!"#"$%&'"((&"(()'*#%&+,-.&-.)&/012
3456&#)((78(&9:7'&-.)&;01&<&=51&
>3?!/5&(@:A)%&
*%&B:"8C7,(&="''):&
M 31
NGC 2997
NGC 1313
M83
M100 SABbc
NGC 1365
N."-&,(&-.)&I"(-&.,(-7:%&79&J,"8-&(I,:"#&
J"#"$,)(O&
!"#$%&'%()#*$+(%,&-%#&.$+"$*&/$,+-*+&)-0-1$#,&
Sample selection
M
J(AB)< -20.3 & 0.4 < z < 0.9
4 fields including CDFS
Imaging
ACS imagery (
!
3 orbits)
3D Spectroscopy
VLT/FLAMES-GIRAFFE
(R=9000, 8-24hrs exposure)
Spitzer
VLT/FORS2 (600RI+600z)
(
!
3 hrs each)
Intermediate-mass galaxies
M
stellar> 1.5 10
10M
!(average ~M*, e.g. MW)
SFR
Metallicity of the gas (O/H)
Color-morphology
comparable to SDSS (depth, resolution)
Spatially resolved kinematics
Large scale dynamics
The IMAGES Survey: provides us with the most complete
description of galaxy properties, 6 Gyr ago
IMAGES : a representative sample
of M* galaxies, 6 billion years ago
63 galaxies
M
J(AB)< -20.3
M
stellar> 1.5 10
10M
!
(average ~M*,
e.g. the Milky Way)
DE-.&B)*:@":%&DFGH& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78&
Yang et al (2008)
P&LF, z=0.5,1
!"#$%&"'(")(*+%',(-.+#%/(*%/%0+1-
(
Today
6 billion years, ago
DE-.&B)*:@":%&DFGH& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& Q&
1.)&;):%&0":J)&1)#)(K7I)&R;01S&
;01T!>U?BB/&
OzPoz
!
GIRAFFE
!
80% of Rotating galaxies have
spiral morphologies
95% of Complex Kinematics have
peculiar morphologies
Agreement between spatially-resolved kinematics
and morphological classifications
Anomalous kinematics of the ionised gas is linked to anomalous morphological
distribution of the stars
DE-.&B)*:@":%&DFGH& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& V&
Neichel et al (2008, A&A 484, 159)
86% of Perturbed Rotation have
peculiar morphologies
Sp
! Peculiar "
# Rotating
# Perturbed
231(%'41-,"#-(")(*+%',(-.+#%/(*%/%0+1-
(
6 billion years ago
231(%'41-,"#-(")(*+%',(
-.+#%/(*%/%0+1-5((
6(7+//+"'(81%#-(%*"
(
="#9&79&-.)'&."A)&I)K@#,":&
'7:I.7#7J,)(&"8L&"87'"#7@(&
X,8)'"MK(&
Y"8&*)&:)I:7L@K)L&*%&
.%L:7L%8"',K"#&'7L)#(&79&
'"Z7:&'):J):(&
PF[&79&J,"8-&(I,:"#&"8K)(-7:(&":)&)$I):,)8K,8J&'"Z7:&
'):J):(
&
VLT/GIRAFFE & HST/ACS
Mergers: observations vs. theory
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)
DE-.&B)*:@":%&DFGH& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& GD&
!
CDM: Hopkins et al., 2010
14\?]6&^&_&G&J"#"$,)(&
1434UU4N6&^&``&G&J"#"$,)(&+,-.&&
/2/01&a&bN51
&
DE-.&B)*:@":%&DFGH& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& Gc&
Multiplex is a key issue for studies of galaxy evolution & formation
See ELT-MOS white paper by Evans, Puech et al.
27th February 2013 Shaping E-ELT Science and Instrumentation
MOAO
GLAO
Spatially resolved
spectroscopy of z
~4-6 galaxies is
required for e.g.
distinguishing merger
from rotation
(Puech et al. 2010)
GLAO does not
suffice: it requires
MOAO Integral Field
Units
27th February 2013 Shaping E-ELT Science and Instrumentation 16
A CENSUS for z >> 1 galaxies
-!
spatially resolved kinematics of z>>1 massive galaxies
-!
spectroscopy of dwarfs and their link to massive galaxies
9,:;8(,31(':$1#":-(;+-,%',(*%/%08(.".:/%&"'(
$
<
=>?@AB6(
d"()L&78&Y?e\/0&K7@8-(&<&
\".#)8&I.7-7f^&
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"#"$,)(S&
&&&&&&6&D&'",8&L,h):)8-&7*():A,8J&'7L)(&
•!
=,J.&L)i8,M78&R=\3j&cF2VF&'"(TI,$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"#"$,)(&,8&"8&/2/01&B7;j&UmPFFF2DFFFF&
5))&Y.:,(&/A"8(f(&-"#X&97:&9@:-.):&(K,)8K)&:)o@,:)')8-(&
Fibre Only Option: High Definition Mode (HDM)
HDM focal plate
Assumptions
12 science channels
Light transfer optics:
- Pick off mirror
- Intermediate fold mirror
- Receiving mirror
In-plane rotation >180deg
Known issues
Further degrees of freedom
required in each optical item.
Pick-and-place system required to
cope with optical items of
different shapes and sizes.
Synchronisation of plate rotation
with LGS system.
Spectrographs
See Poster by Jagourel et al.
Fibre Only Option: High Multiplex Mode
HMM focal plate
Assumptions
120 science channels
Buttons with fibre retraction scheme
Stepped focal plate
In-plane rotation >180deg
Known issues
Change in field curvature causes
difficulty in fibre alignment and
focus.
Synchronisation of plate rotation
with LGS system.
Spectrographs
See Poster by Jagourel et al.
5X%&(@*-:"KM78&+,-.&i*):(&L)'78(-:"-)L&+,-.&B0?3/5&R>2*"8LS&78&(X%&
Expected in J-band: 0.6% of the sky-continuum & much better with IFUs
(Yang et al., Messenger, in press; see also Yang et al’ Poster)
Coordination: François Hammer
BOARD:
Beatriz Barbuy
Jean-Gabriel Cuby
Lex Kaper
Simon Morris
Project Scientist:
Chris Evans
Dep. : Mathieu Puech
Instrument Scientist:
Gavin Dalton
Dep. : Hector Flores
Science Team
Project Manager:
Pascal Jagourel
Dep. : Phil Parr Burman
System Engineer:
Phil Rees
Engineering
Team
Y78K#@(,78(&
•!
!77L&X87+#)LJ)&79&J"#"$%&)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&
DE-.&B)*:@":%&DFGH& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& DH&
100 billions stars per galaxy & 100 billions galaxies:
they require a MOS
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
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
