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Intermediate Mass Galaxy Evolution Sequence
by François Hammer
Coll: H. Flores, M. Puech, R. Delgado-Serrano, B. Neichel, S. Peirani, M. Rodrigues, Y. Yang, J. Wang, S. Fouquet, P. Amram, E. Athanassoula, C. Balkowski, B. Epinat, I. Fuentes-Carrera, Y. Liang
The formation of large galactic disks: revival or survival?
Spiral disk - rotating
Irregular - rotating Compact - complex Minor merger - perturbed Compact - complex Merger - complex
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IoA Cambridge
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M 31 NGC 2997 NGC 1313
M83 M100 SABbc NGC 1365
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Thin disks are fragile to collisions
Mergers with other galaxies can easily destroy thin disks (e.g. Toth & Ostriker, 1992)
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Angular momentum acquired from galaxy interactions at earliest epochs;
Disks are then assumed to evolve without subsequent major mergers Spirals are assumed to be similar to the Milky Way so called “secular” scenario
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Excerpt from Dekel, Paris courses, 2006 28th September 2011
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What is the past history of giant spiral
galaxies?
Their progenitors are within distant galaxies
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Sample selection MJ(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 Mstellar > 1.5 1010Mʘ
(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 a complete description of galaxy properties, 6 Gyr ago
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Classification based on similarities with local galaxies Semi-automatic decision tree: GALFIT + Colour maps + Visual inspection
Morphological classification: semi-automatic decision tree
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• Delgado-Serrano et al, 2010, A&A, 509, 78 • Neichel et al. 2008, A&A, 484, 159 • also Zheng et al. 2005, 2006
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MJ(AB) < -20.3
~ Mstellar > 1.5 1010Mʘ
Morphological fractions in agreement
with van den Bergh (2002)
MJ(AB) < -20.3
~ Mstellar > 1.5 1010Mʘ
Delgado-Serrano et al. 2010,A&A, 509, 78
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Today: z=0
6 Gyrs ago: z=0.65
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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 gaseous component is linked to anomalous morphological distribution of the stars
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Neichel et al (2008, A&A 484, 159)
86% of Perturbed Rotation have peculiar morphologies
Sp Peculiar Comp Merg
# R
otat
ing
# Pe
rturb
ed
# C
ompl
ex
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80% of Rotating galaxies have spiral morphologies
95% of Complex Kinematics have peculiar morphologies
Disagreement between spatially-resolved kinematics and automatic classification
Automatic classifications (ACS, GINI-M20) overestimate by a factor ~2 the fraction of spirals at z~ 0.6
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Neichel et al (2008, A&A 484, 159)
86% of Perturbed Rotation have peculiar morphologies
# R
otat
ing
# Pe
rturb
ed
# C
ompl
ex
Sp Peculiar Comp Merg
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MJ(AB) < -20.3
~ Mstellar > 1.5 1010Mʘ
Today: z=0
6 Gyrs ago, z=0.65:
Delgado-Serrano et al. 2010,A&A, 509, 78
• E/S0 were mostly in place
• half of spirals did not
they had peculiar morphologies
and anomalous kinematics
Spirals: 72%
Peculiars: 52% Spirals: 31% 28th September 2011
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Associating Morpho-kinematics with physical processes
COLD STREAMS
CLUMP FRAGMENT.
MAJOR MERGERS
MINOR MERGERS OUTFLOWS
SECULAR EVOLUTION
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Associating Morpho-kinematics with physical processes
Minor merger? CK galaxies: Morpho-kinematic disturbances are global, not local:
GIRAFFU IFU resolution
~ 7 kpc @ z=0.6
Puech et al. (2007) 28th September 2011
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Associating Morpho-kinematics with physical processes
Outflows: - only a handful of galaxies have significant shifts between abs. and emission lines (Hammer et al. 09; Rodrigues et al., in prep).
Clump fragmentation & cold flows: - only 20% of anomalous galaxies are clumpy (Puech, 2010) - cold gas accretion tends to vanish in massive halos at z<1 (<1.5 Mo/yr at z~0.6 see Keres et al. 2009, Brooks et al. 2009)
Secular evolution: Kinematic perturbations are too strong and extended
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Associating Morpho-kinematics with physical processes
COLD STREAMS
CLUMP FRAGMENT.
MAJOR MERGERS
MINOR MERGERS OUTFLOWS
SECULAR EVOLUTION
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Peculiar morphologies & anomalous kinematics can be reproduced by major mergers
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Hammer et al. 2009, Astronomy & Astrophysics, 507, 1313
Example (Yang et al. 2009, Peirani et al. 2009): the fitting process is over determined
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A giant bar induced by a merger
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VF observed σ observed
VF simulated σ simulated
See Fuentes-Carrera et al. 2010, A&A, 513, 43
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A novel channel to form large disks: rebuilding disks after gas-rich mergers
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The orbital angular momentum from major mergers may solve the spin “catastrophe” (Maller, Dekel & Somerville, 2002)
Mass ratio
Hopkins et al 2010 Rodrigues et al. 2011
Gas
frac
tion
(%)
Lookback time (Gyr)
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Expectations from theory Excerpt from Lia Athanassoula, in Granada, 2009
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What about nearby spirals?
Many simulations report the formation of late-type disk after major mergers (Font+11, Brook+11, Keres
+11 etc…)
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Van den Bergh (2003): «It is suggested that M31 was created by the early merger of two massive galaxies »
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First passage ~ 8.5 Gyr ago, fusion ~ 5.5 Gyr ago
GADGET2, 8M particles
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The tumultuous history of nearby spirals (Martinez-Delgado et al. 2008, 2009)
NGC 5907 NGC 4013
M 63
Simulations from Font et al. 2006 Minor or major mergers?
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NGC 5907 NGC 4013
M 63
The tumultuous history of nearby spirals (Wang et al. , 2011, A&A submitted)
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NGC 5907 NGC 4013
M 63
The tumultuous history of nearby spirals (Wang et al. , 2011, A&A submitted)
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- B/T=0.17 - Thick disk comparable to IRAC 3.6 µm observations
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The tumultuous history of nearby spirals (Wang et al. , 2011, A&A submitted)
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- B/T=0.17 - Thick disk comparable to IRAC 3.6 µm observations - Residuals surrounding the disk are affected by dust (~2 mag at 5kpc)
NGC 5907 NGC 4013
M 63
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Discussion – Conclusions
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• Half of the progenitors of spirals, 6Gyr ago have peculiar morphologies & kinematics ==> excluded from the Hubble Sequence classification
• Half of the progenitors of spirals, 6 Gyr ago are found at different phases of a merger process Is that a too large fraction?
• No, this is because morpho-kinematics analysis ‘a la ‘ IMAGES are sensitive to all the merger phases (pre to post-fusion)
• The deduced merger rate is in good agreement with ΛCDM predictions (Puech, Hammer, Hopkins, Athanassoula, Flores et al, 2011, in prep.)
• This alleviates the disk survival issue and the angular momentum ‘catastrophe’and the hierarchical scenario may apply to both spiral & elliptical galaxies