with MUSE [ Scary Monsters ]...[ Scary Monsters ] Naab l.24) A n g u l a r m o m e n t u m I n s i t...
Transcript of with MUSE [ Scary Monsters ]...[ Scary Monsters ] Naab l.24) A n g u l a r m o m e n t u m I n s i t...
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Most Massive Galaxies with MUSE
[ Scary Monsters ]
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Naab et al. (2014)A
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Various Mass
regimes
⇒ Most massive galaxies
In situ vs Ex situ
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Lin et al. (2013)
Mass Growth @
the high Mass end Time evolu�on
⇒ Most massive galaxies
x 2-4 since z=1.5
Observa�ons
Model
Now
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Or Or ?
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Or Or ?
Why should we care ?
Orbital structure
Morphology, Dynamics, Mass
Constraints on Forma�on / Evolu�on
How are these formed / assembled ?
Naab, Oser, Emsellem et al. 2014
Emsellem, Cappellari, Krajnović et al. 2011
Merri( 2013
Things change at high mass
Angular momentum
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What's happening at Masses > 1011.5 M⊙
?
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[VLT/VIMOS]Jimmy, Brough et al. 2013
BCGs
[MASSIVE – Mitchell Spec + AO-NIFS]
Ma et al. 2014
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a MUSE GTO programme PI Eric Emsellem; Davor Krajnović
The Project
Goals:
Dynamical state, Dark ma-er content, Dynamical state, Dark ma-er content,
SFH, IMF SFH, IMF + Test predic1ons of numerical simula1ons
How:
Stellar content + dynamics
of the most massive galaxies
in densest environments
e.g. Ho3man et al. 2010, Bois et al. 2011,
Naab et al. 2014, Rö(gers et al. 2014,
Vogelsberger et al. 2014 (Illustris), Schaye
et al. 2015 (EAGLE), Hirschmann et al.
2015…
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More massive,
richer, clusters
→ 2 sub-samples (z~0.04)
Shapley Super Cluster
(brighter than -25.7 mag in K)
+
BCGs in rich clusters
The Project
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Shapley Super Cluster
~200 Mpc [~1kpc / arcsec]
Mercurio et al. (2006)
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Why MUSE?
Emsellem, Krajnović, Sarzi 2014
M 87
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MUSE (V-R-I)
“Snapshot”
Images
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PGC018236 and PGC019085
Rota1on around minor axis – counter rota1on
Rota1on around minor axis
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PGC003342 and PGC065588Rota1on around minor and major axis
Rota1on around major axis
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MUSE colour
PGC007300Velocity Dispersion
Age Metallicity
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PGC047202The most massive galaxy in Shapley
4 x 4h
101 merged data cubes...
374 544 spectra
2’
x 2
’
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PGC047202
• ds
Rota1on around minor axis
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PGC046832
• ds
A double A double
KDCKDC
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TYPE #
Prolate-like 8
Oblate-like 5
Including > 3 KDC
Non-rotators 1 (?)
First Results
> ½ show prolate-like rota�on ?
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The morphology of galaxies change with mass
Oblate Mildly Triaxial Prolate ?⇒ ⇒
First Results
Ques�ons
Dynamical models ?Dynamical models ?
Assembly history?Assembly history?
Geometry
Mass
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Age [Fe/H]
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Mass Assembly
Guérou et al. 2016
NGC 3115
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Mass Assembly
Guérou et al. 2016
NGC 3115
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We have great tools !
Zeroth order : Mass, scale
First order : velocity moments, age, metallicity
BUT → are we just geIng V, s, … for any galaxy we observe… ?
aren't we doing this since… 1990?
WHAT IS MISSING ?WHAT IS MISSING ?
True coupling (dynamics/stellar pop) + new perspec1ve
Some (Tequila-weighted) ideas to be applied on M3G Galaxies
⇒ f[ (x,y,z), M, t, [Fe/H], Ang. Mom.](must be robust for comparisons with simula1ons)
How are we doing?
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Something new?
● At VERY high mass Prolateness rules ! (?)⇒● Mass profle transi�on to the cluster HALO⇒● Probing the mass assembly via spectral fOng