Monthly Notices of the Royal Astronomical Society最新文献_第8页

The HYENAS project: a prediction for the X-ray undetected galaxy groups HYENAS项目：对未探测到的X射线星系群的预测

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-10 DOI: 10.1093/mnras/stae2115

Weiguang Cui, Fred Jennings, Romeel Dave, Arif Babul, Ghassem Gozaliasl

{"title":"The HYENAS project: a prediction for the X-ray undetected galaxy groups","authors":"Weiguang Cui, Fred Jennings, Romeel Dave, Arif Babul, Ghassem Gozaliasl","doi":"10.1093/mnras/stae2115","DOIUrl":"https://doi.org/10.1093/mnras/stae2115","url":null,"abstract":"Galaxy groups contain the majority of bound mass with a significant portion of baryons due to the combination of halo mass and abundance (Cui 2024). Hence they serve as a crucial missing piece in the puzzle of galaxy formation and the evolution of large-scale structures in the Universe. In observations, mass-complete group catalogues are normally derived from galaxy redshift surveys detected through various three-dimensional group-finding algorithms. Confirming the reality of such groups, particularly in the X-rays, is critical for ensuring robust studies of galaxy evolution in these environments. Recent works have reported numerous optical groups that are X-ray undetected (see, e.g. Popesso et al. 2024), sparking debates regarding the reasons for the unexpectedly low hot gas fraction in galaxy groups. To address this issue, we utilise zoomed-in simulations of galaxy groups from the novel Hyenas project to explore the range of hot gas fractions within galaxy groups and investigate the intrinsic factors behind the observed variability in X-ray emission. We find that the halo formation time can play a critical role – we see that groups in halos that formed earlier exhibit up to an order of magnitude brighter X-ray luminosities compared to those formed later. This suggests that undetected X-ray groups are preferentially late-formed halos and highlights the connection between gas fraction and halo formation time in galaxy groups. Accounting for these biases in galaxy group identification is essential for advancing our understanding of galaxy formation and achieving precision in cosmological studies.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"138 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177643","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Impact of extragalactic point sources on the low-frequency sky spectrum and cosmic dawn global 21-cm measurements 银河系外点源对低频天空光谱和宇宙曙光全球 21 厘米测量的影响

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-10 DOI: 10.1093/mnras/stae2111

Shikhar Mittal, Girish Kulkarni, Dominic Anstey, Eloy de Lera Acedo

{"title":"Impact of extragalactic point sources on the low-frequency sky spectrum and cosmic dawn global 21-cm measurements","authors":"Shikhar Mittal, Girish Kulkarni, Dominic Anstey, Eloy de Lera Acedo","doi":"10.1093/mnras/stae2111","DOIUrl":"https://doi.org/10.1093/mnras/stae2111","url":null,"abstract":"Contribution of resolved and unresolved extragalactic point sources to the low-frequency sky spectrum is a potentially non-negligible part of the astrophysical foregrounds for cosmic dawn 21-cm experiments. The clustering of such point sources on the sky, combined with the frequency-dependence of the antenna beam, can also make this contribution chromatic. By combining low-frequency measurements of the luminosity function and the angular correlation function of extragalactic point sources, we develop a model for the contribution of these sources to the low-frequency sky spectrum. Using this model, we find that the contribution of sources with flux density &gt;10−6 Jy to the sky-averaged spectrum is smooth and of the order of a few kelvins at 50–200 MHz. We combine this model with measurements of the galactic foreground spectrum and weigh the resultant sky by the beam directivity of the conical log-spiral antenna planned as part of the Radio Experiment for the Analysis of Cosmic Hydrogen (REACH) project. We find that the contribution of point sources to the resultant spectrum is $sim 0.4%$ of the total foregrounds, but still larger by at least an order of magnitude than the standard predictions for the cosmological 21-cm signal. As a result, not accounting for the point-source contribution leads to a systematic bias in 21-cm signal recovery. We show, however, that in the REACH case, this reconstruction bias can be removed by modelling the point-source contribution as a power law with a running spectral index. We make our code publicly available as a Python package labelled epspy.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"43 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177640","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

RT-SNDETR: Real-time Supernova Detection via End-to-End Image Transformers RT-SNDETR：通过端到端图像变换器进行实时超新星探测

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-10 DOI: 10.1093/mnras/stae2107

