The Astrophysical Journal最新文献

Polarization Estimation for Radio Pulsars

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adb7e1

M. M. McKinnon

引用次数: 0

Linking Stellar Populations to H ii Regions across Nearby Galaxies. II. Infrared Reprocessed and UV Direct Radiation Pressure in H ii Regions

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adb484

Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Ashley. T. Barnes, Daniel A. Dale, Ian Blackstone, Simon C. O. Glover, Shyam H. Menon, Jessica Sutter, Thomas G. Williams, Dalya Baron, Francesco Belfiore, Frank Bigiel, Alberto D. Bolatto, Médéric Boquien, Rupali Chandar, Mélanie Chevance, Ryan Chown, Kathryn Grasha, Brent Groves, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Erik Rosolowsky, Karin Sandstrom, Sumit K. Sarbadhicary, Jiayi Sun and Leonardo Úbeda

{"title":"Linking Stellar Populations to H ii Regions across Nearby Galaxies. II. Infrared Reprocessed and UV Direct Radiation Pressure in H ii Regions","authors":"Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Ashley. T. Barnes, Daniel A. Dale, Ian Blackstone, Simon C. O. Glover, Shyam H. Menon, Jessica Sutter, Thomas G. Williams, Dalya Baron, Francesco Belfiore, Frank Bigiel, Alberto D. Bolatto, Médéric Boquien, Rupali Chandar, Mélanie Chevance, Ryan Chown, Kathryn Grasha, Brent Groves, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Erik Rosolowsky, Karin Sandstrom, Sumit K. Sarbadhicary, Jiayi Sun and Leonardo Úbeda","doi":"10.3847/1538-4357/adb484","DOIUrl":"https://doi.org/10.3847/1538-4357/adb484","url":null,"abstract":"Radiation pressure is a key mechanism by which stellar feedback disrupts molecular clouds and drives H ii region expansion. This includes direct radiation pressure exerted by UV photons on dust grains, pressure associated with photoionization, and infrared (IR) radiation pressure on grains due to dust-reprocessed IR photons. We present a new method that combines high-resolution mid-IR luminosities from JWST-MIRI, optical attenuation, and nebular line measurements from the Very Large Telecope Multi-Unit Spectroscopic Explorer (VLT-MUSE), and the Hubble Space Telescope (HST) Hα-based region sizes to estimate the strength of radiation pressure in ≈18,000 H ii regions across 19 nearby star-forming galaxies. This is the most extensive and direct estimate of these terms beyond the Local Group to date. In the disks of galaxies, we find that the total reprocessed IR pressure is on average 5% of the direct UV radiation pressure. This fraction rises to 10% in galaxy centers. We expect reprocessed IR radiation pressure to dominate over UV radiation pressure in regions where . Radiation pressure due to H ionizations is lower than pressure on dust in our sample, but appears likely to dominate the radiation pressure budget in dwarf galaxies similar to the Small Magellanic Cloud. The contribution from all radiation pressure terms appears to be subdominant compared to thermal pressure from ionized gas, reinforcing the view that radiation pressure is most important in compact, heavily embedded, and young regions.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"93 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695450","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Observations and Radiative Transfer Simulations of the Carbon-rich AGB Star V Oph with VLTI/MATISSE*

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adb7e2

Jon Hulberg, Gioia Rau and Markus Wittkowski

{"title":"Observations and Radiative Transfer Simulations of the Carbon-rich AGB Star V Oph with VLTI/MATISSE*","authors":"Jon Hulberg, Gioia Rau and Markus Wittkowski","doi":"10.3847/1538-4357/adb7e2","DOIUrl":"https://doi.org/10.3847/1538-4357/adb7e2","url":null,"abstract":"Carbon-rich asymptotic giant branch (AGB) stars are among the most important contributors of enriched materials to the interstellar medium due to their strong stellar winds. To fully characterize mass loss on the AGB, it is necessary to determine the distributions of dust and gas around the stars, where the dust begins to condense from the gas, and how this extended atmospheric structure evolves over the pulsational period of the star. We present an analysis of L-band (2.8–4.2 μm) interferometric observations of the carbon-rich AGB star V Oph made with the MATISSE instrument at the Very Large Telescope Interferometer at the maximum and minimum of the star’s visual light curve. Using the radiative transfer software RADMC-3D, we model the circumstellar dust shell, and find stellar radii of 395 and 495R⊙ at the two phases, and dust radii of 790 and 742.5R⊙ at the two epochs, respectively. By adding C2H2 and HCN gas to the RADMC-3D models, we are able to fit the visibility spectra well, with some deviations at the 3.11 μm feature. Reasons for this deviation and interpretation of the best fitting models are discussed in the text, and we discuss motivations for follow-up imaging observations of V Oph.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"61 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695513","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Life and Times of Star-forming Cores: An Analysis of Dense Gas in the STARFORGE Simulations

