arXiv subjects

Maurice H. P. M. van Putten

Publications and source records attributed to Maurice H. P. M. van Putten.

At least 19 recordsLinked to original sources

arXiv2026

Cosmological Expansion with Global Phase Normalization by the Hubble Horizon

We argue that cosmological expansion is subject to a global phase normalization in the gravitational path integral, fixed by causal horizon boundary conditions rather than by local dynamics. In this formulation, the cosmological conformal factor is not a propagating degree of freedom but a global gauge variable fixed by the Hamiltonian constraint, rendering the conventional conformal-factor problem inapplicable. A de Sitter turning point $(q=-1)$ uniquely fixes the phase density $Λ= J$ as the leading order integrating factor when the horizon Clausius relation holds, where $J$ is the trace of the Schouten tensor of the cosmological background. We parameterize departures from equilibrium by a single variance parameter $β$ governing non-adiabatic background evolution over a Hubble time scale. The resulting Hubble expansion points to a phantom regime beyond $Λ$CDM without new degrees of freedom. It provides a natural origin for cosmological tensions expressed by cosmographic parameters, arising from global constraints that inhibit a stable de Sitter universe.

gr-qc↗

arXiv2026

Schwarzschild solution from a Raychaudhuri-Huygens relation

Null-congruences encode the causal structure of spacetime, describing a phase space of radiation channels, whose expansion scalar $θ$ satisfies the Raychaudhuri equation. In spherical symmetry, the expansion scalar of wave fronts of area $A=4πr^2$ satisfies $θ= A^\prime/A = 2/r$. About a mass $M$, this carries an encoding area $A_E = λφ\ell_p^2 = λR_g r \le A$ in a UV-IR consistent coupling $\ell_p^2= G\hbar/c^3$ to its Compton phase $φ= (mc/\hbar)r \propto 1/\hbar$. Here, $λ= 8π$ is fixed by the Newtonian limit at large distances and the saturation limit $A_E=A$ at horizon about $M$ based on the non-local extension of the equivalence principle in Rindler spacetime, without using the Einstein equations. In spherical symmetry, this recovers the Schwarzschild metric from a geometric embedding of $p=A_E/A$, which is directly observable in gravitational lensing. The result shows a non-thermal origin of the scaling dimension of two of gravitational phase space, previously derived based on the second law of thermodynamics by Bekenstein (1973), with possible implications for cosmological spacetime.

gr-qc↗

arXiv2026

Efficient searches of small signals across two-channel noisy data: a challenge in Big Data observations

Searching for novel small signals in noisy data is preferably pursued by correlation in two or more independently operating channels. Signals of potential interest exist in tails beyond $κσ$, where $κ$ denotes a multiple of the standard deviation $σ$ of the data. Since moving data is a major cost factor in Big Data analysis and heterogeneous computing more generally, efficiency may be optimized by restricting the correlations computation to the tails of two-channel data exceeding $κσ$. Already, a moderate value $κ\gtrsim2$ realizes a data-reduction by at least an order of magnitude. Here, we study this approach using a novel {\it Excess Probability Ratio} (EPR), correlating Boolean data resulting from tails beyond a cut-off $κσ$. We compare and rank EPR performance against conventional direct cross-correlation (DCC) and Pearson coefficient (PC), applicable to the original data with no cut-off. This benchmark is performed over different combinations of background noise Gaussian, Poisson and Uniform and signals Gaussian, Poisson, Uniform, Chirps and Sine waves. Results show performance of EPR to be comparable to that of PC, providing a new approach for significant improvements in efficiency with essentially no loss of sensitivity, relevant to the present era of Big Data observatories.

astro-ph.IM↗

arXiv2026

Parameter-free prediction of the asymptotic acceleration scale confirmed by weak lensing

