The Astrophysical Journal最新文献_第2页

Disk2Planet: A Robust and Automated Machine Learning Tool for Parameter Inference in Disk–Planet Systems Disk2Planet：用于盘-行星系统参数推断的稳健而自动化的机器学习工具

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad8086

Shunyuan Mao, 顺元毛, Ruobing Dong, 若冰董, Kwang Moo Yi, Lu Lu, Sifan Wang and Paris Perdikaris

引用次数: 0

Radial Distribution of Electron Quasi-thermal Noise in the Inner Heliosphere 内太阳圈电子准热噪声的径向分布

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad85d6

Yi-Lun Li, 逸伦李, Ling Chen, 玲陈, De-Jin Wu and 德金吴

{"title":"Radial Distribution of Electron Quasi-thermal Noise in the Inner Heliosphere","authors":"Yi-Lun Li, 逸伦李, Ling Chen, 玲陈, De-Jin Wu and 德金吴","doi":"10.3847/1538-4357/ad85d6","DOIUrl":"https://doi.org/10.3847/1538-4357/ad85d6","url":null,"abstract":"The electron population in the solar wind plasma can be described with three different components: a core, a halo, and a magnetic field aligned strahl. The electron quasi-thermal noise (QTN) is investigated by using an electron population model consisting of a core with a Maxwellian distribution and a halo with a kappa distribution, based on the empirical equations for electron density and temperature and the index for the kappa halo. The power spectra of the electron QTN are calculated at different heliocentric radial distances from 10 to 200 Rs. The dependence of the QTN spectrum and effective Debye length on model parameters, including the ratio of the halo to the core for the density and temperature, the kappa index, and the antenna length, is further discussed. The results show that the electron QTN spectrum consists of a plateau in the low-frequency band f < fpt, a peak at the total plasma frequency fpt, and a rapidly decreasing part in the high-frequency band f > fpt. The QTN peak and plateau level continuously decrease as the radial distance increases, with the peak’s shape changing due to the variation of the kappa index. Although the model parameters are variable, the QTN plateau level presents less than an order of change with these parameters changing greatly, and only a monotonic change of the plateau is shown when the parameters are close to the practical situation. The results can provide a reference for future deep-space exploration in the inner heliosphere, and also for the design of detectors.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684470","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

Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects 强非重力加速度与误认近地天体的可能性

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad85e3

Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli and Jason T. Wright

{"title":"Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects","authors":"Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli and Jason T. Wright","doi":"10.3847/1538-4357/ad85e3","DOIUrl":"https://doi.org/10.3847/1538-4357/ad85e3","url":null,"abstract":"Nongravitational accelerations in the absence of observed activity have recently been identified on near-Earth objects (NEOs), opening the question of the prevalence of anisotropic mass loss in the near-Earth environment. Motivated by the necessity of nongravitational accelerations to identify 2010 VL65 and 2021 UA12 as a single object, we investigate the problem of linking separate apparitions in the presence of nongravitational perturbations. We find that nongravitational accelerations on the order of 1 × 10–9 au day−2 can lead to a change in plane-of-sky positions of ∼1 × 103 arcsec between apparitions. Moreover, we inject synthetic tracklets of hypothetical nongravitationally accelerating NEOs into the Minor Planet Center orbit identification algorithms. We find that at large nongravitational accelerations (∣Ai∣ ≥ 1 × 10−8 au day−2) these algorithms fail to link a significant fraction of these tracklets. We further show that if orbits can be determined for both apparitions, the tracklets will be linked regardless of nongravitational accelerations, although they may be linked to multiple objects. In order to aid in the identification and linkage of nongravitationally accelerating objects, we propose and test a new methodology to search for unlinked pairs. When applied to the current census of NEOs, we recover the previously identified case but identify no new linkages. We conclude that current linking algorithms are generally robust to nongravitational accelerations, but objects with large nongravitational accelerations may potentially be missed. While current algorithms are well-positioned for the anticipated increase in the census population from future survey missions, it may be possible to find objects with large nongravitational accelerations hidden in isolated tracklet pairs.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"66 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684473","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

Constraining the Low-mass End of the Stellar-to-halo Mass Relation with Surveys of Satellite Galaxies 利用卫星星系观测对恒星与光环质量关系的低质量端进行约束

