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2024Natur.634..804N | Quasiperiodic eruptions QPEs are luminous bursts of soft Xrays from the nuclei of galaxies repeating on timescales of hours to weeksSUP15SUP. The mechanism behind these rare systems is uncertain but most theories involve accretion disks around supermassive black holes SMBHs undergoing instabilitiesSUP68SUP or interacting with a stellar object in a close orbitSUP911SUP. It has been suggested that this disk could be created when the SMBH disrupts a passing starSUP811SUP implying that many QPEs should be preceded by observable tidal disruption events TDEs. Two known QPE sources show longterm decays in quiescent luminosity consistent with TDEsSUP412SUP and two observed TDEs have exhibited Xray flares consistent with individual eruptionsSUP1314SUP. TDEs and QPEs also occur preferentially in similar galaxiesSUP15SUP. However no confirmed repeating QPEs have been associated with a spectroscopically confirmed TDE or an optical TDE observed at peak brightness. Here we report the detection of nine Xray QPEs with a mean recurrence time of approximately 48 h from AT2019qiz a nearby and extensively studied optically selected TDESUP16SUP. We detect and model the Xray ultraviolet UV and optical emission from the accretion disk and show that an orbiting body colliding with this disk provides a plausible explanation for the QPEs. | 2024-10-01T00:00:00Z | ['2024Natur.634..804N', '10.1038/s41586-024-08023-6', '10.48550/arXiv.2409.02181', '2024arXiv240902181N', 'arXiv:2409.02181'] | ['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Solar and Stellar Astrophysics'] | Quasiperiodic Xray eruptions years after a nearby tidal disruption event | 2,024 | 326 | 0.7 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 9 | https://arxiv.org/pdf/2409.02181.pdf |
2024SSRv..220...78J | Meteorites and in particular primitive meteorites chondrites are irreplaceable probes of the solar protoplanetary disk. We review their essential properties and endeavour to place them in astrophysical context. The earliest solar system solids refractory inclusions may have formed over the innermost au of the disk and have been transported outward by its expansion or turbulent diffusion. The age spread of chondrite components may be reconciled with the tendency of draginduced radial drift if they were captured in pressure maxima which may account for the noncarbonaceouscarbonaceous meteorite isotopic dichotomy. The solidgas ratio around unity witnessed by chondrules if interpreted as nebular nonimpact products suggests efficient radial concentration and settling at such locations conducive to planetesimal formation by the streaming instability. The cause of the pressure bumps e.g. Jupiter or condensation lines remains to be ascertained. | 2024-10-01T00:00:00Z | ['10.48550/arXiv.2409.07212', '2024SSRv..220...78J', '2024arXiv240907212J', '10.1007/s11214-024-01112-y', 'arXiv:2409.07212'] | ['Astrophysics - Earth and Planetary Astrophysics', 'Physics - Geophysics'] | The Early Solar System and Its Meteoritical Witnesses | 2,024 | 327 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 0 | https://arxiv.org/pdf/2409.07212.pdf |
2024arXiv240909124P | To maximize the amount of information extracted from cosmological datasets simulations that accurately represent these observations are necessary. However traditional simulations that evolve particles under gravity by estimating particleparticle interactions Nbody simulations are computationally expensive and prohibitive to scale to the large volumes and resolutions necessary for the upcoming datasets. Moreover modeling the distribution of galaxies typically involves identifying virialized dark matter halos which is also a time and memoryconsuming process for large Nbody simulations further exacerbating the computational cost. In this study we introduce CHARM a novel method for creating mock halo catalogs by matching the spatial mass and velocity statistics of halos directly from the largescale distribution of the dark matter density field. We develop multistage neural spline flowbased networks to learn this mapping at redshift z0.5 directly with computationally cheaper lowresolution particle mesh simulations instead of relying on the highresolution Nbody simulations. We show that the mock halo catalogs and painted galaxy catalogs have the same statistical properties as obtained from Nbody simulations in both real space and redshift space. Finally we use these mock catalogs for cosmological inference using redshiftspace galaxy power spectrum bispectrum and waveletbased statistics using simulationbased inference performing the first inference with accelerated forward model simulations and finding unbiased cosmological constraints with wellcalibrated posteriors. The code was developed as part of the Simons Collaboration on Learning the Universe and is publicly available at urlhttpsgithub.comshivampcosmoCHARM. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.09124', 'arXiv:2409.09124', '2024arXiv240909124P'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Statistics - Machine Learning'] | CHARM Creating Halos with AutoRegressive Multistage networks | 2,024 | 328 | 0.5 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.09124.pdf |
2024ApJ...974..195Z | Utilizing JWST MIRIMedium Resolution Spectrograph integral field unit observations of the kiloparsecscale central regions we showcase the diversity of ionized gas distributions and kinematics in six nearby Seyfert galaxies included in the GATOS survey. Specifically we present spatially resolved flux distribution and velocity field maps of six ionized emission lines covering a large range of ionization potentials 15.897.1 eV. Based on these maps we showcase the evidence of ionized gas outflows in the six targets and find some highly disturbed regions in NGC 5728 NGC 5506 and ESO137G034. We propose active galactic nucleus AGNdriven radio jets plausibly play an important role in triggering these highly disturbed regions. With the outflow rates estimated based on Ne V emission we find the six targets tend to have ionized outflow rates converged to a narrower range than the previous finding. These results have an important implication for the outflow properties in AGN of comparable luminosity. | 2024-10-01T00:00:00Z | ['10.3847/1538-4357/ad6a4b', '2024ApJ...974..195Z', '2024arXiv240909771Z', '10.48550/arXiv.2409.09771', 'arXiv:2409.09771'] | ['Active galactic nuclei', 'Seyfert galaxies', 'Infrared spectroscopy', '16', '1447', '2285', 'Astrophysics - Astrophysics of Galaxies'] | The Galaxy Activity Torus and Outflow Survey GATOS. IV. Exploring Ionized Gas Outflows in Central Kiloparsec Regions of GATOS Seyferts | 2,024 | 328 | 0.64 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 5 | https://arxiv.org/pdf/2409.09771.pdf |
2024PSJ.....5..230D | The abundance and distribution of metal in asteroid surfaces can be constrained from thermal emission measurements at radio wavelengths informing our understanding of planetesimal differentiation processes. We observed the Mtype asteroid 22 Kalliope and its moon Linus in thermal emission at 1.3 9 and 20 mm with the Atacama Large Millimetersubmillimeter Array and the Karl G. Jansky Very Large Array over most of Kalliopes rotation period. The 1.3 mm data provide 30 km resolution on the surface of Kalliope while both the 1.3 and 9 mm data resolve Linus from Kalliope. We find a thermal inertia for Kalliope of inlineformula inlineformula J mSUP2SUP sSUP0.5SUP KSUP1SUP and emissivities of 0.65 0.02 at 1.3 mm 0.56 0.03 at 9 mm and 0.77 0.02 at 20 mm. Kalliopes millimeter wavelength emission is suppressed compared to its centimeter wavelength emission and is also depolarized. We measure emissivities for Linus of 0.73 0.04 and 0.85 0.17 at 1.3 and 9 mm respectively indicating a less metalrich surface composition for Linus. Spatial variability in Kalliopes emissivity reveals a region in the northern hemisphere with a high dielectric constant suggestive of enhanced metal content. These results are together consistent with a scenario in which Linus formed from reaggregated ejecta from an impact onto a differentiated Kalliope leaving Kalliope with a higher surface metal content than Linus which is distributed heterogeneously across its surface. The low emissivity and lack of polarization suggest a reduced regolith composition where iron is in the form of metallic grains and constitutes 25 of the surface composition. | 2024-10-01T00:00:00Z | ['2024arXiv240912364D', '2024PSJ.....5..230D', 'arXiv:2409.12364', '10.48550/arXiv.2409.12364', '10.3847/PSJ/ad7797'] | ['Small Solar System bodies', 'Asteroids', 'Main belt asteroids', 'Asteroid satellites', 'Radio astronomy', 'Millimeter astronomy', 'Asteroid surfaces', 'Planetary thermal histories', 'Planetary system formation', '1469', '72', '2036', '2207', '1338', '1061', '2209', '2290', '1257', 'Astrophysics - Earth and Planetary Astrophysics'] | Surface Properties of the KalliopeLinus System from ALMA and VLA Data | 2,024 | 328 | 0.5 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.12364.pdf |
2024arXiv240908314C | Active galactic nuclei AGN are the signposts of black hole growth and likely play an important role in galaxy evolution. An outstanding question is whether AGN of different spectral types indicate different evolutionary stages in the coevolution of black holes and galaxies. We present the angular correlation function between an AGN sample selected from the Hyper Suprime Camera Subaru Strategic Program HSCSSP optical Widefield Infrared Survey Explorer WISE midIR photometry and a luminous red galaxy LRG sample from HSCSSP. We investigate AGN clustering strength as a function of their luminosity and spectral features across three independent HSC fields totaling sim600rm deg2 for zin0.61.2 and AGN with L6mu mgt3times1044rmergs1. There are sim28500 AGN and sim1.5 million LRGs in our primary analysis. We determine the inferred average halo mass for the full AGN sample Mh approx 1012.9h1Modot and note that it does not evolve significantly as a function of redshift over this narrow range or luminosity. We find that on average unobscured AGN Mh approx1013.3h1Modot occupy sim4.5times more massive halos than obscured AGN Mh approx1012.6h1Modot at 5sigma statistical significance using 1D uncertainties and at 3sigma using the full covariance matrix suggesting a physical difference between unobscured and obscured AGN beyond the lineofsight viewing angle. Furthermore we find evidence for a halo mass dependence on reddening level within the Type I AGN population which could support the existence of a previously claimed dustobscured phase in AGNhost galaxy coevolution. However we also find that even quite small systematic shifts in the redshift distributions of the AGN sample could plausibly explain current and previously observed differences in Mh. | 2024-09-01T00:00:00Z | ['2024arXiv240908314C', '10.48550/arXiv.2409.08314', 'arXiv:2409.08314'] | ['Astrophysics - Astrophysics of Galaxies'] | Crosscorrelation of Luminous Red Galaxies with MLselected AGN in HSCSSP Unobscured AGN residing in more massive halos | 2,024 | 329 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.08314.pdf |
2024arXiv240909252K | We investigate betafunctions of quantum gravity using dimensional regularisation. In contrast to minimal subtraction a nonminimal renormalisation scheme is employed which is sensitive to powerlaw divergences from mass terms or dimensionful couplings. By construction this setup respects global and gauge symmetries including diffeomorphisms and allows for systematic extensions to higher loop orders. We exemplify this approach in the context of fourdimensional quantum gravity. By computing oneloop betafunctions we find a nontrivial fixed point. It shows two real critical exponents and is compatible with Weinbergs asymptotic safety scenario. Moreover the underlying structure of divergences suggests that gravity becomes effectively twodimensional in the ultraviolet. We discuss the significance of our results as well as further applications and extensions to higher loop orders. | 2024-09-01T00:00:00Z | ['2024arXiv240909252K', '10.48550/arXiv.2409.09252', 'arXiv:2409.09252'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology'] | Fixed Points of Quantum Gravity from Dimensional Regularisation | 2,024 | 329 | 0.18 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.09252.pdf |
2024ApJ...975..109W | Stellar magnetic fields have a major impact on space weather around exoplanets orbiting lowmass stars. From an analysis of Zeemanbroadened Fe I lines measured in nearinfrared SDSSAPOGEE spectra mean magnetic fields are determined for a sample of 29 M dwarf stars that host closely orbiting small exoplanets. The calculations employed the radiative transfer code Synmast and MARCS stellar model atmospheres. The sample M dwarfs are found to have measurable mean magnetic fields ranging between 0.2 and 1.5 kG falling in the unsaturated regime on the versus P SUBrotSUB plane. The sample systems contain 43 exoplanets which include 23 from Kepler nine from K2 and nine from Transiting Exoplanet Survey Satellite. We evaluated their equilibrium temperatures insolation and stellar habitable zones and found that only Kepler186f and TOI700d are inside the habitable zones of their stars. Using the derived values of for the stars Kepler186 and TOI700 we evaluated the minimum planetary magnetic field that would be necessary to shield the exoplanets Kepler186f and TOI700d from their host stars winds considering reference magnetospheres with sizes equal to those of the presentday and young Earth respectively. Assuming a ratio of 5 between large to smallscale Bfields and a youngEarth magnetosphere Kepler186f and TOI700d would need minimum planetary magnetic fields of respectively 0.05 and 0.24 G. These values are considerably smaller than Earths magnetic field of 0.25 G B 0.65 G which suggests that these two exoplanets might have magnetic fields sufficiently strong to protect their atmospheres and surfaces from stellar magnetic fields. | 2024-11-01T00:00:00Z | ['2024ApJ...975..109W', '10.48550/arXiv.2409.06637', 'arXiv:2409.06637', '2024arXiv240906637W', '10.3847/1538-4357/ad7959'] | ['Near infrared astronomy', 'M dwarf stars', 'Stellar activity', 'Stellar magnetic fields', '1093', '982', '1580', '1610', 'Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Earth and Planetary Astrophysics'] | Magnetic Fields in a Sample of Planethosting M Dwarf Stars from Kepler K2 and TESS Observed by APOGEE | 2,024 | 329 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.06637.pdf |
2024MNRAS.535.3129C | Marked power spectra provide a computationally efficient way to extract nonGaussian information from the matter density field using the usual analysis tools developed for the power spectrum without the need for explicit calculation of higherorder correlators. In this work we explore the optimal form of the mark function used for reweighting the density field to maximally constrain cosmology. We show that adding to the mark function or multiplying it by a constant leads to no additional information gain which significantly reduces our search space for optimal marks. We quantify the information gain of this optimal function and compare it against mark functions previously proposed in the literature. We find that we can gain around inlineformulatexmath idTM0001 notationLaTeXsim 2texmathinlineformula times smaller errors in inlineformulatexmath idTM0002 notationLaTeXsigma 8texmathinlineformula and inlineformulatexmath idTM0003 notationLaTeXsim 4texmathinlineformula times smaller errors in inlineformulatexmath idTM0004 notationLaTeXOmega mathrmmtexmathinlineformula compared to using the traditional power spectrum alone an improvement of inlineformulatexmath idTM0005 notationLaTeXsim 60 rm per centtexmathinlineformula compared to other proposed marks when applied to the same data set. | 2024-12-01T00:00:00Z | ['10.1093/mnras/stae2492', '2024MNRAS.tmp.2426C', '10.48550/arXiv.2409.05695', '2024MNRAS.535.3129C', '2024arXiv240905695C', 'arXiv:2409.05695'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Optimizing marked power spectra for cosmology | 2,024 | 330 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3 | https://arxiv.org/pdf/2409.05695.pdf |
2024arXiv240904535L | Statistics that capture the directional dependence of the baryon distribution in the cosmic web enable unique tests of cosmology and astrophysical feedback. We use constrained oriented stacking of thermal SunyaevZeldovich tSZ maps to measure the anisotropic distribution of hot gas 2.540 Mpc away from galaxy clusters embedded in massive filaments and superclusters. The cluster selection and orientation at a scale of sim15 Mpc use Dark Energy Survey DES Year 3 data while expanded tSZ maps from the Atacama Cosmology Telescope Data Release 6 enable a sim3times more significant measurement of the extended gas compared to the techniques proofofconcept. Decomposing stacks into cosine multipoles of order m we detect a dipole m1 and quadrupole m2 at 810sigma as well as evidence for m4 signal at up to 6sigma indicating sensitivity to latetime nonGaussianity. We compare to the Cardinal simulations with spherical gas models pasted onto dark matter halos. The fiducial tSZ data can discriminate between two models that deplete pressure differently in lowmass halos mimicking astrophysical feedback preferring higher average pressure in extended structures. However uncertainty in the amount of cosmic infrared background contamination reduces the constraining power. Additionally we apply the technique to DES galaxy density and weak lensing to study for the first time their oriented relationships with tSZ. In the tSZtolensing relation averaged on 7.5 Mpc transverse scales we observe dependence on redshift but not shape or radial distance. Thus on large scales the superclustering of gas pressure galaxies and total matter is coherent in shape and extent. | 2024-09-01T00:00:00Z | ['arXiv:2409.04535', '2024arXiv240904535L', '10.48550/arXiv.2409.04535'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey II. Anisotropic largescale coherence in hot gas galaxies and dark matter | 2,024 | 330 | 0.52 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.04535.pdf |
2024ApJ...975..214J | The Fe IIMg II emission line flux ratio in quasar spectra serves as a proxy for the relative Fe to element abundances in the broadline regions of quasars. Due to the expected different enrichment timescales of the two elements they can be used as a cosmic clock in the early Universe. We present a study of the Fe IIMg II ratios in a sample of luminous quasars exploiting highquality nearIR spectra taken primarily by the XQR30 program with VLT XSHOOTER. These quasars have a median bolometric luminosity of logL SUBbolSUBerg sSUP1SUP 47.3 and cover a redshift range of z 6.06.6. The median value of the measured Fe IIMg II ratios is 7.9 with a normalized median absolute deviation of 2.2. In order to trace the cosmic evolution of Fe IIMg II in an unbiased manner we select two comparison samples of quasars with similar luminosities and highquality spectra from the literature one at intermediate redshifts z 3.54.8 and the other at low redshifts z 1.02.0. We perform the same spectral analysis for all these quasars including the usage of the same iron template the same spectral fitting method and the same wavelength fitting windows. We find no significant redshift evolution in the Fe IIMg II ratio over the wide redshift range from z 1 to 6.6. The result is consistent with previous studies and supports the scenario of a rapid iron enrichment in the vicinity of accreting supermassive black holes at high redshift. | 2024-11-01T00:00:00Z | ['10.3847/1538-4357/ad7d09', '10.48550/arXiv.2409.06174', '2024arXiv240906174J', '2024ApJ...975..214J', 'arXiv:2409.06174'] | ['Quasars', 'High-redshift galaxies', 'High-luminosity active galactic nuclei', '1319', '734', '2034', 'Astrophysics - Astrophysics of Galaxies'] | No Redshift Evolution in the Fe IIMg II Flux Ratios of Quasars across Cosmic Time | 2,024 | 331 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3 | https://arxiv.org/pdf/2409.06174.pdf |
2024arXiv240906461T | In this contribution the role of strangeness in astrophysics is discussed and more precisely strange hadronic matter in the interior of neutron stars. A special attention is payed to certain phenomena involving strange hadronic matter such as the hyperon puzzle kaon condensation and the thermal behaviour of hyperons in neutron star mergers. | 2024-09-01T00:00:00Z | ['arXiv:2409.06461', '2024arXiv240906461T', '10.48550/arXiv.2409.06461'] | ['Nuclear Theory', 'Astrophysics - High Energy Astrophysical Phenomena'] | Strangeness in Astrophysics | 2,024 | 331 | 0.41 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.06461.pdf |
2024arXiv240910596R | Type IIn supernovae SNeIIn are a highly heterogeneous subclass of corecollapse supernovae spectroscopically characterized by signatures of interaction with a dense circumstellar medium CSM. Here we systematically model the light curves of 142 archival SNeIIn using MOSFiT the Modular Open Source Fitter for Transients. We find that the observed and inferred properties of SNIIn are diverse but there are some trends. The typical SN CSM is dense sim1012gcm3 with highly diverse CSM geometry with a median CSM mass of sim1Modot. The ejecta are typically massive gtrsim10Modot suggesting massive progenitor systems. We find positive correlations between the CSM mass and the rise and fall times of SNeIIn. Furthermore there are positive correlations between the rise time and fall times and the rband luminosity. We estimate the massloss rates of our sample where spectroscopy is available and find a high median massloss rate of sim102Modotyr1 with a range between 1041Modotyr1. These massloss rates are most similar to the mass loss from great eruptions of luminous blue variables consistent with the direct progenitor detections in the literature. We also discuss the role that binary interactions may play concluding that at least some of our SNeIIn may be from massive binary systems. Finally we estimate a detection rate of 1.6times105yr1 in the upcoming Legacy Survey of Space and Time at the Vera C. Rubin Observatory. | 2024-09-01T00:00:00Z | ['arXiv:2409.10596', '10.48550/arXiv.2409.10596', '2024arXiv240910596R'] | ['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Solar and Stellar Astrophysics'] | Unveiling the Diversity of Type IIn Supernovae via Systematic Light Curve Modeling | 2,024 | 331 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.10596.pdf |
