Annular substructures in protoplanetary discs, ubiquitous in sub-mm observations, can be caused by gravitational coupling between a disc and its embedded planets. Planetary density waves inject angular momentum into the disc leading to gap opening only after travelling some distance and steepening into shocks (in the absence of linear damping); no angular momentum is deposited in the planetary coorbital region, where the wave has not shocked yet. Despite that, simulations show mass evacuation from the coorbital region even in inviscid discs, leading to smooth, double-trough gap profiles. Here we consider the early, time-dependent stages of planetary gap opening in inviscid discs. We find that an often-overlooked contribution to the angular momentum balance caused by the time-variability of the specific angular momentum of the disc fluid (caused, in turn, by the time-variability of the radial pressure support) plays a key role in gap opening. Focusing on the regime of shallow gaps with depths of $lesssim 20~{{%}}$, we demonstrate analytically that early gap opening is a self-similar process, with the amplitude of the planet-driven perturbation growing linearly in time and the radial gap profile that can be computed semi-analytically. We show that mass indeed gets evacuated from the coorbital region even in inviscid discs. This evolution pattern holds even in viscous discs over a limited period of time. These results are found to be in excellent agreement with 2D numerical simulations. Our simple gap evolution solutions can be used in studies of dust dynamics near planets and for interpreting protoplanetary disc observations.
{"title":"Early stages of gap opening by planets in protoplanetary discs","authors":"Amelia J Cordwell, Roman R Rafikov","doi":"10.1093/mnras/stae2089","DOIUrl":"https://doi.org/10.1093/mnras/stae2089","url":null,"abstract":"Annular substructures in protoplanetary discs, ubiquitous in sub-mm observations, can be caused by gravitational coupling between a disc and its embedded planets. Planetary density waves inject angular momentum into the disc leading to gap opening only after travelling some distance and steepening into shocks (in the absence of linear damping); no angular momentum is deposited in the planetary coorbital region, where the wave has not shocked yet. Despite that, simulations show mass evacuation from the coorbital region even in inviscid discs, leading to smooth, double-trough gap profiles. Here we consider the early, time-dependent stages of planetary gap opening in inviscid discs. We find that an often-overlooked contribution to the angular momentum balance caused by the time-variability of the specific angular momentum of the disc fluid (caused, in turn, by the time-variability of the radial pressure support) plays a key role in gap opening. Focusing on the regime of shallow gaps with depths of $lesssim 20~{{%}}$, we demonstrate analytically that early gap opening is a self-similar process, with the amplitude of the planet-driven perturbation growing linearly in time and the radial gap profile that can be computed semi-analytically. We show that mass indeed gets evacuated from the coorbital region even in inviscid discs. This evolution pattern holds even in viscous discs over a limited period of time. These results are found to be in excellent agreement with 2D numerical simulations. Our simple gap evolution solutions can be used in studies of dust dynamics near planets and for interpreting protoplanetary disc observations.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"9 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177572","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}
Robert Zimmerman, David A van Dyk, Vinay L Kashyap, Aneta Siemiginowska
We present a new method to distinguish between different states (e.g., high and low, quiescent and flaring) in astronomical sources with count data. The method models the underlying physical process as latent variables following a continuous-space Markov chain that determines the expected Poisson counts in observed light curves in multiple passbands. For the underlying state process, we consider several autoregressive processes, yielding continuous-space hidden Markov models of varying complexity. Under these models, we can infer the state that the object is in at any given time. The continuous state predictions from these models are then dichotomized with the help of a finite mixture model to produce state classifications. We apply these techniques to X-ray data from the active dMe flare star EV Lac, splitting the data into quiescent and flaring states. We find that a first-order vector autoregressive process efficiently separates flaring from quiescence: flaring occurs over 30–40% of the observation durations, a well-defined persistent quiescent state can be identified, and the flaring state is characterized by higher plasma temperatures and emission measures.
