Gilli, R. and Daddi, E. and Chary, R. and Dickinson, M. and Elbaz, D. and Giavalisco, M. and Kitzbichler, M. and Stern, D. and Vanzella, E. (2007) The spatial clustering of mid-IR selected star forming galaxies at z ∼1 in the GOODS fields. Astronomy and Astrophysics, 475 (1). pp. 83-99. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20100426-104402959
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We present the first spatial clustering measurements of z ~ 1, 24 μm-selected, star forming galaxies in the Great Observatories Origins Deep Survey (GOODS). The sample under investigation includes 495 objects in GOODS-South and 811 objects in GOODS-North selected down to flux densities of f_(24) > 20 μJy and z_(AB) < 23.5 mag, for which spectroscopic redshifts are available. The median redshift, IR luminosity and star formation rate (SFR) of the sample are z ~ 0.8, L_(IR) ~ 4.4 × 10^(10) L_☉, and SFR ~ 7.6 M_☉ yr^(−1), respectively. We measure the projected correlation function w(r_p) on scales of r_p = 0.06−10 h^(−1) Mpc, from which we derive a best fit comoving correlation length of r_0 = 4.0 ± 0.4 h^(−1) Mpc and slope of γ = 1.5 ± 0.1 for the whole f_(24) > 20 μJy sample after combining the two fields. We find indications of a larger correlation length for objects of higher luminosity, with Luminous Infrared Galaxies (LIRGs, L_(IR) > 10^(11) L_☉) reaching r_0 ~ 5.1 h^(−1) Mpc. This would imply that galaxies with larger SFRs are hosted in progressively more massive halos, reaching minimum halo masses of ~3 × 10^(12) M_☉ for LIRGs.We compare our measurements with the predictions from semi-analytic models based on the Millennium simulation. The variance in the models is used to estimate the errors in our GOODS clustering measurements, which are dominated by cosmic variance. The measurements from the two GOODS fields are found to be consistent within the errors. On scales of the GOODS fields, the real sources appear more strongly clustered than objects in the Millennium-simulation based catalogs, if the selection function is applied consistently. This suggests that star formation at z ~ 0.5−1 is being hosted in more massive halos and denser environments than currently predicted by galaxy formation models. Mid-IR selected sources appear also to be more strongly clustered than optically selected ones at similar redshifts in deep surveys like the DEEP2 Galaxy Redshift Survey and the VIMOS-VLT Deep Survey (VVDS), although the significance of this result is ≲3σ when accounting for cosmic variance. We find that LIRGs at z ~ 1 are consistent with being the direct descendants of Lyman Break Galaxies and UV-selected galaxies at z ~ 2−3, both in term of number densities and clustering properties, which would suggest long lasting star-formation activity in galaxies over cosmological timescales. The local descendants of z ~ 0.5−1 star forming galaxies are not luminous IR galaxies but are more likely to be normal, L < L_∗ ellipticals and bright spirals.
|Additional Information:||© 2007 ESO. Received 19 March 2007; accepted 27 July 2007. We wish to thank the referee for comments which improved the paper significantly. We acknowledge G. Zamorani, L. Pozzetti, F. Pozzi, C. Gruppioni, L. Moscardini, E. Branchini and M. Magliocchetti for useful discussions. We are also grateful to E. MacDonald and H. Spinrad for their extensive efforts obtaining some of the redshift measurements used in this work. R.G. acknowledges financial support from the Italian Space Agency (under the contract ASI-INAF I/023/05/0) and from the grant PRIN-MUR 2006-02-5203. The work of D.S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.|
|Subject Keywords:||galaxies: evolution; cosmology: large-scale structure of Universe; cosmology: observations|
|Official Citation:||The spatial clustering of mid-IR selected star forming galaxies at z ~ 1 in the GOODS fields R. Gilli, E. Daddi, R. Chary, M. Dickinson, D. Elbaz, M. Giavalisco, M. Kitzbichler, D. Stern and E. Vanzella A&A 475 (1) 83-99 (2007) DOI: 10.1051/0004-6361:20077506|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||26 Apr 2010 21:37|
|Last Modified:||26 Dec 2012 11:59|
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