Astronomy & Astrophysics最新文献

{"title":"Accuracy of the ‘tip of the red giant branch’ distance determination method","authors":"Vladas Vansevičius","doi":"10.1051/0004-6361/202554442","DOIUrl":"https://doi.org/10.1051/0004-6361/202554442","url":null,"abstract":"<i>Context.<i/> To solve the so-called Hubble tension problem, highly accurate methods of determining extragalactic distances are needed. Therefore, the accuracy and applicability of the tip of the red giant branch (TRGB) method is of the utmost importance.<i>Aims.<i/> In this work, we aim to study variations in the TRGB versus radial distance and location in the M 33 galaxy disc.<i>Methods.<i/> We used colour-magnitude diagrams of stars from the M 33 Subaru Suprime-Cam stellar photometry catalogue (<i>V<i/> and <i>I<i/>-passbands of the Johnson-Cousins system) to test the accuracy and robustness of the TRGB method in determining extragalactic distances.<i>Results.<i/> We derived radial (metallicity) and azimuthal (galaxy inclination) variations in the TRGB magnitude (<i>I<i/><sup>TRGB<sup/>). We find the <i>I<i/><sup>TRGB<sup/> = 20.638 ± 0.008 magnitude to be virtually constant over the radial distance from 7 to 11 kpc. Assuming the absolute TRGB magnitude, <i>M<i/><sub><i>I<i/><sub/><sup>TRGB<sup/> = −4.05, and foreground extinction, <i>A<i/><sub><i>I<i/><sub/> = 0.062, we derived the true distance modulus of the M 33 galaxy to be (<i>I<i/><sup>TRGB<sup/> − <i>M<i/><sub><i>I<i/><sub/><sup>TRGB<sup/>)<sub>0<sub/> = 24.626 ± 0.008<sub>stat<sub/> (∼842 kpc).<i>Conclusions.<i/> We demonstrate the ability of the TRGB method to discern the distance difference between the proximal and distal parts of the galaxy disc, which is ∼1.3% of the distance to M 33. We show that the TRGB method is highly accurate and can be reliably applied to the red giant branch star populations of a low metallicity ([Fe/H] ≲ −1.3). With a slightly lower accuracy, it can also be applied in cases of higher metallicity, which is more common for numerous low-mass spiral galaxies.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"5 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143980024","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":"Fine-scale opposite-polarity magnetic fields in a solar plage revealed by integral field spectropolarimetry","authors":"G. Liu, I. Milić, J. S. Castellanos Durán, J. M. Borrero, M. van Noort, C. Kuckein","doi":"10.1051/0004-6361/202554498","DOIUrl":"https://doi.org/10.1051/0004-6361/202554498","url":null,"abstract":"<i>Context.<i/> Plages are small concentrations of strong, nearly vertical magnetic fields in the solar photosphere that expand with height. A high spatial and spectral resolution that can resolve their fine structure is required to characterize them, and spectropolarimetric capabilities are needed to infer their magnetic fields.<i>Aims.<i/> We constrain the 3D fine structure of the magnetic field in the photosphere of a solar plage from a unique spectropolarimetric dataset with a very high spatial and spectral resolution and a fast temporal cadence.<i>Methods.<i/> We analyzed spectropolarimetric observations of a solar plage in the two magnetically sensitive spectral lines of neutral iron around 630 nm. The observations were obtained with MiHI, which is an integral field unit attached to the Swedish Solar Telescope. MiHI obtained diffraction-limited, high-cadence observations with high spectral fidelity. These observations were interpreted using the spectropolarimetric inversion with magnetohydrostatic constraints, which allowed us to recover the magnetic and thermodynamic structure of the plage on a geometrical scale.<i>Results.<i/> The inversion results reveal that the magnetic field can reach up to 2 kG and that it expands significantly from the deep to the mid-photosphere. Weaker (≈200 G), and very small (subarcsecond) vertical magnetic loops lie beneath this canopy, rooted in the photosphere.<i>Conclusions.<i/> This novel picture of a solar plage, in which weak opposite-polarity field patches surround the main polarity, provides new insight into convection in strongly magnetized plasma.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"40 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143979913","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":"Double-peaked Ca II traces a relativistic broad-line region disk in NGC 4593","authors":"M. W. Ochmann, P. M. Weilbacher, M. A. Probst, W. Kollatschny, D. Chelouche, R. Chini, D. Grupe, M. Haas, S. Kaspi, S. Komossa","doi":"10.1051/0004-6361/202554800","DOIUrl":"https://doi.org/10.1051/0004-6361/202554800","url":null,"abstract":"<i>Context.<i/> Double-peaked emission lines are observed in a small percentage of active galactic nuclei (AGN). These lines allow the determination of fundamental properties of the line-emitting region, known as the broad-line region (BLR).