2024arXiv240911083L | The exoplanet subNeptune population currently poses a conundrum. Are smallsize planets volatilerich cores without atmosphere or are they rocky cores surrounded by HHe envelope To test the different hypotheses from an observational point of view a large sample of smallsize planets with precise mass and radius measurements is the first necessary step. On top of that much more information will likely be needed including atmospheric characterisation and a demographic perspective on their bulk properties. We present the concept and strategy of THIRSTEE a project which aims at shedding light on the composition of the subNeptune population across stellar types by increasing their number and improving the accuracy of bulk density measurements as well as investigating their atmospheres and performing statistical demographic analysis. We report the first results of the program characterising a 2planet system around the M dwarf TOI406. We analyse TESS and groundbased photometry together with ESPRESSO and NIRPSHARPS RVs to derive the orbital parameters and investigate the internal composition of the 2 planets orbiting TOI406 which have radii and masses of Rb 1.32 pm 0.12 Roplus Mb 2.080.220.23 Moplus and Rc 2.080.150.16 Roplus Mc 6.570.901.00 Moplus and periods of 3.3 and 13.2 days respectively. Planet b is consistent with an Earthlike composition while planet c is compatible with multiple internal composition models including volatilerich planets without HHe atmospheres. The 2 planets are located in 2 distinct regions in the massdensity diagram supporting the existence of a density gap among small exoplanets around M dwarfs. With an equilibrium temperature of only 368 K TOI406 c stands up as a particularly interesting target for atmospheric characterisation with JWST in the lowtemperature regime. | 2024-09-01T00:00:00Z | ['arXiv:2409.11083', '2024arXiv240911083L', '10.48550/arXiv.2409.11083'] | ['Astrophysics - Earth and Planetary Astrophysics'] | Characterisation of TOI406 as showcase of the THIRSTEE program A 2planet system straddling the Mdwarf density gap | 2,024 | 331 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.11083.pdf |
2024arXiv240908759M | Here we present the angular diameter distance measurement obtained from the measurement of the Baryonic Acoustic Oscillation BAO feature using the completed Dark Energy Survey DES data summarizing the main results of Phys. Rev. D 110 063514 and Phys. Rev. D 110 063515. We use a galaxy sample optimized for BAO science in the redshift range 0.6 lt z lt 1.2 with an effective redshift of zrm eff 0.85. Our consensus measurement constrains the ratio of the angular distance to the sound horizon scale to DMzrm effrd 19.51 pm 0.41. This measurement is found to be 2.13sigma below the angular BAO scale predicted by Planck. To date it represents the most precise measurement from purely photometric data and the most precise from any StageIII experiment at such high redshift. The analysis was performed blinded to the BAO position and is shown to be robust against analysis choices data removal redshift calibrations and observational systematics. | 2024-09-01T00:00:00Z | ['2024arXiv240908759M', 'arXiv:2409.08759', '10.48550/arXiv.2409.08759'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Dark Energy Survey 2.1 measurement of the Baryon Acoustic Oscillation scale from the final dataset | 2,024 | 332 | 0.37 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.08759.pdf |
2024arXiv240907536C | A formulation of discrete gravity was recently proposed based on defining a lattice and a shift operator connecting the cells. Spinors on such a space will have rotational SOd invariance which is taken as the fundamental symmetry. Inspired by lattice QCD discrete analogues of curvature and torsion were defined that go smoothly to the corresponding tensors in the continuous limit. In this paper we show that the absence of diffeomorphism invariance could be replaced by requiring translational invariance in the tangent space by enlarging the tangent space from SOd to the inhomogeneous Lorentz group ISOd to include translations. We obtain the ISOd symmetry by taking instead the Lie group SOd 1 and perform on it InonuWigner contraction. We show that just as for continuous spaces the zero torsion constraint converts the translational parameter to a diffeomorphism parameter thus explaining the effectiveness of this formulation. | 2024-09-01T00:00:00Z | ['arXiv:2409.07536', '2024arXiv240907536C', '10.48550/arXiv.2409.07536'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Lattice'] | Poincare Invariance in Discrete Gravity | 2,024 | 332 | 0.17 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07536.pdf |
2024A&A...691A..67M | Recent observations of giant planets have revealed unexpected bulk densities. Hot Jupiters in particular appear larger than expected for their masses compared to planetary evolution models while warm Jupiters seem denser than expected. These differences are often attributed to the influence of the stellar incident flux but it has been unclear if they also result from different planet formation processes and if there is a trend linking the planetary density to the chemical composition of the host star. In this work we present the confirmation of three giant planets in orbit around solar analogue stars. TOI2714 b P 2.5 d RSUBpSUB 1.22 RSUBJSUB MSUBpSUB 0.72 MSUBJSUB and TOI2981 b P 3.6 d RSUBPSUB 1.2 RSUBJSUB MSUBPSUB 2 MSUBJSUB are hot Jupiters on nearly circular orbits while TOI4914 b P 10.6 d RSUBPSUB 1.15 RSUBJSUB MSUBpSUB 0.72 MSUBJSUB is a warm Jupiter with a significant eccentricity e 0.41 0.02 that orbits a star more metalpoor FeH 0.13 than most of the stars known to host giant planets. Similarly TOI2981 b orbits a metalpoor star FeH 0.11 while TOI2714 b orbits a metalrich star FeH 0.30. Our radial velocity followup with the HARPS spectrograph allows us to detect their Keplerian signals at high significance 7 30 and 23 respectively and to place a strong constraint on the eccentricity of TOI4914 b 18. TOI4914 b with its large radius RSUBpSUB 1.15 RSUBJSUB and low insolation flux FSUBSUB lt 2 108 erg sSUP1SUP cmSUP2SUP appears to be more inflated than what is supported by current theoretical models for giant planets. Moreover it does not conform to the previously noted trend that warm giant planets orbiting metalpoor stars have low eccentricities. This study thus provides insights into the diverse orbital characteristics and formation processes of giant exoplanets in particular the role of stellar metallicity in the evolution of planetary systems. | 2024-11-01T00:00:00Z | ['2024arXiv240907520M', '2024A&A...691A..67M', '10.48550/arXiv.2409.07520', '10.1051/0004-6361/202451841', 'arXiv:2409.07520'] | ['techniques: photometric', 'techniques: radial velocities', 'planets and satellites: fundamental parameters', 'planets and satellites: gaseous planets', 'stars: fundamental parameters', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics'] | The inflated eccentric warm Jupiter TOI4914 b orbiting a metalpoor star and the hot Jupiters TOI2714 b and TOI2981 b | 2,024 | 333 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.07520.pdf |
2024arXiv240912937Z | To improve the performance of fullshape analyses of largescale structure we consider using a halo occupation distribution HODinformed prior for the effective field theory EFT nuisance parameters. We generate 320 000 mock galaxy catalogs using 10 000 sets of HOD parameters across 32 simulation boxes with different cosmologies. We measure and fit the redshiftspace power spectra using a fast emulator of the EFT model and the resulting bestfit EFT parameter distributions are used to create the prior. This prior effectively constrains the EFT nuisance parameter space limiting it to the space of HODmocks that can be well fit by a EFT model. We have tested the stability of the prior under different configurations including the effect of varying the HOD sample distribution and the inclusion of the hexadecapole moment. We find that our HODinformed prior and the cosmological parameter constraints derived using it are robust. While cosmological fits using the standard EFT prior suffer from prior effects sometimes failing to recover the true cosmology within Bayesian credible intervals the HODinformed prior mitigates these issues and significantly improves cosmological parameter recovery for LambdaCDM and beyond. This work lays the foundation for better fullshape largescale structure analyses in current and upcoming galaxy surveys making it a valuable tool for addressing key questions in cosmology. | 2024-09-01T00:00:00Z | ['2024arXiv240912937Z', 'arXiv:2409.12937', '10.48550/arXiv.2409.12937'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | HODinformed prior for EFTbased fullshape analyses of LSS | 2,024 | 333 | 0.48 | ['EPRINT_HTML', 'EPRINT_PDF'] | 6 | https://arxiv.org/pdf/2409.12937.pdf |
2024arXiv240910265G | Several studies have argued that the Milky Way was a representation of the ancient Egyptian sky goddess Nut. Here I test this assumption by examining Nuts visual depictions on ancient Egyptian coffins. I assemble a catalog of 555 coffin elements which includes 118 cosmological vignettes from the 21st22nd Dynasties and report several observations. First I find that the cosmological vignette on the outer coffin of Nesitaudjatakhet bears a unique feature a thick undulating black curve that bisects Nuts starstudded body and recalls the Great Rift that cleaves the Milky Way in two. Moreover it resembles similar features identified as the Milky Way on the bodies of Navajo Hopi and Zuni spiritual beings. Hence I argue that the undulating curve on Nuts body is the first visual representation of the Milky Way identified in the Egyptian archaeological record. However its rarity strengthens the conclusion reached by Graur 2024a Though Nut and the Milky Way are linked they are not synonymous. Instead of acting as a representation of Nut the Milky Way is one more celestial phenomenon that like the Sun and the stars is associated with Nut in her role as the sky. Second Nuts body is decorated with stars in only a quarter of the vignettes. If we associate Nuts naked and starstudded forms with the day and night sky respectively we would expect to see stars in half of the vignettes. This null hypothesis is rejected at gt6sigma statistical significance. For whatever reason it appears that the Egyptians of the 21st22nd Dynasties preferred the day sky over the night sky. Finally I discuss the interplay between Nuts cosmological vignette and fulllength portraits inside coffins from the New Kingdom to the Roman Period in light of Nuts combined cosmological and eschatological roles as an embodiment of the coffin. | 2024-09-01T00:00:00Z | ['2024arXiv240910265G', '10.48550/arXiv.2409.10265', 'arXiv:2409.10265'] | ['Physics - History and Philosophy of Physics', 'Astrophysics - Astrophysics of Galaxies', 'Physics - Popular Physics'] | The Ancient Egyptian Cosmological Vignette First Visual Evidence of the Milky Way and Trends in Coffin Depictions of the Sky Goddess Nut | 2,024 | 333 | 0.39 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.10265.pdf |
2017Natur.542..456G | One aim of modern astronomy is to detect temperate Earthlike exoplanets that are well suited for atmospheric characterization. Recently three Earthsized planets were detected that transit that is pass in front of a star with a mass just eight per cent that of the Sun located 12 parsecs away. The transiting configuration of these planets combined with the Jupiterlike size of their host starnamed TRAPPIST1makes possible indepth studies of their atmospheric properties with presentday and future astronomical facilities. Here we report the results of a photometric monitoring campaign of that star from the ground and space. Our observations reveal that at least seven planets with sizes and masses similar to those of Earth revolve around TRAPPIST1. The six inner planets form a nearresonant chain such that their orbital periods 1.51 2.42 4.04 6.06 9.1 and 12.35 days are nearratios of small integers. This architecture suggests that the planets formed farther from the star and migrated inwards. Moreover the seven planets have equilibrium temperatures low enough to make possible the presence of liquid water on their surfaces. | 2017-02-01T00:00:00Z | ['2017Natur.542..456G', 'arXiv:1703.01424', '2017arXiv170301424G', '10.1038/nature21360', '10.48550/arXiv.1703.01424'] | ['Astrophysics - Earth and Planetary Astrophysics'] | Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST1 | 2,017 | 334 | 0.7 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 1,257 | https://arxiv.org/pdf/1703.01424.pdf |
2024arXiv240907856L | Massive clusters of galaxies are very rare in the observable Universe. Even rarer are mergers of such clusters observed close to pericenter passage. Here we report on one such case a massive 1015Modot and hot kT 10 keV cluster CL0238.32005 at zapprox 0.42. For this cluster we combine Xray data from SRGeROSITA and Chandra optical images from DESI and spectroscopy from BTA and RTT150 telescopes. The Xray and optical morphologies suggest an ongoing merger with the projected separation of subhalos of sim 200 kpc. The lineofsight velocity of galaxies tentatively associated with the two merging halos differs by 20003000 kms. We conclude that most plausibly the merger axis is neither close to the line of sight nor to the sky plane. We compare CL0238 with two wellknown clusters MACS0416 and Bullet and conclude that CL0238 corresponds to an intermediate phase between the premerging MACS0416 cluster and the postmerger Bullet cluster. Namely this cluster has recently only lesssim 0.1 Gyr ago experienced an almost headon merger. We argue that this just after system is a very rare case and an excellent target for lensing SunyaevZeldovich effect and Xray studies that can constrain properties ranging from dynamics of mergers to selfinteracting dark matter and plasma effects in intracluster medium that are associated with shock waves e.g. electronion equilibration efficiency and relativistic particle acceleration. | 2024-09-01T00:00:00Z | ['arXiv:2409.07856', '2024arXiv240907856L', '10.48550/arXiv.2409.07856'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena'] | Merger of massive galaxy cluster CL0238.32005 at z0.4 just after pericenter passage | 2,024 | 335 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07856.pdf |
2024arXiv240907527K | Alongside the population of several hundred radio millisecond pulsars currently known in Milky Way globular clusters a subset of six slowly spinning pulsars spin periods 0.34s are also observed. With inferred magnetic fields gtrsim 1011G and characteristic ages lesssim108yr explaining the formation of these apparently young pulsars in old stellar populations poses a major challenge. One popular explanation is that these objects are not actually young but instead have been partially spun up via accretion from a binary companion. In this scenario accretion in a typical lowmass Xray binary is interrupted by a dynamical encounter with a neighboring object in the cluster. Instead of complete spin up to millisecond spin periods the accretion is halted prematurely leaving behind a partially recycled neutron star. In this Letter we use a combination of analytic arguments motivated by lowmass Xray binary evolution and Nbody simulations to show that this partialrecycling mechanism is not viable. Realistic globular clusters are not sufficiently dense to interrupt mass transfer on the short timescales required to achieve such slow spin periods. We argue that collapse of massive white dwarfs andor neutron star collisions are more promising ways to form slow pulsars in old globular clusters. | 2024-09-01T00:00:00Z | ['arXiv:2409.07527', '10.48550/arXiv.2409.07527', '2024arXiv240907527K'] | ['Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - High Energy Astrophysical Phenomena'] | Can slow pulsars in Milky Way globular clusters form via partial recycling | 2,024 | 336 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07527.pdf |
2024arXiv240911486G | We study spherical accretion of magnetized plasma with low angular momentum onto a supermassive black hole utilizing global General Relativistic Magnetohydrodynamic simulations. Black holedriven feedback in the form of magnetic eruptions and jets triggers magnetized turbulence in the surrounding medium. We find that when the Bondi radius exceeds a certain value relative to the black holes gravitational radius this turbulence restricts the subsequent inflow of magnetic flux strongly suppressing the strength of the jet. Consequently magnetically arrested disks and powerful jets are not a generic outcome of accretion of magnetized plasma even if there is an abundance of magnetic flux available in the system. However if there is significant angular momentum in the inflowing gas the eruptiondriven turbulence is suppressed sheared out allowing for the presence of a powerful jet. Both the initially rotating and nonrotating flows go through periods of low and high gas angular momentum showing that the angular momentum content of the inflowing gas is not just a feature of the ambient medium but is strongly modified by the eruption and jetdriven black hole feedback. In the lower angular momentum states our results predict that there should be dynamically strong magnetic fields on horizon scales but no powerful jet this state may be consistent with Sgr A in the Galactic Center. | 2024-09-01T00:00:00Z | ['2024arXiv240911486G', 'arXiv:2409.11486', '10.48550/arXiv.2409.11486'] | ['Astrophysics - High Energy Astrophysical Phenomena'] | Strongly magnetized accretion with low angular momentum produces a weak jet | 2,024 | 336 | 0.56 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.11486.pdf |
2024A&A...686L...2G | Context. Gravitational waves from blackhole BH merging events have revealed a population of extragalactic BHs residing in shortperiod binaries with masses that are higher than expected based on most stellar evolution models and also higher than known stellarorigin black holes in our Galaxy. It has been proposed that those highmass BHs are the remnants of massive metalpoor stars. BR Aims Gaia astrometry is expected to uncover many Galactic widebinary systems containing dormant BHs which may not have been detected before. The study of this population will provide new information on the BHmass distribution in binaries and shed light on their formation mechanisms and progenitors. BR Methods As part of the validation efforts in preparation for the fourth Gaia data release DR4 we analysed the preliminary astrometric binary solutions obtained by the Gaia NonSingle Star pipeline to verify their significance and to minimise falsedetection rates in highmassfunction orbital solutions. BR Results The astrometric binary solution of one source Gaia BH3 implies the presence of a 32.70 0.82 MSUBSUB BH in a binary system with a period of 11.6 yr. Gaia radial velocities independently validate the astrometric orbit. Broadband photometric and spectroscopic data show that the visible component is an old very metalpoor giant of the Galactic halo at a distance of 590 pc. BR Conclusions The BH in the Gaia BH3 system is more massive than any other Galactic stellarorigin BH known thus far. The low metallicity of the star companion supports the scenario that metalpoor massive stars are progenitors of the highmass BHs detected by gravitationalwave telescopes. The Galactic orbit of the system and its metallicity indicate that it might belong to the Sequoia halo substructure. Alternatively and more plausibly it could belong to the ED2 stream which likely originated from a globular cluster that had been disrupted by the Milky Way. P Full Table B.1 and Table B.2 with Gaia epoch data are available at the CDS via anonymous ftp to A hrefhttpscdsarc.cds.unistra.frcdsarc.cds.unistra.frA ftp130.79.128.5 or via A hrefhttpscdsarc.cds.unistra.frvizbincatJAA686L2httpscdsarc.cds.unistra.frvizbincatJAA686L2A | 2024-06-01T00:00:00Z | ['2024A&A...686L...2G', '10.48550/arXiv.2404.10486', '10.1051/0004-6361/202449763', '2024arXiv240410486G', 'arXiv:2404.10486'] | ['astrometry', 'binaries: spectroscopic', 'stars: black holes', 'stars: evolution', 'stars: massive', 'stars: Population II', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Solar and Stellar Astrophysics'] | Discovery of a dormant 33 solarmass black hole in prerelease Gaia astrometry | 2,024 | 336 | 0.74 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 68 | https://arxiv.org/pdf/2404.10486.pdf |
2024arXiv240911021M | We study particle production in Vaidya spacetime. Using the WKB approximation the distribution of Hawking radiation is calculated without the nearhorizon approximation which leads to finite corrections to the purely thermal spectrum. We extend our analysis to extremal and nonextremal ReissnerNordstrm and Kerr black holes. Our results can be understood in terms of a thermodynamic toy model where one regards Hawking radiation as Unruh radiation perceived by observers outside of the black hole. Moreover we extend the model to incorporate the backreaction of Hawking quanta on spacetime geometry. Our study suggests that the backreaction may prevent the formation of the event horizon and spacetime singularity. | 2024-09-01T00:00:00Z | ['arXiv:2409.11021', '2024arXiv240911021M', '10.48550/arXiv.2409.11021'] | ['General Relativity and Quantum Cosmology', 'High Energy Physics - Theory'] | Hawking radiation far away from the event horizon | 2,024 | 337 | 0.28 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.11021.pdf |
