Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad7500
Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈 and Ryan Chornock
Close binary systems are the progenitors to both Type Ia supernovae and the compact object mergers that can be detected via gravitational waves. To achieve a binary with a small radial separation, it is believed that the system likely undergoes common envelope (CE) evolution. Despite its importance, CE evolution may be one of the largest uncertainties in binary evolution due to a combination of computational challenges and a lack of observed benchmarks where both the post-CE and pre-CE conditions are known. Identifying post-CE systems in star clusters can partially circumvent this second issue by providing an independent age constraint on the system. For the first time, we conduct a systematic search for white dwarf and main-sequence binary systems in 299 Milky Way open star clusters. Coupling Gaia DR3 photometry and kinematics with multiband photometry from Pan-STARRS1 and the Two Micron All Sky Survey, we apply a machine learning-based approach and find 52 high-probability candidates in 38 open clusters. For a subset of our systems, we present follow-up spectroscopy from the Gemini and Lick Observatories and archival light curves from the Transiting Exoplanet Survey Satellite, Kepler/K2, and the Zwicky Transient Facility. Examples of M dwarfs with hot companions are spectroscopically observed, along with regular system variability. While the kinematics of our candidates are consistent with their host clusters, some systems have spatial positions offset relative to their hosts, potentially indicative of natal kicks. Ultimately, this catalog is a first step to obtaining a set of observational benchmarks to better link post-CE systems to their pre-CE progenitors.
近双星系统是 Ia 型超新星和可通过引力波探测到的紧凑天体合并的起源。为了形成一个径向间隔很小的双星，人们认为该系统很可能经历了共同包络（CE）演化。尽管CE演化非常重要，但它可能是双星演化中最大的不确定因素之一，这是因为计算上的挑战和缺乏观测到的已知后CE和前CE条件的基准。在星团中识别后CE系统可以部分规避第二个问题，因为它可以为系统提供一个独立的年龄约束。我们首次对 299 个银河系开放星团中的白矮星和主序双星系统进行了系统搜索。将盖亚 DR3 光度测量和运动学与 Pan-STARRS1 和两微米全天空巡天的多波段光度测量相结合，我们应用了一种基于机器学习的方法，在 38 个疏散星团中发现了 52 个高概率候选系统。对于我们发现的系统子集，我们展示了来自双子座和里克天文台的后续光谱，以及来自凌日系外行星巡天卫星、开普勒/K2 和兹威基瞬变设施的档案光曲线。通过分光镜观测到了有热伴星的 M 矮星的例子，同时还观测到了有规律的系统变异。虽然我们的候选系统的运动学特性与其宿主星团一致，但有些系统的空间位置相对于宿主有偏移，这可能表明存在原生踢脚现象。最终，这个星表是获得一组观测基准的第一步，以便更好地将后CE系统与其前CE原生系统联系起来。
{"title":"The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution","authors":"Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈 and Ryan Chornock","doi":"10.3847/1538-4357/ad7500","DOIUrl":"https://doi.org/10.3847/1538-4357/ad7500","url":null,"abstract":"Close binary systems are the progenitors to both Type Ia supernovae and the compact object mergers that can be detected via gravitational waves. To achieve a binary with a small radial separation, it is believed that the system likely undergoes common envelope (CE) evolution. Despite its importance, CE evolution may be one of the largest uncertainties in binary evolution due to a combination of computational challenges and a lack of observed benchmarks where both the post-CE and pre-CE conditions are known. Identifying post-CE systems in star clusters can partially circumvent this second issue by providing an independent age constraint on the system. For the first time, we conduct a systematic search for white dwarf and main-sequence binary systems in 299 Milky Way open star clusters. Coupling Gaia DR3 photometry and kinematics with multiband photometry from Pan-STARRS1 and the Two Micron All Sky Survey, we apply a machine learning-based approach and find 52 high-probability candidates in 38 open clusters. For a subset of our systems, we present follow-up spectroscopy from the Gemini and Lick Observatories and archival light curves from the Transiting Exoplanet Survey Satellite, Kepler/K2, and the Zwicky Transient Facility. Examples of M dwarfs with hot companions are spectroscopically observed, along with regular system variability. While the kinematics of our candidates are consistent with their host clusters, some systems have spatial positions offset relative to their hosts, potentially indicative of natal kicks. Ultimately, this catalog is a first step to obtaining a set of observational benchmarks to better link post-CE systems to their pre-CE progenitors.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142637216","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad83bd
Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro and Benjamin D. Wandelt
We apply a suite of different estimators to the Quijote-png halo catalogs to find the best approach to constrain Primordial non-Gaussianity (PNG) at nonlinear cosmological scales, up to . The set of summary statistics considered in our analysis includes the power spectrum, bispectrum, halo mass function, marked power spectrum, and marked modal bispectrum. Marked statistics are used here for the first time in the context of the PNG study. We perform a Fisher analysis to estimate their cosmological information content, showing substantial improvements when marked observables are added to the analysis. Starting from these summaries, we train deep neural networks to perform likelihood-free inference of cosmological and PNG parameters. We assess the performance of different subsets of summary statistics; in the case of , we find that a combination of the power spectrum and a suitable marked power spectrum outperforms the combination of power spectrum and bispectrum, the baseline statistics usually employed in PNG analysis. A minimal pipeline to analyze the statistics we identified can be implemented either with our ML algorithm or via more traditional estimators, if these are deemed more reliable.
