Monthly Notices of the Royal Astronomical Society最新文献_第7页

Small-scale signatures of primordial non-Gaussianity in k-Nearest neighbour cumulative distribution functions k 近邻累积分布函数中原始非高斯性的小尺度特征

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2108

William R Coulton, Tom Abel, Arka Banerjee

{"title":"Small-scale signatures of primordial non-Gaussianity in k-Nearest neighbour cumulative distribution functions","authors":"William R Coulton, Tom Abel, Arka Banerjee","doi":"10.1093/mnras/stae2108","DOIUrl":"https://doi.org/10.1093/mnras/stae2108","url":null,"abstract":"Searches for primordial non-Gaussianity in cosmological perturbations are a key means of revealing novel primordial physics. However, robustly extracting signatures of primordial non-Gaussianity from non-linear scales of the late-time Universe is an open problem. In this paper, we apply k-Nearest Neighbor cumulative distribution functions, kNN-CDFs, to the quijote-png simulations to explore the sensitivity of kNN-CDFs to primordial non-Gaussianity. An interesting result is that for halo samples with Mh &lt; 1014 M⊙ h−1, the kNN-CDFs respond to equilateral PNG in a manner distinct from the other parameters. This persists in the galaxy catalogs in redshift space and can be differentiated from the impact of galaxy modelling, at least within the halo occupation distribution (HOD) framework considered here. kNN-CDFs are related to counts-in-cells and, through mapping a subset of the kNN-CDF measurements into the count-in-cells picture, we show that our results can be modeled analytically. A caveat of the analysis is that we only consider the HOD framework, including assembly bias. It will be interesting to validate these results with other techniques for modeling the galaxy–halo connection, e.g. (hybrid) effective field theory or semi-analytical methods.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"24 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256126","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

Dynamics and spin alignment in massive, gravito-turbulent circumbinary discs around supermassive black hole binaries 超大质量黑洞双星周围大质量、重力湍流环状圆盘的动力学和自旋排列

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2143

Martin A Bourne, Davide Fiacconi, Debora Sijacki, Joanna M Piotrowska, Sophie Koudmani

{"title":"Dynamics and spin alignment in massive, gravito-turbulent circumbinary discs around supermassive black hole binaries","authors":"Martin A Bourne, Davide Fiacconi, Debora Sijacki, Joanna M Piotrowska, Sophie Koudmani","doi":"10.1093/mnras/stae2143","DOIUrl":"https://doi.org/10.1093/mnras/stae2143","url":null,"abstract":"Parsec-scale separation supermassive black hole binaries in the centre of gas-rich galaxy merger remnants could be surrounded by massive circumbinary discs (CBDs). Black hole mass and spin evolution during the gas-rich binary inspiral are crucial in determining the direction and power of relativistic jets that radio observations with LOFAR and SKAO will probe, and for predicting gravitational wave (GW) emission that IPTA and LISA will measure. We present 3D hydrodynamic simulations capturing gas-rich, self-gravitating CBDs around a 2 × 106 M⊙ supermassive black hole binary, that probe different mass ratios, eccentricities and inclinations. We employ a sub-grid Shakura-Sunyaev accretion disc to self-consistently model black hole mass and spin evolution together with super-Lagrangian refinement techniques to resolve gas flows, streams and mini-discs within the cavity, which play a fundamental role in torquing and feeding the binary. We find that higher mass ratio and eccentric binaries result in larger cavities, while retrograde binaries result in smaller cavities. All of the simulated binaries are expected to shrink with net gravitational torques being negative. Unlike previous simulations, we do not find preferential accretion onto the secondary black hole. This implies smaller chirp masses at coalescence and hence a weaker GW background. Critically this means that spin-alignment is faster than the binary inspiral timescale even for low mass ratios. When considering initially misaligned systems, the orientation of the mini-discs around each black hole can vary significantly. We discuss the implications of this behaviour for black hole spin alignment and highlight the need for broader parameter space studies of misaligned systems to understand the impact on black hole recoil velocities.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"208 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269291","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

Imprint of massive neutrinos on Persistent Homology of large-scale structure 大质量中微子对大尺度结构持久同源性的影响