2024arXiv240906056T | We present the detection and analysis of GRB 231115A a candidate extragalactic magnetar giant flare MGF observed by FermiGBM and localized by INTEGRAL to the starburst galaxy M82. This burst exhibits distinctive temporal and spectral characteristics that align with known MGFs including a short duration and a high peak energy. Gammaray analyses reveal significant insights into this burst supporting conclusions already established in the literature our timeresolved spectral studies provide further evidence that GRB 231115A is indeed a MGF. Significance calculations also suggest a robust association with M82 further supported by a high Bayes factor that minimizes the probability of chance alignment with a neutron star merger. Despite extensive followup efforts no contemporaneous gravitational wave or radio emissions were detected. The lack of radio emission sets stringent upper limits on possible radio luminosity. Constraints from our analysis show no fast radio bursts FRBs associated with two MGFs. Xray observations conducted postburst by SwiftXRT and XMMNewton provided additional data though no persistent counterparts were identified. Our study underscores the importance of coordinated multiwavelength followup and highlights the potential of MGFs to enhance our understanding of short GRBs and magnetar activities in the cosmos. Current MGF identification and followup implementation are insufficient for detecting expected counterparts however improvements in these areas may allow for the recovery of followup signals with existing instruments. Future advancements in observational technologies and methodologies will be crucial in furthering these studies. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.06056', 'arXiv:2409.06056', '2024arXiv240906056T'] | ['Astrophysics - High Energy Astrophysical Phenomena'] | Extragalactic Magnetar Giant Flare GRB 231115A Insights from FermiGBM Observations | 2,024 | 337 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.06056.pdf |
2024arXiv240909101R | Many modern applications of Bayesian inference such as in cosmology are based on complicated forward models with highdimensional parameter spaces. This considerably limits the sampling of posterior distributions conditioned on observed data. In turn this reduces the interpretability of posteriors to their one and twodimensional marginal distributions when more information is available in the full dimensional distributions. We show how to learn smooth and differentiable representations of posterior distributions from their samples using normalizing flows which we train with an added evidence error loss term to improve accuracy in multiple ways. Motivated by problems from cosmology we implement a robust method to obtain one and twodimensional posterior profiles. These are obtained by optimizing instead of integrating over other parameters and are thus less prone than marginals to socalled projection effects. We also demonstrate how this representation provides an accurate estimator of the Bayesian evidence with log error at the 0.2 level allowing accurate model comparison. We test our method on multimodal mixtures of Gaussians up to dimension 32 before applying it to simulated cosmology examples. Our code is publicly available at httpsgithub.commraveritensiometer. | 2024-09-01T00:00:00Z | ['2024arXiv240909101R', 'arXiv:2409.09101', '10.48550/arXiv.2409.09101'] | ['Astrophysics - Instrumentation and Methods for Astrophysics', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Understanding posterior projection effects with normalizing flows | 2,024 | 337 | 0.46 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.09101.pdf |
2024arXiv240906258L | Temperate exoplanets between the sizes of Earth and Neptune known as subNeptunes have emerged as intriguing targets for astrobiology. It is unknown whether these planets resemble Earthlike terrestrial worlds with a habitable surface Neptunelike giant planets with deep atmospheres and no habitable surface or something exotic in between. Recent JWST transmission spectroscopy observations of the canonical subNeptune K218 b revealed 1 CH4 1 CO2 and a nondetection of CO in the atmosphere. While previous studies proposed that the observed atmospheric composition could help constrain the lower atmospheres conditions and determine the interior structure of subNeptunes like K218 b the possible interactions between the atmosphere and a hot supercritical water ocean at its base remain unexplored. In this work we investigate whether a global supercritical water ocean resembling a planetaryscale hydrothermal system can explain these observations on K218 blike subNeptunes through equilibrium aqueous geochemical calculations. We find that the observed atmospheric CH4CO2 ratio implies a minimum ocean temperature of 710 K whereas the corresponding COCO2 ratio allows ocean temperatures up to 1070 K. These results indicate that a global supercritical water ocean on K218 b is plausible. While life cannot survive in such an ocean this work represents the first step towards understanding how a global supercritical water ocean may influence observable atmospheric characteristics on volatilerich subNeptunes. Future observations with better constrained CO and NH3 mixing ratios could further help distinguish between possible interior compositions of K218 b. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.06258', 'arXiv:2409.06258', '2024arXiv240906258L'] | ['Astrophysics - Earth and Planetary Astrophysics'] | Volatilerich SubNeptunes as Hydrothermal Worlds The Case of K218 b | 2,024 | 337 | 0.52 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.06258.pdf |
2024arXiv240911361S | Determining the Hubble constant H0 a fundamental parameter describing cosmic expansion remains a challenge due to conflicting measurements from the early and late universe. Gravitational wave GW observations from binary neutron star BNS mergers with identified host galaxies through electromagnetic EM followup offer an independent method to measure H0. However this requires detection of numerous events which could take decades with current GW detectors. LIGOIndia can dramatically accelerate this effort. With sensitivity comparable to the existing LIGO detectors its addition to the LIGOVirgo network could increase detected events by 70. This improvement nearly doubles when accounting for the detectors 70 duty cycle increasing the probability of simultaneous operation of three detectors by a factor of 2. We perform endtoend simulations to estimate triplecoincidence detection rates and sky localization considering realistic BNS populations lightcurves and EM observatory specifications. Our findings suggest LIGOIndia could increase BNS events with observed kilonovae by 27 times. The factor of few improvements in source localization precision with LIGOIndia can allow much deeper EM followup campaigns not considered in the simulations potentially increasing the overall rate of detection of EM counterparts by a factor of 20 which can have an enormous impact in addressing critical questions in different areas of astronomy. We evaluate the impact of LIGOIndia in the context of H0 measurement and argue that it can cut down the required observation time of several decades by a factor of few and possibly to just few years with regular sensitivity upgrades. | 2024-09-01T00:00:00Z | ['arXiv:2409.11361', '10.48550/arXiv.2409.11361', '2024arXiv240911361S'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology'] | Assessing the potential of LIGOIndia in resolving the Hubble Tension | 2,024 | 337 | 0.41 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.11361.pdf |
2024ApJ...975..166B | Planet formation is strongly influenced by the composition and distribution of volatiles within protoplanetary disks. With JWST it is now possible to obtain direct observational constraints on disk ices as recently demonstrated by the detection of ice absorption features toward the edgeon HH 48 NE disk as part of the Ice Age Early Release Science program. Here we introduce a new radiative transfer modeling framework designed to retrieve the composition and mixing status of disk ices using their band profiles and apply it to interpret the HSUB2SUBO COSUB2SUB and CO ice bands observed toward the HH 48 NE disk. We show that the ices are largely present as mixtures with strong evidence for CO trapping in both HSUB2SUBO and COSUB2SUB ice. The HH 48 NE disk ice composition pure versus polar versus apolar fractions is markedly different from earlier protostellar stages implying thermal andor chemical reprocessing during the formation or evolution of the disk. We infer low icephase CO ratios around 0.1 throughout the disk and also demonstrate that the mixing and entrapment of disk ices can dramatically affect the radial dependence of the CO ratio. It is therefore imperative that realistic disk ice compositions are considered when comparing planetary compositions with potential formation scenarios which will fortunately be possible for an increasing number of disks with JWST. | 2024-11-01T00:00:00Z | ['arXiv:2409.08117', '10.3847/1538-4357/ad79fc', '10.48550/arXiv.2409.08117', '2024ApJ...975..166B', '2024arXiv240908117B'] | ['Astrochemistry', 'Protoplanetary disks', 'Radiative transfer', 'Interstellar molecules', '75', '1300', '1335', '849', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Instrumentation and Methods for Astrophysics'] | JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk | 2,024 | 338 | 0.63 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 1 | https://arxiv.org/pdf/2409.08117.pdf |
2024PhRvL.133m5301C | Diffusion coefficients for crystallized Coulomb plasmas are essential microphysics input for modeling white dwarf cores and neutron star crusts but are poorly understood. In this work we present a model for diffusion in Coulomb crystals. We show that melting and diffusion follow the same universal scaling such that diffusion is independent of screening. Our simulations show contrary to prevailing wisdom that the formation of vacancies is not suppressed by the large pressure. Rather vacancy formation and hole diffusion is the dominant mode of selfdiffusion in Coulomb crystals. | 2024-09-01T00:00:00Z | ['10.1103/PhysRevLett.133.135301', '2024PhRvL.133m5301C', '2024arXiv240907513C', '10.48550/arXiv.2409.07513', 'arXiv:2409.07513'] | ['Plasma and Solar Physics', 'Accelerators and Beams', 'Physics - Plasma Physics', 'Astrophysics - High Energy Astrophysical Phenomena'] | Universal Diffusion in Coulomb Crystals | 2,024 | 338 | 0.46 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 0 | https://arxiv.org/pdf/2409.07513.pdf |
2024Univ...10..383G | The stellar initial mass function IMF represents a fundamental quantity in astrophysics and cosmology describing the mass distribution of stars from low mass all the way up to massive and very massive stars. It is intimately linked to a wide variety of topics including stellar and binary evolution galaxy evolution chemical enrichment and cosmological reionization. Nonetheless the IMF still remains highly uncertain. In this work we aim to determine the IMF with a novel approach based on the observed rates of transients of stellar origin. We parametrize the IMF with a simple but flexible Larson shape and insert it into a parametric model for the cosmic UV luminosity density local stellar mass density type Ia supernova SN Ia corecollapse supernova CCSN and long gammaray burst LGRB rates as a function of redshift. We constrain our free parameters by matching the model predictions to a set of empirical determinations for the corresponding quantities via a Bayesian Markov Chain Monte Carlo method. Remarkably we are able to provide an independent IMF determination with a characteristic mass inlineformulammlmath idmm1mmlsemanticsmmlmrowmmlmsubmmlmimmmlmimmlmicmmlmimmlmsubmmlmommlmommlmn0mmlmnmmlmo.mmlmommlmsubsupmmlmn10mmlmnmmlmrowmmlmommlmommlmn0.08mmlmnmmlmrowmmlmrowmmlmommlmommlmn0.24mmlmnmmlmrowmmlmsubsupmmlmsubmmlmi mathvariantnormalMmmlmimmlmommlmommlmsubmmlmrowmmlsemanticsmmlmathinlineformula and highmass slope inlineformulammlmath idmm3mmlsemanticsmmlmrowmmlmimmlmimmlmommlmommlmommlmommlmn2mmlmnmmlmo.mmlmommlmsubsupmmlmn53mmlmnmmlmrowmmlmommlmommlmn0.27mmlmnmmlmrowmmlmrowmmlmommlmommlmn0.24mmlmnmmlmrowmmlmsubsupmmlmrowmmlsemanticsmmlmathinlineformula that are in accordance with the widely used IMF parameterizations e.g. Salpeter Kroupa Chabrier. Moreover the adoption of an uptodate recipe for the cosmic metallicity evolution allows us to constrain the maximum metallicity of LGRB progenitors to inlineformulammlmath idmm4mmlsemanticsmmlmrowmmlmsubmmlmiZmmlmimmlmrowmmlmimmmlmimmlmiammlmimmlmixmmlmimmlmrowmmlmsubmmlmommlmommlmn0mmlmnmmlmo.mmlmommlmsubsupmmlmn12mmlmnmmlmrowmmlmommlmommlmn0.05mmlmnmmlmrowmmlmrowmmlmommlmommlmn0.29mmlmnmmlmrowmmlmsubsupmmlmsubmmlmi mathvariantnormalZmmlmimmlmommlmommlmsubmmlmrowmmlsemanticsmmlmathinlineformula. We also find which progenitor fraction actually leads to SN Ia or LGRB emission e.g. due to binary interaction or jetlaunching conditions put constraints on the CCSN and LGRB progenitor mass ranges and test the IMF universality. These results show the potential of this kind of approach for studying the IMF its putative evolution with the galactic environment and cosmic history and the properties of SN Ia CCSN and LGRB progenitors especially considering the wealth of data incoming in the future. | 2024-09-01T00:00:00Z | ['arXiv:2409.09118', '10.3390/universe10100383', '2024Univ...10..383G', '2024arXiv240909118G', '10.48550/arXiv.2409.09118'] | ['initial mass function', 'stellar and binary evolution', 'supernovae', 'gamma-ray bursts', 'galaxy evolution', 'Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Solar and Stellar Astrophysics'] | Constraining the Initial Mass Function via Stellar Transients | 2,024 | 338 | 0.53 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 0 | https://arxiv.org/pdf/2409.09118.pdf |
2024arXiv240907553R | Disc dominated galaxies can be difficult to accommodate in a hierarchical formation scenario like LambdaCDM where mergers are an important growth mechanism. However observational evidence indicates that these galaxies are common. We seek to characterise the conditions that lead to the formation of disc dominated galaxies within LambdaCDM. We use dynamical decomposition in all galaxies with stellar mass M1010 rm 1011 rm Modot within the simulation Illustris TNG100. We select a sample of 43 mostlydisc galaxies having less than sim 10 of their mass into a bulge component. For comparison we also study two additional stellarmass matched samples 43 intermediate galaxies having sim 30 of their mass in the bulge and 43 with purely spheroidallike morphology. We find that the selection based on stellar dynamics is able to reproduce the expected stellar population trends of different morphologies with higher starformation rates and younger stars in discdominated galaxies. Halo spin seems to play no role in the morphology of the galaxies. At fixed M our mostlydisc and intermediate samples form in dark matter haloes that are 210 times less massive than the spheroidal sample highlighting a higher efficiency in disc galaxies to retain and condensate their baryons. On average mergers are less prevalent in the build up of discs than in spheroidal galaxies but there is a large scatter including the existence of mostlydisc galaxies with 1530 of their stars from accreted origin. Discs start forming early on settling their low vertical velocity dispersion as early as 910 Gyr ago although the dominance of the disc over the spheroid gets established more recently 34 Gyr ago. The most rotationally supported discs form in haloes with the lowest mass in the sample and best aligned distribution of angular momentum in the gas. | 2024-09-01T00:00:00Z | ['2024arXiv240907553R', '10.48550/arXiv.2409.07553', 'arXiv:2409.07553'] | ['Astrophysics - Astrophysics of Galaxies'] | The assembly of the most rotationally supported disc galaxies in the TNG100 simulations | 2,024 | 339 | 0.53 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07553.pdf |
2013ARA&A..51..511K | Supermassive black holes BHs have been found in 85 galaxies by dynamical modeling of spatially resolved kinematics. The Hubble Space Telescope revolutionized BH research by advancing the subject from its proofofconcept phase into quantitative studies of BH demographics. Most influential was the discovery of a tight correlation between BH mass Formula see text and the velocity dispersion of the bulge component of the host galaxy. Together with similar correlations with bulge luminosity and mass this led to the widespread belief that BHs and bulges coevolve by regulating each others growth. Conclusions based on one set of correlations from Formula see text in brightest cluster ellipticals to Formula see text in the smallest galaxies dominated BH work for more than a decade. New results are now replacing this simple story with a richer and more plausible picture in which BHs correlate differently with different galaxy components. A reasonable aim is to use this progress to refine our understanding of BHgalaxy coevolution. BHs with masses of 10SUP5SUP10SUP6SUPMSUBSUB are found in many bulgeless galaxies. Therefore classical ellipticalgalaxylike bulges are not necessary for BH formation. On the other hand although they live in galaxy disks BHs do not correlate with galaxy disks. Also any Formula see text correlations with the properties of diskgrown pseudobulges and dark matter halos are weak enough to imply no close coevolution. The above and other correlations of hostgalaxy parameters with each other and with Formula see text suggest that there are four regimes of BH feedback. 1 Local secular episodic and stochastic feeding of small BHs in largely bulgeless galaxies involves too little energy to result in coevolution. 2 Global feeding in major wet galaxy mergers rapidly grows giant BHs in shortduration quasarlike events whose energy feedback does affect galaxy evolution. The resulting hosts are classical bulges and corelessrotatingdisky ellipticals. 3 After these AGN phases and at the highest galaxy masses maintenancemode BH feedback into Xrayemitting gas has the primarily negative effect of helping to keep baryons locked up in hot gas and thereby keeping galaxy formation from going to completion. This happens in giant corenonrotatingboxy ellipticals. Their properties including their tight correlations between Formula see text and core parameters support the conclusion that core ellipticals form by dissipationless major mergers. They inherit coevolution effects from smaller progenitor galaxies. Also 4 independent of any feedback physics in BH growth modes 2 and 3 the averaging that results from successive mergers plays a major role in decreasing the scatter in Formula see text correlations from the large values observed in bulgeless and pseudobulge galaxies to the small values observed in giant elliptical galaxies. | 2013-08-01T00:00:00Z | ['2013ARA&A..51..511K', '2013arXiv1304.7762K', 'arXiv:1304.7762', '10.1146/annurev-astro-082708-101811', '10.48550/arXiv.1304.7762'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Coevolution Or Not of Supermassive Black Holes and Host Galaxies | 2,013 | 340 | 0.8 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3,407 | https://arxiv.org/pdf/1304.7762.pdf |
2024arXiv240906040L | We present textscMathpop a novel method to infer the globular cluster GC counts in ultradiffuse galaxies UDGs and lowsurface brightness galaxies LSBGs. Many known UDGs have a surprisingly high ratio of GC number to surface brightness. However standard methods to infer GC counts in UDGs face various challenges such as photometric measurement uncertainties GC membership uncertainties and assumptions about the GC luminosity functions GCLFs. textscMathpop tackles these challenges using the markdependent thinned point process enabling joint inference of the spatial and magnitude distributions of GCs. In doing so textscMathpop allows us to infer and quantify the uncertainties in both GC counts and GCLFs with minimal assumptions. As a precursor to textscMathpop we also address the data uncertainties coming from the selection process of GC candidates we obtain probabilistic GC candidates instead of the traditional binary classification based on the colormagnitude diagram. We apply textscMathpop to 40 LSBGs in the Perseus cluster using GC catalogs from a textitHubble Space Telescope imaging program. We then compare our results to those from an independent study using the standard method. We further calibrate and validate our approach through extensive simulations. Our approach reveals two LSBGs having GCLF turnover points much brighter than the canonical value with Bayes factor being sim4.5 and sim2.5 respectively. An additional crude maximumlikelihood estimation shows that their GCLF TO points are approximately 0.9mag and 1.1mag brighter than the canonical value with pvalue sim 108 and sim 105 respectively. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.06040', '2024arXiv240906040L', 'arXiv:2409.06040'] | ['Astrophysics - Astrophysics of Galaxies', 'Statistics - Applications'] | Discovery of Two UltraDiffuse Galaxies with Unusually Bright Globular Cluster Luminosity Functions via a MarkDependently Thinned Point Process MATHPOP | 2,024 | 340 | 0.52 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.06040.pdf |
2024arXiv240912271B | The new tools of gravitational wave and multimessenger astronomy allow for the study of astrophysical phenomenon in new ways and enables light to be shed on some of the longestenduring mysteries of highenergy astrophysics. Among the latter stands the Galactic center gammaray excess associated with a source whose nature could be annihilating dark matter or a yetunresolved population of millisecond pulsars MSPs. MSPs are most likely asymmetric about their axis of rotation and are thus thought to also source quasimonochromatic gravitational waves that dark matter processes would not emit. Using statistical methods we simulate realistic MSP population samples with differing morphology and moment of inertia that could give rise to the gammaray excess and we compute the corresponding gravitational wave signal amplitude and frequency. We find that the gravitational wave signal frequency likely ranges between sim200 and 1400 Hz and that the collective dimensionless strain from the center of the Galaxy has an amplitude between 1026 and 1024 thus most likely beyond current and nearterm detectors unless the unresolved MSPs are extraordinarily gammaray dim. | 2024-09-01T00:00:00Z | ['2024arXiv240912271B', 'arXiv:2409.12271', '10.48550/arXiv.2409.12271'] | ['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | On the Gravitational Wave Counterpart to a Gammaray Galactic Center Signal from Millisecond Pulsars | 2,024 | 340 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.12271.pdf |
