Astronomy & Astrophysics最新文献

{"title":"Radio dimming associated with filament eruptions in the meter and decimeter wavebands","authors":"Zhenyong Hou, Hui Tian, Jingye Yan, Maria S. Madjarska, Jiale Zhang, Yu Xu, Hechao Chen, Zhao Wu, Lin Wu, Xuning Lv, Yang Yang, Yujie Liu, Li Deng, Li Feng, Ye Qiu","doi":"10.1051/0004-6361/202453282","DOIUrl":"https://doi.org/10.1051/0004-6361/202453282","url":null,"abstract":"Filament eruptions are considered to be a common phenomenon on the Sun and other stars, yet they are rarely directly imaged in the meter and decimeter wavebands. Using imaging data from the DAocheng solar Radio Telescope (DART) in the 150−450 MHz frequency range, we present two eruptive filaments that manifest as radio dimmings (i.e., emission depressions). Simultaneously, portions of these eruptive filaments are discernible as dark features in the chromospheric images. The sun-as-a-star flux curves of brightness temperature, derived from the DART images, exhibit obvious radio dimmings. The dimming depths range from 1.5% to 8% of the background level and show a negative correlation with radio frequencies and a positive correlation with filament areas. Our investigation suggests that radio dimming is caused by free-free absorption during filament eruptions obscuring the solar corona. This may provide a new method for detecting stellar filament eruptions.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"272 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506807","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 evolution of extragalactic peaked-spectrum sources down to 54 megahertz","authors":"Sai Zhai, Anniek J. Gloudemans, Gülay Gürkan, Femke J. Ballieux, Martin J. Hardcastle, Francesco De Gasperin, Huub J. A. Röttgering","doi":"10.1051/0004-6361/202452979","DOIUrl":"https://doi.org/10.1051/0004-6361/202452979","url":null,"abstract":"Peaked-spectrum sources, known for their distinct peaked radio spectra, are a type of radio-loud active galactic nuclei. One subtype, megahertz-peaked-spectrum (MPS) sources, which exhibit a spectral peak at a frequency of a hundred megahertz, have emerged as a potential tool for identifying high-redshift candidates. However, the potential evolutionary link between the fraction of these sources and their redshifts remains unclear and requires further investigation. The recent, high-sensitivity Low Frequency Array (LOFAR) surveys enable statistical studies of these objects down to ultra-low frequencies (< 150 MHz). In this study we first used the multi-radio data to investigate the evolution of spectral index with redshift for 1187 quasars from the 16th SDSS quasar catalog. For each quasar, we analyzed available data from the LOFAR Low Band Antenna at 54 MHz, the High Band Antenna at 144 MHz, and the Very Large Array Faint Images of the Radio Sky at Twenty centimeters at 1.4 GHz. We measured the spectral index ( and ) and find no significant change in their median values with redshift. Extended sources have steeper spectral indices than compact sources, which is consistent with previous findings. Based on the spectral index information, we identified MPS sources using the criteria and , and analyzed their properties. We find that the fraction of MPS sources is constant with the redshift (0.1 − 4.8), bolometric luminosity (10<sup>44<sup/> − 10<sup>48<sup/> erg/s), and supermassive black hole mass (10<sup>7<sup/> − 10<sup>10.5<sup/> M<sub>⊙<sub/>), which suggests that MPS sources have relatively stable physical conditions or formation mechanisms across various evolutionary stages and environments.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"51 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143507254","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":"NEUTRALUNIVERSEMACHINE: How filaments and dark-matter haloes influence the galaxy’s cold gas content","authors":"Wenlin Ma, Hong Guo, Michael G. Jones","doi":"10.1051/0004-6361/202451932","DOIUrl":"https://doi.org/10.1051/0004-6361/202451932","url":null,"abstract":"<i>Aims.<i/> We aim to investigate the influence of the distance to filaments and dark-matter haloes on galaxy cold-gas content in the empirical model NEUTRALUNIVERSEMACHINE (NUM) and the hydrodynamical simulation IllustrisTNG.<i>Methods.