Astronomy & Astrophysics最新文献

{"title":"A search for the three isomers of cyano-1,3-butadiene in TMC-1: Implications for bottom-up routes involving 1,3-butadiene⋆","authors":"M. Agúndez, C. Cabezas, N. Marcelino, B. Tercero, R. Fuentetaja, P. de Vicente, J. Cernicharo","doi":"10.1051/0004-6361/202554343","DOIUrl":"https://doi.org/10.1051/0004-6361/202554343","url":null,"abstract":"The molecule 1,3-butadiene (CH<sub>2<sub/>CHCHCH<sub>2<sub/>) could play a key role in the synthesis of the cyclic molecules cyclopentadiene and benzene in cold dense clouds. Since 1,3-butadiene is non-polar, we searched for its cyano derivative, which exists in the form of three different polar isomers, in the cold dense cloud TMC-1. We used the most recent data obtained with the Yebes 40 m telescope in the Q band (31.0−50.3 GHz) in the frame of the QUIJOTE project. We did not detect either of the isomers of 1-cyano-1,3-butadiene, and we derive 3 <i>σ<i/> upper limits to their column densities of 1.2 × 10<sup>10<sup/> cm<sup>−2<sup/> and 2.0 × 10<sup>10<sup/> cm<sup>−2<sup/> for <i>E<i/>- and <i>Z<i/>-1-cyano-1,3-butadiene, respectively. Our results are not consistent with those from , ApJ, 948, 133), who determine a column density of 3.8 × 10<sup>10<sup/> cm<sup>−2<sup/> for <i>E<i/>-1-cyano-1,3-butadiene in TMC-1 using GBT data and a line stack technique. At the current level of sensitivity of our data, there is tentative evidence for the presence of the third cyano derivative isomer, 2-cyano-1,3-butadiene, although a firm detection must await more sensitive data. We derive an upper limit to its column density of 3.1 × 10<sup>10<sup/> cm<sup>−2<sup/>. This isomer cannot be formed in the reaction between CN and 1,3-butadiene, according to experimental and theoretical studies, and thus we speculate whether it could arise from neutral-neutral reactions, such as C<sub>2<sub/> H<sub>3<sub/>+CH<sub>2<sub/> CHCN and CH<sub>2<sub/> CCN+C<sub>2<sub/> H<sub>4<sub/>. From the upper limit on the abundance of 1-cyano-1,3-butadiene derived here, we estimate that the abundance of 1,3-butadiene in TMC-1 is below 10<sup>−11<sup/>−10<sup>−10<sup/> relative to H<sub>2<sub/>. The low abundance inferred for 1,3-butadiene makes it unlikely that it plays an important role in bottom-up routes to cyclopentadiene and benzene.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"17 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933496","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Understanding the baryon cycle: Fueling star formation via inflows in Milky Way-like galaxies","authors":"Filippo Barbani, Raffaele Pascale, Federico Marinacci, Paul Torrey, Laura V. Sales, Hui Li, Mark Vogelsberger","doi":"10.1051/0004-6361/202452608","DOIUrl":"https://doi.org/10.1051/0004-6361/202452608","url":null,"abstract":"<i>Context.<i/> Galaxies are not isolated systems, as they interact with their surroundings throughout their lifetimes by both ejecting gas via stellar feedback and accreting gas from their environment. Understanding the interplay between the gas ejected from the disc and the circumgalactic medium (CGM) is crucial to learning how star-forming galaxies evolve.<i>Aims.<i/> Our goal is to understand how gas in the CGM is accreted onto the inner regions of the star-forming disc, making it available for the formation of new stars. Specifically, we explore the connection between stellar feedback and gas accretion from the CGM in Milky Way-like galaxies, aiming to unveil the complex mechanisms driving the evolution of star-forming galaxies. We focus on the distribution of vertical and radial gas flows to and from the disc as a function of galactocentric radius and examine the implications of these processes for the evolution of such galaxies.<i>Methods.<i/> We used the moving-mesh code AREPO coupled with the <i>SMUGGLE<i/> sub-grid model to perform hydrodynamic <i>N<i/>-body simulations of nine different galaxies surrounded by a hot (<i>T<i/> ∼ 10<sup>6<sup/> K) CGM (also called galactic corona). Each simulation has a different structure of the gaseous disc in terms of mass and scale length, which allows us to study how the dynamics of the gas can be affected by disc structure.<i>Results.<i/> We find evidence of a crucial link between stellar feedback processes and gas accretion from the CGM, which collectively play an essential role in sustaining ongoing star formation in the disc. In particular, the ejection of gas from the plane of the disc by stellar feedback leads to the generation of a baryon cycle where the CGM gas is preferentially accreted onto the external regions of the disc (≈3 − 10 M<sub>⊙<sub/> yr<sup>−1<sup/> of gas is accreted into the entire disc). From these regions, it is then transported to the centre with radial mass rates of ≈1 − 4 M<sub>⊙<sub/> yr<sup>−1<sup/> on average, owing to angular momentum conservation. It then leads to the formation of new stars and restarts the whole cycle. We find that both vertical accretion onto the inner regions of the disc and the radial transport of gas from the disc outskirts are necessary to sustain star formation.