The de Sitter transition scale $a_{dS}=cH$ to anomalous galaxy dynamics was previously derived from first principles based on the background Hubble expansion $H$ and the velocity of light $c$. It introduces a $C^0$-transition across $a_{dS}$, which is in tension with predictions of $Λ$CDM galaxy models at a significance of $6σ$. Tracing late-time cosmology, it predicted the deep-asymptotic acceleration scale $a_0^{th}\simeq 1.66\times 10^{-8}{\rm cm\,s^{-2}}$ without adjustable parameters based on $H$ and the deceleration parameter $q$. A recent weak-lensing determination of $a_0^{WL} = 1.63_{-0.20}^{+0.23}\times 10^{-8}{\rm cm\,s}^{-2}$ now provides an independent empirical test of this prediction. The agreement with the updated theoretical value $a_0^{th} = 1.63_{-0.14}^{+0.13}\times 10^{-8}{\rm cm\,s^{-2}}$ closes the logical chain between cosmology, galaxy dynamics, and asymptotic scaling. Unlike phenomenological fits to rotation curves, this result does not rely on tuning or baryonic modeling but follows directly from background cosmology. This parameter-free model suggests some further tests by galaxy surveys extending over a finite range of redshifts.

astro-ph.GA↗

arXiv2026

Is Dark Energy Increasing or Decreasing in the Late Universe?

The concordance cosmological model $Λ$CDM assumes dark energy to be a constant, consistent with early-time observations, evidenced by Planck-$Λ$CDM analyses. However, in the face of late-time tensions, the nature of dark energy remains a central open problem. Modern precision cosmology offers a potential new window in the $w(a){\rm CDM}$ framework, which provides a model-independent prescription for its unknown equation of state $w(a)$. A confrontation of $w(a){\rm CDM}$ with data generally constitutes a nonlinear inference problem. We find that $w_0w_a$ estimates posterior to a fully non-linear $w(a)$ analysis are stabilized by the {\it Baryon Acoustic Oscillation} (BAO) constraint on $c_M=Ω_{m,0}h^2$, inherited for instance from Planck-$Λ$CDM analysis of the CMB. It produces $w_0w_a$ estimates that are invariant under constraint-preserving variations in $Ω_{m,0}$. In contrast, the early-linearization $w_0w_a$CDM shows pronounced correlation with $Ω_{m,0}$ even when preserving $c_M$. We quantify this correlation resulting from the non-commutativity of $w_0w_a$ estimation and linearization in $w(a)$CDM. This discrepancy is demonstrated in controlled mock-data experiments. Applied to cosmic chronometer data, $w_0w_a$ estimates from correlation-free late linearization of $w(a)$CDM analysis favor $w_0<-1$, whereas $w_0w_a$CDM favors $w_0>-1$. If the correlation between $w_0$ and $Ω_{m,0}$ in $w_0w_a$CDM is interpreted as arising from linearization effects rather than a physical origin, application to DESI DR2 may shift $w_0$ downward, potentially extending to $w_0 < -1$, corresponding to increasing dark energy at the present epoch. Alternatively, if the correlation is of hitherto unseen physical origin, the $w_0w_a$CDM parametrization is self-consistent and no such correction to the DESI inference may be required.

astro-ph.CO↗

arXiv2026

Multimessenger Constraints on the Central Engine in SN 2023ixf: Neutron Star or Black Hole?

The physical trigger of core-collapse supernova (CC-SNe) is a central theme in modern surveys of the transient Universe. A multi-messenger approach may provide a unique window to CC-SNe produced by a newly born neutron star (NS) or black hole (BH). Here we apply joint electromagnetic-gravitational wave (EM-GW) analysis to the nearby event SN 2023ixf using a model-independent broadband search with a GW-energy detection threshold of a few times $10^{-5} M_\odot c^2$ for chirps and $10^{-2}$ $M_\odot c^2$ for noise-like emission below 1\,kHz. No joint LIGO Hanford-Livingston (H1-L1) signal associated with SN 2023ixf is observed over a 2.5 day window proceeding the first discovery. Together with EM photometric-spectroscopic data, we interpret this null result to indicate the absence of BH formation, in part by mass-scaling of the BH powering GW170817B following GW170817. This multi-messenger outcome supports, hereby, scenarios consistent with NS formation, consistent with a progenitor mass likely below $\sim 20 M_\odot$ estimated by EM interpretations.

