The Astrophysical Journal Supplement Series最新文献

{"title":"FAST Ultra-Deep Survey: Data Release for FUDS0","authors":"Hongwei Xi, Bo Peng, Lister Staveley-Smith, Bi-Qing For, Bin Liu and Dejian Ding","doi":"10.3847/1538-4365/ad67d5","DOIUrl":"https://doi.org/10.3847/1538-4365/ad67d5","url":null,"abstract":"We have used the Five-hundred-meter Aperture Spherical radio Telescope (FAST) to conduct a blind ultradeep survey for neutral hydrogen (H i). We present the complete results from the first of six fields (FUDS0). These observations of 95 hr allowed us to achieve a high-sensitivity (∼50 μJy beam−1) and a high-frequency resolution (22.9 kHz) over an area of 0.72 deg2. We detected 128 galaxies in H i distributed over the redshift range of 0 < z < 0.4, with H i masses in the range of , and three faint high-velocity clouds, with a peak column density of NH i ≤ 3.1 × 1017 cm−2. Of the galaxies, 95 are new detections and six have z > 0.38, where no unlensed H i emission has previously been directly detected. Estimates of completeness and reliability are presented for the catalog. The consistency of continuum and H i flux estimates with the NRAO VLA Sky Survey and the Arecibo Ultra-Deep Survey, respectively, confirms the accuracy of the calibration method and data reduction pipeline developed for the full FAST Ultra-Deep Survey.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187535","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}

{"title":"New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9","authors":"C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel","doi":"10.3847/1538-4365/ad527e","DOIUrl":"https://doi.org/10.3847/1538-4365/ad527e","url":null,"abstract":"We have conducted a search for strong gravitational lensing systems in the Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Surveys Data Release 9. This is the third paper in a series. These surveys together cover ∼19,000 deg² visible from the Northern Hemisphere, reaching a <italic toggle=\"yes\">z</italic>-band AB magnitude of ∼22.5. We use a deep residual neural network, trained on a compilation of known lensing systems and high-grade candidates as well as nonlenses in the same footprint. After applying our trained neural network to the survey data, we visually inspect and rank images with probabilities above a threshold which has been chosen to balance precision and recall. We have found 1895 lens candidates, of which 1512 are identified for the first time. Combining the discoveries from this work with those from Papers I (335) and II (1210), we have discovered a total of 3057 new candidates in the Legacy Surveys.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187536","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}

{"title":"A Swift X-Ray View of the SMS4 Sample. II. X-Ray Properties of 17 Bright Radio Sources","authors":"Alessandro Maselli, William R. Forman, Christine Jones, Ralph P. Kraft, Matteo Perri","doi":"10.3847/1538-4365/ad5dac","DOIUrl":"https://doi.org/10.3847/1538-4365/ad5dac","url":null,"abstract":"Based on a proposal to observe 18 bright radio sources from the SMS4 catalog with the Neil Gehrels Swift Observatory (hereafter Swift), we obtained X-ray observations of 17 targets (one target was not observed). Following up our first paper that discussed 31 sources (see Maselli et al.; 20 sources detected as point sources and one very extended source), we present results for this final sample of 17 radio sources that previously lacked dedicated, pointed narrow-field-of-view (FOV) X-ray observations. One of these 17 sources, undetected by Swift due to a very short exposure, was instead detected by eROSITA, and given in the Data Release 1 (DR1) Catalog. No 1eRASS source was found in the DR1 for the remaining source, unobserved by Swift. The new Swift observations led to 11 X-ray source detections in the 0.3–10 keV band and six upper limits. We investigated the extent of the X-ray emission and the hardness ratio, and when statistics allowed, we carried out a spectral analysis. The X-ray emission of eight sources is consistent with pointlike emission, while three sources show clear evidence of extent, each with peculiar properties. We used the X-ray determined positions and uncertainties of the 12 detected sources to establish associations with infrared and optical sources from the AllWISE and the GSC 2.4.2 catalogs. Requiring a detection in both the infrared and the optical bands to establish a candidate counterpart for our X-ray detections, we identify counterparts for all 12 sources. Following this X-ray-based approach to derive the position of the active nucleus, we are able to confirm the same IR counterparts previously proposed by White et al. for eight sources, and provide four new IR candidates. In the optical, we identify counterparts that match the candidates previously given by Burgess &amp; Hunstead for all sources. We discuss the interesting structure of MRC B0344−345 and PKS B2148−555, two of the six extended X-ray sources that we detected in both our Swift campaigns, and suggest they are very promising for further X-ray and radio investigations. For the 38 SMS4 sources that lack pointed, narrow-FOV X-ray telescope observations, after our Swift campaigns, we list 18 likely counterparts from the eROSITA DR1 catalog.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187537","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}