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"119 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933498","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Three-dimensional non-LTE radiative transfer effects in Fe I lines","authors":"R. Holzreuter, H. N. Smitha, S. K. Solanki","doi":"10.1051/0004-6361/202553965","DOIUrl":"https://doi.org/10.1051/0004-6361/202553965","url":null,"abstract":"<i>Context.<i/> In the first three papers of this series, we investigated the formation of photospheric neutral iron lines in different atmospheres ranging from idealized flux tube models to complex three-dimensional magneto-hydrodynamic (3D MHD) simulations. The overarching goal was to understand the role of non-local thermodynamic equilibrium (NLTE) and horizontal radiative transfer (RT) effects in the formation of these lines.<i>Aims.<i/> In the present paper, we extend this investigation using a high-resolution MHD simulation, with a grid spacing much smaller than the scales currently resolvable by telescopes. We aim to understand whether the horizontal RT effects imposes an intrinsic limit on the small-scale structures that can be observed by telescopes, by spatially smearing out these structures in the solar atmosphere.<i>Methods.<i/> We synthesized the Stokes profiles of two iron line pairs, one at 525 nm and other at 630 nm in 3D NLTE. We compared our results with the ones in previous papers and checked the impact of horizontal transfer on the quality of the images.<i>Results.<i/> Our results with the high-resolution simulations align with the ones inferred from lower-resolution simulations in the previous papers of this series. The spatial smearing due to horizontal RT, although present, is quite small. The degradation caused by the point spread function of a telescope is much stronger.<i>Conclusions.<i/> In the photospheric layers, we do not see an image degradation caused by horizontal RT that is large enough to smear out the small-scale structures in the simulation box. The current generation of telescopes with spatial resolutions smaller than the horizontal photon mean free path should in principle be able to observe the small-scale structures, at least in the photosphere.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933450","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Neutrinos from stochastic acceleration in black hole environments","authors":"Martin Lemoine, Frank Rieger","doi":"10.1051/0004-6361/202453296","DOIUrl":"https://doi.org/10.1051/0004-6361/202453296","url":null,"abstract":"Recent experimental results from the IceCube detector and their phenomenological interpretation suggest that the magnetized turbulent corona of nearby X-ray luminous Seyfert galaxies can produce ∼1 − 10 TeV neutrinos via photo-hadronic interactions. We investigate the physics of stochastic acceleration in these environments in detail and examine the conditions under which the inferred proton spectrum can be explained. To this end, we used recent findings on particle acceleration in turbulence and paid particular attention to the transport equation, notably for transport in momentum space, turbulent transport outside of the corona, and advection through the corona. We first remark that the spectra we obtained are highly sensitive to the value of the acceleration rate, for instance, to the Alfvénic velocity. Then, we examined three prototype scenarios, one scenario of turbulent acceleration in the test-particle picture, another scenario in which particles were preaccelerated by turbulence and further energized by shear acceleration, and a final scenario in which we considered the effect of particle backreaction on the turbulence (damping), which self-regulates the acceleration process. We show that it is possible to obtain satisfactory fits to the inferred proton spectrum in all three cases, but we stress that in the first two scenarios, the energy content in suprathermal protons has to be fixed in an ad hoc manner to match the inferred spectrum at an energy density close to that contained in the turbulence. Interestingly, self-regulated acceleration by turbulence damping naturally brings the suprathermal particle energy content close to that of the turbulence and allowed us to reproduce the inferred flux level without additional fine-tuning. We also suggest that based on the strong sensitivity of the highest proton energy to the Alfvénic velocity (or acceleration rate), any variation in this quantity in the corona might affect (and in fact, set) the slope of the high-energy proton spectrum.