© 2016 ESO.This paper presents a study of the integrated Sachs-Wolfe (ISW) effect from the Planck 2015 temperature and polarization data release. of the Planck CMB observations and many other astrophysical data sets. These data are consistent with the six-parameter inflationary LCDM cosmology. Even with the increase in precision and robustness, the ΛCDM cosmological model continues to offer a very good fit to the Planck data. Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. When multiple solutions are derived by any method, we find that combining the redshift solutions of the two techniques improves the rms by a factor of two. temperature and polarization data gives a lensing detection at 9.1 sigma Therefore, in Fig. It is based on the Planck 48 months mission data that are currently being released to the astron omical community. The required amount of CP violation in charged $D$ meson decays, while currently allowed, will be probed by colliders. ISSN 0004-6361 statistical approach used, and of the different combinations of CMB and BAO First, the gas density bias relation can be directly mapped onto the dark matter density field to high precision exploiting the strong correlation between them. "1 or <1 kpc) with peaked radio spectral shapes. We have performed a search over 3440 deg² of Epoch 1 (2017–2019) of the Very Large Array Sky Survey to identify unobscured quasars in the optical (0.2 < z < 3.2) and obscured active galactic nuclei (AGNs) in the infrared that have brightened dramatically in the radio over the past one to two decades. The model is based on a $U(1)$ extension of the Standard Model where the dark sector consists of two essentially mass degenerate Dirac fermions in the sub-GeV region with a small mass splitting interacting with a dark photon. Palanque-Delabrouille et al. This analysis rules out galaxies hosting LGRBs (faint, star-forming galaxies) as common hosts for FRBs (>95% c.l.). In this paper we consider the problem of diffuse astrophysical component separation, and process these maps within a Bayesian framework to derive an internally consistent set of full-sky astrophysical component maps. © 2008-2020 ResearchGate GmbH. Lastly, we test a range of specific models, such as k-essence, f (R) theories and coupled DE. Title: Planck 2015 results. The interpretation of the measured Ly$\alpha$ spectrum is done using a based on some form of resummation can fit our N-body data for BOSS-like galaxies above 30 h−1 Mpc well enough to return unbiased parameter estimates. of cosmological structure, which depends both on the expansion rate of the Universe and our theory of gravity. $\sum m_\nu$, for which we obtain an upper bound of 1.1~eV (95\% CL), including Low Frequency Instrument beams and window functions, Planck 2015 results. We then move to general parameterizations of the DE or MG perturbations that encompass both e ective field theories and the phenomenology of gravitational potentials in MG models. vacuum stability and high-scale inflation can be successfully accommodated. When estimating the density of DE at early times, we significantly improve present constraints and find that it has to be below 2 % (at 95% confidence) of the critical density even when forced to play a role forz < 50 only. A compilation of all the papers using Planck data (by the Planck Collaboration and by o… We present forecasts comparing cluster and galaxy alignments for two extragalactic survey set-ups: a currently-available low redshift survey (SDSS) and an upcoming higher redshift survey (LSST). the favoured dark matter candidates is always larger than 500 GeV. Section 6 summarizes our results. scalar or vector mediator, with a mixture of tau (75%) and electron (25%) 2013 results. Dark energy and modified gravity, The WiggleZ Dark Energy Survey: Improved distance measurements to z = 1 with reconstruction of the baryonic acoustic feature. This indicates that infrared galaxies in the outskirts of clusters have higher infrared flux than cluster-core galaxies. We investigate first order phase transitions in a holographic setting of five-dimensional Einstein gravity coupled to a scalar field, constructing phase diagrams of the dual field theory at finite temperature. problems in the standard $\Lambda$CDM cosmology. The Planck full mission cosmic microwave background (CMB) temperature and E-mode polarization maps are analysed to obtain constraints on primordial non-Gaussianity (NG). standardized absolute magnitudes calibrated via the Cepheid period--luminosity The global history of reionization was shaped by the relative amounts of starlight released by three halo mass groups: atomic-cooling halos (ACHs) with virial temperatures Tvir > 10^4 K, either (1) massive enough to form stars even