{"title":"Correction to: TESS light curves of cataclysmic variables – III – More superhump systems among old novae and nova-like variables","authors":"Albert Bruch","doi":"10.1093/mnras/stae1751","DOIUrl":"https://doi.org/10.1093/mnras/stae1751","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"93 5","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141797986","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}
J. Vitorino, J. Loison, V. Wakelam, E. Congiu, F. Dulieu
In comets and in the cold phase of the interstellar medium (ISM), ammonium salts are key molecular species due to their role in the retention of volatile compounds on cold surfaces. In the case of sulphur, the H2S/OCS ratio observed in protostars could be explained by the presence of ammonium hydrosulphide (NH4SH) salts. However, laboratory data on the properties of NH4SH in ISM cold relevant conditions are rather scarce, as they usually focus on the atmosphere of Jupiter. We propose to consolidate the laboratory data regarding NH4SH on grains, by performing temperature programmed desorption experiments and Fourier transform infrared reflection spectroscopy. The salt was also exposed to H atoms to mimic the ISM conditions. NH4SH was found to form in situ at 10 K, from a mixture of ammonia (NH3) and hydrogen sulphide (H2S). The NH4+ infrared feature (1485 cm−1) is the most prominent one at 80 K. As pure species, H2S and NH3 desorb at 76 K and 90 K, respectively, whereas they are released into the gas phase at 153 K when adsorbed in the form of salt. The presence of water delays the desorption of the salt until the very end of the water desorption, but does not affect the desorption kinetics. During H-exposure, the salt is dissociated and no new product was detected. As a comparative study, salts have been included in the Nautilus gas-grain model. The results show a good correlation with the observations of IRAS 16293-2422B, as opposed to when NH2SH is not included in the model.
在彗星和星际介质（ISM）的冷阶段，铵盐是关键的分子物种，因为它们在冷表面保留挥发性化合物方面发挥作用。就硫而言，在原恒星中观测到的 H2S/OCS 比率可以用硫氢化铵（NH4SH）盐的存在来解释。然而，关于 NH4SH 在 ISM 冷相关条件下的特性的实验室数据却相当稀少，因为这些数据通常都集中在木星的大气层中。我们建议通过进行温度编程解吸实验和傅立叶变换红外反射光谱分析来巩固有关 NH4SH 在晶粒上的实验室数据。我们还将盐暴露在 H 原子中，以模拟 ISM 条件。结果发现，NH4SH 是在 10 K 温度下由氨气（NH3）和硫化氢（H2S）的混合物就地形成的。作为纯物种，H2S 和 NH3 分别在开氏 76 度和开氏 90 度时解吸，而当它们以盐的形式被吸附时，则在开氏 153 度时释放到气相中。水的存在会延迟盐的解吸，直到水解吸的最后阶段，但不会影响解吸动力学。在氢暴露过程中，盐被解离，没有检测到新的产物。作为一项比较研究，在 Nautilus 气粒模型中加入了盐。结果表明，与模型中不包含 NH2SH 的情况相比，IRAS 16293-2422B 的观测结果具有很好的相关性。
{"title":"Sulphur storage in cold molecular clouds: the case of the NH4+SH- salt on interstellar dust grains","authors":"J. Vitorino, J. Loison, V. Wakelam, E. Congiu, F. Dulieu","doi":"10.1093/mnras/stae1747","DOIUrl":"https://doi.org/10.1093/mnras/stae1747","url":null,"abstract":"\u0000 In comets and in the cold phase of the interstellar medium (ISM), ammonium salts are key molecular species due to their role in the retention of volatile compounds on cold surfaces. In the case of sulphur, the H2S/OCS ratio observed in protostars could be explained by the presence of ammonium hydrosulphide (NH4SH) salts. However, laboratory data on the properties of NH4SH in ISM cold relevant conditions are rather scarce, as they usually focus on the atmosphere of Jupiter. We propose to consolidate the laboratory data regarding NH4SH on grains, by performing temperature programmed desorption experiments and Fourier transform infrared reflection spectroscopy. The salt was also exposed to H atoms to mimic the ISM conditions. NH4SH was found to form in situ at 10 K, from a mixture of ammonia (NH3) and hydrogen sulphide (H2S). The NH4+ infrared feature (1485 cm−1) is the most prominent one at 80 K. As pure species, H2S and NH3 desorb at 76 K and 90 K, respectively, whereas they are released into the gas phase at 153 K when adsorbed in the form of salt. The presence of water delays the desorption of the salt until the very end of the water desorption, but does not affect the desorption kinetics. During H-exposure, the salt is dissociated and no new product was detected. As a comparative study, salts have been included in the Nautilus gas-grain model. The results show a good correlation with the observations of IRAS 16293-2422B, as opposed to when NH2SH is not included in the model.