Zhi-Ren Pan, Bo Qiu, Guang-Wei Li

{"title":"RT-SNDETR: Real-time Supernova Detection via End-to-End Image Transformers","authors":"Zhi-Ren Pan, Bo Qiu, Guang-Wei Li","doi":"10.1093/mnras/stae2107","DOIUrl":"https://doi.org/10.1093/mnras/stae2107","url":null,"abstract":"In large-scale astronomical surveys, traditional supernova detection pipelines rely on complex and relatively inefficient image differencing techniques. This paper proposes an end-to-end deep-learning supernova detection network, the Real-Time SuperNova DEtection TRansformer (RT-SNDETR). This network partially replaces traditional pipelines by integrating image differencing, source detection, and Real-bogus classification, achieving a speed 51.49 times that of the fastest image differencing method, SFFT. Additionally, it remains competitive with methods like YOLO v8, offering a well-balanced trade-off between speed and accuracy. Experimental results highlight RT-SNDETR’s superior performance, with an average precision(AP) of 96.30% on synthetic samples and 76.60% on real supernova samples. It significantly outperforms other detection networks, including RT-DETR (+5.6% AP on synthetic/+5.1% AP on real samples) and Cascade R-CNN (+8.9% AP on synthetic/+28.6% AP on real samples). The incorporation of CycleGAN-based data generation methods plays a significant role in enhancing RT-SNDETR’s performance. These methods simulate realistic PSF variations, enabling the object detection network to learn more robust features and improving its generalization to real supernovae data. Additionally, by integrating unsupervised domain adaptation techniques, RT-SNDETR achieves an AP of 81.70% on real SDSS supernova survey samples. This study demonstrates RT-SNDETR’s potential to significantly enhance both the speed and accuracy of supernova detection, making it a highly effective solution for large-scale astronomical surveys.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"16 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177550","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Dissipated correction map method with trapezoidal rule for the simulations of gravitational waves from spinning compact binary 利用梯形法则的耗散修正图法模拟来自旋转紧凑双星的引力波

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-10 DOI: 10.1093/mnras/stae1997

Junjie Luo, Hong-Hao Zhang, Weipeng Lin

{"title":"Dissipated correction map method with trapezoidal rule for the simulations of gravitational waves from spinning compact binary","authors":"Junjie Luo, Hong-Hao Zhang, Weipeng Lin","doi":"10.1093/mnras/stae1997","DOIUrl":"https://doi.org/10.1093/mnras/stae1997","url":null,"abstract":"The correction map method means extended phase-space algorithm with correction map. In our research, we have developed a correction map method, specifically the dissipated correction map method with trapezoidal rule, for numerical simulations of gravitational waves from spinning compact binary systems. This new correction map method, denoted as $CM3$, has shown remarkable performance in various simulation results, such as phase-space distance, dissipated energy error, and gravitational waveform, closely resembling the high-order precision implicit Gaussian algorithm. When compared with the previously used mid-point map which is denoted as $C_2$, the $CM3$ consistently exhibits a closer alignment with the highly accurate Gaussian algorithm in waveform evolution and orbital trajectory analysis. Through detailed comparisons and analyses, it is evident that $CM3$ outperforms other algorithms, including $CM2$ and $C_2$ mentioned in this paper, in terms of accuracy and precision in simulating spinning compact binary systems. The incorporation of the trapezoidal rule and the optimization with a scale factor $gamma$ have significantly enhanced the performance of $CM3$, making it a promising method for future numerical simulations in astrophysics. With the groundbreaking detection of gravitational waves by the LIGO/VIRGO collaboration, interest in this research domain has soared. Our work contributes valuable insights for the application of matched filtering techniques in the analysis of gravitational wave signals, enhancing the precision and reliability of these detection.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"10 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177551","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The MAGPI Survey: Orbital distributions, intrinsic shapes, and mass profiles for MAGPI-like Eagle galaxies using Schwarzschild dynamical models MAGPI 巡天观测：使用施瓦兹柴尔德动力学模型的 MAGPI 样鹰星系的轨道分布、本征形状和质量剖面图

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-10 DOI: 10.1093/mnras/stae2114

Giulia Santucci, Claudia Del P Lagos, Katherine E Harborne, Caro Derkenne, Adriano Poci, Sabine Thater, Richard M McDermid, J Trevor Mendel, Emily Wisnioski, Scott M Croom, Anna Ferré-Mateu, Eric G M Muller, Jesse van de Sande, Gauri Sharma, Sarah M Sweet, Takafumi Tsukui, Lucas M Valenzuela, Glenn van de Ven, Tayyaba Zafar