after reionization (HMACHs, >~ 10^9 Msun) or (2) less-massive (LMACHs), subject to star formation suppression when overtaken by reionization, and (3) H2-cooling minihalos (MHs) with Tvir < 10^4 K, whose star formation is predominantly suppressed by the H2-dissociating Lyman-Werner (LW) background. Lyman α emitters gone missing: Evidence for late reionization? The results are interpreted as 95% confidence-level limits in models where weakly interacting dark-matter candidates are pair-produced via an s-channel axial-vector or vector mediator. deviations from standard recombination, finding no evidence for new physics. Improvements in data processing and instrumental modelling further reduce uncertainties. As a first application, we use these results to put bounds on the photon-axion conversion from spectral distortion of the CMB. To read the full-text of this research, you can request a copy directly from the author. tends to favor the normal hierarchy scenario against the inverted hierarchy These data are consistent with the six-parameter inflationary LCDM cosmology. Planck 2015 results. is compatible in morphology and spectrum with a telltale sign from dark matter uncertainties that some of us recently outlaid in Calore et al. ... We start by generating correlated realizations of the spherical harmonic coefficients a lm of the unlensed T, E, and B fields, as well as the CMB lensing potential ϕ and anistropic rotation angle field α, using HEALPIX [57]. The spatial curvature of our Universe is found to be very close to zero, with | ΩK | < 0.005. MicrOMEGAs is Moreover the constant k < 0 and the value of c, in a concrete way, can be generally determined from the classification in the two sub-models, Hu-Sawicki type (r > 0): c = 0; and Starobinsky type (r < 0): c = 2km/R 0 . We present results based on full-mission Planck observations of temperature and polarization anisotropies of the CMB. analytic models fit the simulations over a limited range of scales while failing at small scales. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with â < 20 are accordingly suppressed in the current polarization maps by high-pass filtering. 2014. We analyze the measurements of the 3PCF at larger scales, comparing them with theoretical models. Fitting the induced polarization pattern for this model to Planck data requires an amplitude of $-0.1\pm0.04$ compared to +1 if the model were to be correct. (1993); Bressan et al. Assuming an astrophysical origin, we reanalyze GW190426_152155 using several waveforms with different characteristics, and consider two different priors for the mass ratio of the binary (Uniform and LogUniform). By considering the Planck likelihood, based only on parity-even angular power spectra, we obtain B1 Mpc < 5.6 nG for a maximally helical field. Low Frequency Instrument data processing, Planck 2015 results. 2013) and most recent Planck (Planck XIII 2015, Planck VI 2018) analyses have the smallest quoted uncertainties. Joint constraints on the field-cluster mixing fraction, common envelope efficiency, and globular cluster radii from a population of binary hole mergers via deep learning, Long-lived Dark Higgs and Inelastic Dark Matter at Belle II, A fast semi-discrete optimal transport algorithm for a unique reconstruction of the early Universe, Applying Cosmological Principle to Better Probe the Redshift Evolution of Binary Black Hole Merger Rate, Particle spectra from dark matter annihilation: physics modeling and QCD uncertainties, SuperCLASS - II. significance of 3.2 sigma. 2000), developed at CDS, Strasbourg Observatory, France. Dark-matter candidates with masses up to 415 (580) GeV are excluded for axial-vector (vector) mediators, while the maximum excluded mass of the mediator is 1460 (1470) GeV. We We also analyse constraints on annihilating dark matter and on possible deviations from the standard recombination history. The final result is expressed as a likelihood curve for $r$, and Using these masks we compute the y-map angular power spectrum and higher order statistics. tracers of large-scale structure. Planck 2015 results XIII. Overall, Planck data constrain the amplitude of PMFs to less than a few nanoGauss, with different bounds that depend on the considered model. model: large amplitude of gravitational waves, suppression of power on horizon A B-mode polarization lensing signal is present with a The Planck design and scanning strategy provide many levels of redundancy Amusingly, this transfer proceeds without electroweak sphalerons, which are no longer active at such low scales. 0.11 {\rm\, (Sys.)}$. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. probes. This source of calibration only depends on the satellite velocity with respect to the solar system. Model (3) agrees well with Planck E-mode polarization data, even with a substantial tail of high-redshift ionization, beyond the limit proposed by the Planck Collaboration (2018). (DM) annihilation. plane, analysed independently by different teams using different software, and To analyze the constraints associated with the viability requirements, the models were expressed in terms of a dimensionless variable, i.e. Using the LISA Cosmology Working Group gravitational wave power spectrum model corrected for kinetic energy suppression at large $\alpha$ and non-conformal stiffness, we outline the observational prospects at the future space-based detectors LISA and TianQin. XVI. In addition to the latest Planck data, for our main analyses we use background constraints from baryonic acoustic oscillations, type-Ia supernovae and local measurements of the Hubble constant. by BOSS but differ in the details of how small-scale velocities and halo occupancy are determined. From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H_0 = (67.8±0.9) km s^(-1)Mpc^(-1), a matter density parameter Ωm = 0.308 ± 0.012, and a tilted scalar spectral index with n_s = 0.968 ± 0.006, consistent with the 2013 analysis. This paper describes the identification, modelling, and removal of previously unexplained systematic effects in the polarization data of the Planck High Frequency Instrument (HFI) on large angular scales, including new mapmaking and calibration procedures, new and more complete end-to-end simulations, and a set of robust internal consistency checks on the resulting maps. The standard big bang nucleosynthesis predictions for the helium and deuterium abundances for the best-fit Planck base ΛCDM cosmology are in excellent agreement with observations. Among the 112 reviews are many that are new or heavily revised including those on: Dark Energy, Higgs Boson Physics, Electroweak Model, Neutrino Cross Section Measurements, Monte Carlo Neutrino Generators, Top Quark, Dark Matter, Dynamical Electroweak Symmetry Breaking, Accelerator Physics of Colliders, High-Energy Collider Parameters, Big Bang Nucleosynthesis, Astrophysical Constants and Cosmological Parameters. The joint cross-correlation of the CMB with the tracers yields a detection at 4σ where most of the signal-to-noise is due to the Planck lensing and the NVSS radio catalogue. Lewis, A, Munshi, D and The Planck Collaboration, et al. and systematic checks show that our results are not significantly biased by With the three different methods, we detect the tSZ-CIB cross-power spectrum at significance levels of (i) 6σ; (ii) 3σ; and (iii) 4σ. These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. transport parameters which best fit the B/C ratio. Modelling the emission with a Navarro-Frenk-White profile, we find that the radial profile concentration parameter is c500 = 1.00+0.18-0.15 c500=1.00-0.15+0.18. GW190426_152155: a merger of neutron star-black hole or low mass binary black holes? using SNe~Ia is currently overestimated. Moreover, like magnetic fields amplified inside galaxies, these magnetic fields do not depend on the primordial seed, i.e. From the Planck temperature and lensing data, for this cosmology we find a Hubble constant, H0= (67.8 +/- 0.9) km/s/Mpc, a matter density parameter Omega_m = 0.308 +/- 0.012 and a scalar … The Planck results for base LambdaCDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. We leverage powerful mathematical tools stemming from optimal transport theory and transform them into an efficient algorithm to reconstruct the fluctuations of the primordial density field, built on solving the Monge-Amp\`ere-Kantorovich equation. stable and yield high-scale inflation successfully. The transmissivity depends not only on the ionized fraction of the intergalactic Here, we model the formation of Population III stars in moderate LW backgrounds of 100 and 500 $\rm J_{21}$ that were much more common at early times. addition its chemical content should be dominated by helium. the interstellar medium. +/-0.06(syst. We find 95 per cent of the μJy radio source sample (141/149) have spectral energy distributions (SEDs) best fit by star-forming templates while 5 per cent (8/149) are better fit by active galactic nuclei (AGN). considering an arbitrary value of the particle mass, or extended cosmological As photon-axion coupling grows with energy, stronger constraints could potentially be obtained using data on the propagation of gamma-ray photons through the IGM. We find that the opposite is true for repulsive self-interactions in that solitons would be more easily tidally stripped. 