vvds first epoch resultsmoriond.in2p3.fr/j04/trans/ilbert.pdf · vvds first epoch results o. le...
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![Page 1: VVDS FIRST EPOCH RESULTSmoriond.in2p3.fr/J04/trans/ilbert.pdf · VVDS FIRST EPOCH RESULTS O. Le Fèvre, G. Vettolani and the VVDS team. Olivier Ilbert (LAM-OAMP) Moriond – March](https://reader031.vdocuments.mx/reader031/viewer/2022041117/5f2b4d3c76b81a35ec5069d8/html5/thumbnails/1.jpg)
Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
GALAXY LUMINOSITY FUNCTIONS UP TO Z=1.5
Olivier ILBERT
L. Tresse O. IlbertS. Arnouts
E. ZuccaS. Bardelli G. Zamorani
Laboratoire d'Astrophysique de Marseille – OAMP
VVDS FIRST EPOCH RESULTS
O. Le Fèvre, G. Vettolani and the VVDS team
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
THE VVDS DEEP SAMPLE
Spectroscopic data combined with (U)BVRI(JK) multi-color catalogue
Purely magnitude selected sample17.5 ≤ I ≤ 24
(H. J. McCracken et al. 2003, A&A, 410,17)
3 observing runs, 200220 VIMOS pointing , 4h exposure, R=200
10,500 spectraThe largest spectroscopic sample at I ≤ 24 up to now !
The deep VVDS 0226-04 field : 1.2 deg 2
AB
AB
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
DEEP SPECTROSCOPIC SAMPLE
(O. Le Fèvre et al. 2004)
Preliminary deep spectroscopic sample :
485 stars + 45 QSOs
Full sample being assembled (up to z=5)
Data reduction is on-going
VVDS 0226-04
4,500 redshifts of galaxies @z < 1.5<z> = 0.73
Area already covered 0.5 deg2
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
LUMINOSITY FUNCTION TOOL
Fit the best template on multi-color data : SED, k-correctionAbsolute magnitude
Three non-parametric estimators , 1/Vmax , C+ , SWML
The VVDS LF tool
(Ilbert et al. , 2004, MNRAS, in press, astro-ph/0402202)
One parametric estimator, STY , using Schechter function
Le Phare , www.oamp.fr/arnouts/LE_PHARE.html , S. Arnouts & O. Ilbert
Procedure to limit the model dependency using multi-color data
Can be applied on any multi-color data
Quality control of the LF tool on simulated data
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
GLOBAL LF UP TO Z=1.5
~1,000 galaxies at 0.8 ≤ z < 1 !
Strong constrain on the slopeup to z=1.5
Study the LF evolution up toz=1.5 with a same sample
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
GLOBAL LF UP TO Z=1.5
~1,000 galaxies at 0.8 ≤ z < 1 !
Strong constrain on the slopeup to z=1.5
Study the LF evolution up toz=1.5 with a same sample
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
EVOLUTION OF THE GLOBAL LF SHAPE
68% error contour90% error contour
SDSS (Blanton et al., 2001, ApJ, 121, 2358)
evolution of the global LF shape from z=0.05 up to z=1.5
Brightening of 2 mag in M*
Steepening of the slope
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
EVOLUTION OF THE LUMINOSITY DENSITY
Good constraint on the LDup to z=1.2
Dashed lines :
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
LF PER TYPE : CLASSIFICATION
Fit the best template on multi-color data
Split our sample in four photometric typesfrom the CWW set of template
Photometric type
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
THE EVOLUTION OF TYPE 1 LF
WEAK EVOLUTIONFOR REDDEST TYPES
TO
STRONG EVOLUTION FOR BLUEST TYPES
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
THE EVOLUTION OF TYPE 2 LF
WEAK EVOLUTIONFOR REDDEST TYPES
TO
STRONG EVOLUTION FOR BLUEST TYPES
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
THE EVOLUTION OF TYPE 3 LF
WEAK EVOLUTIONFOR REDDEST TYPES
TO
STRONG EVOLUTION FOR BLUEST TYPES
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
THE EVOLUTION OF TYPE 4 LF
WEAK EVOLUTIONFOR REDDEST TYPES
TO
STRONG EVOLUTION FOR BLUEST TYPES
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
SHAPE OF THE LF PER TYPE
Steepening of the slope from
reddestto
bluest photometric types
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