我们对Quijote-png光晕星表应用了一套不同的估计方法，以找到在非线性宇宙学尺度下约束原始非高斯性（PNG）的最佳方法，最高可达......。 我们分析中考虑的一组汇总统计量包括功率谱、双谱、光晕质量函数、标记功率谱和标记模态双谱。这里首次在 PNG 研究中使用了标记统计量。我们通过费雪分析来估算它们的宇宙学信息含量，结果表明在分析中加入标记观测数据后，它们的信息含量有了很大提高。从这些摘要开始，我们训练深度神经网络，对宇宙学参数和 PNG 参数进行无似然推断。我们评估了不同汇总统计子集的性能；在Ⅳ的情况下，我们发现功率谱和合适的标记功率谱的组合优于功率谱和双谱的组合，后者是 PNG 分析中通常采用的基准统计。分析我们确定的统计数据的最小管道可以通过我们的 ML 算法或更传统的估计器（如果这些估计器被认为更可靠的话）来实现。
{"title":"Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity","authors":"Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro and Benjamin D. Wandelt","doi":"10.3847/1538-4357/ad83bd","DOIUrl":"https://doi.org/10.3847/1538-4357/ad83bd","url":null,"abstract":"We apply a suite of different estimators to the Quijote-png halo catalogs to find the best approach to constrain Primordial non-Gaussianity (PNG) at nonlinear cosmological scales, up to . The set of summary statistics considered in our analysis includes the power spectrum, bispectrum, halo mass function, marked power spectrum, and marked modal bispectrum. Marked statistics are used here for the first time in the context of the PNG study. We perform a Fisher analysis to estimate their cosmological information content, showing substantial improvements when marked observables are added to the analysis. Starting from these summaries, we train deep neural networks to perform likelihood-free inference of cosmological and PNG parameters. We assess the performance of different subsets of summary statistics; in the case of , we find that a combination of the power spectrum and a suitable marked power spectrum outperforms the combination of power spectrum and bispectrum, the baseline statistics usually employed in PNG analysis. A minimal pipeline to analyze the statistics we identified can be implemented either with our ML algorithm or via more traditional estimators, if these are deemed more reliable.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142637247","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad8bc1
Austin J. King and Benjamin C. Bromley
Light echoes offer a means of studying protoplanetary disks, including their geometry and composition, even when they are not spatially resolved. We present a test of this approach applied specifically to optically thick, geometrically flared disks around active stars. Here we adopt stellar parameters of an active M dwarf to calculate light echoes for disks and rings with radii that would produce time delays consistent with TESS short cadence (about 2 minutes) time bins. Our results show successful fits to disk parameters, highlighting the potential effectiveness of this method in the search for protoplanetary disks.
