-LAM, Marseille

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  1. Magpop Midterm ReviewNode OAMP-LAM, Marseille Coordinator: V. Buat E.R.: Jakob Walcher S. Arnouts1, S. Boissier, A. Boselli, D. Burgarella, J. Iglesias-Paramo2 & L. Tresse 1: also at CFHT 2:also at IAA, Granada, Spain

  2. Summary of the activities • Main input from OAMP/LAM: GALEX & VVDS data, interpretation. • Topic 1: Nearby Galaxies, physics of star forming galaxies • Topic 2: Distant Galaxies, star formation characteristics

  3. The GALEX missionP.I: C. Martin, Caltech, participation of CNES/ LAM M31, mosaics 1.2 deg ELAIS-S1, 12 000 sec GALEX: A UV surveyor with a large field of view

  4. The GALEX missionP.I: C. Martin, Caltech, participation of CNES/ LAM GALEX satellite, launch: Avril 2003, still observing Imaging mode at 1530Å(FUV) and 2315 Å (NUV), spatial resolution ~5 arcsec • All Sky Imaging Survey@ 20-21ABmag/14000 fields • Medium Imaging Survey@ 23 ABmag/1200 fields • Deep Imaging Surveys @ 25.5 ABmag/150 fields • Nearby Galaxies Survey: ~1000 galaxies X-correlations with surveys at other wavelengths

  5. GALEX sky coverage 10/02/2006

  6. The VIMOS VLT Deep Survey More than 220 galaxies observed simultaneously (march 2002) VIMOS mounted at Nasmyth B focus of VLT Melipal

  7. The VIMOS VLT Deep SurveyP.I.: O. Le Fèvre & G. Vettolani • 16 deg2 in four separate fields • Imaging survey (CFHT, ESO) UBVRI-K • Spectroscopic survey: few thousands of spectra @ R=250, redshift measurements I band selection: shallow survey IAB= 22.5 mag and deep survey IAB=24 mag (2 deg2/1 field) --> galaxies from z ~0 to z ~5 <z>=0.8

  8. Multi-wavelengths analyses Combining several wavelengths from ultraviolet to far infrared enables us to study: • Current Star formation in an unbiased way • Dust obscuration • Star formation history • Environmental effects In the nearby and more distant universe

  9. Nearby Galaxies: star formation laws Based on the Nearby Galaxies Survey of GALEX: UCM Madrid/OAMP-LAM Marseille Boissier et al. 06 The star formation as seen in UV extends to significantly lower gas densities than in H: for low levels of SF the H radiation becomes stochastic (very low number of ionizing stars) whereas the UV radiation due to older stars in larger number shows no break

  10. Nearby Galaxies: The effect of the environment on the evolution of galaxiesLAM/UCM Boselli et al. 06 NGC 4569: a typical HI deficient, anemic Virgo galaxy Models for ram pressure stripping consistent with the observed profiles (from NIR to FUV). A method to age-date the interaction.

  11. Nearby galaxies: other on-going projects • The dwarf galaxy survey: P.I. R. Peletier Groningen/LAM/UCM/Nottingam/Padova Obs. • Observation of a UV selected sample of ~ 100 dwarf irregular and quiescent galaxies in the Virgo cluster and in the field in imaging mode : near-IR, H imaging, low- res. and 2D spectroscopy • Status: 48 night (5% of the whole telescope time) allocated in two semesters 2006 at WHT, TNG, INT, NOT; 12 nights allocated in the first semester 2007. 2006 data under reduction • SFH in normal late type galaxies: LAM/Padova Obs • Constraining the star formation history of normal, late-type galaxies by comparing the UV to radio centimetric SED to the GRASIL model Status: work just started

  12. Nearby universe: Understanding star formation and dust obscuration • GALEX/IRAS samples in the nearby universe: several hundreds of galaxies carefully selected • Several studies: • Statistical analyses, IR/UV luminosity functions Buat et al. 06 • Star formation history and dust attenuation through SED fitting Burgarella et al. 05 • Dust attenuation analysis: Buat et al. 05, Panuzzo et al. 06, Inoue et al. 05 • Star formation estimations: Iglesias-Paramo et al. 05

  13. Understanding dust obscuration in nearby galaxies: Panuzzo et al 06 Based on GRASIL models: Padova obs. /OAMP-LAM Starbursts locus • A MW extinction curve is consistent with the FTIR/FFUV vs FUV-NUV color: the age-dependent extinction reduces the presence of the 2175 A bump • The wavelength dependence of the scattering albedo has also a strong impact on the FUV-NUV color (Inoue et al. 2005) FTIR/FFUV measures the amount of dust attenuation FUV-NUV color is sensitive to the wavelength dependance of dust attenuation

  14. Analyses of Spectral Energy Distributions of galaxies at z>0 • GALEX/SPITZER-SWIRE: SED fitting of UV selected galaxies with GRASIL models • GALEX/SPITZER-MIPS: SED fitting of Lyman Break Galaxies at z~1 • GALEX/VVDS/SWIRE: SED fitting of optically selected galaxies from z=0 to z~5--> Jakob Walcher talk

  15. UV (rest-frame) selected galaxies from z~0 to z~1 with GALEX/SWIREIglesias-Paramo et al. 07 • Templates:GRASIL models • Data: GALEX/ELAIS/SWIRE data UV vis NIR+MIR+FIR

  16. UV (rest-frame) selected galaxies from z~0 to z~1 with GALEX/SWIRE Ldust/LUV SFR/Mstar Total galaxy luminosity Mstar A diminution of dust attenuation in UV selected galaxies as z increases The so-called downsizing also seen in a pure UV selection

  17. Lyman Break Galaxies @ z~1 with GALEX/MIPS Burgarella et al. 06 FUV dropouts, z=0.9-1.3. CDFS: photometric redshifts, optical photometry, IRAC and MIPS data Observed wavelength A

  18. Thank you for your attention and please listen to Jakob for the continuation of the story….

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