2024A&A...691A..53S | Aims. SWEETCat Stars With ExoplanETs Catalog was originally introduced in 2013 and since then the number of confirmed exoplanets has increased significantly. A crucial step for a comprehensive understanding of these new worlds is the precise and homogeneous characterization of their host stars. Methods. We used a large number of highresolution spectra to continue the addition of new stellar parameters for planethosting stars in SWEETCat following the new detection of exoplanets listed both in the Extrasolar Planets Encyclopedia and in the NASA exoplanet archive. We obtained highresolution spectra for a significant number of these planethosting stars either observed by our team or collected through public archives. For FGK stars the spectroscopic stellar parameters were derived for the spectra following the same homogeneous process using ARESMOOG as for the previous SWEETCat releases. The stellar properties were combined with the planet properties to study possible correlations that could shed more light on the starplanet connection studies. Results. We have increased the number of stars with homogeneous parameters by 232 25 from 959 to 1191. We focus on the exoplanets that have had both mass and radius determined to review the massradius relation and we find results consistent with the ones previously reported in the literature. For the massive planets we also revisit the radius anomaly confirming a metallicity correlation for the radius anomaly already hinted at in previous results. | 2024-11-01T00:00:00Z | ['arXiv:2409.11965', '10.48550/arXiv.2409.11965', '10.1051/0004-6361/202451704', '2024arXiv240911965S', '2024A&A...691A..53S'] | ['planets and satellites: formation', 'planets and satellites: fundamental parameters', 'stars: abundances', 'stars: fundamental parameters', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics'] | SWEETCat A view on the planetary massradius relation | 2,024 | 340 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 1 | https://arxiv.org/pdf/2409.11965.pdf |
2024arXiv240913010S | The way in which the largescale cosmic environment affects galactic properties is not yet understood. Dark matter halos which embed galaxies initially evolve following linear theory. Their subsequent evolution is driven by nonlinear structure formation in the halo region and in its outer environment. In this work we present the first study where we explicitly control the linear part of the evolution of the halo thus revealing the role of nonlinear effects on halo formation. We focus specifically on the effect of proximity to a large cosmological filament. We employ the splicing method to keep fixed the initial density velocity and potential fields where a halo will form while changing its outer environment from an isolated state to one where the halo is near a large filament. In the regime of Milky Waymass halos we find that mass and virial radius of such halos are not affected by even drastic changes of environment whereas halo spin and shape orientation with respect to a massive filament is largely impacted with fluctuations of up to 80 around the mean value. Our results suggest that halo orientation and shape cannot be predicted accurately from a local analysis in the initial conditions alone. This has direct consequences on the modeling of intrinsic alignment for cosmic shear surveys like Euclid. Our results highlight that nonlinear couplings to the largescale environment may have an amplitude comparable to linear effects and should thus be treated explicitly in analytical models of dark matter halo formation. | 2024-09-01T00:00:00Z | ['arXiv:2409.13010', '2024arXiv240913010S', '10.48550/arXiv.2409.13010'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies'] | The causal effect of cosmic filaments on dark matter halos | 2,024 | 342 | 0.52 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.13010.pdf |
2024arXiv240911448F | We explore indefinite causal order between events in the context of quasiclassical spacetimes in superposition. We introduce several new quantifiers to measure the degree of indefiniteness of the causal order for an arbitrary finite number of events and spacetime configurations in superposition. By constructing diagrammatic and knottheoretic representations of the causal order between events we find that the definiteness or maximal indefiniteness of the causal order is topologically invariant. This reveals an intriguing connection between the field of quantum causality and knot theory. Furthermore we provide an operational encoding of indefinite causal order and discuss how to incorporate a measure of quantum coherence into our classification. | 2024-09-01T00:00:00Z | ['2024arXiv240911448F', '10.48550/arXiv.2409.11448', 'arXiv:2409.11448'] | ['General Relativity and Quantum Cosmology', 'High Energy Physics - Theory', 'Quantum Physics'] | Knot invariants and indefinite causal order | 2,024 | 345 | 0.17 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.11448.pdf |
2024arXiv240911818R | This brief review is based on a lecture given by one of the authors at the international youth conference AYSS2023. It is devoted to multimessenger astronomy which studies astrophysical objects and phenomena using various particles and waves that bring information from space. The messengers include electromagnetic and gravitational waves neutrinos and cosmic rays. We discuss new opportunities that open up with the combined use of several carriers of information. Combination of data obtained through various observation channels allows one to obtain more complete and accurate information about the processes occurring in the Universe and even to use it for studying fundamental physics. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.11818', 'arXiv:2409.11818', '2024arXiv240911818R'] | ['Astrophysics - High Energy Astrophysical Phenomena'] | Multimessenger astronomy | 2,024 | 348 | 0.41 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.11818.pdf |
2024arXiv240905716S | Recent largescale structure LSS surveys have revealed a persistent tension in the value of S8 compared to predictions from the standard cosmological model. This tension may suggest the need for new physics beyond the standard model but an accurate characterisation of baryonic effects is essential to avoid biases. Although some studies indicate that baryonic effects are too small to resolve this tension others propose that more aggressive feedback mechanisms could reconcile differences between cosmic microwave background CMB measurements and lowredshift LSS observations. In this paper we investigate the role of baryonic effects in alleviating the S8 tension. We extend the SPk model Salcido et al. 2023 which was trained on hundreds of cosmological hydrodynamical simulations to map the suppression of the matter power spectrum to the baryon fraction in groups and clusters to predict the required baryon fraction for a given Pk suppression. We then compare predictions from recent cosmic shear weak lensing analyses with the latest baryon budget measurements from Xray and weak gravitational lensing studies. Our findings show that studies marginalising over baryonic effects while fixing cosmological parameters to a Plancklike cosmology predict strong Pk suppression and baryon fractions that are much lower than existing lowredshift baryon budget estimates of galaxy groups and clusters. Conversely most studies that marginalise over both cosmological parameters and baryonic effects imply baryon fractions that are consistent with observations but lower values of S8 than inferred from the CMB. Unless the observed baryon fractions are biased high by a factor of several these results suggest that a mechanism beyond baryonic physics alone is required to modify or slow down the growth of structure in the universe in order to resolve the S8 tension. | 2024-09-01T00:00:00Z | ['arXiv:2409.05716', '2024arXiv240905716S', '10.48550/arXiv.2409.05716'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Implications of feedback solutions to the S8 tension for the baryon fractions of galaxy groups and clusters | 2,024 | 348 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 5 | https://arxiv.org/pdf/2409.05716.pdf |
2024arXiv240907851K | We study multicomponent dark matter scenarios and the Galactic 511 keV gammaray emission line signal in the framework of a local dark U1D extension of the Standard Model. A light vector dark matter particle associated with the dark U1D may decay and annihilate to electronpositron pairs. The produced positrons may in turn form positroniums that subsequently annihilate to two photons accounting for the observed line signal of the Galactic 511 keV gammaray emission. Three scenarios are investigated. First we consider the minimal U1D extension where a dark gauge boson and a dark Higgs boson are newly introduced to the particle content. As a second scenario we consider WIMPtype dark matter with the introduction of an extra dark fermion which in addition to the dark gauge boson may contribute to the dark matter relic abundance. It is thus a multicomponent dark matter scenario with a UVcomplete dark U1D symmetry. In particular the vector dark matter may account for a small fraction of the total dark matter relic abundance. Finally we consider the scenario where the dark matter particles are of the FIMPtype. In this case both the light vector and fermion dark matter particles may be produced via the freezein and superWIMP mechanisms. Considering theoretical and observational constraints we explore the allowed parameter space where the Galactic 511 keV gammaray line signal and the dark matter relic can both be explained. We also discuss possible observational signatures. | 2024-09-01T00:00:00Z | ['2024arXiv240907851K', '10.48550/arXiv.2409.07851', 'arXiv:2409.07851'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Multicomponent dark matter and Galactic 511 keV gammaray emission | 2,024 | 349 | 0.46 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07851.pdf |
2024arXiv240906760A | We introduce a set of special functions called multiple polyexponential integrals defined as iterated integrals of the exponential integral textEiz. These functions arise in certain perturbative expansions of the local solutions of secondorder ODEs around an irregular singularity. In particular their recursive definition describes the asymptotic behavior of these local solutions. To complement the study of the multiple polyexponential integrals on the entire complex plane we relate them with two other sets of special functions the undressed and dressed multiple polyexponential functions which are characterized by their Taylor series expansions around the origin. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.06760', '2024arXiv240906760A', 'arXiv:2409.06760'] | ['Mathematics - Classical Analysis and ODEs', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Theory', 'Mathematical Physics'] | Basics of Multiple Polyexponential Integrals | 2,024 | 350 | 0.23 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.06760.pdf |
2024AJ....168..179L | The discovery and characterization of freefloating planetarymass objects FFPMOs is fundamental to our understanding of star and planet formation. Here we report results from an extremely deep spectroscopic survey of the young star cluster NGC1333 using NearInfraRed Imager and Slitless Spectrograph NIRISS wide field slitless spectroscopy on the James Webb Space Telescope. The survey is photometrically complete to K 21 and includes useful spectra for objects as faint as K 20.5. The observations cover 19 known brown dwarfs for most of which we confirm spectral types using NIRISS spectra. We discover six new candidates with Ldwarf spectral types that are plausible planetarymass members of NGC1333 with estimated masses between 5 and 15 M SUBJupSUB. One at 5 M SUBJupSUB shows clear infrared excess emission and is a good candidate to be the lowestmass object known to have a disk. We do not find any objects later than midL spectral type M 4 M SUBJupSUB. The paucity of Jupitermass objects despite the surveys unprecedented sensitivity suggests that our observations reach the lowestmass objects that formed like stars in NGC1333. Our findings put the fraction of FFPMOs in NGC1333 at 10 of the number of cluster members significantly more than expected from the typical lognormal stellar mass function. We also search for wide binaries in our images and report a young brown dwarf with a planetarymass companion. | 2024-10-01T00:00:00Z | ['2024AJ....168..179L', '2024arXiv240812639L', 'arXiv:2408.12639', '10.48550/arXiv.2408.12639', '10.3847/1538-3881/ad6f0c'] | ['Brown dwarfs', 'L dwarfs', 'T dwarfs', 'Free floating planets', 'Star formation', 'Star forming regions', 'Planet formation', 'Circumstellar disks', '185', '894', '1679', '549', '1569', '1565', '1241', '235', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Solar and Stellar Astrophysics'] | The JWSTNIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Freefloating Planets | 2,024 | 350 | 0.65 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2 | https://arxiv.org/pdf/2408.12639.pdf |
2013PASP..125..306F | We introduce a stable well tested Python implementation of the affineinvariant ensemble sampler for Markov chain Monte Carlo MCMC proposed by Goodman amp Weare 2010. The code is open source and has already been used in several published projects in the astrophysics literature. The algorithm behind emcee has several advantages over traditional MCMC sampling methods and it has excellent performance as measured by the autocorrelation time or function calls per independent sample. One major advantage of the algorithm is that it requires handtuning of only 1 or 2 parameters compared to NSUP2SUP for a traditional algorithm in an Ndimensional parameter space. In this document we describe the algorithm and the details of our implementation. Exploiting the parallelism of the ensemble method emcee permits any user to take advantage of multiple CPU cores without extra effort. The code is available online at A hrefhttpdan.iel.fmemceehttpdan.iel.fmemceeA under the GNU General Public License v2. | 2013-03-01T00:00:00Z | ['2012arXiv1202.3665F', '10.1086/670067', 'arXiv:1202.3665', '10.48550/arXiv.1202.3665', '2013PASP..125..306F'] | ['Astrophysics - Instrumentation and Methods for Astrophysics', 'Physics - Computational Physics', 'Statistics - Computation'] | emcee The MCMC Hammer | 2,013 | 351 | 0.84 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 9,888 | https://arxiv.org/pdf/1202.3665.pdf |
2024A&A...691A..70N | The Milky Ways Central Molecular Zone CMZ differs dramatically from our local solar neighbourhood both in the extreme interstellar medium conditions it exhibits e.g. high gas stellar and feedback density and in the strong dynamics at play e.g. due to shear and gas influx along the bar. Consequently it is likely that there are largescale physical structures within the CMZ that cannot form elsewhere in the Milky Way. In this paper we present new results from the Atacama Large Millimetersubmillimeter Array ALMA large programme ACES ALMA CMZ Exploration Survey and conduct a multiwavelength and kinematic analysis to determine the origin of the M0.80.2 ring a molecular cloud with a distinct ringlike morphology. We estimate the projected inner and outer radii of the M0.80.2 ring to be 79 and 154 respectively 3.1 pc and 6.1 pc at an assumed Galactic Centre distance of 8.2 kpc and calculate a mean gas density gt10SUP4SUP cmSUP3SUP a mass of 10SUP6SUP MSUBSUB and an expansion speed of 20 km sSUP1SUP resulting in a high estimated kinetic energy gt10SUP51SUP erg and momentum gt10SUP7SUP MSUBSUB km sSUP1SUP. We discuss several possible causes for the existence and expansion of the structure including stellar feedback and largescale dynamics. We propose that the most likely cause of the M0.80.2 ring is a single highenergy hypernova explosion. To viably explain the observed morphology and kinematics such an explosion would need to have taken place inside a dense very massive molecular cloud the remnants of which we now see as the M0.80.2 ring. In this case the structure provides an extreme example of how supernovae can affect molecular clouds. | 2024-11-01T00:00:00Z | ['10.48550/arXiv.2409.12185', '10.1051/0004-6361/202451190', '2024A&A...691A..70N', 'arXiv:2409.12185', '2024arXiv240912185N'] | ['ISM: bubbles', 'ISM: clouds', 'ISM: kinematics and dynamics', 'ISM: supernova remnants', 'Galaxy: center', 'Astrophysics - Astrophysics of Galaxies'] | Disruption of a massive molecular cloud by a supernova in the Galactic Centre Initial results from the ACES project | 2,024 | 353 | 0.61 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3 | https://arxiv.org/pdf/2409.12185.pdf |
2024A&A...690A.332S | Fast radio bursts FRBs are bright extragalactic transients likely produced by magnetars. We study the propagation of FRBs in magnetar winds assuming that the wind is strongly magnetized and composed of electronpositron pairs. We focused on the regime where the strength parameter of the radio wave aSUB0SUB is larger than unity and the wave frequency SUB0SUB is larger than the Larmor frequency in the background magnetic field SUBLSUB. We show that strong radio waves with aSUB0SUB gt 1 are able to propagate when SUB0SUB gt aSUB0SUBSUBLSUB as the plasma current is a linear function of the wave electric field. The dispersion relation is independent of the wave strength parameter when SUB0SUB gt aSUB0SUBSUBLSUB. Radio waves could instead be damped when SUB0SUB lt aSUB0SUBSUBLSUB as a significant fraction of the wave energy is used to compress the plasma and amplify the background magnetic field. Our results suggest that FRBs should be produced at large distances from the magnetar i.e. R gt 10SUP12SUP cm where the condition SUB0SUB gt aSUB0SUBSUBLSUB is satisfied. Alternatively the structure of the magnetar wind should be strongly modified during a flare to allow for the escape of FRBs produced at radii R lt 10SUP12SUP cm. | 2024-10-01T00:00:00Z | ['2024A&A...690A.332S', '10.1051/0004-6361/202451725', '2024arXiv240910732S', 'arXiv:2409.10732', '10.48550/arXiv.2409.10732'] | ['plasmas', 'waves', 'stars: magnetars', 'Astrophysics - High Energy Astrophysical Phenomena', 'Physics - Plasma Physics'] | Escape of fast radio bursts from magnetars | 2,024 | 354 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2 | https://arxiv.org/pdf/2409.10732.pdf |
2024ApJ...976...83K | The redshiftdependent relation between galaxy stellar mass and star formation rate SFR known as the starforming sequence SFS is a key observational yardstick for galaxy assembly. We use the SAGAbgA sample of background galaxies from the Satellites Around Galactic Analogs SAGA Survey to model the lowredshift evolution of the lowmass SFS. The sample is comprised of 23258 galaxies with Hbased SFRs spanning inlineformula mmlmath overflowscrollmmlmn6mmlmnmmlmoltmmlmommlmsubmmlmilogmmlmimmlmn10mmlmnmmlmsubmmlmo stretchyfalsemmlmommlmsubmmlmiMmmlmimmlmommlmommlmsubmmlmo stretchytruemmlmommlmo stretchyfalsemmlmommlmsubmmlmiMmmlmimmlmommlmommlmsubmmlmo stretchyfalsemmlmommlmo stretchyfalsemmlmommlmoltmmlmommlmn10mmlmnmmlmath inlineformula and z lt 0.21 t lt 2.5 Gyr. Although it is common to bin or stack galaxies at z 0.2 for galaxy population studies the difference in lookback time between z 0 and z 0.21 is comparable to the time between z 1 and z 2. We develop a model to account for both the physical evolution of lowmass SFS and the selection function of the SAGA Survey allowing us to disentangle redshift evolution from redshiftdependent selection effects across the SAGAbgA redshift range. Our findings indicate significant evolution in the SFS over the last 2.5 Gyr with a rising normalization inlineformula mmlmath overflowscrollmmlmo stretchyfalseltmmlmommlmiSFRmmlmimmlmo stretchyfalsemmlmommlmsubmmlmiMmmlmimmlmommlmommlmsubmmlmommlmommlmsupmmlmn10mmlmnmmlmn8.5mmlmnmmlmsupmmlmsubmmlmiMmmlmimmlmommlmommlmsubmmlmo stretchyfalsemmlmommlmo stretchyfalsegtmmlmommlmo stretchyfalsemmlmommlmizmmlmimmlmo stretchyfalsemmlmommlmommlmommlmsubsupmmlmn1.24mmlmnmmlmrowmmlmommlmommlmn0.23mmlmnmmlmrowmmlmrowmmlmommlmommlmn0.25mmlmnmmlmrowmmlmsubsupmmlmspace width0.33emmmlmspacemmlmizmmlmimmlmommlmommlmsubsupmmlmn1.47mmlmnmmlmrowmmlmommlmommlmn0.03mmlmnmmlmrowmmlmrowmmlmommlmommlmn0.03mmlmnmmlmrowmmlmsubsupmmlmath inlineformula. We also identify the redshift limit at which a static SFS is ruled out at the 95 confidence level which is z 0.05 based on the precision of the SAGAbgA sample. Comparison with cosmological hydrodynamic simulations reveals that some contemporary simulations underpredict the recent evolution of the lowmass SFS. This demonstrates that the recent evolution of the lowmass SFS can provide new constraints on the assembly of the lowmass Universe and highlights the need for improved models in this regime. | 2024-11-01T00:00:00Z | ['10.48550/arXiv.2409.12221', '2024arXiv240912221K', '2024ApJ...976...83K', '10.3847/1538-4357/ad8137', 'arXiv:2409.12221'] | ['Dwarf galaxies', 'Star formation', 'Galaxy evolution', '416', '1569', '594', 'Astrophysics - Astrophysics of Galaxies'] | SAGAbg. II. The Lowmass Starforming Sequence Evolves Significantly between 0.05 lt z lt 0.21 | 2,024 | 354 | 0.56 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 1 | https://arxiv.org/pdf/2409.12221.pdf |
2024arXiv240910613N | Recent observations by the James Webb Telescope JWST have unveiled numerous galaxy candidates between z sim 9 16.5 hinting at an overabundance of the brightend of the UV Luminosity Function UV LF z gtrsim 11. Possible solutions require extremely bursty star formation these systems being dustfree an evolving initial mass function or even cosmic variance. In this work we develop an analytic formalism to study dust enrichment and its impact on the UV luminosity of both mainsequence early galaxies and extremely bursty star formers. Our dust model including the key processes of dust production in type II Supernovae dust destruction ejection growth and sputtering is calibrated against the latest datasets from the Atacama Large Millimeter Array ALMA at z sim 47. The model has only 3 free parameters i the star formation efficiency ii the dust growth timescale and iii the dust distribution radius. Our key results are i explaining the observed UV LF requires an average star formation efficiency that increases with redshift as fz 100.13z3.5 at z sim 513 with a number of observations hinting at objects lying a factor 10 above this mainsequence. ii The dust enrichment of early systems is driven by dust production in SNII ejecta growth and sputtering are the second and third most crucial processes impacting the dust mass by 60 and 40 respectively at z sim 7. iii In our model galaxies at z gtrsim 9 can still host significant amounts of dust reaching average dusttostellar mass ratios of 0.19 0.14 at z sim 9 z sim 11. Dust attenuation decreases with redshift due to dust being increasingly more dispersed within the halo. iv the galaxies observed by ALMA at z sim 7 comprise a biased sample that is not representative of the average population that makes up the UV LF. | 2024-09-01T00:00:00Z | ['2024arXiv240910613N', '10.48550/arXiv.2409.10613', 'arXiv:2409.10613', '2024arXiv240910613P'] | ['Astrophysics - Astrophysics of Galaxies'] | A phenomenological model for bright galaxies in the highredshift Universe | 2,024 | 354 | 0.51 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.10613.pdf |
