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Physics

A fresh look into the interacting dark matter scenario

Profile image of Pablo Villanueva DomingoPablo Villanueva Domingo

2018, Journal of Cosmology and Astroparticle Physics

https://doi.org/10.1088/1475-7516/2018/06/007
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34 pages

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Abstract

The elastic scattering between dark matter particles and radiation represents an attractive possibility to solve a number of discrepancies between observations and standard cold dark matter predictions, as the induced collisional damping would imply a suppression of small-scale structures. We consider this scenario and confront it with measurements of the ionization history of the Universe at several redshifts and with recent estimates of the counts of Milky Way satellite galaxies. We derive a conservative upper bound on the dark matterphoton elastic scattering cross section of σ γDM < 8×10 −10 σ T (m DM /GeV) at 95% CL, about one order of magnitude tighter than previous constraints from satellite number counts. Due to the strong degeneracies with astrophysical parameters, the bound on the dark matter-photon scattering cross section derived here is driven by the estimate of the number of Milky Way satellite galaxies. Finally, we also argue that future 21 cm probes could help in disentangling among possible non-cold dark matter candidates, such as interacting and warm dark matter scenarios. Let us emphasize that bounds of similar magnitude to the ones obtained here could be also derived for models with dark matter-neutrino interactions and would be as constraining as the tightest limits on such scenarios.

