Constraints on neutrino mass from Sunyaev-Zeldovich cluster surveys

Mak, D. S. Y.; Pierpaoli, E.

doi:10.1103/physrevd.87.103518

Cited by 9 publications

(4 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Of further importance is the different degeneracy direction between structure growth parameters probed by clusters compared to cosmic microwave background (CMB) or Baryonic Acoustic Oscillations (BAO) which provides compelling joint constraints. This has been demonstrated previously in the literature (for example, Mantz et al 2008;Vikhlinin et al 2009;von der Linden et al 2014;de Haan et al 2016;Salvati et al 2018;Bocquet et al 2019;Zubeldia & Challinor 2019) and the potential of clusters as cosmological probes from future surveys has also been a subject of extensive study (for example, Holder et al 2001;Lima & Hu 2004;Sartoris et al 2012;Mak &Pierpaoli 2013, andrecently Louis &Madhavacheril et al 2017;Cromer et al 2019;Gupta et al 2020).…”

Section: Introductionsupporting

confidence: 52%

Constraining Cluster Virialization Mechanism and Cosmology using Thermal-SZ-selected clusters from Future CMB Surveys

Raghunathan,

Whitehorn,

Alvarez

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

We forecast the number of galaxy clusters that can be detected via the thermal Sunyaev-Zel'dovich (tSZ) signals by future cosmic microwave background (CMB) experiments, primarily the wide area survey of the CMB-S4 experiment but also CMB-S4's smaller delensing survey and the proposed CMB-HD experiment. We predict that CMB-S4 will detect 75,000 clusters with its wide survey of f sky = 50% and 14,000 clusters with its deep survey of f sky = 3%. Of these, approximately 1350 clusters will be at z ≥ 2, a regime that is difficult to probe by optical or X-ray surveys. We assume CMB-HD will survey the same sky as the S4-Wide, and find that CMB-HD will detect ×3 more overall and an order of magnitude more z ≥ 2 clusters than CMB-S4. These results include galactic and extragalactic foregrounds along with atmospheric and instrumental noise. Using CMB-cluster lensing to calibrate cluster tSZ-mass scaling relation, we combine cluster counts with primary CMB to obtain cosmological constraints for a two parameter extension of the standard model (ΛCDM + m ν + w 0 ). Besides constraining σ(w 0 ) to 1%, we find that both surveys can enable a ∼ 2.5 − 4.5σ detection of m ν , substantially strengthening CMB-only constraints. We also study the evolution of intracluster medium by modelling the cluster virialization v(z) and find tight constraints from CMB-S4, with further factors of 3-4 improvement for CMB-HD.

show abstract

Section: Introductionsupporting

confidence: 52%

Constraining Cluster Virialization Mechanism and Cosmology using Thermal-SZ-selected clusters from Future CMB Surveys

Raghunathan,

Whitehorn,

Alvarez

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…Thus, as a net effect massive neutrinos cause a suppression in the amplitude of the matter power spectrum on small scales with respect to an equivalent massless neutrinos model. The dependence of these effects on the total neutrino mass indicates that astrophysical observations have the potential to provide constraints on the value of Σm ν , as it has been shown by several recent theoretical works (see e. g. Viel et al 2010;Marulli et al 2011;Shimon et al 2012;Carbone 2013;Costanzi Alunno Cerbolini et al 2013;Mak & Pierpaoli 2013;Roncarelli et al 2015;Palanque-Delabrouille et al 2015). In fact, the list of cosmological probes that can be used to place limits on the sum of neutrino masses is nowadays long and heterogeneous, including galaxy redshift surveys (Elgarøy et al 2002;Tegmark et al 2006;Thomas et al 2010), galaxy clustering (Saito et al 2011;Zhao et al 2013;Beutler et al 2014;Sánchez et al 2014), cosmic microwave background (CMB) observations from the Wilkinson Microwave Anisotropy Probe (WMAP; Komatsu et al 2009Komatsu et al , 2011Hinshaw et al 2013) and Planck (Planck Collaboration XIII 2016), Ly-α forest studies (Croft et al 1999;Viel et al 2010;Palanque-Delabrouille et al 2015), galaxy clusters mass function (Mantz et al 2010(Mantz et al , 2015 and future 21cm intensity mapping observations (Villaescusa-Navarro et al 2015).…”

Section: Introductionmentioning

confidence: 80%

The kinematic Sunyaev–Zel’dovich effect of the large-scale structure (I): dependence on neutrino mass