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-12 DOI: 10.1093/mnras/stae2044

M H Jalali Kanafi, S Ansarifard, S M S Movahed

{"title":"Imprint of massive neutrinos on Persistent Homology of large-scale structure","authors":"M H Jalali Kanafi, S Ansarifard, S M S Movahed","doi":"10.1093/mnras/stae2044","DOIUrl":"https://doi.org/10.1093/mnras/stae2044","url":null,"abstract":"Exploiting the Persistent Homology technique and its complementary representations, we examine the footprint of summed neutrino mass (Mν) in the various density fields simulated by the publicly available Quijote suite. The evolution of topological features by utilizing the super-level filtration on three-dimensional density fields at zero redshift, reveals a remarkable benchmark for constraining the cosmological parameters, particularly Mν and σ8. The abundance of independent closed surfaces (voids) compared to the connected components (clusters) and independent loops (filaments), is more sensitive to the presence of Mν for R = 5 Mpc h−1 irrespective of whether using the total matter density field (m) or CDM+baryons field (cb). Reducing the degeneracy between Mν and σ8 is achieved via Persistent Homology for the m field but not for the cb field. The uncertainty of Mν at 1σ confidenc interval from the joint analysis of Persistent Homology vectorization for the m and cb fields smoothed by R = 5 Mpc h−1 at z = 0 reaches 0.0152 eV and 0.1242 eV, respectively. Noticing the use of the 3-dimensional underlying density field at z = 0, the mentioned uncertainties can be treated as the theoretical lower limits.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"31 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256160","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

Fossil Groups analysis using weak gravitational lensing 利用弱引力透镜分析化石群

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-12 DOI: 10.1093/mnras/stae2078

M Castejon, E S Cypriano, A Z Vitorelli

{"title":"Fossil Groups analysis using weak gravitational lensing","authors":"M Castejon, E S Cypriano, A Z Vitorelli","doi":"10.1093/mnras/stae2078","DOIUrl":"https://doi.org/10.1093/mnras/stae2078","url":null,"abstract":"The overall objective of this study is to investigate claims found in the literature that fossil groups, characterized by a large magnitude gap between their two brightest galaxies, are darker, i.e. exhibit higher mass-to-light ratios (M/L), compared to regular groups. Specifically, we aim to measure the mass of these systems using the weak gravitational lensing technique. To achieve this, we obtained deep images of four fossil systems with the CFHT telescope in the r and g bands. Through a careful process of weak gravitational shear measurement, including corrections for the point spread function (PSF) and contamination from group and foreground galaxies, we fit NFW models and obtained mass measurements as a result. Similarly, we quantified the light distribution produced by these groups, taking into account relevant data gaps in the images due to the presence of bright stars, as well as contamination from foreground and background galaxies. We obtained masses and M/L ratios that are consistent with previous results where mass was estimated from galaxy dynamics. Indeed, the four fossil systems studied here exhibit high M/L ratios compared to the general population of systems. Drawing more generalizable conclusions from a sample of only four systems is challenging. However, the procedure outlined in this study can be applied to large image surveys, allowing for a revisiting of this question with significantly reduced statistical uncertainties. This will enable a more homogeneous comparison between fossil groups and clusters and the overall population.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"1 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256127","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

Relativistic X-ray reflection from the accreting millisecond X-ray pulsar IGR J17498-2921 来自吸积毫秒 X 射线脉冲星 IGR J17498-2921 的相对论 X 射线反射

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-12 DOI: 10.1093/mnras/stae2135

Mahasweta Bhattacharya, Aditya S Mondal, Mayukh Pahari, Biplab Raychaudhuri, Rohit Ghosh, Gulab C Dewangan

