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2024arXiv240904525H | We study dipole ChernSimons theory with and without a cosmological constant in 21 dimensions. We write the theory in a second order formulation and show that this leads to a fracton gauge theory coupled to Aristotelian geometry which can also be coupled to matter. This coupling exhibits the remarkable property of generalizing dipole gauge invariance to curved spacetimes without placing any limitations on the possible geometries. We also use the second order formulation to construct a higher dimensional generalization of the action. Finally for the 21dimensional ChernSimons theory we find solutions and interpret these as electric monopoles analyze their charges and argue that the asymptotic symmetries are infinitedimensional. | 2024-09-01T00:00:00Z | ['2024arXiv240904525H', '10.48550/arXiv.2409.04525', 'arXiv:2409.04525'] | ['High Energy Physics - Theory', 'Condensed Matter - Strongly Correlated Electrons', 'General Relativity and Quantum Cosmology'] | Fractons on curved spacetime in 21 dimensions | 2,024 | 390 | 0.17 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.04525.pdf |
2024arXiv240912697D | We revisit the Unruh effect with a direct probabilitylevel calculation. We rederive the transition rate of a uniformly accelerating UnruhDeWitt monopole detector coupled to a massive scalar field from both the perspective of an inertial Minkowski observer and an accelerating Rindler observer. We show that for a measurement at a finite time after the initial state is prepared the two perspectives give the same transition rate. We show that an inertial detector in a thermal bath of Minkowski particles responds differently to the accelerated detector which perceives a thermal bath of Rindler particles except in the case of a massless field where there is agreement at all times. Finally numerical results for the transition rate are presented and explained. We highlight the transient effects caused by forcing the field to initially be in the Minkowski vacuum state. | 2024-09-01T00:00:00Z | ['arXiv:2409.12697', '2024arXiv240912697D', '10.48550/arXiv.2409.12697'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology'] | A new study of the Unruh effect | 2,024 | 390 | 0 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.12697.pdf |
2024arXiv240910616S | Orbits of celestial objects especially the geocentric and heliocentric ones have been well explored to constrain new longrange forces beyond the Standard Model SM often referred to as fifth forces. In this paper for the first time we apply the motion of a spacecraft around Jupiter to probe fifth forces that dont violate the equivalence principle. The spacecraft is the Juno orbiter and ten of its early orbits already allow a precise determination of the Jovian gravitational field. We use the shift in the precession angle as a proxy to test nongravitational interactions between Juno and Jupiter. Requiring that the contribution from the fifth force does not exceed the uncertainty of the precession shift inferred from data we find that a new parameter space with the mass of the fifthforce mediator around 1014 eV is excluded at 95 C.L. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.10616', '2024arXiv240910616S', 'arXiv:2409.10616'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'Physics - Space Physics'] | The Juno Mission as a Probe of LongRange New Physics | 2,024 | 392 | 0.37 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.10616.pdf |
2024JCAP...10..065B | We investigate the implications of memory burden on the gravitational wave GW spectrum arising from the Hawking evaporation of light primordial black holes PBHs. By considering both rotating Kerr and nonrotating Schwarzschild PBHs we demonstrate that the overproduction of primordial GWs from burdened PBHs could impose stringent constraints on the parameters governing backreaction effects. These constraints derived from N SUBeffSUB measurements by Planck and prospective experiments such as CMBS4 and CMBHD offer novel insights into the impact of memory burden on PBH dynamics. | 2024-10-01T00:00:00Z | ['arXiv:2409.05953', '10.48550/arXiv.2409.05953', '2024arXiv240905953B', '10.1088/1475-7516/2024/10/065', '2024JCAP...10..065B'] | ['physics of the early universe', 'primordial black holes', 'recombination', 'General Relativity and Quantum Cosmology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Constraining burdened PBHs with gravitational waves | 2,024 | 392 | 0.36 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 7 | https://arxiv.org/pdf/2409.05953.pdf |
2024arXiv240907515D | We demonstrate that the anomalous ionization rate observed in the Central Molecular Zone can be attributed to MeV dark matter annihilations into ee pairs for galactic dark matter profiles with slopes gammagt1. The low annihilation crosssections required avoid cosmological constraints and imply no detectable inverse Compton bremsstrahlung or synchrotron emissions in radio X and gamma rays. The possible connection to the source of the unexplained 511 keV line emission in the Galactic Center suggests that both observations could be correlated and have a common origin. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.07515', '2024arXiv240907515D', 'arXiv:2409.07515'] | ['High Energy Physics - Phenomenology', 'Astrophysics - High Energy Astrophysical Phenomena'] | Anomalous Ionization in the Central Molecular Zone by subGeV Dark Matter | 2,024 | 393 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07515.pdf |
2024arXiv240906771Z | Models of a dark radiation sector with a mass threshold WZDR have proved to be an appealing alternative to LambdaCDM. These models provide simple comparison models grounded in wellunderstood particle physics and with limited additional parameters. In addition they have shown relevance in easing existing cosmological tensions specifically the H0 tension and the S8 tension. Recently measurements of CMB lensing by the ACT collaboration have provided strong additional information on clustering at late times. Within LambdaCDM these results yield a high value of S8 at odds with weaklensing measurements. In this work we study this in the context of WZDR and find a much wider range of allowed values of S8 and in particular much better agreement between data sets and an overall improvement of fit versus LambdaCDM. We expand our analyses to include a wide set of data including the ACTDR6 lensing data as well as primary CMB information from ACTDR4 and SPT3G scaledependent power spectra from DES and measurements of H0 from SH0ES. We find that there is little to no tension in measurements of structure within the data sets and the inferred value of S8 is generally lower than that in LambdaCDM. We find that the inclusion of DES generally favors a higher H0 but there is some direct tension between the highell multipole data and this result. Future data should clarify whether this is a statistical artifact or a true incompatibility of these datasets within this model. | 2024-09-01T00:00:00Z | ['arXiv:2409.06771', '10.48550/arXiv.2409.06771', '2024arXiv240906771Z'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Searching for Dark Matter Interactions with ACT SPT and DES | 2,024 | 393 | 0.35 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.06771.pdf |
2024AJ....168..281B | Planets and the stars they orbit are born from the same cloud of gas and dust and the primordial compositions of rocky exoplanets have been assumed to have iron and refractory abundance ratios consistent with their host star. To test this assumption we modeled the interior irontorock ratio of 20 superEarthsized 11.8 R SUBSUB exoplanets around stars with homogeneously measured stellar parameters. We computed the core mass fraction CMF for each planet and an equivalent core mass fraction for each host star based on its Fe and Mg abundances. We then fit a linear correlation using two methods ordinary least squares and orthogonal distance regression between planetary and stellar CMF obtaining substantially different slopes between these two methods m 1.3 1.0 and m 5.6 1.6 respectively. Additionally we find that 75 of planets have a CMF consistent with their host star to within 1 and do not identify a distinct population of highdensity superMercuries. Overall we conclude that current uncertainties in observational data and differences in modeling methods prevent definitive conclusions about the relationship between planet and hoststar chemical compositions. | 2024-12-01T00:00:00Z | ['2024AJ....168..281B', '2024arXiv240908361B', '10.48550/arXiv.2409.08361', '10.3847/1538-3881/ad82eb', 'arXiv:2409.08361'] | ['Exoplanet astronomy', 'Extrasolar rocky planets', '486', '511', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics'] | Revisiting the Relationship Between Rocky Exoplanet and Stellar Compositions Reduced Evidence for a SuperMercury Population | 2,024 | 393 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2 | https://arxiv.org/pdf/2409.08361.pdf |
2024arXiv240905850B | In arXiv2312.14108 we argued that a sliver at the black hole mass in the Hilbert space of a quantum field theory on an AdS black hole with a stretched horizon has many desirable features of black hole microstates. A key observation is that the stretched horizon requires a finite Planck length i.e. finiteN. Therefore it is best viewed as a quantum horizon a proxy for the UVcomplete bulk description and not directly an element in the bulk EFT. It was shown in arXiv2312.14108 that despite the manifest absence of the interior the 2point function in the sliver is indistinguishable from the smooth horizon correlator up to the Page time. In this paper instead of boundary correlators we work directly in the bulk and demonstrate the appearance of the bulk HartleHawking correlator in the largeN limit. This is instructive because it shows that the analytic continuation across the horizon is emergent. It is a bulk transition to a Type III algebra and provides a structural distinction between black holes and weakly coupled thermal systems. We also identify a mechanism for universal code subspaces and interior tensor factors to appear via a quantum horizon version of thermal factorization. Our claims apply directly only within a Page window so they are not in immediate tension with firewall arguments. During a Page window typical heavy microstates probed by light single trace operators respond with effectively smooth horizons in lowpoint correlators. We work in 21 dimensions to be concrete but expect our results to hold in all higher dimensions. We discuss some important differences between our approach and the conventional fuzzball program and also argue that probenotions like infalling boundary conditions must be distinguished from microstatenotions like size of the EinsteinRosen bridge to make meaningful statements about postPage smoothness. | 2024-09-01T00:00:00Z | ['2024arXiv240905850B', '10.48550/arXiv.2409.05850', 'arXiv:2409.05850'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology'] | A BottomUp Approach to Black Hole Microstates | 2,024 | 396 | 0.25 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.05850.pdf |
2024ApJ...975..151H | Traditional star formation subgrid models implemented in cosmological galaxy formation simulations such as that of V. Springel amp L. Hernquist hereafter SH03 employ adjustable parameters to satisfy constraints measured in the local Universe. In recent years however theory and spatially resolved simulations of the turbulent multiphase starforming interstellar medium ISM have begun to produce new firstprinciples models which when fully developed can replace traditional subgrid prescriptions. This approach has advantages of being physically motivated and predictive rather than empirically tuned and allowing for varying environmental conditions rather than being tied to localUniverse conditions. As a prototype of this new approach by combining calibrations from the TIGRESS numerical framework with the pressureregulated feedbackmodulated PRFM theory simple formulae can be obtained for both the gas depletion time and an effective equation of state. Considering galaxies in TNG50 we compare the native simulation outputs with postprocessed predictions from PRFM. At TNG50 resolution the total midplane pressure is nearly equal to the total ISM weight indicating that galaxies in TNG50 are close to satisfying vertical equilibrium. The measured gas scale height is also close to theoretical equilibrium predictions. The slopes of the effective equations of states are similar but with effective velocity dispersion normalization from SH03 slightly larger than that from current TIGRESS simulations. Because of this and the decrease in PRFM feedback yield at high pressure the PRFM model predicts shorter gas depletion times than the SH03 model at high densities and redshift. Our results represent a first step toward implementing new numerically calibrated subgrid algorithms in cosmological galaxy formation simulations. | 2024-11-01T00:00:00Z | ['arXiv:2409.09121', '10.3847/1538-4357/ad73a4', '10.48550/arXiv.2409.09121', '2024arXiv240909121H', '2024ApJ...975..151H'] | ['Star formation', 'Interstellar medium', 'Stellar feedback', 'Magnetohydrodynamical simulations', '1569', '847', '1602', '1966', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Toward Implementation of the Pressureregulated Feedbackmodulated Model of Star Formation in Cosmological Simulations Methods and Application to TNG | 2,024 | 396 | 0.61 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 1 | https://arxiv.org/pdf/2409.09121.pdf |
2024arXiv240907524B | We introduce a treelevel chemical potential mechanism for spin1 particles within cosmological collider physics allowing them to be detected in primordial nonGaussianities for masses above the inflationary Hubble scale. We apply this mechanism to orbifold grand unification and the massive unification partners of the standard model gauge bosons. Our mechanism requires at least a pair of massive vector fields which are singlets of the standard model a condition which is satisfied in the classic trinification scenario. Assuming that the gauge hierarchy problem is solved by supersymmetry gauge coupling running points to unification partners at 1015 GeV. We show that within highscale inflation chemical potential enhancement can lead to observably strong signals for trinification partners in future cosmological surveys. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.07524', '2024arXiv240907524B', 'arXiv:2409.07524'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Grand Unification at the Cosmological Collider with Chemical Potential | 2,024 | 398 | 0.26 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.07524.pdf |
2024MNRAS.534.2858X | Giant planets on longperiod orbits around the nearest stars are among the easiest to directly image. Unfortunately these planets are difficult to fully constrain by indirect methods e.g. transit and radial velocity RV. In this study we present the discovery of a superJupiter HD 222237 b orbiting a star located inlineformulatexmath idTM0001 notationLaTeX11.445pm 0.002texmathinlineformula pc away. By combining RV data Hipparcos and multiepoch Gaia astrometry we estimate the planetary mass to be inlineformulatexmath idTM0002 notationLaTeX5.190.580.58 Mrm Juptexmathinlineformula with an eccentricity of inlineformulatexmath idTM0003 notationLaTeX0.560.030.03texmathinlineformula and a period of inlineformulatexmath idTM0004 notationLaTeX40.84.55.8texmathinlineformula yr making HD 222237 b a promising target for imaging using the MidInfrared Instrument MIRI of JWST. A comparative analysis suggests that our method can break the inclination degeneracy and thus differentiate between prograde and retrograde orbits of a companion. We further find that the inferred contrast ratio between the planet and the host star in the F1550C filter inlineformulatexmath idTM0005 notationLaTeX15.50 mu rm mtexmathinlineformula is approximately inlineformulatexmath idTM0006 notationLaTeX1.9times 104texmathinlineformula which is comparable with the measured limit of the MIRI coronagraphs. The relatively low metallicity of the host star inlineformulatexmath idTM0007 notationLaTeXrm 0.32 dextexmathinlineformula combined with the unique orbital architecture of this system presents an excellent opportunity to probe the planetmetallicity correlation and the formation scenarios of giant planets. | 2024-11-01T00:00:00Z | ['2024MNRAS.534.2858X', 'arXiv:2409.08067', '10.48550/arXiv.2409.08067', '2024MNRAS.tmp.2178X', '2024arXiv240908067X', '10.1093/mnras/stae2151'] | ['Astrophysics - Earth and Planetary Astrophysics'] | HD 222237 b a longperiod superJupiter around a nearby star revealed by radialvelocity and HipparcosGaia astrometry | 2,024 | 399 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.08067.pdf |
2024ApJ...976...33L | The James Webb Space Telescope opens a new window to directly probe luminous quasars powered by billion solar mass black holes in the Epoch of Reionization and their coevolution with massive galaxies with unprecedented details. In this paper we report the first results from a deep NIRSpec integral field unit spectroscopic study of a quasar at z 7.5. We obtain a bolometric luminosity of 1.8 10SUP47SUP erg sSUP1SUP and a black hole mass of 0.72.5 10SUP9SUP M SUBSUB based on the H emission line in the quasar spectrum. We discover 2 kpc scale highly blueshifted 870 km sSUP1SUP and broad 1400 km sSUP1SUP O III line emission after the quasar pointspread function has been subtracted. Such line emission most likely originates from a fast quasardriven outflow the earliest one at galactic scales known so far. The dynamical properties of this outflow fall within the typical ranges of quasardriven outflows at lower redshift and the outflow may be fast enough to reach the circumgalactic medium. Combining both the extended and nuclear outflow together the mass outflow rate 300 M SUBSUB yrSUP1SUP is 60380 of the star formation rate of the quasar host galaxy suggesting that the outflow may expel a significant amount of gas from the inner region of the galaxy. The kinetic energy outflow rate 3.6 10SUP44SUP erg sSUP1SUP is 0.2 of the quasar bolometric luminosity which is comparable to the minimum value required for negative feedback based on simulation predictions. The dynamical timescale of the extended outflow is 1.7 Myr consistent with the typical quasar lifetime in this era. | 2024-11-01T00:00:00Z | ['2024arXiv240913189L', '10.3847/1538-4357/ad7de4', '2024ApJ...976...33L', 'arXiv:2409.13189', '10.48550/arXiv.2409.13189'] | ['Quasars', 'Supermassive black holes', 'AGN host galaxies', '1319', '1663', '2017', 'Astrophysics - Astrophysics of Galaxies'] | Fast Outflow in the Host Galaxy of the Luminous z 7.5 Quasar J10072115 | 2,024 | 399 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.13189.pdf |
2024arXiv240906778S | Axionlike scalar fields can induce temporary deviations from the standard expansion history of the universe. The scalar fields contribution to the energy density of the universe grows while the field is held constant by Hubble friction but when the scalar field starts to evolve its energy density decreases faster than the radiation density for some potentials. We explore the observational signatures of such a scalar field that becomes dynamical between big bang nucleosynthesis and matterradiation equality which we call very Early Dark Energy vEDE. If vEDE momentarily dominates the energy density of the universe it generates a distinctive feature in the matter power spectrum that includes a bump on scales that enter the horizon just after the scalar field starts to evolve. For k gtrsim 10htextMpc1 the amplitude of this bump can exceed the amplitude of the standard matter spectrum. The power on scales on either side of this peak is suppressed relative to the standard power spectrum but only scales that are within the horizon while the scalar field makes a significant contribution to the total energy density are affected. We determine how vEDE scenarios are constrained by observations of the cosmic microwave background measurements of the primordial deuterium abundance and probes of the latetime expansion history. We find that current observations are consistent with vEDE scenarios that enhance power on scales k gtrsim 30htextMpc1 and nearly double the amplitude of the matter power spectrum around 200htextMpc1. These scenarios also suppress power on scales between 0.3htextMpc1 and 30htextMpc1. | 2024-09-01T00:00:00Z | ['2024arXiv240906778S', '10.48550/arXiv.2409.06778', 'arXiv:2409.06778'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Signatures of Very Early Dark Energy in the Matter Power Spectrum | 2,024 | 400 | 0.38 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.06778.pdf |
2024AJ....168..252A | The detection of stellar variability often relies on the measurement of selected activity indicators such as coronal emission lines and nonthermal emissions. On the flip side the effective stellar temperature is normally seen as one of the key fundamental parameters with mass and radius to understanding the basic physical nature of a star and its relation with its environment e.g. planetary instellation. We present a novel approach for measuring diskaveraged temperature variations to subKelvin accuracy inspired by algorithms developed for precision radial velocity pRV. This framework uses the entire content of the spectrum not just preidentified lines and can be applied to existing data obtained with highresolution spectrographs. We demonstrate the framework by recovering the known rotation periods and temperature modulation of Barnard star and AU Mic in data sets obtained in the infrared with SPIRou at CHFT and at optical wavelengths on Eridani with HARPS at ESO 3.6 m telescope. We use observations of the transiting hot Jupiter HD189733b obtained with SPIRou to show that this method can unveil the minute temperature variation signature expected during the transit event an effect analogous to the RossiterMcLaughlin effect but in temperature space. This method is a powerful new tool for characterizing stellar activity and in particular temperature and magnetic features at the surfaces of cool stars affecting both pRV and transit spectroscopic observations. We demonstrate this method in the context of highresolution spectroscopy but it could be used at lower resolution. | 2024-12-01T00:00:00Z | ['arXiv:2409.07260', '10.3847/1538-3881/ad7b30', '2024AJ....168..252A', '2024arXiv240907260A', '10.48550/arXiv.2409.07260'] | ['Stellar effective temperatures', 'High resolution spectroscopy', 'Time series analysis', '1597', '2096', '1916', 'Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Instrumentation and Methods for Astrophysics'] | Measuring SubKelvin Variations in Stellar Temperature with Highresolution Spectroscopy | 2,024 | 401 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.07260.pdf |