{"title":"The Self-organized Criticality Behaviors of Pulses in Magnetar Bursts","authors":"Shuo Xiao, Mei-Xin Hong, Zi-Yi You, Tong-Lei Liao, Shao-Lin Xiong, Shu-Xu Yi, Ping Wang, Jiao-Jiao Yang, Zheng-Huo Jiang, Yue Wang, Yan-Qiu Zhang, Ming-Yu Ge, Zhen Zhang, Xi-Hong Luo, Shi-Jun Dang, Ru-shuang Zhao, Ai-Jun Dong, Qi-Jun Zhi, He Gao, Di Li, Shuang-Nan Zhang","doi":"10.3847/1538-4365/ad6b18","DOIUrl":"https://doi.org/10.3847/1538-4365/ad6b18","url":null,"abstract":"The overall temporal and spectral characteristics (e.g., duration, fluence, peak flux, peak count rate, and total counts) of X-ray bursts (XRBs) originating from magnetars have been extensively studied to confirm their self-organized criticality (SOC) behaviors. However, for the pulses in XRBs, which are an important part of unraveling radiation processes such as magnetic reconnection and crustal rupture, their variable statistical characteristics are still unclear. In this work, we investigate the distributions of fluctuations in duration, waiting time, peak count rate, and total counts of pulses within bursts from two active and prolific magnetars, SGR J1935+2154 and SGR J1550-5418, observed by Fermi’s Gamma-ray Burst Monitor, Insight-HXMT, and GECAM. We report that the waiting time for pulses follows SOC, whereas previous studies indicated for bursts do not, possibly due to incomplete observations. Besides, the duration, peak count rate, and total counts for pulses are also SOC behaviors. The <italic toggle=\"yes\">α</italic>-values for the duration of pulses for both magnetars are ∼2, and the inferred Euclidean dimension <italic toggle=\"yes\">S</italic> is 3. Our findings provide evidence for the SOC of each radiation process during a burst, for example, multiple pulses produced by multiple magnetic reconnections triggered by a single starquake. Finally, the similar statistical characteristics for pulses from both magnetars lend support to their shared radiation processes.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187540","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}

{"title":"ALMA-IMF. XIV. Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters","authors":"Roberto Galván-Madrid, Daniel J. Díaz-González, Frédérique Motte, Adam Ginsburg, Nichol Cunningham, Karl M. Menten, Mélanie Armante, Mélisse Bonfand, Jonathan Braine, Timea Csengeri, Pierre Dell’Ova, Fabien Louvet, Thomas Nony, Rudy Rivera-Soto, Patricio Sanhueza, Amelia M. Stutz, Friedrich Wyrowski, Rodrigo H. Álvarez-Gutiérrez, Tapas Baug, Sylvain Bontemps, Leonardo Bronfman, Manuel Fernández-López, Antoine Gusdorf, Atanu Koley, Hong-Li Liu, Javiera Salinas, Allison P. M. Towner, Anthony P. Whitworth","doi":"10.3847/1538-4365/ad61e6","DOIUrl":"https://doi.org/10.3847/1538-4365/ad61e6","url":null,"abstract":"We use the H41<italic toggle=\"yes\">α</italic> recombination line to create templates of the millimeter free–free emission in the ALMA-IMF continuum maps, which allows us to separate it from dust emission. This method complements spectral-index information and extrapolation from centimeter-wavelength maps. We use the derived maps to estimate the properties of up to 34 H <sc>ii</sc> regions across the ALMA-IMF protoclusters. The hydrogen ionizing photon rate <italic toggle=\"yes\">Q</italic>\u0000₀ and spectral types follow the evolutionary trend proposed by Motte et al. The youngest protoclusters lack detectable ionized gas, followed by protoclusters with increasing numbers of OB stars. The total <italic toggle=\"yes\">Q</italic>\u0000₀ increases from ∼10⁴⁵ s⁻¹ to &gt;10⁴⁹ s⁻¹. We used the adjacent He41<italic toggle=\"yes\">α</italic> line to measure the relative number abundances of helium, finding values consistent with the Galactic interstellar medium, although a few outliers are discussed. A search for sites of maser amplification of the H41<italic toggle=\"yes\">α</italic> line returned negative results. We looked for possible correlations between the electron densities, emission measures, and <italic toggle=\"yes\">Q</italic>\u0000₀ with H <sc>ii</sc> region size <italic toggle=\"yes\">D</italic>. The latter is the best correlated, with <italic toggle=\"yes\">Q</italic>\u0000₀ ∝ <italic toggle=\"yes\">D</italic>\u0000^{2.49 ± 0.18}. This favors interpretations in which smaller ultracompact H <sc>ii</sc> regions are not necessarily the less dynamically evolved versions of larger ones but rather are ionized by less massive stars. Moderate correlations were found between the dynamical width Δ<italic toggle=\"yes\">V</italic>\u0000_dyn with <italic toggle=\"yes\">D</italic> and <italic toggle=\"yes\">Q</italic>\u0000₀. Δ<italic toggle=\"yes\">V</italic>\u0000_dyn increases from about 1 to 2 times the ionized-gas sound speed. Finally, an outlier H <sc>ii</sc> region south of W43-MM2 is discussed. We suggest that this source could harbor an embedded stellar or disk wind.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187538","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}