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adb71d

Stella S. R. Offner, Josh Taylor and Michael Y. Grudíc

{"title":"The Life and Times of Star-forming Cores: An Analysis of Dense Gas in the STARFORGE Simulations","authors":"Stella S. R. Offner, Josh Taylor and Michael Y. Grudíc","doi":"10.3847/1538-4357/adb71d","DOIUrl":"https://doi.org/10.3847/1538-4357/adb71d","url":null,"abstract":"Dense gas in molecular clouds is an important signature of ongoing and future star formation. We identify and track dense cores in the starforge simulations, following the core evolution from birth through dispersal by stellar feedback for typical Milky Way cloud conditions. Only ∼8% of cores host protostars, and most disperse before forming stars. The median starless and protostellar core lifetimes are ∼0.5–0.6 Myr and ∼0.8–1.1 Myr, respectively, where the protostellar phase lasts Myr. While core evolution is stochastic, we find that virial ratios and line widths decline in prestellar cores, coincident with turbulent decay. Collapse occurs over ∼0.1 Myr, once the central density exceeds ≳106 cm−3. Starless cores, only, follow line-width–size and mass–size relations, σ ∝ R0.3 and M ∝ R1. The core median mass, radius, and velocity dispersion scale weakly with the cloud magnetic field strength. We cluster the core properties and find that protostellar cores have >80% likelihood of belonging to three particular groups that are characterized by high central densities, compact radii, and lower virial parameters. Overall, core evolution appears to be universally set by the interplay of gravity and magnetized turbulence, while stellar feedback dictates protostellar core properties and sets the protostellar phase lifetime.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695451","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Can Neutron Star Tidal Effects Obscure Deviations from General Relativity?

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adb966

Stephanie M. Brown, Badri Krishnan, Rahul Somasundaram and Ingo Tews

{"title":"Can Neutron Star Tidal Effects Obscure Deviations from General Relativity?","authors":"Stephanie M. Brown, Badri Krishnan, Rahul Somasundaram and Ingo Tews","doi":"10.3847/1538-4357/adb966","DOIUrl":"https://doi.org/10.3847/1538-4357/adb966","url":null,"abstract":"One of the main goals of gravitational-wave astrophysics is to study gravity in the strong-field regime and constrain deviations from general relativity (GR). Any such deviation affects not only binary dynamics and gravitational-wave emission but also the structure and tidal properties of compact objects. In the case of neutron stars, masses, radii, and tidal deformabilities can all differ significantly between different theories of gravity. Currently, the measurement uncertainties in neutron star radii and tidal deformabilities are quite large. However, much less is known about how the large uncertainty in the nuclear equation of state (EOS) might affect tests of GR using binary neutron star mergers. Conversely, using the wrong theory of gravity might lead to incorrect constraints on the nuclear EOS. Here, we study this problem within scalar–tensor (ST) theory. We apply the recently derived ℓ = 2 tidal Love numbers in this theory to parameter estimation of GW170817. Correspondingly, we test if physics beyond GR could bias measurements of the nuclear EOS and neutron star radii. We find that parameter inference for both the GR and ST cases returns consistent component masses and tidal deformabilities. The radius and the EOS posteriors, however, differ between the two theories, but neither is excluded by current observational limits. This indicates that measurements of the nuclear EOS may be biased and that deviations from GR could go undetected when analyzing current binary neutron star mergers.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"215 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695514","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

SDSS-IV MaNGA: Spatial Evolution of Gas-phase Metallicity Changes Induced by Galaxy Interactions

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adbbd2

Hsi-An Pan, 璽安潘, Lihwai Lin, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros and Bau-Ching Hsieh

{"title":"SDSS-IV MaNGA: Spatial Evolution of Gas-phase Metallicity Changes Induced by Galaxy Interactions","authors":"Hsi-An Pan, 璽安潘, Lihwai Lin, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros and Bau-Ching Hsieh","doi":"10.3847/1538-4357/adbbd2","DOIUrl":"https://doi.org/10.3847/1538-4357/adbbd2","url":null,"abstract":"Gas-phase metallicity in interacting and merging galaxies offers key insights into their star formation processes and evolutionary histories. This study investigates the spatial evolution of gas-phase metallicity (i.e., oxygen abundance, 12 + log(O/H)) in these galaxies using integral field unit data from the SDSS-IV MaNGA survey, focusing on changes in metallicity gradients across different stages of interactions—from early encounters to final coalescence. By comparing interacting and merging galaxies with isolated counterparts, we identify characteristic trends in how interactions influence metallicity gradients over time. Our analysis reveals that metallicity gradients typically flatten shortly after the first pericenter passage, likely due to radial gas mixing, with later stages showing either metallicity enrichment or dilution depending on the intensity of the interaction and star formation activity. These changes can result in gradients that are either flatter or steeper than the initial profiles. Notably, we observe steeper metallicity gradients in interacting galaxies at certain merger stages, which is inconsistent with predictions from some galaxy simulations. This discrepancy emphasizes the complexity of galaxy interactions. Overall, our findings provide valuable insights into how galaxy interactions reshape metallicity distribution, enhancing our understanding of the processes driving galaxy evolution during mergers.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"97 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695517","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Magnetic Field Structures In and Around Seyfert Galaxy Outflows

