We present a timing and broadband spectral study of the AstroSat observation of the black hole low mass X-ray binary Swift J151857.0–572147, focusing on its evolution across two temporal segments, S1 and S2. During the first segment S1 lasting ∼ 50.6 ks, the source shows a clear type-C QPO at ∼8.02 Hz and a low-frequency bump (LFB) in the power density spectrum. By the later segment S2, the strength of the QPO feature decreases significantly and is no longer consistent with a coherent QPO, along with the simultaneous disappearance of the LFB. An energy-dependent analysis reveals that both the RMS amplitude and the time lag of the QPO in S1 increase monotonically with energy, suggesting a low inclination nature of the source. The QPO and LFB centroid frequencies show a strong positive correlation across orbital segments, with a Pearson coefficient of 0.98. Our variability analysis and hardness-intensity diagram reveal a spectral state transition of the source coincident with the turn-off of the QPO and the LFB, a conclusion supported by the evolution of broadband spectral parameters. Notably, the orbit-resolved spectral analysis reveals that the non-thermal parameters, photon index, and electron temperature of the corona exhibit significant deviation as the source traverses from S1 to S2, whereas the thermal parameters scatter without any systematic variation between the two segments. The simultaneous turn-off of the type-C QPO and the low-frequency broadband noise component, both originating from the hot inner flow, indicates a rapid reorganization of the inner accretion geometry. Our results strongly suggest a coronal origin for the QPO and demonstrate that the disappearance of both features reflects a substantial transformation of the Comptonizing region across the spectral transition.
The idea of a mirror AdS-dS transition induced by a rapidly sign-switching cosmological constant in the late universe forms the basis of the ΛsCDM model in general relativity. In this paper, we replace general relativity with minimal deviation Rastall gravity in a sign-switch dark energy model, and also investigate the significant cosmology parameters derived for the Rastall-ΛsCDM model at the background level. We evaluate this model using a comprehensive set of recent observational data, including DESI survey (Baryon Acoustic Oscillations), Type Ia Supernovae samples (PantheonPlus, DES5yr, SH0ES), and Planck (Cosmic Microwave Background). We find that the Rastall parameter ϵ constraint reveals only a 3.4σ departure from zero (GR-based ϵ=0) with an amplitude of order 10−3 from Pk18+DES5yr data, which departure remains statistically significant from a cosmological perspective within astrophysics. Compared to the GR-ΛsCDM model, the Rastall-based sign-switch model provides a tighter upper-bound constraint on z† with better-defined upper 1σ uncertainty from Pk18+DR2+DES5yr data. This model also alleviates the Hubble tension and S8 tension. Further, we performed model comparison using the Akaike Information Criterion (AIC), and Bayesian evidence. According to the AIC, the Rastall-ΛsCDM model provides a better statistical fit than the standard model for the Pk18+DR2 and Pk18+DR2+PP dataset combinations. However, we show that the Rastall-ΛsCDM model features moderate Bayesian evidence over the standard model only when the PantheonPlus Type Ia supernova sample is calibrated using Cepheid distance measurements from SH0ES.
In this study, we explore the gravitational baryogenesis mechanism within the context of f(Q) gravity, where Q is a non-metricity scalar. We consider a special case of this theory which demonstrate the universe spatially curved FRW model by considering a variable temporal function γ(t). For Underlying framework, we examine two distinct forms of f(Q) models: (i) f=αQm (power law form), (ii) f=αQ+βQ2 (quadratic polynomial). We also discuss the different cases of γ(t) for these two models. We investigate the baryon asymmetry by calculating the dimensionless ratio YB=ηBs, where ηB represents the baryon number density while s reflects the universe’s entropy density. We compare our theoretical predictions for the baryon-to-entropy ratio, YB, to the observed restriction of YB=9.42×10−11. Our numerical results confirm the experimentally known value, indicating that our modified gravitational framework may explain the observed baryon asymmetry in the cosmos.