<i/> We used DisPerSE to identify cosmic web structures and calculate the distance of galaxies to filaments for both observations and models. We show the results of the H I and H<sub>2<sub/> mass functions, H I- and H<sub>2<sub/>-halo-mass relations, H I- and H<sub>2<sub/>-stellar-mass relations for galaxies in the NUM model and IllustrisTNG with different distances to filaments and compare them with observational measurements. We also show the evolution of H I and H<sub>2<sub/> mass densities at different distances to filament bins.<i>Results.<i/> We find that how filaments affect the H I gas is generally less significant compared to the halo environment. There is a weak trend in the observations at <i>z<i/> = 0 that low-mass haloes lying closer to the filaments tend to have reduced H I masses. However, this trend reverses for massive haloes with log(<i>M<i/><sub>vir<sub/>/<i>M<i/><sub>⊙<sub/>) > 12.5. This behaviour is accurately reproduced in the NUM model due to the dependence of H I gas on the halo formation time, but it does not appear in IllustrisTNG. The influence of filaments on the H I gas becomes slightly weaker at higher redshifts and is only significant for galaxies that reside in massive haloes in the NUM model. Filaments have almost no impact on the H<sub>2<sub/>-stellar-mass relation in both models, confirming that H<sub>2<sub/> is primarily determined by the galaxy stellar mass and star formation rate.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"74 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506806","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":"Impact of radiative accelerations on the stellar characterization of FGK-type stars using spectroscopic and seismic constraints","authors":"Nuno Moedas, Morgan Deal, Diego Bossini","doi":"10.1051/0004-6361/202453130","DOIUrl":"https://doi.org/10.1051/0004-6361/202453130","url":null,"abstract":"<i>Context.<i/> Chemical transport mechanisms are fundamental processes in stellar evolution models. They are responsible for the chemical distribution, and their impact determines how accurately we can characterize stars. Radiative accelerations are one of these processes. They allow the accumulation of elements at different depths in the star.<i>Aims.<i/> We aim to assess the impact of radiative accelerations on the modeling of FGK-type stars and their impact on the prediction of surface abundances.<i>Methods.<i/> To reduce the cost of the computation of radiative accelerations, we implemented the single-valued parameters (SVP) method in the stellar evolution code MESA. The SVP method is more efficient in calculating radiative accelerations, which enables computations of large enough grids of models for stellar characterization.<i>Results.<i/> Compared to models that include atomic diffusion (with only gravitational settling), the inclusion of radiative accelerations has a small effect on the inference of fundamental properties, with an impact of 2%, 0.7%, and 5% for mass, radius, and age. However, the treatment of radiative accelerations is necessary to predict the chemical composition of and accurately characterize stars.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506808","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":"GA-NIFS: Multiphase analysis of a star-forming galaxy at z ∼ 5.5","authors":"Eleonora Parlanti, Stefano Carniani, Giacomo Venturi, Rodrigo Herrera-Camus, Santiago Arribas, Andrew J. Bunker, Stéphane Charlot, Francesco D’Eugenio, Roberto Maiolino, Michele Perna, Hannah Übler, Torsten Böker, Giovanni Cresci, Mirko Curti, Gareth C. Jones, Isabella Lamperti, Pablo G. Pérez-González, Bruno Rodríguez Del Pino, Sandra Zamora","doi":"10.1051/0004-6361/202451692","DOIUrl":"https://doi.org/10.1051/0004-6361/202451692","url":null,"abstract":"In this study, we present a detailed multiphase analysis of HZ4, a main-sequence star-forming galaxy at <i>z<i/> ∼ 5.5, known for being a turbulent rotating disk and having a detection of a [C II] outflow in the ALMA observations. We exploited JWST/NIRSpec observations in the integral field spectroscopy mode with low- and high-spectral resolution which allow us, for the first time, to spatially resolve the rest-frame UV and optical emission of the galaxy to investigate the galaxy properties. In particular, the high-resolution dataset allowed us to study the kinematics of the ionized gas phase, and the conditions of the interstellar medium, such as the excitation mechanism, dust