我们提出了一种新方法来区分天文源计数数据的不同状态（如高和低、静止和闪烁）。该方法将基本物理过程建模为一个连续空间马尔可夫链的潜变量，该连续空间马尔可夫链决定了多通带观测光曲线中的预期泊松计数。对于基本状态过程，我们考虑了几个自回归过程，从而得到复杂程度不同的连续空间隐马尔可夫模型。根据这些模型，我们可以推断出天体在任何给定时间内所处的状态。在有限混合模型的帮助下，这些模型的连续状态预测结果会被二分，从而产生状态分类。我们将这些技术应用于活跃的 dMe耀斑恒星 EV Lac 的 X 射线数据，将数据分为静态和耀斑状态。我们发现，一个一阶矢量自回归过程可以有效地将耀斑和静止状态区分开来：耀斑发生在 30-40% 的观测持续时间内，可以识别出一个定义明确的持续静止状态，而耀斑状态的特点是等离子体温度和发射测量值较高。
{"title":"Separating States in Astronomical Sources Using Hidden Markov Models: With a Case Study of Flaring and Quiescence on EV Lac","authors":"Robert Zimmerman, David A van Dyk, Vinay L Kashyap, Aneta Siemiginowska","doi":"10.1093/mnras/stae2082","DOIUrl":"https://doi.org/10.1093/mnras/stae2082","url":null,"abstract":"We present a new method to distinguish between different states (e.g., high and low, quiescent and flaring) in astronomical sources with count data. The method models the underlying physical process as latent variables following a continuous-space Markov chain that determines the expected Poisson counts in observed light curves in multiple passbands. For the underlying state process, we consider several autoregressive processes, yielding continuous-space hidden Markov models of varying complexity. Under these models, we can infer the state that the object is in at any given time. The continuous state predictions from these models are then dichotomized with the help of a finite mixture model to produce state classifications. We apply these techniques to X-ray data from the active dMe flare star EV Lac, splitting the data into quiescent and flaring states. We find that a first-order vector autoregressive process efficiently separates flaring from quiescence: flaring occurs over 30–40% of the observation durations, a well-defined persistent quiescent state can be identified, and the flaring state is characterized by higher plasma temperatures and emission measures.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"168 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177567","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}
Void number counts (VNC) indicates the number of low-density regions in the large-scale structure (LSS) of the Universe, and we propose to use it as an effective cosmological probe. By generating the galaxy mock catalog based on Jiutian simulations and considering the spectroscopic survey strategy and instrumental design of the China Space Station Telescope (CSST), which can reach a magnitude limit ∼23 AB mag and spectral resolution R ≳ 200 with a sky coverage 17,500 deg2, we identify voids using the watershed algorithm without any assumption of void shape, and obtain the mock void catalog and data of the VNC in six redshift bins from z = 0.3 to1.3. We use the Markov Chain Monte Carlo (MCMC) method to constrain the cosmological and VNC parameters. The void linear underdensity threshold δv in the theoretical model is set to be a free parameter at a given redshift to fit the VNC data and explore its redshift evolution. We find that, the VNC can correctly derive the cosmological information, and the constraint strength on the cosmological parameters is comparable to that from the void size function (VSF) method, which can reach a few percentage level in the CSST full spectroscopic survey. This is because that, since the VNC is not sensitive to void shape, the modified theoretical model can match the data better by integrating over void features, and more voids could be included in the VNC analysis by applying simpler selection criteria, which will improve the statistical significance. It indicates that the VNC can be an effective cosmological probe for exploring the LSS.