In this investigation, we discuss a viable approach for constructing hybrid relativistic stellar structures using the non-metricity-inspired gravity model, rather than curvature corrections. To describe the distribution of quark matter in self-gravitational stellar fluids, we use the well-motivated MIT model. We model the radial metric potential through analytical approach which enables the viable generation of compact stars. However, the complexity-free constraint, which is characteristic of a compact star with uniform density and isotropic pressure, presents a straightforward gravitational scheme. Using this approach, we model the temporal metric potential. We apply an extensive examination of the profiles of physical variables, along with other necessary astrophysical constraints, to ensure that the relativistic model is physically sound. For this purpose, we used the radii and masses of different observed compact stellar configurations to ensure that the presented solution remains singular-free and stable. Therefore, the presented relativistic solution confirms its capability to describe the formation of hybrid stellar configurations within the framework of nonmetricity corrections. In addition, the reported findings highlight the potential of the nonmetricity-based gravitational framework to describe compact stars undergoing phase transitions and to offer new understandings of the consistency and interior structure of hybrid matter systems.
We present a new class of exact charged isotropic compact star solutions in the framework of f(Q, T) gravity, where the nonmetricity scalar Q is linearly coupled with the trace of the energy–momentum tensor T. The Einstein–Maxwell field equations are solved for a static, spherically symmetric interior by adopting physically motivated metric potentials, and the interior spacetime is smoothly matched to the exterior Reissner–Nordström geometry at the stellar boundary. The resulting solutions describe three families of configurations determined by the charge parameter N corresponding to 0 ≤ N < 1, N=1, and N > 1. Closed analytical expressions for the energy density, pressure, and electric charge are obtained and shown to satisfy all fundamental physical requirements for realistic compact stars, including regularity at the center, positive and monotonically decreasing thermodynamic quantities, causal sound speeds, and dynamical stability through the adiabatic index. The modified Tolman–Oppenheimer–Volkoff equation further confirms that equilibrium is maintained through the combined action of gravitational, hydrostatic, electric, and matter–geometry coupling forces. The coupling parameters σ1 and σ2 significantly influence the internal stiffness and compactness of the stellar configuration. The predicted mass–radius relations are consistent with observational constraints from massive neutron stars and gravitational-wave sources such as PSR J0437-4715, PSR J1012+5307, PSR J0740+6620, PSR J0952-0607, and the mass-gap event GW190814. In particular, the model allows Pulsars-like objects with radii in the range [11.3 km, 17.5 km] and GW190814-like objects with radii in the range [13.5 km, 17.2 km]. Among the three configurations, the case N < 1 tends to produce higher masses and smaller radii with increasing σ1, while the case N=1 permits comparatively larger radii as σ2 increases, and the case N > 1 provides an intermediate behaviour between these two limits. Overall, the results indicate that f(Q, T) gravity offers a flexible and physically consistent framework for modelling ultra-dense compact stars compatible with current astrophysical observations.
In this work, we investigated the modified emergent dark energy model using the baryon acoustic oscillation data from the Dark Energy Spectroscopic Instrument Data Release 2, together with CMB information from the LoLLiPoP (low-ℓ) and HiLLiPoP (high-ℓ) likelihoods based on the latest Planck NPIPE PR4 data release, along with the Planck PR4 lensing and ACT DR6 lensing likelihoods, as well as three different Type Ia supernova datasets (Pantheon + , DES-Dovekie, and Union3). Our analysis shows that the MEDE model remains largely consistent with the standard ΛCDM cosmology. Although the model allows small deviations from ΛCDM, the inclusion of SNe Ia datasets drives the parameters toward values consistent with the standard cosmological model within the 1σ level. In particular, the parameter α does not show any statistically significant deviation from α=0. We further find that the MEDE model does not significantly alleviate the current H0 and S8 tensions. The inferred values of H0 remain lower than the SH0ES measurement, while the sound horizon scale rd stays nearly unchanged compared to the ΛCDM prediction. Similarly, although the MEDE model predicts slightly lower values of S8, the reduction is not sufficient to ease the tension with weak-lensing observations. The evolution of the cosmological quantities closely follows that of ΛCDM, with deviations generally remaining below the 0.5σ level. Moreover, the CMB + DESI DR2 dataset combination favors a full phantom regime, whereas the inclusion of SNe Ia datasets shifts the evolution toward a full quintessence regime. Finally, the ΔχMAP2 and ΔAIC analyses indicate a slightly better fit of the MEDE model to the observational data, whereas the logarithmic Bayes factor shows inconclusive evidence in favour of the MEDE model over the ΛCDM model. Despite its overall consistency with the standard cosmological scenario, the MEDE model does not show the phantom-crossing behavior suggested by recent DESI DR2 observations.
