• DOI:10.1051/0004-6361/201321476
• Corpus ID: 54812737

The VIMOS Public Extragalactic Redshift Survey (VIPERS) ⋆ Luminosity and stellar mass dependence of galaxy clustering at 0.5< z< 1.1

@article{Marulli2013TheVP,
  title={The VIMOS Public Extragalactic Redshift Survey (VIPERS) ⋆ Luminosity and stellar mass dependence of galaxy clustering at 0.5< z< 1.1},
  author={Federico Marulli and Micol Bolzonella and Enzo Branchini and Iary Davidzon and Sylvain de la Torre and Benjamin R. Granett and Luigi Guzzo and Angela Iovino and Lauro Moscardini and Agnieszka Pollo and Ummi Abbas and Christophe Adami and St{\'e}phane Arnouts and Julien Bel and Dario Bottini and Alberto Cappi and Jean Coupon and Olga Cucciati and Gabriella De Lucia and Alexander Fritz and Paolo Franzetti and Marco Fumana and Bianca Garilli and Olivier Ilbert and Janusz Krywult and Vincent Le Brun and Olivier Le F{\`e}vre and Dario Maccagni and Katarzyna Małek and Henry Joy McCracken and Luigi Paioro and Maria del Carmen Polletta and H. Schlagenhaufer and Marco Scodeggio and L. A. M. Tasca and Rita Tojeiro and Daniela Vergani and Alessandro Zanichelli and Angela Burden and C. D. N. Porto and Alessandro Marchetti and Christian Marinoni and Yannick Mellier and Robert C. Nichol and John A Peacock and Will J. Percival and Stefanie Phleps and Melody Wolk and Giovanni Zamorani},
  journal={Astronomy and Astrophysics},
  year={2013},
  volume={557},
  pages={1-15}
}

• F. Marulli, M. Bolzonella, +46 authors G. Zamorani
• Published 11 March 2013
• Physics
• Astronomy and Astrophysics

Aims. We investigate the dependence of galaxy clustering on luminosity and stellar mass in the redshift range 0.5 < z < 1.1, using the first ~ 55 000 redshifts from the VIMOS Public Extragalactic Redshift Survey (VIPERS). Methods. We measured the redshift-space two-point correlation functions (2PCF), ξ(s) and ξ(rp,π) , and the projected correlation function, wp(rp), in samples covering different ranges of B-band absolute magnitudes and stellar masses. We considered both threshold and binned galaxy samples, with median B-band absolute magnitudes − 21.6 ≲ MB − 5log (h) ≲ − 19.5 and median stellar masses 9.8 ≲ log (M⋆ [h-2 M⊙]) ≲ 10.7. We assessed the real-space clustering in the data from the projected correlation function, which we model as a power law in the range 0.2 < rp [h-1 Mpc ] < 20. Finally, we estimated the galaxy bias as a function of luminosity, stellar mass, and redshift, assuming a flat Λ cold dark matter model to derive the dark matter 2PCF. Results. We provide the best-fit parameters of the power-law model assumed for the real-space 2PCF – the correlation length, r0, and the slope, γ – as well as the linear bias parameter, as a function of the B-band absolute magnitude, stellar mass, and redshift. We confirm and provide the tightest constraints on the dependence of clustering on luminosity at 0.5 < z < 1.1. We prove the complexity of comparing the clustering dependence on stellar mass from samples that are originally flux-limited and discuss the possible origin of the observed discrepancies. Overall, our measurements provide stronger constraints on galaxy formation models, which are now required to match, in addition to local observations, the clustering evolution measured by VIPERS galaxies between z = 0.5 and z = 1.1 for a broad range of luminosities and stellar masses.