astro-ph.HE↗

arXiv2025

Prospects for observing chiral symmetry breaking in lepton colliders

Weak interactions in neutron $β$-decay exhibit parity violation through the preferential emission of right-handed antineutrinos. We identify this symmetry breaking with a reduction of phase space due to the small neutrino mass. During a brief interval of momentum exchange, a small mass neutrino puts the emission process close to the bifurcation horizon of Rindler space, doubly covered by Minkowski space ${\cal M}$ as dictated by the Equivalence Principle of general relativity. In the limit of arbitrarily small mass, this two-sheet covering effectively collapses into a single sheet, reducing the dimension of Dirac spinors from four to two, leaving neutrinos single-handed. This predicts a similar reduction to single-handed particle states in electrons created at TeV energies, which may be tested with the planned linear leptonic colliders. If confirmed, right-handed small mass neutrinos are expected to exist at sufficiently low energies.

hep-ph↗

arXiv2025

Prospects for high-resolution probes of galaxy dynamics tracing background cosmology in MaNGA

Large-$N$ galaxy surveys offer unprecedented opportunities to probe weak gravitation in galaxy dynamics that may contain correlations tracing background cosmology. Of particular interest is the potential of finite sensitivities to the background de Sitter scale of acceleration $a_{dS}=cH$, where $H$ is the Hubble parameter and $c$ is the velocity of light. At sufficiently large $N$, this is possibly probed by ensemble-averaged ("stacked") rotation curves (RCs) at resolutions on par with present estimates of the Hubble parameter $H_0$. Here, we consider the prospect for studies using the large $N$ Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) at APO survey. In a first and preliminary step, we consider unbiased control of sub-sample size by consistency in the three Position Angles, $θ$ , from photometry and velocity fields of gas and stars by spectroscopy within $30^\circ$. In sub-samples of size $N=N_i(θ)$, the scatter in-the-mean $σ/\sqrt{N}$ is found to reach one percent levels, differentiated over inclination angle $i$ and $θ$. In regular propagation of uncertainties, this scatter contributes $κσ/\sqrt{N}$ to the standard error in-the-mean to the observable, where $κ$ is determined by the choice of observables. As a lower bound to scatter in stacked RCs, MaNGA hereby appears promising for high-resolution analysis of sensitivity to RCs to background cosmology, notably across a sharp $C^0$-transition (van Putten 2018) of Newtonian to anomalous dynamics across $a_{dS}$ and, further out, the baryonic Tully-Fisher relation. In turn, these markers provide a novel measurement of cosmological parameters.

astro-ph.CO↗

arXiv2024

On the Hubble expansion in a Big Bang quantum cosmology

The Hubble expansion of the Universe is considered in the classical limit of a Big Bang quantum cosmology. In an IR-consistent coupling to the the bare cosmological constant, we infer a dark energy as a relic of the Big Bang by loss of time-translation invariance on a Hubble time-scale. This dark energy is identified with the trace $J$ of the Schouten tensor permitting an analytic solution $H(z)$. Anchored by the {\em Baryonic Accoustic Oscillations}, $J$CDM predicts a Hubble constant $H_0=\sqrt{6/5}\,H_0^Λ$ alleviating $H_0$-tension between the Local Distance Ladder and $H_0^Λ$ in $Λ$CDM, whose dark energy $Λ$ is a constant. Emulated by $w(a)Λ$CDM, a CAMB analysis shows a $J$CDM fit to the {\em Planck} 2018 $C_l^{TT}$ power spectrum on par with $Λ$CDM with small positive curvature consistent with {\em Planck}-$Λ$CDM with no extra relativistic degrees of freedom. In late-time cosmology, $J$CDM is also consistent with the BAO recently measured by DESI. { $J$CDM offers a novel framework to address $H_0$-tension, predicting background quantities consistent with the uncertainties in BAO measurements and early-Universe observations.} It predicts a deceleration parameter $q_0\simeq-1$, that may be tested with upcoming low-redshift galaxy surveys.

astro-ph.CO↗

arXiv2024

Unveiling the central engine of core-collapse supernovae in the Local Universe: NS or BH?

