dynamics at high redshifts:

Dynamics at high redshifts:

the case of a cluster at z=1.47

Sandro Bardelli - INAF Osservatorio Astronomico di Bologna

Christian Marinoni - LAM Marseille

Angela Iovino - INAF Osservatorio Astronomico di Brera

M.Scodeggio, O.Cucciati, O.Ilbert, M.Bolzonella, E.Zucca, C. Adami,A. Zanichelli, L. Guzzo, L.Tresse, G.Zamorani, S.Arnouts, A.Cappi,

L.Pozzetti, D.Bottini, B.Garilli, V.LeBrun, O.LeFevre, D.Maccagni, J.P.Picat, R.Scaramella, G.Vettolani, M.Arnaboldi, S.Charlot, P.Ciliegi, T.Contini,

S.Foucaud, P.Franzetti, I.Gavignaud, H.J.McCracken, B.Marano, A.Mazure, B.Meneux, R.Merighi, S.Paltani, R.Pello`, A.Pollo, M.Radovich, M.Bondi,

A.Bongiorno, G.Busarello, S.Temporin, D.Vergani,L.Gregorini, F.Lamareille, G.Mathez, Y.Mellier, P.Merluzzi,V.Ripepi, D.Rizzo

Fi

Figure 1

z=1.4

z=1.5 Figure 2

Figure 3

The cluster atz=1.47

Figure 4

Spectroscopicredshift histogramin the cluster region

The deep F02 field of the VIMOS VLT Deep Survey (VVDS, PI Le Fevre) gives a unique possibility to study in depth (up to z~1.5) the large scale structure of the Universe (Figure1). This survey collected redshifts of galaxies to IAB<24 in an area of 0.4 x 0.4 deg2 . Moreover deep photometry is available in the UBVRIJK bands.

Using the Voronoi Delaunay technique (Marinoni et al. 2002) on thespectroscopic sample, we detected a significant system of galaxiesat z=1.47 (Figure 2). All spectra present features that assure good redshift determination (Figure 3). This structure has been detected because of thepresence of 9 galaxies in a 7x7 arcmin region (correspondingto 3.5x3.5 Mpc).

If we consider a wider region of 13x13 arcmin (6.5x6.5 Mpc),the number of concordant redshifts increases: in Figure 4 we show theredshifts histogram with the solid line representing the smoothed totalredshifts distribution of the VVDS.

No X ray emission has been found in a unfavourable XMM archive observation.

The UBVRIJK coverage of the F02 field permits to compute high quality photometric redshifts. In this figure (left) we performed an adaptive kernel filtering of the whole F02 area, by selecting objects with photometric redshift in the range [1.4 - 1.6]. Black points corresponds to galaxies with spectroscopic redshifts in the range [1.46 - 1.48], while red points correspond to a subclump of 5 very red galaxies. The structure has a dimension of about 8x6 Mpc.

Figure 5

Figure 7Figure 6

Figure 6

Figure 7

In Figure 7 we show the color - color relation of the galaxies in the cluster region. Symbols are the same as in Figure 6, while the red lines correspond to the expected colors of a z=1.47 elliptical.

This structure lack of a definite color - magnitude relation.In Figure 6 we show the (I - J) - I color magnitude plot of galaxies in the cluster area. Triangles are galaxies with photometric redshiftwithin the range [1.3 - 1.8], blue triangles are the red galaxies shown inFigure 5. Note that at z=1.47, M* of elliptical galaxies has a magnitude ofIAB=25, while extreme blue galaxies have IAB=24.3 (Zucca et al, 2006) .The red band represents the expected position of the color - magnitude relation for red galaxies.

DISCUSSION: Cluster or Forming structure?

This structure appears as an overdensity both in the photometric and spectroscopic redshifts and is formed by three subclumps and resemble the much more massive cluster complexes in the Shapley Concentration(Bardelli et al. 1998).The velocity dispersion of the central clump is 775 + / - 312 km/s (based on 9 galaxies within a region of 7’x8’) and is one of the most distant cluster known(with those found by Mullis et al. 2005 and Stanford et al. 2005 both at z=1.4).This structure does not present evident color - magnituderelation, but this is not surprising because it was foundas a purely optical detection (see Donahue et al. 2002)

The VVDS CONE

3000 Mpc

VVDS 0226-04 VVDS 0226-04 “cone”“cone”

6217 galaxies with secure redshifts, IAB24

Coverage on 30x30 arcmin² so far

Current volume sampled: 3x106 Mpc3

=1/16th of final goal

3000 Mpc