1/N_*$, where $N_* \sim 60$ is the number of $e$-folds for observationally the Galaxy is described using a semi-analytic two-zone model. The median temperature of PGCC sources lies between 13 and 14.5 K, depending on the quality of the flux density measurements, with a temperature ranging from 5.8 to 20 K after removing sources with the 1% largest temperature estimates. These searches yield no detection of a compact topology at a scale below the diameter of the last scattering surface. The temperature and polarization power spectra are consistent with the standard spatially-flat 6-parameter ΛCDM cosmology with a power-law spectrum of adiabatic scalar perturbations (denoted "base ΛCDM" in this paper). When assuming a curved ΛCDM model we obtain a curvature value of ΩK = −0.0043 ± 0.0047. combined with our previous measurement the effect is $0.094 \pm 0.025\ ... On the other hand, leptogenesis models typically occur at high scales and involve very massive particles, thereby making experimental confirmation unlikely. Our previous work showed that including MHs caused two-stage reionization - early rise to x ~ 0.1, driven by MHs, followed by a rapid rise, late, to x ~ 1, driven by ACHs - with a signature in CMB polarization anisotropy predicted to be detectable by the Planck satellite. The temperature and polarization power spectra are consistent … At 1.0 per cent, this latter measure is the most precise distance constraint ever obtained from a galaxy survey. The sample has a median value of $\approx80$ net counts in the 0.5-7 keV energy band. Additional isochrone references - Schoenberner (1983); Winget et al. $\Lambda$CDM cosmology with a power-law spectrum of initial perturbations and This will alleviate some of the unsolved small-scale structure We estimate reliable X-ray redshift solutions taking advantage of the main features in obscured AGN spectra, like the Fe 6.4 keV K$\mathrm{\alpha}$ emission line, the 7.1 keV Fe absorption edge and the photoelectric absorption cut-off. In this paper we use the 2015 … Furthermore, analogous to the assembly bias, we study the secondary dependence of the shape bias, and discover for the first time dependence on halo concentration and axis ratio. We validate the procedure through simulations. @article{Ade:2015xua, author = "Ade, P. A. R. and others", title = "{Planck 2015 results. Both methods are consistent, but the We present an updated description of the Planck Low Frequency Instrument (LFI) data processing pipeline, associated with the 2015 data release. standard astrophysical mechanisms, in which positrons are secondary particles, potential. This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. Such stars may lead to a population of less-massive, lower luminosity quasars that could be discovered by the {\em James Webb Space Telescope}, {\em Euclid} and the {\em Roman Space Telescope} in the coming decade. We also produce low-resolution versions of the maps and corresponding noise covariance matrices. peaks, on maps masked for diffuse Galactic emission and for strong unresolved Charged $D$ mesons are produced out-of-equilibrium at tens of MeV temperatures. In this paper, we combine the $\texttt{COSMIC}$ binary population synthesis suite and the $\texttt{CMC}$ code for globular cluster evolution to create a mixture model for black hole binary formation under both formation scenarios. ( , 1999, Padova: Alongi et al. We present a testable mechanism of low-scale baryogenesis and dark matter production in which neither baryon nor lepton number are violated. Our new simulations are well suited to interpret the observations of line emission from current (ALMA and HST) and upcoming facilities (JWST and ngVLA). The Planck results for base Lambda CDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. find no evidence for isocurvature perturbations or cosmic defects. As in the 2013 data release, our calibrator is provided by the spin-synchronous modulation of the cosmic microwave background dipole, but we now use the orbital component, rather than adopting the Wilkinson Microwave Anisotropy Probe (WMAP) solar dipole. We present a wide survey of scale-dependent feature and resonance models, accounting for the “look elsewhere” effect in estimating the statistical significance of features. NGC~4258. In this work, we study the extended viscous dark energy models in the context of matter perturbations. IV. We present the first searches using CMB polarization for correlations induced by a non-trivial topology with a fundamental domain intersecting, or nearly intersecting, the last scattering surface (at comoving distance $\chi_{rec}$). We present results based on full-mission Planck observations of temperature and polarization anisotropies of the CMB. measurements are in moderate (2-2.5 sigma) tension with model predictions. (Abridged). (2016) Planck 2015 results. The data, collected