Rapid growth of the multimessenger and multiwavelength astrophysics had led to an increasing number of observations of the same events with instruments with different point spread functions. In particular pointing instruments with good angular resolution are used to pin-point the source of poorly-localized alert. In case no clear detection of the source counterpart is reached, the interpretation of the results requires statistical analysis. We investigate two approaches using the probability density function of the alert: frequentist and Bayesian, as well as agnostic approach not using this information. We discuss the advantages and problems of all the methods, and compare their reliability and performance. We consider both a simple one-dimensional toy simulations and a realistic use case of full simulations of the follow-up of a gravitational wave event with gamma-ray telescopes. The performance of both frequentist and Bayesian approaches for weak signals is comparable and superior to the agnostic one.
We present a systematic X-ray spectral analysis of 27 giant radio galaxies (GRGs) using archival XMM-Newton and Chandra data. Roughly 44% of the sample show intrinsic absorption (NH,int≳1021cm−2), while several exhibit narrow Fe Kα emission lines with equivalent widths up to ∼ 570 eV. Soft X-ray features are also common, including thermal plasma emission (kT ∼ 0.2–0.8 keV) and ionized absorbers, in some cases consistent with high-velocity outflows. The photon indices are typically hard (median Γ ∼ 1.6), in line with radio-loud AGN. A comparison between nuclear X-ray luminosity and extended radio power shows that many sources host relatively strong X-ray cores compared to their lobes, pointing toward possible restarted nuclear activity. For 10 GRGs with published black hole masses, we explore preliminary relations with X-ray luminosity, Eddington ratio, and photon index. We find a positive trend between MBH and L2−10keV, while Eddington ratios show no clear dependence on mass. A tentative negative relation between λEdd and Γ hints at inefficient accretion, although confirmation will require larger samples. Overall, GRGs display diverse nuclear conditions and accretion states, supporting scenarios where obscuration, episodic or restarted activity, and low-efficiency accretion shape their long-term evolution.
We present a timing-based framework for interpreting braking-index measurements in young pulsars within a four-channel spin-down model that includes particle-wind, magnetic-dipole, mass-quadrupole, and current-quadrupole torques. In this formulation, the observed braking index is a torque-weighted average of the channel exponents, allowing equation-of-state-independent constraints on the torque fraction of a possible r-mode-like current-quadrupole component from timing data alone. For a positive, slowly varying secular model, the physically allowed range is 1 ≤ nobs ≤ 7. Within this domain, the lower and capped physical upper bounds on the k=7 torque fraction are f7,min=max[0,(nobs−5)/2] and f7,maxphys=min{1,max[0,(nobs−1)/6]}, respectively. These bounds are conditional on the non-negativity and slow secular evolution of the effective torque coefficients; if these assumptions are relaxed, a large braking index need not uniquely imply a current-quadrupole torque. Applying this bracket analysis to young pulsars with measured braking indices, we find that most sources do not require a gravitational-wave torque and can be explained by wind-plus-dipole electromagnetic spin-down. Sources with 3 < nobs < 5 require some higher-order contribution beyond the wind and dipole terms, but timing alone cannot uniquely identify this contribution as an r-mode torque. PSR J0537 - 6910 remains the most suggestive case: its large inter-glitch braking index approaches the n ≃ 7 limit, where the timing bounds are consistent, within the restricted positive secular model, with a strong current-quadrupole-like contribution. This interpretation is not unique, however, because vortex-creep and superfluid-recovery effects can generate similar effective inter-glitch braking behaviour without invoking gravitational-wave emission. We also translate the timing constraints into stellar-model-dependent r-mode amplitude bounds, braking-index-corrected characteristic ages, and gravitational-wave ranking metrics for continuous-wave searches with current and future detectors, including the reduction in sensitivity expected for glitch-limited semi-coherent searches.