{"title":"Void Number Counts as a cosmological probe for the large-scale structure","authors":"Yingxiao Song, Qi Xiong, Yan Gong, Furen Deng, Kwan Chuen Chan, Xuelei Chen, Qi Guo, Yun Liu, Wenxiang Pei","doi":"10.1093/mnras/stae2094","DOIUrl":"https://doi.org/10.1093/mnras/stae2094","url":null,"abstract":"Void number counts (VNC) indicates the number of low-density regions in the large-scale structure (LSS) of the Universe, and we propose to use it as an effective cosmological probe. By generating the galaxy mock catalog based on Jiutian simulations and considering the spectroscopic survey strategy and instrumental design of the China Space Station Telescope (CSST), which can reach a magnitude limit ∼23 AB mag and spectral resolution R ≳ 200 with a sky coverage 17,500 deg2, we identify voids using the watershed algorithm without any assumption of void shape, and obtain the mock void catalog and data of the VNC in six redshift bins from z = 0.3 to1.3. We use the Markov Chain Monte Carlo (MCMC) method to constrain the cosmological and VNC parameters. The void linear underdensity threshold δv in the theoretical model is set to be a free parameter at a given redshift to fit the VNC data and explore its redshift evolution. We find that, the VNC can correctly derive the cosmological information, and the constraint strength on the cosmological parameters is comparable to that from the void size function (VSF) method, which can reach a few percentage level in the CSST full spectroscopic survey. This is because that, since the VNC is not sensitive to void shape, the modified theoretical model can match the data better by integrating over void features, and more voids could be included in the VNC analysis by applying simpler selection criteria, which will improve the statistical significance. It indicates that the VNC can be an effective cosmological probe for exploring the LSS.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"152 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177562","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}
L Bigwood, A Amon, A Schneider, J Salcido, I G McCarthy, C Preston, D Sanchez, D Sijacki, E Schaan, S Ferraro, N Battaglia, A Chen, S Dodelson, A Roodman, A Pieres, A Ferté, A Alarcon, A Drlica-Wagner, A Choi, A Navarro-Alsina, A Campos, A J Ross, A Carnero Rosell, B Yin, B Yanny, C Sánchez, C Chang, C Davis, C Doux, D Gruen, E S Rykoff, E M Huff, E Sheldon, F Tarsitano, F Andrade-Oliveira, G M Bernstein, G Giannini, H T Diehl, H Huang, I Harrison, I Sevilla-Noarbe, I Tutusaus, J Elvin-Poole, J McCullough, J Zuntz, J Blazek, J DeRose, J Cordero, J Prat, J Myles, K Eckert, K Bechtol, K Herner, L F Secco, M Gatti, M Raveri, M Carrasco Kind, M R Becker, M A Troxel, M Jarvis, N MacCrann, O Friedrich, O Alves, P-F Leget, R Chen, R P Rollins, R H Wechsler, R A Gruendl, R Cawthon, S Allam, S L Bridle, S Pandey, S Everett, T Shin, W G Hartley, X Fang, Y Zhang, M Aguena, J Annis, D Bacon, E Bertin, S Bocquet, D Brooks, J Carretero, F J Castander, L N da Costa, M E S Pereira, J De Vicente, S Desai, P Doel, I Ferrero, B Flaugher, J Frieman, J García-Bellido, E Gaztanaga, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D Huterer, D J James, K Kuehn, O Lahav, S Lee, J L Marshall, J Mena-Fernández, R Miquel, J Muir, M Paterno, A A Plazas Malagón, A Porredon, A K Romer, S Samuroff, E Sanchez, D Sanchez Cid, M Smith, M Soares-Santos, E Suchyta, M E C Swanson, G Tarle, C To, N Weaverdyck, J Weller, P Wiseman, M Yamamoto
Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev-Zel’dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, ‘baryonification’. First, using WL only, we compare the S8 constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of S8 and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters, with the joint WL + kSZ analysis constraining $S_8=0.823^{+0.019}_{-0.020}$. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.
