arXiv - PHYS - High Energy Astrophysical Phenomena最新文献_第6页

Parameter constraints for accreting millisecond pulsars with synthetic NICER data 利用合成 NICER 数据对吸积毫秒脉冲星的参数约束

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-12 DOI: arxiv-2409.07908

Bas Dorsman, Tuomo Salmi, Anna L. Watts, Mason Ng, Satish Kamath, Anna Bobrikova, Juri Poutanen, Vladislav Loktev, Yves Kini, Devarshi Choudhury, Serena Vinciguerra, Slavko Bogdanov, Deepto Chakrabarty

{"title":"Parameter constraints for accreting millisecond pulsars with synthetic NICER data","authors":"Bas Dorsman, Tuomo Salmi, Anna L. Watts, Mason Ng, Satish Kamath, Anna Bobrikova, Juri Poutanen, Vladislav Loktev, Yves Kini, Devarshi Choudhury, Serena Vinciguerra, Slavko Bogdanov, Deepto Chakrabarty","doi":"arxiv-2409.07908","DOIUrl":"https://doi.org/arxiv-2409.07908","url":null,"abstract":"Pulse profile modelling (PPM) is a technique for inferring mass, radius and\u0000hotspot properties of millisecond pulsars. PPM is now regularly used for\u0000analysis of rotation-powered millisecond pulsars (RMPs) with data from the\u0000Neutron Star Interior Composition ExploreR (NICER). Extending PPM to accreting\u0000millisecond pulsars (AMPs) is attractive, because they are a different source\u0000class featuring bright X-ray radiation from hotspots powered by accretion. In\u0000this paper, we present a modification of one of the PPM codes, X-PSI, so that\u0000it can be used for AMPs. In particular, we implement a model of an accretion\u0000disc and atmosphere model appropriate for the hotspots of AMPs, and improve the\u0000overall computational efficiency. We then test parameter recovery with\u0000synthetic NICER data in two scenarios with reasonable parameters for AMPs. We\u0000find in the first scenario, where the hotspot is large, that we are able to\u0000tightly and accurately constrain all parameters including mass and radius. In\u0000the second scenario, which is a high inclination system with a smaller hotspot,\u0000we find degeneracy between a subset of model parameters and a slight bias in\u0000the inferred mass and radius. This analysis of synthetic data lays the ground\u0000work for future analysis of AMPs with NICER data. Such an analysis could be\u0000complemented by future (joint) analysis of polarization data from the Imaging\u0000X-ray Polarimetry Explorer (IXPE).","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206791","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

An Integral-Based Technique (IBT) to Accelerate the Monte-Carlo Radiative Transfer Computation for Supernovae 基于积分的技术（IBT）加速超新星的蒙特卡洛辐射传输计算

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-12 DOI: arxiv-2409.07729

Xingzhuo Chen, Lifan Wang, Daniel Kasen

{"title":"An Integral-Based Technique (IBT) to Accelerate the Monte-Carlo Radiative Transfer Computation for Supernovae","authors":"Xingzhuo Chen, Lifan Wang, Daniel Kasen","doi":"arxiv-2409.07729","DOIUrl":"https://doi.org/arxiv-2409.07729","url":null,"abstract":"We present an integral-based technique (IBT) algorithm to accelerate\u0000supernova (SN) radiative transfer calculations. The algorithm utilizes\u0000``integral packets'', which are calculated by the path integral of the\u0000Monte-Carlo energy packets, to synthesize the observed spectropolarimetric\u0000signal at a given viewing direction in a 3-D time-dependent radiative transfer\u0000program. Compared to the event-based technique (EBT) proposed by (Bulla et al.\u00002015), our algorithm significantly reduces the computation time and increases\u0000the Monte-Carlo signal-to-noise ratio. Using a 1-D spherical symmetric type Ia\u0000supernova (SN Ia) ejecta model DDC10 and its derived 3-D model, the IBT\u0000algorithm has successfully passed the verification of: (1) spherical symmetry;\u0000(2) mirror symmetry; (3) cross comparison on a 3-D SN model with\u0000direct-counting technique (DCT) and EBT. Notably, with our algorithm\u0000implemented in the 3-D Monte-Carlo radiative transfer code SEDONA, the\u0000computation time is faster than EBT by a factor of $10-30$, and the\u0000signal-to-noise (S/N) ratio is better by a factor of $5-10$, with the same\u0000number of Monte-Carlo quanta.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"50 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206792","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Follow-up of Neutron Star Mergers with CTA and Prospects for Joint Detection with Gravitational-Wave Detectors 用 CTA 跟踪中子星合并以及与引力波探测器联合探测的前景

