Debiasing cosmic gravitational wave sirens

ABSTRACT Accurate estimation of the Hubble constant, and other cosmological parameters, from distances measured by cosmic gravitational wave sirens requires sufficient allowance for the dark energy evolution. We demonstrate how model-independent statistical methods, specifically Gaussian process regression, can remove bias in the reconstruction of H(z), and can be combined to model independently with supernova distances. This allows stringent tests of both H0 and Λ cold dark matter, and can detect unrecognized systematics. We also quantify the redshift systematic control necessary for the use of dark sirens, showing that it must approach spectroscopic precision to avoid significant bias.

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Cosmological parameter analyses using transversal BAO data

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2036 ◽

2020 ◽

Vol 497 (2) ◽

pp. 2133-2141 ◽

Cited By ~ 1

Author(s):

Rafael C Nunes ◽

Santosh K Yadav ◽

J F Jesus ◽

Armando Bernui

Keyword(s):

Cold Dark Matter ◽

Cosmological Parameters ◽

Mass Scale ◽

Joint Analysis ◽

Observational Constraints ◽

Independent Analysis ◽

Local Measurements ◽

Model Independent ◽

Free Parameters ◽

Dynamical Dark Energy

ABSTRACT We investigate observational constraints on cosmological parameters combining 15 measurements of the transversal BAO scale (obtained free of any fiducial cosmology) with Planck–CMB data to explore the parametric space of some cosmological models. We investigate how much Planck + transversal BAO data can constraint the minimum Lambda cold dark matter (ΛCDM) model, and extensions, including neutrinos mass scale Mν, and the possibility for a dynamical dark energy (DE) scenario. Assuming the ΛCDM cosmology, we find H0 = 69.23 ± 0.50 km s−1 Mpc−1, Mν < 0.11 eV, and rdrag = 147.59 ± 0.26 Mpc (the sound horizon at drag epoch) from Planck + transversal BAO data. When assuming a dynamical DE cosmology, we find that the inclusion of the BAO data can indeed break the degeneracy of the DE free parameters, improving the constraints on the full parameter space significantly. We note that the model is compatible with local measurements of H0 and there is no tension on H0 estimates in this dynamical DE context. Also, we discuss constraints and consequences from a joint analysis with the local H0 measurement from SH0ES. Finally, we perform a model-independent analysis for the deceleration parameter, q(z), using only information from transversal BAO data.

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On Dark Gravitational Wave Standard Sirens as Cosmological Inference and Forecasting the Constraint on Hubble Constant using Binary Black Holes Detected by Deci-Hertz Observator

Research in Astronomy and Astrophysics ◽

10.1088/1674-4527/ac3992 ◽

2021 ◽

Author(s):

Ju Chen ◽

Changshuo Yan ◽

Youjun Lu ◽

Yuetong Zhao ◽

Junqiang Ge

Keyword(s):

Black Holes ◽

Gravitational Wave ◽

Signal To Noise Ratio ◽

Cosmological Parameters ◽

Hubble Constant ◽

Luminosity Distance ◽

Host Galaxies ◽

Binary Black Holes ◽

Merger Rate ◽

Electromagnetic Signals

Abstract Gravitational wave (GW) signals from compact binary coalescences can be used as standard sirens to constrain cosmological parameters if its redshift can be measured independently by electromagnetic signals. However, mergers of stellar binary black holes (BBHs) may not have electromagnetic counterparts and thus have no direct redshift measurements. These dark sirens may be still used to statistically constrain cosmological parameters by combining their GW measured luminosity distances and localization with deep redshift surveys of galaxies around it. We investigate this dark siren method to constrain cosmological parameters in details by using mock BBH and galaxy samples. We find that the Hubble constant can be well constrained with an accuracy $\lesssim 1\%$ with a few tens or more BBH mergers at redshift up to $1$ if GW observations can provide accurate estimates of its luminosity distance (with relative error of $\lesssim 0.01$) and localization ($\lesssim 0.1\mathrm{deg}^2$), though the constraint may be significantly biased if the luminosity distance and localization errors are larger. We further generate mock BBH samples, according to current constraints on BBH merger rate and the distributions of BBH properties, and find that Deci-Hertz Observatory (DO) in a half year observation period may detect about one hundred BBHs with signal-to-noise ratio $\varrho \gtrsim 30$, relative luminosity distance error $\lesssim 0.02$, and localization error $\lesssim 0.01\mathrm{deg}^2$. By applying the dark standard siren method, we find that the Hubble constant can be constrained to $\sim 0.1-1\%$ level using these DO BBHs, an accuracy comparable to the constraints obtained by using electromagnetic observations in the near future, thus it may provide insight into the Hubble tension. We also demonstrate that the constraint on the Hubble constant using this dark siren method are robust and do not depend on the choice of the prior for the properties of BBH host galaxies.