2024arXiv240911359E | A dark sector with a very large number of massive degrees of freedom is generically constrained by radiative corrections to Newtons constant. However there are caveats to this statement especially if the degrees of freedom are light or massless. Here we examine in detail and update a number of constraints on the possible number of dark degrees of freedom including from black hole evaporation from perturbations to systems including an evaporating black hole from direct gravitational production at colliders from highenergy cosmic rays and from supernovae energy losses. | 2024-09-01T00:00:00Z | ['2024arXiv240911359E', 'arXiv:2409.11359', '10.48550/arXiv.2409.11359'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena', 'High Energy Physics - Theory'] | Constraints on the maximal number of dark degrees of freedom from black hole evaporation cosmic rays colliders and supernovae | 2,024 | 401 | 0.35 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.11359.pdf |
2024arXiv240808513M | The Ohio State University Big Ear radio telescope detected in 1977 the Wow Signal one of the most famous and intriguing signals of extraterrestrial origin. Characterized by its strong relative intensity and narrow bandwidth near the 1420 MHz hydrogen line its source has never been detected again despite numerous followup attempts. Arecibo Wow is a new technosignature project using archived data from the Arecibo Observatory. Here we present our first results of drift scans made between February and May 2020 at 1420 MHz. The methods frequency and bandwidth of these observations are similar to those used to detect the Wow Signal. However our observations are more sensitive have better temporal resolution and include polarization measurements. We report the detection of narrowband signals 10 kHz near the hydrogen line similar to the Wow Signal although twoorders of magnitude less intense and in multiple locations. Despite the similarities these signals are easily identifiable as small interstellar clouds of cold hydrogen HI in the galaxy. We hypothesize that the Wow Signal was caused by a sudden brightening of the hydrogen line in these clouds triggered by a strong transient radiation source such as a magnetar flare or a soft gamma repeater SGR. A maser flare or superradiance mechanisms can produce stimulated emission consistent with the Wow Signal. Our hypothesis explains all observed properties of the Wow Signal proposes a new source of false positives in technosignature searches and suggests that the Wow Signal could be the first recorded event of an astronomical maserlike flare in the hydrogen line. | 2024-08-01T00:00:00Z | ['arXiv:2408.08513', '10.48550/arXiv.2408.08513', '2024arXiv240808513M'] | ['Astrophysics - High Energy Astrophysical Phenomena'] | Arecibo Wow I An Astrophysical Explanation for the Wow Signal | 2,024 | 402 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2408.08513.pdf |
2024MNRAS.534.1827J | Binary systems comprise approximately 15 per cent of the nearEarth asteroid population yet thermalinfrared IR data are often interpreted for these bodies as if they are single objects. ThermalIR light curves of binary asteroids 3905 Doppler and 175706 1996 FG3 are analysed using an adaptation of the Advanced Thermophysical Model deriving new constraints on their thermal inertias as inlineformulatexmath idTM0001 notationLaTeXGamma 114 pm 31 mathrmJ mathrmm2 mathrmK1 mathrms12texmathinlineformula and inlineformulatexmath idTM0002 notationLaTeXGamma 142 pm 6 mathrmJ mathrmm2 mathrmK1 mathrms12texmathinlineformula respectively. We determine that this adapted model is suitable for binary systems where their primary rotation to secondary orbit period ratios can be approximately characterized by small integers. Objects with more complex orbital states require a model with alternative temperature convergence methodologies. Thermal inertia is shown to have a strong effect on binary thermophysical lightcurve morphology introducing significant modulations both inside and outside of mutual event times. The depths of eclipse events are shown to be suppressed at longer wavelengths due to the sensitivity to cooler parts of the surface meanwhile surface roughness is shown to have little effect on the thermal lightcurve morphology. A proof of concept model for the 65803 Didymos system is demonstrated showing how such a binary model could be used to study the system during the European Space Agencys Hera mission and the applicability of this adapted model to NASAs Lucy mission is also briefly discussed. | 2024-11-01T00:00:00Z | ['10.48550/arXiv.2409.12703', '10.1093/mnras/stae2196', '2024MNRAS.534.1827J', '2024MNRAS.tmp.2146J', '2024arXiv240912703J', 'arXiv:2409.12703'] | ['Astrophysics - Earth and Planetary Astrophysics'] | Thermophysical modelling of eclipse and occultation events in binary asteroid systems | 2,024 | 403 | 0.49 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.12703.pdf |
2024arXiv240904624D | A successful theory of star formation should predict the number of objects as a function of their mass produced through starforming events. Previous studies in starforming regions and the solar neighborhood identify a mass function increasing from the hydrogenburning limit down to about 10 MJ. Theory predicts a limit to the fragmentation process providing a natural turnover in the mass function down to the opacity limit of turbulent fragmentation thought to be 210 MJ. Programs to date have not been sensitive enough to probe the hypothesized opacity limit of fragmentation. Here we present the first identification of a turnover in the initial mass function below 12 MJ within NGC 2024 a young starforming region. With JWSTNIRCam deep exposures across 0.75 mum we identified several free floating objects down to 3 MJ with sensitivity to 0.5 MJ. We present evidence for a double power law model increasing from about 60 MJ to roughly 12 MJ consistent with previous studies followed by a decrease down to 0.5 MJ. Our results support the predictions of star and brown dwarf formation theory identifying the theoretical turnover in the mass function and suggest the fundamental limit of turbulent fragmentation near 3 MJ. | 2024-09-01T00:00:00Z | ['arXiv:2409.04624', '2024arXiv240904624D', '10.48550/arXiv.2409.04624'] | ['Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Astrophysics of Galaxies'] | Identification of a turnover in the initial mass function of a young stellar cluster down to 0.5 MJ | 2,024 | 404 | 0.63 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.04624.pdf |
2024arXiv240912231B | We motivate a relation between dark energy and the scale of new physics in weakly coupled string theory. This mixing between infrared and ultraviolet physics leads to a unique corner for realworld phenomenology barring finetunings we are naturally led to the dark dimension scenario a single mesoscopic extra dimension of micron size with the standard model localized on Dbranes. Our explicit topdown worldsheet derivation establishes it on a more solid grounding. Allowing some finetuning such that the vacuum energy only arise at higher orders in string perturbation theory the little string theory scenario with a very weakly coupled string is an alternative possibility. In this case the string scale lies at the edge of detectability of particle accelerators. | 2024-09-01T00:00:00Z | ['arXiv:2409.12231', '10.48550/arXiv.2409.12231', '2024arXiv240912231B'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Phenomenology'] | Dark dimension with little strings attached | 2,024 | 404 | 0.23 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.12231.pdf |
2024RNAAS...8..240C | It was recently claimed that evidence for a stochastic gravitational wave background observed by pulsar timing arrays can be attributed instead to random perturbations of the Suns motion by transiting asteroids. I show that that this would lead to a large dipole component accompanying a much smaller quadrupolar perturbation of pulsar timing signals which would not be confused with a gravitational wave signal. Such an anomalous dipole would have been detected and identified as a spurious background by the PTA collaborations if it existed. | 2024-09-01T00:00:00Z | ['2024RNAAS...8..240C', 'arXiv:2409.13692', '10.3847/2515-5172/ad7e19', '2024arXiv240913692C', '10.48550/arXiv.2409.13692'] | ['Gravitational wave astronomy', '675', 'General Relativity and Quantum Cosmology', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics'] | No Pulsar Timing Noise from Brownian Motion of the Sun | 2,024 | 405 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 0 | https://arxiv.org/pdf/2409.13692.pdf |
2024ApJ...976L..11R | We present updated constraints on cosmological parameters in a 12parameter model extending the standard sixparameter CDM by including dynamical dark energy DE w SUB0SUB w SUB a SUB the sum of neutrino masses m SUB SUB the effective number of nonphoton radiation species N SUBeffSUB the lensing amplitude scaling A SUBlensSUB and the running of the scalar spectral index SUB s SUB. For cosmic wave background CMB data we use the Planck Public Release PR 4 2020 HiLLiPoP and LoLLiPoP likelihoods Planck PR4Atacama Cosmology Telescope ACT DR6 lensing and Planck 2018 low TT likelihoods along with DESI DR1 baryon acoustic oscillations BAO and Pantheon and DESY5 uncalibrated Type Ia supernovae SNe likelihoods. Key findings are the following i Contrary to DESI results CMBBAOPantheon data include a cosmological constant within 2 while CMBBAODESY5 excludes it at over 2 indicating the dynamical nature of DE is not yet robust. Potential systematics in the DESY5 sample may drive this exclusion. ii Some data combinations show a 1 detection of nonzero m SUB SUB indicating possible future detection. We also provide a robust upper bound of m SUB SUB 0.3 eV 95 confidence limit CL. iii With CMBBAOSNe A SUBlensSUB 1 is included at 2 albeit not at 1 indicating no significant lensing anomaly in this extended cosmology with Planck PR4 likelihoods. iv The Hubble tension persists at 3.2 to 3.9 suggesting these simple extensions do not resolve it. v The S SUB8SUB tension with Dark Energy Survey Year 3 weak lensing is reduced to 1.4 likely due to additional parameters and the Planck PR4 likelihoods. | 2024-11-01T00:00:00Z | ['2024ApJ...976L..11R', '10.3847/2041-8213/ad8c26', 'arXiv:2409.13022', '10.48550/arXiv.2409.13022', '2024arXiv240913022C'] | ['Dark energy', 'Neutrino masses', 'Cosmological neutrinos', 'Hubble constant', 'Cosmic microwave background radiation', 'Baryon acoustic oscillations', 'Type Ia supernovae', '351', '1102', '338', '758', '322', '138', '1728', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Updated Cosmological Constraints in Extended Parameter Space with Planck PR4 DESI Baryon Acoustic Oscillations and Supernovae Dynamical Dark Energy Neutrino Masses Lensing Anomaly and the Hubble Tension | 2,024 | 405 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 14 | https://arxiv.org/pdf/2409.13022.pdf |
2024ApJ...975..113J | We present a suite of six highresolution chemodynamical simulations of isolated galaxies spanning observed diskdominated environments on the starforming main sequence as well as quenched bulgedominated environments. We compare and contrast the physics driving star formation and stellar feedback among the galaxies with a view to modeling these processes in cosmological simulations. We find that the mass loading of galactic outflows is coupled to the clustering of supernova explosions which varies strongly with the rate of galactic rotation v SUBcircSUBR via the Toomre length leading to smoother gas disks in the bulgedominated galaxies. This sets an equation of state in the starforming gas that also varies strongly with so that the bulgedominated galaxies have higher midplane densities lower velocity dispersions and higher molecular gas fractions than their mainsequence counterparts. The star formation rate in five out of six galaxies is independent of and is consistent with regulation by the midplane gas pressure alone. In the sixth galaxy which has the most centrally concentrated bulge and thus the highest we reproduce dynamical suppression of the star formation efficiency in agreement with observations. This produces a transition away from pressureregulated star formation. | 2024-11-01T00:00:00Z | ['2024ApJ...975..113J', '10.48550/arXiv.2409.09114', 'arXiv:2409.09114', '10.3847/1538-4357/ad793f', '2024arXiv240909114J'] | ['Disk galaxies', 'Lenticular galaxies', 'Spiral galaxies', 'Interstellar medium', 'Star formation', 'Hydrodynamical simulations', 'Stellar feedback', 'Galactic and extragalactic astronomy', 'Galaxy processes', 'Galaxy properties', 'Galaxy structure', '391', '915', '1560', '847', '1569', '767', '1602', '563', '614', '615', '622', 'Astrophysics - Astrophysics of Galaxies'] | Learning the Universe GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Mainsequence and Quenched Galactic Environments | 2,024 | 407 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.09114.pdf |
2024A&A...689A.250C | Context. Atmospheric and dynamical processes are thought to play a major role in shaping the distribution of closein exoplanets. A striking feature of such distribution is the Neptunian desert a dearth of Neptunes on the shortestperiod orbits. Aims. We aimed to define the boundaries of the Neptunian desert and study its transition into the savanna a moderately populated region at larger orbital distances. Our goal was to acquire new insight into the processes that carved out the Neptunian landscape and to provide the exoplanet community with a framework for conducting studies on planet formation and evolution. Methods. We built a sample of planets and candidates based on the Kepler DR25 catalogue and weighed it according to the transit and detection probabilities. We then used the corrected distribution to study occurrences across the period and periodradius spaces. Results. We delimited the Neptunian desert as the closein region of the periodradius space with no planets at a 3 level and provide the community with simple readytouse approximate boundaries. We identified an overdensity of planets separating the Neptunian desert from the savanna 3.2 days PSUBorbSUB 5.7 days that stands out at a 4.7 level above the desert and at a 3.5 level above the savanna which we propose to call the Neptunian ridge. The period range of the ridge matches that of the wellknown hot Jupiter pileup 35 days which suggests that similar evolutionary processes might act on both populations. We find that the occurrence fraction between the pileup and warm Jupiters SUBpileupwarmSUB 5.3 1.1 is about twice that between the Neptunian ridge and savanna SUBridgesavannaSUB 2.7 0.5. This indicates either that the processes that drive or maintain planets in the overdensity are more efficient for Jupiters or that the processes that drive or maintain planets in the warm region are more efficient for Neptunes. Conclusions. Our revised landscape supports a previous hypothesis that a fraction of Neptunes were brought to the edge of the desert i.e. the newly identified ridge through higheccentricity tidal migration HEM late in their life surviving the evaporation that eroded Neptunes having arrived earlier in the desert. The ridge thus appears as a true physical feature illustrating the interplay between photoevaporation and HEM providing further evidence of their role in shaping the distribution of closein Neptunes. | 2024-09-01T00:00:00Z | ['arXiv:2409.10517', '10.48550/arXiv.2409.10517', '2024A&A...689A.250C', '10.1051/0004-6361/202450957', '2024arXiv240910517C'] | ['planets and satellites: atmospheres', 'planets and satellites: dynamical evolution and stability', 'planets and satellites: formation', 'planets and satellites: gaseous planets', 'planets and satellites: physical evolution', 'Astrophysics - Earth and Planetary Astrophysics'] | Mapping the exoNeptunian landscape A ridge between the desert and savanna | 2,024 | 408 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 4 | https://arxiv.org/pdf/2409.10517.pdf |
2024arXiv240905946O | We investigate the spatial offsets between dust and ultraviolet UV emission in highredshift galaxies using the Cosmic Dawn III CoDa III simulation a stateoftheart fully coupled radiationhydrodynamics cosmological simulation. Recent observations have revealed puzzling spatial disparities between ALMA dust continuum and UV emission as seen by HST and JWST in galaxies at z57 compelling us to propose a physical interpretation of such offsets. Our simulation which incorporates a dynamical dust model naturally reproduces these offsets in massive UVbright galaxies log10MrmDMModotgt11.5 MrmAB1500lt20. We find that dustUV offsets increase with halo mass and UV brightness reaching up to sim 2 pkpc for the most massive systems in good agreement with observational data from the ALPINE and REBELS surveys. Our analysis reveals that these offsets primarily result from severe dust extinction in galactic centers rather than a misalignment between dust and stellar mass distributions. The dust remains wellaligned with the bulk stellar component and we predict the dust continuum should therefore align well with the stellar restframe NIR component less affected by dust attenuation. This study provides crucial insights into the complex interplay between star formation dust distribution and observed galaxy morphologies during the epoch of reionization highlighting the importance of dust in shaping the appearance of early galaxies at UV wavelengths. | 2024-09-01T00:00:00Z | ['2024arXiv240905946O', 'arXiv:2409.05946', '10.48550/arXiv.2409.05946'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | DustUV offsets in highredshift galaxies in the Cosmic Dawn III simulation | 2,024 | 408 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.05946.pdf |
2024arXiv240906504K | Context. Supernova remnants SNRs are the late stages of supernovae before their merging into the surrounding medium. Oxygenrich supernova remnants represent a rare subtype with strong visible light oxygen emission. Aims. We present a new method to detect SNRs exploiting the capabilities of modern visiblelight integralfield units based on the shapes of the SNR emission lines. Methods. We search for unresolved shocked regions with broadened emission lines using the mediumresolution integralfield spectrograph MUSE on the Very Large Telescope. The spectral resolving power allows shocked emission sources to be differentiated from photoionised sources based on the linewidths. Results. We find 307 supernova remnants including seven Orich SNRs. For all Orich SNRs we observe the O IIIlambdalambda49595007 emission doublet. In addition we observe emissions from O Ilambdalambda63006364 O IIlambdalambda73207330 HalphaN IIlambda6583 and S IIlambdalambda67176731 to varying degrees. The linewidths for the Orich SNRs are generally broader than the rest of the SNRs in the sample of this article. The oxygen emission complexes are reminiscient of SNR 44491 and some longlasting SNe. For the Orich SNRs we also search for counterparts in archival data of other telescopes we detect Xray and midIR counterparts for a number of remnants. Conclusions. We have shown efficacy of the method to detect SNRs presented in this article. In addition the method is also effective in detecting the rare Orich SNRs doubling the sample size in the literature. The origin of Orich SNRs and their link to specific SN types or environments is still unclear but further work into this new sample will unquestionably help us shed light on these rare remnants. | 2024-09-01T00:00:00Z | ['arXiv:2409.06504', '2024arXiv240906504K', '10.48550/arXiv.2409.06504'] | ['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Astrophysics of Galaxies'] | Discovery of young oxygenrich supernova remnants in PHANGSMUSE galaxies | 2,024 | 408 | 0.53 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.06504.pdf |
2024arXiv240908932Z | In this letter we highlight the structure and main properties of an abstract approach to quantum cosmology and gravity dubbed SUinftyQGR. Beginning from the concept of the Universe as an isolated quantum system the main axiom of the model is the existence of infinite number of mutually commuting observables. Consequently the Hilbert space of the Universe represents SUinfty symmetry. This Universe as a whole is static and topological. Nonetheless quantum fluctuations induce local clustering in its quantum state and divide it to approximately isolated subsystems representing G times SUinfty symmetry where G is a generic finite rank internal symmetry for each subsystem that is entangled to the rest of the Universe by the global SUinfty symmetry. In addition to parameters characterizing representation of G by subsystems their states depend on 4 continuous parameters two of them characterize the representation of SUinfty a dimensionful parameter arises from the possibility of comparing representations of SUinfty by different subsystems and the forth parameter is a measurable used as time registered by an arbitrary subsystem chosen as a quantum clock. They introduce a relative dynamics for subsystem formulated by a symmetry invariant effective Lagrangian defined on the 31D parameter space. At lowest quantum order it is a YangMills field theory for both SUinfty and internal symmetries. We identify the common SUinfty symmetry and its interaction with gravity. Thus SUinftyQGR predicts a spin1 mediator for quantum gravity. Apparently this is in contradiction with classical gravity. Nonetheless we show that an observer unable to detect the quantumness of gravity perceives its effect as the curvature of the space of average values of aforementioned parameters. We prove that emergent spacetime has a Lorentzian geometry. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.08932', '2024arXiv240908932Z', 'arXiv:2409.08932'] | ['General Relativity and Quantum Cosmology', 'High Energy Physics - Theory', 'Quantum Physics'] | SUinfty Quantum Gravity and Cosmology | 2,024 | 410 | 0.3 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.08932.pdf |