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-12 DOI: arxiv-2409.07916

T. Mondal, S. Chakraborty, L. Resmi, D. Bose

{"title":"Follow-up of Neutron Star Mergers with CTA and Prospects for Joint Detection with Gravitational-Wave Detectors","authors":"T. Mondal, S. Chakraborty, L. Resmi, D. Bose","doi":"arxiv-2409.07916","DOIUrl":"https://doi.org/arxiv-2409.07916","url":null,"abstract":"The joint gravitational wave (GW) and electromagnetic observations of the\u0000binary neutron star (BNS) merger GW170817 marked a giant leap in\u0000multi-messenger astrophysics. The extensive observation campaign of the\u0000associated Gamma-Ray Burst (GRB) and its afterglow has strengthened the\u0000hypothesis associating GRBs with BNS mergers and provided insights on mass\u0000ejection, particularly the relativistic outflow launched in BNS mergers. In\u0000this paper, we investigate the joint detection probabilities of BNS mergers by\u0000GW detectors and the upcoming ground-based very-high-energy (VHE) $gamma$-ray\u0000instrument, the Cherenkov Telescope Array (CTA). Using an empirical relation\u0000that constrains the distance-inclination angle plane, we simulated BNS mergers\u0000detectable in the O5 run of the LIGO/Virgo/Kagra (LVK) network with $300$~Mpc\u0000BNS horizon. Assuming Gaussian structured jets and ignoring large sky\u0000localization challenges of GW detectors, we estimated VHE afterglow detection\u0000probability by CTA. We have explored the afterglow parameter space to identify\u0000conditions favourable for detecting synchrotron self-Compton emission by CTA.\u0000Our study reveals that events viewed at angles $lesssim3$ times the jet core\u0000angle are detectable by CTA when the initial bulk Lorentz factor at the jet\u0000axis ranges between 100 and 800. We find high kinetic energy ($E_k>10^{50}$\u0000erg), ambient density ($n_0>10^{-1}$ $cm^{-3}$), and energy content in\u0000non-thermal electrons significantly enhance the likelihood of CTA detection\u0000within 300 Mpc. The joint detection rate varies significantly with afterglow\u0000parameter distributions, ranging from $0.003$ to $0.5$ per year.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206788","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

MLody -- Deep Learning Generated Polarized Synchrotron Coefficients MLody -- 深度学习生成的极化同步辐射系数

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-12 DOI: arxiv-2409.08007

Jordy Davelaar

{"title":"MLody -- Deep Learning Generated Polarized Synchrotron Coefficients","authors":"Jordy Davelaar","doi":"arxiv-2409.08007","DOIUrl":"https://doi.org/arxiv-2409.08007","url":null,"abstract":"Polarized synchrotron emission is a fundamental process in high-energy\u0000astrophysics, particularly in the environments around black holes and pulsars.\u0000Accurate modeling of this emission requires precise computation of the\u0000emission, absorption, rotation, and conversion coefficients, which are critical\u0000for radiative transfer simulations. Traditionally, these coefficients are\u0000derived using fit functions based on precomputed ground truth values. However,\u0000these fit functions often lack accuracy, particularly in specific plasma\u0000conditions not well represented in the datasets used to generate them. In this\u0000work, we introduce ${tt MLody}$, a deep neural network designed to compute\u0000polarized synchrotron coefficients with high accuracy across a wide range of\u0000plasma parameters. We demonstrate ${tt MLody}$'s capabilities by integrating\u0000it with a radiative transfer code to generate synthetic polarized synchrotron\u0000images for an accreting black hole simulation. Our results reveal significant\u0000differences, up to a factor of two, in both linear and circular polarization\u0000compared to traditional methods. These differences could have important\u0000implications for parameter estimation in Event Horizon Telescope observations,\u0000suggesting that ${tt MLody}$ could enhance the accuracy of future\u0000astrophysical analyses.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"62 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206547","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Merger of massive galaxy cluster CL0238.3+2005 at z~0.4: just after pericenter passage? z~0.4级大质量星系团CL0238.3+2005的合并：刚刚经过中心？

