German theoretical physicist

**306**PODCASTS**464**EPISODES**41m**AVG DURATION**5**WEEKLY NEW EPISODES**Sep 26, 2022**LATEST

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- InsurTechs Planck, Federato, CoverTree, Bamboo Connect With Investors Carrier Management - Sep 20, 2022
- Latest round of funding brings Planck’s total to $71m ReinsuranceNe.ws - Sep 20, 2022
- Planck Raises $23M in Funding FinSMEs - Sep 18, 2022
- Planck Raises $23M to Expand Cognitive Business Analytics Platform Insurance Innovation Reporter - Sep 16, 2022
- HTML5 prototype of “Block it” using Box2D in an Arcade way, powered by Phaser and written in TypeScript – Particle explosions and score Emanuele Feronato - Sep 15, 2022
- Hitting the Books: How to uncover the true nature of the multiverse Engadget - Sep 11, 2022
- [ASAP] Frequency-Dependent Dielectric Permittivity in Poisson–Nernst–Planck Model The Journal of Physical Chemistry B: Latest Articles (ACS Publications) - Aug 19, 2022
- AeroVironment Acquires Planck Aerosystems UAS VISION - Aug 19, 2022
- AeroVironment acquires Planck Aerosystems, a leading provider of advanced unmanned aircraft navigation solutions sUAS News â€“ The Business of Drones - Aug 18, 2022
- Planck's constant TheServerSide.com - Aug 16, 2022

Patchy reionization bias on the primordial gravitational wave signal: Better to be sure than sorry by Divesh Jain et al. on Monday 26 September One of the major goals of future cosmic microwave background (CMB) $B$-mode polarization experiments is the detection of primordial gravitational waves through an unbiased measurement of the tensor-to-scalar ratio $r$. Robust detection of this signal will require mitigating all possible contamination to the $B$-mode polarization from astrophysical origins. One such extragalactic contamination arises from the patchiness in the electron density during the reionization epoch. Along with the signature on CMB polarization, the patchy reionization can source secondary anisotropies on the CMB temperature through the kinetic Sunyaev-Zeldovich (kSZ) effect. To study this foreground impact, we use a physically motivated model of reionization to evaluate its contribution to the CMB $B$-mode polarization and temperature anisotropies for upcoming CMB missions. We show that the value of $r$ can bias towards a higher value if the secondary contribution from reionization is neglected. However, combining small-scale kSZ signal, large-scale $E$-mode polarization, and $B$-mode polarization measurements, we can put constraints on the patchiness in electron density during reionization and can mitigate its impact on the value of $r$. CMB missions such as CMB-S4 and PICO may experience a bias of $>0.17sigma$ which can go as high as $sim 0.73sigma$ for extreme reionization models allowed by the Planck and SPT CMB measurements. As future experiments target to measure $r$ at $5sigma$, this is likely to affect the measurement significance and hence possibly affect the claim of detection of $r$, if not mitigated properly by using joint estimations of different reionization observables. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.12672v1

Using the cosmological recombination radiation to probe early dark energy and fundamental constant variations by Luke Hart et al. on Monday 26 September The cosmological recombination radiation (CRR) is one of the guaranteed spectral distortion signals from the early Universe. The CRR photons from hydrogen and helium pre-date the last scattering process and as such allow probing physical phenomena in the pre-recombination era. Here we compute the modifications to the CRR caused by early dark energy models and varying fundamental constants. These new physics examples have seen increased recent activity in connection with the Hubble tension, motivating the exploratory study presented here. The associated CRR responses are spectrally-rich but the level of the signals is small. We forecast the possible sensitivity of future spectrometers to these effects. Our estimates demonstrate that the CRR directly depends to changes in the expansion history and recombination physics during the pre-recombination era. However, futuristic sensitivities are required for spectrometer-only constraints that are competitive with other cosmological probes. Nevertheless, measurements of the CRR can directly reach into phases that otherwise remain inaccessible, highlighting the potential these types of observations could have as a probe of the early Universe. A combination with ${it Planck}$ data further shows that a synergistic approach is very promising. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.12290v1

Excess of lensing amplitude in the Planck CMB power spectrum by Rahima Mokeddem et al. on Monday 26 September Precise measurements of the Planck cosmic microwave background (CMB) angular power spectrum (APS) at small angles have stimulated accurate statistical analyses of the lensing amplitude parameter $A_{L}$. To confirm if it satisfies the value expected by the flat-$Lambda$CDM concordance model, i.e. $A_{L} = 1$, we investigate the spectrum difference obtained as: the difference of the measured Planck CMB APS and the Planck best-fit $Lambda$CDM APS model. To know if this residual spectrum corresponds to statistical noise or if it has a hiden signature that can be accounted for with a larger lensing amplitude $A_{L} > 1$, we apply the Ljung-Box statistical test and find, with high statistical significance, that the spectrum difference is not statistical noise. This spectrum difference is then analysed in detail using simulated APS, based on the Planck $Lambda$CDM best-fit model, where the lensing amplitude is a free parameter. We explore different binnations of the multipole order ,$ell$, and look for the best-fit lensing amplitude parameter that accounts for the spectrum difference in a $chi^2$ procedure. We find that there is an excess of signal that is well explained by a $Lambda$CDM APS with a non-null lensing amplitude parameter $A_{lens}$, with values in the interval $[0.10,0.29]$ at 68% confidence level. Furthermore, the lensing parameter in the Planck APS should be $1 + A_{lens} > 1$ at $sim 3 sigma$ of statistical confidence. Additionally, we perform statistical tests that confirm the robustness of this result. Important to say that this excess of lensing amplitude, not accounted in the Planck's flat-$Lambda$CDM model, could have an impact on the theoretical expectation of large-scale structures formation once the scales where it was detected correspond to these matter clustering processes. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.11660v1

New cosmological constraints on f T gravity in the light of full Planck-CMB and type Ia Supernovae data by Suresh Kumar et al. on Sunday 25 September We investigate two new observational perspectives in the context of torsional gravitational modification of general relativity, i.e., the $f(T)$ gravity: i) We use Pantheon data of type Ia supernovae motivated by a time variation of the Newton's constant on the supernovae distance modulus relation, and find that a joint analysis with Baryon Acoustic Oscillations (BAO) and Big Bang Nucleosynthesis (BBN), i.e., Pantheon+BAO+BBN, provides constraints on the effective free parameter of the theory to be well compatible with the $Lambda$CDM prediction; ii) We present the framework of $f(T)$ gravity at the level of linear perturbations with the phenomenological functions, namely the effective gravitational coupling $mu$ and the light deflection parameter $Sigma$, which are commonly used to parameterize possible modifications of the Poisson equation relating the matter density contrast to the lensing and the Newtonian potentials, respectively. We use the available Cosmic Microwave Background (CMB) data sets from the Planck 2018 release to constrain the free parameters of the $f(T)$ gravity and $Lambda$CDM models. We find that CMB data, and its joint analyses with Pantheon and BAO data constrain the $f(T)$ gravity scenario to be practically indistinguishable from the $Lambda$CDM model. We obtain the strongest limits ever reported on $f(T)$ gravity scenario at the cosmological level. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.11131v1