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"13 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141817147","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":"Correction to: The variability patterns of the TeV blazar PG 1553 + 113 from a decade of MAGIC and multiband observations","authors":"","doi":"10.1093/mnras/stae1563","DOIUrl":"https://doi.org/10.1093/mnras/stae1563","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"114 20","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141822132","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}
Paul H. Goubert, A. Bluck, J. Piotrowska, Roberto Maiolino
{"title":"Correction to: The role of environment and AGN feedback in quenching local galaxies: comparing cosmological hydrodynamical simulations to the SDSS","authors":"Paul H. Goubert, A. Bluck, J. Piotrowska, Roberto Maiolino","doi":"10.1093/mnras/stae1667","DOIUrl":"https://doi.org/10.1093/mnras/stae1667","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"107 26","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141821750","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":"Correction to: The environmental dependence of the stellar mass–gas metallicity relation in Horizon Run 5","authors":"","doi":"10.1093/mnras/stae1699","DOIUrl":"https://doi.org/10.1093/mnras/stae1699","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"101 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141821845","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}
SDSS J083942.11+380526.3 (z = 2.315) is a FeLoBAL quasar that exhibits visible Balmer absorption lines (Hα), implying a significant n = 2 population. The quasar also shows an array of absorption lines, including O I, Ni II, Fe II, Mg II, Al III to C IV and N V. The high-ionization absorption lines such as C IV and Si IV are revealed by slightly blueshifted BAL troughs. The resonance doublets such as Mg II and Al III are saturated but did not reached zero intensity which indicates that the BLR is partially covered. Overall, however, the absorption is predominantly from low-ionization Fe II lines, emitted from ground and excited states up to at least 3.814 eV. This implies that the absorbing gas spans the hydrogen ionization front and extends into the partially ionized zone where neutral hydrogen is certainly present. Notably, the hydrogen line spectrum of the quasar shows no signature of expected Lyα absorption. Instead, the line spectrum shows an unusual Lyα emission characterized by a fully filled emission line spectrum which is a composite of a strong narrow core superposed on a weak broad base. Taking into account the effect of partial covering to BLR, we have extracted a strong DLA trough in Lyα emission region. To fit the spectrum, we performed photoionized model calculations and compared them to the observations. We found that photoionization modeling using CLOUDY can successfully reproduce the main characteristics of the quasar spectrum, and the predicted neutral hydrogen column density arising from the clouds responsible for the low-ionization absorption provides a good match to the extracted DLA trough. This indicates that both the DLA and the low-ionization absorption arise from the same medium that is roughly collocated with the dusty torus.
