!"#"$%&'"((&"(()'*#%&+,-.&-.)&/012 3456&#)((78(&9:7'&-.)&;01&<&=51& >3?!/5&(@:A)%& *%&B:"8C7,(&="''):& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& G&
M83 NGC 1365 M100 SABbc M 31 NGC 2997 NGC 1313 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& D&
N."-&,(&-.)&I"(-&.,(-7:%&79&J,"8-&(I,:"#& J"#"$,)(O&!"#$%&'%()#*$+(%,&-%#&.$+"$*&/$,+-*+&)-0-1$#,& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& H&
The IMAGES Survey: provides us with the most complete description of galaxy properties, 6 Gyr ago Sample selection M J(AB) < -20.3 & 0.4 < z < 0.9 4 fields including CDFS Intermediate-mass galaxies M stellar > 1.5 10 10 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
IMAGES : a representative sample of M* galaxies, 6 billion years ago M J(AB) < -20.3 M stellar > 1.5 10 10 M! (average ~M*, e.g. the Milky Way) LF, z=0.5,1 Pozzetti et al 2003 63 galaxies 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& Yang et al (2008) P&
!"#$%&"'(")(*+%',(-.+#%/(*%/%0+1-( Today 6 billion years, ago @ NASA, ESA, Sloan Digital Sky Survey, R. Delgado-Serrano, F. Hammer, Y.B. Yang, M. Puech & H. Flores (Observatoire de Paris) 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& Q&
1.)&;):%&0":J)&1)#)(K7I)&R;01S& ;01T!>U?BB/& OzPoz! GIRAFFE! 27th February 2013 Shaping E-ELT Science and Instrumentation 7
Agreement between spatially-resolved kinematics and morphological classifications Neichel et al (2008, A&A 484, 159) # Rotating # Perturbed # Complex 95% of Complex Kinematics have peculiar morphologies 86% of Perturbed Rotation have peculiar morphologies 80% of Rotating galaxies have spiral morphologies Sp! Peculiar " Anomalous kinematics of the ionised gas is linked to anomalous morphological distribution of the stars 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& V&
231(%'41-,"#-(")(*+%',(-.+#%/(*%/%0+1-( 6 billion years ago 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& W&
231(%'41-,"#-(")(*+%',( -.+#%/(*%/%0+1-5(( 6(7+//+"'(81%#-(%*"( ="#9&79&-.)'&."A)&I)K@#,":& '7:I.7#7J,)(&"8L&"87'"#7@(& X,8)'"MK(& Y"8&*)&:)I:7L@K)L&*%&.%L:7L%8"',K"#&'7L)#(&79& '"Z7:&'):J):(& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& GF&
PF[&79&J,"8-&(I,:"#&"8K)(-7:(&":)&)$I):,)8K,8J&'"Z7:& '):J):(& VLT/GIRAFFE & HST/ACS 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& @ ESO, S. Peirani, F. Hammer & H. Flores (Observatoire de Paris) GG&
Mergers: observations vs. theory!cdm: Hopkins et al., 2010 IMAGES: Puech et al. 2012 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) 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& GD&
14\?]6&^&_&G&J"#"$,)(& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& GH&
1434UU4N6&^&``&G&J"#"$,)(&+,-.& /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. 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& Gc&
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
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
9,:;8(,31(':$1#":-(;+-,%',(*%/%08(.".:/%&"'( 2344&)-0-1$#,&-+&56&278&$*&-*&9:9;!&<(=&>?(,+0@&/.-%A,B& 2!&&4:,J,8&79&L+":A)(6&I:,'7:L,"#&J"#"$,)(&7:&&ML"#&L+":9(O& 2!&07+&(@:9"K)&*:,J.-8)((&J"#"$,)(&,8&-.)&J"()7@(2:,K.&g8,A):()& 2!1)(-&79&K@:A"-@:)&R!&@(,8J&=>>&J"#"$,)(S& $ < =>?@AB6( d"()l&78&y?e\/0&k7@8-(&<& \".#)8&I.7-7f^& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& GE&
&&&&&&6&D&'",8&L,h):)8-&7*():A,8J&'7L)(&! =,J.&L)i8,M78&R=\3j&cF2VF&'"(TI,$S&+,-.&kGF&34?4&>Bg(& )ljlj&/?!0/&(k,)8k)&k"()& &L)-",#)L&X,8)'"MK(&79&J"#"$,)(&@I&-7&^mPj&UmPFFF&! =,J.&'@#MI#)$&R=33j&GFF2DPFSj&!0?4T()),8J&:)(7#@M78& )ljlj&4n1>3452/;/&(k,)8k)&k"()& &GQFF&^&`&GlP&J"#"$,)(&,8&"8&/2/01&B7;j&UmPFFF2DFFFF& 5))&Y.:,(&/A"8(f(&-"#X&97:&9@:-.):&(K,)8K)&:)o@,:)')8-(&
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.
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.
5X%&(@*-:"KM78&+,-.&i*):(&L)'78(-:"-)L&+,-.&B0?3/5&R>2*"8LS&78&(X%& 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)
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
Y78K#@(,78(&!!77L&X87+#)LJ)&79&J"#"$%&)A7#@M78&^&_&G&R>3?!/5S&! 5M##&o@)(M78(&"-&^`G2D6&'):J):(&A):(@(&K7#L&"KK:)M78& R)lJl&:)I:)()8-"MA)&("'I#)(&<&L)I-.S&! &?8&/2/01&B7;&K78-",8(&GQFF&&^&`&GlP&J"#"$,)(&! &=,J.&'@#MI#)$&<&.,J.&L)i8,M78&'7L)(&8))L)L6&-.,(&,(& 345?>Y&! &48#%&"&345p/2/01&K"8&L)-)K-&-.)&i:(-&#,J.-j&(7#A)&-.)& :),78,("M78&I:7*#)'&<&I:7*)&-.)&J"#"$%&'"((&"(()'*#%& &>,##&C7&DE*0('F&CG&HEI@&J&K7&<0(%#,&+-0L,B& 100 billions stars per galaxy & 100 billions galaxies: they require a MOS 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& DH&
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.
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