attenuation, and metallicity. The lower spectral-resolution observations allowed us to study the continuum emission and infer the stellar populations’ ages and properties. Our findings suggest that HZ4 is a galaxy merger rather than a rotating disk as previously inferred from lower-resolution [C II] data. The merger is associated with an extended broad, blueshifted emission, potentially indicative of an outflow originating from a region of intense star formation and extending up to 4 kpc. In light of these new observations, we reanalyzed the ALMA data to compare the multiphase gas properties. If we interpret the broad components seen in [C II] and [O III]<i>λ<i/>5007 Å as outflows, the neutral and ionized components are co-spatial, and the mass loading factor of the ionized phase is significantly lower than that of the neutral phase, aligning with trends observed in multiphase systems at lower redshifts. Nonetheless, additional observations and larger statistical samples are essential to determine the role of mergers and outflows in the early Universe and to clarify the origin of the broad emission components observed in this system.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"26 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506809","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":"eROSITA X-ray analysis of the PeVatron candidate Westerlund 1","authors":"Konstantin Haubner, Manami Sasaki, Alison Mitchell, Gabriele Ponti, Gavin Rowell, Sabrina Einecke, Miroslav Filipović, Sanja Lazarević, Gerd Pühlhofer, Andrew Strong","doi":"10.1051/0004-6361/202451964","DOIUrl":"https://doi.org/10.1051/0004-6361/202451964","url":null,"abstract":"<i>Context.<i/> It is still unclear which fraction of cosmic rays above an energy of 1 PeV is accelerated by the observed Galactic PeVatron population. These sources of unknown physical origin are detected through their <i>γ<i/>-ray emission, which also identifies them as particle accelerators. However, their <i>γ<i/>-ray data are typically degenerate between hadronic and leptonic emission scenarios, which hinders their straightforward association with the mainly hadronic cosmic ray population.<i>Aims.<i/> In this study, we aimed to distinguish between leptonic and hadronic particle acceleration scenarios for the PeVatron candidate HESS J1646−458, which is associated with the star cluster Westerlund 1 (Wd 1). To this end, we first studied the diffuse X-ray emission from Wd 1 to better understand if its origin is of thermal or nonthermal nature. In addition, we searched for X-ray synchrotron emission from the associated PeVatron candidate HESS J1646−458 to put new constraints on the magnetic field strength and the leptonic particle population of this source.<i>Methods.<i/> We used data from the all-sky surveys 1 to 4 of the <i>extended Roentgen Survey with an Imaging Telescope Array<i/> (<i>eROSITA<i/>) on board the Spectrum-Roentgen-Gamma orbital platform to spectrally analyze the diffuse emission from Wd 1 and HESS J1646−458. For Wd 1, we fitted and compared a purely thermal model and a model with a thermal and a nonthermal component. Next, we analyzed the spectra of four annuli around Wd 1 that coincide with HESS J1646−458 to search for synchrotron radiation.<i>Results.<i/> We find that <i>eROSITA<i/> data cannot distinguish between thermal and nonthermal source scenarios for the diffuse emission from Wd 1 itself. For a thermal source scenario, the observed X-ray flux can be explained in large part by unresolved pre-main sequence stars or by thermalized stellar wind shocks. In the case of the PeVatron candidate HESS J1646−458, we find no evidence of synchrotron emission. We estimated an upper confidence bound of the synchrotron flux up to 40 ′ around Wd 1 of 1.9 ⋅ 10<sup>−3<sup/> keV<sup>−1<sup/> cm<sup>−2<sup/> s<sup>−1<sup/>. We used this result to study the spectral energy distribution of the source. From that, we obtained an upper 1<i>σ<i/> confidence bound on the magnetic field strength of HESS J1646−458 of 7 μG.<i>Conclusions.<i/> Our upper bound on the magnetic field strength in HESS J1646−458 is compatible with a previous estimate in the literature for a fully leptonic source scenario. Therefore, a purely leptonic emission scenario is compatible with our results. The same is the case for hadronic and hybrid scenarios, for which even less synchrotron flux is expected compared to the leptonic scenario.