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adae05

Salmoli Ghosh, Preeti Kharb, Biny Sebastian, Jack Gallimore, Alice Pasetto, Christopher P. O’Dea, Timothy Heckman and Stefi A. Baum

{"title":"Magnetic Field Structures In and Around Seyfert Galaxy Outflows","authors":"Salmoli Ghosh, Preeti Kharb, Biny Sebastian, Jack Gallimore, Alice Pasetto, Christopher P. O’Dea, Timothy Heckman and Stefi A. Baum","doi":"10.3847/1538-4357/adae05","DOIUrl":"https://doi.org/10.3847/1538-4357/adae05","url":null,"abstract":"We present radio polarimetric images of 12 Seyfert and low-ionization nuclear emission-line region (LINER) galaxies belonging to the Centre for Astrophysics +12 μm sample exhibiting kiloparsec-scale radio outflows (KSRs). These observations have been carried out at 10 GHz with the Karl G. Jansky Very Large Array in D array and at 1.4 GHz with the BnA → A array configurations. We find signatures of organized magnetic (B) field structures in the cores, jets, and lobes of these galaxies. The linear polarization fraction varies from a few percent in the cores to 47% ± 18% in the lobes. The inferred B fields are toroidal in the cores of several sources making them consistent with the presence of either a sheath-like or a wind-like component surrounding the jet. The in-band spectral index images typically show the presence of flat/inverted spectrum cores and steep spectrum lobes. Radio cores with flatter spectra are found to have lower Eddington ratios, while the steeper ones have higher. A strong correlation is observed between the Seyfert/LINER radio outflow properties and the mass of the supermassive black holes; correlations with Eddington ratios are weaker. We find signatures of jet-medium interaction and both positive and negative active galactic nuclei (AGN) feedback in these sources. Overall, our study indicates that radio-quiet AGN with KSRs possess radio outflows driven by magnetic fields anchored to their black hole—accretion disk systems, which significantly impact their environments.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"71 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695447","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Filament Mass Losses Forced by Magnetic Reconnection in the Solar Corona

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adbae8

Craig D. Johnston, Lars K. S. Daldorff, Peter W. Schuck, Mark G. Linton, Will T. Barnes, James E. Leake and Simon Daley-Yates

{"title":"Filament Mass Losses Forced by Magnetic Reconnection in the Solar Corona","authors":"Craig D. Johnston, Lars K. S. Daldorff, Peter W. Schuck, Mark G. Linton, Will T. Barnes, James E. Leake and Simon Daley-Yates","doi":"10.3847/1538-4357/adbae8","DOIUrl":"https://doi.org/10.3847/1538-4357/adbae8","url":null,"abstract":"Recent observations of the solar atmosphere in cool extreme-ultraviolet lines have reported the prevalence of coronal rain falling from coronal cloud filaments that are associated with the magnetic dips of coronal X-point structures. These filaments mysteriously appear as clouds of mass in the corona that subsequently shrink and disappear due to mass losses that drain as coronal rain along arced field lines. Using a two-and-a-half-dimensional magnetohydrodynamic model, we investigated evaporation-condensation as the formation mechanism of the subset of coronal cloud filaments that form above coronal X-points. Our simulation included the effects of field-aligned thermal conduction and optically thin radiation, and used the state-of-the-art transition region adaptive conduction (TRAC) method to model the formation, maintenance, and mass loss of a filament above a coronal X-point. This paper presents a physical model that demonstrates magnetic reconnection as a filament loss mechanism, producing hybrid filament/coronal rain via mass losses through the X-point. A detailed analysis of how the mass of the filament forces the field to reconnect is also presented, revealing three phases that characterize the evolution of the reconnecting current sheet and associated mass losses. We conclude that the formation of certain coronal cloud filaments and subsequent mass losses via coronal rain can be explained by the evaporation-condensation model combined with filament mass losses forced by magnetic reconnection. We also report that rebound shocks generated by the impact of coronal rain condensations on the chromosphere together with retractive upflows can cause upward-propagating condensations to form through a dynamic thermal runaway process.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"35 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695516","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Identification and Analysis of Galactic Bars in DESI Legacy Imaging Surveys

