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1 !"#"$%&'"((&"(()'*#%&+,-.&-.)&/ &#)((78(&9:7'&-.)&;01&<&=51& *%&B:"8C7,(&="''):& G&

2 M83 NGC 1365 M100 SABbc M 31 NGC 2997 NGC 1313 D&

3 N."-&,(&-.)&I"(-&.,(-7:%&79&J,"8-&(I,:"#& J"#"$,)(O&!"#$%&'%()#*$+(%,&-%#&.$+"$*&/$,+-*+&)-0-1$#,& H&

4 The IMAGES Survey: provides us with the most complete description of galaxy properties, 6 Gyr ago Sample selection M J(AB) < & 0.4 < z < fields including CDFS Intermediate-mass galaxies M stellar > M! (average ~M*, e.g. MW) Imaging ACS imagery (! 3 orbits) 3D Spectroscopy VLT/FLAMES-GIRAFFE (R=9000, 8-24hrs exposure) Spitzer VLT/FORS2 (600RI+600z) (! 3 hrs each) Color-morphology comparable to SDSS (depth, resolution) Spatially resolved kinematics Large scale dynamics SFR Metallicity of the gas (O/H) 27th February 2013 Shaping E-ELT Science and Instrumentation 4

5 IMAGES : a representative sample of M* galaxies, 6 billion years ago M J(AB) < M stellar > M! (average ~M*, e.g. the Milky Way) LF, z=0.5,1 Pozzetti et al galaxies Yang et al (2008) P&

6 !"#$%&"'(")(*+%',(-.+#%/(*%/%0+1-( Today 6 billion years, NASA, ESA, Sloan Digital Sky Survey, R. Delgado-Serrano, F. Hammer, Y.B. Yang, M. Puech & H. Flores (Observatoire de Paris) Q&

7 1.)&;):%&0":J)&1)#)(K7I)&R;01S& ;01T!>U?BB/& OzPoz! GIRAFFE! 27th February 2013 Shaping E-ELT Science and Instrumentation 7

8 Agreement between spatially-resolved kinematics and morphological classifications Neichel et al (2008, A&A 484, 159) # Rotating # Perturbed # Complex 95% of Complex Kinematics have peculiar morphologies 86% of Perturbed Rotation have peculiar morphologies 80% of Rotating galaxies have spiral morphologies Sp! Peculiar " Anomalous kinematics of the ionised gas is linked to anomalous morphological distribution of the stars V&

9 231(%'41-,"#-(")(*+%',(-.+#%/(*%/%0+1-( 6 billion years ago W&

10 231(%'41-,"#-(")(*+%',( -.+#%/(*%/%0+1-5(( 6(7+//+"'(81%#-(%*"( X,8)'"MK(& '"Z7:&'):J):(& GF&

11 PF[&79&J,"8-&(I,:"#&"8K)(-7:(&":)&)$I):,)8K,8J&'"Z7:& '):J):(& VLT/GIRAFFE & ESO, S. Peirani, F. Hammer & H. Flores (Observatoire de Paris) GG&

12 Mergers: observations vs. theory!cdm: Hopkins et al., 2010 IMAGES: Puech et al Both!CDM theory and observations predict that spirals have rebuilt their disks after a major merger (see also Keres+2011; Guedes+11, Font+11, Brook+11) GD&

13 14\?]6&^&_&G&J"#"$,)(& GH&

14 1434UU4N6&^&``&G&J"#"$,)(&+,-.& /2/01&a&bN51& Multiplex is a key issue for studies of galaxy evolution & formation See ELT-MOS white paper by Evans, Puech et al. Gc&

15 Spatially resolved spectroscopy of z ~4-6 galaxies is required for e.g. distinguishing merger from rotation (Puech et al. 2010) MOAO GLAO does not suffice: it requires MOAO Integral Field Units GLAO 27th February 2013 Shaping E-ELT Science and Instrumentation 15

16 A CENSUS for z >> 1 galaxies 30 arcseconds -! spatially resolved kinematics of z>>1 massive galaxies -! spectroscopy of dwarfs and their link to massive galaxies 27th February 2013 Shaping E-ELT Science and Instrumentation 16

17 9,:;8(,31(':$1#":-(;+-,%',(*%/%08(.".:/%&"'( 2!&&4:,J,8&79&L+":A)(6&I:,'7:L,"#&J"#"$,)(&7:&&ML"#&L+":9(O& $ < \".#)8&I.7-7f^& GE&

18 &&&&&&6&D&'",8&L,h):)8-&7*():A,8J&'7L)(&! =,J.&L)i8,M78&R=\3j&cF2VF&'"(TI,$S&+,-.&kGF&34?4&>Bg(& )ljlj&/?!0/&(k,)8k)&k"()& )ljlj&4n1>3452/;/&(k,)8k)&k"()& &GQFF&^&`&GlP&J"#"$,)(&,8&"8&/2/01&B7;j&UmPFFF2DFFFF&

19 Fibre Only Option: High Definition Mode (HDM) HDM focal plate Assumptions 12 science channels Light transfer optics: - Pick off mirror - Intermediate fold mirror - Receiving mirror In-plane rotation >180deg Courtesy: David Pearson Known issues Further degrees of freedom required in each optical item. Pick-and-place system required to cope with optical items of different shapes and sizes. Synchronisation of plate rotation with LGS system. Spectrographs See Poster by Jagourel et al.

20 Fibre Only Option: High Multiplex Mode HMM focal plate Courtesy: David Pearson Assumptions 120 science channels Buttons with fibre retraction scheme Stepped focal plate In-plane rotation >180deg Known issues Change in field curvature causes difficulty in fibre alignment and focus. Synchronisation of plate rotation with LGS system. Spectrographs See Poster by Jagourel et al.

21 Expected in J-band: 0.6% of the sky-continuum & much better with IFUs (Yang et al., Messenger, in press; see also Yang et al Poster)

22 BOARD: Beatriz Barbuy Jean-Gabriel Cuby Lex Kaper Simon Morris Coordination: François Hammer Project Manager: Pascal Jagourel Dep. : Phil Parr Burman Project Scientist: Chris Evans Dep. : Mathieu Puech Science Team Engineering Team System Engineer: Phil Rees Instrument Scientist: Gavin Dalton Dep. : Hector Flores Other contacts: LNA & AIP (fibers), Univ. Nice, Vienna, Stockholm

23 R)lJl&:)I:)()8-"MA)&("'I#)(&<&L)I-.S&! &?8&/2/01&B7;&K78-",8(&GQFF&&^&`&GlP&J"#"$,)(&! 345?>Y&! &48#%&"&345p/2/01&K"8&L)-)K-&-.)&i:(-&#,J.-j&(7#A)&-.)& :),78,("M78&I:7*#)'&<&I:7*)&-.)&J"#"$%&'"((&"(()'*#%& 100 billions stars per galaxy & 100 billions galaxies: they require a MOS DH&

24 Mixed Architecture Design: implementation Focal plate close up 1x LGS light path 1x NGS light path 1xHDM light path 6x HMM or IGM light paths See Poster by Jagourel et al.

25 nu/5/e1&51?1g5&4b&345?>y& Science:! a white paper written for all science cases (to be sent to the Project Science Group): too much Science Cases for a MOS at E-ELT!! all science cases require both high multiplex and high definition modes! trade-off between pixel size and need for K-band (high definition mode, MOAO-IFUs) and the high multiplex mode (100 to 300)! final trade-off expected mid-2013

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