{"title":"Relativistic X-ray reflection from the accreting millisecond X-ray pulsar IGR J17498-2921","authors":"Mahasweta Bhattacharya, Aditya S Mondal, Mayukh Pahari, Biplab Raychaudhuri, Rohit Ghosh, Gulab C Dewangan","doi":"10.1093/mnras/stae2135","DOIUrl":"https://doi.org/10.1093/mnras/stae2135","url":null,"abstract":"The accreting millisecond X-ray pulsar IGR J17498-2921 went into X-ray outburst on April 13-15, 2023, for the first time since its discovery on August 11, 2011. Here, we report on the first follow-up NuSTAR observation of the source, performed on April 23, 2023, around ten days after the peak of the outburst. The NuSTAR spectrum of the persistent emission (3 − 60 keV band) is well described by an absorbed blackbody with a temperature of kTbb = 1.61 ± 0.04 keV, most likely arising from the NS surface and a Comptonization component with power-law index Γ = 1.79 ± 0.02, arising from a hot corona at kTe = 16 ± 2 keV. The X-ray spectrum of the source shows robust reflection features which have not been observed before. We use a couple of self-consistent reflection models, relxill and relxillCp, to fit the reflection features. We find an upper limit to the inner disc radius of 6 RISCO and 9 RISCO from relxill and relxillCp model, respectively. The inclination of the system is estimated to be ≃ 40○ from both reflection models. Assuming magnetic truncation of the accretion disc, the upper limit of magnetic field strength at the pole of the NS is found to be B ≲ 1.8 × 108 G. Furthermore, the NuSTAR observation revealed two type I X-ray bursts and the burst spectroscopy confirms the thermonuclear nature of the burst. The blackbody temperature reaches nearly 2.2 keV at the peak of the burst.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"16 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256161","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

Quantifying azimuthal variations within the interstellar medium of z ∼ 0 spiral galaxies with the TYPHOON survey 利用 TYPHOON 勘测量化 z∼0 螺线星系星际介质的方位角变化

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-11 DOI: 10.1093/mnras/stae2119

Qian-Hui Chen, Kathryn Grasha, Andrew J Battisti, Emily Wisnioski, Zefeng Li, Hye-Jin Park, Brent Groves, Paul Torrey, Trevor Mendel, Barry F Madore, Mark Seibert, Eva Sextl, Alex M Garcia, Jeff A Rich, Rachael L Beaton, Lisa J Kewley

{"title":"Quantifying azimuthal variations within the interstellar medium of z ∼ 0 spiral galaxies with the TYPHOON survey","authors":"Qian-Hui Chen, Kathryn Grasha, Andrew J Battisti, Emily Wisnioski, Zefeng Li, Hye-Jin Park, Brent Groves, Paul Torrey, Trevor Mendel, Barry F Madore, Mark Seibert, Eva Sextl, Alex M Garcia, Jeff A Rich, Rachael L Beaton, Lisa J Kewley","doi":"10.1093/mnras/stae2119","DOIUrl":"https://doi.org/10.1093/mnras/stae2119","url":null,"abstract":"Most star formation in the local Universe occurs in spiral galaxies, but their origin remains an unanswered question. Various theories have been proposed to explain the development of spiral arms, each predicting different spatial distributions of the interstellar medium. This study maps the star formation rate (SFR) and gas-phase metallicity of nine spiral galaxies with the TYPHOON survey to test two dominating theories: density wave theory and dynamic spiral theory. We discuss the environmental effects on our galaxies, considering reported environments and merging events. Taking advantage of the large field of view covering the entire optical disk, we quantify the fluctuation of SFR and metallicity relative to the azimuthal distance from the spiral arms. We find higher SFR and metallicity in the trailing edge of NGC 1365 (by 0.117 dex and 0.068 dex, respectively) and NGC 1566 (by 0.119 dex and 0.037 dex, respectively), which is in line with density wave theory. NGC 2442 shows a different result with higher metallicity (0.093 dex) in the leading edge, possibly attributed to an ongoing merging. The other six spiral galaxies show no statistically significant offset in SFR or metallicity, consistent with dynamic spiral theory. We also compare the behaviour of metallicity inside and outside the co-rotation radius (CR) of NGC 1365 and NGC 1566. We find comparable metallicity fluctuations near and beyond the CR of NGC 1365, indicating gravitational perturbation. NGC 1566 shows the greatest fluctuation near the CR, in line with the analytic spiral arms. Our work highlights that a combination of mechanisms explains the origin of spiral features in the local Universe.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"17 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256162","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