SHAPE OF THE LF PER TYPE
Steepening of the slope from
reddestto
bluest photometric types
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
LF PER ENVIRONMENT
Environment classification on large scale (C. Marinoni) :
Smoothing with a Gaussian of caracteristic length 5 Mpc
Definition of a local density contrast :
δ < 0 => under-dense regionδ ≥ 0 => over-dense region
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
GLOBAL LF PER ENVIRONMENT
Significant dependency of the global LF shape with large-scale environment
90% confidence level
One sigma confidence level
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
CONCLUSIONS
Global LF up to z=1.5 with 4,500 spectroscopic redshifts
Brightening of the M* parameter of 2 magnitudes
Steepening of the slope with redshift
Evolution of the LF for four photometric types
Strong evolution of bluest type, weak evolution of reddest type
Steep slope of bluest type , deacreasing slope of reddest type
Dependency of the global LF shape with large-scale environment
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
PERSPECTIVES
LF, LD and SFR by type and environment simultaneously
Extend the measurement of the LF and LD to a larger λ rangeFUV, NUV with GALEXNIR with J and K bands from VVDS
Use photometric redshifts trained on spectroscopic data to Improve the statistic Go deeper
Radio with VLA data
On-going acquisition of 100,000 spectra with VIMOS
LD evolution with a same sample from z=0.05 to z=4New expertise of the VVDS team in the redshift desert (1.5-3)
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
LF TOOL : ABSOLUTE MAGNITUDE
Fit the best template on BVRI multi-color data
Derived the k-correction with the template SED
We used the flux in the observer frame
Limits the template dependency
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
COMPARISON WITH THE CFRS
Canada-France Redshift Survey (CFRS) : 591 secured redshift Iab<22.5Luminosity function and luminosity density from Lilly et al. 1995
Agreement
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
SHAPE OF THE LF PER TYPE
Fit the best template on BVRI multi-color data => photometric type
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
SHAPE OF THE LF PER TYPE
Steepening of the slope from
reddestto
bluest photometric types
Fit the best template on BVRI multi-color data => photometric type
![Page 25: VVDS FIRST EPOCH RESULTSmoriond.in2p3.fr/J04/trans/ilbert.pdf · VVDS FIRST EPOCH RESULTS O. Le Fèvre, G. Vettolani and the VVDS team. Olivier Ilbert (LAM-OAMP) Moriond – March](https://reader031.vdocuments.mx/reader031/viewer/2022041117/5f2b4d3c76b81a35ec5069d8/html5/thumbnails/25.jpg)
Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
SHAPE OF THE LF PER TYPE
Steepening of the slope from
reddestto
bluest photometric types
Fit the best template on BVRI multi-color data => photometric type
![Page 26: VVDS FIRST EPOCH RESULTSmoriond.in2p3.fr/J04/trans/ilbert.pdf · VVDS FIRST EPOCH RESULTS O. Le Fèvre, G. Vettolani and the VVDS team. Olivier Ilbert (LAM-OAMP) Moriond – March](https://reader031.vdocuments.mx/reader031/viewer/2022041117/5f2b4d3c76b81a35ec5069d8/html5/thumbnails/26.jpg)
Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
SHAPE OF THE LF PER TYPE
Steepening of the slope from
reddestto
bluest photometric types
Fit the best template on BVRI multi-color data => photometric type
![Page 27: VVDS FIRST EPOCH RESULTSmoriond.in2p3.fr/J04/trans/ilbert.pdf · VVDS FIRST EPOCH RESULTS O. Le Fèvre, G. Vettolani and the VVDS team. Olivier Ilbert (LAM-OAMP) Moriond – March](https://reader031.vdocuments.mx/reader031/viewer/2022041117/5f2b4d3c76b81a35ec5069d8/html5/thumbnails/27.jpg)
Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004
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Olivier Ilbert(LAM-OAMP) 1Moriond – March 2004