We present PSRDISP, a novel approach to modeling deterministic and stochastic dispersive processes in pulsar timing datasets using high-precision epoch-wise dispersion measure (DM) estimates, with a Gaussian Process based approach. Unlike the conventional single-pulsar noise analysis methodology, which is applied to frequency-resolved times of arrival (ToAs) of pulses, this technique is applied to epoch-wise DMs which are derived from these ToAs. It can also be applied to wideband DMs measured simultaneously with wideband ToAs. Therefore, this framework provides a paradigm-agnostic approach to characterise single-pulsar dispersive processes. This method is expected to minimise the impact of achromatic red noise processes while characterising these dispersive effects. We substantiate the discussed technique with representative examples using simulated narrowband and wideband datasets with realistic noise injections. We found the recovery to be in close agreement with the injections, and agnostic to the estimation technique. Our method applies to pulsar timing experiments where precise, epoch-wise DM estimates are possible, such as the Indian Pulsar Timing Array. This technique can serve as a powerful diagnostic tool for validating single-pulsar noise analyses, which is crucial for precision pulsar timing experiments, such as Pulsar Timing Arrays.
We investigate the accretion dynamics produced by Bondi-Hoyle-Lyttleton (BHL) accretion onto a black hole with a global monopole by solving the general relativistic hydrodynamic (GRH) equations on a fixed global-monopole spacetime background. Using a controlled sequence of models, we reveal how the monopole parameters η and λ affect the shock-cone morphology formed around the black hole, the near-horizon density distribution, the variation of the mass-accretion rate, and the QPO-like timing signatures. The numerical results show that increasing the monopole deviation systematically transforms the narrow Schwarzschild-type shock cone into a broad bow-shock-like structure. During this process, the matter trapped inside the shock cone is redistributed over a wider angular region, and the accretion dynamics is strongly modified. The mass-accretion-rate evolution further reveals that strong monopole deviations enhance long-timescale variability, especially in the MOPO10 and MOPO12 models. The power spectral density (PSD) analysis, together with constrained Lorentzian fitting, shows the formation of coherent QPO-like modes. A 2:1 harmonic structure is found in the MOPO2 and MOPO4 models, a 3:2 resonance-like pair appears in the MOPO6 model, and strong low-frequency peaks are obtained in the highly deformed MOPO10 and MOPO12 models. These frequencies are scaled with the black-hole mass, and their relation to QPO frequencies observed from stellar-mass, intermediate-mass, and supermassive black-hole sources is discussed in detail. In particular, the 2:1 harmonic pairs obtained from MOPO2 and MOPO4 are compared with AGN QPO candidates, showing that the scaled masses fall within the supermassive black-hole range and are broadly consistent with the mass scales of narrow-line Seyfert galaxies such as 1H 0707-495 and ESO 113-G010. Our numerical results show that shock-cone morphology, accretion-rate variability, QPO coherence, and mass-scaled harmonic or resonant timing features provide important diagnostics for testing global-monopole gravity in black-hole accretion flows.
Hadronic stars and strange quark stars could coexist within the so-called two-families scenario. In this respect, hadronic matter and strange quark matter correspond to two distinct equilibrium phases described by two different equations of state. We perform here the first detailed Bayesian analysis that makes use of astrophysical and laboratory data in order to constrain the equations of state adopted within the two-families scenario for hadronic and strange quark matter. In particular, in hadronic matter we consider the possible formation of hyperons and delta resonances (beside nucleons) within a class of non linear relativistic mean field models and in quark matter we consider the possible formation of a color-superconducting phase within a bag-like model. Results of the analysis indicate that, while at present both scenarios remain compatible with the data, the comparison of the Bayesian evidences shows a preference for the two-families scenario relative to our purely hadronic one-family baseline. Evaluating whether the data similarly favor the two-families scenario over a one-family model that includes hybrid stars is left to future work. The strength of this preference depends on the adopted dataset: it is moderate when only the most conservative astrophysical constraints are used, and becomes strong once the small-radius object PSR J0614–3329, the light and compact object HESS J1731–347, and the heavy-ion-collision flow data are included. Specifically, the two-families framework naturally relieves the tension between the intermediate-density softness of the equation of state required by small-radius objects, and the high-density stiffness needed to support massive pulsars. Ultimately, future detections of even more massive compact objects, very compact ordinary-mass objects, or precise measurements of two distinct masses with the same radius, would particularly strengthen the preference for two distinct compact-star families.