A Deep Learning Approach to Infer Galaxy Cluster Masses from Planck Compton -y parameter maps by Daniel de Andres et al. on Wednesday 21 September Galaxy clusters are useful laboratories to investigate the evolution of the Universe, and accurately measuring their total masses allows us to constrain important cosmological parameters. However, estimating mass from observations that use different methods and spectral bands introduces various systematic errors. This paper evaluates the use of a Convolutional Neural Network (CNN) to reliably and accurately infer the masses of galaxy clusters from the Compton-y parameter maps provided by the Planck satellite. The CNN is trained with mock images generated from hydrodynamic simulations of galaxy clusters, with Planck's observational limitations taken into account. We observe that the CNN approach is not subject to the usual observational assumptions, and so is not affected by the same biases. By applying the trained CNNs to the real Planck maps, we find cluster masses compatible with Planck measurements within a 15% bias. Finally, we show that this mass bias can be explained by the well known hydrostatic equilibrium assumption in Planck masses, and the different parameters in the Y500-M500 scaling laws. This work highlights that CNNs, supported by hydrodynamic simulations, are a promising and independent tool for estimating cluster masses with high accuracy, which can be extended to other surveys as well as to observations in other bands. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.10333v1

Type Ia supernovae data with scalar-tensor gravity by Mario Ballardini et al. on Wednesday 21 September We study the use of type Ia supernovae (SNe Ia) in the context of scalar-tensor theories of gravity, taking as a working example induced gravity, equivalent to Jordan-Brans-Dicke theory. Winking at accurate and precision cosmology, we test the correction introduced by a time variation of the Newton's constant, predicted by scalar-tensor theories, on the SNe distance modulus relation. We find that for induced gravity the coupling parameter is constrained from $xi < 0.0095$ (95% CL) using Pantheon SNe data alone down to $xi < 0.00063$ (95% CL) in combination with {em Planck} data release DR3 and a compilation of baryon acoustic oscillations (BAO) measurements from BOSS DR12. In this minimal case the improvements in terms of constraints on the cosmological parameters coming from the addition of SNe data to cosmic microwave background (CMB) and BAO measurements is limited, $sim7%$ on the 95% CL upper bound on $xi$. Allowing for the value of the gravitational constant today to depart from the Newton constant, we find that the addition of SNe further tightens the constraints obtained by CMB and BAO data on the standard cosmological parameters and by 22% on the coupling parameter, i.e., $xi < 0.00064$ at 95% CL. We finally show that in this class of modified gravity models the use a prior on the absolute magnitude $M_B$ in combination with the Pantheon SNe sample leads to results which are very consistent with those obtained by imposing a prior on $H_0$, as happens for other {em early-type} models which accommodate a larger value of $H_0$ compared to the $Lambda$CDM results. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2112.15126v4

A reanalysis of the latest SH0ES data for H 0 : Effects of new degrees of freedom on the Hubble tension by Leandros Perivolaropoulos et al. on Tuesday 20 September We reanalyze the recently released SH0ES data for the determination of $H_0$. We focus on testing the homogeneity of the Cepheid+SnIa sample and the robustness of the results in the presence of new degrees of freedom in the modeling of Cepheids and SnIa. We thus focus on the four modeling parameters of the analysis: the fiducial luminosity of SnIa $M_B$ and Cepheids $M_W$ and the two parameters ($b_W$ and $Z_W$) standardizing Cepheid luminosities with period and metallicity. After reproducing the SH0ES baseline model results, we allow for a transition of the value of any one of these parameters at a given distance $D_c$ or cosmic time $t_c$ thus adding a single degree of freedom in the analysis. When the SnIa absolute magnitude $M_B$ is allowed to have a transition at $D_csimeq 50Mpc$ (about $160Myrs$ ago), the best fit value of the Hubble parameter drops from $H_{0}=73.04pm1.04,km,s^{-1},Mpc^{-1}$ to $H_0=67.32pm 4.64, km,s^{-1},Mpc^{-1}$ in full consistency with the Planck value. Also, the best fit SnIa absolute magnitude $M_B^>$ for $D>D_c$ drops to the Planck inverse distance ladder value $M_{B}^>=-19.43pm 0.15$ while the low distance best fit $M_B^

CHEX-MATE: pressure profiles of 6 galaxy clusters as seen by SPT and Planck by Filippo Oppizzi et al. on Tuesday 20 September Pressure profiles are sensitive probes of the thermodynamic conditions and the internal structure of galaxy clusters. The intra-cluster gas resides in hydrostatic equilibrium within the Dark Matter gravitational potential. However, this equilibrium may be perturbed, e.g. as a consequence of thermal energy losses, feedback and non-thermal pressure supports. Accurate measures of the gas pressure over the cosmic times are crucial to constrain the cluster evolution as well as the contribution of astrophysical processes. In this work we presented a novel algorithm to derive the pressure profiles of galaxy clusters from the Sunyaev-Zeldovich (SZ) signal measured on a combination of Planck and South Pole Telescope (SPT) observations. The synergy of the two instruments made it possible to track the profiles on a wide range of spatial scales. We exploited the sensitivity to the larger scales of the Planck High-Frequency Instrument to observe the faint peripheries, and the higher spatial resolution of SPT to solve the innermost regions. We developed a two-step pipeline to take advantage of the specifications of each instrument. We first performed a component separation on the two data-sets separately to remove the background (CMB) and foreground (galactic emission) contaminants. Then we jointly fitted a parametric pressure profile model on a combination of Planck and SPT data. We validated our technique on a sample of 6 CHEX-MATE clusters detected by SPT. We compare the results of the SZ analysis with profiles derived from X-ray observations with XMM-Newton. We find an excellent agreement between these two independent probes of the gas pressure structure. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09601v1