{"title":"Weak lensing combined with the kinetic Sunyaev Zel’dovich effect: A study of baryonic feedback","authors":"L Bigwood, A Amon, A Schneider, J Salcido, I G McCarthy, C Preston, D Sanchez, D Sijacki, E Schaan, S Ferraro, N Battaglia, A Chen, S Dodelson, A Roodman, A Pieres, A Ferté, A Alarcon, A Drlica-Wagner, A Choi, A Navarro-Alsina, A Campos, A J Ross, A Carnero Rosell, B Yin, B Yanny, C Sánchez, C Chang, C Davis, C Doux, D Gruen, E S Rykoff, E M Huff, E Sheldon, F Tarsitano, F Andrade-Oliveira, G M Bernstein, G Giannini, H T Diehl, H Huang, I Harrison, I Sevilla-Noarbe, I Tutusaus, J Elvin-Poole, J McCullough, J Zuntz, J Blazek, J DeRose, J Cordero, J Prat, J Myles, K Eckert, K Bechtol, K Herner, L F Secco, M Gatti, M Raveri, M Carrasco Kind, M R Becker, M A Troxel, M Jarvis, N MacCrann, O Friedrich, O Alves, P-F Leget, R Chen, R P Rollins, R H Wechsler, R A Gruendl, R Cawthon, S Allam, S L Bridle, S Pandey, S Everett, T Shin, W G Hartley, X Fang, Y Zhang, M Aguena, J Annis, D Bacon, E Bertin, S Bocquet, D Brooks, J Carretero, F J Castander, L N da Costa, M E S Pereira, J De Vicente, S Desai, P Doel, I Ferrero, B Flaugher, J Frieman, J García-Bellido, E Gaztanaga, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D Huterer, D J James, K Kuehn, O Lahav, S Lee, J L Marshall, J Mena-Fernández, R Miquel, J Muir, M Paterno, A A Plazas Malagón, A Porredon, A K Romer, S Samuroff, E Sanchez, D Sanchez Cid, M Smith, M Soares-Santos, E Suchyta, M E C Swanson, G Tarle, C To, N Weaverdyck, J Weller, P Wiseman, M Yamamoto","doi":"10.1093/mnras/stae2100","DOIUrl":"https://doi.org/10.1093/mnras/stae2100","url":null,"abstract":"Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev-Zel’dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, ‘baryonification’. First, using WL only, we compare the S8 constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of S8 and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters, with the joint WL + kSZ analysis constraining $S_8=0.823^{+0.019}_{-0.020}$. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"2 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177566","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}
We decomposed the molecular gas in the spiral galaxy NGC 628 (M74) into multi-scale hub-filament structures using the CO (2−1) line by the dendrogram algorithm. All leaf structures as potential hubs were classified into three categories, i.e. leaf-HFs-A, leaf-HFs-B and leaf-HFs-C. leaf-HFs-A exhibit the best hub-filament morphology, which also have the highest density contrast, the largest mass and the lowest virial ratio. We employed the FILFINDER algorithm to identify and characterize filaments within 185 leaf-HFs-A structures, and fitted the velocity gradients around the intensity peaks. Measurements of velocity gradients provide evidence for gas inflow within these structures, which can serve as a kinematic evidence that these structures are hub-filament structures. The numbers of the associated 21 μm and Hα structures and the peak intensities of 7.7 μm, 21 μm and Hα emissions decrease from leaf-HFs-A to leaf-HFs-C. The spatial separations between the intensity peaks of CO and 21 μm structures of leaf-HFs-A are larger than those of leaf-HFs-C. These evidence indicate that leaf-HFs-A are more evolved than leaf-HFs-C. There may be an evolutionary sequence from leaf-HFs-C to leaf-HFs-A. Currently, leaf-HFs-C lack a distinct gravitational collapse process that would result in a significant density contrast. The density contrast can effectively measure the extent of the gravitational collapse and the depth of the gravitational potential of the structure which, in turn, shapes the hub-filament morphology. Combined with the kinematic analysis presented in previous studies, a picture emerges that molecular gas in spiral galaxies is organized into network structures through the gravitational coupling of multi-scale hub-filament structures. Molecular clouds, acting as knots within these networks, serve as hubs, which are local gravitational centers and the main sites of star formation.
