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Title: H-ATLAS/GAMA: magnification bias tomography. Astrophysical constraints above ∼1 arcmin

Abstract

An unambiguous manifestation of the magnification bias is the cross-correlation between two source samples with non-overlapping redshift distributions. In this work we measure and study the cross-correlation signal between a foreground sample of GAMA galaxies with spectroscopic redshifts in the range 0.2< z <0.8, and a background sample of H-ATLAS galaxies with photometric redshifts ∼>1.2. It constitutes a substantial improvement over the cross-correlation measurements made by Gonzalez-Nuevo et al. (2014) with updated catalogues and wider area (with S / N ∼> 5 below 10 arcmin and reaching S / N ∼ 20 below 30 arcsec). The better statistics allow us to split the sample in different redshift bins and to perform a tomographic analysis (with S / N ∼> 3 below 10 arcmin and reaching S / N ∼ 15 below 30 arcsec). Moreover, we implement a halo model to extract astrophysical information about the background galaxies and the deflectors that are producing the lensing link between the foreground (lenses) and background (sources) samples. In the case of the sources, we find typical mass values in agreement with previous studies: a minimum halo mass to host a central galaxy, M {sub min}∼ 10{sup 12.26} M {sub ⊙}, and a pivotmore » halo mass to have at least one sub-halo satellite, M {sub 1∼} 10{sup 12.84} M {sub ⊙}. However, the lenses are massive galaxies or even galaxy groups/clusters, with minimum mass of M {sub min}{sup lens}∼ 10{sup 13.06} M {sub ⊙}. Above a mass of M {sub 1}{sup lens}∼ 10{sup 14.57} M {sub ⊙} they contain at least one additional satellite galaxy which contributes to the lensing effect. The tomographic analysis shows that, while M {sub 1}{sup lens} is almost redshift independent, there is a clear evolution of increase M {sub min}{sup lens} with redshift in agreement with theoretical estimations. Finally, the halo modeling allows us to identify a strong lensing contribution to the cross-correlation for angular scales below 30 arcsec. This interpretation is supported by the results of basic but effective simulations.« less

Authors:
;  [1]; ;  [2];  [3]; ; ; ; ; ;  [4];  [5];  [6]; ;  [7];  [8];  [9]
  1. Departamento de Física, Universidad de Oviedo, C. Federico García Lorca 18, E-33007 Oviedo (Spain)
  2. SISSA, Via Bonomea 265, I-34136 Trieste (Italy)
  3. INAF, Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, I-35122 Padova (Italy)
  4. School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA (United Kingdom)
  5. Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ (United Kingdom)
  6. Department of Physics and Astronomy, University of California, Irvine, CA, 92697 (United States)
  7. School of Physics and Astronomy, Nottingham University, University Park, Nottingham, NG7 2RD (United Kingdom)
  8. European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching (Germany)
  9. Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH (United Kingdom)
Publication Date:
OSTI Identifier:
22667642
Resource Type:
Journal Article
Resource Relation:
Journal Name: Journal of Cosmology and Astroparticle Physics; Journal Volume: 2017; Journal Issue: 10; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; CORRELATIONS; DISTRIBUTION; EVOLUTION; GALAXIES; GRAVITATIONAL LENSES; MASS; RED SHIFT; SATELLITES; SIMULATION; STATISTICS