{"title":"The MAGPI Survey: Orbital distributions, intrinsic shapes, and mass profiles for MAGPI-like Eagle galaxies using Schwarzschild dynamical models","authors":"Giulia Santucci, Claudia Del P Lagos, Katherine E Harborne, Caro Derkenne, Adriano Poci, Sabine Thater, Richard M McDermid, J Trevor Mendel, Emily Wisnioski, Scott M Croom, Anna Ferré-Mateu, Eric G M Muller, Jesse van de Sande, Gauri Sharma, Sarah M Sweet, Takafumi Tsukui, Lucas M Valenzuela, Glenn van de Ven, Tayyaba Zafar","doi":"10.1093/mnras/stae2114","DOIUrl":"https://doi.org/10.1093/mnras/stae2114","url":null,"abstract":"Schwarzschild dynamical models are now regularly employed in large surveys of galaxies in the local and distant Universe to derive information on galaxies’ intrinsic properties such as their orbital structure and their (dark matter and stellar) mass distribution. Comparing the internal orbital structures and mass distributions of galaxies in the distant Universe with simulations is key to understanding what physical processes are responsible for shaping galaxy properties. However it is first crucial to understand whether observationally derived properties are directly comparable with intrinsic ones in simulations. To assess this, we build Schwarzschild dynamical models for MUSE-like IFS cubes (constructed to be like those obtained by the MAGPI survey) of 75 galaxies at z ∼ 0.3 from the Eagle simulations. We compare the true particle-derived properties with the galaxies’ model-derived properties. In general, we find that the models can recover the true galaxy properties qualitatively well, with the exception of the enclosed dark matter, where we find a median offset of 48%, which is due to the assumed NFW profile not being able to reproduce the dark matter distribution in the inner region of the galaxies. We then compare our model-derived properties with Schwarzschild models-derived properties of observed MAGPI galaxies and find good agreement between MAGPI and Eagle: the majority of our galaxies (57%) have non-oblate shapes within 1 effective radius. More triaxial galaxies show higher fractions of hot orbits in their inner regions and tend to be more radially anisotropic.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"17 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177549","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Rapid automatic multiple moving objects detection method based on feature extraction from images with non-sidereal tracking 基于图像特征提取和非实时跟踪的多移动物体快速自动检测方法

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-09 DOI: 10.1093/mnras/stae2073

Lei Wang, Xiaoming Zhang, Chunhai Bai, Haiwen Xie, Juan Li, Jiayi Ge, Jianfeng Wang, Xianqun Zeng, Jiantao Sun, Xiaojun Jiang

{"title":"Rapid automatic multiple moving objects detection method based on feature extraction from images with non-sidereal tracking","authors":"Lei Wang, Xiaoming Zhang, Chunhai Bai, Haiwen Xie, Juan Li, Jiayi Ge, Jianfeng Wang, Xianqun Zeng, Jiantao Sun, Xiaojun Jiang","doi":"10.1093/mnras/stae2073","DOIUrl":"https://doi.org/10.1093/mnras/stae2073","url":null,"abstract":"Optically observing and monitoring moving objects, both natural and artificial, is important to human space security. Non-sidereal tracking can improve the system’s limiting magnitude for moving objects, which benefits the surveillance. However, images with non-sidereal tracking include complex background, as well as objects with different brightness and moving mode, posing a significant challenge for accurate multi-object detection in such images, especially in wide field of view (WFOV) telescope images. To achieve a higher detection precision in a higher speed, we proposed a novel object detection method, which combines the source feature extraction and the neural network. First, our method extracts object features from optical images such as centroid, shape, and flux. Then it conducts a naive labeling based on those features to distinguish moving objects from stars. After balancing the labeled data, we employ it to train a neural network aimed at creating a classification model for point-like and streak-like objects. Ultimately, based on the neural network model’s classification outcomes, moving objects whose motion modes consistent with the tracked objects are detected via track association, while objects with different motion modes are detected using morphological statistics. The validation, based on the space objects images captured in target tracking mode with the 1-meter telescope at Nanshan, Xinjiang Astronomical Observatory, demonstrates that our method achieves 94.72% detection accuracy with merely 5.02% false alarm rate, and a processing time of 0.66s per frame. Consequently, our method can rapidly and accurately detect objects with different motion modes from wide-field images with non-sidereal tracking.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"9 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177553","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The origin of the Hα line profiles in simulated disc galaxies 模拟圆盘星系中 Hα 线剖面的起源