{"title":"Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties","authors":"Suman Saha","doi":"10.3847/1538-4365/ad6a60","DOIUrl":"https://doi.org/10.3847/1538-4365/ad6a60","url":null,"abstract":"Precise physical properties of the known transiting exoplanets are essential for their precise atmospheric characterization using modern and upcoming instruments. Leveraging the large volume of high-signal-to-noise-ratio photometric follow-up data from TESS, highly precise physical properties can be estimated for these systems, especially for those discovered using ground-based instruments prior to the TESS mission. In this work, I have used the publicly available TESS follow-up data for 28 transiting systems with 10 &lt; <italic toggle=\"yes\">V</italic>\u0000_mag &lt; 10.5, with an aim to update their known physical properties. The observed lightcurves have been analyzed by implementing a state-of-the-art critical noise treatment algorithm to effectively reduce both time-correlated and uncorrelated noise components, using sophisticated techniques like wavelet denoising and Gaussian-process regression. Compared with the previous studies, the estimated transit parameters are found to be more precise for most of the targets, including a few cases where a larger space-based instrument like Spitzer, Kepler, or CHEOPS has been used in the previous study. The large volume of transit observations used for each target has also resulted in a more accurate estimation of the physical properties, as this overcomes any error in parameter estimations from bias present in a smaller volume of data. Thus, comparing with the literature values, statistically significant improvements in the known physical properties of several targeted systems have been reported from this work. The large volume of transit-timing information from the analyses was also used to search for transit-timing variation trends in these targets, which has resulted in no significant detection.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187539","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}

{"title":"pop-cosmos: A Comprehensive Picture of the Galaxy Population from COSMOS Data","authors":"Justin Alsing, Stephen Thorp, Sinan Deger, Hiranya V. Peiris, Boris Leistedt, Daniel Mortlock, Joel Leja","doi":"10.3847/1538-4365/ad5c69","DOIUrl":"https://doi.org/10.3847/1538-4365/ad5c69","url":null,"abstract":"We present <monospace>pop-cosmos</monospace>: a comprehensive model characterizing the galaxy population, calibrated to 140,938 (<italic toggle=\"yes\">r</italic> &lt; 25 selected) galaxies from the Cosmic Evolution Survey (COSMOS) with photometry in 26 bands from the ultraviolet to the infrared. We construct a detailed forward model for the COSMOS data, comprising: a population model describing the joint distribution of galaxy characteristics and its evolution (parameterized by a flexible score-based diffusion model); a state-of-the-art stellar population synthesis model connecting galaxies’ intrinsic properties to their photometry; and a data model for the observation, calibration, and selection processes. By minimizing the optimal transport distance between synthetic and real data, we are able to jointly fit the population and data models, leading to robustly calibrated population-level inferences that account for parameter degeneracies, photometric noise and calibration, and selection. We present a number of key predictions from our model of interest for cosmology and galaxy evolution, including the mass function and redshift distribution; the mass–metallicity-redshift and fundamental metallicity relations; the star-forming sequence; the relation between dust attenuation and stellar mass, star formation rate, and attenuation-law index; and the relation between gas-ionization and star formation. Our model encodes a comprehensive picture of galaxy evolution that faithfully predicts galaxy colors across a broad redshift (<italic toggle=\"yes\">z</italic> &lt; 4) and wavelength range.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142224511","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}