Searching for High-Energy Neutrino Emission from Galaxy Clusters with IceCube by R. Abbasi et al. on Monday 19 September Galaxy clusters have the potential to accelerate cosmic rays (CRs) to ultra-high energies via accretion shocks or embedded CR acceleration sites. CRs with energies below the Hillas condition will be confined within the cluster and will eventually interact with the intracluster medium (ICM) gas to produce secondary neutrinos and $gamma$ rays. Using 9.5 years of muon-neutrino track events from the IceCube Neutrino Observatory, we report the results of a stacking analysis of 1094 galaxy clusters, with masses $gtrsim 10^{14}$ (textup{M}_odot) and redshifts between 0.01 and $sim$1, detected by the {it Planck} mission via the Sunyaev-Zeldovich (SZ) effect. We find no evidence for significant neutrino emission and report upper limits on the cumulative unresolved neutrino flux from massive galaxy clusters after accounting for the completeness of the catalog up to a redshift of 2, assuming three different weighting scenarios for the stacking and three different power-law spectra. Weighting the sources according to mass and distance, we set upper limits at $90%$ confidence level that constrain the flux of neutrinos from massive galaxy clusters ($gtrsim 10^{14}$ (textup{M}_odot)) to be no more than $4.6%$ of the diffuse IceCube observations at 100~TeV, assuming an unbroken $E^{-2.5}$ power-law spectrum. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2206.02054v2

Natural Inflation with non minimal coupling to gravity in R^2 gravity under the Palatini formalism by M. AlHallak et al. on Monday 19 September Natural Inflation with non-minimal coupling (NMC) to gravity, embodied by a Lagrangian term $xi phi^2 R $, is investigated in the context of an extended gravity of the form $R+ alpha R^2$. The treatment is performed in the Palatini formalism. We discuss various limits of the model ``$alpha gg 1$'' and ``$alpha ll 1$'' in light of two scenarios of inflation: a ``Slow roll'' and a ``Constant roll'' scenario. By analyzing the observational consequences of the model, our results show a significant improvement regarding compatibility between the theoretical results of this model and the observational constraints from Planck 2018 and BICEP/Keck 2018, as exemplified by the tensor-to-scalar ratio and spectral index. Furthermore, a broader range for the parameter space of natural inflation is now compatible with the confidence contours of Planck & BICEP/Keck results. The joint effects of the contributions of both the NMC to gravity and the $alpha R^2$ make a significant improvement: $alpha R^2$ gravity influences scalar-tensor ratio values, whereas NMC to gravity has a more significant impact on the spectral index values. Contributions from both terms allow more previously excluded intervals to be included being compatible now with observational data. These conclusions about the roles of NMC to gravity and, particularly, the extended gravity remain mainly valid with a periodic NMC similar in form to the natural inflation potential. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2202.01002v3

The Gamma-ray Bursts fundamental plane correlation as a cosmological tool by M. G. Dainotti et al. on Monday 19 September Cosmological models and their corresponding parameters are widely debated because of the current discrepancy between the results of the Hubble constant, $H_{0}$, obtained by SNe Ia, and the Planck data from the Cosmic Microwave Background Radiation. Thus, considering high redshift probes like Gamma-Ray Bursts (GRBs) is a necessary step. However, using GRB correlations between their physical features to infer cosmological parameters is difficult because GRB luminosities span several orders of magnitude. In our work, we use a 3-dimensional relation between the peak prompt luminosity, the rest-frame time at the end of the X-ray plateau, and its corresponding luminosity in X-rays: the so-called 3D Dainotti fundamental plane relation. We correct this relation by considering the selection and evolutionary effects with a reliable statistical method, obtaining a lower central value for the intrinsic scatter, $sigma_{int}=0.18 pm 0.07$ (47.1 %) compared to previous results, when we adopt a particular set of GRBs with well-defined morphological features, called the platinum sample. We have used the GRB fundamental plane relation alone with both Gaussian and uniform priors on cosmological parameters and in combination with SNe Ia and BAO measurements to infer cosmological parameters like $H_{0}$, the matter density in the universe ($Omega_{M}$), and the dark energy parameter $w$ for a $w$CDM model. Our results are consistent with the parameters given by the $Lambda$CDM model but with the advantage of using cosmological probes detected up to $z=5$, much larger than the one observed for the furthest SNe Ia. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.08675v1

Planck ISW-lensing likelihood and the CMB temperature by Julien Carron et al. on Sunday 18 September We present a new Planck CMB lensing-CMB temperature cross-correlation likelihood that can be used to constrain cosmology via the Integrated Sachs-Wolfe (ISW) effect. CMB lensing is an excellent tracer of ISW, and we use the latest PR4 Planck data maps and lensing reconstruction to produce the first public Planck likelihood to constrain this signal. We demonstrate the likelihood by constraining the CMB background temperature from Planck data alone, where the ISW-lensing cross-correlation is a powerful way to break the geometric degeneracy, substantially improving constraints from the CMB and lensing power spectra alone. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07395v1

Multipole expansion for 21cm Intensity Mapping power spectrum: forecasted cosmological parameters estimation for the SKA Observatory by Maria Berti et al. on Sunday 18 September The measurement of the large scale distribution of neutral hydrogen in the late Universe, obtained with radio telescopes through the hydrogen 21cm line emission, has the potential to become a key cosmological probe in the upcoming years. We explore the constraining power of 21cm intensity mapping observations on the full set of cosmological parameters that describe the $Lambda$CDM model. We assume a single-dish survey for the SKA Observatory and simulate the 21cm linear power spectrum monopole and quadrupole within six redshift bins in the range $z=0.25-3$. Forecasted constraints are computed numerically through Markov Chain Monte Carlo techniques. We extend the sampler texttt{CosmoMC} by implementing the likelihood function for the 21cm power spectrum multipoles. We assess the constraining power of the mock data set alone and combined with Planck 2018 CMB observations. We include a discussion on the impact of extending measurements to non-linear scales in our analysis. We find that 21cm multipoles observations alone are enough to obtain constraints on the cosmological parameters comparable with other probes. Combining the 21cm data set with CMB observations results in significantly reduced errors on all the cosmological parameters. The strongest effect is on $Omega_ch^2$ and $H_0$, for which the error is reduced by almost a factor four. The percentage errors we estimate are $sigma_{Omega_ch^2} = 0.25%$ and $sigma_{H_0} = 0.16%$, to be compared with the Planck only results $sigma_{Omega_ch^2} = 0.99%$ and $sigma_{H_0} = 0.79%$. We conclude that 21cm SKAO observations will provide a competitive cosmological probe, complementary to CMB and, thus, pivotal for gaining statistical significance on the cosmological parameters constraints, allowing a stress test for the current cosmological model. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07595v1

