Comparison of the linear bias models in the light of the Dark Energy Survey

Papageorgiou, A.; Basilakos, Spyros; Plionis, M.

doi:10.1093/mnras/sty396

Cited by 2 publications

(2 citation statements)

References 62 publications

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“…The second result is that the differences of the bias models are absorbed in the fitted value of the DM halo mass in which LRGs live, and which ranges from ∼ 6.2 × 10 12 h −1 M ⊙ − 1.2 × 10 13 h −1 M ⊙ , for the different bias models and in the case of DESY1COSMO bias. As it can also be seen from Table II, our derived mass of the host DM halo mass is consistent with that of Papageorgiou et al [61], while Sawangwit et al [62] and Pouri et al [63] found M h ≃ (1.9 − 2) × 10 13 h −1 M ⊙ .…”

Section: Constant Growth Indexsupporting

confidence: 91%

Growth index of matter perturbations in the light of Dark Energy Survey

Basilakos

Anagnostopoulos

2020

Eur. Phys. J. C

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We study how the cosmological constraints from growth data are improved by including the measurements of bias from Dark Energy Survey (DES). In particular, we utilize the biasing properties of the DES Luminous Red Galaxies (LRGs) and the growth data provided by the various galaxy surveys in order to constrain the growth index (γ) of the linear matter perturbations. Considering a constant growth index we can put tight constraints, up to ∼ 10% accuracy, on γ. Specifically, using the priors of the Dark Energy Survey and implementing a joint likelihood procedure between theoretical expectations and data we find that the best fit value is in between γ = 0.64 ± 0.075 and 0.65 ± 0.063. On the other hand utilizing the Planck priors we obtain γ = 0.680 ± 0.089 and 0.690 ± 0.071. This shows a small but non-zero deviation from General Relativity (γGR ≈ 6/11), nevertheless the confidence level is in the range ∼ 1.3 − 2σ. Moreover, we find that the estimated mass of the dark-matter halo in which LRGs survive lies in the interval ∼ 6.2 × 10 12 h −1 M⊙ and 1.2 × 10 13 h −1 M⊙, for the different bias models. Finally, allowing γ to evolve with redshift [Taylor expansion: γ(z) = γ0 +γ1z/(1+z)] we find that the (γ0, γ1) parameter solution space accommodates the GR prediction at ∼ 1.7 − 2.9σ levels.PACS numbers: 98.80.Bp, 98.65.Dx, 95.35.+d, 95.36.+x * Electronic address: svasil@academyofathens.gr † Electronic address: fotis-anagnostopoulos@hotmail.com

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Section: Constant Growth Indexsupporting

confidence: 91%

Growth index of matter perturbations in the light of Dark Energy Survey

Basilakos

Anagnostopoulos

2020

Eur. Phys. J. C

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“…We have fitted two different bias evolution models to the data, the Basilakos et al (2008) and the Tinker et al (2010) models, using a χ 2 minimization procedure and we derive the DM host halo mass (details and comparisons of the different bias models can be found in Papageorgiou et al 2012Papageorgiou et al , 2018. We find log 10 M h /[h −1 M ] = 13.04 ± 0.06 and 12.98 ± 0.07 for the two models, respectively.…”

Section: Resultsmentioning

confidence: 99%

The XXL Survey

Plionis

Koutoulidis

Koulouridis

et al. 2018

A&A

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The XMM-XXL Survey spans two fields of 25 deg2 each observed for more than 6 Ms with XMM, which provided a sample of tens of thousands of point sources with a flux limit of ~2.2 × 10−15 and ~1.4 × 10−14 erg s−1 cm2, corresponding to 50% of the area curve, in the soft band (0.5–2 keV) and hard band (2–10 keV), respectively. In this paper we present the spatial clustering properties of ~3100 and ~1900 X-ray active galactic nuclei (AGNs) in the soft and hard bands, respectively, which have been spectroscopically observed with the AAOmega facility. This sample is 90% redshift complete down to an optical magnitude limit of r ≲ 21.8. The sources span the redshift interval 0 < z < 5.2, although in the current analysis we limit our samples to z ≤ 3, with corresponding sample median values of z̅ ≃ 0.96 and 0.79 for the soft band and hard band, respectively. We employ the projected two-point correlation function to infer the spatial clustering and find a correlation length r0 = 7.0(±0.34) and 6.42(±0.42) h−1 Mpc, respectively, for the soft- and hard-band detected sources with a slope for both cases of γ = 1.44(±0.1). The power-law clustering was detected within comoving separations of 1 and ~25 h−1 Mpc. These results, as well as those derived in two separate redshift ranges, provide bias factors of the corresponding AGN host dark matter halos that are consistent with a halo mass of log10[Mh∕(h−1M⊙)] = 13.04 ± 0.06, confirming the results of most recent studies based on smaller X-ray AGN samples.

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Comparison of the linear bias models in the light of the Dark Energy Survey

Cited by 2 publications

References 62 publications

Growth index of matter perturbations in the light of Dark Energy Survey

Growth index of matter perturbations in the light of Dark Energy Survey

The XXL Survey

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