2024OJAp....7E.107M | Recent observations by the James Webb Space Telescope confirm the existence of massive black holes gt106 beyond the redshift of z10. However their formation mechanisms still remain an open question. Light seed black holes are one such formation pathway forming as the end stage of metalfree Population III stars. Light seed black holes can grow into massive black holes as long as they accrete near the Eddington limit for substantial periods or undergo several bursts of superEddington accretion. In this work our aim is to ascertain if light seeds can grow in gas rich galaxies similar to those expected at high redshift z 10. Using the Arepo code we follow selfconsistently the formation of Population III stars and black holes in galaxies with total masses in the range 108 . We find that in the absence of feedback black holes can grow to 105 in just 104 years. These black holes do not decouple from the gas clumps in which they are born and are able to accrete at hyperEddington rates. In the presence of supernova feedback the number of actively growing black holes diminishes by an order of magnitude. However we still observe hyperEddington accretion in approximately 1 of the black hole population despite supernova feedback. This idealised work lays the foundation for future works where we will test our models in a cosmological framework. In this work we neglect radiative feedback processes from stellar evolution and from accretion onto the growing black holes. This likely means that our results represent an upper limit to light seed growth. We will address these shortcomings in a future work. | 2024-11-01T00:00:00Z | ['10.48550/arXiv.2409.08326', '2024OJAp....7E.107M', '10.33232/001c.126629', '2024arXiv240908326M', 'arXiv:2409.08326'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Growth of LightSeed Black Holes in GasRich Galaxies at High Redshift | 2,024 | 410 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 3 | https://arxiv.org/pdf/2409.08326.pdf |
2024arXiv240813803F | We study finite temperature effects in string cosmology and their potential gravitational wave signature. Expanding on our recent work arXiv2310.11494 we consider a general configuration of highly excited open and closed strings at high enough temperature to be in the Hagedorn phase in 31 dimensions in order to explore its cosmological implications. We find conditions which can be satisfied in compactifications with moduli stabilization that allow the long strings to remain in equilibrium in a controlled effective field theory with equilibration driven by the joining and splitting of the dominant open string population. We calculate the emission rate of gravitons by long open strings which we show is determined by ten dimensional flat space transition amplitudes available in the literature and then find the total gravitational wave spectrum generated by the gas of long strings. The gravitational wave spectrum has robust characteristics. It peaks at frequencies of order 50100 GHz the same as for gravitational waves from the reheating epoch of the Standard Model. But the amplitude of the string signal is significantly larger than predicted by the Standard Model and its field theoretic extensions. The amplitude and other physical observables such as the contribution to Delta Ntext eff are directly proportional to the string scale Ms indicating that a potential signal may also determine the string scale. Our calculations provide one of the few examples of a signal of stringy origin that dominates over the field theory predictions. We give a physical explanation of our results and discuss further implications. | 2024-08-01T00:00:00Z | ['10.48550/arXiv.2408.13803', 'arXiv:2408.13803', '2024arXiv240813803F'] | ['High Energy Physics - Theory', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Gravitational Waves from High Temperature Strings | 2,024 | 411 | 0.23 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2408.13803.pdf |
2024arXiv240913441F | Recent observations by the James Webb Space Telescope JWST have revealed a previously hidden population of extremely bright and compact objects between redshifts of z sim 4 and z sim 10. Given their extreme red colouring in the observed frame these galaxies have been dubbed Little Red Dots LRDs. The aim of this project was to identify LRDs using photometric data from previously uninvestigated JWST datasets and to estimate their AGN fractions by fitting the spectral energy distribution of each galaxy against well calibrated templates using CIGALE. We identified a list of potential LRDs using a single colour cut of F444WF277W gt1.5 mag and by applying a morphological analysis. We used EAZY to estimate the photometric redshift and CIGALE to estimate the AGN fraction of each LRD. Overall we identified 14 LRDs applying accurate SED fits to 11 of them. We found that 7 of them had a high AGN fraction with the AGN component generating more than 50 of the observed flux a further two LRDs had AGN contribution in excess of approximately 40. In total nine LRDs our of 14 are likely to have a supermassive black hole in their centre. Interestingly the three LRDs which could not be well fit by CIGALE displayed extremely high photometric redshifts zphot gtrsim 11 and require further analysis and may also host a supermassive black hole in their centre. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.13441', 'arXiv:2409.13441', '2024arXiv240913441F'] | ['Astrophysics - Astrophysics of Galaxies'] | Searching For JWSTs Little Red Dots | 2,024 | 412 | 0.56 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.13441.pdf |
2024A&A...691L...2S | Aims. The cold molecular gas mass is one of the crucial yet challenging parameters in galaxy evolution studies. Here we introduce a new calibration and a method for estimating molecular gas masses using midinfrared MIR photometry. This topic is timely as the James Webb Space Telescope JWST now allows us to detect the MIR emission of typical mainsequence galaxies across a wide range of masses and star formation rates with modest time investments. Additionally this Letter highlights the strong synergy between ALMA and JWST for studies of dust and gas at cosmic noon. Methods. We combined a sample of 14 mainsequence galaxies at z 1 3 with robust CO detections and multiband MIR photometry along with a literature sample at z 0 4 with CO and polycyclic aromatic hydrocarbon PAH spectroscopy to study the relationship between PAH CO10 and total IR luminosities. PAH luminosities are derived by modelling a wealth of restframe UV to submillimetre data. The new z 1 3 sample extends previous highz studies to PAH and CO luminosities that are about an order of magnitude lower into the regime of local starbursts for the first time. Results. The PAHtoCO luminosity ratio remains constant across a wide range of luminosities for various galaxy types and throughout the explored redshift range. In contrast the PAHtoIR and COtoIR luminosity ratios deviate from a constant value at high IR luminosities. The intrinsic scatter in the LPAHLCO relation is 0.21 dex with a median of 1.40 and a powerlaw slope of 1.07 0.04. Both the PAHIR and COIR relations are sublinear. Given the tight and uniform PAHCO relation over 3 orders of magnitude we provide a recipe for estimating the cold molecular gas mass of galaxies from PAH luminosities with a PAHtomolecular gas conversion factor of SUBPAHSUB7.7SUBSUB 3.08 1.084.3SUBCOSUB MSUBSUBLSUBSUB. This method opens a new window to explore the gas content of galaxies beyond the local Universe using multiwavelength JWSTMIRI imaging. | 2024-11-01T00:00:00Z | ['2024arXiv240905710S', '10.1051/0004-6361/202451826', '2024A&A...691L...2S', 'arXiv:2409.05710', '10.48550/arXiv.2409.05710'] | ['dust', 'extinction', 'ISM: general', 'galaxies: evolution', 'galaxies: formation', 'galaxies: ISM', 'Astrophysics - Astrophysics of Galaxies'] | The tight correlation between PAH and CO emission from z 0 to 4 | 2,024 | 413 | 0.62 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2 | https://arxiv.org/pdf/2409.05710.pdf |
2024arXiv240905815S | The radial distribution of gas within galactic haloes is connected to the star formation rate and the nature of baryondriven feedback processes. Using six variants of the hydrodynamic simulation Simba we study the impact of different stellarAGN feedback prescriptions on the gas density profiles of haloes in the total mass range 1011 mathrmModot lt Mmathrm200c lt 1014 mathrmModot and redshift interval 0ltzlt4. We find that the radial profiles are well represented by a power law and that for a fixed total halo mass the slope and amplitude of such power law are generally weakly dependent on redshift. Once AGNdriven jets are activated in the simulation the gas density profile of haloes with Mrm 200c gtrsim 1013 rm Modot declines more gently with radial distance. We argue that this distinctive feature could be exploited with current observations to discriminate amongst the predictions of the different feedback models. We introduce a universal fitting formula for the slope and amplitude of the gas density profile as a function of total halo mass and redshift. The bestfit functions are suitable for all feedback variants considered and their predictions are in excellent agreement with the numerical results. We provide the values of all fit parameters making our fitting formula a versatile tool to mimic the effect of Simba feedback models onto Nbody simulations and semianalytical models of galaxy formation. Our results can also aid observational estimates of the gas mass within haloes that assume a specific slope for the underlying gas density profile. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.05815', 'arXiv:2409.05815', '2024arXiv240905815S'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | The impact of feedback on the evolution of gas density profiles from galaxies to clusters a universal fitting formula from the Simba suite of simulations | 2,024 | 415 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.05815.pdf |
2024A&A...690A.109C | The observation of a massive galaxy with an extremely low dark matter content i.e. NGC 1277 has posed questions about how such objects form and evolve in a hierarchical universe. We here report on the finding of several massive dark matterdeficient galaxies in a set of 324 galaxy clusters theoretically modelled by means of fullphysics hydrodynamical simulations. We first focus on two example galaxies selected amongst the most massive and dark matterdeficient ones. By tracing the evolution of these galaxies we find that their lack of dark matter is a result of multiple pericentre passages. While orbiting their host halo tidal interactions gradually strip away dark matter while preserving the stellar component. A statistical analysis of all massive satellite galaxies in the simulated clusters shows that the stellartototal mass ratio today is strongly influenced by the number of orbits and the distance at pericentres. Galaxies with more orbits and closer pericentres are more dark matterdeficient. Additionally we find that massive dark matterdeficient galaxies at the present day are either the remnants of very massive galaxies at infall or former central galaxies of infalling groups. We conclude that such massive yet dark matterdeficient galaxies exist and are natural byproducts of typical cluster galaxy evolution with no specific requirement for an exotic formation scenario. | 2024-10-01T00:00:00Z | ['2024arXiv240910356C', '2024A&A...690A.109C', '10.1051/0004-6361/202451271', 'arXiv:2409.10356', '10.48550/arXiv.2409.10356'] | ['methods: numerical', 'galaxies: clusters: general', 'galaxies: general', 'galaxies: interactions', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | The Three Hundred The existence of massive dark matterdeficient satellite galaxies in cosmological simulations | 2,024 | 415 | 0.55 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 1 | https://arxiv.org/pdf/2409.10356.pdf |
2024AJ....168..276S | We present a JWST NearInfraRed Spectrograph NIRSpec transmission spectrum of the superEarth exoplanet L 9859 c. This small R SUB p SUB 1.385 0.085R SUBSUB M SUB p SUB 2.22 0.26 R SUBSUB warm T SUBeqSUB 553 K planet resides in a multiplanet system around a nearby bright J 7.933 M3V star. We find that the transmission spectrum of L 9859 c is featureless at the precision of our data. We achieve precisions of 22 ppm in NIRSpec G395Hs NRS1 detector and 36 ppm in the NRS2 detector at a resolution R 200 30 pixel wide bins. At this level of precision we are able rule out primordial HSUB2SUBHe atmospheres across a range of cloud pressure levels up to at least 0.1 mbar. By comparison to atmospheric forward models we also rule out atmospheric metallicities below 300 solar at 3 or equivalently atmospheric mean molecular weights below 10 g molSUP1SUP. We also rule out pure methane atmospheres. The remaining scenarios that are compatible with our data include a planet with no atmosphere at all or highermeanmolecularweight atmospheres such as COSUB2SUB or HSUB2SUBOrich atmospheres. This study adds to a growing body of evidence suggesting that planets 1.5 R SUBSUB lack extended atmospheres. | 2024-12-01T00:00:00Z | ['10.48550/arXiv.2409.07552', 'arXiv:2409.07552', '10.3847/1538-3881/ad73cf', '2024arXiv240907552S', '2024AJ....168..276S'] | ['Exoplanet astronomy', 'Exoplanet atmospheres', 'Exoplanet atmospheric composition', 'Exoplanets', 'Super Earths', '486', '487', '2021', '498', '1655', 'Astrophysics - Earth and Planetary Astrophysics'] | JWST COMPASS The 35 m Transmission Spectrum of the SuperEarth L 9859 c | 2,024 | 416 | 0.61 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.07552.pdf |
2024arXiv240906100G | We analyze textitJWST CEERS NIRCam images to present the first estimate of the observed fraction and properties of bars out to z sim 4. We analyze a sample of 1770 galaxies with stellar mass Mstar gt 1010 Modot at 0.5 leq z leq 4 and identify barred galaxies via ellipse fits and visual classification of both F200W and F444W images. Our results apply mainly to bars with projected semimajor axis arm bar gt 1.5 kpc sim 2 times PSF in F200W images that can be robustly traced by ellipse fits. For such bars the observed bar fraction at zsim 24 is low lesssim 10 and they appear to be emerging at least as early as zsim 4 when the Universe was sim 13 of its present age. At zsim 24 compared to our results TNG50 simulations predict a significantly larger bar fraction due to a large population of small bars with arm bar lt 1.5 kpc that we cannot robustly detect. If such a population exists the true bar fraction may be significantly higher than our results. At z ge 1.5 many barred galaxies show nearby neighbors suggesting bars may be tidally triggered. From z sim 4 to z sim 0.5 the observed bar fraction average projected bar length and projected bar strength rise. Our results highlight the early emergence and evolution of barred galaxies and the rising importance of bardriven secular evolution from z sim4 to today. | 2024-09-01T00:00:00Z | ['2024arXiv240906100G', 'arXiv:2409.06100', '10.48550/arXiv.2409.06100'] | ['Astrophysics - Astrophysics of Galaxies'] | The Abundance and Properties of Barred Galaxies out to z sim 4 Using textitJWST CEERS Data | 2,024 | 418 | 0.61 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.06100.pdf |
2024arXiv240907185S | The Euclid mission is a visionary project undertaken by the European Space Agency ESA to probe the universes evolution and geometry by surveying the position and gravitational shape distortion of billions of galaxies. These observations bear the potential to offer unprecedented measurements of the cosmological parameters thereby advancing our understanding of the cosmos. This work revolves around the central theme of quantifying the constraining power of the upcoming Euclid 3times2pt photometric survey accounting for several factors which have been neglected to this date in the official forecasts especially more subtle sources of uncertainty which need to be included in the forecast and data analysis due to the precision of the observations. First we include and study the impact of supersample covariance a source of sample variance coming from the incomplete sampling of the density and shear field Fourier modes caused by the limited survey volume. Second we examine the effect of scale cuts translating them from Fourier to harmonic space through the use of the BNT transform which offers an efficient way of separating angular scales for the cosmic shear signal. This analysis allows quantifying and mitigating the bias coming from the uncertainty on our modelling of small scales. These updated forecasts validated against the reference Euclid ones provide insights into the expected precision achieved on the cosmological and nuisance parameters for a variety of survey settings and for the inclusion of different realistic systematics such as multiplicative shear bias magnification bias uncertainty in the mean of the redshift distribution and so on. | 2024-09-01T00:00:00Z | ['2024arXiv240907185S', 'arXiv:2409.07185', '10.48550/arXiv.2409.07185'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Deriving Cosmological Parameters from the Euclid mission | 2,024 | 418 | 0.45 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07185.pdf |
2024arXiv240904625H | Investigating the metal enrichment in the early universe helps us constrain theories about the first stars and study the ages of galaxies. The lensed galaxy MACS0647JD at z10.17 is the brightest galaxy known at z gt 10. Previous work analyzing JWST NIRSpec and MIRI data yielded a direct metallicity rm12logOH7.79pm0.09 sim 0.13 Zodot and electron density rmlogne rmcm3 2.9 pm 0.5 the most distant such measurements to date. Here we estimate the direct CO abundance for the first time at z gt 10 finding a subsolar rm logCO0.440.060.07. This is higher than other zgt6 galaxies with direct CO measurements likely due to higher metallicity. It is also slightly higher than galaxies in the local universe with similar metallicity. This may suggest a very efficient and rapid burst of star formation a low effective oxygen abundance yield or the presence of unusual stellar populations including supermassive stars. Alternatively the strong CIIIrm lambdalambda19071909 emission 14pm 3 restframe EW may originate from just one of the two component star clusters JDB r sim 20 pc. Future NIRSpec IFU spectroscopic observations of MACS0647JD will be promising for disentangling CO in the two components to constrain the chemistry of individual star clusters just 460 Myr after the Big Bang. | 2024-09-01T00:00:00Z | ['arXiv:2409.04625', '2024arXiv240904625H', '10.48550/arXiv.2409.04625'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | First direct carbon abundance measured at zgt10 in the lensed galaxy MACS0647JD | 2,024 | 419 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.04625.pdf |
2024arXiv240906697L | Superpuffs are lowdensity planets of unknown origin and composition. If they form by accreting nebular gas through a circumplanetary disk one might expect superpuffs to be spinning quickly. Here we derive upper limits on the rotational oblateness of the superpuff Kepler51d based on precise transit observations with the NIRSpec instrument aboard the James Webb Space Telescope. The absence of detectable oblatenessrelated anomalies in the light curve leads to an upper limit of about 0.15 on the planets skyprojected oblateness. Assuming the skyprojected oblateness to be representative of the true oblateness the rotation period of Kepler51d is gtrsim 40 hours or equivalently its rotation speed is lesssim 42 of the breakup speed. Alternatively if the apparently low density of Kepler51d is due to an opaque planetary ring the ring must be oriented within 30 of faceon and have an inner radius smaller than 1.2 times the planets radius. Separately the lack of anomalies exceeding 0.01 in the ingress and egress portions of the light curve places a constraint on the model of Wang amp Dai in which the planets apparently low density is due to a dusty outflowing atmosphere. | 2024-09-01T00:00:00Z | ['2024arXiv240906697L', 'arXiv:2409.06697', '10.48550/arXiv.2409.06697'] | ['Astrophysics - Earth and Planetary Astrophysics'] | Slow Rotation for the SuperPuff Planet Kepler51d | 2,024 | 420 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.06697.pdf |
2024arXiv240908322B | We demonstrate a new technique to search for dark compact objects. When dark matter comprising a dark compact object interacts with photons the compact object can disperse light traveling though it. As these objects pass between the Earth and a distant star they act as lampshades that dim the star. We examine how dimming effects from clumps of dark matter in the galaxy could be searched for in microlensing surveys which measure the brightness of stars as a function of time. Using the EROS2 and OGLE surveys we show that a dimming analysis of existing data can be used to constrain dark sectors and could be used to discover dark matter in compact objects. | 2024-09-01T00:00:00Z | ['arXiv:2409.08322', '2024arXiv240908322B', '10.48550/arXiv.2409.08322'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Illuminating dark objects with dark matter lampshades | 2,024 | 420 | 0.39 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.08322.pdf |