{"title":"Molecular clouds as hubs in spiral galaxies : gas inflow and evolutionary sequence","authors":"J W Zhou, Sami Dib, Timothy A Davis","doi":"10.1093/mnras/stae2101","DOIUrl":"https://doi.org/10.1093/mnras/stae2101","url":null,"abstract":"We decomposed the molecular gas in the spiral galaxy NGC 628 (M74) into multi-scale hub-filament structures using the CO (2−1) line by the dendrogram algorithm. All leaf structures as potential hubs were classified into three categories, i.e. leaf-HFs-A, leaf-HFs-B and leaf-HFs-C. leaf-HFs-A exhibit the best hub-filament morphology, which also have the highest density contrast, the largest mass and the lowest virial ratio. We employed the FILFINDER algorithm to identify and characterize filaments within 185 leaf-HFs-A structures, and fitted the velocity gradients around the intensity peaks. Measurements of velocity gradients provide evidence for gas inflow within these structures, which can serve as a kinematic evidence that these structures are hub-filament structures. The numbers of the associated 21 μm and Hα structures and the peak intensities of 7.7 μm, 21 μm and Hα emissions decrease from leaf-HFs-A to leaf-HFs-C. The spatial separations between the intensity peaks of CO and 21 μm structures of leaf-HFs-A are larger than those of leaf-HFs-C. These evidence indicate that leaf-HFs-A are more evolved than leaf-HFs-C. There may be an evolutionary sequence from leaf-HFs-C to leaf-HFs-A. Currently, leaf-HFs-C lack a distinct gravitational collapse process that would result in a significant density contrast. The density contrast can effectively measure the extent of the gravitational collapse and the depth of the gravitational potential of the structure which, in turn, shapes the hub-filament morphology. Combined with the kinematic analysis presented in previous studies, a picture emerges that molecular gas in spiral galaxies is organized into network structures through the gravitational coupling of multi-scale hub-filament structures. Molecular clouds, acting as knots within these networks, serve as hubs, which are local gravitational centers and the main sites of star formation.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"42 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177570","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}
Heartbeat stars (HBSs) are ideal astrophysical laboratories to study the formation and evolution of binary stars in eccentric orbits and the internal structural changes of their components under strong tidal action. We discover 23 new HBSs based on TESS photometric data. The orbital parameters, including orbital period, eccentricity, orbital inclination, argument of periastron, and epoch of periastron passage of these HBSs are derived by using a corrected version of Kumar et al. model based on the Markov Chain Monte Carlo (MCMC) method. The preliminary results show that these HBSs have orbital periods in the range from 2.7 to 20 days and eccentricities in the range from 0.08 to 0.70. The eccentricity-period relation of these objects shows a positive correlation between eccentricity and period, and also shows the existence of orbital circularization. The Hertzsprung-Russell diagram shows that the HBSs are not all located in a particular area. The distribution of the derived parameters suggests a selection bias within the TESS survey towards HBSs with shorter periods. These objects are a very useful source to study the structure and evolution of eccentricity orbit binaries and to extend the TESS HBS catalog.
{"title":"Twenty-three new Heartbeat Star systems discovered based on TESS data","authors":"Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun","doi":"10.1093/mnras/stae2057","DOIUrl":"https://doi.org/10.1093/mnras/stae2057","url":null,"abstract":"Heartbeat stars (HBSs) are ideal astrophysical laboratories to study the formation and evolution of binary stars in eccentric orbits and the internal structural changes of their components under strong tidal action. We discover 23 new HBSs based on TESS photometric data. The orbital parameters, including orbital period, eccentricity, orbital inclination, argument of periastron, and epoch of periastron passage of these HBSs are derived by using a corrected version of Kumar et al. model based on the Markov Chain Monte Carlo (MCMC) method. The preliminary results show that these HBSs have orbital periods in the range from 2.7 to 20 days and eccentricities in the range from 0.08 to 0.70. The eccentricity-period relation of these objects shows a positive correlation between eccentricity and period, and also shows the existence of orbital circularization. The Hertzsprung-Russell diagram shows that the HBSs are not all located in a particular area. The distribution of the derived parameters suggests a selection bias within the TESS survey towards HBSs with shorter periods. These objects are a very useful source to study the structure and evolution of eccentricity orbit binaries and to extend the TESS HBS catalog.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"79 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177565","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}