光回波提供了一种研究原行星盘的方法，包括它们的几何形状和组成，即使它们没有空间分辨率。我们对这种方法进行了测试，并将其专门应用于活跃恒星周围光学厚度大、几何形状耀斑的星盘。在这里，我们采用一颗活跃的 M 矮星的恒星参数来计算盘和环的光回波，其半径所产生的时间延迟与 TESS 的短周期（约 2 分钟）时间带一致。我们的结果表明，我们成功地拟合了星盘参数，突出了这种方法在搜索原行星盘方面的潜在有效性。
{"title":"Light Echoes of Protoplanetary Disks","authors":"Austin J. King and Benjamin C. Bromley","doi":"10.3847/1538-4357/ad8bc1","DOIUrl":"https://doi.org/10.3847/1538-4357/ad8bc1","url":null,"abstract":"Light echoes offer a means of studying protoplanetary disks, including their geometry and composition, even when they are not spatially resolved. We present a test of this approach applied specifically to optically thick, geometrically flared disks around active stars. Here we adopt stellar parameters of an active M dwarf to calculate light echoes for disks and rings with radii that would produce time delays consistent with TESS short cadence (about 2 minutes) time bins. Our results show successful fits to disk parameters, highlighting the potential effectiveness of this method in the search for protoplanetary disks.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"35 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142637206","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad8229
Dong-Woo Kim and Giuseppina Fabbiano
We explore the evolution of the ∼107 K hot gas in normal galaxies out to redshift = 0.5 (lookback time = 5 Gyr), using X-ray luminosity functions (XLFs) built from a sample of 575 normal galaxies with z < 0.6 detected in five high-galactic-latitude Chandra wide-field surveys. After estimating the emission due to the hot gas component (reducing the sample to ∼400 galaxies), we compared the XLF in three redshift bins (z = 0.1, 0.3, and 0.5), finding increases in the number of galaxies per unit comoving volume from z = 0.1 to 0.3 and then from z = 0.3 to 0.5. These XLF changes suggest a significant (∼5σ) X-ray luminosity evolution of the hot gas, with LX,GAS decreasing by a factor of 6–10 in the last 5 Gyr (from z = 0.5 to 0.1). The relative abundance of LX,GAS ∼ 1041 erg s−1 galaxies at higher z suggests that high-z, moderate-LX,GAS galaxies may be the optimal target to solve the missing baryon problem. In early-type galaxies, this observational trend is qualitatively consistent with (but larger than) the expected time-dependent mass-loss rate in cooling flow models without active galactic nucleus feedback. In late-type galaxies, the observational trend is also qualitatively consistent with (but larger than) the effect of the z-dependent star formation rate.
我们利用从五个高星系纬度钱德拉宽视场巡天中探测到的 575 个 z < 0.6 的正常星系样本建立的 X 射线光度函数（XLFs），探索了正常星系中热气体的演化，直至红移 = 0.5（回望时间 = 5 Gyr）。在估算了热气体成分引起的辐射（将样本减少到 400 个星系）之后，我们比较了三个红移区（z = 0.1、0.3 和 0.5）的 XLF，发现从 z = 0.1 到 0.3，再从 z = 0.3 到 0.5，单位移动体积内的星系数量都在增加。这些 XLF 变化表明热气体的 X 射线光度发生了显著的（∼5σ）演变，LX,GAS 在过去 5 个 Gyr（从 z = 0.5 到 0.1）中减少了 6-10 倍。在更高的z值，LX,GAS ∼ 1041 erg s-1星系的相对丰度表明，高z值、中等LX,GAS星系可能是解决重子缺失问题的最佳目标。在早期型星系中，这种观测趋势与没有活动星系核反馈的冷却流模型中预期的随时间变化的质量损失率在性质上是一致的（但要大于）。在晚型星系中，观测趋势在性质上也符合（但大于）随z变化的恒星形成率的影响。
{"title":"Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5","authors":"Dong-Woo Kim and Giuseppina Fabbiano","doi":"10.3847/1538-4357/ad8229","DOIUrl":"https://doi.org/10.3847/1538-4357/ad8229","url":null,"abstract":"We explore the evolution of the ∼107 K hot gas in normal galaxies out to redshift = 0.5 (lookback time = 5 Gyr), using X-ray luminosity functions (XLFs) built from a sample of 575 normal galaxies with z < 0.6 detected in five high-galactic-latitude Chandra wide-field surveys. After estimating the emission due to the hot gas component (reducing the sample to ∼400 galaxies), we compared the XLF in three redshift bins (z = 0.1, 0.3, and 0.5), finding increases in the number of galaxies per unit comoving volume from z = 0.1 to 0.3 and then from z = 0.3 to 0.5. These XLF changes suggest a significant (∼5σ) X-ray luminosity evolution of the hot gas, with LX,GAS decreasing by a factor of 6–10 in the last 5 Gyr (from z = 0.5 to 0.1). The relative abundance of LX,GAS ∼ 1041 erg s−1 galaxies at higher z suggests that high-z, moderate-LX,GAS galaxies may be the optimal target to solve the missing baryon problem. In early-type galaxies, this observational trend is qualitatively consistent with (but larger than) the expected time-dependent mass-loss rate in cooling flow models without active galactic nucleus feedback. In late-type galaxies, the observational trend is also qualitatively consistent with (but larger than) the effect of the z-dependent star formation rate.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"222 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142643161","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad7fe1
Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose and Archana Gupta
Understanding the origins of massive black hole seeds and their coevolution with their host galaxy requires studying intermediate-mass black holes (IMBHs) and estimating their mass. However, measuring the masses of these IMBHs is challenging, due to the high-spatial-resolution requirement. Spectrophotometric reverberation monitoring is performed for a low-luminosity Seyfert 1 galaxy, NGC 4395, to measure the size of the broad-line region and black hole mass. The data were collected using the 1.3 m Devasthal fast optical telescope and 3.6 m Devasthal optical telescope at ARIES, Nainital, over two consecutive days in 2022 March. The analysis revealed strong emission lines in the spectra and light curves of the merged 5100 Å spectroscopic continuum flux (f5100) with the photometric continuum V band and Hα, with fractional variabilities of 6.38% and 6.31% respectively. In comparison to several previous studies with lag estimation <90 minutes, our calculated Hα lag supersedes them by minutes, using the ICCF and JAVELIN methods. The velocity dispersion (σline) of the broad-line clouds is measured to be km s−1, yielding a black hole mass of ∼ and an Eddington ratio of 0.06.
{"title":"Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395","authors":"Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose and Archana Gupta","doi":"10.3847/1538-4357/ad7fe1","DOIUrl":"https://doi.org/10.3847/1538-4357/ad7fe1","url":null,"abstract":"Understanding the origins of massive black hole seeds and their coevolution with their host galaxy requires studying intermediate-mass black holes (IMBHs) and estimating their mass. However, measuring the masses of these IMBHs is challenging, due to the high-spatial-resolution requirement. Spectrophotometric reverberation monitoring is performed for a low-luminosity Seyfert 1 galaxy, NGC 4395, to measure the size of the broad-line region and black hole mass. The data were collected using the 1.3 m Devasthal fast optical telescope and 3.6 m Devasthal optical telescope at ARIES, Nainital, over two consecutive days in 2022 March. The analysis revealed strong emission lines in the spectra and light curves of the merged 5100 Å spectroscopic continuum flux (f5100) with the photometric continuum V band and Hα, with fractional variabilities of 6.38% and 6.31% respectively. In comparison to several previous studies with lag estimation <90 minutes, our calculated Hα lag supersedes them by minutes, using the ICCF and JAVELIN methods. The velocity dispersion (σline) of the broad-line clouds is measured to be km s−1, yielding a black hole mass of ∼ and an Eddington ratio of 0.06.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142637201","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad70b6
Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke and Ryan J. Cooke
We present the design and first results of the inner circumgalactic medium (CGM) of QSO line-of-sight emitting galaxies at z ∼ 2–3, Keck Baryonic Structure Survey (KBSS)-InCLOSE. The survey will connect galaxy properties (e.g., stellar mass M*, interstellar medium, hereafter ISM, metallicity) with the physical conditions of the inner CGM (e.g., kinematics, metallicity) to directly observe the galaxy-scale baryon cycle. We obtain deep Keck/KCWI optical IFU pointings of KBSS QSOs to discover new star-forming galaxies at small projected distances b ≲ 12″ (98 kpc, ), then obtain follow-up Keck/MOSFIRE near-IR spectra to confirm their redshifts. We leverage KBSS images and Keck/High Resolution Echelle Spectrometer QSO spectra to model stellar populations and inner CGM absorption. In this paper, we analyze two QSO fields and discover more than 15 new galaxies with KCWI, then use MOSFIRE for two galaxies Q2343-G1 (z = 2.43; G1) and Q2233-N1 (z = 3.15; N1), which are both associated with damped Lyα absorbers. We find that G1 has typical M*, UV/optical emission properties. N1 has lower M* with very strong nebular emission. We jointly analyze neutral phase CGM and ionized ISM in N/O (for the first time at this z), dust extinction, and high-ionization CGM finding that G1's CGM is metal poor and less evolved than its ISM, while N1's CGM and ISM abundances are comparable; their CGM shows ∼1 dex less dust extinction than the ISM; and G1's CGM has direct evidence of hot, metal-rich galactic outflow ejecta. These findings support that metals and dust are driven into the CGM from outflows, but may also be, e.g., stripped ISM gas or satellite enrichment. The full KBSS-InCLOSE sample will explore these scenarios.