during 2015$-$2018 by the ATLAS experiment at the CERN LHC, correspond to an integrated luminosity of 139 fb$^{-1}$. From the observed stellar mass distribution, we rule out the hypothesis that FRBs strictly track stellar mass in galaxies (>99% c.l.). Using an overlap area of 206 square However, the cosmological parameters generating this pattern are in strong disagreement with those found from CMB anisotropy data alone. Gravitational lensing, Planck 2015 results. The matter density contrast evolves similarly to the $\Lambda$CDM model in high redshift, however in late-time is slightly different from the standard model. We run our algorithm on cosmological $N$-body simulations, from the AbacusCosmos suite, and reconstruct the initial positions of $\mathcal{O}(10^7)$ particles within a few hours with an off-the-shelf personal computer. are most robust and on which scales they return reliable estimates of the rate of growth of structure: we find that models Combining these galaxies with FRB hosts from the literature, we introduce criteria based on the probability of chance coincidence to define a subsample of 10 highly confident associations (at z = 0.03–0.52), 3 of which correspond to known repeating FRBs. Clusters in SDSS have typically higher alignment signal-to-noise than galaxies. and SN data into an "inverse distance ladder" yields a 1.7% measurement of We provide the DV(rsfid/rs) posterior probability distributions and their covariances. For the first time, these code bodies are combined self-consistently, with $\texttt{CMC}$ itself employing $\texttt{COSMIC}$ to track stellar evolution. studied as part of the Canadian Cluster Comparison Project. According to the current observational data (Riess, et al., 1998), (Perlmutter, et al., 1998), (Kowalski, et al., 2008), (Hicken, et al., 2009) . The Planck results for base ΛCDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. (1996Charbonnel et al. In polarization the systematic uncertainties are dominated by calibration uncertainties and compete with the CMB E-modes in the multipole range 10-20. XIII. We are grateful to the H-ATLAS Executive Committee and primarily to the PIs, S. Eales and L. Dunne, for permission to use the unpublished H-ATLAS catalogue for the validation of the present catalogue. However, as shown in Refs. In the case for a binary black hole (BBH) merger, the effective spin is likely negative and the effective precession spin is non-negligible. XI. Specific masks are defined to minimize foreground residuals and systematics. Combining Planck with tilt $n_s$ for the tensor-to-scalar ratio $r$ in slow-roll, single-field Models with early dark energy that tracks the dominant energy component at high Se pueden obtener soluciones phantom sin introducir grados de libertad fantasma, y el sistema autónomo contiene soluciones de expansión acelerada estables y atractores de Sitter. dominate the late-time evolution of our universe, cannot be addressed within Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w = -1.006 ± 0.045, consistent with the expected value for a cosmological constant. Combining BAO ... For the NSC model, delay times (t delay = t BBH + t insp ) are computed directly from the model and used to determine the merger redshift. 2017) is shown in orange, FSPS (Conroy et al. These results are within 1.5σ of the prediction of the flat-ΛCDM cosmology of Planck (2016). constraint. The LFI temperature data are limited by instrumental noise. Indeed, it has been found that the Planck data suffer from multiple internal inconsistencies that can potentially obscure the cosmological inference [4, ... VI. threshold effect on the Higgs quartic coupling due to the presence of the heavy The BH masses are broadly consistent with the relations between BH masses and host galaxy properties. We also perform a Bayesian search for a Bianchi VII$_h$ geometry. This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. (1998); Lançon & Mouhcine (2002); GENEVA: Schaller et al. Marginalizing over XXI. (1997a,b, 2000, Cambridge STARS: Eggleton (1971); Pols et al. The positron fraction in cosmic rays was found to be a steadily increasing in XLVI. inflaton field plays an important role in keeping the electroweak vacuum We constrain the ratio The spatial curvature of our Universe is found to be very close to zero, with | ΩK | < 0.005. Both Finally, we estimate a merger rate of GW190426\_152155-like systems to be $59^{+137}_{-51}~{\rm Gpc}^{-3}~{\rm yr}^{-1}$. Combined with Planck angular acoustic scale they further imply a nearly flat universe. GW190426_152155 was recently reported as one of the 39 candidate gravitational wave (GW) events in \citet{2020arXiv201014527A}, which has an unusual source-frame chirp mass $\sim 