RAPOC : the Rosseland and Planck opacity converter A user-friendly and fast opacity program for Python by Lorenzo V. Mugnai et al. on Sunday 18 September RAPOC (Rosseland and Planck Opacity Converter) is a Python 3 code that calculates Rosseland and Planck mean opacities (RPMs) from wavelength-dependent opacities for a given temperature, pressure, and wavelength range. In addition to being user-friendly and rapid, RAPOC can interpolate between discrete data points, making it flexible and widely applicable to the astrophysical and Earth-sciences fields, as well as in engineering. For the input data, RAPOC can use ExoMol and DACE data, or any user-defined data, provided that it is in a readable format. In this paper, we present the RAPOC code and compare its calculated Rosseland and Planck mean opacities with other values found in the literature. The RAPOC code is open-source and available on Pypi and GitHub. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07535v1

This week, Gleaux steps into the DMB hotseat, joining Kyt_Kutcha for a discussion of all things PVP in Season of Plunder. We're talking scrimming, matchmaking, map rotation, hopes for the future, and - of course - breaking down the Seasonal Weapons, including Tarnished Mettle, Blood Feud, Brigand's Law, No Reprieve, Cry Mutiny, Planck's Stride, and Sailspy Pitchglass. Note: This episode was recorded early in the week, prior to the Quitting Penalty implementation and the map rotation weighting changes announced by Bungie on Thursday. Check out more from Gleaux on his Twitch and YouTube channels, and connect with his community in Discord: https://t.co/Ceq0tUDKeQ (discord.gg/krewe) BECOME A PATRON: https://www.patreon.com/massivebreakdownpodcast (https://www.patreon.com/massivebreakdownpodcast) PVE POD: https://pve-podcast-versus-enemies.captivate.fm/listen (https://pve-podcast-versus-enemies.captivate.fm/listen) STAR WARS POD: https://beneath-twin-suns.captivate.fm/listen (https://beneath-twin-suns.captivate.fm/listen) CHAT SERVER: https://discord.gg/TheyfeQ (https://discord.gg/TheyfeQ) HOME PAGE: https://destinymassivebreakdowns.com (https://destinymassivebreakdowns.com) YOUTUBE: https://www.youtube.com/channel/UCqCi3pvTA17HLRaow-K3U5w (https://www.youtube.com/channel/UCqCi3pvTA17HLRaow-K3U5w) Editing and Post Production by Nettie Smith.

Constraining Interacting Dark Energy Models from Future Generation PICO and DESI Missions by Albin Joseph et al. on Thursday 15 September The next-generation CMB satellite missions are expected to provide robust constraints on a wide range of cosmological parameters with unprecedented precision. But these constraints on the parameters could weaken if we do not attribute dark energy to a cosmological constant. The cosmological models involving interaction between dark energy and dark matter can give rise to comparable energy densities at the present epoch, thereby alleviating the so-called cosmic coincidence problem. In the present paper, we perform a forecast analysis to test the ability of the future generation high-sensitive Cosmic Microwave Background (CMB), and Baryon Acoustic Oscillation (BAO) experiments to constrain phenomenological interacting dark energy models. We consider cosmic variance limited future CMB polarization experiment PICO along with BAO information from the DESI experiment to constrain the parameters of the interacting dark sector. Based on the stability of the cosmological perturbations, we consider two possibilities for the interaction scenario. We investigate the impact of both the coupling constant and the equation of state parameter of dark energy on the CMB temperature power spectrum, matter power spectrum, and $fsigma_8$. We have used simulated temperature and polarization data from PICO within the multipole ranges ($ell = 2 - 4000$), and as expected, we do see PICO alone produces better constraints than Planck on the $Lambda$CDM parameters. With the integration of the PICO and DESI missions, we observe a significant improvement in the constraints on several cosmological parameters, especially the equation of state parameter of dark energy. However, we note that additional data is required to constrain a small positive coupling constant. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07167v1

Marginal Bayesian Statistics Using Masked Autoregressive Flows and Kernel Density Estimators with Examples in Cosmology by Harry Bevins et al. on Wednesday 14 September Cosmological experiments often employ Bayesian workflows to derive constraints on cosmological and astrophysical parameters from their data. It has been shown that these constraints can be combined across different probes such as Planck and the Dark Energy Survey and that this can be a valuable exercise to improve our understanding of the universe and quantify tension between multiple experiments. However, these experiments are typically plagued by differing systematics, instrumental effects and contaminating signals, which we collectively refer to as `nuisance' components, that have to be modelled alongside target signals of interest. This leads to high dimensional parameter spaces, especially when combining data sets, with > 20 dimensions of which only around 5 correspond to key physical quantities. We present a means by which to combine constraints from different data sets in a computationally efficient manner by generating rapid, reusable and reliable marginal probability density estimators, giving us access to nuisance-free likelihoods. This is possible through the unique combination of nested sampling, which gives us access to Bayesian evidences, and the marginal Bayesian statistics code MARGARINE. Our method is lossless in the signal parameters, resulting in the same posterior distributions as would be found from a full nested sampling run over all nuisance parameters, and typically quicker than evaluating full likelihoods. We demonstrate our approach by applying it to the combination of posteriors from the Dark Energy Survey and Planck. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2207.11457v2

Determining the Hubble Constant without the Sound Horizon: A 3 6 % Constraint on H 0 from Galaxy Surveys, CMB Lensing and Supernovae by Oliver H. E. Philcox et al. on Wednesday 14 September Many theoretical resolutions to the so-called "Hubble tension" rely on modifying the sound horizon at recombination, $r_s$, and thus the acoustic scale used as a standard ruler in the cosmic microwave background (CMB) and large scale structure (LSS) datasets. As shown in a number of recent works, these observables can also be used to compute $r_s$-independent constraints on $H_0$ by making use of the horizon scale at matter-radiation equality, $k_{rm eq}$, which has different sensitivity to high redshift physics than $r_s$. As such, $r_s$- and $k_{rm eq}$-based measurements of $H_0$ (within a $Lambda$CDM framework) may differ if there is new physics present pre-recombination. In this work, we present the tightest constraints on the latter from current data, finding $H_0=64.8^{+2.2}_{-2.5}$ at 68% CL (in $mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$ units) from a combination of BOSS galaxy power spectra, Planck CMB lensing, and the newly released Pantheon+ supernova constraints, as well as physical priors on the baryon density, neutrino mass, and spectral index. The BOSS and Planck measurements have different degeneracy directions, leading to the improved combined constraints, with a bound of $H_0 = 67.1^{+2.5}_{-2.9}$ ($63.6^{+2.9}_{-3.6}$) from BOSS (Planck) alone. The results show some dependence on the neutrino mass bounds, with the constraint broadening to $H_0 = 68.0^{+2.9}_{-3.2}$ if we instead impose a weak prior on $sum m_nu$ from terrestrial experiments, or shifting to $H_0 = 64.6pm2.4$ if the neutrino mass is fixed to its minimal value. Even without dependence on the sound horizon, our results are in $approx 3sigma$ tension with those obtained from the Cepheid-calibrated distance ladder, which begins to cause problems for new physics models that vary $H_0$ by changing acoustic physics or the expansion history immediately prior to recombination. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2204.02984v4