{"title":"KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 *","authors":"Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke and Ryan J. Cooke","doi":"10.3847/1538-4357/ad70b6","DOIUrl":"https://doi.org/10.3847/1538-4357/ad70b6","url":null,"abstract":"We present the design and first results of the inner circumgalactic medium (CGM) of QSO line-of-sight emitting galaxies at z ∼ 2–3, Keck Baryonic Structure Survey (KBSS)-InCLOSE. The survey will connect galaxy properties (e.g., stellar mass M*, interstellar medium, hereafter ISM, metallicity) with the physical conditions of the inner CGM (e.g., kinematics, metallicity) to directly observe the galaxy-scale baryon cycle. We obtain deep Keck/KCWI optical IFU pointings of KBSS QSOs to discover new star-forming galaxies at small projected distances b ≲ 12″ (98 kpc, ), then obtain follow-up Keck/MOSFIRE near-IR spectra to confirm their redshifts. We leverage KBSS images and Keck/High Resolution Echelle Spectrometer QSO spectra to model stellar populations and inner CGM absorption. In this paper, we analyze two QSO fields and discover more than 15 new galaxies with KCWI, then use MOSFIRE for two galaxies Q2343-G1 (z = 2.43; G1) and Q2233-N1 (z = 3.15; N1), which are both associated with damped Lyα absorbers. We find that G1 has typical M*, UV/optical emission properties. N1 has lower M* with very strong nebular emission. We jointly analyze neutral phase CGM and ionized ISM in N/O (for the first time at this z), dust extinction, and high-ionization CGM finding that G1's CGM is metal poor and less evolved than its ISM, while N1's CGM and ISM abundances are comparable; their CGM shows ∼1 dex less dust extinction than the ISM; and G1's CGM has direct evidence of hot, metal-rich galactic outflow ejecta. These findings support that metals and dust are driven into the CGM from outflows, but may also be, e.g., stripped ISM gas or satellite enrichment. The full KBSS-InCLOSE sample will explore these scenarios.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"18 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142637219","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad808b
Christine Lochmann, Sruthi Purushu Melath, Robert Wild, Ersin Yurtsever, Alberto Martín Santa Daría, Lola González-Sánchez, Francesco A. Gianturco and Roland Wester
We present the temperature-dependent reaction rate coefficients of CN− and C3N− with atomic hydrogen in the temperature range from 7 to 290 K, measured in a 16-pole radio-frequency ion trap. The rate of C3N− with H steadily increases toward lower temperatures, while the rate coefficients for the CN− + H system show a sudden change around 160 K. Fits to the data were performed to determine temperature-dependent reaction rate coefficients. The fits reveal a rate coefficient of cm3 s−1 for C3N− + H. For CN−, we determined a rate coefficient for the temperature regime below 160 K of cm3 s−1. Given our present results, higher rate coefficients than previously reported must be assumed for the modeling of cold interstellar environments involving these H atom reactions.