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adbcac

Wenwen Wang and Zhimin Zhou

{"title":"Identification and Analysis of Galactic Bars in DESI Legacy Imaging Surveys","authors":"Wenwen Wang and Zhimin Zhou","doi":"10.3847/1538-4357/adbcac","DOIUrl":"https://doi.org/10.3847/1538-4357/adbcac","url":null,"abstract":"We present a comprehensive study of bar structures in the local universe using data from the DESI Legacy Imaging Surveys. Through isophotal analysis of 232,142 galaxies, we identify bars and classify them into strong and weak categories based on normalized bar length, using a threshold of 0.4. We find a total bar fraction of 42.9%, rising to 62.0% in disk galaxies, with strong barred galaxies accounting for 30.0%. For barred galaxies in our sample, deprojected bar lengths are measured both in absolute terms and normalized by galaxy size. Most bars are found to have absolute lengths of 3–7 kpc, and normalized bar lengths concentrated around a median value of 0.4. Bar ellipticity mainly ranges from 0.2 to 0.6, with a median value of 0.3. Our analysis reveals a bimodal distribution of bar fractions with respect to galaxy color, with weak bars in our classification being more prevalent in intermediate-color systems. With respect to stellar mass, strong bars also present a bimodal distribution, while weak bars are distributed uniformly. Normalized bar length remains relatively stable across stellar masses, while absolute bar length positively correlates with stellar mass. Cross-validation with visual classifications from Galaxy Zoo DESI catalog confirms a bar identification accuracy of 93%. These results validate our automated method for bar identification and measurement, demonstrating its reliability. Our findings underscore the importance of bars in galaxy evolution and highlight the potential of upcoming wide-field surveys to deepen our understanding of barred galaxies.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"21 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695758","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

BASS. XLV. Quantifying Active Galactic Nuclei Selection Effects in the Chandra COSMOS-legacy Survey with BASS

The Astrophysical Journal Pub Date : 2025-03-25 DOI: 10.3847/1538-4357/adb8c9

Yarone M. Tokayer, Michael J. Koss, C. Megan Urry, Priyamvada Natarajan, Richard Mushotzky, Mislav Baloković, Franz E. Bauer, Peter Boorman, Alessandro Peca, Claudio Ricci, Federica Ricci, Daniel Stern, Ezequiel Treister and Benny Trakhtenbrot

{"title":"BASS. XLV. Quantifying Active Galactic Nuclei Selection Effects in the Chandra COSMOS-legacy Survey with BASS","authors":"Yarone M. Tokayer, Michael J. Koss, C. Megan Urry, Priyamvada Natarajan, Richard Mushotzky, Mislav Baloković, Franz E. Bauer, Peter Boorman, Alessandro Peca, Claudio Ricci, Federica Ricci, Daniel Stern, Ezequiel Treister and Benny Trakhtenbrot","doi":"10.3847/1538-4357/adb8c9","DOIUrl":"https://doi.org/10.3847/1538-4357/adb8c9","url":null,"abstract":"Deep extragalactic X-ray surveys, such as the Chandra COSMOS-Legacy field (CCLS), are prone to be biased against active galactic nuclei (AGN) with high column densities due to their lower count rates at a given luminosity. To quantify this selection effect, we forward model nearby (z ∼ 0.05) AGN from the BAT AGN Spectroscopic Survey (BASS) with well-characterized (≳1000 cts) broadband X-ray spectra (0.5–195 keV) to simulate the CCLS absorption distribution. We utilize the BASS low-redshift analogs with similar luminosities to the CCLS ( ∼ 1042−45 erg s), which are much less affected by obscuration and low-count statistics, as the seed for our simulations and follow the spectral fitting of the CCLS. Our simulations reveal that Chandra would fail to detect the majority (53.3%; 563/1056) of obscured (NH ≥ 1022 cm−2) simulated BASS AGN given the observed redshift and luminosity distribution of the CCLS. Even for detected sources with sufficient counts (≥30) for spectral modeling, the level of obscuration is significantly overestimated. This bias is most extreme for objects whose best fit indicates a high-column density AGN (NH ≥ 1024 cm−2), since the majority (66.7%; 18/27) of these are actually unobscured sources (NH < 1022 cm−2). This implies that previous studies may have significantly overestimated the increase in the obscured fraction with redshift and the fraction of luminous obscured AGN. Our findings highlight the importance of directly considering obscuration biases and forward modeling in X-ray surveys, as well as the need for higher-sensitivity X-ray missions such as the Advanced X-ray Imaging Satellite (AXIS), and the importance of multiwavelength indicators to estimate obscuration in distant supermassive black holes.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143695520","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0