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"29 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506849","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 synthetic population of ultra-luminous X-ray sources","authors":"Lutendo Nyadzani, Soebur Razzaque, Justin D. Finke","doi":"10.1051/0004-6361/202449208","DOIUrl":"https://doi.org/10.1051/0004-6361/202449208","url":null,"abstract":"This paper presents an analysis of the predicted optical-to-X-ray spectral index (<i>α<i/><sub>ox<sub/>) within the context of ultra-luminous X-ray sources (ULXs) associated with stellar-mass black holes (BHs) and neutron stars (NSs). We used the population synthesis code COSMIC to simulate the evolution of binary systems and investigate the relationship between ultraviolet (UV) and X-ray emission during the ULX phase, namely the <i>α<i/><sub>ox<sub/> relation. Furthermore, we investigated the impact of metallicity on <i>α<i/><sub>ox<sub/> values. Notably, it predicts a significant anti-correlation between <i>α<i/><sub>ox<sub/> and UV luminosity (<i>L<i/><sub>UV<sub/>), consistent with observations. The slope of this relationship varies with metallicity for black hole ULXs (BH-ULXs). The neutron star ULX (NS-ULX) population shows a relatively consistent slope around −0.33 across metallicities, with minor variations. The number of ULXs decreases with increasing metallicity, consistent with observational data. The X-ray luminosity function (XLF) shows a slight variation in its slope with metallicity, exhibiting a relative excess of high-luminosity ULXs at lower metallicities. The inclusion of the beaming effect in the analysis shows a significant impact on the XLF and <i>α<i/><sub>ox<sub/>, particularly at high accretion rates, where the emission is focused into narrower cones. We found that UV emission in ULXs is predominantly disc-dominated, which is the likely origin of the <i>α<i/><sub>ox<sub/> relation, with the percentage of disc-dominated ULXs increasing as metallicity rises.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"26 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143507258","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":"Evidence of a diffuse, extended continuum source in quasars from the relative sizes of the broad line region and the UV-optical continuum source measured with microlensing","authors":"Damien Hutsemékers, Dominique Sluse","doi":"10.1051/0004-6361/202453457","DOIUrl":"https://doi.org/10.1051/0004-6361/202453457","url":null,"abstract":"Microlensing by stars in the lens galaxy of a gravitationally lensed quasar is a phenomenon that can selectively magnify quasar subregions, producing observable changes in the continuum brightness or distortions in the emission line profiles. Hence, microlensing allows us to probe the inner quasar regions. In this paper, we report measurements of the ratio of the broad emission line region (BLR) radius to the continuum source radius in eight lensed quasars, for the C IV, Mg II, and H<i>α<i/> emission lines and their respective underlying continua at <i>λλ<i/> 1550 Å, 2800 Å, and 6563 Å. The microlensing-induced line profile distortions and continuum magnifications were observed in the same single-epoch datasets, and simultaneously compared with microlensing simulations. We found that, on average, the inner radius of the BLR starts at the end of the UV-optical continuum source, independently of the line ionization and the wavelength of the continuum. The half-light radius of the BLR is, on average, a factor of six larger than the half-light radius of the continuum source, independently of the quasar’s bolometric luminosity. We also found a correlation between the BLR radius and the continuum source radius, supporting the idea that the dominant contribution to the UV-optical continuum may come from the BLR itself. Our results independently confirm the results of reverberation mapping studies, and extend them to higher-redshift, higher-luminosity quasars.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"75 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506805","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":"Radial X-ray profiles of simulated galaxies","authors":"S. Vladutescu-Zopp, V. Biffi, K. Dolag","doi":"10.1051/0004-6361/202450989","DOIUrl":"https://doi.org/10.1051/0004-6361/202450989","url":null,"abstract":"<i>Context.