SDSS J083942.11+380526.3（z = 2.315）是一颗FeLoBAL类星体，它显示出可见的巴尔默吸收线（Hα），这意味着有一个重要的n = 2种群。该类星体还显示出一系列吸收线，包括 O I、Ni II、Fe II、Mg II、Al III 到 C IV 和 N V。Mg II 和 Al III 等共振双线已经饱和，但强度并没有达到零，这表明 BLR 被部分覆盖。不过，总的来说，吸收主要来自低电离铁Ⅱ线，它们由基态和激发态发射，至少高达 3.814 eV。这意味着吸收气体跨越了氢离子化前沿，并延伸到了部分电离区，在那里肯定存在中性氢。值得注意的是，类星体的氢线光谱没有显示出预期的 Lyα 吸收。相反，该线谱显示出一种不寻常的 Lyα 发射，其特点是发射线谱完全填充，是一个强窄核心叠加一个弱宽基底的复合体。考虑到 BLR 部分覆盖的影响，我们在 Lyα 发射区域提取了一个强 DLA 波谷。为了拟合光谱，我们进行了光离子化模型计算，并与观测结果进行了比较。我们发现，利用 CLOUDY 进行的光离子化建模能够成功地再现类星体光谱的主要特征，而由云团引起的低电离吸收所预测的中性氢柱密度与提取的 DLA 波谷非常吻合。这表明，DLA 和低电离吸收都来自同一种介质，而这种介质与尘埃环大致位于同一位置。
{"title":"Discovery of a damped Lyα absorber in the circumnuclear zone of the FeLoBAL quasar SDSS J083942.11+380526.3","authors":"Shengmiao Wu, Xiheng Shi, Nibedita Kalita, Xiang Pan, Qiguo Tian, T. Ji, Shaohua Zhang, Xuejie Dai, Peng Jiang, Chenwei Yang, Hongyan Zhou","doi":"10.1093/mnras/stae1728","DOIUrl":"https://doi.org/10.1093/mnras/stae1728","url":null,"abstract":"\u0000 SDSS J083942.11+380526.3 (z = 2.315) is a FeLoBAL quasar that exhibits visible Balmer absorption lines (Hα), implying a significant n = 2 population. The quasar also shows an array of absorption lines, including O I, Ni II, Fe II, Mg II, Al III to C IV and N V. The high-ionization absorption lines such as C IV and Si IV are revealed by slightly blueshifted BAL troughs. The resonance doublets such as Mg II and Al III are saturated but did not reached zero intensity which indicates that the BLR is partially covered. Overall, however, the absorption is predominantly from low-ionization Fe II lines, emitted from ground and excited states up to at least 3.814 eV. This implies that the absorbing gas spans the hydrogen ionization front and extends into the partially ionized zone where neutral hydrogen is certainly present. Notably, the hydrogen line spectrum of the quasar shows no signature of expected Lyα absorption. Instead, the line spectrum shows an unusual Lyα emission characterized by a fully filled emission line spectrum which is a composite of a strong narrow core superposed on a weak broad base. Taking into account the effect of partial covering to BLR, we have extracted a strong DLA trough in Lyα emission region. To fit the spectrum, we performed photoionized model calculations and compared them to the observations. We found that photoionization modeling using CLOUDY can successfully reproduce the main characteristics of the quasar spectrum, and the predicted neutral hydrogen column density arising from the clouds responsible for the low-ionization absorption provides a good match to the extracted DLA trough. This indicates that both the DLA and the low-ionization absorption arise from the same medium that is roughly collocated with the dusty torus.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"3 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141641576","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}
A. Čeki, H. V. Şenavcı, O. Latković, Ebru Uzunçam, Eda Burcu Yorulmaz, Engin Bahar
This is the first comprehensive study of the eclipsing binaries V527 Dra and V2846 Cyg, based on radial velocities and ground- and space-based light curves. We perform detailed modeling of these data to derive the absolute parameters and the orbital properties of the two systems. V527 Dra is found to be a semi-detached, and V2846 Cyg a contact binary. Both show continual out-of-eclipse variations that can be explained by migrating dark spots of magnetic origin. We also perform the eclipse timing variation (ETV) analysis which reveals that V527 Dra has a tertiary companion whose mass (∼1M⊙) and orbital inclination (∼70○) are additionally constrained by radial velocities. The ETV diagram of V2846 Cyg displays a quadratic trend accompanied by a low-amplitude cyclic variation, likely due to a magnetic cycle, although further eclipse times are needed to provide a clearer explanation. Lastly, we demonstrate a correlation between the variations in spot parameters obtained via light curve modeling for individual orbital cycles and the residual ETVs, essentially confirming the assumption of magnetic activity in both systems.