Roncarelli

Villaescusa-Navarro

Baldi

2017

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The study of neutrinos in astrophysics requires the combination of different observational probes. The temperature anisotropies of the cosmic microwave background induced via the kinematic Sunyaev-Zel'dovich (kSZ) effect may provide interesting information since they are expected to receive significant contribution from high-redshift plasma. We present a set of cosmological hydrodynamical simulations that include a treatment of the neutrino component considering four different sum of neutrino masses: Σm ν = (0, 0.15, 0.3, 0.6) eV. Using their outputs, we modelled the kSZ effect due to the large-scale structure after the reionization by producing mock maps, then computed the kSZ power spectrum and studied how it depends on z re and Σm ν . We also run a set of four simulations to study and correct possible systematics due to resolution, finite box size and astrophysics. With massless neutrinos we obtain D kSZ 3000 = 4.0 µK 2 (z re =8.8), enough to account for all of the kSZ signal of D kSZ 3000 = (2.9 ± 1.3) µK 2 measured with the South Pole Telescope. This translates into an upper limit on the kSZ effect due to patchy reionization of D kSZ,patchy 3000 < 1.0 µK 2 (95 per cent confidence level). Massive neutrinos induce a damping of kSZ effect power of about 8, 12 and 40 per cent for Σm ν = (0.15, 0.3, 0.6) eV, respectively. We study the dependence of the kSZ signal with z re and the neutrino mass fraction, f ν , and obtain D kSZ 3000 ∝z re 0.26 (1 − f ν ) 14.3 . Interestingly, the scaling with f ν is significantly shallower with respect to the equivalent thermal SZ effect, and may be used to break the degeneracy with other cosmological parameters. 1 This limit applies in the case of normal hierarchy, for the inverted hierarchy the limit is Σm ν > 0.1 eV. 2012Lesgourgues et al. 2013; Gonzalez-Garcia 2014, and references therein).From the astrophysical point of view, the existence of massive neutrinos influences the evolution of the large-scale structure (LSS) formation via gravitational interaction, thus requiring a generalization of the standard Λ cold dark matter (ΛCDM) cosmological model to account for Σm ν as an additional free parameter, leading to a ΛCDMν scenario. The effect of this new component is twofold. On early times it contributes to the Universe energy budget as radiation, with density of ρ ν = 7 8 4 11where ρ γ is the photon energy density, and N eff is the effective number of neutrino species (N eff = 3.046, according to the SM). This causes a postponing of the matter-radiation equality for a fixed value of Ω m h 2 (where Ω m is the ratio between the total matter denc 2016 RAS

show abstract

“…Besides these, the tSZ effect is also one of the most efficient methods used for detecting galaxy clusters (see catalogs from Bleem et al 2015;Planck Collaboration et al srinirag@illinois.edu 2016a; Hilton et al 2020;Huang et al 2020;Bleem et al 2020). The abundance of clusters as a function of mass and redshift can also place tight constraints on the parameters that govern structure formation and geometry of the Universe (Holder et al 2001;Lima & Hu 2004;Allen et al 2011;Sartoris et al 2012;Mak & Pierpaoli 2013) like, for example, dark energy equation of state w 0 , normalization of the matter power spectrum σ 8 , and the sum of neutrino masses m ν as demonstrated using data (recently by Zubeldia & Challinor 2019;Bocquet et al 2019;Planck Collaboration et al 2020;To et al 2021;Costanzi et al 2021;Mantz et al 2021;Salvati et al 2021). Thanks to its redshift independent nature (Sunyaev & Zel'dovich 1970), the tSZ effect allows us to detect clusters at high redshifts where the signal-tonoise (S/N) of other cluster observables like richness estimates or X-ray flux drop rapidly.…”

Section: Introductionmentioning

confidence: 99%

Assessing the Importance of Noise from Thermal Sunyaev-Zel{'}dovich Signals for CMB Cluster Surveys and Cluster Cosmology

Raghunathan

2021

Preprint

View full text Add to dashboard Cite

We explore the significance of noise from thermal Sunyaev-Zel'dovich (tSZ) signals for cluster detection using cosmic microwave background (CMB) surveys. The noise arises both from neighboring objects and also from haloes below the detection limit. A wide range of surveys are considered: SPT-SZ, SPTpol, and SPT-3G from the South Pole Telescope; SO-Baseline and SO-Goal configurations for Simons Observatory; CMB-S4's wide area (S4-Wide) and deep (S4-Ultra deep) surveys; and the futuristic CMB-HD experiment. We find that the noise from tSZ signals has a significant impact on CMB-HD and to some extent on S4-Ultra deep. For other experiments, the effect is negligible as the noise in the tSZ map is dominated by residual foregrounds or experimental noise. In the limit when the noise from tSZ signals is important, we find that removing the detected clusters and rerunning the cluster finder allows us to find a new set of less massive and distant clusters. Since the detected clusters are the dominant source of the tSZ power, removing them reduces the power at = 3000 by: ×5 for CMB-HD; ×3.1 of S4-Ultra deep; ×2.4 for S4-Wide and SPT-3G; ×1.5 for SO-Goal and SPTpol; ×1.35 for SO-Baseline; and ×1.08 for SPT-SZ. We forecast the expected number of clusters and also derive parameter constraints by combining cluster counts with primary CMB and tSZ power spectra finding that the future surveys can reduce the error on the dark energy equation of state parameter to sub-percent levels and can also enable ≥ 3σ detection of the sum of neutrino masses. The simulation products and results can be downloaded from this link .

show abstract

Constraints on neutrino mass from Sunyaev-Zeldovich cluster surveys

Cited by 9 publications

References 32 publications

Constraining Cluster Virialization Mechanism and Cosmology using Thermal-SZ-selected clusters from Future CMB Surveys

Constraining Cluster Virialization Mechanism and Cosmology using Thermal-SZ-selected clusters from Future CMB Surveys

The kinematic Sunyaev–Zel’dovich effect of the large-scale structure (I): dependence on neutrino mass

Assessing the Importance of Noise from Thermal Sunyaev-Zel{'}dovich Signals for CMB Cluster Surveys and Cluster Cosmology

Contact Info

Product

Resources

About