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The emergence of the red-sequence. Gabriella De Lucia Max-Planck Institut für Astrophysik. A Workshop on Massive Galaxies over Cosmic Time II, Tucson, November 1st. An old result. Visvanathan & Sandage (1977). Mei et al. 2006. Coma. 5 mag!!!. De Propris et al. (1998). - PowerPoint PPT Presentation
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Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
The emergence of the The emergence of the red-sequencered-sequence
Gabriella De LuciaGabriella De LuciaMax-Planck Institut für AstrophysikMax-Planck Institut für Astrophysik
A Workshop on Massive Galaxies over Cosmic Time II, Tucson, November 1stA Workshop on Massive Galaxies over Cosmic Time II, Tucson, November 1st
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
An old result
Visvanathan & Sandage (1977)
De Propris et al. (1998)
5 mag!!!
Coma
The CMR - some factsThe CMR - some facts
Mei et al. 2006
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
This model may be too naiveThis model may be too naive a galaxy does not have a single well defined progenitor at a galaxy does not have a single well defined progenitor at each redshift each redshift (De Lucia & Blaizot 2006)
a it neglects the infall of new galaxiesa it neglects the infall of new galaxies
The CMR - the conjectures #1The CMR - the conjectures #1
A monolithic collapse occuring at high redshiftA monolithic collapse occuring at high redshift slope naturally arises taking into account SNe winds slope naturally arises taking into account SNe winds (Arimoto & Yoshii 1987)
a tight CM up to high redshift consistent with a passivea tight CM up to high redshift consistent with a passive evolution evolution (Kodama et al. 1998)
Gladders et al. 1998
obs. data
De Lucia & Blaizot 2006
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
The CMR - the conjectures #2The CMR - the conjectures #2
A hierarchical merger modelA hierarchical merger model slope arises because more massive Es form from theslope arises because more massive Es form from the mergers of more massive discs mergers of more massive discs (Kauffmann & Charlot 1998)
a tight CM up to high redshift - the results are robusta tight CM up to high redshift - the results are robustagainst halo-to-halo scatter against halo-to-halo scatter (De Lucia, PhD thesis)
Mean progenitor mass normalised to final mass
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
A truncation in the A truncation in the CMR in high CMR in high
redshift clusters?redshift clusters?
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
deep optical photometry from VLT (14 nights) deep optical photometry from VLT (14 nights)
Completed – White et al. 2005Completed – White et al. 2005
near-IR photometry from NTT (20 nights)near-IR photometry from NTT (20 nights)
Completed - Aragon-Salamanca et al. in preparationCompleted - Aragon-Salamanca et al. in preparation
multi-object spectroscopy with FORS2 on VLT (25 nights)multi-object spectroscopy with FORS2 on VLT (25 nights)
Completed - Halliday+ 2006; Milvang-Jensen+ in prepCompleted - Halliday+ 2006; Milvang-Jensen+ in prep
80 orbits of HST to image 10 high-z clusters!!!80 orbits of HST to image 10 high-z clusters!!!
Completed - Desai et al. in preparationCompleted - Desai et al. in preparation
WFI R (120m), V, I (60m) WFI R (120m), V, I (60m)
CompletedCompleted
A detailed follow-up of 20 clusters from LCDCS (Gonzalez et al. A detailed follow-up of 20 clusters from LCDCS (Gonzalez et al. 2001)2001)
10 clusters at z 10 clusters at z 0.5 and 10 clusters at z 0.5 and 10 clusters at z 0.8 0.8
The The EEso so DisDistant tant CCluster luster SSurveyurvey
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
A wide range of masses and A wide range of masses and structural propertiesstructural properties
White et al. 2005
Some Some EDisCS EDisCS clustersclusters
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
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Some Some EDisCS EDisCS CMRsCMRs
De Lucia et al. 2006, astro-ph/0610373
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
# o
f gala
xie
s z = 0.45 z = 0.57
z = 0.75
# o
f gala
xie
s
MI(obs)
MI(obs)
MV(rest)MV(rest)MV(rest)
The build-up of the CMR #1The build-up of the CMR #1
De Lucia et al. 2006, astro-ph/0610373
l/f = 0.48 +/- 0.08l/f = 0.53 +/- 0.09
0.71 +/- 0.10 0.86 +/- 0.13
0.89 +/- 0.14 0.95 +/- 0.14
redshift
nlu
m/
nfa
int
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
Kajisawa et al. (2000)