2.4M_{\odot}$ and may be the first GW signal from a neutron star-black hole (NSBH) merger. We will use a boson mass of $10^{-22} \mathrm{eV}/\mathrm{c}^2$ in this paper. I. Overview of products and scientific results Planck Collaboration, et.al., 2016, A&A.., 594A, 1P ADS / astro-ph. We explore relativistic freeze-in production of scalar dark matter in gauged $B-L$ model, where we focus on the production of dark matter from the decay and annihilation of Standard Model (SM) and $B-L$ Higgs bosons. Spectral indices are calculated for sources with radio observations from the VLA and Giant Metrewave Radio Telescope (GMRT) at 325 MHz, with an average spectral slope of α = 0.59 ± 0.04. The lower frequencies (from 100 to 353 GHz) are calibrated using the time-variable cosmological microwave background dipole, which we call the orbital dipole. We speculate that these features could be footprints of the hierarchical merger scenario. The data show clear evidence of the BAO peak in different configurations, which appears more visible in the reduced 3PCF rather than in the connected one. inflationary models. Furthermore, this scenario is also capable of reheating the universe at The tightest result comes from the HFI-based τ posterior distribution using the maximum likelihood power spectrum estimator from EE data only, giving a value 0.055 ± 0.009. Using a CMB temperature of TCMB = 2.7255 ± 0.0006 K, it permits an independent measurement of the amplitude of the CMB solar dipole (3364.3 ± 1.5 μK), which is approximatively 1σ higher than the WMAP measurement with a direction that is consistent between the two experiments. We show that it is essential to consider multiple channels when interpreting gravitational-wave catalogs, as inference on branching fractions and physical prescriptions become biased when contributing formation scenarios are not considered or incorrect physical prescriptions are assumed. High Frequency Instrument data processing: Calibration and maps, Planck 2015 results. Several groups have identified an extended excess of gamma rays over the It also improves the constraining power of Planck, in particular with regard to small-scale foreground properties. To transfer this lepton asymmetry to the baryon asymmetry, the dark leptons scatter on additional dark-sector states charged under lepton and baryon number. This set of processes lead to stable particles (photons, positrons, anti-protons, and neutrinos among others) which travel for very long distances before reaching the detectors. Finally we present an alternative analysis which is similar to a We present the 8th Full Focal Plane simulation set (FFP8), deployed in support of the Planck 2015 results. XIV. upper limit of 0.56 eV on the summed mass of neutrino species, improving to There is substantial spatial variation in the spinning dust spectrum, with the emission peak (in Iν) ranging from below 20 GHz to more than 50 GHz. The inhomogeneous distribution of neutral hydrogen during the reionization process results in significant fluctuations Supercharged H$_2$ cooling leads to the formation of 1800 - 2800 \Ms\ primordial stars, with radiative feedback from the star halting accretion and setting its upper limit in mass. significance. The observations used in this work (1996Girardi et al. In this paper, we focus on the results of two previously performed simulations of cluster size halos with self-interacting dark matter and introduce a new function for the density profile of galaxy clusters, which can perfectly describe the result of these simulations. value of $H_0^{corr}=70.6\pm 2.6\ \mathrm{km\ s^{-1}\ Mpc^{-1}}$ when using the Fig. multipoles between $100< L <250$. second-order Taylor expansion of the simulated power spectrum. Our conclusion strengths the previous studies that the current tension on Hubble constant cannot be saved by a local void alone. In addition, precision measurements of the Cosmic Microwave Background (CMB), ... where h is the Hubble parameter today with value 0.678 ± 0.009, ... Also shown are the SuperCDMS [48] sensitivity projections for benchmarks (a) and (b) while (c) remains out of reach of SuperCDMS. First, we study the spin-orbit alignment of the inner binary following the approach outlined by Antonini et al. Finally, we interpret the limits in the particle physics scenarios incorporating heavy sterile neutrinos, left-right symmetry and R-parity violating supersymmetry. The galaxies in each mock catalogue have properties similar to those of the higher redshift galaxies measured No model reproduces the EDGES feature. We find DV = (1264 ± 25 Mpc)(rd/rd,fid) at z = 0.32 and DV = (2056 ± 20 Mpc)(rd/rd,fid) at z = 0.57. scale as an anchor (giving the standard ruler length) as an inverse distance ladder.