这是对食双星V527 Dra和V2846 Cyg的首次全面研究，研究以径向速度和地基与天基光曲线为基础。我们对这些数据进行了详细建模，得出了这两个系统的绝对参数和轨道特性。我们发现V527 Dra是一个半分离双星，而V2846 Cyg是一个接触双星。两者都显示出持续的日食外变化，这可以用磁性暗斑的迁移来解释。我们还进行了日食时间变化（ETV）分析，发现V527 Dra有一个三级伴星，其质量（∼1M⊙）和轨道倾角（∼70○）受到径向速度的额外约束。V2846 Cyg的ETV图显示了一个二次曲线趋势，并伴随着低振幅的周期性变化，这很可能是由于磁周期造成的，不过还需要更多的日食时间来提供更清晰的解释。最后，我们展示了通过光曲线建模获得的单个轨道周期的光斑参数变化与残余 ETV 之间的相关性，基本上证实了这两个系统都存在磁活动的假设。
{"title":"Comprehensive analysis of the eclipsing binaries V527 Dra and V2846 Cyg","authors":"A. Čeki, H. V. Şenavcı, O. Latković, Ebru Uzunçam, Eda Burcu Yorulmaz, Engin Bahar","doi":"10.1093/mnras/stae1709","DOIUrl":"https://doi.org/10.1093/mnras/stae1709","url":null,"abstract":"\u0000 This is the first comprehensive study of the eclipsing binaries V527 Dra and V2846 Cyg, based on radial velocities and ground- and space-based light curves. We perform detailed modeling of these data to derive the absolute parameters and the orbital properties of the two systems. V527 Dra is found to be a semi-detached, and V2846 Cyg a contact binary. Both show continual out-of-eclipse variations that can be explained by migrating dark spots of magnetic origin. We also perform the eclipse timing variation (ETV) analysis which reveals that V527 Dra has a tertiary companion whose mass (∼1M⊙) and orbital inclination (∼70○) are additionally constrained by radial velocities. The ETV diagram of V2846 Cyg displays a quadratic trend accompanied by a low-amplitude cyclic variation, likely due to a magnetic cycle, although further eclipse times are needed to provide a clearer explanation. Lastly, we demonstrate a correlation between the variations in spot parameters obtained via light curve modeling for individual orbital cycles and the residual ETVs, essentially confirming the assumption of magnetic activity in both systems.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"90 18","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141642795","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}
S. Chastain, A. J. van der Horst, G. Anderson, L. Rhodes, D. d'Antonio, M. E. Bell, R. Fender, P. J. Hancock, A. Horesh, C. Kouveliotou, K. Mooley, A. Rowlinson, S. Vergani, R. Wijers, P. Woudt
Short gamma-ray bursts (GRBs) are explosive transients caused by binary mergers of compact objects containing at least one neutron star. Multi-wavelength afterglow observations provide constraints on the physical parameters of the jet, its surrounding medium, and the microphysics of the enhanced magnetic fields and accelerated electrons in the blast wave at the front of the jet. The synchrotron radio emission can be tracked for much longer than in other spectral regimes, and it can pin down the evolution of the spectral peak. We present the results of a systematic observing campaign of eight short GRBs with the MeerKAT radio telescope. Additionally, we present observations of four of these short GRBs using the ATCA radio telescope and two of these short GRBs with the e-MERLIN radio telescope. Using these results we report one possible detection of a short GRB afterglow from GRB 230217A and deep upper limits for the rest of our short GRB observations. We use these observations to place constraints on some of the physical parameters, in particular those related to electron acceleration, the circumburst density, and gamma-ray energy efficiency. We discuss how deeper observations with new and upgraded telescopes should be able to determine if the gamma-ray efficiency differs between long and short GRBs. We also report detections of the likely host galaxies for four of the eight GRBs and upper limits for another GRB, increasing the number of detected host galaxies in the radio with implications for the star formation rate in these galaxies.