Shi-Fan Chen, Cullan Howlett, Martin White, Patrick McDonald, Ashley J Ross, Hee-Jong Seo, Nikhil Padmanabhan, J Aguilar, S Ahlen, S Alam, O Alves, U Andrade, R Blum, D Brooks, X Chen, S Cole, K Dawson, A de la Macorra, Arjun Dey, Z Ding, P Doel, S Ferraro, A Font-Ribera, D Forero-Sánchez, J E Forero-Romero, C Garcia-Quintero, E Gaztañaga, S Gontcho A Gontcho, M M S Hanif, K Honscheid, T Kisner, A Kremin, A Lambert, M Landriau, M E Levi, M Manera, A Meisner, J Mena-Fernández, R Miquel, A Munoz-Gutierrez, E Paillas, N Palanque-Delabrouille, W J Percival, A Pérez-Fernández, F Prada, M Rashkovetskyi, M Rezaie, A Rosado-Marin, G Rossi, R Ruggeri, E Sanchez, D Schlegel, J Silber, G Tarlé, M Vargas-Magaña, B A Weaver, J Yu, S Yuan, R Zhou, Z Zhou
This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument’s (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential biases in measurements of the isotropic (αiso) and anisotropic (αap) BAO distance scales, and how these can be effectively removed with an appropriate choice of reconstruction algorithm. We then demonstrate how theory leads to a clear choice for how to model the BAO and develop, implement and validate a new model for the remaining smooth-broadband (i.e., without BAO) component of the galaxy clustering. Finally, we explore the impact of all remaining modelling choices on the BAO constraints from DESI using a suite of high-precision simulations, arriving at a set of best-practices for DESI BAO fits, and an associated theory and modelling systematic error. Overall, our results demonstrate the remarkable robustness of the BAO to all our modelling choices and motivate a combined theory and modelling systematic error contribution to the post-reconstruction DESI BAO measurements of no more than 0.1% (0.2%) for its isotropic (anisotropic) distance measurements. We expect the theory and best-practices laid out to here to be applicable to other BAO experiments in the era of DESI and beyond.
本文全面概述了在即将推出的暗能量光谱仪（DESI）2024 年结果中如何利用其 DR1 数据集进行重子声振荡（BAO）拟合，以及从 BAO 理论和建模中得出的相关系统误差预算。我们得出的新结果表明，星系聚类中的非线性如何导致各向同性（αiso）和各向异性（αap）BAO距离尺度测量的潜在偏差，以及如何通过选择适当的重建算法有效地消除这些偏差。然后，我们展示了理论如何为如何建立 BAO 模型带来明确的选择，并为星系聚类中剩余的平滑宽带（即不含 BAO）部分建立、实施和验证了一个新模型。最后，我们利用一套高精度模拟，探讨了所有剩余建模选择对来自DESI的BAO约束的影响，得出了一套DESI BAO拟合的最佳做法，以及相关的理论和建模系统误差。总之，我们的结果表明，BAO 对我们所有的建模选择都具有显著的鲁棒性，并激励我们将理论和建模的系统误差结合起来，使 DESI BAO 重建后的各向同性（各向异性）距离测量值不超过 0.1%（0.2%）。我们希望这里提出的理论和最佳实践能够适用于 DESI 时代及以后的其他 BAO 实验。
{"title":"Baryon Acoustic Oscillation Theory and Modelling Systematics for the DESI 2024 results","authors":"Shi-Fan Chen, Cullan Howlett, Martin White, Patrick McDonald, Ashley J Ross, Hee-Jong Seo, Nikhil Padmanabhan, J Aguilar, S Ahlen, S Alam, O Alves, U Andrade, R Blum, D Brooks, X Chen, S Cole, K Dawson, A de la Macorra, Arjun Dey, Z Ding, P Doel, S Ferraro, A Font-Ribera, D Forero-Sánchez, J E Forero-Romero, C Garcia-Quintero, E Gaztañaga, S Gontcho A Gontcho, M M S Hanif, K Honscheid, T Kisner, A Kremin, A Lambert, M Landriau, M E Levi, M Manera, A Meisner, J Mena-Fernández, R Miquel, A Munoz-Gutierrez, E Paillas, N Palanque-Delabrouille, W J Percival, A Pérez-Fernández, F Prada, M Rashkovetskyi, M Rezaie, A Rosado-Marin, G Rossi, R Ruggeri, E Sanchez, D Schlegel, J Silber, G Tarlé, M Vargas-Magaña, B A Weaver, J Yu, S Yuan, R Zhou, Z Zhou","doi":"10.1093/mnras/stae2090","DOIUrl":"https://doi.org/10.1093/mnras/stae2090","url":null,"abstract":"This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument’s (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential biases in measurements of the isotropic (αiso) and anisotropic (αap) BAO distance scales, and how these can be effectively removed with an appropriate choice of reconstruction algorithm. We then demonstrate how theory leads to a clear choice for how to model the BAO and develop, implement and validate a new model for the remaining smooth-broadband (i.e., without BAO) component of the galaxy clustering. Finally, we explore the impact of all remaining modelling choices on the BAO constraints from DESI using a suite of high-precision simulations, arriving at a set of best-practices for DESI BAO fits, and an associated theory and modelling systematic error. Overall, our results demonstrate the remarkable robustness of the BAO to all our modelling choices and motivate a combined theory and modelling systematic error contribution to the post-reconstruction DESI BAO measurements of no more than 0.1% (0.2%) for its isotropic (anisotropic) distance measurements. We expect the theory and best-practices laid out to here to be applicable to other BAO experiments in the era of DESI and beyond.