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-07 DOI: 10.1093/mnras/stae2099

Timmy Ejdetjärn, Oscar Agertz, Göran Östlin, Martin P Rey, Florent Renaud

{"title":"The origin of the Hα line profiles in simulated disc galaxies","authors":"Timmy Ejdetjärn, Oscar Agertz, Göran Östlin, Martin P Rey, Florent Renaud","doi":"10.1093/mnras/stae2099","DOIUrl":"https://doi.org/10.1093/mnras/stae2099","url":null,"abstract":"Observations of ionised Hα gas in high-redshift disc galaxies have ubiquitously found significant line broadening, σHα ∼ 10 − 100 km s−1. To understand whether this broadening reflects gas turbulence within the interstellar medium (ISM) of galactic discs, or arises from out-of-plane emission in mass-loaded outflows, we perform radiation hydrodynamic (RHD) simulations of isolated Milky Way-mass disc galaxies in a gas-poor (low-redshift) and gas rich (high-redshift) condition and create mock Hα emission line profiles. We find that the majority of the total (integrated) Hα emission is confined within the ISM, with extraplanar gas contributing $sim 45~{{%}}$ of the extended profile wings (vz ≥ 200${, rm {km, s^{-1}} }$) in the gas-rich galaxy. This substantiates using the Hα emission line as a tracer of mid-plane disc dynamics. We investigate the relative contribution of diffuse and dense Hα emitting gas, corresponding to diffuse ionised gas (DIG; ρ ≲ 0.1 cm−3, T ∼ 8 000 K) and HII regions (ρ ≳ 10 cm−3, T ∼ 10 000 K), respectively, and find that DIG contributes $f_{rm DIG}lesssim 10~{{%}}$ of the total LHα. However, the DIG can reach upwards of σHα ∼ 60 − 80 km s−1 while the HII regions are much less turbulent σHα ∼ 10 − 40 km s−1. This implies that the σHα observed using the full Hα emission line is dependent on the relative Hα contribution from DIG/HII regions and a larger fDIG would shift σHα to higher values. Finally, we show that σHα evolves, in both the DIG and HII regions, with the galaxy gas fraction. Our high-redshift equivalent galaxy is roughly twice as turbulent, except for in the DIG which has a more shallow evolution.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"4 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177552","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A targeted search for strongly lensed supernovae with the Las Cumbres Observatory 利用拉斯坎布雷斯天文台有针对性地搜索强透镜超新星

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-07 DOI: 10.1093/mnras/stae2103

Peter Craig, Kyle O’Connor, Sukanya Chakrabarti, Steven A Rodney, Justin R Pierel, Curtis McCully, Ismael Perez-Fournon

{"title":"A targeted search for strongly lensed supernovae with the Las Cumbres Observatory","authors":"Peter Craig, Kyle O’Connor, Sukanya Chakrabarti, Steven A Rodney, Justin R Pierel, Curtis McCully, Ismael Perez-Fournon","doi":"10.1093/mnras/stae2103","DOIUrl":"https://doi.org/10.1093/mnras/stae2103","url":null,"abstract":"Gravitationally lensed supernovae (glSNe) are of interest for time delay cosmology and SN physics. However, glSNe detections are rare, owing to the intrinsic rarity of SN explosions, the necessity of alignment with a foreground lens, and the relatively short window of detectability. We present the Las Cumbres Observatory Lensed Supernova Search, LCOLSS, a targeted survey designed for detecting glSNe in known strong lensing systems. Using cadenced r′-band imaging, LCOLSS targeted 114 galaxy-galaxy lensing systems with high expected SN rates, based on estimated star formation rates. No plausible glSN was detected by LCOLSS during our two year observing program. We carry out an analysis here to measure a detection efficiency for these observations. We then perform Monte Carlo simulations using the predicted supernova rates to determine the expected number of glSN detections. The results of the simulation suggest an expected number of detections and $68%$ Poisson confidence intervals, NSN = 0.20, [0, 2.1], NIa = 0.08, [0, 2.0], NCC = 0.12, [0, 2.0], for all SNe, Type Ia SNe, and core-collapse (CC) SNe respectively. These results are broadly consistent with the absence of a detection in our survey. Analysis of the survey strategy can provide insights for future efforts to develop targeted glSN discovery programs, especially considering the large anticipated yields of upcoming surveys.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"2020 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177555","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Mean-motion resonances with interfering density waves 具有干涉密度波的均动共振