2024MNRAS.534.2244F | Due to their short orbital periods and relatively highflux ratios irradiated brown dwarfs in binaries with white dwarfs offer better opportunities to study irradiated atmospheres than hot Jupiters which have lower planettostar flux ratios. WD1032011 is an eclipsing tidally locked white dwarfbrown dwarf binary with a 9950 K white dwarf orbited by a 69.7 Minlineformulatexmath idTM0001 notationLaTeXtextJuptexmathinlineformula brown dwarf in a 0.09 d orbit. We present timeresolved Hubble Space Telescope Wide Field Camera 3 spectrophotometric data of WD1032011. We isolate the phasedependent spectra of WD1032011B finding a 210 K difference in brightness temperature between the dayside and nightside. The spectral type of the brown dwarf is identified as L1 peculiar with atmospheric retrievals and comparison to field brown dwarfs showing evidence for a cloudfree atmosphere. The retrieved temperature of the dayside is 1748inlineformulatexmath idTM0002 notationLaTeX6667texmathinlineformula K with a nightside temperature of 1555inlineformulatexmath idTM0003 notationLaTeX7662texmathinlineformula K showing an irradiationdriven temperature contrast coupled with inefficient heat redistribution from the dayside to the nightside. The brown dwarf radius is inflated likely due to the constant irradiation from the white dwarf making it the only known inflated brown dwarf in an eclipsing white dwarfbrown dwarf binary. | 2024-11-01T00:00:00Z | ['2024arXiv240906874F', '10.1093/mnras/stae2121', '2024MNRAS.534.2244F', '2024MNRAS.tmp.2095F', 'arXiv:2409.06874', '10.48550/arXiv.2409.06874'] | ['Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Earth and Planetary Astrophysics'] | The only inflated brown dwarf in an eclipsing white dwarfbrown dwarf binary WD1032011B | 2,024 | 355 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.06874.pdf |
2017ApJ...848L..12A | On 2017 August 17 a binary neutron star coalescence candidate later designated GW170817 with merger time 124104 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gammaray Burst Monitor independently detected a gammaray burst GRB 170817A with a time delay of 1.7 s with respect to the merger time. From the gravitationalwave signal the source was initially localized to a sky region of 31 degSUP2SUP at a luminosity distance of 40SUB8SUBSUP8SUP Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 MSUB SUB. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient SSS17a now with the IAU identification of AT 2017gfo in NGC 4993 at 40 Mpc less than 11 hours after the merger by the OneMeter Two Hemisphere 1M2H team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over 10 days. Following early nondetections Xray and radio emission were discovered at the transients position 9 and 16 days respectively after the merger. Both the Xray and radio emission likely arise from a physical process that is distinct from the one that generates the UVopticalnearinfrared emission. No ultrahighenergy gammarays and no neutrino candidates consistent with the source were found in followup searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gammaray burst GRB 170817A and a kilonovamacronova powered by the radioactive decay of rprocess nuclei synthesized in the ejecta. P Any correspondence should be addressed to . | 2017-10-01T00:00:00Z | ['10.3847/2041-8213/aa91c9', '2017ApJ...848L..12A', '10.48550/arXiv.1710.05833', 'arXiv:1710.05833', '2017arXiv171005833L'] | ['gravitational waves', 'stars: neutron', 'Astrophysics - High Energy Astrophysical Phenomena', 'General Relativity and Quantum Cosmology'] | Multimessenger Observations of a Binary Neutron Star Merger | 2,017 | 356 | 0.8 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3,398 | https://arxiv.org/pdf/1710.05833.pdf |
2024A&A...690A.391B | The escaping ionising efficiency from galaxies fSUBescSUBSUBionSUB is a crucial ingredient for understanding their contribution to hydrogen reionisation but both of its components fSUBescSUB and SUBionSUB are extremely difficult to measure. We measured the average escaping ionising efficiency fSUBescSUBSUBionSUB of galaxies at z 5 implied by the mean level of ionisation in the intergalactic medium via the Lyman forest. We used the fact that NSUBionSUB SUBUVSUB fSUBescSUB SUBionSUB ltinlineformula idFI1gt ltalternativesgt mmlmath xmlnsmmlhttpwww.w3.org1998MathMathML displayinline idmmleq1 mmlmrow mmlmsub mmlmover accenttrue mmlmiNmmlmi mmlmommlmo mmlmover mmlmi mathvariantnormalionmmlmi mmlmsub mmlmommlmo mmlmsub mmlmimmlmi mmlmi mathvariantnormalUVmmlmi mmlmsub mmlmsub mmlmifmmlmi mmlmi mathvariantnormalescmmlmi mmlmsub mmlmsub mmlmimmlmi mmlmi mathvariantnormalionmmlmi mmlmsub mmlmrow mmlmath texmath idtexeq1ltCDATA dotNmathrmion rhomathrmUV fmathrmesc ximathrmion gttexmath ltinlinegraphic xmlnsxlinkhttpwww.w3.org1999xlink idimgeq1 mimesubtypegif mimetypeimage xlinkhrefaa5146324eq1.gifgt ltalternativesgt inlineformula the product of the ionising output and the UV density SUBUVSUB can be calculated from the known average strength of the UV background and the mean free path of ionising photons. These quantities as well as SUBUVSUB are robustly measured at z 6. We calculated the missing factor of fSUBescSUBSUBionSUB at z 5 during a convenient epoch after hydrogen reionisation had been completed and the intergalactic medium had reached ionisation equilibrium but before bright quasars began to dominate the ionising photon production. Intuitively our constraint corresponds to the required escaping ionising production from galaxies in order to avoid over or underionising the Lyman forest. We obtained a measurement of logfSUBescSUBSUBionSUBerg HzSUP1SUP 24.28SUP0.21SUPSUB0.20SUB ltinlineformula idFI2gt ltalternativesgt mmlmath xmlnsmmlhttpwww.w3.org1998MathMathML displayinline idmmleq2 mmlmrow mmlmsup mmlmrow mmlmrow mmlmommlmo mmlmn1mmlmn mmlmrow mmlmsup mmlmommlmo mmlmn24mmlmn mmlmo.mmlmo mmlmsubsup mmlmn28mmlmn mmlmrow mmlmommlmo mmlmn0.20mmlmn mmlmrow mmlmrow mmlmommlmo mmlmn0.21mmlmn mmlmrow mmlmsubsup mmlmrow mmlmath texmath idtexeq2ltCDATA 1 24.280.200.21 gttexmath ltinlinegraphic xmlnsxlinkhttpwww.w3.org1999xlink idimgeq2 mimesubtypegif mimetypeimage xlinkhrefaa5146324eq2.gifgt ltalternativesgt inlineformula at z 5 when integrating the SUBUVSUB down to a limiting magnitude MSUBlimSUB 11. Our measurement of the escaping ionising efficiency of galaxies is in rough agreement with both observations of early galaxies and with most models. | 2024-10-01T00:00:00Z | ['10.1051/0004-6361/202451463', '2024arXiv240908315B', 'arXiv:2409.08315', '2024A&A...690A.391B', '10.48550/arXiv.2409.08315'] | ['galaxies: high-redshift', 'intergalactic medium', 'dark ages', 'reionization', 'first stars', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | A measurement of the escaping ionising efficiency of galaxies at redshift 5 | 2,024 | 356 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2 | https://arxiv.org/pdf/2409.08315.pdf |
2024arXiv240904517C | We provide the most complete analysis so far of quasinormal modes of rotating black holes in a general higherderivative extension of Einsteins theory. By finding the corrections to the Teukolsky equation and expressing them in a simple form we are able to apply a generalized continued fraction method that allows us to find the quasinormal mode frequencies including overtones. We obtain the leadingorder corrections to the Kerr quasinormal mode frequencies of all the lmn modes with l234 lle mle l and n012 and express them as a function of the black hole spin chi using polynomial fits. We estimate that our results remain accurate up to spins between chisim 0.7 and chisim 0.95 depending on the mode. We report that overtones are overall more sensitive to corrections which is expected from recent literature on this topic. We also discuss the limit of validity of the linear corrections to the quasinormal mode frequencies by estimating the size of nonlinear effects in the higherderivative couplings. All our results are publicly available in an online repository. | 2024-09-01T00:00:00Z | ['arXiv:2409.04517', '10.48550/arXiv.2409.04517', '2024arXiv240904517C'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - High Energy Astrophysical Phenomena', 'High Energy Physics - Theory'] | Higherderivative corrections to the Kerr quasinormal mode spectrum | 2,024 | 358 | 0.27 | ['EPRINT_HTML', 'EPRINT_PDF'] | 5 | https://arxiv.org/pdf/2409.04517.pdf |
2024arXiv240910846W | A massive black hole can develop a darkmatter overdensity and the dark matter changes the evolution of a stellarmass compact object inspiraling around the massive black hole through the dense darkmatter environment. Specifically dynamical friction speeds up the inspiral of the compact object and causes feedback on the darkmatter distribution. These intermediate massratio inspirals with dark matter are a source of gravitational waves GWs and the waves can dephase significantly from an equivalent system in vacuum. Prior work has shown that this dephasing needs to be modeled to detect the GWs from these systems with LISA the Laser Interferometer Space Antenna it also showed that the density and distribution of dark matter can be inferred from a GW measurement. In this paper we study whether the parametrized postEinsteinian ppE framework can be used to infer the presence of dark matter in these systems. We confirm that if vacuum waveform templates are used to model the GWs from an inspiral in a darkmatter halo then the resulting parameter estimation is biased. We then apply the ppE framework to determine whether it can reduce the parameterestimation biases and we find that adding one ppE phase term to a waveform template eliminates the parameterestimation biases statistical errors become larger than the systematic ones but the effective postNewtonian order in the ppE framework must be specified without uncertainties. When the postNewtonian order has uncertainty we find that the systematic errors on the ppE and the binarys parameters exceed the statistical errors. Thus the simplest ppE framework would not give unbiased results for these systems and a further extension of it or dedicated parameter estimation with gravitational waveforms that include darkmatter effects would be needed. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.10846', '2024arXiv240910846W', 'arXiv:2409.10846'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Probing darkmatter effects with gravitational waves using the parameterized postEinsteinian framework | 2,024 | 358 | 0.18 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.10846.pdf |
2024AsBio..24..856J | Rocky planets may acquire a primordial atmosphere by the outgassing of volatiles from their magma ocean. The distribution of O between HSUB2SUBO CO and COSUB2SUB in chemical equilibrium subsequently changes significantly with decreasing temperature. We consider here two chemical models one where CHSUB4SUB and NHSUB3SUB are assumed to be irrevocably destroyed by photolysis and second where these molecules persist. In the first case we show that CO cannot coexist with HSUB2SUBO since CO oxidizes at low temperatures to form COSUB2SUB and HSUB2SUB. In both cases H escapes from the thermosphere within a few 10 million years by absorption of stellar XUV radiation. This escape drives an atmospheric selfoxidation process whereby rocky planet atmospheres become dominated by COSUB2SUB and HSUB2SUBO regardless of their initial oxidation state at outgassing. HCN is considered a potential precursor of prebiotic compounds and RNA. Oxidizing atmospheres are inefficient at producing HCN by lightning. Alternatively we have demonstrated that lightningproduced NO which dissolves as nitrate in oceans and interplanetary dust particles may be the main sources of fixed nitrogen in emerging biospheres. Our results highlight the need for originoflife scenarios where the first metabolism fixes its C from COSUB2SUB rather than from HCN and CO. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.11070', '2024arXiv240911070J', 'arXiv:2409.11070', '2024AsBio..24..856J', '10.1089/ast.2023.0104'] | ['Earth—Meteorites', 'meteors', 'meteoroids—Planets and satellites: formation—Planets and satellites: atmospheres—Planets and satellites: composition—Planets and satellites: terrestrial planets', 'Astrophysics - Earth and Planetary Astrophysics'] | SelfOxidation of the Atmospheres of Rocky Planets with Implications for the Origin of Life | 2,024 | 358 | 0.45 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 1 | https://arxiv.org/pdf/2409.11070.pdf |
2024MNRAS.533.3517Q | We use the latest data set of supernova SN host galaxies to investigate how the host properties stellar mass star formation rate SFR metallicity absolute magnitude and colourdiffer across SN types with redshiftdriven selection effects controlled. SN Ib and Ic host galaxies on average are more massive metalrich and redder than SN II hosts. For subtypes SN Ibn and IcBL have bluer hosts than their normal SN Ib and Ic siblings SN IIb has consistent host properties with SN Ib while hosts of SN IIn are more metalrich than those of SN II. Hydrogendeficient superluminous SNe feature bluer and lower luminosity hosts than most subtypes of corecollapse supernova CC SN. Assuming simple proportionality of CC SN rates and host SFRs does not recover the observed mean host properties either a population of longlived progenitors or a metallicitydependent SN production efficiency better reproduces the observed host properties. Assuming the latter case the rates of SN II are insensitive to host metallicity but the rates of SN Ib and Ic are substantially enhanced in metalrich hosts by a factor of inlineformulatexmath idTM0001 notationLaTeXsim 10texmathinlineformula per dex increase in metallicity. Hosts of SN Ia are diverse in their observed properties subtypes including SN Ia91T Ia02cx and IaCSM prefer starforming hosts while subtypes like SN Ia91bg and Carich prefer quiescent hosts. The rates of SN Ia91T Ia02cx and IaCSM are closely dependent on or even proportional to their host SFRs indicating relatively shortlived progenitors. Conversely the rates of SN Ia91bg and Carich transients are proportional to the total stellar mass favouring longlived progenitors. | 2024-09-01T00:00:00Z | ['10.1093/mnras/stae1921', '2024MNRAS.533.3517Q', '10.48550/arXiv.2409.11461', 'arXiv:2409.11461', '2024arXiv240911461Q', '2024MNRAS.tmp.1874Q'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Solar and Stellar Astrophysics'] | Linking transients to their host galaxies II. A comparison of host galaxy properties and rate dependencies across supernova types | 2,024 | 358 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 1 | https://arxiv.org/pdf/2409.11461.pdf |
2024arXiv240906713F | Relativistic charged particle beam can be used as destructive beam weapons in space for debris removal tasks. The trajectories of charged particles are affected by both electric and magnetic forces in the Earths magnetic field. In this paper we firstly analyzed the correlation parameters of the charged particle beam as a weapon when it propagated in the geomagnetic field. Then the models were constructed based on COMSOL Multiphysics and the IGRF model was adopted in the simulation. The gyroradius and the related uncertainty were analyzed by simulation of the charged particle transport in the geomagnetic field at different altitudes. The charged beam spot radius divergency was also simulated. The magnetic field pinch effect can be found and can limit the beam spreading. | 2024-08-01T00:00:00Z | ['10.48550/arXiv.2409.06713', 'arXiv:2409.06713', '2024arXiv240906713F'] | ['Physics - Space Physics', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'High Energy Physics - Phenomenology'] | Study of the relativistic charged particle beam propagation in Earths magnetic field | 2,024 | 359 | 0.24 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.06713.pdf |
2024arXiv240910651K | The detection of the gravitationalwave event GW230529 presumably a neutron starblack hole NSBH merger by the LIGOVirgoKAGRA LVK Collaboration is an exciting discovery for multimessenger astronomy. The black hole BH has a high probability of falling within the mass gap between the peaks of the neutron star NS and the BH mass distributions. Because of the low primary mass the binary is more likely to produce an electromagnetic counterpart than previously detected NSBH mergers. We investigate the possible kilonova KN emission from GW230529 and find that if it was an NSBH there is a sim 241 probability depending on the assumed equation of state that GW230925 produced a KN with magnitude peaking at sim 12 day post merger at g lesssim 23.5 ilt23. Hence it could have been detected by groundbased telescopes. If it was a binary neutron star BNS merger we find sim 012 probability that it produced a KN. Motivated by these numbers we simulated a broader population of mgNSBH mergers that may be detected in O4 and we obtained a 921 chance of producing a KN which would be detectable with glesssim 25 and i lesssim 24 typically fainter than what is expected from GW230529. Based on these findings DECamlike instruments may be able to detect up to 80 of future mgNSBH KNe thus up to sim1 multimessenger mgNSBH per year may be discoverable at the current level of sensitivity O4. | 2024-09-01T00:00:00Z | ['arXiv:2409.10651', '10.48550/arXiv.2409.10651', '2024arXiv240910651K'] | ['Astrophysics - High Energy Astrophysical Phenomena'] | Kilonova emission from GW230529 and mass gap neutron starblack hole mergers | 2,024 | 359 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.10651.pdf |
2024arXiv240403576K | We present a sample of 341 little red dots LRDs spanning the redshift range zsim211 using data from the CEERS PRIMER JADES UNCOVER and NGDEEP surveys. These sources are likely heavilyreddened AGN that trace a previouslyhidden phase of dustobscured black hole growth in the early Universe. Unlike past use of color indices to identify LRDs we employ continuum slope fitting using shifting bandpasses to sample the same restframe emission blueward and redward of the Balmer break. This approach allows us to identify LRDs over a wider redshift range and is less susceptible to contamination from galaxies with strong breaks that otherwise lack a rising red continuum. The redshift distribution of our sample increases at zlt8 and then undergoes a rapid decline at zsim4.5 which may tie the emergence and obscuration of these sources to the insideout growth that galaxies experience during this epoch. We find that LRDs are 23 dex more numerous than bright quasars at zsim57 but their number density is only 0.61 dex higher than Xray and UV selected AGN at these redshifts. Within our sample we have identified the first Xray detected LRDs at z3.1 and z4.66. An Xray spectral analysis confirms that these AGN are moderately obscured with logNrm Hrm cm2 of 23.30.41.3 and 22.720.130.16. Our analysis reveals that reddened AGN emission dominates their restoptical light while the restUV originates from their host galaxies. We also present NIRSpec followup spectroscopy of 17 LRDs that show broad emission lines consistent with AGN activity. The confirmed AGN fraction of our sample is 71 for sources with F444Wlt26.5. In addition we find three LRDs with narrow blueshifted Balmer absorption features in their spectra suggesting an outflow of highdensity low ionization gas from near the central engine of these faint red AGN. | 2024-04-01T00:00:00Z | ['2024arXiv240403576K', 'arXiv:2404.03576', '10.48550/arXiv.2404.03576'] | ['Astrophysics - Astrophysics of Galaxies'] | The Rise of Faint Red AGN at zgt4 A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields | 2,024 | 359 | 0.73 | ['EPRINT_HTML', 'EPRINT_PDF'] | 87 | https://arxiv.org/pdf/2404.03576.pdf |
2024A&A...691A.136L | Context. Current and future large surveys will produce unprecedented amounts of data. Realistic simulations have become essential for the design and development of these surveys as well as for the interpretation of the results. Aims. We present MAMBO a flexible and efficient workflow to build empirical galaxy and active galactic nucleus AGN mock catalogues that reproduce the physical and observational properties of these sources. Methods. We started with simulated dark matter DM haloes to preserve the link with the cosmic web and we populated them with galaxies and AGN using abundance matching techniques. We followed an empirical methodology using stellar mass functions host galaxy AGN mass functions and AGN accretion rate distribution functions studied at different redshifts to assign among other properties stellar masses the fraction of quenched galaxies or the AGN activity demography obscuration multiwavelength emission etc.. Results. As a proof test we applied the method to a Millennium DM lightcone of 3.14 deg2 up to a redshift of z 10 and down to stellar masses of 1075 MSUBSUB. We show that the AGN population from the mock lightcone presented here reproduces with good accuracy various observables such as stateoftheart luminosity functions in the Xray up to z7 and in the ultraviolet up to z5 opticalnearinfrared colourcolour diagrams and narrow emission line diagnostic diagrams. Finally we demonstrate how this catalogue can be used to make useful predictions for large surveys. Using Euclid as a case example we compute among other forecasts the expected surface densities of galaxies and AGN detectable in the Euclid HSUBESUB band. We find that Euclid might observe on HSUBESUB only about 107 and 8 107 type 1 and 2 AGN respectively and 2 109 galaxies at the end of its 14 679 deg2 Wide survey in good agreement with other published forecasts. | 2024-11-01T00:00:00Z | ['10.1051/0004-6361/202451509', 'arXiv:2409.06700', '10.48550/arXiv.2409.06700', '2024A&A...691A.136L', '2024arXiv240906700L'] | ['methods: numerical', 'methods: statistical', 'catalogs', 'surveys', 'galaxies: general', 'quasars: general', 'Astrophysics - Astrophysics of Galaxies'] | MAMBO An empirical galaxy and AGN mock catalogue for the exploitation of future surveys | 2,024 | 359 | 0.56 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2 | https://arxiv.org/pdf/2409.06700.pdf |