The physical trigger powering supernovae following the core collapse of massive stars is believed to involve a neutron star (NS) or a black hole (BH), depending largely on progenitor mass. A potentially distinct signature is a long-duration gravitational wave (GW) burst from BH central engines by their ample energy reservoir $E_J$ in angular momentum, far more so than an NS can provide. A natural catalyst for this radiation is surrounding high-density matter in the form of a non-axisymmetric disk or torus. Here, we derive a detailed outlook on LVK probes of core-collapse supernovae CC-SNe during the present observational run O4 based on their event rate, an association with normal long GRBs and mass-scaling of GW170817B/GRB170817A. For BH central engines of mass $M$, GW170817B predicts a descending GW-chirp of energy ${\cal E}_{GW}\simeq 3.5\% M_\odot c^2 \left(M/M_0\right)$ at frequency $f_{GW}\lesssim 700\,{\rm Hz}\left(M_0/M\right)$, where $M_0\simeq 2.8\,M_\odot$. For a few tens of events per year well into the Local Universe within 50-100Mpc, probes at the detector-limited sensitivity are expected to break the degeneracy between their NS or BH central engines {by GW calorimetry.

astro-ph.HE↗

arXiv2024

A temperature scale of $1\sim2$ eV in the mass-radius relationship of white dwarfs of type DA

The mass-radius relationship of white dwarfs (WDs) is one of their defining characteristics, largely derived from electron degeneracy pressure. We present a model-independent study of the observed mass-radius relationship in WD binaries of \cite{Parsons_2017}, listing data over a broad temperature range up to about 60,000 K (5 eV). The data show an appreciable temperature sensitivity with pronounced intrinsic scatter (beyond measurement uncertainty) for the canonical He-models with proton-to-neutron ratio 1:1. We characterize temperature sensitivity by a temperature scale $T_0$ in model-agnostic power-law relations with temperature normalized radius. For low-mass WDs, the results identify a remarkably modest $T_0 = 1 \sim 2 $ eV. We comment on a potential interpretation for atmospheres insulating super-Eddington temperature cores from the sub-Eddington photospheres of low-mass WDs.

astro-ph.SR↗

arXiv2024

The Hubble parameter of the Local Distance Ladder from dynamical dark energy with no free parameters

Our cosmology contains Big Bang relic fluctuations by a loss of time-translation symmetry on a Hubble time scale. The contribution to the vacuum is identified with dynamical dark energy $Λ\simeq α_pΛ_0$ by an IR coupling $α_p\sim \hbar$ of the bare cosmological constant $Λ_0\sim\hbar^{-1}$ consistent with general relativity, where $\hbar$ is the Planck constant. Described by the trace $J=(1-q)H^2$ of the Schouten tensor derived from a path integral formulation with gauged global phase, the proposed $J$CDM takes us beyond the $Λ$CDM limit of frozen $J=Λ$. The Hubble constant $H_0$ in $J$CDM is effectively $\sqrt{6/5}$ times the {\em Planck} value in $Λ$CDM analysis of the CMB according to $H(z)=H_0\sqrt{1+(6/5)Ω_{M,0} Z_5(z) + Ω_{r,0}Z_6(z)}/(1+z)$, where $Z_n=(1+z)^n-1$ given densities of matter $Ω_{M,0}$ and radiation $Ω_{r,0}$. With no free parameters, $J$CDM hereby agrees with the Local Distance Ladder when satisfying the BAO measured by {\em Planck}. On this cosmological background, galaxies possess an essentially $C^0$-transition to anomalous dynamics due to reduced inertia below the de Sitter scale of acceleration $a_{dS}=cH$, where $c$ is the velocity of light. This is confirmed in SPARC over a 6$σ$ tension in $Λ$CDM galaxy models, pointing to ultra-light CDM of mass $m_Dc^2<3\times 10^{-21}$eV. Sensitivity to this cosmological background explains the JWST 'Impossible galaxies' at cosmic dawn by rapid gravitational collapse. We comment on an outlook on future confrontations with observations by {\em Euclid}.