<i>Aims.<i/> We investigated the structure and kinematics of the BLR in the nearby Seyfert galaxy NGC 4593 through an analysis of the near-infrared (NIR) line blend of Ca II<i>λ<i/>8498, <i>λ<i/>8542, <i>λ<i/>8662, and O I<i>λ<i/>8446 observed in a 2019 VLT/MUSE spectrum.<i>Methods.<i/> We performed a detailed decomposition of the NIR Ca II triplet and O I<i>λ<i/>8446 blend, extracting clean profiles of Ca II<i>λ<i/>8498, <i>λ<i/>8542, <i>λ<i/>8662, and O I<i>λ<i/>8446. We then fitted Ca II<i>λ<i/>8662 with a relativistic elliptical line-emitting accretion disk model.<i>Results.<i/> The extracted line profiles are double-peaked with a full width at half maximum (FWHM) of ∼3700 km s<sup>−1<sup/> and exhibit a redward asymmetry with a red-to-blue peak ratio of 4:3. The Ca II triplet lines have an intensity ratio of 1:1:1 and show no evidence of a central narrow or intermediate-width component. The profiles of Ca II and O I are remarkably similar, suggesting a common region of origin. Given the 1:1:1 ratio of the Ca II triplet, this region is likely a high-density emission zone, and the Ca II<i>λ<i/>8662 profile is well described by a mildly eccentric, low-inclination relativistic line-emitting disk with minimal internal turbulence. The profile represents one of the clearest kinematic signatures of a relativistic disk observed in BLR emission lines to date.<i>Conclusions.<i/> The double-peaked profiles of the NIR Ca II triplet and O I<i>λ<i/>8446 in NGC 4593 represent the first detection of double-peaked Ca II and O I<i>λ<i/>8446 in a nontransient AGN spectrum. The minimal intrinsic turbulence (the lowest value reported for an AGN emission line to date) and the absence of narrow or intermediate-width components in Ca II<i>λ<i/>8662 make it a powerful diagnostic tool of BLR structure and kinematics. Further investigations of the profiles of Ca II and O I in other AGN are recommended to better constrain BLR properties and the nature of the underlying accretion flow.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"4 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143979914","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":"Tuning into the spatial frequency space","authors":"J. P. Carvajal, F. E. Bauer, I. Reyes-Jainaga, F. Förster, A. M. Muñoz Arancibia, M. Catelan, P. Sánchez-Sáez, C. Ricci, A. Bayo","doi":"10.1051/0004-6361/202452880","DOIUrl":"https://doi.org/10.1051/0004-6361/202452880","url":null,"abstract":"<i>Context.<i/> A significant challenge in the study of transient astrophysical phenomena is the identification of bogus events, among which human-made Earth-orbiting satellites and debris remain major contaminants. Existing pipelines can effectively identify satellite trails, but they often miss more complex signatures, such as collections of satellite glints. In the Rubin Observatory era, the scale of operations will increase tenfold with respect to its precursor, the <i>Zwicky<i/> Transient Facility (ZTF), requiring crucial improvements in classification purity, data compression for informative alerts, and pipeline speed.<i>Aims.<i/> We explore the use of a 2D Fast Fourier Transform (FFT) on difference images as a tool to improve satellite-detection machine learning algorithms.<i>Methods.<i/> Using the Automatic Learning for the Rapid Classification of Events (ALeRCE) single-stamp classifier as a baseline, we adapted its architecture to receive a cutout of the FFT of the difference image, in addition to the three (science, reference, difference) ZTF image cutouts (hereafter stamps). We explored various stamp sizes and resolutions, assessing the benefits of incorporating FFT images, particularly when data compression is critical due to alert size limitations and pipeline speed constraints (e.g., in large-scale surveys such as the Legacy Survey of Space and Time).<i>Results.<i/> The inclusion of the FFT can significantly improve satellite detection performance. The most notable improvement occurred in the smallest field-of-view model (16″), whose satellite classification accuracy increased from (72.0 ± 2.9)% to (87.8 ± 1.3)% after including the FFT, computed from the full 63″ difference images. This demonstrates the effectiveness of FFT in compressing and extracting relevant large-scale satellite features. However, the FFT alone did not fully match the accuracy achieved by the full 63″, (95.9 ± 1.3)% and multiscale (90.6 ± 0.8)% models, highlighting the complementary importance of contextual spatial information.<i>Conclusions.<i/> We show how FFTs can be leveraged to cull satellite and space debris signatures from alert streams.