Fredrik snackar med Daniel som berättar allt om sitt tangentbordsbygge HS22K och vägen som ledde dit. Från stora och ganska vanliga tangentbord via Colemak och Planck hela vägen till att designa sitt eget kretskort och skriva en väldigt stor del av koden som driver det hela. Plus givetvis att gradvis komma fram till en behaglig tangentbordslayout med så lite som 22 tangenter. Ett stort tack till Cloudnet som sponsrar vår VPS! Har du kommentarer, frågor eller tips? Vi är @kodsnack, @tobiashieta, @oferlund, och @bjoreman på Twitter, har en sida på Facebook och epostas på info@kodsnack.se om du vill skriva längre. Vi läser allt som skickas. Gillar du Kodsnack får du hemskt gärna recensera oss i iTunes! Du kan också stödja podden genom att ge oss en kaffe (eller två!) på Ko-fi, eller handla något i vår butik. Länkar Kodsnack fyller tio - kom och fira med oss! Spelsylt #7 Indio studios Daniel HS22K - Daniels tangentbord Cherry mx blue Ben Vallack Planck Let's split Colemak Kyria Nice nano v2 ZMK Daniels layout Nice 60 Oryx Magnet Kicad Kailh choc-switchar Splitkb Work louder-tangenter Programming on 34 keys Titlar Ett konstigt tangentbord 22,5 grader Vad är tanken med tangentbordet? Skriva på ett rimligt sätt på ett tangentbord För att komma upp ska man gå rakt Fyra tangenter i mitten Hur många tangenter behöver jag? Då kan jag väl göra ett tangentbord Viljan att skriva allt från scratch Mentalt är det tre rader

Constraining the physics of star formation from CIB-cosmic shear cross-correlations by Baptiste Jego et al. on Tuesday 13 September Understanding the physics of star formation is one of the key problems facing modern astrophysics. The Cosmic Infrared Background (CIB), sourced by the emission from all dusty star-forming galaxies since the epoch of reionisation, is a complementary probe to study the star formation history, as well as an important extragalactic foreground for studies of the Cosmic Microwave Background (CMB). Understanding the physics of the CIB is therefore of high importance for both cosmology and galaxy formation studies. In this paper, we make high signal-to-noise measurements of the cross-correlation between maps of the CIB from the Planck experiment, and cosmic shear measurements from the Dark Energy Survey and Kilo-Degree Survey. Cosmic shear, sourced mainly by the weak gravitational lensing of photons emitted by background galaxies, is a direct tracer of the matter distribution, and thus we can use its cross-correlation with the CIB to directly test our understanding of the link between the star formation rate (SFR) density and the matter density. We use our measurements to place constraints on a halo-based model of the SFR that parametrises the efficiency with which gas is transformed into stars as a function of halo mass and redshift. These constraints are enhanced by combining our data with model-independent measurements of the bias-weighted SFR density extracted from the tomographic cross-correlation of galaxies and the CIB. We are able to place constraints on the peak efficiency at low redshifts, $eta=0.445^{+0.055}_{-0.11}$, and on the halo mass at which this peak efficiency is achieved today $log_{10}(M_1/M_odot) = 12.17pm0.25$. Our constraints are in excellent agreement with direct measurements of the SFR density, as well as other CIB-based studies. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.05472v1

Measuring cosmic filament spin with the kinetic Sunyaev-Zel'dovich effect by Yi Zheng et al. on Monday 12 September The spin of intergalactic filaments has been predicted from simulations, and supported by tentative evidence from redshift-space filament shapes in a galaxy redshift survey: generally, a filament is redshifted on one side of its axis, and blueshifted on the other. Here, we investigate whether filament spins could have a measurable kinetic Sunyaev-Zel'dovich (kSZ) signal, from CMB photons scattering off of moving ionized gas; this pure velocity information is rather complementary to filament redshift-space shapes. We develop a technique to measure the kSZ dipole by combining galaxy redshift surveys with CMB experiments. We base our S/N analyses first on an existing filament catalogue, making simple assumptions about how ionised gas follows the galaxies and matter in each filament, and its combination with Planck data. We then investigate the detectability of the kSZ dipole using the combination of DESI or SKA-2 with next-stage CMB experiments. We find that the gas halos of filament galaxies co-rotating with filaments induce a stronger kSZ dipole signal than that from the diffuse filamentary gas, but both signals seem too small to detect in near-term surveys such as DESI+future CMB experiments. But the combination of SKA-2 with future CMB experiments could give a more than $10sigma$ detection. The gain comes mainly from an increased area overlap and an increased number of filaments, but also the low noise and high resolution in future CMB experiments are important to capture signals from filaments small on the sky. Successful detection of the signals may help to find the gravitomagnetic effect in large-scale structure and advance our understanding on baryons in the cosmic web. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04464v1

Bernard Haisch, Ph.D., is an astrophysicist and author of over 130 scientific publications. He served as a scientific editor of the Astrophysical Journal for ten years, and was Principal Investigator on several NASA research projects. After earning his Ph.D. from the University of Wisconsin in Madison, Haisch did postdoctoral research at the Joint Institute for Laboratory Astrophysics, University of Colorado at Boulder and the University of Utrecht, the Netherlands. His professional positions include Staff Scientist at the Lockheed Martin Solar and Astrophysics Laboratory; Deputy Director of the Center for Extreme Ultraviolet Astrophysics at the University of California, Berkeley; and Visiting Scientist at the Max? Planck?Institut fuer Extraterrestrische Physik in Garching, Germany. He was also Editor?in?Chief of the Journal of Scientific Exploration. Prior to his career in astrophysics, Haisch attended the Latin School of Indianapolis and the St. Meinrad Seminary as a student for the Catholic priesthood. His first book, The God Theory, received excellent reviews. - www.warwickassociates.net******************************************************************To listen to all our XZBN shows, with our compliments go to: https://www.spreaker.com/user/xzoneradiotv*** AND NOW ***The ‘X' Zone TV Channel on SimulTV - www.simultv.comThe ‘X' Chronicles Newspaper - www.xchroniclesnewpaper.com