短伽马射线暴（GRB）是由至少包含一颗中子星的紧凑天体的双星合并引起的爆炸性瞬变。多波长余辉观测为喷流、其周围介质的物理参数以及喷流前端爆炸波中增强磁场和加速电子的微物理学提供了约束条件。同步辐射射电发射的跟踪时间比其他光谱区长得多，而且可以确定光谱峰的演化过程。我们介绍了利用 MeerKAT 射电望远镜对 8 个短 GRB 进行系统观测的结果。此外，我们还利用 ATCA 射电望远镜观测了其中的四个短巨 violentB，利用 e-MERLIN 射电望远镜观测了其中的两个短巨 violentB。利用这些结果，我们报告了从 GRB 230217A 中可能探测到的一个短 GRB 余辉，以及我们对其余短 GRB 观测的深度上限。我们利用这些观测结果对一些物理参数，特别是与电子加速度、环爆密度和伽马射线能量效率有关的参数进行了限制。我们讨论了如何利用新的和升级的望远镜进行更深入的观测，以确定伽马射线效率在长GRB和短GRB之间是否存在差异。我们还报告了探测到的 8 个伽马射线暴中 4 个可能的宿主星系，以及另一个伽马射线暴的上限，从而增加了探测到的射电宿主星系的数量，并对这些星系的恒星形成率产生了影响。
{"title":"Constraints on short gamma-ray burst physics and their host galaxies from systematic radio follow-up campaigns","authors":"S. Chastain, A. J. van der Horst, G. Anderson, L. Rhodes, D. d'Antonio, M. E. Bell, R. Fender, P. J. Hancock, A. Horesh, C. Kouveliotou, K. Mooley, A. Rowlinson, S. Vergani, R. Wijers, P. Woudt","doi":"10.1093/mnras/stae1568","DOIUrl":"https://doi.org/10.1093/mnras/stae1568","url":null,"abstract":"\u0000 Short gamma-ray bursts (GRBs) are explosive transients caused by binary mergers of compact objects containing at least one neutron star. Multi-wavelength afterglow observations provide constraints on the physical parameters of the jet, its surrounding medium, and the microphysics of the enhanced magnetic fields and accelerated electrons in the blast wave at the front of the jet. The synchrotron radio emission can be tracked for much longer than in other spectral regimes, and it can pin down the evolution of the spectral peak. We present the results of a systematic observing campaign of eight short GRBs with the MeerKAT radio telescope. Additionally, we present observations of four of these short GRBs using the ATCA radio telescope and two of these short GRBs with the e-MERLIN radio telescope. Using these results we report one possible detection of a short GRB afterglow from GRB 230217A and deep upper limits for the rest of our short GRB observations. We use these observations to place constraints on some of the physical parameters, in particular those related to electron acceleration, the circumburst density, and gamma-ray energy efficiency. We discuss how deeper observations with new and upgraded telescopes should be able to determine if the gamma-ray efficiency differs between long and short GRBs. We also report detections of the likely host galaxies for four of the eight GRBs and upper limits for another GRB, increasing the number of detected host galaxies in the radio with implications for the star formation rate in these galaxies.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"21 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141641447","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}
Chloe M. Cheng, M. Kriek, Aliza G. Beverage, A. van der Wel, R. Bezanson, F. d’Eugenio, M. Franx, Pavel E. Mancera Pina, A. Nersesian, Martje Slob, K. Suess, P. V. van Dokkum, Po-Feng Wu, A. Gallazzi, S. Zibetti
We present spatially resolved, SSP-equivalent ages, stellar metallicities, and abundance ratios for 456 massive (10.3 ≲ log (M*/M⊙) ≲ 11.8) quiescent galaxies at 0.6 ≲ z ≲ 1.0 from the LEGA-C survey, derived using full-spectrum models. Typically, we find flat age and [Mg/Fe] gradients, and negative [Fe/H] gradients, implying iron-rich cores. We also estimate intrinsic [Fe/H] gradients via forward-modeling. We examine the observed gradients in three age bins. Younger quiescent galaxies typically have negative [Fe/H] gradients