2024arXiv240911457S | We explore the physical properties of five massive quiescent galaxies at zsim2.5 revealing the presence of nonnegligible dust reservoirs. JWST NIRSpec observations were obtained for each target finding no significant line emission multiple star formation tracers independently place upper limits between 0.110Modot mathrmyr. Spectral energy distribution modeling with Prospector infers stellar masses between log10M Modot sim 1011 and stellar massweighted ages between 12 Gyr. The inferred massweighted effective radii reffsim 0.41.4 kpc and inner 1 kpc stellar surface densities log10Sigma Modot mathrmkpc2 gtrsim 9 are typical of quiescent galaxies at z gtrsim 2. The galaxies display negative color gradients redder core and bluer outskirts for one galaxy this effect results from a dusty core while for the others it may be evidence of an insideout growth process. Unlike local quiescent galaxies we identify significant reddening in these typical cosmic noon passive galaxies all but one require AV gtrsim 0.4. This finding is in qualitative agreement with previous studies but our deep 20band NIRCam imaging is able to significantly suppress the dustage degeneracy and confidently determine that these galaxies are reddened. We speculate about the physical effects that may drive the decline in dust content in quiescent galaxies over cosmic time. | 2024-09-01T00:00:00Z | ['arXiv:2409.11457', '10.48550/arXiv.2409.11457', '2024arXiv240911457S'] | ['Astrophysics - Astrophysics of Galaxies'] | UNCOVER Significant Reddening in Cosmic Noon Quiescent Galaxies | 2,024 | 424 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.11457.pdf |
2024arXiv240907298J | On the 29th of May 2023 the LIGOVirgoKAGRA Collaboration observed a compact binary coalescence event consistent with a neutron starblack hole merger though the heavier object of mass 2.54.5 Modot would fall into the purported lower mass gap. An alternative explanation for apparent observations of events in this mass range has been suggested as strongly gravitationally lensed binary neutron stars. In this scenario magnification would lead to the source appearing closer and heavier than it really is. Here we investigate the chances and possible consequences for the GW230529 event to be gravitationally lensed. We find this would require high magnifications and we obtain low rates for observing such an event with a relative fraction of lensed versus unlensed observed events of 2 times 103 at most. When comparing the lensed and unlensed hypotheses accounting for the latest rates and population model we find a 158 chance of lensing disfavoring this option. Moreover when the magnification is assumed to be strong enough to bring the mass of the heavier binary component below the standard limits on neutron star masses we find high probability for the lighter object to have a subsolar mass making the binary even more exotic than a massgap neutron starblack hole system. Even when the secondary is not subsolar its tidal deformability would likely be measurable which is not the case for GW230529. Finally we do not find evidence for extra lensing signatures such as the arrival of additional lensed images typeII image dephasing or microlensing. Therefore we conclude it is unlikely for GW230529 to be a strongly gravitationally lensed binary neutron star signal. | 2024-09-01T00:00:00Z | ['2024arXiv240907298J', '10.48550/arXiv.2409.07298', 'arXiv:2409.07298'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - High Energy Astrophysical Phenomena'] | What is the nature of GW230529 An exploration of the gravitational lensing hypothesis | 2,024 | 425 | 0.51 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.07298.pdf |
2024arXiv240913047L | A multitude of JWST studies reveal a surprising overabundance of overmassive accreting supermassive blackholes SMBHs leading to a deepening tension between theory and observation in the first billion years of cosmic time. Across Xray to infrared wavelengths models built off of preJWST predictions fail to easily reproduce observed AGN signatures or lack thereof driving uncertainty around the true nature of these sources. Using a sample of JWST AGN identified via their broadened Halpha emission and covered by the deepest Xray surveys we find neither any measurable Xray emission nor any detection of highionization emission lines frequently associated with accreting SMBHs. We propose that these sources are accreting at or beyond the Eddington limit which reduces the need for efficient production of heavy SMBH seeds at cosmic dawn. Using a theoretical model of superEddington accretion we can produce the observed relative dearth of both Xray and ultraviolet emission as well as the high Balmer decrements without the need for significant dust attenuation. This work indicates that superEddington accretion is easily achieved throughout the early Universe and further study is required to determine what environments are required to trigger this mode of black hole growth. | 2024-09-01T00:00:00Z | ['2024arXiv240913047L', '10.48550/arXiv.2409.13047', 'arXiv:2409.13047'] | ['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Astrophysics of Galaxies'] | The Case for SuperEddington Accretion Connecting Weak Xray and UV Line Emission in JWST BroadLine AGN During the First Gyr of Cosmic Time | 2,024 | 425 | 0.65 | ['EPRINT_HTML', 'EPRINT_PDF'] | 10 | https://arxiv.org/pdf/2409.13047.pdf |
2024arXiv240910514G | The resonant conversion of cosmic microwave background CMB photons into axions within largescale structure induces an anisotropic spectral distortion in CMB temperature maps. Applying stateoftheart foreground cleaning techniques to textitPlanck CMB observations we construct maps of axioninduced patchy screening of the CMB. We crosscorrelate these maps with data from the textitunWISE galaxy survey and find no evidence of axions. We constrain the axionphoton coupling gagammagamma lesssim 2 times 1012rm GeV1 at the 95 confidence level for axion masses in the range 1013rm eV lesssim ma lesssim 1012rm eV. These constraints are competitive with the tightest astrophysical axion limits in this mass range and are inferred from robust populationlevel statistics which makes them complementary to existing searches that rely on modeling of individual systems. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.10514', 'arXiv:2409.10514', '2024arXiv240910514G'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Constraints on axions from patchy screening of the cosmic microwave background | 2,024 | 431 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.10514.pdf |
2024arXiv240904529W | Our understanding of the assembly timeline of the Milky Way has been transforming along with the dramatic increase in astrometric and spectroscopic data available over the past several years. Many substructures in chemodynamical space have been discovered and identified as the remnants of various galactic mergers. To investigate the timeline of these mergers we select main sequence turn off amp subgiant stars MSTOs from the H3 survey finding members in seven metal poor components of the halo GSE the Helmi Streams Thamnos Sequoia WukongLMS1 Arjuna and Iitoi. We also select out the metal poor in situ disk to facilitate comparison to the evolution of the Milky Way itself at these early epochs. We fit individual isochrone ages to the MSTOs in each of these substructures and use the resulting age distributions to infer simple star formation histories. For GSE we resolve an extended star formation history that truncates approx10 Gyr ago as well as a clear age metallicity relation. From this age distribution and measured star formation history we infer that GSE merged with the Milky Way at a time 9.510.2 Gyr ago in agreement with previous estimates. We infer that the other mergers occurred at various times ranging from 913 Gyr ago and that the metal poor component of the disk built up within only a few billion years. These results reinforce the emerging picture that both the disk and halo of the Milky Way experienced a rapid assembly. | 2024-09-01T00:00:00Z | ['arXiv:2409.04529', '2024arXiv240904529W', '10.48550/arXiv.2409.04529'] | ['Astrophysics - Astrophysics of Galaxies'] | The Rapid Formation of the Metal Poor Milky Way | 2,024 | 432 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.04529.pdf |
2024Univ...10..367A | We present thought experiments to measure the ArnowittDeserMisner inlineformulammlmath idmm1mmlsemanticsmmlmsubmmlmiEmmlmimmlmiADMmmlmimmlmsubmmlsemanticsmmlmathinlineformula and BondiSachs energy inlineformulammlmath idmm2mmlsemanticsmmlmsubmmlmiEmmlmimmlmiBSmmlmimmlmsubmmlsemanticsmmlmathinlineformula of isolated systems in general relativity. The expression of inlineformulammlmath idmm3mmlsemanticsmmlmsubmmlmiEmmlmimmlmiBSmmlmimmlmsubmmlsemanticsmmlmathinlineformula used in the protocol is likely to have other applications. In particular it is wellsuited to be promoted to an operator in nonperturbative loop quantum gravity. | 2024-09-01T00:00:00Z | ['10.3390/universe10090367', '10.48550/arXiv.2409.06698', 'arXiv:2409.06698', '2024arXiv240906698A', '2024Univ...10..367A'] | ['isolated gravitating systems', 'asymptotic flatness', 'observables', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Theory', 'Mathematical Physics'] | The Operational Meaning of Total Energy of Isolated Systems in General Relativity | 2,024 | 432 | 0.22 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 0 | https://arxiv.org/pdf/2409.06698.pdf |
2024A&A...689A.324B | We present a detailed study of the gas and galaxy properties of the cluster PSZ2 G282.2849.94 detected in the Planck allsky survey. The intracluster medium ICM of this object at z0.56 exhibits a cometarylike shape. Combining Chandra and TNG observations we characterised the spatially resolved thermodynamical properties of the gas and the spatial and velocity distribution of 73 galaxy members. The cluster structure is quite complex with an elongated core region containing the two brightest cluster galaxies and one dense group to the southeast. Since there is no velocity difference between the core and the southeast group we suggest the presence of a merger along the plane of the sky. This structure is related to complex Xray and radio features and thus the merger has likely been caught during the postmerger phase. Comparing the distribution of the ICM and of member galaxies we find a large offset of 350 kpc between the position of the Xray peak and the centre of a concentration of galaxies preceding it in the likely direction of motion. This configuration is similar to the famous Bullet Cluster leading us to dub PSZ2 G282.2849.94 the Planck bullet and represents an ideal situation to provide astrophysical constraints to the selfinteraction crosssection m of dark matter particles. These results illustrate the power of a multiwavelength approach to probe the merging scenario of such complex and distant systems. | 2024-09-01T00:00:00Z | ['2024arXiv240907290B', '10.48550/arXiv.2409.07290', '2024A&A...689A.324B', 'arXiv:2409.07290', '10.1051/0004-6361/202450468'] | ['galaxies: clusters: intracluster medium', 'galaxies: distances and redshifts', 'dark matter', 'galaxies: clusters: individual: PSZ2 G282.28+49.94', 'large-scale structure of Universe', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | PSZ2 G282.2849.94 a recently discovered analogue of the famous Bullet Cluster | 2,024 | 433 | 0.57 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.07290.pdf |
2024A&A...691A.114M | We analyzed Multi Unit Spectroscopic Explorer observations of 42 local z 0.1 type 1 active galactic nucleus AGN host galaxies taken from the PalomarGreen quasar sample and the close AGN reference survey. Our goal was to study the relation between the black hole mass MSUBSUB and bulge stellar velocity dispersion SUBeSUB for type 1 active galaxies. The sample spans black hole masses of 10SUP6.0SUP 10SUP9.2SUP MSUBSUB bolometric luminosities of 10SUP42.9SUP 10SUP46.0SUP erg sSUP1SUP and Eddington ratios of 0.006 1.2. We avoided AGN emission by extracting the spectra over annular apertures. We modeled the calcium triplet stellar features and measured stellar velocity dispersions of SUBSUB 60 230 km sSUP1SUP for the host galaxies. We find stellar velocity dispersion values in agreement with previous measurements for local z 0.1 AGN host galaxies but slightly lower compared with those reported for nearby Xrayselected type 2 quasars. Using a novel annular aperture correction recipe to estimate SUBeSUB from SUBSUB that considers the bulge morphology and observation beamsmearing we estimate fluxweighted SUBeSUB 60 250 km sSUP1SUP. If we consider the bulge type when estimating MSUBSUB we find no statistical difference between the distributions of AGN hosts and the inactive galaxies on the MSUBSUBSUBeSUB plane for MSUBSUB 10SUP8SUP MSUBSUB. Conversely if we do not consider the bulge type when computing MSUBSUB we find that both distributions disagree. We find no correlation between the degree of offset from the MSUBSUBSUBeSUB relation and Eddington ratio for MSUBSUB 10SUP8SUP MSUBSUB. The current statistics preclude firm conclusions from being drawn for the highmass range. We argue these observations support notions that a significant fraction of the local type 1 AGNs and quasars have undermassive black holes compared with their host galaxy bulge properties. | 2024-11-01T00:00:00Z | ['10.1051/0004-6361/202348353', 'arXiv:2409.08893', '10.48550/arXiv.2409.08893', '2024A&A...691A.114M', '2024arXiv240908893M'] | ['galaxies: active', 'Astrophysics - Astrophysics of Galaxies'] | The MSUBSUBSUBeSUB relation for local type 1 AGNs and quasars | 2,024 | 433 | 0.58 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 1 | https://arxiv.org/pdf/2409.08893.pdf |
2024arXiv240907643B | We study the thermodynamics of Einstein gravity with vanishing cosmological constant subjected to conformal boundary conditions. Our focus is on comparing the series of subextensive terms to predictions from thermal effective field theory with which we find agreement for the boundary theory on a spatial sphere hyperbolic space and flat space. We calculate the leading Wilson coefficients and observe that the first subextensive correction to the free energy is negative. This violates a conjectured bound on this coefficient in quantum field theory which we interpret as a signal that gravity does not fully decouple in the putative boundary dual. | 2024-09-01T00:00:00Z | ['2024arXiv240907643B', 'arXiv:2409.07643', '10.48550/arXiv.2409.07643'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology'] | Flat space gravity at finite cutoff | 2,024 | 438 | 0.19 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.07643.pdf |
2024arXiv240912232T | JWST has revealed diverse new populations of highredshift zsim411 AGN and extreme starforming galaxies that challenge current models. In this paper we use restframe UV emissionline diagnostics to identify AGN candidates and other exceptional ionizing sources complementing previous studies predominantly focused on broadline AGN. In this paper we use restframe UV emissionline diagnostics to identify AGN candidates and other exceptional ionizing sources complementing previous studies predominantly focused on broadline AGN. From a parent sample of 205 mathrmzspecgt3 UNCOVER galaxies with NIRSpecPRISM followup we identify 12 C IV He II and C III emitters. Leveraging the combined restoptical and UV coverage of PRISM we limit the emissionline model space using the samples O IIIHbeta distribution significantly decreasing the overlap between AGN and starformation models in the UV diagnostics. We then find that the five He II emitters are the strongest AGN candidates with further support from two Ne V detections and one Xray detection from Chandra. We cannot robustly quantify the AGN fraction in this sample but we note that close to 20 of mathrmMgt2times109Modot parent sample galaxies are AGN candidates. The lowermass line emitters which are consistent with both AGN and starforming photoionization models have more compact sizes and higher specific star formation rates than the parent sample. Higherresolution and deeper data on these UV line emitters should provide much stronger constraints on the obscured AGN fraction at z gt 3. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.12232', 'arXiv:2409.12232', '2024arXiv240912232T'] | ['Astrophysics - Astrophysics of Galaxies'] | UNCOVERing the HighRedshift AGN Population Among Extreme UV Line Emitters | 2,024 | 438 | 0.62 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.12232.pdf |
2024arXiv240905140Z | We present new Galactic reddening maps of the high Galactic latitude sky using DESI imaging and spectroscopy. We directly measure the reddening of 2.6 million stars by comparing the observed stellar colors in gr and rz from DESI imaging with the synthetic colors derived from DESI spectra from the first two years of the survey. The reddening in the two colors is on average consistent with the citefitzpatrickcorrecting1999 extinction curve with RmathrmV3.1. We find that our reddening maps differ significantly from the commonly used citeschlegelmaps1998 SFD reddening map by up to 80 mmag in EBV and we attribute most of this difference to systematic errors in the SFD map. To validate the reddening map we select a galaxy sample with extinction correction based on our reddening map and this yields significantly better uniformity than the SFD extinction correction. Finally we discuss the potential systematic errors in the DESI reddening measurements including the photometric calibration errors that are the limiting factor on our accuracy. The Egr and Egr maps presented in this work and for convenience their corresponding EBV maps with SFD calibration are publicly available. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.05140', '2024arXiv240905140Z', 'arXiv:2409.05140'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Stellar reddening map from DESI imaging and spectroscopy | 2,024 | 441 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.05140.pdf |
2024ApJ...973L..41I | Recent midinfrared observations with JWSTs MidInfrared Instrument Low Resolution Spectrometer MIRI LRS have resulted in the first direct detections of absorption features from silicate clouds in the transmission spectra of two transiting exoplanets WASP17 b and WASP107 b. In this Letter we measure the midinfrared 512 m dayside emission spectrum of the benchmark hot Jupiter HD 189733 b with MIRI LRS by combining data from two secondaryeclipse observations. We confirm the previous detection of HSUB2SUBO absorption at 6.5 m from Spitzers Infrared Spectrograph IRS and additionally detect HSUB2SUBS as well as an absorption feature at 8.7 m in both secondaryeclipse observations. The excess absorption at 8.7 m can be explained by the presence of small 0.01 m grains of SiOSUB2SUBs in the uppermost layers of HD 189733 bs dayside atmosphere. This is the first direct detection of silicate clouds in HD 189733 bs atmosphere and the first detection of a distinct absorption feature from silicate clouds on the dayside of any hot Jupiter. We find that models including SiOSUB2SUBs are preferred by 67 over clear models and those with other potential cloud species. The highaltitude location of these silicate particles is best explained by formation in the hottest regions of HD 189733 bs dayside atmosphere near the substellar point. We additionally find that HD 189733 bs emission spectrum longward of 9 m displays residual features not well captured by our current atmospheric models. When combined with other JWST observations of HD 189733 bs transmission and emission spectra at shorter wavelengths these observations will provide us with the most detailed picture to date of the atmospheric composition and cloud properties of this benchmark hot Jupiter. | 2024-10-01T00:00:00Z | ['arXiv:2409.11395', '10.3847/2041-8213/ad725e', '10.48550/arXiv.2409.11395', '2024arXiv240911395I', '2024ApJ...973L..41I'] | ['Exoplanet atmospheres', 'Exoplanet atmospheric composition', 'Exoplanet astronomy', 'Hot Jupiters', '487', '2021', '486', '753', 'Astrophysics - Earth and Planetary Astrophysics'] | Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b | 2,024 | 444 | 0.64 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3 | https://arxiv.org/pdf/2409.11395.pdf |
2024NuPhB100816711O | The ratios mmlmath altimgsi1.svgmmlmsqrtmmlmrowmmlmn8mmlmnmmlmo stretchyfalsemmlmommlmn9mmlmnmmlmrowmmlmsqrtmmlmo linebreakgoodbreak linebreakstyleaftermmlmommlmn2mmlmnmmlmsqrtmmlmrowmmlmn2mmlmnmmlmrowmmlmsqrtmmlmo stretchyfalsemmlmommlmn3mmlmnmmlmommlmommlmn0.9428mmlmnmmlmath and mmlmath altimgsi2.svgmmlmsqrtmmlmrowmmlmn3mmlmnmmlmrowmmlmsqrtmmlmo stretchyfalsemmlmommlmn2mmlmnmmlmommlmommlmn0.866mmlmnmmlmath appear in various contexts of black hole physics as values of the chargetomass ratio mmlmath altimgsi161.svgmmlmiQmmlmimmlmo stretchyfalsemmlmommlmiMmmlmimmlmath or the rotation parameter mmlmath altimgsi168.svgmmlmiammlmimmlmo stretchyfalsemmlmommlmiMmmlmimmlmath for ReissnerNordstrm and Kerr black holes respectively. In this work in the ReissnerNordstrm case I relate these ratios with the quantization of the horizon area or equivalently of the entropy. Furthermore these ratios are related to a centuryold work of Kasner in which he conjectured that certain sequences arising from complex analysis may have a quantum interpretation. These numbers also appear in the case of Kerr black holes but the explanation is not as straightforward. The Kasner ratio may also be relevant for understanding the random matrix and random graph approaches to black hole physics such as fast scrambling of quantum information via a bound related to Ramanujan graph. Intriguingly some other pure mathematical problems in complex analysis notably complex interpolation in the unit disk appear to share some mathematical expressions with the black hole problem and thus also involve the Kasner ratio. | 2024-11-01T00:00:00Z | ['2024NuPhB100816711O', 'arXiv:2409.08236', '10.1016/j.nuclphysb.2024.116711', '2024arXiv240908236O', '10.48550/arXiv.2409.08236'] | ['General Relativity and Quantum Cosmology', 'High Energy Physics - Theory', 'Mathematics - Complex Variables'] | Black holes complex curves and graph theory Revising a conjecture by Kasner | 2,024 | 446 | 0.28 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 1 | https://arxiv.org/pdf/2409.08236.pdf |