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"5 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933456","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Volume-limited sample of low-mass red giant stars, the progenitors of hot subdwarf stars","authors":"Diego Benitez-Palacios, Murat Uzundag, Maja Vučković, Eduardo Arancibia-Rojas, Alex Durán-Reyes, Joris Vos, Alexey Bobrick, Mónica Zorotovic, Matías I. Jones","doi":"10.1051/0004-6361/202452782","DOIUrl":"https://doi.org/10.1051/0004-6361/202452782","url":null,"abstract":"<i>Context.<i/> Binary hot subdwarf B (sdB) stars are typically produced from low-mass red giant branch (RGB) stars that have lost almost all their envelopes through binary mass transfer while still fusing helium in their cores. Particularly, when a low-mass red giant enters stable Roche lobe overflow (RLOF) mass transfer near the tip of the RGB, a long-period sdB binary may be formed.<i>Aims.<i/> We aim to extend our previous volume-limited sample of 211 stars within 200 pc, a homogeneous sample of low-mass red giants, predicted progenitors of wide sdB binaries, to 500 pc and validate it. Additionally, our goal is to provide the distribution of stellar parameters for these stars.<i>Methods.<i/> We refined our original 500 pc sample by incorporating Gaia DR3 parallax values and interstellar extinction measurements. Next, we collected multi-epoch high-resolution spectra for 230 stars in the volume-limited sample using the CORALIE échelle spectrograph from 2019 to 2023. To confirm or discard binarity, we combined astrometric parameters from Gaia with the resulting radial velocity variations. We derived the distribution of stellar parameters using evolutionary models and employed the equivalent evolutionary phase to verify the evolutionary stage of the stars in our sample. Finally, we compared our stellar parameters with the literature.<i>Results.<i/> The derived stellar parameters confirmed that 82% of stars in our sample are indeed in the RGB phase, while 18% are red clump (RC) contaminants. This was expected due to the overlapping of RGB and RC stars in the colour-magnitude diagram. Additionally, 75% of the confirmed RGB stars have a high probability of being part of a binary system. Comparison with the literature shows good overall agreement with a scatter ≲15% in stellar parameters, while the masses show somewhat higher dispersion (∼20%).<i>Conclusions.<i/> We have obtained the most complete volume-limited sample of binary RGB star candidates within 500 pc. These systems are likely progenitors of hot subdwarfs and other classes of stripped helium stars.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"108 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143927308","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cosmological measurement of the gravitational constant G using the CMB, BAO, and BBN","authors":"B. Lamine, Y. Ozdalkiran, L. Mirouze, F. Erdogan, S. Ilic, I. Tutusaus, R. Kou, A. Blanchard","doi":"10.1051/0004-6361/202451602","DOIUrl":"https://doi.org/10.1051/0004-6361/202451602","url":null,"abstract":"Recent cosmological observations have provided numerous new observations with an increasing level of precision, ushering in an era of precision cosmology. The exquisite quality of these observations opens up new possibilities in terms of measuring fundamental constants with good precision on scales that are complementary to laboratory references. In particular, the cosmic microwave background (CMB) temperature and polarisation spectra contain a wealth of information that goes well beyond the basic cosmological parameters. In this paper, we update the precision on a cosmological determination of the gravitational constant, <i>G<i/>, by using the latest Planck data release (PR4) in combination with the latest baryon acoustic oscillation (BAO) from the Dark Energy Spectroscopic Instrument (DESI) data release 1 and the BBN prior on the primordial helium fraction. We demonstrate a precision of 1.8%, corresponding to a ∼40% improvement with regard to previous results in the literature. This is comparable to the level achieved by Cavendish in 1873 using a torsion balance. However, it is a complementary measurement because it has been obtained under wildly different physical environments compared to laboratory results or even studies of the very nearby Universe. Our analysis takes into account the modification of the primordial helium fraction predicted by Big Bang nucleosynthesis (BBN), induced by a variation in <i>G<i/>. We also point out the importance of the polarisation data in attaining the ultimate level of precision. In particular, we discuss the constraints that can be obtained by considering either the low-<i>ℓ<i/> or the high-<i>ℓ<i/> part of the spectra. Within the ΛCDM model, we find <i>G<i/> = (6.75 ± 0.12)×10<sup>−11<sup/> <i>m<i/><sup>3<sup/> <i>kg<i/><sup>−1<sup/> <i>s<i/><sup>−2<sup/>. This measurement is compatible with laboratory results within one standard deviation. Finally, we show that this cosmological measurement of <i>G<i/> is robust against several assumptions made on the cosmological model, particularly when considering a non-standard dark energy fluid or non-flat models.