A tomographic test of cosmic anisotropy with the recently-released quasar sample

Abstract

We test the cosmic anisotropy in the dipole-modulated $$\Lambda $$ Λ CDM model and Finslerian cosmological model with the recently-released quasar sample. Based on the redshift tomographic method, the quasar sample is divided into two subsets $$z \le z_{cut}$$ z ≤ z cut and $$z > z_{cut}$$ z > z cut by different cutting redshifts. The dipole amplitudes of the two cosmological models from the subsets $$z \le z_{cut}$$ z ≤ z cut are very weak. We find that quasars at a higher redshift range may provide more detailed information about the dipole amplitude $$A_D$$ A D . The dipole directions of each cosmological model from the subsets $$z \le 1.1$$ z ≤ 1.1 and $$z > 1.1$$ z > 1.1 are deviated by $$1\sigma $$ 1 σ level. The Pantheon sample is combined with the two subsets. The dipole amplitude from the two combined datasets is also very weak. In the dipole-modulated $$\Lambda $$ Λ CDM model, the dipole direction from the combined dataset quasar at $$z \le 1.1$$ z ≤ 1.1 and Pantheon sample is far away from the one given by the Pantheon sample. In the Finslerian cosmological model, the dipole directions from the two combined datasets are close to the one in the Pantheon sample.

Large‐scale asymmetry in galaxy spin directions: Analysis of galaxies with spectra in DES, SDSS, and DESI Legacy Survey

“…The preparation of that dataset is described in detail in Shamir (2020d). The galaxies from the DESI Legacy Survey are the subset of galaxies used by Shamir (2021b) that had spectroscopic redshift through the catalog of Zhou et al (2021). The entire DESI Legacy Survey dataset contained 807,898 galaxies (Shamir 2021b), but only 23,715 of these galaxies had spectroscopic redshift through the catalog of Zhou et al (2021).…”

“…Perhaps the most notable and thoroughly studied probe showing evidence of cosmological‐scale anisotropy and a cosmological‐scale axis is the cosmic microwave background (Abramo et al 2006; Ade et al 2014; Campanelli et al 2007; Cline et al 2003; Dong et al 2015; Eriksen et al 2004; Gordon & Hu 2004; Gruppuso et al 2018; Land & Magueijo 2005; Mariano & Perivolaropoulos 2013; Santos et al 2015; Yeung & Chu 2022; Zhe et al 2015). Other messengers that show cosmological anisotropy and possible axes in the large‐scale structure include radio sources (Ghosh et al 2016; Tiwari & Jain 2015; Tiwari & Nusser 2016), LX‐T scaling (Migkas et al 2020), short gamma ray bursts (Mészáros 2019), cosmological acceleration rates (Krishnan et al 2021; Migkas et al 2021; Perivolaropoulos 2014), galaxy morphology types (Javanmardi & Kroupa 2017), Ia supernova (Javanmardi et al 2015; Lin et al 2016), dark energy (Adhav 2011; Adhav et al 2011; Colin et al 2019; Perivolaropoulos 2014), fine structure constant (Webb et al 2011), galaxy motion (Skeivalas et al 2021), (Luongo et al 2021), polarization of quasars (Hutsemékers et al 2005; Secrest et al 2021; Semenaite et al 2021; Zhao & Xia 2021), and high‐energy cosmic rays (Aab et al 2017).…”

Asymmetry in Galaxy Spin Directions -- Analysis of Data from DES and Comparison to Four Other Sky Surveys

“…Other observations include probes that show cosmological-scale anisotropy or other anomalies [6]. Such probes include the cosmic microwave background [7][8][9][10][11][12][13][14][15][16][17][18][19][20][21][22][23][24], radio sources [25][26][27][28][29][30], short gamma ray bursts [31], LX-T scaling [32], cosmological acceleration rates [33][34][35], Ia supernova [36,37], galaxy morphology types [38], dark energy [33,[39][40][41], fine structure constant [42], galaxy motion [43], H o [44], polarization of quasars [45][46][47][48][49], and cosmic rays [50][51][52][53][54]...…”

Large-scale asymmetry in galaxy spin directions -- analysis of galaxies with spectra in DES, SDSS, and DESI Legacy Survey

“…Perhaps the most notable and thoroughly studied probe showing evidence of cosmological-scale anisotropy and a cosmological-scale axis is the cosmic microwave background (Eriksen et al, 2004;Cline et al, 2003;Gordon and Hu, 2004;Campanelli et al, 2007;Zhe et al, 2015;Abramo et al, 2006;Mariano and Perivolaropoulos, 2013;Land and Magueijo, 2005;Ade et al, 2014;Santos et al, 2015;Dong et al, 2015;Gruppuso et al, 2018;Yeung and Chu, 2022). Other messengers that show cosmological anisotropy and possible axes in the large-scale structure include radio sources (Ghosh et al, 2016;Tiwari and Jain, 2015;Tiwari and Nusser, 2016), LX-T scaling (Migkas et al, 2020), short gamma ray bursts (Mészáros, 2019), cosmological acceleration rates (Perivolaropoulos, 2014;Migkas et al, 2021;Krishnan et al, 2021), galaxy morphol-ogy types (Javanmardi and Kroupa, 2017), Ia supernova (Javanmardi et al, 2015;Lin et al, 2016), dark energy (Adhav et al, 2011;Adhav, 2011;Perivolaropoulos, 2014;Colin et al, 2019), fine structure constant (Webb et al, 2011), galaxy motion (Skeivalas et al, 2021), H o (Luongo et al, 2021), polarization of quasars (Hutsemékers et al, 2005;Secrest et al, 2021;Zhao and Xia, 2021;Semenaite et al, 2021), and high-energy cosmic rays…”