and positive age gradients, possibly indicating a recent central starburst. Additionally, this finding suggests that photometrically-measured flat colour gradients in young quiescent galaxies are the result of the positive age and negative metallicity gradients cancelling each other. For older quiescent galaxies, the age gradients become flat and [Fe/H] gradients weaken, though remain negative. Thus, negative colour gradients at older ages are likely driven by metallicity gradients. The diminishing age gradient may result from the starburst fading. Furthermore, the persistence of the [Fe/H] gradients may suggest that the outskirts are simultaneously built up by mergers with lower-metallicity satellites. On the other hand, the gradients could be inherited from the star-forming phase, in which case mergers may not be needed to explain our findings. This work illustrates the need for resolved spectroscopy, instead of just photometry, to measure stellar population gradients. Extending these measurements to higher redshift is imperative for understanding how stellar populations in quiescent galaxies are assembled over cosmic time.
我们利用全谱模型，给出了LEGA-C巡天中456个大质量（10.3 ≲ log (M*/M⊙) ≲ 11.8）、0.6 ≲ z ≲ 1.0的静止星系的空间分辨率、SSP等效年龄、恒星金属性和丰度比。通常情况下，我们会发现平坦的年龄和[Mg/Fe]梯度，以及负的[Fe/H]梯度，这意味着富含铁的核心。我们还通过前向建模估计了内在的[Fe/H]梯度。我们从三个年龄段来研究观测到的梯度。较年轻的静态星系通常具有负的[Fe/H]梯度和正的年龄梯度，这可能表明最近发生了中心星爆。此外，这一发现还表明，在年轻的静止星系中，光度测量到的平坦颜色梯度是正年龄梯度和负金属性梯度相互抵消的结果。对于较老的静止星系，年龄梯度变得平坦，[Fe/H]梯度减弱，但仍为负值。因此，年龄较大时的负颜色梯度很可能是由金属性梯度驱动的。年龄梯度的减弱可能是由于恒星爆发的消退。此外，[Fe/H]梯度的持续存在可能表明，外围星体是通过与低金属性卫星星合并同时形成的。另一方面，梯度可能是从恒星形成阶段继承下来的，在这种情况下，可能不需要合并来解释我们的发现。这项工作说明，测量恒星群梯度需要分辨光谱，而不仅仅是光度测量。要了解静态星系中的恒星群是如何随着宇宙时间的推移而组合起来的，就必须将这些测量扩展到更高的红移。
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Gaseous, disk-halo interfaces are shaped by processes that are critical to galaxy evolution, including gas accretion and outflows. Extraplanar diffuse ionized gas (eDIG) layers are characterized by scale heights that largely exceed those predicted by their temperature, suggesting the presence of turbulent energy injection from star formation feedback. However, the origin of this large scale height remains uncertain. To explore the connection between eDIG and star-forming disks, we present a spatially-resolved case study of a nearby pair of sub-L*, intermediately inclined disk galaxies NGC 3511/3513. We decompose optical nebular lines observed using long-slit spectroscopy into narrow and broad velocity components. In NGC 3511, the broad component has three distinctive characteristics in comparison to the narrow component: (1) significantly higher velocity dispersions (a median 〈σ〉Broad = 24 km s−1compared to 〈σ〉Narrow = 13 km s−1), (2) elevated [N ii]λ6583/Hα and [S ii]λ6716/Hα line ratios, and (3) a rotational velocity lag. These characteristics support the origin of the broad component in an extraplanar, gaseous disk. In NGC 3513, the broad component reveals disk-halo circulation via localized outflows at radius ≲ 1 kpc. For NGC 3511, we test a vertical hydrostatic equilibrium model with pressure support supplied by thermal and turbulent motions. Under this assumption, the eDIG velocity dispersion corresponds to a scale height hz ≳ 0.2 − 0.4 kpc at R = 3 − 5 kpc, a factor of a few above the thermal scale height (hz ≲ 0.1 kpc). This highlights the importance of turbulent motions to the vertical structure of the gaseous, disk-halo interface.