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-12 DOI: arxiv-2409.07856

N. Lyskova, E. Churazov, I. Khabibullin, I. F. Bikmaev, R. A. Burenin, W. R. Forman, I. M. Khamitov, K. Rajpurohit, R. Sunyaev, C. Jones, R. Kraft, I. Zaznobin, M. A. Gorbachev, M. V. Suslikov, R. I. Gumerov, N. A. Sakhibullin

{"title":"Merger of massive galaxy cluster CL0238.3+2005 at z~0.4: just after pericenter passage?","authors":"N. Lyskova, E. Churazov, I. Khabibullin, I. F. Bikmaev, R. A. Burenin, W. R. Forman, I. M. Khamitov, K. Rajpurohit, R. Sunyaev, C. Jones, R. Kraft, I. Zaznobin, M. A. Gorbachev, M. V. Suslikov, R. I. Gumerov, N. A. Sakhibullin","doi":"arxiv-2409.07856","DOIUrl":"https://doi.org/arxiv-2409.07856","url":null,"abstract":"Massive clusters of galaxies are very rare in the observable Universe. Even\u0000rarer are mergers of such clusters observed close to pericenter passage. Here,\u0000we report on one such case: a massive (~ $10^{15},M_odot$) and hot (kT ~ 10\u0000keV) cluster CL0238.3+2005 at $zapprox 0.42$. For this cluster, we combine\u0000X-ray data from SRG/eROSITA and Chandra, optical images from DESI, and\u0000spectroscopy from BTA and RTT-150 telescopes. The X-ray and optical\u0000morphologies suggest an ongoing merger with the projected separation of\u0000subhalos of $sim 200$ kpc. The line-of-sight velocity of galaxies tentatively\u0000associated with the two merging halos differs by 2000-3000 km/s. We conclude\u0000that, most plausibly, the merger axis is neither close to the line of sight nor\u0000to the sky plane. We compare CL0238 with two well-known clusters MACS0416 and\u0000Bullet, and conclude that CL0238 corresponds to an intermediate phase between\u0000the pre-merging MACS0416 cluster and the post-merger Bullet cluster. Namely,\u0000this cluster has recently (only $lesssim 0.1$ Gyr ago) experienced an almost\u0000head-on merger. We argue that this \"just after\" system is a very rare case and\u0000an excellent target for lensing, Sunyaev-Zeldovich effect, and X-ray studies\u0000that can constrain properties ranging from dynamics of mergers to\u0000self-interacting dark matter, and plasma effects in intracluster medium that\u0000are associated with shock waves, e.g., electron-ion equilibration efficiency\u0000and relativistic particle acceleration.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"63 1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206839","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The early radio afterglow of short GRB 230217A 短GRB 230217A的早期射电余辉

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-12 DOI: arxiv-2409.07686

G. E. Anderson, G. Schroeder, A. J. van der Horst, L. Rhodes, A. Rowlinson, A. Bahramian, S. I. Chastain, B. P. Gompertz, P. J. Hancock, T. Laskar, J. K. Leung, R. A. M. J. Wijers