2024arXiv240907455L | We introduce genesismetallicity a gasphase metallicity measurement python software employing the direct and strongline methods depending on the available oxygen lines. The nonparametric strongline estimator is calibrated based on a kernel density estimate in the 4dimensional space of O2 O IIlambdalambda 372729Hbeta O3 O IIIlambda 5007Hbeta Hbeta equivalent width EWHbeta and gasphase metallicity 12 logOH. We use a calibration sample of 1551 galaxies at 0 lt z lt 10 with directmethod metallicity measurements compiled from the JWSTNIRSpec and groundbased observations. In particular we report 145 new NIRSpec directmethod metallicity measurements at z gt 1. We show that the O2 O3 and EWHbeta measurements are sufficient for a gasphase metallicity estimate that is more accurate than 0.09 dex. Our calibration is universal meaning that its accuracy does not depend on the target redshift. Furthermore the directmethod module employs a nonparametric teO II electron temperature estimator based on a kernel density estimate in the 5dimensional space of O2 O3 EWHbeta teO II and teO III. This teO II estimator is calibrated based on 1001 spectra with O IIIlambda 4363 and O IIlambdalambda 732030 detections notably reporting 30 new NIRSpec detections of the O IIlambdalambda 732030 doublet. We make genesismetallicity and its calibration data publicly available and commit to keeping both uptodate in light of the incoming data. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.07455', 'arXiv:2409.07455', '2024arXiv240907455L'] | ['Astrophysics - Astrophysics of Galaxies'] | GenesisMetallicity Universal NonParametric GasPhase Metallicity Estimation | 2,024 | 360 | 0.62 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07455.pdf |
2024arXiv240908318Z | TOI836 is a sim23 Gyr K dwarf with an inner super Earth R1.7Roplus P3.8d and an outer mini Neptune R2.6Roplus P8.6d. Recent JWSTNIRSpec 2.85.2 mum observations have revealed flat transmission spectra for both planets. We present KeckNIRSPEC observations of escaping helium from this system. While planet b shows no absorption in the 1083 nm line to deep limits lt0.2 836c shows strong 0.7 absorption in both visits. These results demonstrate that the inner superEarth has lost its primordial atmosphere while the outer miniNeptune has not. Selfconsistent 1D radiativehydrodynamic models of c using pyTPCI an updated version of The PLUTOCLOUDY Interface reveal that the helium signal is highly sensitive to metallicity its equivalent width collapses by a factor of 13 as metallicity increases from 10x to 100x solar and by a further factor of 12 as it increases to 200x solar. The observed equivalent width is 88 of the model prediction for 100x metallicity suggesting that c may have an atmospheric metallicity close to 100x solar. This is similar to K218b and TOI270d the first two miniNeptunes with detected absorption features in JWST transmission spectra. We highlight the helium triplet as a potentially powerful probe of atmospheric composition with complementary strengths and weaknesses to atmospheric retrievals. The main strength is its extreme sensitivity to metallicity in the scientifically significant range of 10200x solar and the main weakness is the enormous model uncertainties in outflow suppression and confinement mechanisms such as magnetic fields and stellar winds. | 2024-09-01T00:00:00Z | ['2024arXiv240908318Z', 'arXiv:2409.08318', '10.48550/arXiv.2409.08318'] | ['Astrophysics - Earth and Planetary Astrophysics'] | Constraining atmospheric composition from the outflow helium observations reveal the fundamental properties of two planets straddling the radius gap | 2,024 | 361 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.08318.pdf |
2024arXiv240906479C | We discuss a systematic way in which a relational dynamics can be established relative to periodic clocks both in the classical and quantum theories emphasising the parallels between them. We show that 1 classical and quantum relational observables that encode the value of a quantity relative to a periodic clock are only invariant along the gauge orbits generated by the Hamiltonian constraint if the quantity itself is periodic and otherwise the observables are only transiently invariant per clock cycle this implies in particular that counting winding numbers does not lead to invariant observables relative to the periodic clock 2 the quantum relational observables can be obtained from a partial group averaging procedure over a single clock cycle 3 there is an equivalence trinity between the quantum theories based on the quantum relational observables of the clockneutral picture of Dirac quantisation the relational Schrdinger picture of the PageWootters formalism and the relational Heisenberg picture that follows from quantum deparametrisation all three taken relative to periodic clocks implying that the dynamics in all three is necessarily periodic 4 in the context of periodic clocks the original PageWootters definition of conditional probabilities fails for systems that have a continuous energy spectrum and using the equivalence between the PageWootters and the clockneutral gaugeinvariant formalism must be suitably updated. Finally we show how a system evolving periodically with respect to a periodic clock can evolve monotonically with respect to an aperiodic clock without inconsistency. The presentation is illustrated by several examples and we conclude with a brief comparison to other approaches in the literature that also deal with relational descriptions of periodic clocks. | 2024-09-01T00:00:00Z | ['arXiv:2409.06479', '10.48550/arXiv.2409.06479', '2024arXiv240906479C'] | ['Quantum Physics', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Theory'] | Relational Dynamics with Periodic Clocks | 2,024 | 362 | 0.17 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.06479.pdf |
2024arXiv240912118F | One of the fundamental questions of cosmology is the origin and mechanisms responsible for the reionization of the Universe beyond zsim6. To address this question many studies over the past decade have focused on local zsim0.3 galaxies which leak ionizing radiation Lyman continuum or LyC. However lineofsight effects and data quality have prohibited deeper insight into the nature of LyC escape. To circumvent these limitations we analyze stacks of a consolidated sample of it HSTCOS observations of the LyC in 89 galaxies at zsim0.3. From fitting of the continuum we obtain information about the underlying stellar populations and neutral ISM geometry. We find that most LyC nondetections are not leaking appreciable LyC fescrm LyClt1 but also that exceptional cases point to spatial variations in the LyC escape fraction fescrm LyC. Stellar populations younger than 3 Myr lead to an increase in ionizing feedback which in turn increases the isotropy of LyC escape. Moreover mechanical feedback from supernovae in 810 Myr stellar populations is important for anisotropic gas distributions needed for LyC escape. While mechanical feedback is necessary for any LyC escape high fescrm LyC gt5 also requires a confluence of young stars and ionizing feedback. A twostage burst of star formation could facilitate this optimal LyC escape scenario. | 2024-09-01T00:00:00Z | ['arXiv:2409.12118', '2024arXiv240912118F', '10.48550/arXiv.2409.12118'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | The LowRedshift Lyman Continuum Survey The Roles of Stellar Feedback and ISM Geometry in LyC Escape | 2,024 | 363 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF'] | 6 | https://arxiv.org/pdf/2409.12118.pdf |
2024arXiv240906681A | We utilize three complementary approaches to pinpoint the exact form of scattering amplitudes in Schwarzschild spacetime. First we solve the ReggeWheeler equation perturbatively in the smallfrequency regime. We use the obtained solutions to determine the monodromy in the nearspatial infinity region which leads to a specific partial differential equation on the elements of the scattering matrix. As a result it can be written in terms of the elements of the infinitesimal generator of the monodromy transformation and an integration constant. This constant is further related to the NekrasovShatashvili free energy through the resummation of infinitely many instantons. The quasinormal mode frequencies are also studied in the smallfrequency approximation. | 2024-09-01T00:00:00Z | ['arXiv:2409.06681', '10.48550/arXiv.2409.06681', '2024arXiv240906681A'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology', 'Mathematical Physics'] | Black hole scattering amplitudes via analytic smallfrequency expansion and monodromy | 2,024 | 363 | 0.27 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.06681.pdf |
2014ARA&A..52..415M | Over the past two decades an avalanche of new data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Here we review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation heavy element production and reionization of the Universe from the cosmic dark ages to the present epoch. A consistent picture is emerging whereby the starformation rate density peaked approximately 3.5 Gyr after the Big Bang at z1.9 and declined exponentially at later times with an efolding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before a redshift z 1.3. About 25 formed before the peak of the cosmic starformation rate density and another 25 formed after z 0.7. Less than 1 of todays stars formed during the epoch of reionization. Under the assumption of a universal initial mass function the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding starformation activity. The comoving rates of star formation and central black hole accretion follow a similar rise and fall offering evidence for coevolution of black holes and their host galaxies. The rise of the mean metallicity of the Universe to about 0.001 solar by z 6 one Gyr after the Big Bang appears to have been accompanied by the production of fewer than ten hydrogen Lymancontinuum photons per baryon a rather tight budget for cosmological reionization. | 2014-08-01T00:00:00Z | ['10.48550/arXiv.1403.0007', 'arXiv:1403.0007', '2014ARA&A..52..415M', '2014arXiv1403.0007M', '10.1146/annurev-astro-081811-125615'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Cosmic StarFormation History | 2,014 | 363 | 0.8 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3,400 | https://arxiv.org/pdf/1403.0007.pdf |
2024arXiv240910471N | We study conversion processes between gravitons and dark photons and reveal the effects of dark photons on the polarization of gravitational waves. Considering cosmological dark magnetic fields we investigate the evolution of the intensity and polarization of gravitational waves through the conversion. Specifically we demonstrate that for minimal coupling between gravitons and dark photons the intensity circular polarization and linear polarization evolve separately. We derive explicit formulas for the statistical mean and variance of the intensity and polarization when the gravitational waves pass through magnetic fields with random orientation. The formulas capture how the initial polarization of dark photons will be imprinted on the observed gravitational wave background. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.10471', 'arXiv:2409.10471', '2024arXiv240910471N'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Imprints of Dark Photons on Gravitational Wave Polarizations | 2,024 | 363 | 0.28 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.10471.pdf |
2024arXiv240905482F | This study applied machine learning models to estimate stellar rotation periods from corrected light curve data obtained by the NASA Kepler mission. Traditional methods often struggle to estimate rotation periods accurately due to noise and variability in the light curve data. The workflow involved using initial period estimates from the LSPeriodogram and Transit Least Squares techniques followed by splitting the data into training validation and testing sets. We employed several machine learning algorithms including Decision Tree Random Forest KNearest Neighbors and Gradient Boosting and also utilized a Voting Ensemble approach to improve prediction accuracy and robustness. The analysis included data from multiple Kepler IDs providing detailed metrics on orbital periods and planet radii. Performance evaluation showed that the Voting Ensemble model yielded the most accurate results with an RMSE approximately 50 lower than the Decision Tree model and 17 better than the KNearest Neighbors model. The Random Forest model performed comparably to the Voting Ensemble indicating high accuracy. In contrast the Gradient Boosting model exhibited a worse RMSE compared to the other approaches. Comparisons of the predicted rotation periods to the photometric reference periods showed close alignment suggesting the machine learning models achieved high prediction accuracy. The results indicate that machine learning particularly ensemble methods can effectively solve the problem of accurately estimating stellar rotation periods with significant implications for advancing the study of exoplanets and stellar astrophysics. | 2024-09-01T00:00:00Z | ['arXiv:2409.05482', '10.48550/arXiv.2409.05482', '2024arXiv240905482F'] | ['Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'Computer Science - Machine Learning'] | Advancing Machine Learning for Stellar Activity and Exoplanet Period Rotation | 2,024 | 363 | 0.5 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.05482.pdf |
2024arXiv240909259T | We consider how charging performances of a quantum battery modeled as a twolevel system are influenced by the presence of vacuum fluctuations of a quantum field satisfying the Dirichlet transparent and Neumann boundary conditions in the BTZ spacetime. The quantum battery is subjected to an external static driving which works as a charger. Meanwhile the quantum field is assumed to be coupled to both longitudinal and transverse spin components of the quantum battery including decoherence and pure dephasing mechanisms. Charging and discharging dynamics of the quantum battery are derived by extending the previous open quantum system approach in the relativistic framework to this more general scenario including both the driving and multiple coupling. Analytic expressions for the time evolution of the energy stored are presented. We find that when the driving amplitude is strongerweaker than the energylevel spacing of the quantum battery the pure dephasing dissipative coupling results in betterworse charging performances than the decoherence dissipative coupling case. We also find that higher Hawking temperature helps to improve the charging performance under certain conditions compared with the closed quantum buttery case implying the feasibility of energy extraction from vacuum fluctuations in curved spacetime via dissipation in charging protocol. Different boundary conditions for quantum field may lead to different charging performance. Furthermore we also address the charging stability by monitoring the energy behaviour after the charging protocol has been switched off. Our study presents a general framework to investigate relaxation effects in curved spacetime and reveals how spacetime properties and field boundary condition affect the charging process which in turn may shed light on the exploration of the spacetime properties and thermodynamics via the charging protocol. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.09259', 'arXiv:2409.09259', '2024arXiv240909259T'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology', 'Quantum Physics'] | Dissipative dynamics of an open quantum battery in the BTZ spacetime | 2,024 | 364 | 0.26 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.09259.pdf |
2024A&A...691A.279M | We report the discovery of the Fe K line emission at 6.62SUB0.06SUBSUP0.06SUP keV with a width of 0.19SUB0.05SUBSUP0.05SUP keV using two epochs of Chandra archival data for the nucleus of the galaxy 4C37.11 which is known to host a binary supermassive black hole BSMBH system where the SMBHs are separated by 7 mas or 7pc. Our study reports the first detection of the Fe K line from a known binary AGN which has an Fstatistic value of 20.98 and a probability of 2.47 10SUP12SUP. Stacking two spectra reveals another Fe K line component at 7.87SUB0.09SUBSUP0.19SUP keV. Different model scenarios indicate that the lines originate from the combined effects of accretion disk emission and circumnuclear collisionally ionized medium. The observed low column density favors a gaspoor merger scenario where the high temperature of the hot ionized medium may be associated with the shocked gas in the binary merger and not with star formation activity. The estimated total BSMBH mass and disk inclination are 1.5 10SUP10SUP MSUBSUB and 75 indicating that the BSMBH is probably a highinclination system. We were not able to tightly constrain the spin parameter using the present data sets. Our results draw attention to the fact that detecting the Fe K line emissions from BSMBHs is important for estimating the individual SMBH masses and the spins of the binary SMBHs as well as for exploring their emission regions. | 2024-11-01T00:00:00Z | ['2024A&A...691A.279M', '2024arXiv240905717M', '10.1051/0004-6361/202450616', '10.48550/arXiv.2409.05717', 'arXiv:2409.05717'] | ['accretion', 'accretion disks', 'radiative transfer', 'Galaxy: nucleus', 'galaxies: interactions', 'galaxies: jets', 'Astrophysics - High Energy Astrophysical Phenomena'] | Detection of the Fe K lines from the binary AGN in 4C37.11 | 2,024 | 365 | 0.53 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.05717.pdf |
2024arXiv240908138F | In this paper we investigate the impact of loop quantum gravity LQG on extreme massratio inspirals EMRIs and the results indicate that LQG effects cause the orbital decay to occur faster compared to the Schwarzschild case. Furthermore we use the augmented analytic kludge approach to generate EMRI waveforms and study the LISAs capability to detect the LQG effect with faithfulness. Additionally employing the Fisher information matrix method for parameter estimation we estimate that after one year of observation the uncertainty in r0 reduces to approximately 6.59times 104 with a signaltonoise ratio of 49. | 2024-09-01T00:00:00Z | ['2024arXiv240908138F', 'arXiv:2409.08138', '10.48550/arXiv.2409.08138'] | ['General Relativity and Quantum Cosmology', 'High Energy Physics - Theory'] | Probing Quantum Gravity Effects with Eccentric Extreme MassRatio Inspirals | 2,024 | 365 | 0.33 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.08138.pdf |
2024arXiv240909290S | Using the FIRE2 cosmological zoomin simulations we investigate the temporal evolution of gasphase metallicity radial gradients of Milky Waymass progenitors in the redshift range of 0.4ltzlt3. We pay special attention to the occurrence of positive i.e. inverted metallicity gradients where metallicity increases with galactocentric radius. This trend contrary to the more commonly observed negative radial gradients has been frequently seen in recent spatially resolved grism observations. The occurrence rate of positive gradients in FIRE2 is about sim10 for 0.4ltzlt3 and sim16 at higher redshifts 1.5ltzlt3 broadly consistent with observations. Moreover we investigate the correlations among galaxy metallicity gradient stellar mass star formation rate SFR and degree of rotational support. Our results show that galaxies with lower mass higher specific SFR sSFR and more turbulent disks are more likely to exhibit positive metallicity gradients. The FIRE2 simulations show evidence for positive gradients that occur both before andor after major episodes of star formation manifesting as sharp rises in a galaxys starformation history. Positive gradients occurring before major starformation episodes are likely caused by metalpoor gas inflows whereas those appearing afterwards often result from metalenriched gas outflows driven by strong stellar feedback. Our results support the important role of stellar feedback in governing the chemostructural evolution and disk formation of Milky Waymass galaxies at the cosmic noon epoch. | 2024-09-01T00:00:00Z | ['arXiv:2409.09290', '10.48550/arXiv.2409.09290', '2024arXiv240909290S'] | ['Astrophysics - Astrophysics of Galaxies'] | The physical origin of positive metallicity radial gradients in highredshift galaxies insights from the FIRE2 cosmological hydrodynamic simulations | 2,024 | 365 | 0.56 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.09290.pdf |
2024JCAP...11..062S | We measure the speed of light with current observations such as Type Ia Supernova galaxy ages radial BAO mode as well as simulations of forthcoming redshift surveys and gravitational waves as standard sirens. By means of a Gaussian Process reconstruction we find that the precision of such measurements can be improved from roughly 6 and to about 22.5 when the gravitational wave simulations are considered and to 1.52 when redshift survey are included in the analysis as well. This result demonstrates that we will be able to perform a cosmological measurement of a fundamental physical constant with significantly improved precision which will help us underpinning if its value is truly consistent with local measurements as predicted by the standard model of Cosmology. | 2024-11-01T00:00:00Z | ['10.48550/arXiv.2409.05838', 'arXiv:2409.05838', '10.1088/1475-7516/2024/11/062', '2024JCAP...11..062S', '2024arXiv240905838S'] | ['baryon acoustic oscillations', 'cosmological simulations', 'Machine learning', 'supernova type Ia - standard candles', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology'] | Measuring the speed of light with cosmological observations current constraints and forecasts | 2,024 | 366 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 2 | https://arxiv.org/pdf/2409.05838.pdf |
2024arXiv240911333H | Ultralight primordial black holes PBHs with masses Mrm PBHlt5times 108mathrmg can dominate transiently the energy budget of the Universe and reheat the Universe through their evaporation taking place before Big Bang Nucleosynthesis. The isocurvature energy density fluctuations associated to the inhomogeneous distribution of a population of such PBHs can induce an abundant production of GWs due to secondorder gravitational effects. In this work we discuss the effect of primordial nonGaussianity on the clustering properties of PBHs and study the effect of a clustered PBH population on the spectral shape of the aforementioned induced GW signal. In particular focusing on localtype nonGaussianity we find a doublepeaked GW signal with the amplitude of the lowfrequency peak being proportional to the square of the nonGaussian parameter taumathrmNL. Remarkably depending on the PBH mass Mrm PBH and the initial abundance of PBHs at formation time i.e. OmegamathrmPBHf this doublepeaked GW signal can lie well within the frequency bands of forthcoming GW detectors namely LISA ET SKA and BBO hence rendering this signal falsifiable by GW experiments and promoting it as a novel portal probing the primordial nonGaussianity. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.11333', '2024arXiv240911333H', 'arXiv:2409.11333'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology'] | Gravitational waves from primordial black hole isocurvature the effect of nonGaussianities | 2,024 | 366 | 0.31 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.11333.pdf |
