Constraining cosmology with the velocity function of low-mass galaxies

Schneider, Aurel; Trujillo-Gomez, Sebastian

doi:10.1093/mnras/sty054

Cited by 5 publications

(3 citation statements)

References 112 publications

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“…This number can be further pushed down to 0.7 (1.7) percent for the WL+X-ray scenario with Planck priors. We conclude that for small particle masses, expected limits on the fraction of warm/hot DM relics are significantly tighter than current constraints that are at the 10-20 percent level [71][72][73][74][75] .…”

Section: Jcap04(2020)020contrasting

confidence: 60%

Baryonic effects for weak lensing. Part II. Combination with X-ray data and extended cosmologies

Schneider

Réfrégier

Grandis

et al. 2020

J. Cosmol. Astropart. Phys.

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An accurate modelling of baryonic feedback effects is required to exploit the full potential of future weak-lensing surveys such as Euclid or LSST. In this second paper in a series of two, we combine Euclid-like mock data of the cosmic shear power spectrum with an eROSITA X-ray mock of the cluster gas fraction to run a combined likelihood analysis including both cosmological and baryonic parameters. Following the first paper of this series, the baryonic effects (based on the baryonic correction model of Ref.[1]) are included in both the tomographic power spectrum and the covariance matrix. However, this time we assume the more realistic case of a ΛCDM cosmology with massive neutrinos and we consider several extensions of the currently favoured cosmological model. For the standard ΛCDM case, we show that including X-ray data reduces the uncertainties on the sum of the neutrino mass by ∼ 30 percent, while there is only a mild improvement on other parameters such as Ω m and σ 8 . As extensions of ΛCDM, we consider the cases of a dynamical dark energy model (wCDM), a f (R) gravity model (fRCDM), and a mixed dark matter model (ΛMDM) with both a cold and a warm/hot dark matter component. We find that combining weak-lensing with X-ray data only leads to a mild improvement of the constraints on the additional parameters of wCDM, while the improvement is more substantial for both fRCDM and ΛMDM. Ignoring baryonic effects in the analysis pipeline leads significant false-detections of either phantom dark energy or a light subdominant dark matter component. Overall we conclude that for all cosmologies considered, a general parametrisation of baryonic effects is both necessary and sufficient to obtain tight constraints on cosmological parameters.

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Section: Jcap04(2020)020contrasting

confidence: 60%

Baryonic effects for weak lensing. Part II. Combination with X-ray data and extended cosmologies

Schneider

Réfrégier

Grandis

et al. 2020

J. Cosmol. Astropart. Phys.

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“…Observationally, blind H I surveys with single-dish radio telescopes provide the spatially integrated H I line-width (W H I ), which is a proxy for twice the rotation velocity of galaxies. The VF from H I surveys is well-described by a modified Schechter function and differs from the one predicted arXiv:1911.00517v1 [astro-ph.GA] 1 Nov 2019 in ΛCDM via V DM max (e.g., Zwaan et al 2010;Papastergis et al 2011) with possible implications for cosmology and the nature of DM (Zavala et al 2009;Klypin et al 2015;Schneider et al 2017;Schneider & Trujillo-Gomez 2018). The comparison between theory and observations, however, is complex because the relation between V DM max and W H I may be strongly non-linear (e.g., Brook & Shankar 2016;Macciò et al 2016;Brooks et al 2017;Chauhan et al 2019;Dutton et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Halo Mass Function of Late-type Galaxies from H i Kinematics

Lelli

McGaugh

et al. 2019

ApJL

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We present an empirical method to measure the halo mass function (HMF) of galaxies. We determine the relation between the H I line-width from single-dish observations and the dark matter halo mass (M 200 ) inferred from rotation curve fits in the SPARC database, then we apply this relation to galaxies from the H I Parkes All Sky Survey (HIPASS) to derive the HMF. This empirical HMF is well fit by a Schecther function, and matches that expected in ΛCDM over the range 10 10.5 < M 200 < 10 12 M . More massive halos must be poor in neutral gas to maintain consistency with the power law predicted by ΛCDM. We detect no discrepancy at low masses. The lowest halo mass probed by HIPASS, however, is just greater than the mass scale where the Local Group missing satellite problem sets in. The integrated mass density associated with the dark matter halos of H I-detected galaxies sums to Ω m,gal ≈ 0.03 over the probed mass range.

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“…However, during the last decade it has become more and more evident that baryonic effects driven by supernova feedback and high-redshift reionisation have the potential to solve most of these tensions [e.g. [13][14][15]; but see also 16,17] Independently of whether alternative dark matter models provide a better match to the data, it is possible to constrain them with astrophysical observations. The currently strongest limits come from the Lyman-α forest constraining the thermal particle mass of warm dark matter (WDM) to m TH > ∼ 3.5 keV [18,19][20].…”

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confidence: 99%

Constraining noncold dark matter models with the global 21-cm signal

2018

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Any particle dark matter (DM) scenario featuring a suppressed power spectrum of astrophysical relevance results in a delay of galaxy formation. As a consequence, such scenarios can be constrained using the global 21-cm absorption signal initiated by the UV radiation of the first stars. The Experiment to Detect the Global Epoch of Reionization Signature (EDGES) recently reported the first detection of such an absorption signal at redshift ∼ 17. While its amplitude might indicate the need for new physics, we solely focus on the timing of the signal to test non-cold DM models. Assuming conservative limits for the stellar-to-baryon fraction (f * < 0.03) and for the minimum cooling temperature (Tvir > 10 3 Kelvin) motivated by radiation-hydrodynamic simulations, we are able to derive unprecedented constraints on a variety of non-cold DM models. For example, the mass of thermal warm DM is limited to mTH > 6.1 keV, while mixed DM scenarios (featuring a cold and a hot component) are constrained to a hot DM fraction below 17 percent. The ultra-light axion DM model is limited to masses ma > 8 × 10 −21 eV, a regime where its wave-like nature is pushed far below the kiloparsec scale. Finally, sterile neutrinos from resonant production can be fully disfavoured as a dominant DM candidate. The results of this paper show that the 21-cm absorption signal is a powerful discriminant of non-cold dark matter, allowing for significant improvements over to the strongest current limits. Confirming the result from EDGES is paramount in this context.

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Constraining cosmology with the velocity function of low-mass galaxies

Cited by 5 publications

References 112 publications

Baryonic effects for weak lensing. Part II. Combination with X-ray data and extended cosmologies

Baryonic effects for weak lensing. Part II. Combination with X-ray data and extended cosmologies

The Halo Mass Function of Late-type Galaxies from H i Kinematics

Constraining noncold dark matter models with the global 21-cm signal

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