naoyuki tamura (university of durham) the universe at redshifts from 1 to 2 for early-type galaxies...
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Naoyuki Tamura(University of Durham)
The Universe at Redshifts from 1 to 2
for Early-Type Galaxies~ Unveiling “Build-up Era” with FMOS ~
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Outline
Summary
Galaxy population at z < 1 and z > 2
To understand the histories ofearly-type galaxies …Does stellar population tell us all ?
What are expected at 1 < z < 2 ?
Revisit the starting point :
How can the strengths of Subaru/FMOS be exploited ?
Extremely Red ObjectsLimitation due to lack of spectrum
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NGC 3923 : E4SFR
tEvolutions of CM relation & Fundamental Plane up to z ~ 1 look passive.
No active star formation is on-going at z=0. The bulk of stars seem to be old.
Stars in Elliptical Galaxies
Star formation Passiveevolutionstopped.
z > 2 ?
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Ages at z = 0 from spectroscopy
[km/s] 100 200 300 [km/s]
60 100 180
Trager et al. (2000)
Caldwell et al. (2003)
Cluster Group
Field Virgo
Field
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What does “age” tell us ?
“Galaxy formation history”
- when did a galaxy become an elliptical ?
“Star formation history”
- when did most of the stellar content form ??
Monolithic Collapse ScenarioStarburst
Gas rich
Hierarchical Merging ScenarioMajor mergerLuminosity
Function
Stellar Population
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Luminosity Function of E/S0s at z < 1COMBO-17~ 2800 arcmin^2, R < 26 (5), ~ 25000 galaxies
~ 5000 galaxies on the red sequence at 0.2 < z < 1.2.
Rix et al. (2004)
GEMSHigh resolution imaging follow-up with ACS/HST
Most of them (~ 85 %) seem to be morphologically early-type.
Evolution of luminosity function
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Luminosity Function of E/S0s at z < 1COMBO-
17
Bell et al. (2003)
About half of the local population were already in place at z ~ 1 ?
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Luminosity Function of E/S0s at z < 1
Morphology
Spectroscopy
Multi-band photometry
Im et al. (2002): DEEP Groth Strip survey
Chen et al. (2003): Las Campanas IR survey
Pozzetti et al. (2003): K20 survey
Suggest a mild evolution up to z ~ 150 ~ 80 % were already in place at z
~ 1 ?
(HST/WFPC2 images)
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Any “bona-fide” E/S0s at z > 2 ?
Radio galaxies
Rocca-Volmerange et al. (2004)
Pentericci et al. (2001)
(z = 2.3)
(z = 2.4)
Passive evolution prediction
(z = 10, M = 10 M )
f12
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Any “bona-fide” E/S0s at z > 2 ?
Lyman Break GalaxiesSCUBA Galaxies
Red galaxies from FIRES
No clear Hubble sequence ?A population of passive E/S0s have not revealed
yet ?
Stellar mass ~ 10 M
J-K ~ 2 or redder
z = 2 ~ 3 (?)
z > 3
Strong clustering
<z> ~ 2.5 (1 < z < 4)SFR ~ 1000 M /yr
SFR ~ 1 - 100 M /yr
Starburst galaxies ?
10
Investigations are on-going ...
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How can they be linked at z = 1 ~ 2 ? Star forming
galaxies Passive evolution phase
Luminosity function of passive galaxiesand its evolution at z = 1 ~ 2 A number of post-starburst galaxies ?
Half or more of the local population show up in this epoch ?
Consumption ?
Distant clusters are revealed ?
Through redshift survey …
somehowEnvironmental effect ?
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Extremely Red Objects (EROs)
Good candidates for passive ellipticals at z > 1.
Heterogeneity Although the colour criterion seems to
work for isolating passive ellipticals …
Luminosity function of EROs has been studied.Our understandings of EROs have
been limited due to lack of spectra.
R-K > 5 / I-K > 4
(Cimatti et al. 2003; Yan et al. 2004)
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Smith et al. (2002)
Smail et al. (2002)
Mannucci et al. (2002)
Colour criterion to classify EROs Cimatti et al.
(2003)
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Miyazaki et al. (2002)
Caputi et al. (2004)
Evolution of ERO LF at z > 1 ?
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Extremely Red Objects (EROs)
Good candidates for passive ellipticals at z > 1.
Heterogeneous Although the colour criterion seems to
work for isolating passive ellipticals …
Luminosity function of EROs has been studied.
Photo-z : z ~ 0.3 at z ~ 1.5
Our understandings of EROs have been limited due to lack of spectra.
Too coarse to investigate evolution at 1 < z < 2 ?
R-K > 5 / I-K > 4
(Cimatti et al. 2003; Yan et al. 2004)
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What we need to do are :To perform deep spectroscopic
observations and to get quality data.
Redshift
ClassificationAbsorption line
To collect a large number of galaxies at z > 1 from a large survey area.
Good statistics Cosmic variance
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The other word of FMOS (1)Wide spectral coverage in the NIRSpectral features in the rest frame optical
are available for galaxies at z > 1.
Combination with UKIDSS-DXS
Optimal for redshift survey.
(& Subaru/Suprime-Cam)
Allows us to efficiently pick up candidates for galaxies at z > 1 with colour information.
Luminosity can be derived with the aid of redshift.
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The other word of FMOS (2)Wide field & high multiplicity
30’
FMOS-FOV / 400 fibres
~ 200 fibres will be available for objects in one exposure.
Better statisticsLonger integration
Highly efficient !
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Simulated Spectrum
H = 20.5 mag
Old stellar population (3.0 Gyr age) at z = 1.5
8 hr integration (1 hr x 8) & 5 pix. binning
4000 A
G-band
H
Mgb
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Gemini Deep Deep Survey
4 x 30 arcmin^2 fieldNod & shuffle technique
Gemini Multi-Object Spectrograph
> 30 hr integration per field
Fibre Multi-Object SpectrographFOV ~ 700
arcmin^2200/200 fibres for object/sky(+ Double beam switching obs. ?)??? hr integration per
FOV
???????????????? Survey
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Simulated Spectrum
H = 22.0 mag
Old stellar population (3.0 Gyr age) at z = 1.5
100 hr integration (1 hr x 100) & 5 pix. binning
4000 A
G-band
H
MgbNaD
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Summary
Luminosity function of passive galaxies Evolution of LF between z = 1
and 2.A number of post-starburst galaxies ?
To understand history of early-type galaxyLuminosity
FunctionStellar Population
Bridging two epochs ? z <
12 < z
Need to look at absorption lines
Star forming galaxiesPassive evolution
Wide field & high multiplicity can beexploited for deep observation.