Dark Energy Constraintsfrom Quasar Observations

Martínez-Aldama, Mary Loli; Wojtkowska, G.; Marziani, Paola; Dultzin, D.; Naddaf, Mohammad-Hassan; Panda, Swayamtrupta; Prince, Raj; Przyłuski, Robert; Rałowski, Mateusz; Śniegowska, Marzena

doi:10.12693/aphyspola.139.389

Cited by 29 publications

(21 citation statements)

References 31 publications

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“…While we have discovered an issue with the SDSS-4XMM data, it is at present not known if this was generated during the original compilation process or whether the SDSS-4XMM QSOs have an 𝐿 𝑋 − 𝐿 𝑈 𝑉 relation that evolves with 𝑧 and so are non-standardizable. We also note that other, somewhat lower 𝑧, reverberation-measured Mg II time-lag, radius-luminosity standardized, QSO constraints are consisitent with the standard flat ΛCDM model (Martínez-Aldama et al 2019;Czerny et al 2021;Zajaček et al 2021;Yu et al 2021;Khadka et al 2021b).…”

Section: Introductionmentioning

confidence: 58%

Using quasar X-ray and UV flux measurements to constrain cosmological model parameters

Khadka

Ratra

2020

Monthly Notices of the Royal Astronomical Society

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Risaliti and Lusso have compiled X-ray and UV flux measurements of 1598 quasars (QSOs) in the redshift range 0.036 ≤ z ≤ 5.1003, part of which, z ∼ 2.4 − 5.1, is largely cosmologically unprobed. In this paper we use these QSO measurements, alone and in conjunction with baryon acoustic oscillation (BAO) and Hubble parameter [H(z)] measurements, to constrain cosmological parameters in six different cosmological models, each with two different Hubble constant priors. In most of these models, given the larger uncertainties, the QSO cosmological parameter constraints are mostly consistent with those from the BAO + H(z) data. A somewhat significant exception is the nonrelativistic matter density parameter Ωm0 where QSO data favor Ωm0 ∼ 0.5 − 0.6 in most models. As a result, in joint analyses of QSO data with H(z) + BAO data the one-dimensional Ωm0 distributions shift slightly toward larger values. A joint analysis of the QSO + BAO + H(z) data is consistent with the current standard model, spatially-flat ΛCDM, but mildly favors closed spatial hypersurfaces and dynamical dark energy. Since the higher Ωm0 values favored by QSO data appear to be associated with the z ∼ 2 − 5 part of these data, and conflict somewhat with strong indications for Ωm0 ∼ 0.3 from most z < 2.5 data as well as from the cosmic microwave background anisotropy data at z ∼ 1100, in most models, the larger QSO data Ωm0 is possibly more indicative of an issue with the z ∼ 2 − 5 QSO data than of an inadequacy of the standard flat ΛCDM model.

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Section: Introductionmentioning

confidence: 58%

Using quasar X-ray and UV flux measurements to constrain cosmological model parameters

Khadka

Ratra

2020

Monthly Notices of the Royal Astronomical Society

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“…A appear to be in highly star forming hosts, very metal rich, possibly with enrichment associated with a circumnuclear Starburst or nuclear accretion modified stars (D'Onofrio & Marziani 2018). Preliminary attempts to build a Hubble diagram with xA sources are still affected by large dispersion in the distance modulus estimates (Czerny et al 2021; Dultzin et al 2020). Large samples (ideally recognized via machine learning, Jankov et al 2021; Peruzzi et al 2021 could help) reduce the statistical dispersion.…”

Section: Discussionmentioning

confidence: 99%

The main sequence of quasars: The taming of the extremes

Marziani

Bon

et al. 2021

Astron Nachr

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The last few years have seen the confirmation of several trends associated with the quasar main sequence. The idea of a main sequence for quasars is relatively recent, and its full potential for the observational classification and contextualization of quasars' properties has yet to be fully exploited. The main sequence drivers are discussed in terms of the properties of extreme objects. We briefly summarize developments that constrain the viewing angle of the accretion disk in a particular class of quasars (extreme Population B, radiating at low Eddington ratio), as well as inferences on the chemical composition of the broad line emitting gas, and on the nature of radio emission along the quasar main sequence.

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“…Farooq et al 2017;Scolnic et al 2018;Planck Collaboration 2020;eBOSS Collaboration 2021). The measurements, however, are not yet decisive enough (see, surements that reach to z ∼ 7.5 (Risaliti & Lusso 2015Khadka & Ratra 2020a,b, 2021Lusso et al 2020;Zhao & Xia 2021;Rezaei et al 2022;Luongo et al 2021;Leizerovich et al 2021;Colgáin et al 2022;Dainotti et al 2022a), 1 and -the main subject of our paper -gamma-ray burst (GRB) observations that reach to z ∼ 8.2 (Cardone et al 2009(Cardone et al , 2010Samushia & Ratra 2010;Dainotti et al 2013;Postnikov et al 2014;Wang et al 2015Wang et al , 2016Dainotti & Del Vecchio 2017;Dainotti & Amati 2018;Wang et al 2022;Fana Dirirsa et al 2019;Amati et al 2019;Khadka & Ratra 2020c;Hu et al 2021;Demianski et al 2021;Khadka et al 2021b;Luongo et al 2021;Luongo & Muccino 2021;Cao et al 2021a;Liu et al 2022). In this paper the highest redshift GRB we use is at z = 9.4 (Cucchiara et al 2011), but GRBs might be detectable to z = 20 (Lamb & Reichart 2000).…”

Section: Introductionmentioning

confidence: 85%

Gamma-ray burst data strongly favor the three-parameter fundamental plane (Dainotti) correlation relation over the two-parameter one

Cao¹,

Dainotti²,

Ratra³

2022

Preprint

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Gamma-ray bursts (GRBs), observed to redshift z = 9.4, are potential probes of the largely unexplored z ∼ 2.7 − 9.4 part of the early Universe. Thus, finding relevant relations among GRB physical properties is crucial. We find that the Platinum GRB data compilation, with 50 long GRBs (with relatively flat plateaus and no flares) in the redshift range 0.553 ≤ z ≤ 5.0, and the LGRB95 data compilation, with 95 long GRBs in 0.297 ≤ z ≤ 9.4, as well as the 145 GRB combination of the two, strongly favor the three-dimensional (3D) fundamental plane (Dainotti) correlation relation (between the peak prompt lumininosity, the luminosity at the end of the plateau emission, and its rest frame duration) over the two-dimensional one (between the luminosity at the end of the plateau emission and its duration). The 3D Dainotti correlations in the three data sets are standardizable. We find that while LGRB95 data have ∼ 50% larger intrinsic scatter parameter values than the better-quality Platinum data, they provide somewhat tighter constraints on cosmological-model and GRB-correlation parameters, perhaps solely due to the larger number of data points, 95 versus 50. This suggests that when compiling GRB data for the purpose of constraining cosmological parameters, given the quality of current GRB data, intrinsic scatter parameter reduction must be balanced against reduced sample size.

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Dark Energy Constraintsfrom Quasar Observations

Cited by 29 publications

References 31 publications

Using quasar X-ray and UV flux measurements to constrain cosmological model parameters

Using quasar X-ray and UV flux measurements to constrain cosmological model parameters

The main sequence of quasars: The taming of the extremes

Gamma-ray burst data strongly favor the three-parameter fundamental plane (Dainotti) correlation relation over the two-parameter one

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