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad834e

J. Sebastian Monzon, Frank C. van den Bosch and Kaustav Mitra

{"title":"Constraining the Low-mass End of the Stellar-to-halo Mass Relation with Surveys of Satellite Galaxies","authors":"J. Sebastian Monzon, Frank C. van den Bosch and Kaustav Mitra","doi":"10.3847/1538-4357/ad834e","DOIUrl":"https://doi.org/10.3847/1538-4357/ad834e","url":null,"abstract":"The abundance of satellite galaxies is set by the hierarchical assembly of their host halo. We leverage this to investigate the low-mass end (MH < 1011M⊙) of the stellar-to-halo mass relation (SHMR), which is key to constraining theories of galaxy formation and cosmology. We argue that recent analyses of satellite galaxies in the Local Group environment have not adequately modeled the dominant source of scatter in satellite stellar mass functions: the variance in accretion histories for a fixed host halo mass. We present a novel inference framework that not only properly accounts for this halo-to-halo variance but also naturally identifies the amount of host halo mass mixing, which is generally unknown. Specifically, we use the semianalytical SatGen model to construct mock satellite galaxy populations consistent with the third data release of the Satellites Around Galactic Analogs survey. We demonstrate that even under the most idealized circumstances, the halo-to-halo variance makes it virtually impossible to put any meaningful constraints on the scatter in the SHMR. Even a satellite galaxy survey made up 100 hosts can at best only place an upper limit of ∼0.5 dex on the scatter (at the 95% confidence level). This is because the large variance in halo assembly histories dominates over the scatter in the SHMR. This problem can be overcome by increasing the sample size of the survey by an order of magnitude (∼1000 host galaxies), something that should be fairly straightforward with forthcoming spectroscopic surveys.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684465","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

Stellar Bars Form Dark Matter Counterparts in TNG50 恒星条在 TNG50 中形成暗物质对应物

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad863a

Neil Ash, Monica Valluri, Yingtian Chen and Eric F. Bell

{"title":"Stellar Bars Form Dark Matter Counterparts in TNG50","authors":"Neil Ash, Monica Valluri, Yingtian Chen and Eric F. Bell","doi":"10.3847/1538-4357/ad863a","DOIUrl":"https://doi.org/10.3847/1538-4357/ad863a","url":null,"abstract":"Dark matter (DM) bars that shadow stellar bars have been previously shown to form in idealized simulations of isolated disk galaxies, but have yet to be studied in a fully cosmological context. In this work, we analyze a population of disk galaxies within the TNG50 simulation to determine the characteristics of their dark bars. We estimate bar strength and orientation using both the in-plane Fourier A2 density moments and the quadrupolar coefficients of the spherical harmonic basis function expansions of the density. We additionally present two novel methods for measuring the bar pattern speed Ωp and rotation axis orientation using these coefficients, and apply them to one sample galaxy located in a TNG50 subbox. Consistent with isolated simulations, DM bars are shorter than their stellar counterparts and are 75% weaker in A2. DM bars dominate the shape of the inner halo potential and are apparent in the time series of quadrupolar coefficients. In our selected subbox galaxy, the stellar and dark bars remain co-aligned throughout the last 8 Gyr and have identical Ωp. Pattern speed Ωp evolves considerably over the last 8 Gyr, consistent with torques on the bars due to dynamical friction and gas accretion, and is seen to increase following a merger at tlb = 1.5 Gyr. Rather than remaining static in time, the bar rotation axis displays both precession and nutation possibly caused by torques outside the plane of rotation. We find that the shape of the stellar and DM mass distributions are tightly correlated with Ωp.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"36 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684474","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