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"14 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143945740","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":"The nature of Martian plume during solar wind interaction with Mars","authors":"Yuchen Cao, Haoyu Lu, Jinbin Cao, Shibang Li, Yihui Song, Nihan Chen, Jianxuan Wang, Jianing Zhao, Bingzhao Li","doi":"10.1051/0004-6361/202452882","DOIUrl":"https://doi.org/10.1051/0004-6361/202452882","url":null,"abstract":"Investigating the physical mechanism of ion escape on Mars is crucial for comprehending the evolution of Martian space environment. The plume structure located in the +E hemisphere of Mars plays a crucial role in the escape of planetary ions, contributing more than 20 percent to the overall ion escape rate. In this study, a three-dimensional multi-fluid Hall magnetohydrodynamics (MHD) numerical model is utilized to simulate the ion escape process of Mars. A force analysis is conducted to examine the electric field exerted on O<sup>+<sup/> and to investigate the density, velocity, and escape flux of O<sup>+<sup/>. Numerical results indicate that both the convection field and the magnetic force field play essential roles in driving ion escape in the plume region and shaping the morphology of ion escaping fluxes. The plume is positioned above the magnetic pile-up boundary (MPB), as the convection field directed towards the +<i>Z<i/> direction primarily influences the area above the MPB. Furthermore, the Hall field points outward and reaches the peak values at the MPB, while the ambipolar field peaks at the bow shock (BS). In addition, the ions escaping from the plume predominantly originates from the middle and high latitudes of the +E hemisphere on the Martian dayside. The plume escape rate and the tail escape rate are 4.33 × 10<sup>23<sup/> s<sup>−1<sup/> and 1.74 × 10<sup>24<sup/> s<sup>−1<sup/> respectively. The plume escape rate accounts for 24.83% of the tail escape rate and 19.89% of the overall escape rate.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"51 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933453","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":"A multiscale view of the magnetic field morphology in the hot molecular core G31.41+0.31","authors":"C. Y. Law, M. T. Beltrán, R. S. Furuya, J. M. Girart, D. Galli, R. Cesaroni, L. Moscadelli, D. Arzoumanian, A. Lorenzani, M. Padovani, A. Sanna, G. Surcis","doi":"10.1051/0004-6361/202453510","DOIUrl":"https://doi.org/10.1051/0004-6361/202453510","url":null,"abstract":"Multiscale studies of the morphology and strength of the magnetic field are crucial to properly unveil its role and relative importance in high-mass star and cluster formation. G31.41+0.31 (G31) is a hub-filament system that hosts a high-mass protocluster embedded in a hot molecular core (HMC). G31 is one of the few sources showing a clear hourglass morphology of the magnetic field on scales between 1000 au and a few 100 au in previous interferometric observations. This strongly suggests a field-regulated collapse. To complete the study of the magnetic field properties in this high-mass star-forming region, we carried out observations with the James Clerk Maxwell Telescope 850 μm of the polarized dust emission. These observations had a spatial resolution of ∼0.2 pc at 3.75 kpc. The aim was to study the magnetic field in the whole cloud and to compare the magnetic field orientation toward the HMC from ∼50 000 au to ∼260 au scales. The large-scale (∼5 pc) orientation of the magnetic field toward the position of the HMC is consistent with that observed at the core (∼4000 au) and circumstellar (∼260 au) scales. The self-similarity of the magnetic field orientation at these different scales might arise from the brightest sources in the protocluster, whose collapse is dragging the magnetic field. These sources dominate the gravitational potential and the collapse in the HMC. The cloud-scale magnetic field strength of the G31 hub-filament system, which we estimated using the Davis-Chandrasekhar-Fermi method, is in the range 0.04–0.09 mG. The magnetic field orientation in the star-forming region shows a bimodal distribution, and it changes from an NW–SE direction in the north to an E–W direction in the south. The change in the orientation occurs in the close vicinity of the HMC. This favors a scenario of a cloud-cloud collision for the formation of this star-forming region. The different magnetic field orientations would be the remnant of the pristine orientations of the colliding clouds in this scenario.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"2 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933493","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":"X-ray and radio data obtained by XMM-Newton and VLA constrain the stellar wind of the magnetic quasi-Wolf-Rayet star in HD45166","authors":"P. Leto, L. M. Oskinova, T. Shenar, G. A. Wade, S. Owocki, C. S. Buemi, R. Ignace, C. Trigilio, G. Umana, A. ud-Doula, H. Todt, W. -R. Hamann","doi":"10.1051/0004-6361/202452899","DOIUrl":"https://doi.org/10.1051/0004-6361/202452899","url":null,"abstract":"<i>Context.