{"title":"Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars","authors":"Lifu Zhang, Hongwei Ge, Xuefei Chen, Zhanwen Han","doi":"10.3847/1538-4365/ad6263","DOIUrl":"https://doi.org/10.3847/1538-4365/ad6263","url":null,"abstract":"The unstable mass transfer situation in binary systems will asymptotically cause the adiabatic expansion of the donor star and finally lead to the common envelope phase. This process could happen in helium binary systems once the helium donor star fills its Roche-lobe. We have calculated the adiabatic mass-loss model of naked helium stars with a mass range of 0.35 <italic toggle=\"yes\">M</italic>\u0000_⊙–10 <italic toggle=\"yes\">M</italic>\u0000_⊙, and every mass sequence evolved from the helium-zero-age main sequence to the cooling track of white dwarf or carbon ignition. In consideration of the influence of stellar wind, massive helium stars are not considered in this paper. Comparing the stellar radius with the evolution of the Roche-lobe under the assumption of conservative mass transfer, we give the critical mass ratio <italic toggle=\"yes\">q</italic>\u0000_crit = <italic toggle=\"yes\">M</italic>\u0000_He/<italic toggle=\"yes\">M</italic>\u0000_accretor as the binary stability criteria of low- and intermediate-mass helium binary stars. On the helium main sequence, the result shows 1.0 &lt; <italic toggle=\"yes\">q</italic>\u0000_crit &lt; 2.6, which is more unstable than the classical result of polytropic model <italic toggle=\"yes\">q</italic>\u0000_crit = 3. After the early helium Hertzsprung Gap, the <italic toggle=\"yes\">q</italic>\u0000_crit quickly increases even larger than 10 (more stable compared with the widely used result of <italic toggle=\"yes\">q</italic>\u0000_crit = 4), which is dominated by the expansion of the radiative envelope. Our result could be useful for these quick mass transfer binary systems such as AM CVns, ultra-compact X-ray binaries, and helium novae, and it could guide the binary population synthesis for the formation of special objects such as type Ia supernova and gravitational wave sources.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187541","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}

{"title":"Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C","authors":"Sheng Jin, Wenxin Jiang, Dong-Hong Wu","doi":"10.3847/1538-4365/ad6300","DOIUrl":"https://doi.org/10.3847/1538-4365/ad6300","url":null,"abstract":"Due to the high dimensionality or multimodality that is common in modern astronomy, sampling Bayesian posteriors can be challenging. Several publicly available codes based on different sampling algorithms can solve these complex models, but the execution of the code is not always efficient or fast enough. The article introduces a C language general-purpose code, Nii-C, that implements a framework of automatic parallel tempering Markov Chain Monte Carlo. Automatic in this context means that the parameters that ensure an efficient parallel tempering process can be set by a control system during the inital stages of a sampling process. The autotuned parameters consist of two parts, the temperature ladders of all parallel tempering Markov Chains and the proposal distributions for all model parameters across all parallel tempering chains. In order to reduce dependencies in the compilation process and increase the code’s execution speed, Nii-C code is constructed entirely in the C language and parallelized using the message-passing interface protocol to optimize the efficiency of parallel sampling. These implementations facilitate rapid convergence in the sampling of high-dimensional and multimodal distributions, as well as the expeditious code execution time. The Nii-C code can be used in various research areas to trace complex distributions due to its high sampling efficiency and quick execution speed. This article presents a few applications of the Nii-C code.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142224512","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}

{"title":"Atomic Transition Probabilities for Ultraviolet and Optical Lines of Tm ii * * Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS5-26555 (program GO-15657). This paper also includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.","authors":"E. A. Den Hartog, G. T. Voith, I. U. Roederer","doi":"10.3847/1538-4365/ad614f","DOIUrl":"https://doi.org/10.3847/1538-4365/ad614f","url":null,"abstract":"We report new branching fraction measurements for 224 ultraviolet and optical transitions of Tm <sc>ii</sc>. These transitions range in wavelength (wavenumber) from 2350 to 6417 Å (42,532–15,579 cm⁻¹) and originate in 13 odd-parity and 24 even-parity upper levels. Thirty-five of the 37 levels, accounting for 213 of the 224 transitions, are studied for the first time. Branching fractions are determined for two levels studied previously for comparison to earlier results. The levels studied for the first time are high lying, ranging in energy from 35,753 to 54,989 cm⁻¹. The branching fractions are determined from emission spectra from two different high-resolution spectrometers. These are combined with radiative lifetimes reported in an earlier study to produce a set of transition probabilities and log(<italic toggle=\"yes\">gf</italic>) values with accuracy ranging from 5% to 30%. Comparison is made to experimental and theoretical transition probabilities from the literature where such data exist. These new log(<italic toggle=\"yes\">gf</italic>) values are used to derive an abundance from one previously unused Tm <sc>ii</sc> line in the UV spectrum of the <italic toggle=\"yes\">r</italic>-process-enhanced metal-poor star HD 222925, and this abundance is consistent with previous determinations based on other Tm <sc>ii</sc> lines.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142187571","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}