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H0LiCOW – XIII. A 2.4 per cent measurement of H0 from lensed quasars: 5.3σ tension between early- and late-Universe probes

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz3094 ◽

2019 ◽

Vol 498 (1) ◽

pp. 1420-1439 ◽

Cited By ~ 64

Author(s):

Kenneth C Wong ◽

Sherry H Suyu ◽

Geoff C-F Chen ◽

Cristian E Rusu ◽

Martin Millon ◽

...

Keyword(s):

Time Delay ◽

Cold Dark Matter ◽

Cosmological Parameters ◽

Hubble Constant ◽

Joint Analysis ◽

Type Ia Supernovae ◽

Acoustic Oscillations ◽

Type Ia ◽

Measured Time ◽

Ia Supernovae

ABSTRACT We present a measurement of the Hubble constant (H0) and other cosmological parameters from a joint analysis of six gravitationally lensed quasars with measured time delays. All lenses except the first are analysed blindly with respect to the cosmological parameters. In a flat Λ cold dark matter (ΛCDM) cosmology, we find $H_{0} = 73.3_{-1.8}^{+1.7}~\mathrm{km~s^{-1}~Mpc^{-1}}$, a $2.4{{\ \rm per\ cent}}$ precision measurement, in agreement with local measurements of H0 from type Ia supernovae calibrated by the distance ladder, but in 3.1σ tension with Planck observations of the cosmic microwave background (CMB). This method is completely independent of both the supernovae and CMB analyses. A combination of time-delay cosmography and the distance ladder results is in 5.3σ tension with Planck CMB determinations of H0 in flat ΛCDM. We compute Bayes factors to verify that all lenses give statistically consistent results, showing that we are not underestimating our uncertainties and are able to control our systematics. We explore extensions to flat ΛCDM using constraints from time-delay cosmography alone, as well as combinations with other cosmological probes, including CMB observations from Planck, baryon acoustic oscillations, and type Ia supernovae. Time-delay cosmography improves the precision of the other probes, demonstrating the strong complementarity. Allowing for spatial curvature does not resolve the tension with Planck. Using the distance constraints from time-delay cosmography to anchor the type Ia supernova distance scale, we reduce the sensitivity of our H0 inference to cosmological model assumptions. For six different cosmological models, our combined inference on H0 ranges from ∼73 to 78 km s−1 Mpc−1, which is consistent with the local distance ladder constraints.

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A Model-independent Determination of the Hubble Constant from Lensed Quasars and Supernovae Using Gaussian Process Regression

The Astrophysical Journal ◽

10.3847/2041-8213/ab5308 ◽

2019 ◽

Vol 886 (1) ◽

pp. L23 ◽

Cited By ~ 11

Author(s):

Kai Liao ◽

Arman Shafieloo ◽

Ryan E. Keeley ◽

Eric V. Linder

Keyword(s):

Gaussian Process ◽

Gaussian Process Regression ◽

Hubble Constant ◽

Independent Determination ◽

Model Independent

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Cosmological Parameter Survey Using the Gravitational Lensing Method

Publications of the Astronomical Society of Australia ◽

10.1071/as01022 ◽

2001 ◽

Vol 18 (2) ◽

pp. 201-206 ◽

Cited By ~ 2

Author(s):

Premana W. Premadi ◽

Hugo Martel ◽

Richard Matzner ◽

Toshifumi Futamase

Keyword(s):