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"56 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143927309","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Are quasars reliable standard candles?","authors":"E. Lusso, G. Risaliti, E. Nardini","doi":"10.1051/0004-6361/202453504","DOIUrl":"https://doi.org/10.1051/0004-6361/202453504","url":null,"abstract":"In this paper, we address the question of whether the non-linear relation between the X-ray and UV emission of quasars can be used to derive their distances. In previous works of our group, we demonstrated that such a relation does not show any redshift evolution in its slope. The derived distances are in agreement with the concordance (standard) model of cosmology up to <i>z<i/> ∼ 1.5, but they show significant deviations at higher redshifts. Yet, several authors have suggested that this discrepancy is due to inconsistencies between the low- and high-redshift sources within the parent sample, or to a redshift evolution of the relation. Here, we discuss these issues through a quantitative comparison with supernova-derived distances in the common redshift range, complemented by simulations showing that all the claimed inconsistencies would naturally arise from any limitation of the cosmological model adopted for the data analysis; that is, from our ignorance of the “true” cosmology. We argue that the reliability of the method can only be based on a cosmology-independent evaluation of the hypothesis of the non-evolution of the X-ray to UV relation at <i>z<i/> > 1.5, subsequent to a careful check of the sample selection and of the flux measurements for possible redshift-dependent systematic effects. Since we cannot conceive of any physical reason for a sudden change in the normalisation of the relation at <i>z<i/> > 1.5, and we can exclude any severe systematic effect in the data selection and flux measurements, we conclude that the application of the X-ray to UV relation to cosmology is well motivated. To further strengthen this point, we need to achieve a better understanding of the physical process behind the observed relation and/or an independent observational proof possibly confirming the discrepancy with ΛCDM found with quasars, such as future supernova measurements at <i>z<i/> ∼ 2 or higher.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"36 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143927346","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Analysing the evolution of the thermal and magnetic properties of an X-class flare in the low solar atmosphere","authors":"F. Ferrente, C. Quintero Noda, F. Zuccarello, S. L. Guglielmino","doi":"10.1051/0004-6361/202451875","DOIUrl":"https://doi.org/10.1051/0004-6361/202451875","url":null,"abstract":"We analysed the evolution of the spatial distribution and stratification of the physical parameters of the atmosphere of an X-class flare in the photosphere and chromosphere. We analysed the full Stokes vector of the Fe I 617.3 nm and Ca II 854.2 nm transitions recorded by the Interferometric Bidimensional Spectropolarimeter instrument on the 22 October 2014. We used the DeSIRe code to infer the atmospheric parameters at photospheric and chromospheric layers over the observed field of view and the entire time series spanning more than one hour. Our findings reveal that at the beginning of the observing run right after the flare peak, the chromosphere is characterised by temperature enhancements and strong upflows in the flare ribbon area, indicating that the flaring event produces hot material moving outwards from the Sun. The temperature enhancements and strong upflows decrease in amplitude and area occupied for subsequent snapshots, signalling that the flare activity is slowly and continuously fading. Concerning the magnetic field vector, we observe the presence of large-scale mixed polarities in the regions where the flare ribbon was located which do not change abruptly with time, in contrast with the high-temperature areas. Thus, it seems that the time series covered here reveals that the post-flare activity diminishes with time with no re-appearance of heating sources or any other thermal or magnetic activity; that is, the presence and traces of flaring activity fade away without significant restructuring of the low atmosphere in this confined flare event.