2024arXiv240908672W | In galaxies with significant ongoing star formation there is an impressively tight correlation between total infrared luminosity LTIR and Halpha luminosity LHalpha when Halpha is properly corrected for stellar absorption and dust attenuation. This longstanding result gives confidence that both measurements provide accurate estimates of a galaxys star formation rate SFR despite their differing origins. To test the extent to which this holds in galaxies with lower specific SFR sSFRSFRMgal where Mgal is the stellar mass we combine optical spectroscopy from the Sloan Digital Sky Survey SDSS with multiwavelength FUV to FIR photometric observations from the Galaxy And Mass Assembly survey GAMA. We find that LTIRLHalphaincreases steadily with decreasing Halpha equivalent width WHalpha a proxy for sSFR indicating that both luminosities cannot provide a valid measurement of SFR in galaxies below the canonical starforming sequence. For both retired galaxies and poststarburst galaxies LTIRLHalpha can be up to a factor of 30 larger than for starforming galaxies. The smooth change in LTIRLHalpha irrespective of star formation history ionisation or heating source dust temperature or other properties suggests that the value of LTIRLHalpha is given by the balance between starforming regions and ambient interstellar medium contributing to both LTIR and LHalpha. While LHalpha can only be used to estimate the SFR for galaxies with WHalpha gt 3A sSFR gtrsim 1011.5yr we argue that the mid and farinfrared can only be used to estimate the SFR of galaxies on the starforming sequence and in particular only for galaxies with WHalpha gt10 A sSFR gtrsim 1010.5yr. We find no evidence for dust obscured starformation in poststarburst galaxies. | 2024-09-01T00:00:00Z | ['arXiv:2409.08672', '2024arXiv240908672W', '10.48550/arXiv.2409.08672'] | ['Astrophysics - Astrophysics of Galaxies'] | The infrared luminosity of retired and poststarburst galaxies A cautionary tale for star formation rate measurements | 2,024 | 367 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.08672.pdf |
2023arXiv230501582C | PySR is an opensource library for practical symbolic regression a type of machine learning which aims to discover humaninterpretable symbolic models. PySR was developed to democratize and popularize symbolic regression for the sciences and is built on a highperformance distributed backend a flexible search algorithm and interfaces with several deep learning packages. PySRs internal search algorithm is a multipopulation evolutionary algorithm which consists of a unique evolvesimplifyoptimize loop designed for optimization of unknown scalar constants in newlydiscovered empirical expressions. PySRs backend is the extremely optimized Julia library SymbolicRegression.jl which can be used directly from Julia. It is capable of fusing userdefined operators into SIMD kernels at runtime performing automatic differentiation and distributing populations of expressions to thousands of cores across a cluster. In describing this software we also introduce a new benchmark EmpiricalBench to quantify the applicability of symbolic regression algorithms in science. This benchmark measures recovery of historical empirical equations from original and synthetic datasets. | 2023-05-01T00:00:00Z | ['10.48550/arXiv.2305.01582', 'arXiv:2305.01582', '2023arXiv230501582C'] | ['Astrophysics - Instrumentation and Methods for Astrophysics', 'Computer Science - Machine Learning', 'Computer Science - Neural and Evolutionary Computing', 'Computer Science - Symbolic Computation', 'Physics - Data Analysis', 'Statistics and Probability'] | Interpretable Machine Learning for Science with PySR and SymbolicRegression.jl | 2,023 | 367 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 132 | https://arxiv.org/pdf/2305.01582.pdf |
2024arXiv240910605M | Washin leptogenesis is an attractive mechanism to produce the baryon asymmetry of the Universe. It treats righthandedneutrino interactions as spectator processes on the same footing as electroweak sphalerons that reprocess primordial charge asymmetries in the thermal plasma into a baryonminuslepton asymmetry. The origin of these primordial charges must be accounted for by new CPviolating dynamics at very high energies. In this paper we propose such a scenario of chargegenesis that unlike earlier proposals primarily relies on new interactions in the gravitational sector. We point out that a coupling of a conserved current to the divergence of the Ricci scalar during reheating can lead to nonzero effective chemical potentials in the plasma that together with a suitable chargeviolating interaction can result in the production of a primordial charge asymmetry. Gravitational chargegenesis represents a substantial generalization of the idea of gravitational baryogenesis. We provide a detailed analysis of a generic and minimal realization that is consistent with inflation and show that it can successfully explain the baryon asymmetry of the Universe. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.10605', '2024arXiv240910605M', 'arXiv:2409.10605'] | ['High Energy Physics - Phenomenology', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Theory'] | Gravitational chargegenesis | 2,024 | 370 | 0.17 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.10605.pdf |
2024arXiv240909468W | Primordial Black Holes PBHs are capable of emitting extremely energetic particles independent of their interactions with the Standard Model. In this work we investigate a particularly interesting scenario in which PBHs evaporating in the early universe may be responsible for some of the observed highenergy neutrinos above the TeV or PeV scale in the present universe. We compute the energy spectrum of neutrinos directly emitted by PBHs with a monochromatic mass function and estimate the washout point which determines the maximum energy of the spectrum. We find that the spectrum generally extends to high energies following a power law of Enu3 until it reaches the washout point which crucially depends on the PBH mass. For PBHs of 1013 grams the spectrum can extend up to the PeV scale though the flux is too low for detection. We also consider an indirect production mechanism involving dark particles that are emitted by PBHs and decay into neutrinos at a much later epoch. This mechanism allows lighter such as those in the gram to kilogram range PBHs to produce more energetic neutrino fluxes without being washed out by the thermal plasma in the early universe. In this scenario we find that ultrahighenergy neutrinos around or above the EeV scale can be generated with sufficiently high fluxes detectable by current and future highenergy neutrino observatories such as IceCube and GRAND. | 2024-09-01T00:00:00Z | ['arXiv:2409.09468', '2024arXiv240909468W', '10.48550/arXiv.2409.09468'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena'] | HighEnergy and UltraHighEnergy Neutrinos from Primordial Black Holes | 2,024 | 371 | 0.35 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.09468.pdf |
2024arXiv240904552G | Magnetic monopoles MMs are wellmotivated hypothetical particles whose discovery would symmetrize Maxwell equations explain quantization of electric charge and probe the gauge structure of the unified theory. Recent models predict MMs with low masses reinvigorating searches at colliders. However most theories predict composite MMs whose production in partonparton collisions is expected to be suppressed. The Schwinger process whereby MM pairs tunnel through the vacuum barrier in the presence of a strong magnetic field is not subject to this limitation. Additionally the Schwinger cross section can be calculated nonperturbatively. Together these make it a golden channel for lowmass MM searches. We investigate the Schwinger production of MMs in heavyion collisions at future colliders in collisions of cosmic rays with the atmosphere and in decay of magnetic fields of cosmic origin. We find that a nextgeneration collider would provide the best sensitivity. At the same time exploiting the infrastructure of industrial ore extraction and Antarctic ice drilling could advance the field at a faster timescale and with only a modest investment. We also propose deploying dedicated MM detectors in conjunction with cosmic ray observatories to directly investigate if the unexplained highest energy cosmic rays are MMs. Together the proposed efforts would define the field of MM searches in the next decades. | 2024-09-01T00:00:00Z | ['arXiv:2409.04552', '10.48550/arXiv.2409.04552', '2024arXiv240904552G'] | ['High Energy Physics - Phenomenology', 'Astrophysics - High Energy Astrophysical Phenomena', 'High Energy Physics - Experiment'] | The next frontiers for magnetic monopole searches | 2,024 | 373 | 0.3 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.04552.pdf |
2024arXiv240912228A | Distinct behavior of decaying particles in true and false vacua of the theory can lead to enhanced generation of baryon asymmetry a scenario we call textitphase separation baryogenesis. We demonstrate that for leptogenesis this naturally allows for right handed neutrinos to generate resonantlyenhanced lepton asymmetry without finetuning of their masses as in typical theories. Our mechanism allows for a variety of neutrino mass hierarchies and hence possible novel connections with observations. We present a concrete realization in a minimal model with a scalar field undergoing a phase transition. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.12228', '2024arXiv240912228A', 'arXiv:2409.12228'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Phase Separation Baryogenesis | 2,024 | 376 | 0.17 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.12228.pdf |
2024A&A...690A.371L | We present observations of the two closest globular clusters NGC 6121 and NGC 6397 taken with the NIRISS detector of JWST. The combination of our new JWST data with archival Hubble Space Telescope HST images allows us to compute proper motions disentangle cluster members from field objects and probe the main sequence MS of the clusters down to lt0.1 MSUBSUB as well as the brighter part of the whitedwarf sequence. We show that theoretical isochrones fall short in modeling the lowmass MS and discuss possible explanations for the observed discrepancies. Our analysis suggests that the lowestmass members of both clusters are significantly more metalrich and oxygenpoor than their highermass counterparts. It is unclear whether the difference is caused by a genuine massdependent chemical heterogeneity lowtemperature atmospheric processes altering the observed abundances or systematic shortcomings in the models. We computed the presentday local luminosity and mass functions of the two clusters our data reveal a strong flattening of the mass function indicative of a significant preferential loss of lowmass stars in agreement with previous dynamical models for these two clusters. We have made our NIRISS astrophotometric catalogs and stacked images publicly available to the community. | 2024-10-01T00:00:00Z | ['10.1051/0004-6361/202451295', '2024A&A...690A.371L', '2024arXiv240906774L', 'arXiv:2409.06774', '10.48550/arXiv.2409.06774'] | ['techniques: photometric', 'astrometry', 'proper motions', 'globular clusters: individual: NGC 6121', 'globular clusters: individual: NGC 6397', 'Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Astrophysics of Galaxies'] | JWST imaging of the closest globular clusters IV. Chemistry luminosity and mass functions of the lowestmass members in the NIRISS parallel fields | 2,024 | 376 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.06774.pdf |
2024arXiv240912261T | Studying the orbital motion of stars around Sagittarius A in the Galactic Center provides a unique opportunity to probe the gravitational potential near the supermassive black hole at the heart of our Galaxy. Interferometric data obtained with the GRAVITY instrument at the Very Large Telescope Interferometer VLTI since 2016 has allowed us to achieve unprecedented precision in tracking the orbits of these stars. GRAVITY data have been key to detecting the inplane prograde Schwarzschild precession of the orbit of the star S2 as predicted by General Relativity. By combining astrometric and spectroscopic data from multiple stars including S2 S29 S38 and S55 for which we have data around their time of pericenter passage with GRAVITY we can now strengthen the significance of this detection to an approximately 10 sigma confidence level. The prograde precession of S2s orbit provides valuable insights into the potential presence of an extended mass distribution surrounding Sagittarius A which could consist of a dynamically relaxed stellar cusp comprised of old stars and stellar remnants along with a possible dark matter spike. Our analysis based on two plausible density profiles a powerlaw and a Plummer profile constrains the enclosed mass within the orbit of S2 to be consistent with zero establishing an upper limit of approximately 1200 Modot with a 1 sigma confidence level. This significantly improves our constraints on the mass distribution in the Galactic Center. Our upper limit is very close to the expected value from numerical simulations for a stellar cusp in the Galactic Center leaving little room for a significant enhancement of dark matter density near Sagittarius A. | 2024-09-01T00:00:00Z | ['2024arXiv240912261T', 'arXiv:2409.12261', '10.48550/arXiv.2409.12261'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - High Energy Astrophysical Phenomena'] | Improving constraints on the extended mass distribution in the Galactic Center with stellar orbits | 2,024 | 377 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.12261.pdf |
2024arXiv240906783F | We use the cosmological magnetohydrodynamical simulation TNG50 to study the relationship between black hole feedback the presence of stellar bars and star formation quenching in Milky Waylike disc galaxies. Of our sample of 198 discs about 63 per cent develop stellar bars that last until z0. After the formation of their bars the majority of these galaxies develop persistent 315 kpc wide holes in the centres of their gas discs. Tracking their evolution from z4 to 0 we demonstrate that barred galaxies tend to form within dark matter haloes that become centrally disc dominated early on and are thus unstable to bar formation whereas unbarred galaxies do not barred galaxies also host central black holes that grow more rapidly than those of unbarred galaxies. As a result most barred galaxies eventually experience kinetic wind feedback that operates when the mass of the central supermassive black hole exceeds MBH gt 108 Modot. This feedback ejects gas from the central disc into the circumgalactic medium and rapidly quenches barred galaxies of their central star formation. If kinetic black hole feedback occurs in an unbarred disc it suppresses subsequent star formation and inhibits its growth stabilising the disc against future bar formation. Consequently most barred galaxies develop black holedriven gas holes though a gas hole alone does not guarantee the presence of a stellar bar. This subtle relationship between black hole feedback cold gas disc morphology and stellar bars may provide constraints on subgrid physics models for supermassive black hole feedback. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.06783', '2024arXiv240906783F', 'arXiv:2409.06783'] | ['Astrophysics - Astrophysics of Galaxies'] | Supermassive black hole feedback quenches disc galaxies and suppresses bar formation in TNG50 | 2,024 | 377 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.06783.pdf |
2024arXiv240911450L | Autonomous precision navigation to land onto the Moon relies on vision sensors. Computer vision algorithms are designed trained and tested using synthetic simulations. High quality terrain models have been produced by Moon orbiters developed by several nations with resolutions ranging from tens or hundreds of meters globally down to few meters locally. The SurRender software is a powerful simulator able to exploit the full potential of these datasets in raytracing. New interfaces include tools to fuse multiresolution DEMs and procedural texture generation. A global model of the Moon at 20m resolution was integrated representing several terabytes of data which SurRender can render continuously and in realtime. This simulator will be a precious asset for the development of future missions. | 2024-09-01T00:00:00Z | ['2024arXiv240911450L', '10.48550/arXiv.2409.11450', 'arXiv:2409.11450'] | ['Astrophysics - Instrumentation and Methods for Astrophysics', 'Astrophysics - Earth and Planetary Astrophysics', 'Computer Science - Graphics', 'Computer Science - Robotics'] | High performance Lunar landing simulations | 2,024 | 378 | 0.32 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.11450.pdf |
2024SSRv..220...76D | Meteorites trace planet formation in the Suns protoplanetary disk but they also record the influence of the Suns birth environment. Whether the Sun formed in a region like TaurusAuriga with inlineformula idIEq1mmlmathmmlmommlmommlmsupmmlmrowmmlmn10mmlmnmmlmrowmmlmrowmmlmn2mmlmnmmlmrowmmlmsupmmlmathinlineformula stars or a region like the Carina Nebula with inlineformula idIEq2mmlmathmmlmommlmommlmsupmmlmrowmmlmn10mmlmnmmlmrowmmlmrowmmlmn6mmlmnmmlmrowmmlmsupmmlmathinlineformula stars matters for how large the Suns disk was for how long and from how far away it accreted gas from the molecular cloud and how it acquired radionuclides like SUP26SUPAl. To provide context for the interpretation of meteoritic data we review what is known about the Suns birth environment. Based on an inferred gas disk outer radius inlineformula idIEq3mmlmathmmlmommlmommlmn50mmlmnmmlmommlmommlmn90mmlmnmmlmathinlineformula AU radial transport in the disk and the abundances of noble gases in Jupiters atmosphere the Suns molecular cloud and protoplanetary disk were exposed to an ultraviolet flux inlineformula idIEq4mmlmathmmlmsubmmlmiGmmlmimmlmn0mmlmnmmlmsubmmlmommlmommlmn30mmlmnmmlmommlmommlmn3000mmlmnmmlmathinlineformula during its birth and first inlineformula idIEq5mmlmathmmlmommlmommlmn10mmlmnmmlmathinlineformula Myr of evolution. Based on the orbits of Kuiper Belt objects the Solar System was subsequently exposed to a stellar density inlineformula idIEq6mmlmathmmlmommlmommlmspace width0.2emmmlmspacemmlmn100mmlmnmmlmspace width0.2emmmlmspacemmlmsubmmlmiMmmlmimmlmommlmommlmsubmmlmspace width0.2emmmlmspacemmlmsupmmlmi mathvariantnormalpcmmlmimmlmrowmmlmommlmommlmn3mmlmnmmlmrowmmlmsupmmlmathinlineformula for inlineformula idIEq7mmlmathmmlmommlmommlmn100mmlmnmmlmathinlineformula Myr strongly implying formation in a bound cluster. These facts suggest formation in a region like the outskirts of the Orion Nebula perhaps 2 pc from the center. The protoplanetary disk might have accreted gas for many Myr but a few inlineformula idIEq8mmlmathmmlmommlmommlmsupmmlmrowmmlmn10mmlmnmmlmrowmmlmrowmmlmn5mmlmnmmlmrowmmlmsupmmlmathinlineformula yr seems more likely. It probably inherited radionuclides from its molecular cloud enriched by inputs from supernovae and especially WolfRayet star winds and acquired a typical amount of SUP26SUPAl. | 2024-10-01T00:00:00Z | ['2024arXiv240910638D', '10.1007/s11214-024-01113-x', '2024SSRv..220...76D', '10.48550/arXiv.2409.10638', 'arXiv:2409.10638'] | ['Stars: formation', 'Stars: Wolf-Rayet', 'Photon-dominated region (PDR)', 'Protoplanetary disks', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics', 'Physics - Geophysics'] | The Suns Birth Environment Context for Meteoritics | 2,024 | 378 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 1 | https://arxiv.org/pdf/2409.10638.pdf |
2024arXiv240912940A | The cosmic microwave background CMB spectrum is an extraordinary tool for exploring physics beyond the Standard Model. The exquisite precision of the measurement makes it particularly sensitive to small effects caused by hidden sector interactions. In particular CMB spectral distortions can unveil the existence of dark photons which are kinetically coupled to the standard photon. In this work we use the COBEFIRAS dataset to derive accurate and robust limits on photontodarkphoton oscillations for a large range of dark photon masses from 1010 to 104 eV. We consider in detail the redshift dependence of the bounds computing CMB distortions due to photon injectionremoval using a Greens function method. Our treatment improves on previous results which had set limits studying energy injectionremoval into baryons rather than photon injectionremoval or ignored the redshift evolution of distortions. The difference between our treatment and previous ones is particularly noticeable in the predicted spectral shape of the distortions a smoking gun signature for photontodarkphoton oscillations. The characterization of the spectral shape is crucial for future CMB missions which could improve the present sensitivity by orders of magnitude exploring regions of the dark photon parameter space that are otherwise difficult to access. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.12940', '2024arXiv240912940A', 'arXiv:2409.12940'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Shaping Dark Photon Spectral Distortions | 2,024 | 378 | 0.32 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.12940.pdf |
2024arXiv240905950S | The ringdown phase following a binary black hole coalescence is a powerful tool for measuring properties of the remnant black hole. Future gravitational wave detectors will increase the precision of these measurements and may be sensitive to the environment surrounding the black hole. This work examines how environments affect the ringdown from a binary coalescence. Our analysis shows that for astrophysical parameters and sensitivity of planned detectors the ringdown signal is indistinguishable from its vacuum counterpart suggesting that ringdownonly analyses can reliably extract the redshifted mass and spin of the remnant black hole. These conclusions include models with spectral instabilities suggesting that these are not relevant from an observational viewpoint. Deviations from inspiralonly estimates could then enhance the characterisation of environmental effects present during the coalescence. | 2024-09-01T00:00:00Z | ['arXiv:2409.05950', '2024arXiv240905950S', '10.48550/arXiv.2409.05950'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - Astrophysics of Galaxies'] | Black hole spectroscopy in environments detectability prospects | 2,024 | 379 | 0.37 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.05950.pdf |
