the relation between the galaxy stellar mass distribution and the mass

The relation between the galaxy stellar mass

distribution and the mass of its hosting halo

BENEDETTA VULCANIKAVLI IPMU

What Regulates Galaxy Evolution? - 2013, April 22th-26th

In collaboration withBianca PoggiantiGabriella De LuciaAlan DresslerKevin Bundy

THE ENVIRONMENTThe properties of galaxies correlate with the environment: Morphology density relation (Dressler 1980, Dressler+ 1997) Denser environments host more massive, redder galaxies with lower

star-formation rates (Kauffmann+ 2004) Galaxies in different environments evolve with different timescales

..But various galaxy properties are strongly correlated even in a fixed environment.. What Regulates Galaxy Evolution? - 2013, April 22th-26th

How are the mass and environment related?


The field mass function(e.g. Fontana+ 2006, Bundy+ 2006, Franceschini+ 2006, Borch+ 2006, Vergani+ 2008, Drory+09, Pozzetti+ 2011)

For high mass galaxies, the evolution of the total mass function from z = 1 to z = 0 is relatively modestLow mass galaxies evolve more than high mass galaxies

Ilbert+ 2010


Several studies have analyzed separately galaxies of different types (colors, star formation activity, structural parameters, morphologies)

Vergani+ 2008

Pannella+ 2006

Borch+ 2006


AND IN CLUSTERS?


ESO Distant Cluster Survey (EDisCS - White+ 2005): Optically selected clusters (σ>400 km/s) and groups (150<σ<400 km/s) at 0.4<z<0.8 Deep optical photometry in B,V,I or V,R,IDeep spectroscopyWide-field imaging

Stellar masses from the relation between LB and B-V color (Bell & De Jong 2001)

WIde field Nearby Galaxy-cluster Survey (WINGS - Fasano+ 06): X rays selected cluster (σ>500 km/s) at 0.04<z<0.07 U,B,V and J,K photometrySpectroscopy

The cluster mass function

Vulcani et al. (2011)

Evolution driven by the mass growth of star forming galaxies in both clusters and in the cluster surrounding areas.

+ MORPHOLOGICAL TRANSFORMATION

z=0.6

z=0.07


IMACS Cluster Building Survey (ICBS - Oemler+ 2013):Cluster selected using the Red Sequence Cluster Survey method (Gladders and Yee 2000) at 0.25<z<0.5IMACS wide fieldBroad band photometry in B,V,R,I or g,r,i,z Spectroscopic data of clusters, groups and field

The shape of the MF does not depend on global environmentVulcani et al. (2013)

The MF in different environments

field

clusters

clustersgroups


The red/blue MF

Red and blue MF are different, but no differences detected in MF in different environments, for red and blue galaxies separately

Vulcani et al. (2013)


Padova Millennium Galaxy Group Catalog (PM2GC – Calvi, Poggianti, BV 2011):

Spectroscopic data of ~38deg2 at 0.04<z<0.1 from the Millennium Galaxy Catalog (Lieske+2003)

Deep and wide B-imaging

Rich sample of groups, binary systems and isolated galaxies

The MF in different environmentsLow-z

Calvi, Poggianti, BV, Fasano (2013)What Regulates Galaxy Evolution? - 2013, April 22th-26th

The evolution

INDEPENDENT OF ENVIRONMENT!Vulcani et al. (2013)What Regulates Galaxy Evolution? - 2013, April 22th-26th

Help from the simulations

What Regulates Galaxy Evolution? - 2013, April 22th-26th BV, De Lucia, Poggianti in prep.


The predicted evolution

BV, De Lucia, Poggianti in prep.


The dependence on halo mass

BV, De Lucia, Poggianti in prep.

MY QUESTIONS1 Why doesn’t the global envirnoment

affect galaxy masses?2 What is the role of the environment at

lower masses?3 Why do simulations overpredict the

number of low mass galaxies?


SUMMARY Both at high and low -z, the total mass function does

not depend on environment. At high-z, red and blue MF are different, but no

differences are detected in MF in different environments, for red and blue galaxies separately.

The evolution of the mass function is very similar in all the environments.

Semianalytic models can reproduce only the observed field mass function at low-z. As a consequence, they do not reproduce neither the observed evolution nor the independence of the mass function on the environment.


the relation between the galaxy stellar mass distribution and the mass

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