<i/> Theoretical models of structure formation predict the presence of a hot gaseous atmosphere around galaxies. While this hot circumgalactic medium (CGM) has been observationally confirmed through UV absorption lines, the detection of its direct X-ray emission remains scarce. Recent results from the eROSITA collaboration have claimed the detection of the CGM out to the virial radius for a stacked sample of Milky Way-mass galaxies.<i>Aims.<i/> We investigate theoretical predictions of the intrinsic CGM X-ray surface brightness (SB) using simulated galaxies and connect them to their global properties, such as the gas temperature, hot gas fraction, and stellar mass.<i>Methods.<i/> We selected a sample of central galaxies from the ultra-high-resolution cosmological volume (48 cMpc h<sup>−1<sup/>) of the Magneticum Pathfinder set of hydrodynamical cosmological simulations. We classified them as star-forming (SF) or quiescent (QU) based on their specific star formation rate (SFR). For each galaxy, we generated X-ray mock data using the X-ray photon simulator PHOX, from which we obtained SB profiles out to the virial radius for different X-ray emitting components; namely, gas, active galactic nuclei (AGNs), and X-ray binaries (XRBs). We fit a <i>β<i/>-profile to the gas component of each galaxy and observed trends between its slope and global quantities of the simulated galaxy.<i>Results.<i/> We found marginal differences among the average total SB profile in SF and QU galaxies beyond <i>r<i/> > 0.05 <i>R<i/><sub>vir<sub/>. The relative contribution from hot gas exceeds 70% and is non-zero (≲10%) for XRBs in both galaxy types. At small radii (<i>r<i/> < 0.05 <i>R<i/><sub>vir<sub/>), XRBs dominate the SB profile over the hot gas for QU galaxies. We found positive correlations between the galaxies’ global properties and the normalization of their SB profiles. The fitted <i>β<i/>-profile slope is correlated with the total gas luminosity, which, in turn, shows strong connections to the current accretion rate of the central supermassive black hole (SMBH). We found the halo scaling relations to be consistent with the literature.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"28 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506810","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":"An energetic absorption outflow in QSO J1402+2330: Analysis of DESI observations","authors":"M. Dehghanian, N. Arav, M. Sharma, G. Walker, K. Johnston, M. Kaupin","doi":"10.1051/0004-6361/202453384","DOIUrl":"https://doi.org/10.1051/0004-6361/202453384","url":null,"abstract":"<i>Context.<i/> Quasar outflows play a significant role in the active galactic nucleus (AGN) feedback, impacting the interstellar medium and potentially influencing galaxy evolution. Characterizing these outflows is essential for understanding AGN-driven processes.<i>Aims.<i/> We aim to analyze the physical properties of the mini-broad absorption line outflow in quasar J1402+2330 using data from the Dark Energy Spectroscopic Instrument (DESI) survey. We seek to measure the outflow’s location, energetics, and potential impact on AGN feedback processes.<i>Methods.<i/> In the spectrum of J1402+2330, we identify multiple ionic absorption lines, including ground and excited states. We measure the ionic column densities and then use photoionization models to determine the total hydrogen column density and ionization parameter of the outflow. We utilized the population ratio of the excited state to the ground state of N III and S IV to determine the electron number density.<i>Results.<i/> The derived electron number density, combined with the ionization parameter, indicates an outflow distance of approximately 2.2 kpc from the central source. Having a mass outflow rate of more than one thousand solar masses per year and a kinetic energy output exceeding 5% of the Eddington luminosity, this outflow can significantly contribute to AGN feedback.<i>Conclusions.<i/> Our findings suggest the absorption outflow in J1402+2330 plays a potentially significant role in AGN feedback processes. This study highlights the value of DESI data in exploring AGN feedback mechanisms.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"66 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143506804","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}