2024ApJ...976...70L | Using a combination of Hubble Space Telescope HST JWST and Atacama Large Millimetersubmillimeter Array ALMA data we perform spatially resolved spectral energy distributions SED fitting of fourteen 4 lt z lt 6 ultraviolet UVselected mainsequence galaxies targeted by the ALMA Large Program C II Resolved ISM in Starforming Galaxies. We consistently model the emission from stars and dust in 0.51 kpc spatial bins to obtain maps of their physical properties. We find no offsets between the stellar masses M SUBSUB and star formation rates SFRs derived from their global emission and those from adding up the values in our spatial bins suggesting there is no bias of outshining by young stars on the derived global properties. We show that ALMA observations are important to derive robust parameter maps because they reduce the uncertainties in L SUBdustSUB hence ASUBVSUB and SFR. Using these maps we explore the resolved starforming main sequence for z 5 galaxies finding that this relation persists in typical starforming galaxies in the early Universe. We find less obscured star formation where the M SUBSUB and SFR surface densities are highest typically in the central regions contrary to the global relation between these parameters. We speculate this could be caused by feedback driving gas and dust out of these regions. However more observations of IR luminosities with ALMA are needed to verify this. Finally we test empirical SFR prescriptions based on the UVIR and C II line luminosity finding they work well at the scales probed approximately kiloparsec. Our work demonstrates the usefulness of joint HST JWST and ALMAresolved SED modeling analyses at high redshift. | 2024-11-01T00:00:00Z | ['arXiv:2409.10961', '2024arXiv240910961L', '10.3847/1538-4357/ad7fee', '2024ApJ...976...70L', '10.48550/arXiv.2409.10961'] | ['Galaxies', 'High-redshift galaxies', 'Galaxy evolution', 'Galaxy stellar content', 'Interstellar medium', 'Star formation', '573', '734', '594', '621', '847', '1569', 'Astrophysics - Astrophysics of Galaxies'] | The ALMACRISTAL Survey Spatially Resolved Star Formation Activity and Dust Content in 4 lt z lt 6 Starforming Galaxies | 2,024 | 450 | 0.63 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 4 | https://arxiv.org/pdf/2409.10961.pdf |
2024A&A...690A.357L | Motivated by the observed 30 variations in flux from the L7 dwarf VHS 1256 b we subjected its timeresolved Hubble Space Telescope HST WFC3 spectra measured in two epochs 2018 and 2020 as well as mediumresolution Very Large Telescope VLT Xshooter and Early Release Science James Webb Space Telescope JWST spectra to a suite of both standard Bayesian nested sampling and machinelearning random forest retrievals. We find that both HST and VLT data require vertically varying abundance profiles of water in order to model the spectra accurately. Despite the large flux variations observed in the HST data the temporal variability cannot be attributed to a single varying atmospheric property. The retrieved atmospheric quantities are consistent with being invariant across time. However we find that model grids offer relatively poor fits to the measured HST spectra and are unsuitable for quantifying the temporal variability of atmospheric properties. Additionally our analysis of JWST spectra using model grids indicates consistency in terms of the retrieved properties across different wavelength channels. Despite the temporal variability in flux the retrieved properties between HST and VLT as well those as between HST and JWST are consistent within the respective posterior uncertainties. Such an outcome bodes well for future retrieval analyses of exoplanetary atmospheres which are expected to exhibit weaker flux variations. | 2024-10-01T00:00:00Z | ['2024A&A...690A.357L', '2024arXiv240908254L', 'arXiv:2409.08254', '10.1051/0004-6361/202451301', '10.48550/arXiv.2409.08254'] | ['techniques: spectroscopic', 'planets and satellites: atmospheres', 'planets and satellites: composition', 'brown dwarfs', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics'] | Retrieved atmospheric properties of the substellar object VHS 1256 b with HST VLT and JWST spectra | 2,024 | 450 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.08254.pdf |
2024arXiv240911151S | Impacts by rocky and icy bodies are thought to have played a key role in shaping the composition of solar system objects including the Earths habitability. Hence it is likely that they play a similar role in exoplanetary systems. We investigate how an icy cometary impact affects the atmospheric chemistry climate and composition of an Earthlike tidallylocked terrestrial exoplanet a prime target in the search for a habitable exoplanet beyond our solar system. We couple a cometary impact model which includes thermal ablation and pressure driven breakup with the 3D Earth System Model WACCM6CESM2 and use this model to investigate the effects of the water and thermal energy delivery associated with an R2.5 km pure water ice cometary impact on an Earthlike atmosphere. We find that water is the primary driver of longer timescale changes to the atmospheric chemistry and composition by acting as a source of opacity cloud ice and atmospheric hydrogenoxygen. The water opacity drives heating at sim5times104 bar and cooling below due to a decreased flux reaching the surface. The increase in atmospheric hydrogen and oxygen also drives an increase in the abundance of hydrogenoxygen rich molecules with the exception of ozone whose column density decreases by sim10. These atmospheric changes are potentially observable for sim 12 years postimpact particularly those associated with cloud ice scattering. They also persist albeit at a much reduced level to our quasisteadystate suggesting that sustained bombardment or multiple large impacts have the potential to shape the composition and habitability of terrestrial exoplanets. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.11151', 'arXiv:2409.11151', '2024arXiv240911151S'] | ['Astrophysics - Earth and Planetary Astrophysics'] | The Response of Planetary Atmospheres to the Impact of Icy Comets I TidallyLocked exoEarths | 2,024 | 452 | 0.47 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.11151.pdf |
2024arXiv240904545A | Theories of dynamical electroweak symmetry breaking predict a strong first order cosmological phase transition we compute the resulting signals primordial black holes and gravitational waves. These theories employ one SMneutral scalar plus some extra modeldependent particle to get the desired quantum potential out of classical scale invariance. We consider models where the extra particle is a scalar singlet or vectors of an extended U1 or SU2 gauge sector. In models where the extra particle is stable it provides a particle Dark Matter candidate with freezeout abundance that tends to dominate over primordial black holes. These can instead be DM in models without a particle DM candidate. Gravitational waves arise at a level observable in future searches even in regions where DM cannot be directly tested. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.04545', '2024arXiv240904545A', 'arXiv:2409.04545'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Gravitational waves and black holes from the phase transition in models of dynamical symmetry breaking | 2,024 | 452 | 0.32 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.04545.pdf |
2024A&A...691A.145M | Spectroscopy with the James Webb Space Telescope has opened the possibility of identifying moderateluminosity active galactic nuclei AGNs in the early Universe at and beyond the epoch of reionisation complementing previous surveys of much more luminous and much rarer quasars. We present 12 new AGNs at 4 lt z lt 7 in the JADES survey in addition to the previously identified AGN in GNz11 at z 10.6 revealed through the detection of a broadline region BLR seen in the Balmer emission lines. The depth of JADES together with the use of three different spectral resolutions enables us to probe a lowermass regime relative to previous studies. In a few cases we find evidence for two broad components of H which suggests that these could be candidate merging black holes BHs although a complex BLR geometry cannot be excluded. The inferred BH masses range from 8 10SUP7SUP MSUBSUB down to 4 10SUP5SUP MSUBSUB interestingly probing the regime expected for direct collapse BHs. The inferred AGN bolometric luminosities 10SUP44SUP 10SUP45SUP ergs imply accretion rates that are lt 0.5 times the Eddington rate in most cases. However small BHs with MSUBBHSUB 10SUP6SUP MSUBSUB tend to accrete at Eddington or superEddington rates. These BHs at z 411 are overmassive relative to their host galaxies stellar masses when compared to the local MSUBBHSUB MSUBstarSUB relation even approaching MSUBBHSUB MSUBstarSUB as was expected from heavy BH seeds andor superEddington accretion scenarios. However we find that these early BHs tend to be more consistent with the local relation between MSUBBHSUB and velocity dispersion as well as between MSUBBHSUB and dynamical mass suggesting that these are more fundamental and universal relations. On the classical optical narrowline excitationdiagnostic diagrams these AGNs are located in the region that is locally occupied by starforming galaxies implying that they would be missed by the standard classification techniques if they did not display broad lines. Their location on the diagram is consistent with what is expected for AGNs hosted in metalpoor galaxies Z 0.1 0.2 ZSUBSUB. The fraction of broadline AGNs with LSUBAGNSUB gt 10SUP44SUP ergs among galaxies in the redshift range of 4 lt z lt 6 is about 10 suggesting that the contribution of AGNs and their hosts to the reionisation of the Universe is gt 10. | 2024-11-01T00:00:00Z | ['10.1051/0004-6361/202347640', '10.48550/arXiv.2308.01230', '2023arXiv230801230M', 'arXiv:2308.01230', '2024A&A...691A.145M'] | ['galaxies: active', 'galaxies: formation', 'galaxies: high-redshift', 'galaxies: nuclei', 'quasars: supermassive black holes', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena'] | JADES The diverse population of infant black holes at 4 lt z lt 11 Merging tiny poor but mighty | 2,024 | 453 | 0.75 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 280 | https://arxiv.org/pdf/2308.01230.pdf |
2024arXiv240909540Y | Our Solar System includes the Sun eight major planets and their moons along with numerous asteroids comets and dust particles collectively known as the small Solar System bodies. Small bodies are relics from the birth of the Solar System and offer valuable insights into planetary formation and the origins of life. This chapter explores this important component of our Solar System discussing the formation and evolution of key small body populations and their interrelations. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.09540', '2024arXiv240909540Y', 'arXiv:2409.09540'] | ['Astrophysics - Earth and Planetary Astrophysics'] | Minor planets asteroids comets and interplanetary dust within 30 au | 2,024 | 454 | 0.46 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.09540.pdf |
2024OJAp....7E..63C | Despite originating in science fiction warp drives have a concrete description in general relativity with Alcubierre first proposing a spacetime metric that supported fasterthanlight travel. Whilst there are numerous practical barriers to their implementation in real life including a requirement for negative energy computationally one can simulate their evolution in time given an equation of state describing the matter. In this work we study the signatures arising from a warp drive containment failure assuming a stiff equation of state for the fluid. We compute the emitted gravitationalwave signal and track the energy fluxes of the fluid. Apart from its rather speculative application to the search for extraterrestrial life in gravitationalwave detector data this work is interesting as a study of the dynamical evolution and stability of spacetimes that violate the null energy condition. Our work highlights the importance of exploring strange new spacetimes to boldly simulate what no one has seen before. | 2024-07-01T00:00:00Z | ['arXiv:2406.02466', '10.48550/arXiv.2406.02466', '2024arXiv240602466C', '10.33232/001c.121868', '2024OJAp....7E..63C'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - High Energy Astrophysical Phenomena'] | What no one has seen before gravitational waveforms from warp drive collapse | 2,024 | 456 | 0.45 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 0 | https://arxiv.org/pdf/2406.02466.pdf |
2024A&A...691A.162G | This study analyses JWST MIRIMRS observations of the infrared IR polycyclic aromatic hydrocarbon PAH bands in the nuclear 0.4 at 11 m 75 pc and circumnuclear regions inner kpc of local active galactic nuclei AGNs from the Galactic Activity Torus and Outflow Survey GATOS. We examine the PAH properties in the circumnuclear regions of AGNs and the projected direction of AGNoutflows and compare them to those in starforming regions and the innermost regions of AGNs. This study employs 4.928.1 m subarcsecond angular resolution data to investigate the properties of PAHs in three nearby sources DSUBLSUB 30 40 Mpc. Our findings are aligned with previous JWST studies demonstrating that the central regions of AGNs display a larger fraction of neutral PAH molecules i.e. elevated 11.36.2 and 11.37.7 m PAH ratios in comparison to starforming galaxies. We find that AGNs might affect not only the PAH population in the innermost region but also in the extended regions up to kpc scales. By comparing our observations to PAH diagnostic diagrams we find that in general regions located in the projected direction of the AGNoutflow occupy similar positions on the PAH diagnostic diagrams as those of the innermost regions of AGNs. Starforming regions that are not affected by the AGNs in these galaxies share the same part of the diagram as starforming galaxies. We also examined the potential of the PAHHSUB2SUB diagram to disentangle AGNversusstarforming activity. Our results suggest that in Seyfertlike AGNs the illumination and feedback from the AGN might affect the PAH population at nuclear and kpc scales particularly with respect to the ionisation state of the PAH grains. However PAH molecular sizes are rather similar. The carriers of the ionised PAH bands 6.2 and 7.7 m are less resilient than those of neutral PAH bands 11.3 m which might be particularly important for strongly AGNhost coupled systems. Therefore caution must be applied when using PAH bands as starformation rate indicators in these systems even at kpc scales with the effects of the AGN being more important for ionised ones. | 2024-11-01T00:00:00Z | ['2024arXiv240905686G', '2024A&A...691A.162G', '10.1051/0004-6361/202450086', 'arXiv:2409.05686', '10.48550/arXiv.2409.05686'] | ['techniques: high angular resolution', 'techniques: spectroscopic', 'galaxies: active', 'galaxies: nuclei', 'galaxies: Seyfert', 'infrared: galaxies', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | The Galaxy Activity Torus and Outflow Survey GATOS V. Unveiling PAH survival and resilience in the circumnuclear regions of AGNs with JWST | 2,024 | 463 | 0.66 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 5 | https://arxiv.org/pdf/2409.05686.pdf |
2024arXiv240906405J | Lyalpha is the transition to the ground state from the first excited state of hydrogen the most common element. Resonant scattering of this line by neutral hydrogen greatly impedes its emergence from galaxies so the fraction of galaxies emitting Lyalpha is a tracer of the neutral fraction of the intergalactic medium IGM and thus the history of reionisation. In previous works we used early JWSTNIRSpec data from the JWST Advanced Deep Extragalactic Survey JADES to classify and characterise Lyalpha emitting galaxies LAEs. This survey is approaching completion and the current sample is nearly an order of magnitude larger. From a sample of 795 galaxies in JADES at 4.0ltzlt14.3 we find evidence for Lyalpha emission in 150sources. We reproduce the previously found correlation between Lyalpha escape fraction fescLyalpha Lyalpha restframe equivalent width REWLyalpha and the negative correlation between Lyalpha velocity offset fescLyalpha. Both fescLyalpha and REWLyalpha decrease with redshift zgtrsim5.5 indicating the progression of reionisation on a population scale. Our data are used to demonstrate an increasing IGM transmission of Lyalpha from zsim146. We measure the completenesscorrected fraction of LAEs xlya from z49.5. An application of these xlya values to the results of previously utilised semianalytical models suggests a high neutral fraction at z7 XHIsim0.80.9. Using an updated fit to the intrinsic distribution of REWLyalpha results in a lower value in agreement with current works XHI0.640.210.13. This sample of LAEs will be paramount for unbiased population studies of galaxies in the EoR. | 2024-09-01T00:00:00Z | ['arXiv:2409.06405', '2024arXiv240906405J', '10.48550/arXiv.2409.06405'] | ['Astrophysics - Astrophysics of Galaxies'] | JADES Measuring reionization properties using Lymanalpha emission | 2,024 | 464 | 0.63 | ['EPRINT_HTML', 'EPRINT_PDF'] | 10 | https://arxiv.org/pdf/2409.06405.pdf |
2024arXiv240907957L | Extrememassratio inspiral EMRI signals pose significant challenges in gravitational wave GW astronomy owing to their lowfrequency nature and highly complex waveforms which occupy a highdimensional parameter space with numerous variables. Given their extended inspiral timescales and low signaltonoise ratios EMRI signals warrant prolonged observation periods. Parameter estimation becomes particularly challenging due to nonlocal parameter degeneracies arising from multiple local maxima as well as flat regions and ridges inherent in the likelihood function. These factors lead to exceptionally high time complexity for parameter analysis while employing traditional matched filtering and random sampling methods. To address these challenges the present study applies machine learning to Bayesian posterior estimation of EMRI signals leveraging the recently developed flow matching technique based on ODE neural networks. Our approach demonstrates computational efficiency several orders of magnitude faster than the traditional Markov Chain Monte Carlo MCMC methods while preserving the unbiasedness of parameter estimation. We show that machine learning technology has the potential to efficiently handle the vast parameter space involving up to seventeen parameters associated with EMRI signals. Furthermore to our knowledge this is the first instance of applying machine learning specifically the Continuous Normalizing Flows CNFs to EMRI signal analysis. Our findings highlight the promising potential of machine learning in EMRI waveform analysis offering new perspectives for the advancement of spacebased GW detection and GW astronomy. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.07957', 'arXiv:2409.07957', '2024arXiv240907957L'] | ['Physics - Computational Physics', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'Computer Science - Artificial Intelligence'] | Rapid Parameter Estimation for Extreme Mass Ratio Inspirals Using Machine Learning | 2,024 | 464 | 0.48 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07957.pdf |
2024arXiv240911383L | Vision Based Navigation consists in utilizing cameras as precision sensors for GNC after extracting information from images. To enable the adoption of machine learning for space applications one of obstacles is the demonstration that available training datasets are adequate to validate the algorithms. The objective of the study is to generate datasets of images and metadata suitable for training machine learning algorithms. Two use cases were selected and a robust methodology was developed to validate the datasets including the ground truth. The first use case is inorbit rendezvous with a manmade object a mockup of satellite ENVISAT. The second use case is a Lunar landing scenario. Datasets were produced from archival datasets Change 3 from the laboratory at DLR TRON facility and at Airbus Robotic laboratory from SurRender software high fidelity image simulator using Model Capture and from Generative Adversarial Networks. The use case definition included the selection of algorithms as benchmark an AIbased pose estimation algorithm and a dense optical flow algorithm were selected. Eventually it is demonstrated that datasets produced with SurRender and selected laboratory facilities are adequate to train machine learning algorithms. | 2024-09-01T00:00:00Z | ['2024arXiv240911383L', '10.48550/arXiv.2409.11383', 'arXiv:2409.11383'] | ['Computer Science - Computer Vision and Pattern Recognition', 'Astrophysics - Earth and Planetary Astrophysics', 'Computer Science - Graphics', 'Computer Science - Machine Learning'] | Training Datasets Generation for Machine Learning Application to Vision Based Navigation | 2,024 | 465 | 0.34 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.11383.pdf |
2024arXiv240904543W | We present cogsworth an opensource Python tool for producing selfconsistent population synthesis and galactic dynamics simulations. With cogsworth one can 1 sample a population of binaries and star formation history 2 perform rapid binary stellar evolution 3 integrate orbits through the galaxy and 4 inspect the full evolutionary history of each star or compact object as well as their positions and kinematics. We include the functionality for postprocessing hydrodynamical zoomin simulations as a basis for galactic potentials and star formation histories to better account for initial spatial stellar clustering and more complex potentials. Alternatively several analytic models are available for both the potential and star formation history. cogsworth can transform the intrinsic simulated population to an observed population through the joint application of dust maps bolometric correction functions and survey selection functions. We provide a detailed explanation of the functionality of cogsworth and demonstrate its capabilities through a series of use cases 1 We predict the spatial distribution of compact objects and runaways in both dwarf and MilkyWaylike galaxies 2 using a star cluster from a hydrodynamical simulation we show how supernovae can change the orbits of stars in several ways and 3 we predict the separation of disrupted binary stellar companions on the sky and create a synthetic Gaia colourmagnitude diagram. We also discuss some current limitations and plans for future developments. We designed cogsworth and its online documentation to provide a powerful tool for constraining binary evolution but also a flexible and accessible resource for the entire community. | 2024-09-01T00:00:00Z | ['2024arXiv240904543W', '10.48550/arXiv.2409.04543', 'arXiv:2409.04543'] | ['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics'] | cogsworth A Gala of COSMIC proportions combining binary stellar evolution and galactic dynamics | 2,024 | 466 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.04543.pdf |