3C 324 z 1.2deficit
De Propris et al.(2003)
V
Composite EDisCS @z=0.75
Coma
I-obs
V-rest
Num
ber
of
gala
xie
s
De Lucia et al. 2004
A controversial resultA controversial result
Kodama et al. 2004
Andreon 2006
MS1054-0321
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
redshift
nlu
m/n
fain
t
The build-up of the CMR #2The build-up of the CMR #2
De Lucia et al. 2006, astro-ph/0610373
the blue galaxies observed in distant galaxy clusters provide the logical progenitors of faint red galaxies at z=0
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
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Semi-analytic Semi-analytic modelsmodels
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
galaxy galaxy formatioformatio
nn
Cooling (metallicity,structure, conductivity)
Star formation (threshold, efficiency, initial mass function)
Dust (formation, distribution, heating and cooling)
Galaxy interactions (morphological transformations, induced star formation)
Winds (IGM heating, IGM enrichment)
Stellar evolution (spectro-photometric evolution, yields,feedback)
AGN (BH growth, feedback)
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
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feedback
star formation
recycling
Hot Gas
Cold Gas cooling
Ejected Gas
Stars
re-incorporation
De Lucia, Kauffmann & White, 2004De Lucia, Kauffmann & White, 2004
- AGN heating- AGN heating
Croton et al. 2006Croton et al. 2006
The SAMs - the (simplified) physicsThe SAMs - the (simplified) physics
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
The evolution of the CM relation in SAM models
ComaSingle burst zf=3Exp. tau = 1
The build-up of the CMR in SAMsThe build-up of the CMR in SAMsDe Lucia et al. in preparation
U-V
U-VU-V
U-V
U-V
MV MV MV
MV MV
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
Very little build-up of the red-sequence!
De Lucia et al. in preparation
The build-up of the CMR in SAMsThe build-up of the CMR in SAMsV
-I V-I
V-I V-I
nlu
m/n
fain
t
MVMI MI
MIMI redshift
l/f = 0.31z = 0.0
l/f = 0.37z = 0.32
l/f = 0.38z = 0.41
l/f = 0.45z = 0.62
l/f = 0.47z = 0.76
U-V
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
u - r
Quantitatively the CM bimodality is not well reproduced
oTail of blue bright objects
o Transition region not well populated
o Excess of faint red satellites
The colour-magnitude bimodalityThe colour-magnitude bimodality
u - r
Mr = -
22.75
Mr = -21.25
Mr = -19.75 Mr = -18.25
Baldry et al. 2004
in preparation
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
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redshift
cluster ellipticals
field ellipticals
Lookback time (Gyr)
Mstar = 1012 Msun
Mstar = 109 Msun
The star formation historyThe star formation history
Most massive elliptical galaxies also the shortest formation timescales
De Lucia et al. 2006
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
1010M 1011M 1012M
cluster
field
Lookback time (Gyr)De Lucia et al. 2005
The star formation historyThe star formation history
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
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50 % stars in a single object
80 %
redshift
Formation and assemblyFormation and assembly
50 % stars formed
80 %
Fract
ion
of
gala
xie
s
redshift De Lucia et al. 2006
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
Mstar [M h-1]
Eff
ect
ive #
of
Eff
ect
ive #
of p
rog
en
itors
pro
gen
itors
Neff = 1/2 Neff = 1/2 Mfinal/<Mform>Mfinal/<Mform>
No disk instability
Disk instability
In the monolithicIn the monolithicapproximation: Neff=1approximation: Neff=1
The ellipticals progenitors numberThe ellipticals progenitors number
De Lucia et al. 2006
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
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Log[Mstar]Log[Mstar]
The age and metallicity dependenceThe age and metallicity dependenceB
- V
B -
V
Log[Mstar]Log[Mstar]
z=0.00z=0.00
z=0.00z=0.00
z=0.28z=0.28
z=0.28z=0.28
z=0.51z=0.51
z=0.51z=0.51
z=0.76z=0.76
z=0.76z=0.76
z=1.08z=1.08
z=1.08z=1.08
Zsta
r/ZZ
star/Z
Age (G
yr)
Age (G
yr)
De Lucia et al. in preparation
Gabriella De Lucia, November Gabriella De Lucia, November 1,Tucson1,Tucson
MPAMPA
QuestionsQuestions
Is there a truncation of the colour-magnitude relation at some redshift? Does this depend on the environment? Are SAMs able to reproduce quantitatively the colour bimodality? Are there too many satellites or just they go red too fast? Is the late assembly time in agreement with the observed evolution of the mass/luminosity function?