我们展示了在 16 极射频离子阱中测量到的 CN- 和 C3N- 与原子氢在 7 至 290 K 温度范围内随温度变化的反应速率系数。C3N- 与氢的反应速率随着温度的降低而稳步上升，而 CN- + H 系统的速率系数则在 160 K 附近出现了突变。拟合结果表明，C3N- + H 的速率系数为 cm3 s-1。对于 CN-，我们确定了 160 K 以下温度下的速率系数为 cm3 s-1。鉴于我们目前的结果，在对涉及这些 H 原子反应的寒冷星际环境建模时，必须假设比以前报告的更高的速率系数。
{"title":"Measurements of the Reaction Rate Coefficients of Atomic Hydrogen with Astrochemical Anions: CN− and C3N−","authors":"Christine Lochmann, Sruthi Purushu Melath, Robert Wild, Ersin Yurtsever, Alberto Martín Santa Daría, Lola González-Sánchez, Francesco A. Gianturco and Roland Wester","doi":"10.3847/1538-4357/ad808b","DOIUrl":"https://doi.org/10.3847/1538-4357/ad808b","url":null,"abstract":"We present the temperature-dependent reaction rate coefficients of CN− and C3N− with atomic hydrogen in the temperature range from 7 to 290 K, measured in a 16-pole radio-frequency ion trap. The rate of C3N− with H steadily increases toward lower temperatures, while the rate coefficients for the CN− + H system show a sudden change around 160 K. Fits to the data were performed to determine temperature-dependent reaction rate coefficients. The fits reveal a rate coefficient of cm3 s−1 for C3N− + H. For CN−, we determined a rate coefficient for the temperature regime below 160 K of cm3 s−1. Given our present results, higher rate coefficients than previously reported must be assumed for the modeling of cold interstellar environments involving these H atom reactions.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"31 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142643170","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad856e
Anthony J. Remijan, Zachary T. P. Fried, Ilsa R. Cooke, Gabi Wenzel, Ryan Loomis, Christopher N. Shingledecker, Andrew Lipnicky, Ci Xue, Michael C. McCarthy and Brett A. McGuire
We used new high spectral resolution observations of propynal (HCCCHO) toward TMC-1 and in the laboratory to update the spectral line catalog available for transitions of HCCCHO—specifically at frequencies lower than 30 GHz, which were previously discrepant in a publicly available catalog. The observed astronomical frequencies provided a high enough spectral resolution that, when combined with high-resolution (∼2 kHz) measurements taken in the laboratory, a new, consistent fit to both the laboratory and astronomical data was achieved. Now with a nearly exact (<1 kHz) frequency match to the J = 2–1 and 3–2 transitions in the astronomical data, using a Markov Chain Monte Carlo analysis, a best fit to the total HCCCHO column density of cm−2 was found with a surprisingly low excitation temperature of just over 3 K. This column density is around a factor of 5 times larger than reported in previous studies. Finally, this work highlights that care is needed when using publicly available spectral catalogs to characterize astronomical spectra. The availability of these catalogs is essential to the success of modern astronomical facilities and will only become more important as the next generation of facilities comes online.
{"title":"High Spectral Resolution Observations of Propynal (HCCCHO) toward TMC-1 from the GOTHAM Large Program on the GBT","authors":"Anthony J. Remijan, Zachary T. P. Fried, Ilsa R. Cooke, Gabi Wenzel, Ryan Loomis, Christopher N. Shingledecker, Andrew Lipnicky, Ci Xue, Michael C. McCarthy and Brett A. McGuire","doi":"10.3847/1538-4357/ad856e","DOIUrl":"https://doi.org/10.3847/1538-4357/ad856e","url":null,"abstract":"We used new high spectral resolution observations of propynal (HCCCHO) toward TMC-1 and in the laboratory to update the spectral line catalog available for transitions of HCCCHO—specifically at frequencies lower than 30 GHz, which were previously discrepant in a publicly available catalog. The observed astronomical frequencies provided a high enough spectral resolution that, when combined with high-resolution (∼2 kHz) measurements taken in the laboratory, a new, consistent fit to both the laboratory and astronomical data was achieved. Now with a nearly exact (<1 kHz) frequency match to the J = 2–1 and 3–2 transitions in the astronomical data, using a Markov Chain Monte Carlo analysis, a best fit to the total HCCCHO column density of cm−2 was found with a surprisingly low excitation temperature of just over 3 K. This column density is around a factor of 5 times larger than reported in previous studies. Finally, this work highlights that care is needed when using publicly available spectral catalogs to characterize astronomical spectra. The availability of these catalogs is essential to the success of modern astronomical facilities and will only become more important as the next generation of facilities comes online.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142643215","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad7feb
Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay and Anke van Dyk