GA-NIFS: NIRSpec reveals evidence for non-circular motions and AGN feedback in GN20 GA-NIFS：近红外探测器揭示了GN20非圆运动和AGN反馈的证据

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-11 DOI: 10.1093/mnras/stae1993

Hannah Übler, Francesco D’Eugenio, Michele Perna, Santiago Arribas, Gareth C Jones, Andrew J Bunker, Stefano Carniani, Stéphane Charlot, Roberto Maiolino, Bruno Rodríguez del Pino, Chris J Willott, Torsten Böker, Giovanni Cresci, Nimisha Kumari, Isabella Lamperti, Eleonora Parlanti, Jan Scholtz, Giacomo Venturi

{"title":"GA-NIFS: NIRSpec reveals evidence for non-circular motions and AGN feedback in GN20","authors":"Hannah Übler, Francesco D’Eugenio, Michele Perna, Santiago Arribas, Gareth C Jones, Andrew J Bunker, Stefano Carniani, Stéphane Charlot, Roberto Maiolino, Bruno Rodríguez del Pino, Chris J Willott, Torsten Böker, Giovanni Cresci, Nimisha Kumari, Isabella Lamperti, Eleonora Parlanti, Jan Scholtz, Giacomo Venturi","doi":"10.1093/mnras/stae1993","DOIUrl":"https://doi.org/10.1093/mnras/stae1993","url":null,"abstract":"We present rest-frame optical data of the $zsim 4$ submillimetre galaxy GN20 obtained with the JWST Near Infrared Spectrograph (NIRSpec) in integral field spectroscopy mode. The H$alpha$ emission is asymmetric and clumpy and extends over a projected distance of &gt;15 kpc. To first order, the large-scale ionized gas kinematics are consistent with a turbulent ($sigma sim 90$ km s$^{-1}$), rotating disc ($v_{rm rot}sim 500$ km s$^{-1}$), congruent with previous studies of its molecular and ionized gas kinematics. However, we also find clear evidence for non-circular motions in the H$alpha$ kinematics. We discuss their possible connection with various scenarios, such as external perturbations, accretion, or radial flows. In the centre of GN20, we find broad-line emission (full width at half-maximum $sim 1000{-}2000$ km s$^{-1}$) in the H$alpha$ + [N ii] complex, suggestive of fast, active galactic nucleus-driven winds or, alternatively, of the broad-line region of an active black hole. Elevated values of [N ii] $lambda 6583$/H$alpha gt 0.4$ and of the Hα equivalent width EW(H$alpha) gt 6$ Å throughout large parts of GN20 suggest that feedback from the active black hole is able to photoionize the interstellar medium. Our data corroborate that GN20 offers a unique opportunity to observe key processes in the evolution of the most massive present-day galaxies acting in concert, over 12 billion years ago.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"169 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177547","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

Isotopic abundance of carbon in the DLA towards QSO B1331+170 向 QSO B1331+170 的 DLA 中碳的同位素丰度

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-11 DOI: 10.1093/mnras/stae2056

Dinko Milaković, John K Webb, Paolo Molaro, Chung-Chi Lee, Prashin Jethwa, Guido Cupani, Michael T Murphy, Louise Welsh, Valentina D’Odorico, Stefano Cristiani, Ricardo Génova Santos, Carlos J A P Martins, Nelson J Nunes, Tobias M Schmidt, Francesco A Pepe, Maria Rosa Zapatero Osorio, Yann Alibert, J I González Hernández, Paolo Di Marcantonio, Enric Palle, Rafael Rebolo, Nuno C Santos, Sérgio G Sousa, Alejandro Suárez Mascareño

