Cosmic anisotropy and fast radio bursts

Qiang, Da-Chun; Deng, Hua-Kai; Hao, Wei

doi:10.1088/1361-6382/ab7f8e

Cited by 20 publications

(20 citation statements)

References 210 publications

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“…Besides the SNe Ia sample, galaxy [18][19][20]54], galaxy cluster [51][52][53], number counts of radio and mid-IR sources [36][37][38][39][40][41][42][43][44][45][46][47][48][49][50], gamma-ray burst [13,66,108], gravitational wave [109], fast radio burst [109,110], and quasar [83,87] are also used to investigate the cosmic anisotropy. The UV and X-ray luminosity of quasars are used to test the cosmic anisotropy by Hu etc.…”

Section: Introductionmentioning

confidence: 99%

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

Zhao

Xia

2021

Eur. Phys. J. C

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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.

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Section: Introductionmentioning

confidence: 99%

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

Zhao

Xia

2021

Eur. Phys. J. C

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“…After that, Mariano and Perivolaropoulos (Mariano & Perivolaropoulos 2012) found a possible preferred anisotropic direction at the 2σ level using the Union2 sample, but by employing the dipole fitting (DF) method. Since then, these two methods have been widely used to explore the cosmic anisotropy (Cai & Tuo 2012;Cai et al 2013;Zhao et al 2013;Li et al 2013;Heneka et al 2014;Bengaly et al 2015;Andrade et al 2018;Sun & Wang 2019) by investigating observational data of, for instance, the Union2.1 sample (Yang et al 2014;Javanmardi et al 2015;Lin et al 2016a), the Joint Light-Curve Analysis (JLA) sample (Lin et al 2016b;Chang et al 2018a;, the Pantheon sample (Sun & Wang 2018), gamma-ray bursts (GRBs; Wang & Wang 2014), galaxies (Zhou et al 2017), as well as gravitational wave and fast radio bursts (Qiang et al 2019;Cai et al 2019). Using HC and DF methods, Zhao et al (2019) studied the cosmic anisotropy via the Pantheon sample.…”

Section: Introductionmentioning

confidence: 99%

Testing cosmic anisotropy with Pantheon sample and quasars at high redshifts

Wang

2020

A&A

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In this paper, we investigate the cosmic anisotropy from the SN-Q sample, consisting of the Pantheon sample and quasars, by employing the hemisphere comparison (HC) method and the dipole fitting (DF) method. Compared to the Pantheon sample, the new sample has a larger redshift range, a more homogeneous distribution, and a larger sample size. For the HC method, we find that the maximum anisotropy level is ALmax = 0.142 ± 0.026 in the direction (l, b) = (316.08°−129.48+27.41, 4.53°−64.06+26.29). The magnitude of anisotropy is A = (−8.46−5.51+4.34) × 10−4 and the corresponding preferred direction points toward (l, b) = (29.31°−30.54+30.59, 71.40°−9.72+9.79) for the quasar sample from the DF method. The combined SN and quasar sample is consistent with the isotropy hypothesis. The distribution of the dataset might impact the preferred direction from the dipole results. The result is weakly dependent on the redshift from the redshift tomography analysis. There is no evidence of cosmic anisotropy in the SN-Q sample. Though some results obtained from the quasar sample are not consistent with the standard cosmological model, we still do not find any distinct evidence of cosmic anisotropy in the SN-Q sample.

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“…Pagano & Fronenberg showed that the highly dispersed FRBs can be used to constraining the epoch of cosmic reionization [27]. Qiang et al showed that FRBs can be used test the possible cosmic anisotropy [28]. In addition, the strongly lensed FRBs can be used to probe the compact dark matter in the Universe [29].…”

Section: Introductionmentioning

confidence: 99%

Probing the anisotropic distribution of baryon matter in the Universe using fast radio bursts

Lin,

Sang

2021

Preprint

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We propose that fast radio bursts (FRBs) can be used as the probes to constrain the possible anisotropic distribution of baryon matter in the Universe. Monte Carlo simulations show that, 400 (800) FRBs are enough to detect the anisotropy at 95% (99%) confidence level, if the dipole amplitude is at the order of magnitude 0.01. However, much more FRBs are required to tightly constrain the dipole direction. Even 1000 FRBs are far from enough to constrain the dipole direction within angular uncertainty ∆θ < 40 • at 95% confidence level. The uncertainty on the dispersion measure of host galaxy does not significantly affect the results. If the dipole amplitude is in the level of 0.001, however, 1000 FRBs are not enough to correctly detect the anisotropic signal.

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Cosmic anisotropy and fast radio bursts

Cited by 20 publications

References 210 publications

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

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

Testing cosmic anisotropy with Pantheon sample and quasars at high redshifts

Probing the anisotropic distribution of baryon matter in the Universe using fast radio bursts

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