2024RNAAS...8..250G | We present NIFTYLS a software package for fast and accurate evaluation of the LombScargle periodogram. NIFTYLS leverages the fact that LombScargle can be computed using a nonuniform fast Fourier transform NUFFT which we evaluate with the Flatiron Institute NUFFT package FINUFFT. This approach achieves a manyfold speedup over the Press amp Rybicki method as implemented in ASTROPY and is simultaneously many orders of magnitude more accurate. NIFTYLS also supports fast evaluation on GPUs via CUDA and integrates with the ASTROPY LombScargle interface. NIFTYLS is publicly available at httpsgithub.comflatironinstituteniftyls. | 2024-10-01T00:00:00Z | ['10.48550/arXiv.2409.08090', 'arXiv:2409.08090', '2024RNAAS...8..250G', '2024arXiv240908090G', '10.3847/2515-5172/ad82cd'] | ['Astronomy software', 'Lomb-Scargle periodogram', 'GPU computing', '1855', '1959', '1969', 'Astrophysics - Instrumentation and Methods for Astrophysics'] | NIFTYLS Fast and Accurate LombScargle Periodograms Using a Nonuniform FFT | 2,024 | 468 | 0.47 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 0 | https://arxiv.org/pdf/2409.08090.pdf |
2024arXiv240910595P | Primordial gravitational waves could be nonGaussian just like primordial scalar perturbations. Although the tensor twopoint function has thusfar remained elusive the threepoint function could in principle be large enough to be detected in Cosmic Microwave Background temperature and polarization anisotropies. We perform a detailed analysis of tensor and mixed tensorscalar nonGaussianity through the Planck PR4 bispectrum placing constraints on eleven primordial templates spanning various phenomenological and physical regimes including modifications to gravity additional fields in inflation and primordial magnetic fields. All analysis is performed using modern quasioptimal binned estimators and yields no evidence for tensor nonGaussianity with a maximum detection significance of 1.8sigma. Our constraints are derived primarily from largescales except for tensorscalarscalar models and benefit greatly from the inclusion of Bmodes. Although we find some loss of information from binning mask effects and residual foreground contamination our frm NL bounds improve over those of previous analyses by 40600 with six of the eleven models being analyzed for the first time. Unlike for scalar nonGaussianity future lownoise experiments such as LiteBIRD the Simons Observatory and CMBS4 will yield considerable improvement in tensor nonGaussianity constraints. | 2024-09-01T00:00:00Z | ['2024arXiv240910595P', '10.48550/arXiv.2409.10595', 'arXiv:2409.10595'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Phenomenology', 'High Energy Physics - Theory'] | NonGaussianity Beyond the Scalar Sector A Search for Tensor and Mixed TensorScalar Bispectra with Planck Data | 2,024 | 468 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.10595.pdf |
2023ApJ...954..169T | Theory of the physics of the early hot universe leads to a prediction of baryon acoustic oscillations BAOs that has received confirmation from the pairwise separations of galaxies in samples of hundreds of thousands of objects. Evidence is presented here for the discovery of a remarkably strong individual contribution to the BAO signal at z 0.068 an entity that is given the name Hooleilana. The radius of the 3D structure is 155rmh751 Mpc. At its core is the Botes supercluster. The Sloan Great Wall Center for Astrophysics Great Wall and Hercules complex all lie within the BAO shell. The interpretation of Hooleilana as a BAO structure with our preferred analysis implies a value of the Hubble constant of 76.94.88.2mathrmkmrms1mathrmMpc1. | 2023-09-01T00:00:00Z | ['2023arXiv230900677T', '10.48550/arXiv.2309.00677', 'arXiv:2309.00677', '2023ApJ...954..169T', '10.3847/1538-4357/aceaf3'] | ['Large-scale structure of the universe', '902', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Hooleilana An Individual Baryon Acoustic Oscillation | 2,023 | 468 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 12 | https://arxiv.org/pdf/2309.00677.pdf |
2024arXiv240908971T | We constrain dark energy and modified gravity within the effective field theory of dark energy framework using the fullshape BOSS galaxy power spectrum combined with Planck cosmic microwave background CMB data and recent baryon acoustic oscillations BAO measurements from DESI. Specifically we focus on a varying braiding parameter alpharm B a running of the effective Planck mass alpharm M and a constant dark energy equation of state w. The analysis is performed with two of these parameters at a time including all the other standard cosmological parameters and marginalizing over bias and nuisance parameters. The fullshape galaxy power spectrum is modeled using the effective field theory of largescale structure up to 1loop order in perturbation theory. We find that the CMB data is most sensitive to alpharm B and that adding largescale structure information only slightly changes the parameter constraints. However the largescale structure data significantly improve the bounds on alpharm M and w by a factor of two. This improvement is driven by background information contained in the BAO which breaks the degeneracy with H0 in the CMB. We confirm this by comparing the BOSS fullshape information with BOSS BAO finding no significant differences. This is likely to change with future highprecision fullshape data from Euclid and DESI however to which the pipeline developed here is immediately applicable. | 2024-09-01T00:00:00Z | ['arXiv:2409.08971', '2024arXiv240908971T', '10.48550/arXiv.2409.08971'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Constraints on dark energy and modified gravity from the BOSS FullShape and DESI BAO data | 2,024 | 469 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.08971.pdf |
2024arXiv240907519G | Compact objects observed in gravitationalwave astronomy so far always come in pairs and never individually. Identifying the two components of a binary system is a delicate operation that is often taken for granted. The labeling procedure i.e. which is object 1 and which is object 2 effectively acts as systematics or equivalently an unspecified prior in gravitationalwave data inference. The common approach is to label the objects solely by their masses on a samplebysample basis while intuitive this leads to degeneracies when binaries have comparable masses. Instead we argue that object identification should be tackled using the posterior distribution as a whole. We frame the problem in terms of constrained clustering a flavor of semisupervised machine learning and find that unfolding the labeling systematics can significantly impact and arguably improve our interpretation of the data. In particular the precision of blackhole spin measurements improves by up to 50 spurious multimodalities and tails tend to disappear posteriors become closer to Gaussian distributions and the identification of the nature of the object i.e. black hole vs. neutron star is facilitated. We estimate that about 10 of the LIGOVirgo posterior samples are affected by this relabeling i.e. they might have been attributed to the wrong compact object in the observed binaries. | 2024-09-01T00:00:00Z | ['arXiv:2409.07519', '2024arXiv240907519G', '10.48550/arXiv.2409.07519'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - High Energy Astrophysical Phenomena'] | Which is which Identification of the two compact objects in gravitationalwave binaries | 2,024 | 471 | 0.47 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07519.pdf |
2024arXiv240804699R | NASAs return to the Moon presents unparalleled opportunities to advance highimpact scientific capabilities. At the cutting edge of these possibilities are extremely highresolution interferometric observations at visible and ultraviolet wavelengths. Such technology can resolve the surfaces of stars explore the inner accretion disks of nascent stars and black holes and eventually enable us to observe surface features and weather patterns on nearby exoplanets. We have been awarded Phase 1 support from NASAs Innovative Advanced Concepts NIAC program to explore the feasibility of constructing a highresolution longbaseline UVoptical imaging interferometer on the lunar surface in conjunction with the Artemis Program. A 1996 study comparing interferometers on the Moon versus freeflyers in space concluded that without preexisting lunar infrastructure freeflyers were preferable. However with the advent of the Artemis Program it is now crucial to revisit the potential of building lunar interferometers. Our objective is to conduct a study with the same level of rigor applied to large baseline freeflying interferometers during the 20032005 NASA Vision Missions Studies. This preparation is essential for timely and effective utilization of the forthcoming lunar infrastructure. In this paper we highlight the groundbreaking potential of a lunar surfacebased interferometer. This concept study will be a huge step forward to larger arrays on both the moon and freeflying in space over a wide variety of wavelengths and science topics. Our Phase 1 study began in April 2024 and here we present a concise overview of our vision and the progress made so far. | 2024-08-01T00:00:00Z | ['arXiv:2408.04699', '2024arXiv240804699R', '10.48550/arXiv.2408.04699'] | ['Astrophysics - Instrumentation and Methods for Astrophysics', 'Astrophysics - Earth and Planetary Astrophysics'] | Artemisenabled Stellar Imager AeSI A Lunar LongBaseline UVOptical Imaging Interferometer | 2,024 | 472 | 0.47 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2408.04699.pdf |
2024JAHH...27..482K | This article provides a firsthand account of the 1982 Arecibo observations that led to the discovery of PSR B193721 the firstknown millisecond pulsar. | 2024-09-01T00:00:00Z | ['arXiv:2409.07540', '10.48550/arXiv.2409.07540', '2024JAHH...27..482K', '10.3724/SP.J.1440-2807.2024.03.03', '2024arXiv240907540K'] | ['millisecond pulsars', '4C21.53', 'Arecibo Telescope', 'D.C. Backer', '2024JAHHvol27/2024JAHH...27..482K.pdf', 'Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Solar and Stellar Astrophysics'] | The discovery of the first millisecond pulsar Personal recollections | 2,024 | 472 | 0.52 | ['ADS_PDF', 'ADS_SCAN', 'EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.07540.pdf |
2024arXiv240906796S | Over the past two decades tight correlations between black hole masses Mbullet and their host galaxy properties have been firmly established for massive galaxies logMModotgtrsim10 at lowz zlt1 indicating coevolution of supermassive black holes and galaxies. However the situation at highz especially beyond cosmic noon zgtrsim2.5 is controversial. With a combination of emphJWST NIRCamwide field slitless spectroscopy WFSS from FRESCO CONGRESS and deep multiband NIRCamimage data from JADES in the GOODS fields we study the black hole to galaxy mass relation at zsim14. After identifying 18 broadline active galactic nuclei BL AGNs at 1ltzlt4 with 8 at zgt2.5 from the WFSS data we measure their black hole masses based on broad nearinfrared lines Pa alpha Pa beta and HeI lambda10833 and constrain their stellar masses M from AGNgalaxy image decomposition or SED decomposition. Taking account of the observational biases the intrinsic scatter of the MbulletM relation and the errors in mass measurements we find no significant difference in the MbulletM ratio for 2.5 lt z lt 4 compared to that at lower redshifts 1 lt z lt 2.5 suggesting no evolution of the Mbullet M relation at logMModotgtrsim10 up to zsim4. | 2024-09-01T00:00:00Z | ['2024arXiv240906796S', '10.48550/arXiv.2409.06796', 'arXiv:2409.06796'] | ['Astrophysics - Astrophysics of Galaxies'] | No evidence for a significant evolution of MbulletM relation in massive galaxies up to zsim4 | 2,024 | 472 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF'] | 5 | https://arxiv.org/pdf/2409.06796.pdf |
2024arXiv240908073A | Interpretation of data from faint dwarf galaxies is made challenging by observations limited to only the brightest stars. We present a major improvement to tackle this challenge by undertaking zoomed cosmological simulations that resolve the evolution of all individual stars more massive than 0.5rm Modot thereby explicitly tracking all observable stars for the Hubble time. For the first time we predict observable colormagnitude diagrams and the spatial distribution of approx 100000 stars within four faint Mstar approx 105 rm Modot dwarf galaxies directly from their cosmological initial conditions. In all cases simulations predict complex light profiles with multiple components implying that typical observational measures of structural parameters can make total Vband magnitudes appear up to 0.5 mag dimmer compared to estimates from simulations. Furthermore when only small lessapprox100 numbers of stars are observable shot noise from realizations of the colormagnitude diagram introduces uncertainties comparable to the population scatter in e.g. total magnitude halflight radius and mean iron abundance measurements. Estimating these uncertainties with fully selfconsistent mass growth star formation and chemical enrichment histories paves the way for more robust interpretation of dwarf galaxy data. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.08073', '2024arXiv240908073A', 'arXiv:2409.08073'] | ['Astrophysics - Astrophysics of Galaxies'] | EDGEINFERNO Simulating every observable star in faint dwarf galaxies and their consequences for resolvedstar photometric surveys | 2,024 | 473 | 0.6 | ['EPRINT_HTML', 'EPRINT_PDF'] | 6 | https://arxiv.org/pdf/2409.08073.pdf |
2024arXiv240906365K | Quantum evaporation of a black hole is conventionally studied semiclassically by assuming selfsimilarity of the black hole throughout the evaporation process. However its validity was recently questioned and the lifetime of a black hole is conjectured to be much extended by the memory burden effect. It gives rise to the possibility that the primordial black holes PBHs lighter than 1010 grams are the dark matter in the Universe. To probe such PBH dark matter we study gravitational waves GWs induced by primordial curvature perturbations that produced the PBHs. We find OmegatextGWftextpeakh2 7 times 109 with the peak frequency ftextpeak 1times 103 MtextPBH1010mathrmg12 mathrmHz and the induced GWs associated with the PBH dark matter whose initial mass is greater than about 107 grams can be tested by future observations such as Cosmic Explorer. Furthermore the scenario can be in principle confirmed by detecting another GW signal from the mergers of PBHs which leads to highfrequency GWs with ftextpeak 2 times 1027 MtextPBH ini1010 mathrmg1 mathrmHz . On the other hand the induced GW signals stronger than expected would contradict the dark matter abundance and exclude the memory burden effect. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.06365', '2024arXiv240906365K', 'arXiv:2409.06365'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology', 'High Energy Physics - Theory'] | Induced Gravitational Waves probing Primordial Black Hole Dark Matter with Memory Burden | 2,024 | 474 | 0.34 | ['EPRINT_HTML', 'EPRINT_PDF'] | 12 | https://arxiv.org/pdf/2409.06365.pdf |
2024arXiv240816903E | We present the framework for measuring angular power spectra in the Euclid mission. The observables in galaxy surveys such as galaxy clustering and cosmic shear are not continuous fields but discrete sets of data obtained only at the positions of galaxies. We show how to compute the angular power spectra of such discrete data sets without treating observations as maps of an underlying continuous field that is overlaid with a noise component. This formalism allows us to compute exact theoretical expectations for our measured spectra under a number of assumptions that we track explicitly. In particular we obtain exact expressions for the additive biases shot noise in angular galaxy clustering and cosmic shear. For efficient practical computations we introduce a spinweighted spherical convolution with a welldefined convolution theorem which allows us to apply exact theoretical predictions to finiteresolution maps including HEALPix. When validating our methodology we find that our measurements are biased by less than 1 of their statistical uncertainty in simulations of Euclids first data release. | 2024-08-01T00:00:00Z | ['2024arXiv240816903E', '10.48550/arXiv.2408.16903', 'arXiv:2408.16903'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics'] | Euclid preparation. LIX. Angular power spectra from discrete observations | 2,024 | 475 | 0.54 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2408.16903.pdf |
2024arXiv240911401P | We develop a transformerbased conditional generative model for discrete point objects and their properties. We use it to build a model for populating cosmological simulations with gravitationally collapsed structures called dark matter halos. Specifically we condition our model with dark matter distribution obtained from fast approximate simulations to recover the correct threedimensional positions and masses of individual halos. This leads to a first model that can recover the statistical properties of the halos at small scales to better than 3 level using an accelerated dark matter simulation. This trained model can then be applied to simulations with significantly larger volumes which would otherwise be computationally prohibitive with traditional simulations and also provides a crucial missing link in making endtoend differentiable cosmological simulations. The code named GOTHAM Generative cOnditional Transformer for Halos Autoregressive Modeling is publicly available at urlhttpsgithub.comshivampcosmoGOTHAM. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.11401', 'arXiv:2409.11401', '2024arXiv240911401P'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Instrumentation and Methods for Astrophysics'] | Teaching dark matter simulations to speak the halo language | 2,024 | 476 | 0.5 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.11401.pdf |
2024A&A...691A.147M | Context. The formation and evolution of protoplanetary disks remains elusive. We have numerous astronomical observations of young stellar objects of different ages with their envelopes andor disks. Moreover in the last decade there has been tremendous progress in numerical simulations of star and disk formation. New simulations use realistic equations of state for the gas and treat the interaction of matter and the magnetic field with the full set of nonideal magnetohydrodynamic MHD equations. However it is still not fully clear how a disk forms and whether it happens from insideout or outsidein. Open questions remain regarding where material is accreted onto the disk and comes from how dust evolves in disks and the timescales of appearance of disks structures. These unknowns limit our understanding of how planetesimals and planets form and evolve. Aims. We attempted to reconstruct the evolutionary history of the protosolar disk guided by the large amount of cosmochemical constraints derived from the study of meteorites while using astronomical observations and numerical simulations as a guide to pinpointing plausible scenarios. Methods. Our approach is highly interdisciplinary and we do not present new observations or simulations in this work. Instead we combine in an original manner a large number of published results concerning young stellar objects observations and numerical simulations along with the chemical isotopic and petrological nature of meteorites. Results. We have achieved a plausible and coherent view of the evolution of the protosolar disk that is consistent with cosmochemical constraints and compatible with observations of other protoplanetary disks and sophisticated numerical simulations. The evidence that hightemperature condensates namely calciumaluminum inclusions CAIs and amoeboid olivine aggregates AOAs formed near the protosun before being transported to the outer disk can be explained in two ways there could have either been an early phase of vigorous radial spreading of the disk that occurred or fast transport of these condensates from the vicinity of the protosun toward large disk radii via the protostellar outflow. The assumption that the material accreted toward the end of the infall phase was isotopically distinct allows us to explain the observed dichotomy in nucleosynthetic isotopic anomalies of meteorites. It leads us toward intriguing predictions on the possible isotopic composition of refractory elements in comets. At a later time when the infall of material waned the disk started to evolve as an accretion disk. Initially dust drifted inward shrinking the radius of the dust component to 45 au probably about to about half of the width of the gas component. Next structures must have emerged producing a series of pressure maxima in the disk which trapped the dust on Myr timescales. This allowed planetesimals to form at radically distinct times without significantly changing any of the isotopic properties. We also conclude that there was no late accretion of material onto the disk via streamers. The disk disappeared at about 5 My as indicated by paleomagnetic data in meteorites. Conclusions. The evolution of the protosolar disk seems to have been quite typical in terms of size lifetime and dust behavior. This suggests that the peculiarities of the Solar System with respect to extrasolar planetary systems probably originate from the chaotic nature of planet formation and not from the properties of the parental disk itself. | 2024-11-01T00:00:00Z | ['10.48550/arXiv.2409.06342', '10.1051/0004-6361/202451388', '2024arXiv240906342M', '2024A&A...691A.147M', 'arXiv:2409.06342'] | ['meteorites', 'meteors', 'meteoroids', 'protoplanetary disks', 'Astrophysics - Earth and Planetary Astrophysics', 'Astrophysics - Solar and Stellar Astrophysics'] | Formation and evolution of a protoplanetary disk Combining observations simulations and cosmochemical constraints | 2,024 | 477 | 0.65 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.06342.pdf |