We investigate late-Universe dynamics in which the dark matter component is described by axion particles. The proposed framework departs from the standard ΛCDM paradigm due to a small fraction of axions driving the system away from thermal equilibrium. We analyze the evolution of the axion energy density using both a kinetic and a classical field approach, yielding an identical macroscopic evolution equation for the dark matter density. We emphasize that the BGK parameter is introduced phenomenologically at the kinetic level and this does not supply an independent microscopic derivation. The present work therefore explores the phenomenological consequences of late-time, out-of-equilibrium axion production rather than claiming a completed microphysical model. The resulting scenario modifies ΛCDM dynamics in the late Universe (specifically at z ≲ 1), while asymptotically recovering the standard baseline at earlier cosmic epochs. We compare the theoretical predictions of our formulation against a comprehensive suite of late-Universe datasets. Our statistical analysis reveals that when the SH0ES local calibration is included, the collisional axion model becomes significantly favored over ΛCDM, yielding a best-fit Hubble constant of H0≃73kms−1Mpc−1. Ultimately, this cosmological scenario successfully accommodates local distance-ladder measurements while maintaining excellent agreement with Baryon Acoustic Oscillation data from the DESI Collaboration.
In this paper, the dynamical behavior of the accelerated expansion of the universe is studied within the framework of f(T) gravity by considering a well-motivated functional form of f(T). A specific form of the Hubble parameter is assumed, which under two different cases, leads to two distinct cosmological models expressed in terms of the redshift parameter H(z), providing insights into cosmic dynamics. These models are employed to explore the expansion history of the universe and the evolution of several cosmological parameters. Using Bayesian statistical techniques based on the χ^2-minimization method, the median values of the model parameters are determined for both the cosmic chronometer (CC) and the joint (CC + Pantheon) datasets. The evolution of the deceleration parameter, energy density, pressure and the equation of state parameter for dark energy is analyzed. Additionally, the validity of the energy conditions and the nature of the statefinder diagnostic are examined. The present age of the universe is also estimated for the proposed models.
Testing the ΛCDM model requires cosmological probes spanning the wide redshift interval between Type Ia Supernovae (SNe Ia, z ≲ 2.9) and the Cosmic Microwave Background (CMB, z ≈ 1100). Gamma-Ray Bursts (GRBs), observed up to redshift z=9.2, offer the opportunity to explore part of this regime. Here, we investigate how many GRBs are needed to become a useful cosmological probe capable of independently testing deviations from ΛCDM suggested by the recent DESI BAO observations. We develop forecasts based on the two-dimensional X-ray and optical Dainotti relations, between the luminosity at the end of the plateau phase and its rest-frame duration. Using simulated GRB samples constructed from the observed population, we evaluate the constraining power of GRBs on cosmological parameters within the wCDM and w0waCDM models, both independently and in combination with CMB observations. Our results show that GRB samples containing several tens to hundreds of well-characterized plateaus can already approach the precision currently achieved by CMB measurements on the Dark Energy (DE) Equation of State (EoS) parameter w. Particularly, a sample of ∼ 66 optical GRBs can reach a precision σw ≈ 0.47, comparable to that obtained from Planck within the wCDM framework. Such sample sizes are already attainable through machine-learning techniques that double the number of GRBs using inferred redshifts. These forecasts indicate that future GRB observations, when combined with next-generation transient missions and improved statistical techniques, will provide an independent high-redshift probe of cosmic expansion and will play an important role in testing the robustness of potential Dynamical DE signals suggested by other cosmological datasets.
The bright γ-ray blazar S5 1044+71 has been identified as showing very significant quasi-periodic oscillations in the Fermi-LAT data in recent studies, with a periodicity of about three years. With the completion of a new three-year γ-ray cycle, we aim to revisit the periodicity in Fermi-LAT data, and analyze all available multi-wavelength (MWL) data to search for possible correlations and time-lags. These observations will be used to test for the compatibility of the observed periodicity with a precessing jet from the supermassive black hole powering the blazar. We analyze data from Fermi-LAT (γ-rays), NuSTAR, Swift-XRT, and AstroSat-SXT (X-rays), Swift-UVOT, AstroSat-UVIT, ASAS-SN, ZTF, Pan-STARRS (ultraviolet and optical), and NEOWISE (infrared). In addition we present an analysis from historical observations from the Palomar and Pulkovo observations. Single-band spectral variability, MWL correlations, and cross-correlations are computed. We then model the Fermi-LAT light curve with a precessing jet model, providing constraints on the geometry of the system and providing the evolution of the Doppler factor with time. The latter is used as a geometrical constraint in the modeling of the MWL spectral energy distributions, to test whether they are compatible with the jet parameters inferred from the light curve study. We confirm previous claims on the existence of a periodic γ-ray signal in S5 1044+71. We detect significant spectral variability in γ-ray, X-rays, and optical/UV data. We detect significant correlation between low-energy (infrared/optical/ultraviolet) data and γ-rays, with a correlation index of about 1; the correlation between X-rays and γ-rays is milder, with a correlation index of about 0.3. We do not detect any significant time-lag between bands. The Fermi-LAT light curve is successfully fit by a precessing jet model. The fit to the spectral energy distributions indicate that S5 1044+71 is a typical blazar, in which the γ-ray emission is located beyond the broad-line region. The existence of a periodic γ-ray signal S5 1044+71 is confirmed. All the MWL observations we present in this work are consistent with the existence of a precessing relativistic jet from the supermassive black hole.