对星系演化至关重要的过程，包括气体吸积和外流，塑造了气态的圆盘-光环界面。平面外弥漫电离气体层（eDIG）的尺度高度大大超过了它们的温度预测值，这表明存在恒星形成反馈的湍流能量注入。然而，这种大尺度高度的起源仍不确定。为了探索 eDIG 与恒星形成盘之间的联系，我们对附近一对亚 L*、中间倾斜的盘状星系 NGC 3511/3513 进行了空间分辨案例研究。我们将使用长缝光谱仪观测到的光学星云线分解为窄速度和宽速度成分。在 NGC 3511 中，与窄分量相比，宽分量有三个显著特点：(1) 明显较高的速度色散（中位数〈σ〉Broad = 24 km s-1，而〈σ〉Narrow = 13 km s-1），(2) [N ii]λ6583/Hα 和 [S ii]λ6716/Hα 线比率升高，以及 (3) 旋转速度滞后。这些特征都支持宽分量起源于一个平面外的气态盘。在 NGC 3513 中，宽分量通过半径 ≲ 1 kpc 的局部外流揭示了圆盘-光环循环。对于 NGC 3511，我们测试了一个由热运动和湍流运动提供压力支持的垂直流体静力学平衡模型。在这一假设下，eDIG速度弥散对应于R = 3 - 5 kpc处的尺度高度hz ≳ 0.2 - 0.4 kpc，比热尺度高度（hz ≲ 0.1 kpc）高出几倍。这凸显了湍流运动对气态盘-光环界面垂直结构的重要性。
{"title":"Spatially resolved properties of extraplanar diffuse ionized gas in NGC 3511 and NGC 3513","authors":"Hanjue Zhu, E. Boettcher, Hsiao-Wen Chen","doi":"10.1093/mnras/stae1708","DOIUrl":"https://doi.org/10.1093/mnras/stae1708","url":null,"abstract":"\u0000 Gaseous, disk-halo interfaces are shaped by processes that are critical to galaxy evolution, including gas accretion and outflows. Extraplanar diffuse ionized gas (eDIG) layers are characterized by scale heights that largely exceed those predicted by their temperature, suggesting the presence of turbulent energy injection from star formation feedback. However, the origin of this large scale height remains uncertain. To explore the connection between eDIG and star-forming disks, we present a spatially-resolved case study of a nearby pair of sub-L*, intermediately inclined disk galaxies NGC 3511/3513. We decompose optical nebular lines observed using long-slit spectroscopy into narrow and broad velocity components. In NGC 3511, the broad component has three distinctive characteristics in comparison to the narrow component: (1) significantly higher velocity dispersions (a median 〈σ〉Broad = 24 km s−1compared to 〈σ〉Narrow = 13 km s−1), (2) elevated [N ii]λ6583/Hα and [S ii]λ6716/Hα line ratios, and (3) a rotational velocity lag. These characteristics support the origin of the broad component in an extraplanar, gaseous disk. In NGC 3513, the broad component reveals disk-halo circulation via localized outflows at radius ≲ 1 kpc. For NGC 3511, we test a vertical hydrostatic equilibrium model with pressure support supplied by thermal and turbulent motions. Under this assumption, the eDIG velocity dispersion corresponds to a scale height hz ≳ 0.2 − 0.4 kpc at R = 3 − 5 kpc, a factor of a few above the thermal scale height (hz ≲ 0.1 kpc). This highlights the importance of turbulent motions to the vertical structure of the gaseous, disk-halo interface.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"17 22","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141647873","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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