Full-shape BOSS constraints on dark matter interacting with dark radiation and lifting the S 8 tension by Henrique Rubira et al. on Sunday 11 September In this work we derive constraints on interacting dark matter-dark radiation models from a full-shape analysis of BOSS-DR12 galaxy clustering data, combined with Planck legacy cosmic microwave background (CMB) and baryon acoustic oscillation (BAO) measurements. We consider a set of models parameterized within the effective theory of structure formation (ETHOS), quantifying the lifting of the $S_8$ tension in view of KiDS weak-lensing results. The most favorable scenarios point to a fraction $fsim 10-100%$ of interacting dark matter as well as a dark radiation temperature that is smaller by a factor $xisim 0.1-0.15$ compared to the CMB, leading to a reduction of the tension to the $sim 1sigma$ level. The temperature dependence of the interaction rate favored by relaxing the $S_8$ tension is realized for a weakly coupled unbroken non-Abelian $SU(N)$ gauge interaction in the dark sector. To map our results onto this $SU(N)$ model, we compute higher-order corrections due to Debye screening. We find a lower bound $alpha_dequiv g_d^2/(4pi)gtrsim 10^{-8} (10^{-9})$ for dark matter mass $1000 (1)$ GeV for relaxing the $S_8$ tension, consistent with upper bounds from galaxy ellipticities and compatible with self-interactions relevant for small-scale structure formation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03974v1

Dark Energy Survey Year 3 results: cosmology with moments of weak lensing mass maps by M. Gatti et al. on Sunday 11 September We present a cosmological analysis using the second and third moments of the weak lensing mass (convergence) maps from the first three years of data (Y3) data of the Dark Energy Survey (DES). The survey spans an effective area of 4139 square degrees and uses the images of over 100 million galaxies to reconstruct the convergence field. The second moment of the convergence as a function of smoothing scale contains information similar to standard shear 2-point statistics. The third moment, or the skewness, contains additional non-Gaussian information. The data is analysed in the context of the $Lambda$CDM model, varying 5 cosmological parameters and 19 nuisance parameters modelling astrophysical and measurement systematics. Our modelling of the observables is completely analytical, and has been tested with simulations in our previous methodology study. We obtain a 1.7% measurement of the amplitude of fluctuations parameter $S_8equiv sigma_8 (Omega_m/0.3)^{0.5} = 0.784pm 0.013$. The measurements are shown to be internally consistent across redshift bins, angular scales, and between second and third moments. In particular, the measured third moment is consistent with the expectation of gravitational clustering under the $Lambda$CDM model. The addition of the third moment improves the constraints on $S_8$ and $Omega_{rm m}$ by $sim$15% and $sim$25% compared to an analysis that only uses second moments. We compare our results with {it Planck} constraints from the Cosmic Microwave Background (CMB), finding a $2.2$ textendash $2.8sigma$ tension in the full parameter space, depending on the combination of moments considered. The third moment independently is in $2.8sigma$ tension with {it Planck}, and thus provides a cross-check on analyses of 2-point correlations. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2110.10141v2

Constraining the growth rate of structure with redshift space distortions including the wide-angle effect by Yan Lai et al. on Sunday 11 September We introduce an improved method for constraining the growth rate of structure with the galaxy overdensity and peculiar velocity power spectrum. This method reduces the modelling systematic error by accounting for the wide-angle effect and the zero-point calibration uncertainty during the modelling process. We also speed up the posterior sampling by around 30 times by first calculating the likelihood at a small number of fiducial points and then interpolating the likelihood values during MCMC sampling. We test the new method on mocks and we find it is able to recover the fiducial growth rate of structure. We applied our new method to the SDSS PV catalogue, which is the largest single peculiar velocity catalogue to date. Our constraint on the growth rate of structure is $fsigma_8= 0.405_{-0.071}^{+0.076}$ (stat) $pm$ 0.009 (sys) at the effective redshift of 0.073. Our constraint is consistent with a Planck 2018 cosmological model, $fsigma_8$ = 0.448, within one standard deviation. Our improved methodology will enable similar analysis on future data, with even larger sample sizes and covering larger angular areas on the sky. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04166v1

Universal scaling laws and density slope for dark matter halos from rotation curves and energy cascade by Zhijie Xu. on Thursday 08 September Smalls scale challenges suggest some missing pieces in our current understandings of dark matter. A cascade theory for dark matter flow is proposed to provide extra insights, similar to the cascade in hydrodynamic turbulence. The energy cascade from small to large scales with a constant rate $varepsilon_u$ ($approx -4.6times 10^{-7}m^2/s^3$) is a fundamental feature of dark matter flow. Energy cascade leads to a two-thirds law for kinetic energy $v_r^2$ on scale $r$ such that $v_r^2 propto (varepsilon_u r)^{2/3}$, as confirmed by N-body simulations. This is equivalent to a four-thirds law for mean halo density $rho_s$ enclosed in the scale radius $r_s$ such that $rho_s propto varepsilon_u^{2/3}G^{-1}r_s^{-4/3}$, as confirmed by data from galaxy rotation curves. By identifying relevant key constants, critical scales of dark matter might be obtained. The largest halo scale $r_l$ can be determined by $-u_0^3/varepsilon_u$, where $u_0$ is the velocity dispersion. The smallest scale $r_{eta}$ is dependent on the nature of dark matter. For collisionless dark matter, $r_{eta} propto (-{Ghbar/varepsilon_{u}}) ^{1/3}approx 10^{-13}m$, where $hbar$ is the Planck constant. A uncertainty principle for momentum and acceleration fluctuations is also postulated. For self-interacting dark matter, $r_{eta} propto varepsilon_{u}^2 G^{-3}(sigma/m)^3$, where $sigma/m$ is the cross-section. On halo scale, the energy cascade leads to an asymptotic slope $gamma=-4/3$ for fully virialized halos with a vanishing radial flow, which might explain the nearly universal halo density. Based on the continuity equation, halo density is analytically shown to be closely dependent on the radial flow and mass accretion such that simulated halos can have different limiting slopes. A modified Einasto density profile is proposed accordingly. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03313v1