<i/> Recently, a powerful magnetic field was discovered in the hot helium star classified as a quasi-Wolf-Rayet (qWR) star (∼2 M<sub>⊙<sub/>), in the HD 45166 system. Upon its explosion as a core-collapse supernova, it is expected to produce a strongly magnetic neutron star – a magnetar. Among the key parameters that govern pre-supernova evolution is the amount of mass lost via stellar wind. However, the magnetic nature of this helium star is expected to affect its stellar wind, which makes the estimation of the wind parameters uncertain.<i>Aims.<i/> We report the first observations of HD 45166 in X-rays with the <i>XMM-Newton<i/> telescope and in radio with the VLA interferometer array. By placing the observation results in a theoretical framework, we aim to provide a reliable estimate of the wind strength of the magnetic qWR star.<i>Methods.<i/> We explain the X-ray properties in the framework of the magnetically confined wind shock scenario, and we apply the semianalytic model of a dynamical magnetosphere (DM) to reproduce the X-ray emission. We compute the thermal radio emission of the wind and its absorption effect on possible gyro-synchrotron emission from the underlying dipolar magnetosphere, sampled in 3D, by integrating the radiative transfer equation.<i>Results.<i/> We did not detect radio emissions, which enabled us to set sensitive upper limits on the radio luminosity. The magnetic qWR star is a slow rotator, and comparison with models reveals that the possible acceleration mechanisms that occur within its DM are not as efficient as in fast-rotating magnetic ApBp-type stars. In contrast, the system is detected in X-rays with log(<i>L<i/><sub>X<sub/>/<i>L<i/><sub>bol<sub/>)∼−5.6. Using suitable models, we constrain the mass lost from this magnetic quasi-Wolf-Rayet star as <i>Ṁ<i/> ≈ 3 × 10<sup>−10<sup/> M<sub>⊙<sub/> yr<sup>−1<sup/>.<i>Conclusions.<i/> This novel empirical estimate of the mass-loss rate in a ∼2 M<sub>⊙<sub/> helium star confirms that it maintains super-Chandrasekhar mass until collapse and can produce a magnetar as its final evolutionary product.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"38 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933495","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":"Improving the spatial resolution of SDO/HMI transverse and line-of-sight magnetograms using GST/NIRIS data with machine learning","authors":"Chunhui Xu, Yan Xu, Jason T. L. Wang, Qin Li, Haimin Wang","doi":"10.1051/0004-6361/202453581","DOIUrl":"https://doi.org/10.1051/0004-6361/202453581","url":null,"abstract":"<i>Context.<i/> High-resolution magnetograms are crucial for studying solar flare dynamics because they enable the precise tracking of magnetic structures and rapid field changes. The Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory (SDO/HMI) has been an essential provider of vector magnetograms. However, the spatial resolution of the HMI magnetograms is limited and hence is not able to capture the fine structures that are essential for understanding flare precursors. The Near InfraRed Imaging Spectropolarimeter on the 1.6 m Goode Solar Telescope (GST/NIRIS) at Big Bear Solar Observatory (BBSO) provides a better spatial resolution and is therefore more suitable to track the fine magnetic features and their connection to flare precursors.<i>Aims.<i/> We propose DeepHMI, a machine-learning method for solar image super-resolution, to enhance the transverse and line-of-sight magnetograms of solar active regions (ARs) collected by SDO/HMI to better capture the fine-scale magnetic structures that are crucial for understanding solar flare dynamics. The enhanced HMI magnetograms can also be used to study spicules, sunspot light bridges and magnetic outbreaks, for which high-resolution data are essential.<i>Methods.<i/> DeepHMI employs a conditional diffusion model that is trained using ground-truth images obtained by an inversion analysis of Stokes measurements collected by GST/NIRIS.<i>Results.