2024MNRAS.534.2014W | We present an artificial neural network ANN model of photospheric lithium depletion in cool stars inlineformulatexmath idTM0001 notationLaTeX3000lt Trm effrm K lt 6500texmathinlineformula producing estimates and probability distributions of age from inlineformulatexmath idTM0002 notationLaTeX7texmathinlineformulaLi 6708 equivalent width LiEW and effective temperature data inputs. The model is trained on the same sample of 6200 stars from 52 open clusters observed in the GaiaESO spectroscopic survey and used to calibrate the previously published analytical EAGLES model with ages 26000 Myr and inlineformulatexmath idTM0003 notationLaTeX0.3 lt texmathinlineformula FeH inlineformulatexmath idTM0004 notationLaTeXlt 0.2texmathinlineformula. The additional flexibility of the ANN provides some improvements including better modelling of the lithium dip at ages inlineformulatexmath idTM0005 notationLaTeXlt 50texmathinlineformula Myr and inlineformulatexmath idTM0006 notationLaTeXTrm effsim 3500texmathinlineformula K and of the intrinsic dispersion in LiEW at all ages. Poor age discrimination is still an issue at ages gt1 Gyr confirming that additional modelling flexibility is not sufficient to fully represent the LiEWageTinlineformulatexmath idTM0007 notationLaTeXtextefftexmathinlineformula relationship and suggesting the involvement of further astrophysical parameters. Expansion to include such parametersrotation accretion and surface gravityis discussed and the use of an ANN means these can be more easily included in future iterations alongside more flexible functional forms for the LiEW dispersion. Our methods and ANN model are provided in an updated version 2.0 of the EAGLES software. | 2024-11-01T00:00:00Z | ['arXiv:2409.07523', '2024arXiv240907523W', '10.1093/mnras/stae2133', '2024MNRAS.534.2014W', '2024MNRAS.tmp.2100W', '10.48550/arXiv.2409.07523'] | ['Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'Computer Science - Machine Learning'] | Using neural network models to estimate stellar ages from lithium equivalent widths an EAGLES expansion | 2,024 | 479 | 0.52 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.07523.pdf |
2024arXiv240907955B | In the summer of 2023 the pulsar timing arrays PTAs announced a compelling evidence for the existence of a nanohertz stochastic gravitational wave background SGWB. Despite this breakthrough however several critical questions remain unanswered What is the source of the signal How can cosmic variance be accounted for To what extent can we constrain nanohertz gravity When will individual supermassive black hole binaries become observable And how can we achieve a stronger detection These open questions have spurred significant interests in PTA science making this an opportune moment to revisit the astronomical and theoretical foundations of the field as well as the data analysis techniques employed. In this review we focus on the theoretical aspects of the SGWB as detected by PTAs. We provide a comprehensive derivation of the expected signal and its correlation presented in a pedagogical manner while also addressing current constraints. Looking ahead we explore future milestones in the field with detailed discussions on emerging theoretical considerations such as cosmic variance the cumulants of the one and twopoint functions subluminal gravitational waves and the anisotropy and polarization of the SGWB. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.07955', '2024arXiv240907955B', 'arXiv:2409.07955'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena', 'General Relativity and Quantum Cosmology'] | Charting the Nanohertz Gravitational Wave Sky with Pulsar Timing Arrays | 2,024 | 479 | 0.48 | ['EPRINT_HTML', 'EPRINT_PDF'] | 2 | https://arxiv.org/pdf/2409.07955.pdf |
2024arXiv240906462D | We argue that dielectric haloscopes like MADMAX originally designed for detecting axion dark matter are also very promising gravitational wave detectors. Operated in resonant mode at frequencies around mathcalO10textGHz these detectors benefit from enhanced gravitational wave to photon conversion at the surfaces of a stack of thin dielectric disks. Since the gravitational wave is relativistic there is an additional enhancement of the signal compared to the axion case due to increased conversion probability of gravitational waves to photons in the vacuum between the disks. A gravitational wave search using a dielectric haloscope imposes stringent requirements on the disk thickness and placement but relaxed requirements on the disk smoothness. An advantage is the possibility of a broadband or hybrid resonantbroadband operation mode which extends the frequency range down to mathcalO100textMHz. We show that strain sensitivities down to 1021 textHz12 times 10textGHzf will be possible in the coming years for the broadband setup while a resonant setup optimized for gravitational waves could even reach 3times 1023 textHz12 times 10textGHzf with current technology. | 2024-09-01T00:00:00Z | ['2024arXiv240906462D', 'arXiv:2409.06462', '10.48550/arXiv.2409.06462'] | ['High Energy Physics - Phenomenology', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Experiment'] | Dielectric Haloscopes as Gravitational Wave Detectors | 2,024 | 482 | 0.29 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.06462.pdf |
2024arXiv240910617S | A very pressing question in contemporary physics is the identity of Dark Matter DM and one that has not been answered affirmatively to any degree so far. Primordial Black Holes PBHs are one of the most wellmotivated DM candidates. Light enough PBHs have been constrained by either the nondetection of their Hawking radiation itself or by the nonobservation of any measurable effects of this radiation on astrophysical and cosmological observables. We constrain the PBH density by their Hawking radiation effect on the intergalactic medium IGM temperature evolution. We use the latest deductions of IGM temperature from Lymanalpha forest observations. We put constraints on the fraction of PBH DM with masses 5 times 1015 g 1017 g separately for spinning and nonspinning BHs. We derive constraints by dealing with the heating effects of the astrophysical reionization of the IGM in two ways. In one way we completely neglect this heating due to astrophysical sources thus giving us weaker constraints but completely robust to the reionization history of the universe. In the second way we utilise some modelling of the ionization and temperature history and use it to derive more stringent constraints. We find that for nonspinning PBHs of mass 1016 g the current measurements can constrain the PBHdensity to be lesssim 0.1 of the total DM. We find that these constraints from the latest Lymanalpha forest temperature measurements are competitive and hence provide a new observable to probe the nature of PBH DM. The systematics affecting Lymanalpha forest measurements are different from other constraining observations and thus this is a complementary probe. | 2024-09-01T00:00:00Z | ['2024arXiv240910617S', '10.48550/arXiv.2409.10617', 'arXiv:2409.10617'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Phenomenology', 'High Energy Physics - Theory'] | Hunting Primordial Black Hole Dark Matter in Lymanalpha Forest | 2,024 | 482 | 0.4 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.10617.pdf |
2024arXiv240904606V | Waveoptics phenomena in gravitational lensing occur when the signals wavelength is commensurate to the gravitational radius of the lens. Although potentially detectable in lensed gravitational waves fast radio bursts and pulsars accurate numerical predictions are challenging to compute. Here we present novel methods for waveoptics lensing that allow the treatment of general lenses. In addition to a general algorithm specialized methods optimize symmetric lenses arbitrary number of images and generic lenses in the singleimage regime. We also develop approximations for simple lenses pointlike and singular isothermal sphere that drastically outperform known solutions without compromising accuracy. These algorithms are implemented in Gravitational Lensing of Waves GLoW an accurate flexible and fast code. GLoW efficiently computes the frequencydependent amplification factor for generic lens models and arbitrary impact parameters in O1 ms to O10 ms depending on the lens configuration and complexity. GLoW is readily applicable to model lensing diffraction on gravitationalwave signals offering new means to investigate the distribution of darkmatter and largescale structure with signals from ground and space detectors. | 2024-09-01T00:00:00Z | ['2024arXiv240904606V', 'arXiv:2409.04606', '10.48550/arXiv.2409.04606'] | ['General Relativity and Quantum Cosmology', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Instrumentation and Methods for Astrophysics'] | GLoW novel methods for waveoptics phenomena in gravitational lensing | 2,024 | 483 | 0.45 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.04606.pdf |
2024arXiv240912950C | We discuss a mechanism of primordial black hole PBH formation that does not require specific features in the inflationary potential revisiting previous literature. In this mechanism a light spectator field evolves stochastically during inflation and remains subdominant during the postinflationary era. Even though the curvature power spectrum stays small at all scales rare perturbations of the field probe a local maximum in its potential leading to nonGaussian tails in the distribution of curvature fluctuations and to copious PBH production. For a concrete axionlike particle ALP scenario we analytically determine the distribution of the compaction function for perturbations showing that it is characterized by a heavy tail which produces an extended PBH mass distribution. We find the ALP mass and decay constant to be correlated with the PBH mass for instance an ALP with a mass ma 5.4 times 1014 eV and a decay constant fa 4.6 times 105 Mpl can lead to PBHs of mass Mrm PBH 1021 g as the entire dark matter DM of the universe and is testable in future PBH observations via lensing in the NGRST and mergers detectable in the LISA and ET Gravitational Waves GW detectors. We then extend our analysis to mixed ALP and PBH dark matter and Higgslike spectator fields. We find that PBHs cluster strongly over all cosmological scales clashing with CMB isocurvature bounds. We argue that this problem is shared by all PBH production from inflationary models that depend solely on large nonGaussianity without a peak in the curvature power spectrum and discuss possible remedies. | 2024-09-01T00:00:00Z | ['2024arXiv240912950C', 'arXiv:2409.12950', '10.48550/arXiv.2409.12950'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Phenomenology', 'High Energy Physics - Theory'] | Stochastic Axionlike Curvaton NonGaussianity and Primordial Black Holes Without Large Power Spectrum | 2,024 | 483 | 0.31 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.12950.pdf |
2024MNRAS.534.1682O | Galaxy properties are known to be affected by their environment. This is well established for the extremes of the density scales between the highdensity cluster environment and the lowdensity field. It is however not fully understood how the intermediatedensity regime of cosmic web filaments affects galaxy evolution. We investigate this environmental effect using a mass complete sample of 23 441 galaxies in the Sloan Digital Sky Survey DR8 Main Galaxy Sample inlineformulatexmath idTM0001 notationLaTeXMtextStellar gt 109.91 textModot texmathinlineformula. We define six environments probing different density regimes and representing unique stages in the structure formation process comparing the differences in star formation activity and morphology between them. We find that galaxies in filaments tend to be less starforming and favour more earlytype morphologies than those in the field. These differences persist when considering stellar massmatched samples suggesting that this is a consequence of the environment. We further investigate whether these trends are a result of the largescale or local environment through constructing samples matched both in stellar mass and local galaxy density. We find that when also matching in local galaxy density the differences observed between the filament and field population vanishes concluding that the environmental effect of filaments can be entirely parametrized by a local galaxy density index. We find that differences can still be seen in comparisons with the interiors of clusters suggesting these are unique environments which can impart additional physical processes not characterized by local galaxy density. | 2024-11-01T00:00:00Z | ['2024MNRAS.tmp.2101O', '2024MNRAS.534.1682O', '2024arXiv240909028O', '10.1093/mnras/stae2142', 'arXiv:2409.09028', '10.48550/arXiv.2409.09028'] | ['Astrophysics - Astrophysics of Galaxies'] | The effect of cosmic web filaments on galaxy evolution | 2,024 | 490 | 0.61 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2 | https://arxiv.org/pdf/2409.09028.pdf |
2024PSJ.....5..184W | Apophiss current trajectory takes it safely past our planet at a distance of several Earth radii on 2029 April 13. Here the possibility is considered that Apophis could collide with a small asteroid like the ones that frequently and unpredictably strike Earth and the resulting perturbation of its trajectory. The probability of an impact that could significantly displace Apophis relative to its keyholes is found to be less than one in 10SUP6SUP requiring a v 0.3 mm sSUP1SUP while for an impact that could significantly displace Apophis compared to its miss distance in 2029 it is less than one in 10SUP9SUP requiring a v 5 cm sSUP1SUP. These probabilities are below the usual thresholds considered by asteroid impact warning systems. Apophis is in the daytime sky and unobservable from mid2021 to 2027. It will be challenging to determine from singlenight observations in 2027 if Apophis has moved on the target plane enough to enter a dangerous keyhole as the deviation from the nominal ephemeris might be only a few tenths of an arcsecond. An impending Earth impact would however be signaled clearly in most cases by deviations of tens of arcseconds of Apophis from its nominal ephemeris in 2027. Thus most of the impact risk could be retired by a single observation of Apophis in 2027 though a minority of cases present some ambiguity and are discussed in more detail. Charts of the onsky position of Apophis under different scenarios are presented for quick assessment by observers. | 2024-08-01T00:00:00Z | ['10.3847/PSJ/ad644d', '2024PSJ.....5..184W', 'arXiv:2409.06059', '10.48550/arXiv.2409.06059', '2024arXiv240906059W'] | ['Small Solar System bodies', 'Close encounters', 'Asteroids', 'Near-Earth objects', '1469', '255', '72', '1092', 'Astrophysics - Earth and Planetary Astrophysics'] | On the Sensitivity of Apophiss 2029 Earth Approach to Small Asteroid Impacts | 2,024 | 496 | 0.42 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.06059.pdf |
2024arXiv240513491E | The current standard model of cosmology successfully describes a variety of measurements but the nature of its main ingredients dark matter and dark energy remains unknown. Euclid is a mediumclass mission in the Cosmic Vision 20152025 programme of the European Space Agency ESA that will provide highresolution optical imaging as well as nearinfrared imaging and spectroscopy over about 14000 deg2 of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe its primary probes for cosmology these exquisite data will enable a wide range of science. This paper provides a highlevel overview of the mission summarising the survey characteristics the various dataprocessing steps and data products. We also highlight the main science objectives and expected performance. | 2024-05-01T00:00:00Z | ['2024arXiv240513491E', 'arXiv:2405.13491', '10.48550/arXiv.2405.13491'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Instrumentation and Methods for Astrophysics'] | Euclid. I. Overview of the Euclid mission | 2,024 | 497 | 0.79 | ['EPRINT_HTML', 'EPRINT_PDF'] | 144 | https://arxiv.org/pdf/2405.13491.pdf |
2024arXiv240906208L | We explore the coevolution of dark matter halos their central galaxies and central supermassive black holes SMBHs using the IllustrisTNG TNG simulation. We find that the evolutionary histories of individual galaxies in the Mrm BHM plane can be decomposed into four distinct phases separated by three transition points. We identify the driving processes of galaxy evolution within each phase and derive the conditions necessary and sufficient for transitions to subsequent phases. The first phase is dominated by star formation with its duration primarily determined by the mass of the SMBH seed and the surrounding gas environment. The second phase is characterized by rapid SMBH growth and the transition to the next phase occurs when the thermalmode feedback of active galactic nucleus AGN can unbind gas from the galaxy. The third phase involves selfregulation of the SMBH and the transition to the quenched phase occurs when the kineticmode feedback of AGN counterbalances gas cooling within the subhalo. The final phase is dominated by mergers. We investigate the use of scaling relations among different mass components and evolutionary phases to understand processes implemented in TNG and other simulations and discuss how current and forthcoming observations can be used to constrain models. | 2024-09-01T00:00:00Z | ['arXiv:2409.06208', '2024arXiv240906208L', '10.48550/arXiv.2409.06208'] | ['Astrophysics - Astrophysics of Galaxies'] | Physical Processes Behind the CoEvolution of Halos Galaxies and Supermassive Black Holes in the IllustrisTNG Simulation | 2,024 | 498 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF'] | 1 | https://arxiv.org/pdf/2409.06208.pdf |
2024ApJ...963..129M | Characterizing the prevalence and properties of faint active galactic nuclei AGNs in the early Universe is key for understanding the formation of supermassive black holes SMBHs and determining their role in cosmic reionization. We perform a spectroscopic search for broad H emitters at z 46 using deep JWSTNIRCam imaging and wide field slitless spectroscopy from the EIGER and FRESCO surveys. We identify 20 H lines at z 4.25.5 that have broad components with line widths from 12003700 km sSUP1SUP contributing 3090 of the total line flux. We interpret these broad components as being powered by accretion onto SMBHs with implied masses 10SUP78SUP M SUBSUB. In the UV luminosity range M SUBUVAGNhostSUB 21 to 18 we measure number densities of 10SUP5SUP cMpcSUP3SUP. This is an order of magnitude higher than expected from extrapolating quasar UV luminosity functions LFs. Yet such AGN are found in only lt1 of starforming galaxies at z 5. The number density discrepancy is much lower when compared to the broad H LF. The SMBH mass function agrees with large cosmological simulations. In two objects we detect complex H profiles that we tentatively interpret as caused by absorption signatures from dense gas fueling SMBH growth and outflows. We may be witnessing early AGN feedback that will clear dustfree pathways through which more massive blue quasars are seen. We uncover a strong correlation between reddening and the fraction of total galaxy luminosity arising from faint AGN. This implies that early SMBH growth is highly obscured and that faint AGN are only minor contributors to cosmic reionization. | 2024-03-01T00:00:00Z | ['2024ApJ...963..129M', '2023arXiv230605448M', '10.48550/arXiv.2306.05448', 'arXiv:2306.05448', '10.3847/1538-4357/ad2345'] | ['High-redshift galaxies', 'Quasars', 'Active galactic nuclei', 'Reionization', '734', '1319', '16', '1383', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics'] | Little Red Dots An Abundant Population of Faint Active Galactic Nuclei at z 5 Revealed by the EIGER and FRESCO JWST Surveys | 2,024 | 500 | 0.75 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 254 | https://arxiv.org/pdf/2306.05448.pdf |
2024ApJ...977...35G | We predict the existence of Ori B a lowmass companion orbiting Betelgeuse. This is motivated by the presence of a 2170 day long secondary period LSP in Betelgeuses lightcurve a periodicity that is 5 times longer than the stars 416 day fundamental radial pulsation mode. While binarity is currently the leading hypothesis for LSPs in general the LSP and the radial velocity RV variations observed in Betelgeuse taken together necessitate a revision of the prevailing physical picture. Specifically the lightcurveRV phase difference requires a companion to be behind Betelgeuse at the LSP luminosity minimum 180 out of phase with the system orientation associated with occultation. We demonstrate the consistency of this model with available observational constraints and identify tensions in all other proposed LSP hypotheses. Within this framework we calculate a mass for Ori B of inlineformula inlineformula and an orbital separation of 1850 70 R SUBSUB or inlineformula inlineformula times the radius of Betelgeuse. We then describe the features of the companion as constrained by the fundamental parameters of Betelgeuse and its orbital system and discuss what would be required to confirm the companions existence observationally. | 2024-12-01T00:00:00Z | ['10.3847/1538-4357/ad87f4', '10.48550/arXiv.2408.09089', 'arXiv:2408.09089', '2024ApJ...977...35G', '2024arXiv240809089G'] | ['Long period variable stars', 'Binary stars', 'Red supergiant stars', 'Circumstellar dust', 'Massive stars', 'Stellar pulsations', 'Pulsation modes', '935', '154', '1375', '236', '732', '1625', '1309', 'Astrophysics - Solar and Stellar Astrophysics', 'Astrophysics - High Energy Astrophysical Phenomena'] | A Buddy for Betelgeuse Binarity as the Origin of the Long Secondary Period in Orionis | 2,024 | 504 | 0.65 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 3 | https://arxiv.org/pdf/2408.09089.pdf |