A grounded perspective on New Early Dark Energy using ACT, SPT, and BICEP Keck by Juan S. Cruz et al. on Wednesday 07 September We examine further the ability of the New Early Dark Energy model (NEDE) to resolve the current tension between the Cosmic Microwave Background (CMB) and local measurements of $H_0$ and the consequences for inflation. We perform new Bayesian analyses, including the current datasets from the ground-based CMB telescopes Atacama Cosmology Telescope (ACT), the South Pole Telescope (SPT), and the BICEP/Keck telescopes, employing an updated likelihood for the local measurements coming from the S$H_0$ES collaboration. Using the S$H_0$ES prior on $H_0$, the combined analysis with Baryonic Acoustic Oscillations (BAO), Pantheon, Planck and ACT improves the best-fit by $Deltachi^2 = -15.9$ with respect to $Lambda$CDM, favors a non-zero fractional contribution of NEDE, $f_{rm NEDE} > 0$, by $4.8sigma$, and gives a best-fit value for the Hubble constant of $H_0 = 72.09$ km/s/Mpc (mean $71.48_{-0.81}^{+0.79}$ with $68%$ C.L.). A similar analysis using SPT instead of ACT yields consistent results with a $Delta chi^2 = - 23.1$ over $Lambda$CDM, a preference for non-zero $f_{rm NEDE}$ of $4.7sigma$ and a best-fit value of $H_0=71.77$ km/s/Mpc (mean $71.43_{-0.84}^{+0.84}$ with $68%$ C.L.). We also provide the constraints on the inflation parameters $r$ and $n_s$ coming from NEDE, including the BICEP/Keck 2018 data, and show that the allowed upper value on the tensor-scalar ratio is consistent with the $Lambda$CDM bound, but, as also originally found, with a more blue scalar spectrum implying that the simplest curvaton model is now favored over the Starobinsky inflation model. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.02708v1

Multiwavelength Survey of Dark Globule DC 314 8-5 1: Point Source Identification and Diffuse Emission Characterization by E. Kosmaczewski et al. on Tuesday 06 September We present an analysis of the multi-wavelength observations of the dark globule, DC 314.8-5.1, using the optical survey Gaia, the near-infrared survey 2MASS, mid-infrared survey WISE along with dedicated imaging with the Spitzer Space Telescope, and finally X-ray data obtained with the Swift-XRT telescope. The main goal of this analysis was to identify possible pre-main sequence stars and young stellar objects (YSOs) associated with the globule. For this purpose, we studied the infrared colors of all point sources coinciding within the boundaries of the cloud, as inferred from the optical extinction maps. After removing the sources with spectra of non-stellar types, we investigated the Gaia parallaxes for the YSO candidates, finding that none of them are physically related to DC 314.8-5.1. In addition, we probed the presence of pre-main sequence stars lacking infrared counterparts with Swift-XRT, and found no candidates down to a luminosity level $lesssim 10^{31}$erg cm$^{-1}$ in the 0.5-10 keV range. Our detailed inspection of the gathered data confirm a very young, ``pre-stellar core'' evolutionary stage of the cloud. As such, DC 314.8-5.1 constitutes a compact reservoir of cold dust and gas, enabling for a truly unique insight into a primordial form of the interstellar medium. Based on the archival Planck and IRAS data, we identify the presence of a hot dust, with temperatures reaching even up to 200 K, in addition to the dominant dust component at 14 K. Finally, we comment on the mass estimates for the globule. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.02372v1

Radó von Kövesligethy, vor 160 Jahren geboren, gewann früh epochale Erkenntnisse über den Aufbau der Sterne. Dieser war damals noch völlig rätselhaft. Einige Jahre nach ihm formulierten die Physiker Wilhelm Wien und Max Planck seine Erkenntnisse neu. Von Dirk Lorenzenwww.deutschlandfunk.de, SternzeitDirekter Link zur Audiodatei

Richard Easther is a scientist, teacher, and communicator. He has been a Professor of Physics at the University of Auckland for over the last 10 years and was previously a professor of physics at Yale University. As a scientist, Richard covers ground that crosses particle physics, cosmology, astrophysics and astronomy, and in particular, focuses on the physics of the very early universe and the ways in which the universe changes between the Big Bang and the present day. In this episode, Richard and I discuss the details of cosmology at large, both technically and historically. We dive into Einstein's equations from general relativity and see what implications they have for an expanding universe alongside a discussion of the cast of characters involved in 20th century cosmology (Einstein, Hubble, Friedmann, Lemaitre, and others). We also discuss inflation, gravitational waves, the story behind Brian Keating's book Losing the Nobel Prize, and the current state of experiments and cosmology as a field. Originally published on May 3, 2022 on YouTube: https://youtu.be/DiXyZgukRmE Timestamps: 00:00:00 : Introduction 00:02:42 : Astronomy must have been one of the earliest sciences 00:03:57 : Eric Weinstein and Geometric Unity 00:13:47 : Outline of podcast 00:15:10 : Brian Keating, Losing the Nobel Prize, Geometric Unity 00:16:38 : Big Bang and General Relativity 00:21:07 : Einstein's equations 00:26:27 : Einstein and Hilbert 00:27:47 : Schwarzschild solution (typo in video) 00:33:07 : Hubble 00:35:54 : One galaxy versus infinitely many 00:36:16 : Olbers' paradox 00:39:55 : Friedmann and FRLW metric 00:41:53 : Friedmann metric was audacious? 00:46:05 : Friedmann equation 00:48:36 : How to start a fight in physics: West coast vs East coast metric and sign conventions. 00:50:05 : Flat vs spherical vs hyperbolic space 00:51:40 : Stress energy tensor terms 00:54:15 : Conversation laws and stress energy tensor 00:58:28 : Acceleration of the universe 01:05:12 : Derivation of a(t) ~ t^2/3 from preceding computations 01:05:37 : a = 0 is the Big Bang. How seriously can we take this? 01:07:09 : Lemaitre 01:11:51 : Was Hubble's observation of an expanding universe in 1929 a fresh observation? 01:13:45 : Without Einstein, no General Relativity? 01:14:45 : Two questions: General Relativity vs Quantum Mechanics and how to understand time and universe's expansion velocity (which can exceed the speed of light!) 01:17:58 : How much of the universe is observable 01:24:54 : Planck length 01:26:33 : Physics down to the Big Bang singularity 01:28:07 : Density of photons vs matter 01:33:41 : Inflation and Alan Guth 01:36:49 : No magnetic monopoles? 01:38:30 : Constant density requires negative pressure 01:42:42 : Is negative pressure contrived? 01:49:29 : Marrying General Relativity and Quantum Mechanics 01:51:58 : Symmetry breaking 01:53:50 : How to corroborate inflation? 01:56:21 : Sabine Hossenfelder's criticisms 02:00:19 : Gravitational waves 02:01:31 : LIGO 02:04:13 : CMB (Cosmic Microwave Background) 02:11:27 : Relationship between detecting gravitational waves and inflation 02:16:37 : BICEP2 02:19:06 : Brian Keating's Losing the Nobel Prize and the problem of dust 02:24:40 : BICEP3 02:26:26 : Wrap up: current state of cosmology Notes: Easther's blogpost on Eric Weinstein: http://excursionset.com/blog/2013/5/25/trainwrecks-i-have-seen Vice article on Eric Weinstein and Geometric Unity: https://www.vice.com/en/article/z3xbz4/eric-weinstein-says-he-solved-the-universes-mysteries-scientists-disagree Further learning: Matts Roos. "Introduction to Cosmology" Barbara Ryden. "Introduction to Cosmology" Our Cosmic Mistake About Gravitational Waves: https://www.youtube.com/watch?v=O0D-COVodzY