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"10 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143927342","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Power spectrum of the CODEX clusters","authors":"V. Lindholm, A. Finoguenov, A. Balaguera-Antolínez, T. Castro","doi":"10.1051/0004-6361/202453402","DOIUrl":"https://doi.org/10.1051/0004-6361/202453402","url":null,"abstract":"<i>Aims.<i/> We analyze the clustering of galaxy clusters in a large contiguous sample, the Constrain Dark Energy with X-ray (CODEX) sample. We construct a likelihood for cosmological parameters by comparing the measured clustering signal and a theoretical prediction, and use this to obtain parameter constraints.<i>Methods.<i/> We measured the three multipole moments (monopole, quadrupole, and hexadecapole, <i>ℓ<i/> = 0, 2, 4) of the power spectrum of a subset of the CODEX clusters. To fully model cluster clustering, we also determined the expected clustering bias of the sample using estimates for the cluster masses and a mass-to-bias model calibrated using <i>N<i/>-body simulations. We estimated the covariance matrix of the measured power spectrum multipoles using a set of simulated dark-matter halo catalogs. Combining all these ingredients, we performed a Markov chain Monte Carlo sampling of cosmological parameters Ω<sub>m<sub/> and <i>σ<i/><sub>8<sub/> to obtain their posterior.<i>Results.<i/> We found the CODEX clustering signal to be consistent with an earlier X-ray selected cluster sample, the REFLEX II sample. We also found that the measured power spectrum multipoles are compatible with the predicted, bias-scaled linear matter power spectrum when the cosmological parameters determined by the Planck satellite are assumed. Furthermore, we found the marginalized parameter constraints of and . The full 2D posterior is consistent, for example, with the Planck cosmology within the 68% confidence region.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"61 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143927343","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Can primordial black holes explain the overabundance of bright super-early galaxies?","authors":"Antonio Matteri, Andrea Pallottini, Andrea Ferrara","doi":"10.1051/0004-6361/202553701","DOIUrl":"https://doi.org/10.1051/0004-6361/202553701","url":null,"abstract":"The James Webb Space Telescope (JWST) is detecting an excess of high-redshift (<i>z<i/> ≳ 10) bright galaxies that challenge most theoretical predictions. To address this issue, we investigated the impact of primordial black holes (PBHs) on the halo mass function and UV luminosity function (LF) of super-early galaxies. We explored two key effects: (i) The enhancement of the massive halo abundance due to the compact nature and spatial distribution of PBHs, and (ii) the luminosity boost, characterized by the Eddington ratio <i>λ<i/><sub>E<sub/>, caused by active galactic nuclei (AGN) that are powered by matter accretion onto PBHs. We built an effective model, calibrated using data at lower redshifts (<i>z<i/> ≈ 4 − 9), to derive the evolution of the LF, including the additional PBH contribution. A Bayesian analysis yielded the following results: (a) Although a small fraction (log <i>f<i/><sub>PBH<sub/> ≈ −5.42) of massive (log <i>M<i/><sub>PBH<sub/>/M<sub>⊙<sub/> ≈ 8.37) nonemitting (<i>λ<i/><sub>E<sub/> = 0) PBHs can explain the galaxy excess via the halo abundance enhancement, this solution is excluded by cosmic microwave background <i>μ<i/>-distortion constraints on monochromatic PBHs. (b) If PBHs power an AGN that emits at super-Eddington luminosity (<i>λ<i/><sub>E<sub/> ≈ 10), the observed LF can be reproduced by a PBH population with a characteristic mass log <i>M<i/><sub>PBH<sub/>/M<sub>⊙<sub/> ≈ 3.69, constituting a tiny (log <i>f<i/><sub>PBH<sub/> ≈ −8.16) fraction of the cosmic dark matter content. In the AGN scenario, about 75% of the observed galaxies with <i>M<i/><sub>UV<sub/> = −21 at <i>z<i/> = 11 should host a PBH-powered AGN and typically reside in low-mass halos, <i>M<i/><sub>h<sub/> = 10<sup>8 − 9<sup/> M<sub>⊙<sub/>. These predictions can be tested with available and forthcoming JWST spectroscopic data. We note that our analysis considered a lognormal PBH mass function and compared its parameters with monochromatic limits on the PBH abundance. Further work is required to relax these limitations.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"16 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143920824","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}