Gravitational Lensing ◽

Light Propagation ◽

Cold Dark Matter ◽

Cosmological Parameters ◽

Angular Size ◽

Hubble Constant ◽

Density Parameter ◽

Multiple Imaging ◽

Light Rays ◽

Insight Into

AbstractUsing a multiple-lens plane algorithm, we study light propagation in inhomogeneous universes for 43 different COBE-normalized Cold Dark Matter models, with various values of the density parameter Ω0, cosmological constant λ0, Hubble constant H0, and rms density fluctuation σ8.We performed a total of 3798 experiments, each experiment consisting of propagating a square beam of angular size 21.9″ 21.9″ composed of 116 281 light rays from the observer up to redshift z = 3. These experiments provide statistics of the magnification, shear, and multiple imaging of distant sources. The results of these experiments might be compared with observations, and eventually help constrain the possible values of the cosmological parameters. Additionally, they provide insight into the gravitational lensing process and its complex relationship with the various cosmological parameters.

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A model-independent constraint on the Hubble constant with gravitational waves from the Einstein Telescope

International Journal of Modern Physics D ◽

10.1142/s0218271820501059 ◽

2020 ◽

Vol 29 (15) ◽

pp. 2050105

Author(s):

Sixuan Zhang ◽

Shuo Cao ◽

Jia Zhang ◽

Tonghua Liu ◽

Yuting Liu ◽

...

Keyword(s):

Cosmological Model ◽

Gravitational Wave ◽

Gravitational Waves ◽

Simulated Data ◽

Hubble Constant ◽

Host Galaxies ◽

Local Universe ◽

Binary Neutron Star ◽

Einstein Telescope ◽

Model Independent

In this paper, we investigate the expected constraints on the Hubble constant from the gravitational-wave standard sirens, in a cosmological-model-independent way. In the framework of the well-known Hubble law, the GW signal from each detected binary merger in the local universe ([Formula: see text]) provides a measurement of luminosity distance [Formula: see text] and thus the Hubble constant [Formula: see text]. Focusing on the simulated data of gravitational waves from the third-generation gravitational wave detector (the Einstein Telescope, ET), combined with the redshifts determined from electromagnetic counter parts and host galaxies, one can expect the Hubble constant to be constrained at the precision of [Formula: see text] with 20 well-observed binary neutron star (BNS) mergers. Additional standard-siren measurements from other types of future gravitational-wave sources (NS-BH and BBH) will provide more precision constraints of this important cosmological parameter. Therefore, we obtain that future measurements of the luminosity distances of gravitational waves sources will be much more competitive than the current analysis, which makes it expectable more vigorous and convincing constraints on the Hubble constant in a cosmological-model-independent way.

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A model-independent test of the evolution of gas depletion factor for SPT-SZ and Planck ESZ clusters

The European Physical Journal C ◽

10.1140/epjc/s10052-021-09099-4 ◽

2021 ◽

Vol 81 (4) ◽

Author(s):

Kamal Bora ◽

Shantanu Desai

Keyword(s):

Hubble Parameter ◽

Mass Fraction ◽

Functional Form ◽

Cosmological Parameters ◽

Gaussian Process Regression ◽

Positive Trend ◽

Explicit Dependence ◽

Cluster Data ◽

Independent Test ◽

Model Independent

AbstractThe gas mass fraction in galaxy clusters has been widely used to determine cosmological parameters. This method assumes that the ratio of the cluster gas mass fraction to the cosmic baryon fraction ($$\gamma (z)$$ γ ( z ) ) is constant as a function of redshift. In this work, we look for a time evolution of $$\gamma (z)$$ γ ( z ) at $$R_{500}$$ R 500 by using both the SPT-SZ and Planck Early SZ (ESZ) cluster data, in a model-independent fashion without any explicit dependence on the underlying cosmology. For this calculation, we use a non-parametric functional form for the Hubble parameter obtained from Gaussian Process regression using cosmic chronometers. We parameterize $$\gamma (z)$$ γ ( z ) as: $$\gamma (z)= \gamma _0(1+\gamma _1 z)$$ γ ( z ) = γ 0 ( 1 + γ 1 z ) to constrain the redshift evolution. We find contradictory results between both the samples. For SPT-SZ, $$\gamma (z)$$ γ ( z ) decreases as a function of redshift (at more than 5$$\sigma $$ σ ), whereas a positive trend with redshift is found for Planck ESZ data (at more than 4$$\sigma $$ σ ). We however find that the $$\gamma _1$$ γ 1 values for a subset of SPT-SZ and Planck ESZ clusters between the same redshift interval agree to within $$1\sigma $$ 1 σ . When we allow for a dependence on the halo mass in the evolution of the gas depletion factor, the $$4-5\sigma $$ 4 - 5 σ discrepancy reduces to $$2\sigma $$ 2 σ .