Steffen Schroeder: Planck oder Als das Licht seine Leichtigkeit verlor / Ralf Rothmann: Die Nacht unterm Schnee / Christian Baron: Schön ist die Nacht / Patrick Modiano: Unterwegs nach Chevreuse / Hörbuch: Hans Fallada: Lilly und ihr Sklave / Das literarische Rätsel

Host James Benham is joined by Leandro DalleMule from Planck. James & Leandro discuss data, analytics and intelligence and their importance in insurance.Find us on social media!We're on Twitter, Facebook, Instagram, and LinkedIn, or follow James on Twitter!Subscribe, rate, and comment.As always -Enjoy the Ride & Geek Out!

Heidi Planck disappeared on October 17, 2021 after attending her son's flag football game. Her dog, Seven, was found wandering alone in an apartment building where Heidi was last seen. Rumors continue to swirl about what happened to her, but she is still missing. https://www.the-sun.com/news/4249697/heidi-planck-missing-california-adderall-party-crypto-gambling/ https://ktla.com/news/6-months-later-search-continues-for-missing-mom-heidi-planck/ https://www.the-sun.com/news/4179498/hunter-biden-linked-fraudster-missing-heidi-plancks-boss/ #MMIW Dawn Walker and Vincent Jansen are missing https://thestarphoenix.com/news/local-news/dawn-walker-search-investigators-searching-cellphone-records-banking-history-of-woman-missing-with-son?utm_term=Autofeed&utm_medium=Social&utm_source=Facebook&fbclid=IwAR0_v4Ll4V_zRmivVI7RLL_uhFR4rq1t27oLyF0XopCsmbpltq-omTkh4UA#Echobox=1659470982 WTF News Dating a Serial Killer https://people.com/crime/former-girlfriend-of-hillside-strangler-killer-speaks-out/ SUBSCRIBE: https://www.youtube.com/channel/UCd85RJRW6kn51aM2un6ButA/featured *Social Media Links* Facebook: www.facebook.com/truecrimeparanormalTPS Facebook Discussion Group: https://www.facebook.com/groups/215774426330767 Website: https://www.truecrimeparanormalpodcast.com/ TikTok: https://www.tiktok.com/@truecrimeparanormal Our Latest Video: https://youtu.be/MM13G8BkD9s Check Out Some of Our Previous Uploads! Todd Kohlhepp, Julie Wheeler, Porn Easter Eggs https://youtu.be/Xj1ViE7x7YE Irene Wairimu Gakwa, Amerie Jo Garza, Nyzireya London Moore https://youtu.be/K9X145wQBp0 Anthony Todt, ConnerJack Oswalt, Shannon Miosek, Lisa Fracassi https://youtu.be/OWEA1-9FOY4 True Crime Paranormal on Spotify https://open.spotify.com/show/5gIPqBHJLftbXdRgs1Bqm1 True Crime Paranormal on Apple https://podcasts.apple.com/us/podcast/true-crime-paranormal/id1525438711?ls=1 Kristi's Crystal Shop https://www.ehcrystals.com/

On Episode 106, Eric and Josh zoom all the way in to the smallest scale of the universe with a discussion about Planck's Constant. Please send your questions, comments, corrections and hate mail to RidingTheTorusPod@gmail.com You can find Eric's research notes for every episode here: https://drive.google.com/folderview?id=1syBwRsJ3b3YnOlUCXXFEEUpgF0NODLL2 Also! If you enjoy the Riding The Torus theme song, you can now download it for FREE from the Bueno Tornado bandcamp page. Here is the link: http://buenotornado.bandcamp.com/track/riding-the-torus-theme Hosts: Eric Beal - twitter.com/ericbealart Josh Campbell - twitter.com/josh_campbell

Jim talks with James Owen Weatherall about his work on viewing general relativity as an effective field theory and where it should give way to another theory. General relativity does a very good job of describing the world we see in astronomical observations, but certain results, e.g. singularities, and certain limits, e.g. the Planck scale, hint that there should be another theory that supersedes it. Jim Weatherall argues that this is in a high curvature regime.Show Notes: http://frontiers.physicsfm.com/66

John Mather is an astrophysicist at NASA who has been involved in important space missions to probe our fundamental understanding of the Universe for over four decades. He helped lead the design and deployment of the Cosmic Background Explorer Satellite (COBE), which launched in 1989 to probe the cosmic microwave background radiation from the Big Bang with a precision that could not be obtained from terrestrial experiments because of absorption of radiation by the atmosphere. The experiments on COBE, and its successor missions WMAP and PLANCK, literally have turned cosmology from an art to a science, allowing the precise measurement of cosmological observables that previously were either not measured at all or only measured to within a factor of two. This has led to a golden age of cosmology, where theories of the early universe can now be compared directly to observation. John directed the building of the Far Infrared Absolute Spectrophotometer (FIRAS) on COBE which was able to show that the cosmic microwave background radiation was indeed an almost perfect ‘black body’ spectrum associated with a very well defined temperature of the Universe at a time of about 300,000 years after the big bang. Indeed, no terrestrial experiment has ever produced such an accurate black body spectrum, which was one of the fundamental predictions that helped develop quantum mechanics early in the 20th century. For his work on COBE, John shared the Nobel Prize with George Smoot. But John didn’t rest on his laurels, for several decades after COBE John helped lead the design and development of the James Webb Space Telescope, which recently launched and will probe both the very early universe and also extra solar planets, possibly helping us discover evidence for life elsewhere in the Universe. John and I talked about his origins in science, the science he has accomplished, and what his future plans are in a discussion that will help provide a valuable perspective for anyone on the current status of cosmology and astrophysics, as well as what we might learn in the future. The ad-free video is available for all paid subscribers to Critical Mass in an adjoining post.. Video with ads will be available on the Podcast YouTube Channel, and audio is also available wherever you listen to podcasts. Enjoy! Get full access to Critical Mass at lawrencekrauss.substack.com/subscribe