{"title":"The early radio afterglow of short GRB 230217A","authors":"G. E. Anderson, G. Schroeder, A. J. van der Horst, L. Rhodes, A. Rowlinson, A. Bahramian, S. I. Chastain, B. P. Gompertz, P. J. Hancock, T. Laskar, J. K. Leung, R. A. M. J. Wijers","doi":"arxiv-2409.07686","DOIUrl":"https://doi.org/arxiv-2409.07686","url":null,"abstract":"We present the radio afterglow of short gamma-ray burst (GRB) 230217A, which\u0000was detected less than 1 day after the gamma-ray prompt emission with the\u0000Australia Telescope Compact Array (ATCA) and the Karl G. Jansky Very Large\u0000Array (VLA). The ATCA rapid-response system automatically triggered an\u0000observation of GRB 230217A following its detection by the Neil Gehrels Swift\u0000Observatory and began observing the event just 32 minutes post-burst at 5.5 and\u00009 GHz for 7 hours. Dividing the 7-hour observation into three time-binned\u0000images allowed us to obtain radio detections with logarithmic central times of\u00001, 2.8 and 5.2 hours post-burst, the first of which represents the earliest\u0000radio detection of any GRB to date. The decline of the light curve is\u0000consistent with reverse shock emission if the observing bands are below the\u0000spectral peak and not affected by synchrotron self-absorption. This makes GRB\u0000230217A the fifth short GRB with radio detections attributed to a reverse shock\u0000at early times ($<1$ day post-burst). Following brightness temperature\u0000arguments, we have used our early radio detections to place the highest minimum\u0000Lorentz factor (${Gamma}_{min} > 50$ at $sim1$ hour) constraints on a GRB in\u0000the radio band. Our results demonstrate the importance of rapid radio follow-up\u0000observations with long integrations and good sensitivity for detecting the\u0000fast-evolving radio emission from short GRBs and probing their reverse shocks.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206790","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Galactic Distribution of Supernovae and OB Associations 超新星和 OB 组合的银河系分布

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-11 DOI: arxiv-2409.07124

M. Kachelriess, V. Mikalsen

引用次数: 0

uGMRT sub-GHz view of the Sausage cluster diffuse radio sources 香肠星团漫射射电源的uGMRT亚GHz视图

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-11 DOI: arxiv-2409.07504

Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H. -Y. Karen Yang

{"title":"uGMRT sub-GHz view of the Sausage cluster diffuse radio sources","authors":"Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H. -Y. Karen Yang","doi":"arxiv-2409.07504","DOIUrl":"https://doi.org/arxiv-2409.07504","url":null,"abstract":"CIZA J2242.8+5301, or the Sausage cluster, is well studied over a range of\u0000frequencies. Since its first discovery, a lot of interesting features and\u0000unique characteristics have been uncovered. In this work, we report some more\u0000new morphological features using the uGMRT band-3 and band-4 data. In the north\u0000relic, we observe variation in spectral index profiles across the relic width\u0000from the east to west, which may indicate a decrease in downstream cooling rate\u0000in that direction. We re-confirm the presence of an additional ~ 930 kpc relic\u0000in the north. We classify the filamentary source in the downstream region to be\u0000a narrow angle tail (NAT) radio galaxy. The bright arc in the east relic shows\u0000sub-structure in the spectral index profile, which may indicate the presence of\u0000finer filaments. We further report the presence of a double-strand structure in\u0000the east relic similar to the 'Toothbrush' relic. We categorize the bright 'L'\u0000shaped structure in the southern relic to be a NAT radio galaxy, as well as\u0000trace the actual ~ 1.1 Mpc relic component. We re-confirm the existence of the\u0000faint southern extent, measuring the relic length to be ~ 1.8 Mpc. Furthermore,\u0000we suggest the southern relic to be a union of individual component relics\u0000rather than a single giant filamentary relic. Lastly, based on the\u0000morphological symmetry between northern and southern relics, we suggest a\u0000schematic shock structure associated with the merger event in an attempt to\u0000explain their formation scenario.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"75 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206840","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Fermi Blazars in the Zwicky Transient Facility Survey: Properties of Large Optical Variations 兹威基瞬变设施巡天中的费米亮星：大光学变化的特性