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Tension with the flat ΛCDM model from a high-redshift Hubble diagram of supernovae, quasars, and gamma-ray bursts

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936223 ◽

2019 ◽

Vol 628 ◽

pp. L4 ◽

Cited By ~ 29

Author(s):

E. Lusso ◽

E. Piedipalumbo ◽

G. Risaliti ◽

M. Paolillo ◽

S. Bisogni ◽

...

Keyword(s):

Cold Dark Matter ◽

Gamma Ray ◽

High Redshift ◽

Cosmological Parameters ◽

New Physics ◽

Gamma Ray Bursts ◽

Hubble Diagram ◽

Data Set ◽

Λcdm Model ◽

Model Independent

In the current framework, the standard parametrization of our Universe is the so-called Lambda cold dark matter (ΛCDM) model. Recently, a ∼4σ tension with the ΛCDM model was shown to exist via a model-independent parametrization of a Hubble diagram of type Ia supernovae (SNe Ia) from the JLA survey and quasars. Model-independent approaches and independent samples over a wide redshift range are key to testing this tension and any possible systematic errors. Here we present an analysis of a combined Hubble diagram of SNe Ia, quasars, and gamma-ray bursts (GRBs) to check the agreement of the quasar and GRB cosmological parameters at high redshifts (z > 2) and to test the concordance flat ΛCDM model with improved statistical accuracy. We build a Hubble diagram with SNe Ia, quasars, and GRBs, where quasars are standardised through the observed non-linear relation between their ultraviolet and X-ray emission and GRBs through the correlation between the spectral peak energy and the isotropic-equivalent radiated energy (the so-called Amati relation). We fit the data with cosmographic models consisting of a fourth-order logarithmic polynomial and a fifth-order linear polynomial, and compare the results with the expectations from a flat ΛCDM model. We confirm the tension between the best-fit cosmographic parameters and the ΛCDM model at ∼4σ with SNe Ia and quasars, at ∼2σ with SNe Ia and GRBs, and at > 4σ with the whole SNe Ia+quasars+GRB data set. The completely independent high-redshift Hubble diagrams of quasars and GRBs are fully consistent with each other, strongly suggesting that the deviation from the standard model is not due to unknown systematic effects but to new physics.

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Space-borne atom interferometric gravitational wave detections. Part I. The forecast of bright sirens on cosmology

Journal of Cosmology and Astroparticle Physics ◽

10.1088/1475-7516/2021/12/017 ◽

2021 ◽

Vol 2021 (12) ◽

pp. 017

Author(s):

Rong-Gen Cai ◽

Tao Yang

Keyword(s):

Dark Energy ◽

Gravitational Wave ◽

Modified Gravity ◽

Cosmological Parameters ◽

Operation Time ◽

Hubble Constant ◽

Gravity Theory ◽

Modified Gravity Theory ◽

Near Future

Abstract Atom interferometers (AIs) as gravitational-wave (GW) detectors have been proposed a decade ago. Both ground and space-based projects will be in construction and preparation in the near future. In this paper, for the first time, we investigate the potential of the space-borne AIs on detecting GW standard sirens and hence the applications on cosmology. We consider AEDGE as our fiducial AI GW detector and estimate the number of bright sirens that would be obtained within a 5-years data-taking period of GW and with the follow-up observation of electromagnetic (EM) counterparts. We then construct the mock catalogue of bright sirens and predict their ability on constraining cosmological parameters such as the Hubble constant, dynamics of dark energy, and modified gravity theory. Our preliminary results show around order 𝒪 (30) bright sirens can be obtained from a 5-years operation time of AEDGE and the follow-up observation of EM counterparts. The bright sirens alone can measure H 0 with a precision 2.1%, which is sufficient to arbitrate the Hubble tension. Combining current most precise electromagnetic experiments, the inclusion of AEDGE bright sirens can improve the measurement of the equation of state of dark energy, though marginally. Moreover, by modifying GW propagation on cosmological scales, the deviations from general relativity (modified gravity theory effects) can be constrained at 5.7% precision level.

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