Citation Formats

González-Nuevo, J., Bonavera, L., Lapi, A., Danese, L., De Zotti, G., Negrello, M., Dunne, L., Eales, S., Maddox, S., Smith, M.W.L., Valiante, E., Bourne, N., Cooray, A., Dye, S., Furlanetto, C., Ivison, R.J., and Loveday, J., E-mail: gnuevo@uniovi.es. H-ATLAS/GAMA: magnification bias tomography. Astrophysical constraints above ∼1 arcmin. United States: N. p., 2017. Web. doi:10.1088/1475-7516/2017/10/024.
González-Nuevo, J., Bonavera, L., Lapi, A., Danese, L., De Zotti, G., Negrello, M., Dunne, L., Eales, S., Maddox, S., Smith, M.W.L., Valiante, E., Bourne, N., Cooray, A., Dye, S., Furlanetto, C., Ivison, R.J., & Loveday, J., E-mail: gnuevo@uniovi.es. H-ATLAS/GAMA: magnification bias tomography. Astrophysical constraints above ∼1 arcmin. United States. doi:10.1088/1475-7516/2017/10/024.
González-Nuevo, J., Bonavera, L., Lapi, A., Danese, L., De Zotti, G., Negrello, M., Dunne, L., Eales, S., Maddox, S., Smith, M.W.L., Valiante, E., Bourne, N., Cooray, A., Dye, S., Furlanetto, C., Ivison, R.J., and Loveday, J., E-mail: gnuevo@uniovi.es. Sun . "H-ATLAS/GAMA: magnification bias tomography. Astrophysical constraints above ∼1 arcmin". United States. doi:10.1088/1475-7516/2017/10/024.
@article{osti_22667642,
title = {H-ATLAS/GAMA: magnification bias tomography. Astrophysical constraints above ∼1 arcmin},
author = {González-Nuevo, J. and Bonavera, L. and Lapi, A. and Danese, L. and De Zotti, G. and Negrello, M. and Dunne, L. and Eales, S. and Maddox, S. and Smith, M.W.L. and Valiante, E. and Bourne, N. and Cooray, A. and Dye, S. and Furlanetto, C. and Ivison, R.J. and Loveday, J., E-mail: gnuevo@uniovi.es},
abstractNote = {An unambiguous manifestation of the magnification bias is the cross-correlation between two source samples with non-overlapping redshift distributions. In this work we measure and study the cross-correlation signal between a foreground sample of GAMA galaxies with spectroscopic redshifts in the range 0.2< z <0.8, and a background sample of H-ATLAS galaxies with photometric redshifts ∼>1.2. It constitutes a substantial improvement over the cross-correlation measurements made by Gonzalez-Nuevo et al. (2014) with updated catalogues and wider area (with S / N ∼> 5 below 10 arcmin and reaching S / N ∼ 20 below 30 arcsec). The better statistics allow us to split the sample in different redshift bins and to perform a tomographic analysis (with S / N ∼> 3 below 10 arcmin and reaching S / N ∼ 15 below 30 arcsec). Moreover, we implement a halo model to extract astrophysical information about the background galaxies and the deflectors that are producing the lensing link between the foreground (lenses) and background (sources) samples. In the case of the sources, we find typical mass values in agreement with previous studies: a minimum halo mass to host a central galaxy, M {sub min}∼ 10{sup 12.26} M {sub ⊙}, and a pivot halo mass to have at least one sub-halo satellite, M {sub 1∼} 10{sup 12.84} M {sub ⊙}. However, the lenses are massive galaxies or even galaxy groups/clusters, with minimum mass of M {sub min}{sup lens}∼ 10{sup 13.06} M {sub ⊙}. Above a mass of M {sub 1}{sup lens}∼ 10{sup 14.57} M {sub ⊙} they contain at least one additional satellite galaxy which contributes to the lensing effect. The tomographic analysis shows that, while M {sub 1}{sup lens} is almost redshift independent, there is a clear evolution of increase M {sub min}{sup lens} with redshift in agreement with theoretical estimations. Finally, the halo modeling allows us to identify a strong lensing contribution to the cross-correlation for angular scales below 30 arcsec. This interpretation is supported by the results of basic but effective simulations.},
doi = {10.1088/1475-7516/2017/10/024},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 10,
volume = 2017,
place = {United States},
year = {Sun Oct 01 00:00:00 EDT 2017},
month = {Sun Oct 01 00:00:00 EDT 2017}
}