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-11 DOI: arxiv-2409.06917

Si-Si SunYunnan University, Zhongxiang WangYunnan University, Shun-hao JiYunnan University

{"title":"Fermi Blazars in the Zwicky Transient Facility Survey: Properties of Large Optical Variations","authors":"Si-Si SunYunnan University, Zhongxiang WangYunnan University, Shun-hao JiYunnan University","doi":"arxiv-2409.06917","DOIUrl":"https://doi.org/arxiv-2409.06917","url":null,"abstract":"We analyze the optical light-curve data, obtained with the Zwicky Transient\u0000Facility (ZTF) survey, for 47 gamma-ray blazars monitored by the Large Area\u0000Telescope onboard {it the Fermi Gamma-ray Space Telescope (Fermi)}. These 47\u0000sources are selected because they are among the Fermi blazars with the largest\u0000optical variations in the ZTF data. Two color-magnitude variation patterns are\u0000seen in them, one being redder to stable when brighter (RSWB; in 31 sources)\u0000and the other being stable when brighter (in 16 sources). The patterns fit with\u0000the results recently reported in several similar studies with different data.\u0000Moreover, we find that the colors in the stable state of the sources share\u0000similar values, which (after corrected for the Galactic extinction) of most\u0000sources are in a range of 0.4--0.55. This feature could be intrinsic and may be\u0000applied in, for example, the study of intragalactic medium. We also determine\u0000the turning points for the sources showing the RSWB pattern, after which the\u0000color changes saturate and become stable. We find a correlation between optical\u0000fluxes and gamma-ray fluxes at the turning points. The physical implications of\u0000the correlation remain to be investigated, probably better with a sample of\u0000high-quality gamma-ray flux measurements.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"6 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206843","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A detailed dive into fitting strategies for GRB afterglows with contamination: A case study with kilonovae 对有污染的 GRB 后辉光拟合策略的详细研究：千新星案例研究

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-11 DOI: arxiv-2409.07539

Wendy Fu Wallace, Nikhil Sarin

{"title":"A detailed dive into fitting strategies for GRB afterglows with contamination: A case study with kilonovae","authors":"Wendy Fu Wallace, Nikhil Sarin","doi":"arxiv-2409.07539","DOIUrl":"https://doi.org/arxiv-2409.07539","url":null,"abstract":"Observations of gamma-ray burst afterglows have begun to readily reveal\u0000contamination from a kilonova or a supernova. This contamination presents\u0000significant challenges towards traditional methods of inferring the properties\u0000of these phenomena from observations. Given current knowledge of kilonova and\u0000afterglow modelling, observations (as expected) with near-infrared bands and at\u0000early observing times provide the greatest diagnostic power for both observing\u0000the presence of a kilonova and inferences on its properties in gamma-ray burst\u0000afterglows. However, contemporaneous observations in radio and X-ray are\u0000critical for reducing the afterglow parameter space and for more efficient\u0000parameter estimation. We compare different methods for fitting joint kilonova\u0000and afterglow observations under different scenarios. We find that ignoring the\u0000contribution of one source (even in scenarios where the source is sub-dominant)\u0000can lead to significantly biased estimated parameters but could still produce\u0000great light curve fits that do not raise suspicion. This bias is also present\u0000for analyses that fit data where one source is \"subtracted\". In most scenarios,\u0000the bias is smaller than the systematic uncertainty inherent to kilonova models\u0000but significant for afterglow parameters, particularly in the absence of\u0000high-quality radio and X-ray observations. Instead, we show that the most\u0000reliable method for inference in any scenario where contamination can not be\u0000confidently dismissed is to jointly fit for both an afterglow and\u0000kilonova/supernova, and showcase a Bayesian framework to make this joint\u0000analysis computationally feasible.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"45 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206793","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0