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    Joan Solà Peracaula

    Journal of High Energy Astrophysics

    Indirect Direct 60 65 70 75 80 85 FIG. 2. 68% CL constraint on H0 from different cosmological probes (based on Refs. [49, 50]). the local value of the H 0 from SNIa, where one does not enforce a universal color-luminosity relation to correct the near-IR Cepheid magnitudes, which gives H 0 = (71.8 ± 1.76) km s −1 Mpc −1 , or H 0 = (66.9 ± 2.5) km s −1 Mpc −1 , at 68% CL depending on the approach [123], and H 0 = (70.8 ± 2.1) km s −1 Mpc −1 at 68% CL in Ref. [124]. At the same time, the impact of known and several previously neglected or unrecognized systematic effects on the center values of the SH0ES results has been constrained to be well below the 1% level [125-129]. Interestingly, correcting reported H 0 values for such systematic effects can result in an increased value of H 0 (e.g., due to time dilation of observed variable star periods, cf. Ref. [126]), and thus, to an increased significance of the discord between the distance ladder and the early Universe-based H 0 values. An independent determination of H 0 is based on calibration of the Type Ia supernovae (SNIa) using the Tip of the Red Giant Branch, where one finds H 0 = (71.17 ± 1.66 (stat) ± 1.87 (sys)) km s −1 Mpc −1 at 68% CL [130], H 0 = (69.8 ± 0.8 (stat) ± 1.7 (sys)) km s −1 Mpc −1 at 68% CL [131], H 0 = (72.4 ± 2.0) km s −1 Mpc −1 at 68% CL [132], and the final H 0 = (69.6 ± 0.8 (stat) ± 1.7 (sys)) km s −1 Mpc −1 at 68% CL [133]. Then we have H 0 = (71.1 ± 1.9) km s −1 Mpc −1 at 68% CL [111], and the H 0 estimate using velocities and TRGB distances to 33 galaxies located between the Local Group and the Virgo cluster, H 0 = (69.5 ± 3.5 (stat) ± 2.4 (sys)) km s −1 Mpc −1 at 68% CL [134]. Moreover, it is important to mention the Freedman result H 0 = (69.8 ± 0.6 (stat) ± 1.6 (sys)) km s −1 Mpc −1 at 68% CL [135], or the re-analysis of Ref. [136] that gives H 0 = (71.5 ± 1.8) km s −1 Mpc −1 at 68% CL. Finally, there are the latest measurements H 0 = (72.4 ± 3.3) km s −1 Mpc −1 at 68% CL of Ref. [137] and H 0 = (76.94 ± 6.4) km s −1 Mpc −1 at 68% CL of Ref. [138]. A larger value for H 0 is preferred also by the analysis of the near-infrared HST WFC3 observations of the Mira variable red giant stars in NGC 1559, that gives H 0 = (73.3 ± 4.0) km s −1 Mpc −1 at 68% CL [139]. A measurement of the Hubble constant can be obtained with the Surface Brightness Fluctuations (SBF) method calibrated from Cepheids, with H 0 = (71.9 ± 7.1) km s −1 Mpc −1 at 68% CL [140] from a single galaxy (the host of GW170817) at 40 Mpc and H 0 = (70.50 ± 2.37 (stat) ± 3.38 (sys)) km s −1 Mpc −1 at 68% CL [141] from using SBF as an intermediate rung between Cepheids and SNIa. A re-analysis of the latter performed by Ref. [142], improving the LMC distance, gives instead H 0 = (71.1 ± 2.4(stat) ± 3.4(sys)) km s −1 Mpc −1 at 68% CL. Moreover, if SBF is used as another long-range indicator calibrated by Cepheids and TRGB, Ref. [142] finds H 0 = (73.3 ± 0.7 (stat) ± 2.4 (sys)) km s −1 Mpc −1 at 68% CL from a new sample of HST NIR data for 63 galaxies out to 100 Mpc. Another possible observable to constrain H 0 is given by the Standardized Type II supernovae. Using 7 SNe II with host-galaxy distances measured from Cepheid variables or the TRGB, the Hubble constant is equal to H 0 = 75.8 +5.2 −4.9 km s −1 Mpc −1 at 68% CL [143], while with 13 SNe II Ref. [144] finds H 0 = 75.4 +3.8 −3.7 km s −1 Mpc −1 at 68% CL. An important independent result was obtained with the Megamaser Cosmology Project, which gives an H 0 estimate by using the geometric distance measurements to megamaser-hosting galaxies, finding H 0 = (66.6±6.0) km s −1 Mpc −1 at 68% CL [145], and H 0 = (73.9 ± 3.0) km s −1 Mpc −1 at 68% CL [146], independent of distance ladders. In addition, there are the estimates of the Hubble constant based on the Tully-Fisher Relation, i.e. the correlation between the rotation rate of spirals and their absolute luminosity used to measure the galaxy distances. Using optical and infrared calibrated Tully-Fisher Relations, the Hubble constant is equal to H 0 = (76.0 ± 1.1 (stat) ± 2.3 (sys)) km s −1 Mpc −1 at 68% CL [147]. Considering the baryonic Tully-Fisher relation (bTFR) as a new distance indicator, instead, the Hubble constant is found to be H 0 = (75.1 ± 2.3 (stat) ± 1.5 (sys)) km s −1 Mpc −1 at 68% CL [148], and H 0 = (75.5 ± 2.5) km s −1 Mpc −1 at 68% CL [149]. An estimate of H 0 can also be obtained by modeling the extragalactic background light and its role in attenuating γ-rays, but this is challenging and the uncertainties may be underestimated. In this case there is Ref. [150] that finds H 0 = 71.8 +4.6 −5.6 (stat) +7.2 −13.8 (sys) km s −1 Mpc −1 at 68% CL, the updated value H 0 = 67.4 +6.0 −6.2 km s −1 Mpc −1 at 68% CL [151], and H 0 = 64.9 +4.6 −4.3 km s −1 Mpc −1 at 68% CL [152]. The HII galaxy measurement can also act as a good distance indicator independent of SNIa to probe the background evolution of the Universe. Using 156 HII galaxy measurements, we obtain the constraint H 0 = 76.12 +3.47 −3.44 km s −1 Mpc −1 at 68% CL [153], which is more consistent with the H 0 value from the SH0ES Team than that from the Planck collaboration (see also [154]) Moreover, we have the strong lensing time delays estimates, that are not ΛCDM model dependent but still astrophysical model dependent, because of the imperfect knowledge of the foreground and lens mass distributions. Here we have the H0LiCOW inferred values H 0 = 71.9 +2.4 −3.0 km s −1 Mpc −1 at 68% CL in 2016 [155], H 0 = 72.5 +2.1 −2.3 km s −1 Mpc −1 at 68% CL in 2018 [156], and H 0 = 73.3 +1.7 −1.8 km s −1 Mpc −1 at 68% CL in 2019 [67], 3 based on strong gravitational lensing effects on quasar systems under standard assumptions on the radial mass density profile of the lensing galaxies. A reanalysis of H0LiCOW's four lenses is performed in Ref. [162] finding H 0 = 73.65 +1.95 −2.26 km s −1 Mpc −1 at 68% CL. Under the same assumptions, the STRIDES collaboration measures from the strong lens system DES J0408-5354

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    Constraining the primordial black hole abundance with 21-cm cosmology
    Pablo Villanueva Domingo

    Physical Review D, 2019

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    Dark matter microphysics and 21 cm observations
    Pablo Villanueva Domingo

    Physical Review D, 2019

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