2024arXiv240908539M | Aims. To investigate the influence of distance to filaments and dark matter halos on galaxy cold gas content in the empirical model NeutralUniverseMachine NUM and the hydrodynamical simulation IllustrisTNG. Methods. We use DisPerSE to identify cosmic web structures and calculate the distance of galaxies to filaments for both observations and models. We show the results of the HI and H2 mass functions HI and H2halo mass relations HI and H2stellar mass relations for galaxies in the NUM model and IllustrisTNG with different distances to filaments and compare them with observational measurements. We also show the evolution of HI H2 mass densities in different distance to filament bins. Results. We find that the role of filaments in affecting the HI gas is generally less significant compared to the halo environment. There is a weak trend in the observations at z 0 that lowmass halos lying closer to filaments tend to have reduced HI masses. However this trend reverses for massive halos with logMvirMsun gt 12.5. This behavior is accurately reproduced in the NUM model due to the dependence of HI gas on the halo formation time but it does not appear in IllustrisTNG. The influence of filaments on the HI gas becomes slightly weaker at higher redshifts and is only significant for galaxies residing in massive halos in the NUM model. Filaments have almost no impact on the H2stellar mass relation in both models confirming that H2 is primarily determined by the galaxy stellar mass and star formation rate. | 2024-09-01T00:00:00Z | ['2024arXiv240908539M', 'arXiv:2409.08539', '10.48550/arXiv.2409.08539'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | NeutralUniverseMachine How Filaments and Dark Matter Halo Influence the Galaxy Cold Gas Content | 2,024 | 381 | 0.49 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.08539.pdf |
2024arXiv240908312H | An axionlike spectator during inflation can trigger a tachyonic instability which amplifies the modes of one of the helicities of the gauge field resulting in the production of parityviolating gravitational waves GWs. In this paper we investigate the impact of the coupling RFF of the gauge field to gravity on the production of GWs. We find that such a coupling introduces a multiplicative factor to the tachyonic mass which effectively enhances the amplitude of the gauge field modes. Produced GWs are expected to be observed by future spacebased GW detectors. Additionally we find that the strong backreaction due to particle production leads to multiple peaks in the energy spectrum of GWs. | 2024-09-01T00:00:00Z | ['2024arXiv240908312H', '10.48550/arXiv.2409.08312', 'arXiv:2409.08312'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Phenomenology'] | Gravitational Waves from a Gauge Field Nonminimally Coupled to Gravity | 2,024 | 382 | 0.3 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.08312.pdf |
2024ApJ...974L..38Z | Shadows are often observed in transition disks which can result from obscuring by materials closer to the star such as a misaligned inner disk. While shadows leave apparent darkened emission as observational signatures they have significant dynamical impact on the disk. We carry out 3D radiationhydrodynamical simulations to study shadows in transition disks and find that the temperature drop due to the shadow acts as an asymmetric driving force leading to spirals in the cavity. These spirals have zero pattern speed following the fixed shadow. The pitch angle is given by tanSUP1SUPc SUB s SUBv SUB SUB 6 if hr 0.1. These spirals transport mass through the cavity efficiently with 10SUP2SUP in our simulation. Besides spirals the cavity edge can also form vortices and flocculent streamers. When present these features could disturb the shadowinduced spirals. By carrying out Monte Carlo radiative transfer simulations we show that these features resemble those observed in nearinfrared scattered light images. In the vertical direction the vertical gravity is no longer balanced by the pressure gradient alone. Instead an azimuthal convective acceleration term balances the gravitypressure difference leading to azimuthally periodic upward and downward gas motion reaching 10 of the sound speed which can be probed by Atacama Large Millimetersubmillimeter Array line observations. | 2024-10-01T00:00:00Z | ['2024arXiv240908373Z', '10.48550/arXiv.2409.08373', 'arXiv:2409.08373', '10.3847/2041-8213/ad815f', '2024ApJ...974L..38Z'] | ['Accretion', 'Protoplanetary disks', 'Radiative transfer', 'Hydrodynamical simulations', 'Radiative magnetohydrodynamics', '14', '1300', '1335', '767', '2009', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Solar and Stellar Astrophysics'] | 3D Radiationhydrodynamical Simulations of Shadows on Transition Disks | 2,024 | 383 | 0.56 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 4 | https://arxiv.org/pdf/2409.08373.pdf |
2024arXiv240906599W | Gravitational waves from cosmological phase transitions are novel probes of fundamental physics making their precise calculation essential for revealing various mysteries of the early Universe. In this work we propose a framework that enables the consistent calculation of such gravitational waves sourced by sound waves. Starting from the Lagrangian this framework integrates the calculation of the dynamics of firstorder phase transitions in a selfconsistent manner eliminating various approximations typically introduced by conventional methods. At the heart of our approach is the congruous evaluation of the phase transition hydrodynamics that at every step is consistently informed by the Lagrangian. We demonstrate the application of our framework using the SMH6 model deriving the corresponding gravitational wave spectrum. Our framework establishes a robust foundation for the precise prediction of gravitational waves from phase transitions. | 2024-09-01T00:00:00Z | ['arXiv:2409.06599', '2024arXiv240906599W', '10.48550/arXiv.2409.06599'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology'] | Selfconsistent prediction of gravitational waves from cosmological phase transitions | 2,024 | 383 | 0.23 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.06599.pdf |
2024MNRAS.535.1874C | Spectral distortions of the cosmic microwave background CMB provide stringent constraints on energy and entropy production in the postBBN big bang nucleosynthesis era. This has been used to constrain dark photon models with COBEFIRAS and forecast the potential gains with future CMB spectrometers. Here we revisit these constraints by carefully considering the photon to dark photon conversion process and evolution of the distortion signal. Previous works only included the effect of CMB energy density changes but neglected the change to the photon number density. We clearly define the dark photon distortion signal and show that in contrast to previous analytic estimates the distortion has an opposite sign and a inlineformulatexmath idTM0001 notationLaTeXsimeq 1.5texmathinlineformula times larger amplitude. We furthermore extend the treatment into the large distortion regime to also cover the redshift range inlineformulatexmath idTM0002 notationLaTeXsimeq 2 times 1064 times 107texmathinlineformula between the era and the end of BBN using COSMOTHERM . This shows that the CMB distortion constraints for dark photon masses in the range inlineformulatexmath idTM0003 notationLaTeX104 rm eVlesssim mrm dlesssim 103 rm eVtexmathinlineformula were significantly underestimated. We demonstrate that in the small distortion regime the distortion caused by photon to dark photon conversion is extremely close to a type distortion independent of the conversion redshift. This opens the possibility to study dark photon models using CMB distortion anisotropies and the correlations with CMB temperature anisotropies as we highlight here. | 2024-12-01T00:00:00Z | ['10.1093/mnras/stae2464', '2024MNRAS.tmp.2395C', 'arXiv:2409.12115', '2024arXiv240912115C', '10.48550/arXiv.2409.12115', '2024MNRAS.535.1874C'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Theory'] | Revisiting dark photon constraints from CMB spectral distortions | 2,024 | 383 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 4 | https://arxiv.org/pdf/2409.12115.pdf |
2024arXiv240911866A | We propose a stochastic interpretation of spacetime noncommutativity starting from the path integral formulation of quantum mechanical commutation relations. We discuss how the noncommutativity of spacetime is inherently related to the continuity or discontinuity of paths in the path integral formulation. Utilizing Wiener processes we demonstrate that continuous paths lead to commutative spacetime whereas discontinuous paths correspond to noncommutative spacetime structures. As an example we introduce discontinuous paths from which the kappaMinkowski spacetime commutators can be obtained. Moreover we focus on modifications of the Leibniz rule for differentials acting on discontinuous trajectories. We show how these can be related to the deformed action of translation generators focusing as a working example on the kappaPoincar algebra. Our findings suggest that spacetime noncommutativity can be understood as a result of fundamental discreteness in temporal andor spatial evolution. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.11866', '2024arXiv240911866A', 'arXiv:2409.11866'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology', 'Mathematical Physics', 'Quantum Physics'] | A Stochastic Origin of Spacetime NonCommutativity | 2,024 | 384 | 0.06 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.11866.pdf |
2024arXiv240906527L | Massive black hole binary MBHB mergers will be detectable in large numbers by the Lisa Interferometer Space Antenna LISA which will thus provide new insights on how they form via repeated dark matter DM halo and galaxy mergers. Here we present a simple analytical model to generate a population of MBHB mergers based on a theoretical prescription that connects them to DM halo mergers. The high flexibility of our approach allows us to explore the broad and uncertain range of MBH seeding and growth mechanisms as well as the different effects behind the interplay between MBH and galactic astrophysics. Such a flexibility is fundamental for the successful implementation and optimisation of the hierarchical Bayesian parameter estimation approach that here we apply to the MBHB population of LISA for the first time. Our inferred population hyperparameters are chosen as proxies to characterise the MBHDM halo mass scaling relation the occupation fraction of MBHs in DM halos and the delay between halo and MBHB mergers. We find that LISA will provide tight constraints at the lowerend of the MBHhalo scaling relation well complementing EM observations which are biased towards large masses. Furthermore our results suggest that LISA will constrain some features of the MBH occupation fraction at high redshift as well as merger time delays of the order of a few hundreds of Myr opening the possibility to constrain dynamical evolution time scales such as the dynamical friction. The analysis presented here constitutes a first attempt at developing a hierarchical Bayesian inference approach to the LISA MBHB population opening the way for several further improvements and investigations. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.06527', '2024arXiv240906527L', 'arXiv:2409.06527'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology'] | Hierarchical Bayesian inference on an analytical model of the LISA massive black hole binary population | 2,024 | 384 | 0.49 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.06527.pdf |
2024arXiv240912125D | We study the Primordial Black Hole PBH reheating scenario where PBHs originate in a general cosmological background. In this scenario ultralight PBHs with masses Mlesssim 108g temporarily dominate the Universe and reheat it via Hawking radiation before Big Bang Nucleosynthesis BBN. We investigate whether the induced Gravitational Wave GW spectrum associated with PBH reheating contains information about the prePBHdominated stage namely the initial equation of state w after inflation. We first derive the transfer functions of curvature fluctuations for general w with adiabatic and isocurvature initial conditions. We find that in general a stiffer equation of state enhances the induced GW amplitude as it allows for a longer PBH dominated phase compared to the radiation dominated case. We also find that the spectral slope of GWs induced by primordial curvature fluctuations is sensitive to w while the spectral slope of GWs induced by PBH number density fluctuations is not. Lastly we derive constraints of the initial PBH abundance as a function of w using BBN and Cosmic Microwave Background CMB observations. A stiffer equation of state leads to stricter constraints on the initial energy density fraction as induced GWs are enhanced. Interestingly we find that such induced GW signals may enter the observational window of several future GW detectors such as LISA and the Einstein Telescope. Our formulas especially the curvature fluctuation transfer functions are applicable to any early matterdominated universe scenario. | 2024-09-01T00:00:00Z | ['2024arXiv240912125D', '10.48550/arXiv.2409.12125', 'arXiv:2409.12125'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | From formation to evaporation Induced gravitational wave probes of the primordial black hole reheating scenario | 2,024 | 385 | 0.35 | ['EPRINT_HTML', 'EPRINT_PDF'] | 6 | https://arxiv.org/pdf/2409.12125.pdf |
2024ApJ...976L..16M | The recent observations by the James Webb Space Telescope JWST have revealed a larger number of bright galaxies at z 10 than was expected. The origin of this excess is still under debate although several possibilities have been presented. We propose that gammaray bursts GRBs are a powerful probe to explore the origin of the excess and hence the star and galaxy formation histories in the early universe. Focusing on the recently launched mission Einstein Probe EP we find that EP can detect several GRBs annually at z 10 assuming the GRB formation rate calibrated by events at z 6 can be extrapolated. Interestingly depending on the excess scenarios the GRB event rate may also show an excess at z 10 and its detection will help to discriminate between the scenarios that are otherwise difficult to distinguish. Additionally we discuss that the puzzling redcolor compact galaxies discovered by JWST the socalled little red dots could host dark GRBs if they are dustobscured starforming galaxies. We are eager for unbiased followup of GRBs and encourage future missions such as HiZGUNDAM to explore the early universe. | 2024-11-01T00:00:00Z | ['2024ApJ...976L..16M', '2024arXiv240911468M', 'arXiv:2409.11468', '10.3847/2041-8213/ad8ce0', '10.48550/arXiv.2409.11468'] | ['Gamma-ray bursts', '629', 'Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Astrophysics of Galaxies'] | Probing the Origin of the Star Formation Excess Discovered by JWST through GammaRay Bursts | 2,024 | 385 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.11468.pdf |
2024arXiv240907702Z | We investigate the first and second order cosmological perturbation equations in fR modified gravity theory and provide the equation of motion of second order scalar induced gravitational waves. We find that the effects of modified gravity not only change the form of the equation of motion of second order scalar induced gravitational waves but also contribute an additional anisotropic stress tensor composed of first order scalar perturbations to the source term of the gravitational waves. We calculate the energy density spectrum of second order scalar induced gravitational waves in the HS model. Utilizing current pulsar timing array observational data we perform a rigorous Bayesian analysis of the parameter space of the HS model. | 2024-09-01T00:00:00Z | ['2024arXiv240907702Z', 'arXiv:2409.07702', '10.48550/arXiv.2409.07702'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Theory'] | Scalar induced gravitational waves in fR gravity | 2,024 | 386 | 0.31 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.07702.pdf |
2024arXiv240911464Z | For the first time we systematically search for galaxies with extended emission line and potential outflows features using mediumband images in the GOODSS field by comparing the morphology in mediumband images to adjacent continuum and UV bands. We look for galaxies that have a maximum extent 50 larger an excess area 30 greater or an axis ratio difference of more than 0.3 in the medium band compared to the reference bands. After visual inspection we find 326 candidate galaxies at 1 lt z lt 6 with a peak in the population near cosmic noon benefiting from the good coverage of the mediumband filters. By examining their SEDs we find that the candidate galaxies are at least 20 more bursty in their starforming activity and have 60 more young stellar populations compared to a control sample selected based on the continuum band flux. Additionally these candidates exhibit a significantly higher production rate of ionizing photons. We further find that candidates hosting known AGN produce extended emission that is more anisotropic compared to nonAGN candidates. A few of our candidates have been spectroscopically confirmed to have prominent outflow signatures through NIRSpec observations showcasing the robustness of the photometric selection. Future spectroscopic followup will better help verify and characterize the kinematics and chemical properties of these systems. | 2024-09-01T00:00:00Z | ['2024arXiv240911464Z', 'arXiv:2409.11464', '10.48550/arXiv.2409.11464'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | A Systematic Search for Galaxies with Extended Emission Line and Potential Outflows in JADES MediumBand Images | 2,024 | 387 | 0.56 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.11464.pdf |
2024arXiv240910963L | We present a spatially resolved analysis of four starforming galaxies at z 4.445.64 using data from the JWST PRIMER and ALMACRISTAL surveys to probe the stellar and interstellar medium properties on the subkpc scale. In the 15murm m JWST NIRCam imaging we find that the galaxies are composed of multiple clumps between 2 and sim 8 separated by simeq 5rm kpc with comparable morphologies and sizes in the restframe UV and optical. Using BAGPIPES to perform pixelbypixel SED fitting to the JWST data we show that the SFR simeq 25rm Modotrm yr and stellar mass rm log10Mstarrm Modot simeq 9.5 derived from the resolved analysis are in close lesssim 0.3rm dex agreement with those obtained by fitting the integrated photometry. In contrast to studies of lowermass sources we thus find a reduced impact of outshining of the older more massive stellar populations in these normal z simeq 5 galaxies. Our JWST analysis recovers bluer restframe UV slopes beta simeq 2.1 and younger ages simeq 100rm Myr than archival values. We find that the dust continuum from ALMACRISTAL seen in two of these galaxies correlates as expected with regions of redder restframe UV slopes and the SEDderived Arm V as well as the peak in the stellar mass map. We compute the resolved IRXbeta relation showing that the IRX is consistent with the local starburst attenuation curve and further demonstrating the presence of an inhomogeneous dust distribution within the galaxies. A comparison of the CRISTAL sources to those from the FirstLight zoomin simulation of galaxies with the same Mstar and SFR reveals similar age and colour gradients suggesting that major mergers may be important in the formation of clumpy galaxies at this epoch. | 2024-09-01T00:00:00Z | ['arXiv:2409.10963', '2024arXiv240910963L', '10.48550/arXiv.2409.10963'] | ['Astrophysics - Astrophysics of Galaxies'] | JWST PRIMER A lack of outshining in four normal z 46 galaxies from the ALMACRISTAL Survey | 2,024 | 388 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.10963.pdf |
2024arXiv240905467S | We show that there exist two qualitatively different turbulent states of the zeronetverticalflux shearing box. The first which has been studied in detail previously is characterized by a weakly magnetized betasim50 midplane with slow periodic reversals of the mean azimuthal field dynamo cycles. The second the lowbeta state which is the main subject of this paper is characterized by a strongly magnetized betasim1 midplane dominated by a coherent azimuthal field with much stronger turbulence and much larger accretion stress alpha sim 1. The lowbeta state is realized in simulations that begin with sufficiently strong azimuthal magnetic fields. The mean azimuthal field in the lowbeta state is quasi steady no cycles and is sustained by a dynamo mechanism that compensates for the continued loss of magnetic flux through the vertical boundaries we attribute the dynamo to the combination of differential rotation and the Parker instability although many of its details remain unclear. Vertical force balance in the lowbeta state is dominated by the mean magnetic pressure except at the midplane where thermal pressure support is always important this is true even when simulations are initialized at betall1 provided the thermal scaleheight of the disk is wellresolved. The efficient angular momentum transport in the lowbeta state may resolve longstanding tension between predictions of magnetorotational turbulence at high beta and observations likewise the bifurcation in accretion states we find may be important for understanding the state transitions observed in dwarf novae Xray binaries and changinglook AGN. We discuss directions for future work including the implications of our results for global accretion disk simulations. | 2024-09-01T00:00:00Z | ['arXiv:2409.05467', '10.48550/arXiv.2409.05467', '2024arXiv240905467S'] | ['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Astrophysics of Galaxies', 'Physics - Plasma Physics'] | Rapid strongly magnetized accretion in the zeronetverticalflux shearing box | 2,024 | 389 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.05467.pdf |
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