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-07 DOI: 10.1093/mnras/stae2097

Huan Yang, Ya-Ping Li

{"title":"Mean-motion resonances with interfering density waves","authors":"Huan Yang, Ya-Ping Li","doi":"10.1093/mnras/stae2097","DOIUrl":"https://doi.org/10.1093/mnras/stae2097","url":null,"abstract":"In this work, we study the dynamics of two less massive objects moving around a central massive object, which are all embedded within a thin accretion disc. In addition to the gravitational interaction between these objects, the disc-object interaction is also crucial for describing the long-term dynamics of the multi-body system, especially in the regime of mean-motion resonances. We point out that near the resonance the density waves generated by the two moving objects generally coherently interfere with each other, giving rise to extra angular momentum fluxes. The resulting backreaction on the objects is derived within the thin-disc scenario, which explicitly depends on the resonant angle and sensitively depends on the smoothing scheme used in the two-dimensional theory. We have performed hydrodynamical simulations with planets embedded within a thin accretion disc and have found qualitatively agreement on the signatures of interfering density waves by measuring the torques on the embedded objects, for the cases of 2 : 1 and 3 : 2 resonance. By including in interference torque and the migration torques in the evolution of a pair of planets, we show that the chance of resonance trapping depends on the sign of the interference torque. For negative interference torques the pairs are more likely located at off-resonance regimes. The negative interference torques may also explain the $1~{{%}}-2~{{%}}$ offset (for the period ratios) from the exact resonance values as observed in Kepler multi-planet systems.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"32 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177554","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The symbiotic recurrent nova V745 Sco at radio wavelengths 射电波长下的共生周期新星V745 Sco

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-07 DOI: 10.1093/mnras/stae2093

Isabella Molina, Laura Chomiuk, Justin D Linford, Elias Aydi, Amy J Mioduszewski, Koji Mukai, Kirill V Sokolovsky, Jay Strader, Peter Craig, Dillon Dong, Chelsea E Harris, Miriam M Nyamai, Michael P Rupen, Jennifer L Sokoloski, Frederick M Walter, Jennifer H S Weston, Montana N Williams

{"title":"The symbiotic recurrent nova V745 Sco at radio wavelengths","authors":"Isabella Molina, Laura Chomiuk, Justin D Linford, Elias Aydi, Amy J Mioduszewski, Koji Mukai, Kirill V Sokolovsky, Jay Strader, Peter Craig, Dillon Dong, Chelsea E Harris, Miriam M Nyamai, Michael P Rupen, Jennifer L Sokoloski, Frederick M Walter, Jennifer H S Weston, Montana N Williams","doi":"10.1093/mnras/stae2093","DOIUrl":"https://doi.org/10.1093/mnras/stae2093","url":null,"abstract":"V745 Sco is a Galactic symbiotic recurrent nova with nova eruptions in 1937, 1989 and 2014. We study the behaviour of V745 Sco at radio wavelengths (0.6–37 GHz), covering both its 1989 and 2014 eruptions and informed by optical, X-ray, and γ-ray data. The radio light curves are synchrotron-dominated. Surprisingly, compared to expectations for synchrotron emission from explosive transients such as radio supernovae, the light curves spanning 0.6–37 GHz all peak around the same time (∼18–26 days after eruption) and with similar flux densities (5–9 mJy). We model the synchrotron light curves as interaction of the nova ejecta with the red giant wind, but find that simple spherically symmetric models with wind-like circumstellar material (CSM) cannot explain the radio light curve. Instead, we conclude that the shock suddenly breaks out of a dense CSM absorbing screen around 20 days after eruption, and then expands into a relatively low density wind ($dot{M}_{out} approx 10^{-9}-10^{-8}$ M⊙ yr−1 for vw = 10 km s−1) out to ∼1 year post-eruption. The dense, close-in CSM may be an equatorial density enhancement or a more spherical red giant wind with $dot{M}_{in} approx [5-10] times 10^{-7}$ M⊙ yr−1, truncated beyond several × 1014 cm. The outer lower-density CSM would not be visible in typical radio observations of Type Ia supernovae: V745 Sco cannot be ruled out as a Type Ia progenitor based on CSM constraints alone. Complementary constraints from the free–free radio optical depth and the synchrotron luminosity imply the shock is efficient at accelerating relativistic electrons and amplifying magnetic fields, with εe and εB ≈ 0.01 − 0.1.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"9 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177560","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0