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"3 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177571","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}
Sagnik Chatterjee, Kamal Krishna Nath, Ritam Mallick
Recycled millisecond pulsars are susceptible to starquakes as they are continuously accreting matter from their binary companion. A starquake happens when the rotational frequency of the star crosses its breaking frequency. In this study, we perform a model analysis of an accreting neutron star suffering a starquake. We analyse two models: a spherical star with accreting mountains and a deformed star with accreting mountains. We find that as the star crosses the breaking frequency and suffers a starquake, there is a sudden change in the continuous gravitational wave signal arriving from it. The amplitude of the gravitational wave signal increases suddenly both for the spherical and deformed star. For the spherical star, the accreting matter entirely dictates the amplitude of the gravitational wave. For the deformed star, both the accreting matter and the deformation from spherical symmetry play a significant role in determining the amplitude of the gravitational wave signal. This sudden change in the continuous gravitational wave signal in recycled millisecond pulsars can be a unique signature for such pulsars undergoing a starquake.
{"title":"Deciphering accretion-driven starquakes in recycled millisecond pulsars using gravitational waves","authors":"Sagnik Chatterjee, Kamal Krishna Nath, Ritam Mallick","doi":"10.1093/mnras/stae2087","DOIUrl":"https://doi.org/10.1093/mnras/stae2087","url":null,"abstract":"Recycled millisecond pulsars are susceptible to starquakes as they are continuously accreting matter from their binary companion. A starquake happens when the rotational frequency of the star crosses its breaking frequency. In this study, we perform a model analysis of an accreting neutron star suffering a starquake. We analyse two models: a spherical star with accreting mountains and a deformed star with accreting mountains. We find that as the star crosses the breaking frequency and suffers a starquake, there is a sudden change in the continuous gravitational wave signal arriving from it. The amplitude of the gravitational wave signal increases suddenly both for the spherical and deformed star. For the spherical star, the accreting matter entirely dictates the amplitude of the gravitational wave. For the deformed star, both the accreting matter and the deformation from spherical symmetry play a significant role in determining the amplitude of the gravitational wave signal. This sudden change in the continuous gravitational wave signal in recycled millisecond pulsars can be a unique signature for such pulsars undergoing a starquake.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"395 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177573","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}
Ricardo G Landim, Harry Desmond, Kazuya Koyama, Samantha Penny
Fifth forces are ubiquitous in modified gravity theories, and must be screened to evade stringent local tests. This can introduce unusual behaviour in galaxy phenomenology by affecting galaxies’ components differently. Here we use the SDSS-IV-MaNGA dataset to search for a systematic excess of gas circular velocity over stellar circular velocity, expected in thin-shell-screened theories in the partially screened regime. Accounting for asymmetric drift and calibrating our model on screened subsamples, we find no significant evidence for a screened fifth force. We bound the fifth-force strength to ΔG/GN < 0.1 for all astrophysical ranges, strengthening to ∼0.01 at Compton wavelength of 3 Mpc for the Hu-Sawicki model, for instance. This implies a stringent constraint on scalar–tensor theories, for example $f_{mathcal {R}0} lesssim 10^{-8}$ in Hu–Sawicki $f(mathcal {R})$ gravity.