{"title":"Isotopic abundance of carbon in the DLA towards QSO B1331+170","authors":"Dinko Milaković, John K Webb, Paolo Molaro, Chung-Chi Lee, Prashin Jethwa, Guido Cupani, Michael T Murphy, Louise Welsh, Valentina D’Odorico, Stefano Cristiani, Ricardo Génova Santos, Carlos J A P Martins, Nelson J Nunes, Tobias M Schmidt, Francesco A Pepe, Maria Rosa Zapatero Osorio, Yann Alibert, J I González Hernández, Paolo Di Marcantonio, Enric Palle, Rafael Rebolo, Nuno C Santos, Sérgio G Sousa, Alejandro Suárez Mascareño","doi":"10.1093/mnras/stae2056","DOIUrl":"https://doi.org/10.1093/mnras/stae2056","url":null,"abstract":"Chemical evolution models predict a gradual build-up of 13C in the Universe, based on empirical nuclear reaction rates and assumptions on the properties of stellar populations. However, old metal-poor stars within the Galaxy contain more 13C than is predicted, suggesting that further refinements to the models are necessary. Gas at high-redshift provides important supplementary information at metallicities $-2lesssim left[{rm Fe/H}right]lesssim -1$, for which there are only a few measurements in the Galaxy. We obtained new, high-quality, VLT/ESPRESSO observations of the QSO B1331$+$170 and used them to measure 12C/13C in the damped Lyman-$alpha$ system (DLA) at $z_{rm abs}=1.776$, with $left[{rm Fe/H}right]$ = −1.27. ai-vpfit, an artificial intelligence tool based on genetic algorithms and guided by a spectroscopic information criterion, was used to explore different possible kinematic structures of the carbon gas. Three hundred independent ai-vpfit models of the absorption system were produced using pre-set 12C/13C values, ranging from 4 to 500. Our results show that ${rm ^{12}C / ^{13}C}=28.5^{+51.5}_{-10.4}$, suggesting a possibility of 13C production at low metallicity.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"173 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256164","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

Rocking the BOAT: the ups and downs of the long-term radio light curve for GRB 221009A 摇摆的 BOAT：GRB 221009A 长期射电光曲线的起伏变化

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-11 DOI: 10.1093/mnras/stae2050

L Rhodes, A J van der Horst, J S Bright, J K Leung, G E Anderson, R Fender, J F Agüí Fernandez, M Bremer, P Chandra, D Dobie, W Farah, S Giarratana, K Gourdji, D A Green, E Lenc, M J Michałowski, T Murphy, A J Nayana, A W Pollak, A Rowlinson, F Schussler, A Siemion, R L C Starling, P Scott, C C Thöne, D Titterington, A de Ugarte Postigo

{"title":"Rocking the BOAT: the ups and downs of the long-term radio light curve for GRB 221009A","authors":"L Rhodes, A J van der Horst, J S Bright, J K Leung, G E Anderson, R Fender, J F Agüí Fernandez, M Bremer, P Chandra, D Dobie, W Farah, S Giarratana, K Gourdji, D A Green, E Lenc, M J Michałowski, T Murphy, A J Nayana, A W Pollak, A Rowlinson, F Schussler, A Siemion, R L C Starling, P Scott, C C Thöne, D Titterington, A de Ugarte Postigo","doi":"10.1093/mnras/stae2050","DOIUrl":"https://doi.org/10.1093/mnras/stae2050","url":null,"abstract":"We present radio observations of the long-duration gamma-ray burst (GRB) 221009A which has become known to the community as the Brightest Of All Time or the BOAT. Our observations span the first 475 days post-burst and three orders of magnitude in observing frequency, from 0.15 to 230 GHz. By combining our new observations with those available in the literature, we have the most detailed radio data set in terms of cadence and spectral coverage of any GRB to date, which we use to explore the spectral and temporal evolution of the afterglow. By testing a series of phenomenological models, we find that three separate synchrotron components best explain the afterglow. The high temporal and spectral resolution allows us to conclude that standard analytical afterglow models are unable to explain the observed evolution of GRB 221009A. We explore where the discrepancies between the observations and the models are most significant and place our findings in the context of the most well-studied GRB radio afterglows to date. Our observations are best explained by three synchrotron emitting regions which we interpret as a forward shock, a reverse shock and an additional shock potentially from a cocoon or wider outflow. Finally, we find that our observations do not show any evidence of any late-time spectral or temporal changes that could result from a jet break but note that any lateral structure could significantly affect a jet break signature.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"108 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177546","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

Photospheric signatures of CME onset CME 开始时的光层特征

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/stae2110

O P M Aslam, D MacTaggart, T Williams, L Fletcher, P Romano

引用次数: 0