<i/> Our experiments show that DeepHMI performs better than the commonly used bicubic interpolation method in terms of four evaluation metrics. In addition, we demonstrate the ability of DeepHMI through a case study of the enhancement of SDO/HMI transverse and line-of-sight magnetograms of AR 12371 to GST/NIRIS data.","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":"143933497","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":"Broad-band noises in GX 339-4 during the 2021 outburst observed with Insight-HXMT and NICER","authors":"Yong-Jie Jin, Xiao Chen, Hai-Fan Zhu, Ze-Jun Jiang, Wei Wang","doi":"10.1051/0004-6361/202453494","DOIUrl":"https://doi.org/10.1051/0004-6361/202453494","url":null,"abstract":"Rapid X-ray variability of GX 339−4 including the low-frequency quasi-periodic oscillations (LFQPOs) and broad-band noises were observed with the Hard X-ray Modulation Telescope (Insight-HXMT) and Neutron star Interior Composition Explorer (NICER) during the 2021 outburst. Here we present a systematic study of the evolution and energy dependence properties of such broad-band noises (BBNs). The outburst from February to March of 2021 can be divided into three stages: the low hard state (LHS), the hard intermediate state (HIMS), and soft intermediate state (SIMS). In the PDSs of the LHS and HIMS, the broad-band noises were well fitted with three Lorentzian components: a low-frequency component <i>L<i/><sub>1<sub/>, a middle-frequency component <i>L<i/><sub>2<sub/>, and a high-frequency component <i>L<i/><sub>3<sub/>. The increasing trend of the characteristic frequencies for <i>L<i/><sub>1<sub/> and <i>L<i/><sub>2<sub/> and the relation between the QPO frequency and characteristic BBN frequency are reported. We find that the energies corresponding to the peaks and shapes of the rms spectra for three BBN components are different. The comparison among three BBN components indicates that energy-dominant bands of these BBN components are distinct. Our results can be explained with the truncated disc and hot flow model with a large variable disc and a small hot inner flow. A possible description of the accretion structure and its evolution from the LHS to the SIMS is proposed. Further research is still required to probe such an accretion structure in GX 339-4.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"67 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933451","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":"The CIELO project: The chemo-dynamical properties of galaxies and the cosmic web","authors":"Patricia B. Tissera, Lucas Bignone, Jenny Gonzalez-Jara, Ignacio Muñoz-Escobar, Pedro Cataldi, Valentina P. Miranda, Daniela Barrientos-Acevedo, Brian Tapia-Contreras, Susana Pedrosa, Nelson Padilla, Rosa Dominguez-Tenreiro, Catalina Casanueva-Villarreal, Emanuel Sillero, Benjamin Silva-Mella, Isha Shailesh, Francisco Jara-Ferreira","doi":"10.1051/0004-6361/202453348","DOIUrl":"https://doi.org/10.1051/0004-6361/202453348","url":null,"abstract":"<i>Context.<i/> The CIELO project introduces a novel set of chemo-dynamical zoom-in simulations, designed to simultaneously resolve galaxies and their nearby environments. The initial conditions (ICs) encompass a diverse range of cosmic structures, including local groups, filaments, voids, and walls, enabling a detailed exploration of galaxies within their broader cosmic web context.<i>Aims.<i/> This study aims to present the ICs and characterise the global properties of CIELO galaxies and their environments. Specifically, it focuses on galaxies with stellar masses ranging from 10<sup>8<sup/> to 10<sup>11<sup/> M<sub>⊙<sub/> and investigates key scaling relations, such as the mass-size relation, the Tully-Fisher relation (TFR), and the mass-metallicity relation (MZR) for both stars and star-forming gas.<i>Methods.<i/> We employed the DisPerSe algorithm to determine the positions of CIELO galaxies within the cosmic web, with a particular focus on the Pehuen haloes. The selection of Local Group (LG) type volumes was guided by criteria based on relative positions and velocities of the two primary galaxies. The Pehuen regions were selected to map walls, filaments and voids. Synthetic SDSS i, r, and g band images were generated using the SKIRT radiative transfer code. Furthermore, a dynamical decomposition was performed to classify galaxy morphologies into bulge, disc, and stellar halo components.<i>Results.<i/> The CIELO galaxies exhibit stellar-to-dark matter fractions consistent with both observational data and other simulation results. These galaxies align with expected scaling relations, such as the mass-size relation and TFR, indicating effective regulation of star formation and feedback processes. The mass-size relation reveals the expected dependence on galaxy morphology. The gas and stellar MZRs also agree well with observational data, with the stellar MZR displaying strong correlations with galaxy size (R<sub>hm<sub/>) and star formation rate (SFR). This indicates that smaller, less star-forming galaxies tend to have higher metallicities. Future investigations will delve into the chemo-dynamical properties of bulges, discs, and stellar haloes, exploring their connections to assembly histories and positions within the cosmic web.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"28 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143933494","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}