{"title":"Testing screened modified gravity with SDSS-IV-MaNGA","authors":"Ricardo G Landim, Harry Desmond, Kazuya Koyama, Samantha Penny","doi":"10.1093/mnras/stae2096","DOIUrl":"https://doi.org/10.1093/mnras/stae2096","url":null,"abstract":"Fifth forces are ubiquitous in modified gravity theories, and must be screened to evade stringent local tests. This can introduce unusual behaviour in galaxy phenomenology by affecting galaxies’ components differently. Here we use the SDSS-IV-MaNGA dataset to search for a systematic excess of gas circular velocity over stellar circular velocity, expected in thin-shell-screened theories in the partially screened regime. Accounting for asymmetric drift and calibrating our model on screened subsamples, we find no significant evidence for a screened fifth force. We bound the fifth-force strength to ΔG/GN &lt; 0.1 for all astrophysical ranges, strengthening to ∼0.01 at Compton wavelength of 3 Mpc for the Hu-Sawicki model, for instance. This implies a stringent constraint on scalar–tensor theories, for example $f_{mathcal {R}0} lesssim 10^{-8}$ in Hu–Sawicki $f(mathcal {R})$ gravity.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"108 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177569","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}
Despite numerous studies, the sources of IceCube cosmic neutrinos are mostly unidentified. Utilizing recently released IceCube neutrino and CHIME fast radio burst (FRB) catalogs, we examine the possibility of an association between neutrinos and CHIME/FRB catalog 1 FRBs for both the entire FRB population and individual FRBs using the unbinned maximum likelihood method. Our results do not directly support the possibility of the above-mentioned association with three weighting schemes: equal, total radio fluence, and event rate. We then attempt to constrain the diffuse muon neutrino flux upper limit from CHIME/FRB catalog 1 FRBs. After considering a completeness correction, we find the 95% diffuse muon neutrino flux upper limit at 100 TeV for all FRB sources in the universe to be ∼ 1.01 × 10−18GeV−1 cm−2s−1sr−1, or ∼ 70.3 % of the 10-year diffuse neutrino flux observed by IceCube. Our results match the non-detection results of other studies, but we do not rule out FRBs being a significant contributor to the diffuse neutrino flux measured by IceCube.
{"title":"Time-integrated constraint on neutrino flux of CHIME fast radio burst sources with 10-year IceCube point-source data","authors":"Jia-Wei Luo, Bing Zhang","doi":"10.1093/mnras/stae2071","DOIUrl":"https://doi.org/10.1093/mnras/stae2071","url":null,"abstract":"Despite numerous studies, the sources of IceCube cosmic neutrinos are mostly unidentified. Utilizing recently released IceCube neutrino and CHIME fast radio burst (FRB) catalogs, we examine the possibility of an association between neutrinos and CHIME/FRB catalog 1 FRBs for both the entire FRB population and individual FRBs using the unbinned maximum likelihood method. Our results do not directly support the possibility of the above-mentioned association with three weighting schemes: equal, total radio fluence, and event rate. We then attempt to constrain the diffuse muon neutrino flux upper limit from CHIME/FRB catalog 1 FRBs. After considering a completeness correction, we find the 95% diffuse muon neutrino flux upper limit at 100 TeV for all FRB sources in the universe to be ∼ 1.01 × 10−18GeV−1 cm−2s−1sr−1, or ∼ 70.3 % of the 10-year diffuse neutrino flux observed by IceCube. Our results match the non-detection results of other studies, but we do not rule out FRBs being a significant contributor to the diffuse neutrino flux measured by IceCube.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"31 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177589","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}
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