astro-ph.CO↗

arXiv2024

Galaxy dynamics tracing quantum cosmology beyond $Λ$CDM below the de Sitter scale of acceleration

It is proposed that the baryonic Tully-Fisher relation (bTFR) and JWST 'Impossible galaxies' at cosmic dawn are unified in weak gravity by the trace $J$ of the Schouten tensor below the Sitter scale of acceleration $a_{dS}=cH$, where $c$ is the velocity of light and $H$ is the Hubble parameter. Across $a_{dS}$, $J$ parametrizes short-period galaxy rotation curves and fast gravitational collapse beyond the predictions of $Λ$CDM. The sensitivity of weak gravitation to $J=\frac{1}{6}R$ is derived in infrared gravitation from a consistent limit of quantum gravity, reducing to general relativity in the limit of a small Planck constant, where $R$ is Ricci scalar tensor. For the first time, it identifies the exact relation $a_0=c^2\sqrt{J}/2π$ of the Milgrom parameter across all redshifts, accounting for the bTFR and early galaxy formation accelerated by a factor $\sim J^{1/8}$. It predicts $a_0^\prime(0)<0$ at the present epoch.

gr-qc↗

arXiv2024

Slide FFT on a homogeneous mesh in wafer-scale computing

Searches for signals at low signal-to-noise ratios frequently involve the Fast Fourier Transform (FFT). For high-throughput searches, we here consider FFT on the homogeneous mesh of Processing Elements (PEs) of a wafer-scale engine (WSE). To minimize memory overhead in the inherently non-local FFT algorithm, we introduce a new synchronous slide operation ({\em Slide}) exploiting the fast interconnect between adjacent PEs. Feasibility of compute-limited performance is demonstrated in linear scaling of Slide execution times with varying array size in preliminary benchmarks on the CS-2 WSE. The proposed implementation appears opportune to accelerate and open the full discovery potential of FFT-based signal processing in multi-messenger astronomy.

eess.SP↗

arXiv2023

The Fast and Furious in JWST high-$z$ galaxies

Recent JWST surveys reveal a striking abundance of massive galaxies at cosmic dawn, earlier than predicted by $Λ$CDM. The implied speed-up in galaxy formation by gravitational collapse is reminiscent of short-period galaxy dynamics described by the baryonic Tully-Fisher relation. This may originate in weak gravitation tracking the de Sitter scale of acceleration $a_{dS}=cH$, where $c$ is the velocity of light and $H(z)\propto \left(1+z\right)^{3/2}$ is the Hubble parameter with redshift $z$. With no free parameters, this produces a speed-up in early galaxy formation by an order of magnitude with essentially no change in initial galaxy mass function. It predicts a deceleration parameter $q_0=1-\left( 2π/GAa_{dS}\right)^2 = -0.98\pm 0.5$, where $G$ is Newton's constant and $A=(47\pm6)M_\odot$\,(km/s)$^{-4}$ is the baryonic Tully-Fisher coefficient (McGaugh 2012). At $3σ$ significance, it identifies dynamical dark energy alleviating $H_0$-tension when combined with independent $q_0$ estimates in the Local Distance Ladder. Conclusive determination of $q_0=d\log(θ(z)H(z))/dz\left|_{z=0}\right.$ is expected from BAO angle $θ(z)$ observations by the recently launched {\em Euclid} mission.