We report on XMM-Newton, NuSTAR, and NICER X-ray observations of CTCV J2056–3014, a cataclysmic variable (CV) with one of the fastest-spinning white dwarfs (WDs) at P = 29.6 s. While previously classified as an intermediate polar, CJ2056 also exhibits the properties of WZ Sge–type CVs, such as dwarf novae and superoutbursts. With XMM-Newton and NICER, we detected the spin period up to ∼2 keV with 7σ significance. We constrained its derivative to s s−1 after correcting for binary orbital motion. The pulse profile is characterized by a single broad peak with ∼25% modulation. NuSTAR detected a fourfold increase in unabsorbed X-ray flux coincident with an optical flare, in 2022 November. The XMM-Newton and NICER X-ray spectra at 0.310 keV are best characterized by an absorbed, optically thin three-temperature thermal plasma model (kT = 0.3, 1.0, and 4.9 keV), while the NuSTAR spectra at 3–30 keV are best fit by a single-temperature thermal plasma model (kT = 8.4 keV), both with Fe abundance ZFe/Z⊙ = 0.3. CJ2056 exhibits similarities to other fast-spinning CVs, such as low plasma temperatures and no significant X-ray absorption at low energies. As the WD’s magnetic field strength is unknown, we applied both nonmagnetic and magnetic CV spectral models (MKCFLOW and MCVSPEC) to determine the WD mass. The derived WD mass range (M = 0.7–1.0 M⊙) is above the centrifugal breakup mass limit of 0.56 M⊙ and consistent with the mean WD mass of local CVs (M ≈ 0.8–0.9 M⊙).
{"title":"A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014","authors":"Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay and Anke van Dyk","doi":"10.3847/1538-4357/ad7feb","DOIUrl":"https://doi.org/10.3847/1538-4357/ad7feb","url":null,"abstract":"We report on XMM-Newton, NuSTAR, and NICER X-ray observations of CTCV J2056–3014, a cataclysmic variable (CV) with one of the fastest-spinning white dwarfs (WDs) at P = 29.6 s. While previously classified as an intermediate polar, CJ2056 also exhibits the properties of WZ Sge–type CVs, such as dwarf novae and superoutbursts. With XMM-Newton and NICER, we detected the spin period up to ∼2 keV with 7σ significance. We constrained its derivative to s s−1 after correcting for binary orbital motion. The pulse profile is characterized by a single broad peak with ∼25% modulation. NuSTAR detected a fourfold increase in unabsorbed X-ray flux coincident with an optical flare, in 2022 November. The XMM-Newton and NICER X-ray spectra at 0.310 keV are best characterized by an absorbed, optically thin three-temperature thermal plasma model (kT = 0.3, 1.0, and 4.9 keV), while the NuSTAR spectra at 3–30 keV are best fit by a single-temperature thermal plasma model (kT = 8.4 keV), both with Fe abundance ZFe/Z⊙ = 0.3. CJ2056 exhibits similarities to other fast-spinning CVs, such as low plasma temperatures and no significant X-ray absorption at low energies. As the WD’s magnetic field strength is unknown, we applied both nonmagnetic and magnetic CV spectral models (MKCFLOW and MCVSPEC) to determine the WD mass. The derived WD mass range (M = 0.7–1.0 M⊙) is above the centrifugal breakup mass limit of 0.56 M⊙ and consistent with the mean WD mass of local CVs (M ≈ 0.8–0.9 M⊙).","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142670344","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}
Pub Date : 2024-11-15DOI: 10.3847/1538-4357/ad84f4
Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda and Shinki Oyabu
Determining the inner structure of the molecular torus around an active galactic nucleus is essential for understanding its formation mechanism. However, spatially resolving the torus is difficult because of its small size. To probe the clump conditions in the torus, we therefore perform the systematic velocity-decomposition analyses of the gaseous 12CO rovibrational absorption lines (v = 0 → 1, ΔJ = ±1) at λ ∼ 4.67 μm observed toward four (ultra)luminous infrared galaxies using the high-resolution (R ∼ 5000–10,000) spectroscopy from the Subaru Telescope. We find that each transition has two to five distinct velocity components with different line-of-sight (LOS) velocities (VLOS ∼ −240 to +100 km s−1) and dispersions (σV ∼ 15–190 km s−1), i.e., the components (a), (b), ⋯, beginning with the broadest one in each target, indicating that the tori have clumpy structures. By assuming a hydrostatic disk ( ), we find that the tori has dynamic inner structures, with the innermost component (a) outflowing with velocity ∣VLOS∣ ∼ 160–240 km s−1, and the outer components (b) and (c) outflowing more slowly or infalling with ∣VLOS∣ ≲ 100 km s−1. In addition, we find that the innermost component (a) can be attributed to collisionally excited hot (≳530 K) and dense ( ) clumps, based on the level populations. Conversely, the outer component (b) can be attributed to cold (∼30–140 K) clumps radiatively excited by a far-infrared-to-submillimeter background with a brightness temperature higher than ∼20–400 K. These observational results demonstrate the clumpy and dynamic structure of tori in the presence of background radiation.