Studying the cross-correlation function between the soft and hard X-ray emission in Neutron Star Low Mass X-ray Binaries provides crucial insight into the structure and dynamics of the innermost accretion regions. In this work, we investigate the CCF of the Z-source GX 349+2 using an XMM-Newton observation. We noted that asymmetric CCFs with lags of a few hundred seconds between soft and hard band light curves in the horizontal branch, whereas CCFs remained symmetric in normal and flaring branches. We also performed a CCF study during the flux transition duration and observed lags of the order of a few tens to hundreds of seconds. Monte Carlo simulations were performed to assess the robustness of these CCFs, confirming their significance at a 95% confidence level. We propose that the observed hard lags arise from the readjustment of the boundary layer/coronal region located near the inner edge of the accretion disk. From the measured lags, we estimate the characteristic size of the boundary layer. We show that the observed lags could also be associated with the depletion timescale of the boundary layer with low viscosity.
We present three-dimensional hydrodynamical simulations of mergers between low-mass hybrid HeCO white dwarfs (WDs), offering new insights into the diversity of thermonuclear transients. Unlike previously studied mergers involving higher-mass HeCO WDs and CO WDs, where helium detonation often triggers core ignition, our simulations reveal incomplete helium shell detonations in comparable-mass, lower-mass WD pairs. The result is a faint, rapidly evolving transient driven by the ejection of intermediate-mass elements and radioactive isotopes such as $^{48}$Cr and $^{52}$Fe, without significant $^{56}$Ni production. These transients may be detectable in upcoming wide-field surveys and could account for a subset of faint thermonuclear supernovae. Long-term evolution of the merger remnant shows that high-velocity PG-1159-type stars might be formed through this scenario, similar to normal CO-CO white dwarf mergers. This work expands our understanding of white dwarf mergers and their implications for nucleosynthesis and stellar evolution.
The concordance cosmological model ΛCDM assumes dark energy to be a constant, consistent with early-time observations, evidenced by Planck-ΛCDM 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 into the nature of dark energy in the w(a)CDM framework, which provides a model-independent prescription for its unknown equation of state w(a). A confrontation of w(a)CDM with data generally constitutes a nonlinear inference problem. We find that w0wa estimates posterior to a fully non-linear w(a) analysis are stabilized by the Baryon Acoustic Oscillation (BAO) constraint on cM=Ωm,0h2, inherited for instance from Planck-ΛCDM analysis of the CMB. This implementation produces w0wa estimates that are invariant under constraint-preserving variations in Ωm,0. In contrast, the early-linearization w0waCDM shows pronounced correlation with Ωm,0 even when preserving cM. We quantify this correlation resulting from the non-commutativity of w0wa estimation and linearization in w(a)CDM. This discrepancy is demonstrated in controlled mock-data experiments. Applied to cosmic chronometer data, w0wa estimates from correlation-free late linearization of w(a)CDM analysis favor w0<−1, whereas w0waCDM favors w0>−1. If the correlation between w0 and Ωm,0 in w0waCDM is interpreted as arising from linearization effects rather than a physical origin, application to DESI DR2 may shift w0 downward, potentially extending to w0<−1, corresponding to increasing dark energy at the present epoch. Alternatively, if the correlation is of hitherto unseen physical origin, the w0waCDM parametrization is self-consistent and no such correction to the DESI inference may be required.