2024arXiv240910609I | We explore fullshape analysis with simulationbased priors which is the simplest approach to galaxy clustering data analysis that combines effective field theory EFT on large scales and numerical simulations on small scales. The core ingredient of our approach is the prior density of EFT parameters which we extract from a suite of 10500 galaxy simulations based on the halo occupation distribution HOD model. We measure the EFT parameters with the fieldlevel forward model which enables us to cancel cosmic variance. On the theory side we develop a new efficient approach to calculate fieldlevel transfer functions using timesliced perturbation theory and the logarithmic fast Fourier transform. We study cosmology dependence of EFT parameters of dark matter halos and HOD galaxies and find that it can be ignored for the purpose of prior generation. We use neural density estimation to model the measured distribution of EFT parameters. Our distribution model is then used as a prior in a reanalysis of the BOSS fullshape galaxy power spectrum data. Assuming the LambdaCDM model we find significant approx 30 and approx 60 improvements for the matter density fraction and the mass fluctuation amplitude which are constrained to Omegam 0.315 pm 0.010 and sigma8 0.671 pm 0.027. The value of the Hubble constant does not change H0 68.7pm 1.1 kmsMpc. This reaffirms earlier reports of the structure growth tension from the BOSS data. Finally we use the measured EFT parameters to constrain galaxy formation physics. | 2024-09-01T00:00:00Z | ['arXiv:2409.10609', '10.48550/arXiv.2409.10609', '2024arXiv240910609I'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Instrumentation and Methods for Astrophysics', 'High Energy Physics - Phenomenology', 'High Energy Physics - Theory'] | Fullshape analysis with simulationbased priors cosmological parameters and the structure growth anomaly | 2,024 | 509 | 0.49 | ['EPRINT_HTML', 'EPRINT_PDF'] | 10 | https://arxiv.org/pdf/2409.10609.pdf |
2013SpPol..29...40H | Deliberate and unintentional radio transmissions from Earth propagate into space. These transmissions could be detected by extraterrestrial watchers over interstellar distances. This article analyzes the harm and benefits of deliberate and unintentional transmissions relevant to Earth and humanity. Comparing the magnitude of deliberate radio broadcasts intended for messaging to extraterrestrial intelligence METI with the background radio spectrum of Earth we find that METI attempts to date have much lower detectability than emissions from current radio communication technologies on Earth. METI broadcasts are usually transient and several orders of magnitude less powerful than other terrestrial sources such as astronomical and military radars which provide the strongest detectable signals. The benefits of radio communication on Earth most probably outweigh the potential harm of detection by extraterrestrial watchers however the uncertainty regarding the outcome of contact with extraterrestrial beings creates difficulty in assessing whether or not to engage in longterm and largescale METI. | 2013-02-01T00:00:00Z | ['10.48550/arXiv.1207.5540', '10.1016/j.spacepol.2012.11.006', '2012arXiv1207.5540H', 'arXiv:1207.5540', '2013SpPol..29...40H'] | ['Physics - Popular Physics', 'Physics - Physics and Society'] | The benefits and harm of transmitting into space | 2,013 | 511 | 0.32 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 21 | https://arxiv.org/pdf/1207.5540.pdf |
2024arXiv240903829W | We report the spectroscopic discovery of a massive quiescent galaxy at zrm spec7.29pm0.01 just sim700Myr after the Big Bang. RUBIESUDSQGz7 was selected from public JWSTNIRCam and MIRI imaging from the PRIMER survey and observed with JWSTNIRSpec as part of RUBIES. The NIRSpecPRISM spectrum reveals one of the strongest Balmer breaks observed thus far at zgt6 no emission lines but tentative Balmer and Ca absorption features as well as a Lyman break. Simultaneous modeling of the NIRSpecPRISM spectrum and NIRCam and MIRI photometry spanning 0.918mum shows that the galaxy formed a stellar mass of logMModot10.230.040.04 in a rapid sim 100200Myr burst of star formation at zsim89 and ceased forming stars by zsim8 resulting in log rmsSFRyr1lt10. We measure a small physical size of 2092433rm pc which implies a high stellar mass surface density within the effective radius of logSigmarm erm Modotkpc210.850.120.11 comparable to the densities measured in quiescent galaxies at zsim25. The 3D stellar mass density profile of RUBIESUDSQGz7 is remarkably similar to the central densities of local massive ellipticals suggesting that at least some of their cores may have already been in place at zgt7. The discovery of RUBIESUDSQGz7 has strong implications for galaxy formation models the estimated number density of quiescent galaxies at zsim7 is gt100times larger than predicted from any model to date indicating that quiescent galaxies have formed earlier than previously expected. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.03829', 'arXiv:2409.03829', '2024arXiv240903829W'] | ['Astrophysics - Astrophysics of Galaxies'] | RUBIES Reveals a Massive Quiescent Galaxy at z7.3 | 2,024 | 511 | 0.69 | ['EPRINT_HTML', 'EPRINT_PDF'] | 22 | https://arxiv.org/pdf/2409.03829.pdf |
2024arXiv240911332M | We examine a century of radial velocity visual magnitude and astrometric observations of the nearest red supergiant Betelgeuse in order to reexamine the centuryold assertion that Betelgeuse might be a spectroscopic binary. These data reveal Betelgeuse varying stochastically over years and decades due to its boiling convective envelope periodically with a 5.78yr long secondary period and quasiperiodically from pulsations with periods of several hundred days. We show that the long secondary period is consistent between astrometric and RV datasets and argue that it indicates a lowmass companion to Betelgeuse less than a solar mass orbiting in a 2110 day period at a separation of just over twice Betelgeuses radius. The companion star would be nearly twenty times less massive and a million times fainter than Betelgeuse with similar effective temperature effectively hiding it in plain sight near one of the beststudied stars in the night sky. The astrometric data favor an edgeon binary with orbital plane aligned with Betelgeuses measured spin axis. Tidal spinorbit interaction drains angular momentum from the orbit and spins up Betelgeuse explaining the spinorbit alignment and Betelgeuses anomalously rapid spin. In the future the orbit will decay until the companion is swallowed by Betelgeuse in the next 10000 years. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.11332', '2024arXiv240911332M', 'arXiv:2409.11332'] | ['Astrophysics - Solar and Stellar Astrophysics'] | Radial Velocity and Astrometric Evidence for a Close Companion to Betelgeuse | 2,024 | 516 | 0.66 | ['EPRINT_HTML', 'EPRINT_PDF'] | 3 | https://arxiv.org/pdf/2409.11332.pdf |
2024arXiv240912200M | The ultrarelativistic limit of general relativity is a theory known as Carroll gravity. We provide a philosophical introduction to the formalism of Carroll gravity and to its status as a limit of general relativity we also explore some of its various conceptually interesting features. | 2024-09-01T00:00:00Z | ['arXiv:2409.12200', '2024arXiv240912200M', '10.48550/arXiv.2409.12200'] | ['Physics - History and Philosophy of Physics', 'General Relativity and Quantum Cosmology'] | A primer on Carroll gravity | 2,024 | 520 | 0.26 | ['EPRINT_HTML', 'EPRINT_PDF'] | 0 | https://arxiv.org/pdf/2409.12200.pdf |
2024arXiv240912219G | In this paper we provide a statecounting derivation of the BekensteinHawking entropy formula for singlesided black holes. We firstly articulate the concept of the black hole microstates. Then we construct explicit mircostates of singlesided black holes in 21dimensional spacetimes with a negative cosmological constant. These microstates are constructed by putting a KarchRandall brane behind the black hole horizon. Their difference is described by different interior excitations which gravitationally backreact. We show that these microstates have nonperturbatively small overlaps with each other. As a result we use this fact to give a statecounting derivation of the BekensteinHawking entropy formula for singlesided black holes. At the end we notice that there are no negative norm states in the resulting Hilbert space of the black hole microstates which in turn ensures unitarity. All calculations in this paper are analytic and can be easily generalized to higher spacetime dimensions. | 2024-09-01T00:00:00Z | ['10.48550/arXiv.2409.12219', 'arXiv:2409.12219', '2024arXiv240912219G'] | ['High Energy Physics - Theory', 'General Relativity and Quantum Cosmology'] | Microscopic Origin of the Entropy of Singlesided Black Holes | 2,024 | 523 | 0.16 | ['EPRINT_HTML', 'EPRINT_PDF'] | 5 | https://arxiv.org/pdf/2409.12219.pdf |
2023A&A...674A...1G | Context. We present the third data release of the European Space Agencys Gaia mission Gaia DR3. This release includes a large variety of new data products notably a much expanded radial velocity survey and a very extensive astrophysical characterisation of Gaia sources. BR Aims We outline the content and the properties of Gaia DR3 providing an overview of the main improvements in the data processing in comparison with previous data releases where applicable and a brief discussion of the limitations of the data in this release. BR Methods The Gaia DR3 catalogue is the outcome of the processing of raw data collected with the Gaia instruments during the first 34 months of the mission by the Gaia Data Processing and Analysis Consortium. BR Results The Gaia DR3 catalogue contains the same source list celestial positions proper motions parallaxes and broad band photometry in the G GSUBBPSUB and GSUBRPSUB passbands already present in the Early Third Data Release Gaia EDR3. Gaia DR3 introduces an impressive wealth of new data products. More than 33 million objects in the ranges GSUBRVSSUB lt 14 and 3100 lt TSUBeffSUB lt 14 500 have new determinations of their mean radial velocities based on data collected by Gaia. We provide GSUBRVSSUB magnitudes for most sources with radial velocities and a line broadening parameter is listed for a subset of these. Mean Gaia spectra are made available to the community. The Gaia DR3 catalogue includes about 1 million mean spectra from the radial velocity spectrometer and about 220 million lowresolution blue and red prism photometer BPRP mean spectra. The results of the analysis of epoch photometry are provided for some 10 million sources across 24 variability types. Gaia DR3 includes astrophysical parameters and source class probabilities for about 470 million and 1500 million sources respectively including stars galaxies and quasars. Orbital elements and trend parameters are provided for some 800 000 astrometric spectroscopic and eclipsing binaries. More than 150 000 Solar System objects including new discoveries with preliminary orbital solutions and individual epoch observations are part of this release. Reflectance spectra derived from the epoch BPRP spectral data are published for about 60 000 asteroids. Finally an additional data set is provided namely the Gaia Andromeda Photometric Survey consisting of the photometric time series for all sources located in a 5.5 degree radius field centred on the Andromeda galaxy. BR Conclusions This data release represents a major advance with respect to Gaia DR2 and Gaia EDR3 because of the unprecedented quantity quality and variety of source astrophysical data. To date this is the largest collection of allsky spectrophotometry radial velocities variables and astrophysical parameters derived from both low and highresolution spectra and includes a spectrophotometric and dynamical survey of SSOs of the highest accuracy. The nonsingle star content surpasses the existing data by orders of magnitude. The quasar host and galaxy light profile collection is the first such survey that is all sky and space based. The astrophysical information provided in Gaia DR3 will unleash the full potential of Gaias exquisite astrometric photometric and radial velocity surveys. | 2023-06-01T00:00:00Z | ['2023A&A...674A...1G', '2022arXiv220800211G', '10.1051/0004-6361/202243940', '10.48550/arXiv.2208.00211', 'arXiv:2208.00211'] | ['techniques: photometric', 'techniques: spectroscopic', 'techniques: radial velocities', 'catalogs', 'astrometry', 'parallaxes', 'Astrophysics - Astrophysics of Galaxies'] | Gaia Data Release 3. Summary of the content and survey properties | 2,023 | 533 | 0.82 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 2,339 | https://arxiv.org/pdf/2208.00211.pdf |
2024Natur.633..318C | The first observations of the James Webb Space Telescope JWST have revolutionized our understanding of the Universe by identifying galaxies at redshift z 13 refs. SUP13SUP. In addition the discovery of many luminous galaxies at Cosmic Dawn z gt 10 has suggested that galaxies developed rapidly in apparent tension with many standard modelsSUP48SUP. However most of these galaxies lack spectroscopic confirmation so their distances and properties are uncertain. Here we present JWST Advanced Deep Extragalactic SurveyNearInfrared Spectrograph spectroscopic confirmation of two luminous galaxies at inlineformula idIEq1mmlmathmmlmrowmmlmizmmlmimmlmommlmommlmsubsupmmlmrowmmlmn14.32mmlmnmmlmrowmmlmrowmmlmommlmommlmn0.20mmlmnmmlmrowmmlmrowmmlmommlmommlmn0.08mmlmnmmlmrowmmlmsubsupmmlmrowmmlmathinlineformula and z 13.90 0.17. The spectra reveal ultraviolet continua with prominent Lyman breaks but no detected emission lines. This discovery proves that luminous galaxies were already in place 300 million years after the Big Bang and are more common than what was expected before JWST. The most distant of the two galaxies is unexpectedly luminous and is spatially resolved with a radius of 260 parsecs. Considering also the very steep ultraviolet slope of the second galaxy we conclude that both are dominated by stellar continuum emission showing that the excess of luminous galaxies in the early Universe cannot be entirely explained by accretion onto black holes. Galaxy formation models will need to address the existence of such large and luminous galaxies so early in cosmic history. | 2024-09-01T00:00:00Z | ['10.1038/s41586-024-07860-9', 'arXiv:2405.18485', '10.48550/arXiv.2405.18485', '2024Natur.633..318C', '2024arXiv240518485C'] | ['Astrophysics - Astrophysics of Galaxies'] | Spectroscopic confirmation of two luminous galaxies at a redshift of 14 | 2,024 | 544 | 0.77 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML'] | 84 | https://arxiv.org/pdf/2405.18485.pdf |
2024arXiv240907976J | As a promising dark matter candidate primordial black holes PBHs lighter than sim1018Modot are supposed to have evaporated by today through Hawking radiation. This scenario is challenged by the memory burden effect which suggests that the evaporation of black holes may slow down significantly after they have emitted about half of their initial mass. We explore the astrophysical implications of the memory burden effect on the PBH abundance by today and the possibility for PBHs lighter than sim1018Modot to persist as dark matter. Our analysis utilizes current LIGOVirgoKAGRA data to constrain the primordial power spectrum and infer the PBH abundance. We find a null detection of scalarinduced gravitational waves that accompanied the formation of the PBHs. Then we find that PBHs are ruled out within the mass range sim10241019Modot. Furthermore we expect that nextgeneration gravitational wave detectors such as the Einstein Telescope and the Cosmic Explorer will provide even more stringent constraints. Our results indicate that future detectors can reach sensitivities that could rule out PBH as dark matter within sim1029Modot1016Modot in the null detection of scalarinduced gravitational waves. | 2024-09-01T00:00:00Z | ['arXiv:2409.07976', '2024arXiv240907976J', '10.48550/arXiv.2409.07976'] | ['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Theory'] | Constraints on the Primordial Black Hole Abundance through ScalarInduced Gravitational Waves from Advanced LIGO and Virgos First Three Observing Runs | 2,024 | 547 | 0.37 | ['EPRINT_HTML', 'EPRINT_PDF'] | 5 | https://arxiv.org/pdf/2409.07976.pdf |
2024ApJ...974L..28B | Hubble Space Telescope imaging shows that most starforming galaxies at cosmic noonthe peak of cosmic star formation historyappear diskdominated leaving the origin of the dense cores in their quiescent descendants unclear. With the James Webb Space Telescopes highresolution imaging to 5 m we can now map the restframe nearinfrared emission a much closer proxy for stellar mass distribution in these massive galaxies. We selected 70 starforming galaxies with 10 lt logM lt 12 and 1.5 lt z lt 3 in the CEERS survey and compare their morphologies in the restframe optical to those in the restframe nearIR. While the bulk of these galaxies are diskdominated in 1.5 m restframe optical imaging they appear more bulgedominated at 4.4 m restframe nearinfrared. Our analysis reveals that in massive starforming galaxies at z 2 the radial surface brightness profiles steepen significantly from a slope of 0.3 dexSUP1SUP at 1.5 m to 1.4 dexSUP1SUP at 4.4 m within radii lt1 kpc. Additionally we find their total flux contained within the central 1 kpc is approximately 7 times higher in F444W than in F150W. In restoptical emission a galaxys central surface density appears to be the strongest indicator of whether it is quenched or starforming. Our most significant finding is that at redder wavelengths the central surface density ratio between quiescent and starforming galaxies dramatically decreases from 10 to 1. This suggests the high central densities associated with galaxy quenching are already in place during the starforming phase imposing new constraints on the transition from star formation to quiescence. | 2024-10-01T00:00:00Z | ['arXiv:2409.08328', '10.3847/2041-8213/ad7e27', '2024arXiv240908328B', '2024ApJ...974L..28B', '10.48550/arXiv.2409.08328'] | ['Galaxy evolution', 'Galaxy formation', 'Galaxy structure', 'Galaxy bulges', 'Quenched galaxies', '594', '595', '622', '578', '2016', 'Astrophysics - Astrophysics of Galaxies'] | JWST Reveals Bulgedominated Starforming Galaxies at Cosmic Noon | 2,024 | 555 | 0.59 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.08328.pdf |
2024ApJ...977...83R | CIZA J2242.85301 or the Sausage cluster is wellstudied over a range of frequencies. Since its first discovery a lot of interesting features and unique characteristics have been uncovered. In this work we report some more new morphological features using the uGMRT band3 and band4 data. In the north relic we observe variation in the spectral index profiles across the relic width from the east to west which may indicate a decrease in the downstream cooling rate in that direction. We reconfirm the presence of an additional 930 kpc relic in the north. We classify the filamentary source in the downstream region to be a narrowangle tail NAT radio galaxy. The bright arc in the east relic shows a substructure in the spectral index profile which may indicate the presence of finer filaments. We further report the presence of a doublestrand structure in the east relic similar to the Toothbrush relic. We categorize the bright Lshaped structure in the southern relic to be a NAT radio galaxy as well as trace the actual 1.1 Mpc relic component. We reconfirm the existence of the faint southern extent measuring the relic length to be 1.8 Mpc. Furthermore we suggest the southern relic to be a union of individual component relics rather than a single giant filamentary relic. Lastly based on the morphological symmetry between northern and southern relics we suggest a schematic shock structure associated with the merger event in an attempt to explain their formation scenario. | 2024-12-01T00:00:00Z | ['2024arXiv240907504R', 'arXiv:2409.07504', '10.48550/arXiv.2409.07504', '2024ApJ...977...83R', '10.3847/1538-4357/ad8920'] | ['Galaxy clusters', 'Extragalactic astronomy', 'Intracluster medium', 'Non-thermal radiation sources', 'High energy astrophysics', '584', '506', '858', '1119', '739', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'Astrophysics - Astrophysics of Galaxies', 'Astrophysics - High Energy Astrophysical Phenomena'] | uGMRT SubGHz View of the Sausage Cluster Diffuse Radio Sources | 2,024 | 567 | 0.45 | ['EPRINT_HTML', 'EPRINT_PDF', 'PUB_HTML', 'PUB_PDF'] | 0 | https://arxiv.org/pdf/2409.07504.pdf |
2024arXiv240907521E | We derive a cutting rule for equaltime inin correlators including cosmological correlators based on Keldysh ra basis which decomposes diagrams into fully retarded functions and cutpropagators consisting of Wightman functions. Our derivation relies only on basic assumptions such as unitarity locality and the causal structure of the inin formalism and therefore holds for theories with arbitrary particle contents and local interactions at any loop order. As an application we show that nonlocal cosmological collider signals arise solely from cutpropagators under the assumption of microcausality. Since the cutpropagators do not contain antitimeordering theta functions the conformal time integrals are factorized simplifying practical calculations. | 2024-09-01T00:00:00Z | ['2024arXiv240907521E', '10.48550/arXiv.2409.07521', 'arXiv:2409.07521'] | ['High Energy Physics - Theory', 'Astrophysics - Cosmology and Nongalactic Astrophysics', 'High Energy Physics - Phenomenology'] | Cutting rule for inin correlators and cosmological collider | 2,024 | 568 | 0.21 | ['EPRINT_HTML', 'EPRINT_PDF'] | 4 | https://arxiv.org/pdf/2409.07521.pdf |