确定活动星系核周围分子环的内部结构对于了解其形成机制至关重要。然而，由于环的尺寸较小，很难对其进行空间分辨。为了探究环内的团块状况，我们利用斯巴鲁望远镜的高分辨率（R ∼ 5000-10000）光谱，对气态 12CO 震荡吸收线（v = 0 → 1，ΔJ = ±1）在 λ ∼ 4.67 μm 处观测到的四个（超）亮红外星系进行了系统的速度分解分析。我们发现每个转变都有两到五个不同的速度分量，它们具有不同的视线速度（VLOS ∼ -240 to +100 km s-1）和色散（σV ∼ 15-190 km s-1），即分量(a)、(b)、⋯，从每个目标中最宽的一个分量开始，表明环状结构是团块状的。通过假定一个静水盘（ ），我们发现环状体具有动态的内部结构，最内层的成分（a）以∣VLOS∣ ∼ 160-240 km s-1的速度外流，而外层的成分（b）和（c）则以∣VLOS∣ ≲ 100 km s-1的速度缓慢外流或内陷。此外，我们还发现，最内侧的成分（a）可以归因于碰撞激发的热（≳530 K）和致密（ ）团块，这是基于水平种群。相反，外围部分（b）可以归因于被远红外到亚毫米波背景辐射激发的冷（∼30-140 K）团块，其亮度温度高于∼20-400 K。
{"title":"Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines*","authors":"Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda and Shinki Oyabu","doi":"10.3847/1538-4357/ad84f4","DOIUrl":"https://doi.org/10.3847/1538-4357/ad84f4","url":null,"abstract":"Determining the inner structure of the molecular torus around an active galactic nucleus is essential for understanding its formation mechanism. However, spatially resolving the torus is difficult because of its small size. To probe the clump conditions in the torus, we therefore perform the systematic velocity-decomposition analyses of the gaseous 12CO rovibrational absorption lines (v = 0 → 1, ΔJ = ±1) at λ ∼ 4.67 μm observed toward four (ultra)luminous infrared galaxies using the high-resolution (R ∼ 5000–10,000) spectroscopy from the Subaru Telescope. We find that each transition has two to five distinct velocity components with different line-of-sight (LOS) velocities (VLOS ∼ −240 to +100 km s−1) and dispersions (σV ∼ 15–190 km s−1), i.e., the components (a), (b), ⋯, beginning with the broadest one in each target, indicating that the tori have clumpy structures. By assuming a hydrostatic disk ( ), we find that the tori has dynamic inner structures, with the innermost component (a) outflowing with velocity ∣VLOS∣ ∼ 160–240 km s−1, and the outer components (b) and (c) outflowing more slowly or infalling with ∣VLOS∣ ≲ 100 km s−1. In addition, we find that the innermost component (a) can be attributed to collisionally excited hot (≳530 K) and dense ( ) clumps, based on the level populations. Conversely, the outer component (b) can be attributed to cold (∼30–140 K) clumps radiatively excited by a far-infrared-to-submillimeter background with a brightness temperature higher than ∼20–400 K. These observational results demonstrate the clumpy and dynamic structure of tori in the presence of background radiation.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142670345","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}
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