astro-ph.CO↗

arXiv2023

A unit of information in black hole evaporation

Black holes evolve by evaporation of their event horizon. While this process is believed to be unitary, there is no consensus on the recovery of information in black hole entropy. A missing link is a unit of information in black hole evaporation. Distinct from Hawking radiation, we identify evaporation in entangled pairs by $\mathbb{P}^2$ topology of the event horizon consistent with the Bekenstein-Hawking entropy in a uniformly spaced horizon area, where $k_B$ denotes the Boltzmann constant. It derives by continuation of $\mathbb{P}^2$ in Rindler spacetime prior to gravitational collapse, subject to a tight correlation of the fundamental frequency of Quasi-Normal-Mode (QNM) ringing in gravitational and electromagnetic radiation. Information extraction from entangled pairs by detecting one over the surface spanned by three faces of a large cube carries a unit of information of $2\log3$ upon including measurement of spin.

hep-th↗

arXiv2023

Observational prospects of double neutrons star mergers and their multi-messenger afterglows: LIGO discovery power, event rates and diversity

The double neutron star (DNS) merger event GW170817 signifies the first multimessenger (MM) event with electromagnetic-gravitational (EM-GW) observations. LIGO-Virgo-KAGRA observational runs O4-5 promise to detect similar events and as yet unknown GW signals, which require confirmation in two or more detectors with comparable performance. To this end, we quantify duty cycles of comparable science quality of data in coincident H1L1-observations, further to seek consistent event rates of astrophysical transients in upcoming EM-GW surveys. Quite generally, discovery power scales with exposure time, sensitivity, and critically depends on the percentage of time when detectors operate at high quality. We quantify coincident duty cycles over a time-frequency domain $W\times B$, defined by segments of duration $W=8$s, motivated by a long-duration descending GW-chirp during GRB170817A, and the minimum detector noise over about $B=100-250\,$Hz. This detector yield factor satisfies $1\%-25 \%$ in S5-6 and O1-O3ab, significantly different from duty cycles of H1 and L1 individually with commensurable impact on consistency in event rates in EM-GW surveys. Significant gain in discovery power for signals whose frequency varies slowly in time may be derived from improving detector yield factors by deploying time-symmetric data analysis methods. For O4-5, these can yield improvements by factors up to $\mathcal{O}(10^5)$ relative to existing data and methods. Furthermore, the diversity of MM afterglows to DNS mergers may be greatest for systems similar to GW170817 but possibly less so for systems of substantially different mass such as GW190425. We summarize our findings with an outlook on EM-GW surveys during O4-5 and perspectives for next-generation GRB missions like THESEUS.

astro-ph.HE↗

arXiv2023

A bound on the cosmic opacity of unparticles from the CMB temperature

Unparticle cosmology gives an unconventional outlook on the dark sector of cosmology, increasingly challenging $Λ\mbox{CDM}$ by $H_0$-tension. This model derives from a finite temperature broken conformal symmetry of radiation, described by a non-radiative correction with unknown sign in energy density. This symmetry breaking has a sign ambiguity, in which corrections about the IR fixed point are normal or tachyonic. While the first has been ruled out in a recent study, the latter possesses a late-time temperature $T_c\simeq 4\,T_{CMB}$ associated with $Ω_{\cal U}\simeq 1$ ($Ω_{\cal U} \simeq 10^4 Ω_{CMB}$), where $T_{CMB}$ denotes the temperature of the Cosmic Microwave Background (CMB). Thus exposed to the enormous heat bath of unparticles, $T_{CMB}$ is constrained by the astronomical age of the Universe $T_{u,0}$. The relative temperature shift $ΔT/T$ in any heat exchange to the CMB is hereby limited to the uncertainty of a few percent in $T_{u,0}$. This bounds the effective cross-section of unparticles interactions with CMB photons to $σ_{γ\mathcal{U}} \lesssim 10^{-40}\ \mbox{m}^2=10^{-3}\ \mbox{nb}$. Assuming a standard cross-section across the broadband mass and energy spectrum of unparticles, a more stringent bound $σ_{γ\mathcal{U}} \lesssim 10^{-3}\,\mbox{pb}$ derives from COBE-FIRAS constraints on spectral distortions. The first is midway of photon-neutrino $σ_{γν}$ and photon-photon cross sections $σ_{γγ}$, the second is on par with $σ_{γν}$. These constraints put late-time unparticle cosmology, if present, at the edge of the standard model.

astro-ph.CO↗