Whole-disk Sampling of Molecular Clouds in M83 对 M83 分子云的全盘取样

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad8228

Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka and Yoshimasa Watanabe

{"title":"Whole-disk Sampling of Molecular Clouds in M83","authors":"Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka and Yoshimasa Watanabe","doi":"10.3847/1538-4357/ad8228","DOIUrl":"https://doi.org/10.3847/1538-4357/ad8228","url":null,"abstract":"We present a catalog of clouds identified from the 12CO (1–0) data of M83, which was observed using the Atacama Large Millimeter/submillimeter Array with a spatial resolution of ∼46 pc and a mass sensitivity of ∼104M⊙ (3σ). The almost full-disk coverage and high sensitivity of the data allowed us to sample 5724 molecular clouds with a median mass of ∼1.9 × 105M⊙, which is comparable to the most frequently sampled mass of giant molecular clouds by surveys in the Milky Way (MW). About 60% of the total CO luminosity in M83's disk arises from clouds more massive than 106M⊙. Such massive clouds comprise 16% of the total clouds in number and tend to concentrate toward the arm, bar, and center, while smaller clouds are more prevalent in interarm regions. Most >106M⊙ clouds have peak brightness temperatures Tpeak above 2 K with the current resolution. Comparing the observed cloud properties with the scaling relations determined by P. M. Solomon et al. (1987, hereafter S87), Tpeak > 2 K clouds follow the relations, but Tpeak < 2 K clouds, which are dominant in number, deviate significantly. Without considering the effect of beam dilution, the deviations would suggest modestly high virial parameters (median αvir ∼ 2.7) and low surface mass densities (median Σ ∼ 22 M⊙ pc−2) for the entire cloud samples, which are similar to values found for the MW clouds by T. S. Rice et al. (2016) and M.-A Miville-Deschênes et al. (2017). However, once beam dilution is taken into account, the observed αvir and Σ for a majority of the clouds (mostly Tpeak <2 K) can be potentially explained with intrinsic Σ of ∼100 M⊙ pc−2 and αvir of ∼1, which are similar to the clouds of S87.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684261","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

A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB 向 CHIME/FRB 发现的重复快速射电暴寻找持续射电源

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad808e

Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin and Kendrick M. Smith

{"title":"A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB","authors":"Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin and Kendrick M. Smith","doi":"10.3847/1538-4357/ad808e","DOIUrl":"https://doi.org/10.3847/1538-4357/ad808e","url":null,"abstract":"The identification of persistent radio sources (PRSs) coincident with two repeating fast radio bursts (FRBs) supports FRB theories requiring a compact central engine. However, deep nondetections in other cases highlight the diversity of repeating FRBs and their local environments. Here, we perform a systematic search for radio sources towards 37 CHIME/FRB repeaters using their arcminute localizations and a combination of archival surveys and targeted observations. Through multiwavelength analysis of individual radio sources, we identify two (20181030A-S1 and 20190417A-S1) for which we disfavor an origin of either star formation or an active galactic nucleus in their host galaxies and thus consider them candidate PRSs. We do not find any associated PRSs for the majority of the repeating FRBs in our sample. For eight FRB fields with Very Large Array imaging, we provide deep limits on the presence of PRSs that are 2–4 orders of magnitude fainter than the PRS associated with FRB 20121102A. Using Very Large Array Sky Survey imaging of all 37 fields, we constrain the rate of luminous (≳1040 erg s−1) PRSs associated with repeating FRBs to be low. Within the context of FRB-PRS models, we find that 20181030A-S1 and 20190417A-S1 can be reasonably explained within the context of magnetar, hypernebulae, gamma-ray burst afterglow, or supernova ejecta models—although we note that both sources follow the radio luminosity versus rotation measure relationship predicted in the nebula model framework. Future observations will be required to both further characterize and confirm the association of these PRS candidates with the FRBs.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"129 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684460","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

Cracking the Relation between Mass and 1P-star Fraction of Globular Clusters. II. The Masses in 1P and 2P Stars as a Second Tool 破解球状星团质量与 1P 星比例之间的关系。II.以 1P 和 2P 恒星的质量为第二工具

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad85d7

Geneviève Parmentier

{"title":"Cracking the Relation between Mass and 1P-star Fraction of Globular Clusters. II. The Masses in 1P and 2P Stars as a Second Tool","authors":"Geneviève Parmentier","doi":"10.3847/1538-4357/ad85d7","DOIUrl":"https://doi.org/10.3847/1538-4357/ad85d7","url":null,"abstract":"Galactic globular clusters contain two main groups of stars, the pristine or 1P stars, and the polluted or 2P stars. The pristine-star fraction in clusters, F1P, is a decreasing function of the cluster present-day mass, mprst. Paper I has introduced a model mapping the region of the (mprst, F1P) space occupied by clusters, with the cluster mass threshold for 2P-star formation a key building block. We now expand this model to the pristine-star fraction in dependence of the pristine- and polluted-population masses. A. P. Milone et al. found that F1P anticorrelates more tightly with the polluted-population present-day mass, m2P,prst, than with the cluster total mass, mprst. By contrast, F1P anticorrelates poorly with the pristine-population current mass, m1P,prst. We show the loose anticorrelation between F1P and m1P,prst to result from a roughly constant pristine-population mass in clusters as they start their long-term evolution in the Galactic tidal field. As for the tight anticorrelation between m2P,prst and F1P, it stems from the initially shallow relation between m2P and F1P. Clusters of the Large and Small Magellanic Clouds (LMC and SMC, respectively) appear to behave unexpectedly with respect to each other. For a given F1P, LMC clusters are more massive than SMC clusters despite their enduring a stronger tidal field. This is opposite to how the Galactic outer- and inner-halo clusters behave. The explanation may lie in cluster formation conditions. Finally, we wonder whether the single-population clusters NGC 419 and Rup 106 formed as multiple-population clusters.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"38 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684472","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

Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5 极端之间：利用 ∼500 个 z ≥ 5 的已确认源建立高红移星系的 JWST 光谱基准

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad85d3

Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini and Piero Rosati

{"title":"Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5","authors":"Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini and Piero Rosati","doi":"10.3847/1538-4357/ad85d3","DOIUrl":"https://doi.org/10.3847/1538-4357/ad85d3","url":null,"abstract":"The exceptional spectra of the most luminous z > 10 sources observed so far have challenged our understanding of early galaxy evolution, requiring a new observational benchmark for meaningful interpretation. As such, we construct spectroscopic templates representative of high-redshift, star-forming populations, using 482 confirmed sources at z = 5.0−12.9 with JWST/NIRSpec prism observations, and report on their average properties. We find z = 5−11 galaxies are dominated by blue UV continuum slopes (β = −2.3 to −2.7) and reduced Balmer indices, characteristic of dust-poor and young systems, with a shift towards bluer slopes and younger ages with redshift. The evolution is mirrored by ubiquitous C iii] detections across all redshifts (rest-frame equivalent widths of 5−14 Å), which increase in strength towards early times. Rest-frame optical lines reveal elevated ratios (O32 = 7–31, R23 = 5–8, and Ne3O2 = 1−2) and subsolar metallicities (log(O/H) = 7.3−7.9), typical of ionization conditions and metallicities rarely observed in z ∼ 0 populations. Within our sample, we identify 57 Lyα emitters, which we stack and compare to a matched sample of nonemitters. The former are characterized by more extreme ionizing conditions with enhanced C iii], C iv, and He ii + [O iii] line emission, younger stellar populations from Balmer jumps, and a more pristine interstellar medium seen through bluer UV slopes and elevated rest-frame optical line ratios. The novel comparison illustrates important intrinsic differences between the two populations, with implications for Lyα visibility. The spectral templates derived here represent a new observational benchmark with which to interpret high-redshift sources, lifting our constraints on their global properties to unprecedented heights and extending out to the earliest of cosmic times.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"51 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684475","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

Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies 通过分析类星体寄主星系中分子气体的静水平衡来约束类星体反馈

The Astrophysical Journal Pub Date : 2024-11-22 DOI: 10.3847/1538-4357/ad7e26

Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer and Ezequiel Treister

{"title":"Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies","authors":"Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer and Ezequiel Treister","doi":"10.3847/1538-4357/ad7e26","DOIUrl":"https://doi.org/10.3847/1538-4357/ad7e26","url":null,"abstract":"We investigate the kinematics and dynamics of the molecular and ionized gas in the host galaxies of three Palomar-Green quasars at low redshifts, benefiting from the archival millimeter-wave interferometric and optical integral field unit data. We study the kinematics of both cold molecular and hot ionized gas by analyzing the CO and Hα data cubes, and construct the mass distributions of our sample through gas dynamics, utilizing a priori knowledge regarding the galaxy light distribution. We find no systematic offset between the stellar mass derived from our dynamical method and that from the broadband photometry and mass-to-light ratio, suggesting the consistency of both methods. We then study the kinetic pressure and the weight of the interstellar medium (ISM) using our dynamical mass model. By studying the relationship between kinetic pressure and gravitational pressure of the quasar host galaxies, we find an equivalence in the hydrostatic equilibrium states of ISM in the quasar host galaxies, similar to the result of gas equilibrium in normal star-forming galaxies, suggesting minimal quasar feedback. Regarding noncircular motion as indicative of quasar-driven outflows, we observe an exceptionally low coupling efficiency between molecular gas outflow and active galactic nucleus bolometric luminosities. These results demonstrate the marginal influence of the central engine on the properties of cold molecular gas in quasar host galaxies.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"46 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142684461","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