Monthly Notices of the Royal Astronomical Society最新文献_第6页

Photometric Re-calibration of VPHAS+ u-band photometry with the stellar colour regression method and gaia DR3 利用恒星颜色回归法和 gaia DR3 对 VPHAS+ u 波段光度测量进行光度再校准

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-22 DOI: 10.1093/mnras/stae1104

Bing-Qiu Chen, Hai-Bo Yuan, Bo-Wen Huang

{"title":"Photometric Re-calibration of VPHAS+ u-band photometry with the stellar colour regression method and gaia DR3","authors":"Bing-Qiu Chen, Hai-Bo Yuan, Bo-Wen Huang","doi":"10.1093/mnras/stae1104","DOIUrl":"https://doi.org/10.1093/mnras/stae1104","url":null,"abstract":"\u0000 The u band magnitude is vital for determining stellar parameters and investigating specific astronomical objects. However, flux calibration in the u band for stars in the Galactic disk presents significant challenges. In this study, we introduce a comprehensive re-calibration of u-band photometric magnitudes of the VPHAS+ Data Release 4 (DR4), employing the Stellar Colour Regression (SCR) technique. By leveraging the expansive set of XP spectra and GBP photometry from Gaia Data Release 3 (DR3), as well as the individual stellar extinction values provided by the literature, we have obtained precise model magnitudes of nearly 3 million stars. Our analysis identifies systematic magnitude offsets that exhibit a standard deviation of 0.063 mag across different observational visits, 0.022 mag between various CCDs, and 0.009 mag within pixel bins. We have implemented precise corrections for these observational visits, CCD chips, and pixel bins-dependent magnitude offsets. These corrections have led to a reduction in the standard deviation between the observed magnitudes and the model magnitudes from 0.088 mag to 0.065 mag, ensuring that the calibrated magnitudes are independent of stellar magnitude, colour, and extinction. The enhanced precision of these magnitudes substantially improves the quality of astrophysical research and offers substantial potential for furthering our understanding of stellar astrophysics.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"45 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140672872","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 impact of a top-heavy IMF on the formation and evolution of dark star clusters 头重脚轻的 IMF 对暗星团形成和演化的影响

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-22 DOI: 10.1093/mnras/stae936

Ali Rostami Shirazi, H. Haghi, A. H. Zonoozi, Ahmad Farhani Asl, P. Kroupa

{"title":"The impact of a top-heavy IMF on the formation and evolution of dark star clusters","authors":"Ali Rostami Shirazi, H. Haghi, A. H. Zonoozi, Ahmad Farhani Asl, P. Kroupa","doi":"10.1093/mnras/stae936","DOIUrl":"https://doi.org/10.1093/mnras/stae936","url":null,"abstract":"\u0000 The Spitzer instability leads to the formation of a black hole sub-system (BHSub) at the center of a star cluster providing energy to luminous stars (LSs) and increasing their rate of evaporation. When the self-depletion time of the BHSub exceeds the evaporation time of the LSs, a dark star cluster (DSC) will appear. Using the NBODY7 code, we performed a comprehensive set of direct N-body simulations over a wide range of initial conditions to study the pure effect of the top-heaviness of the IMF on the formation of the DSC phase. In the Galactic tidal field, top-heavy IMFs lead to the fast evaporation of LSs and the formation of DSCs. Therefore, DSCs can be present even in the outer region of the Milky Way (MW). To successfully transition to the DSC phase, the MW Globular Clusters (GCs) must possess an initial BH mass fraction of $widetilde{mathit {M}}_mathrm{BH}(0)>0.05$. For star clusters with $widetilde{mathit {M}}_mathrm{BH}(0)>0.08$, the DSC phase will be created for any given initial density of the cluster and Galactocentric distance. The duration of the cluster’s lifetime spent in the DSC phase shows a negative (positive) correlation with the initial density, and Galactocentric distance of the star cluster if $widetilde{mathit {M}}_mathrm{BH}(0)le 0.12$ ($widetilde{mathit {M}}_mathrm{BH}(0)ge 0.15$). Considering the canonical IMF, it is unlikely for any MW GCs to enter the DSC phase. We discuss the BH retention fraction in view of the observed properties of the GCs of the MW.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"1 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140674654","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 formation of transiting circumplanetary debris discs from the disruption of satellite systems during planet–planet scattering 行星-行星散射过程中卫星系统被扰乱而形成的凌星环行碎片盘

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-18 DOI: 10.1093/mnras/stae1074

A. Mustill, Melvyn B. Davies, M. Kenworthy

{"title":"The formation of transiting circumplanetary debris discs from the disruption of satellite systems during planet–planet scattering","authors":"A. Mustill, Melvyn B. Davies, M. Kenworthy","doi":"10.1093/mnras/stae1074","DOIUrl":"https://doi.org/10.1093/mnras/stae1074","url":null,"abstract":"\u0000 Several stars show deep transits consistent with discs of roughly 1 R⊙ seen at moderate inclinations, likely surrounding planets on eccentric orbits. We show that this configuration arises naturally as a result of planet–planet scattering when the planets possess satellite systems. Planet–planet scattering explains the orbital eccentricities of the discs’ host bodies, while the close encounters during scattering lead to the exchange of satellites between planets and/or their destabilisation. This leads to collisions between satellites and their tidal disruption close to the planet. Both of these events lead to large quantities of debris being produced, which in time will settle into a disc such as those observed. The mass of debris required is comparable to a Ceres-sized satellite. Through N-body simulations of planets with clones of the Galilean satellite system undergoing scattering, we show that 90 % of planets undergoing scattering will possess debris from satellite destruction. Extrapolating to smaller numbers of satellites suggests that tens of percent of such planets should still possess circumplanetary debris discs. The debris trails arising from these events are often tilted at tens of degrees to the planetary orbit, consistent with the inclinations of the observed discs. Disruption of satellite systems during scattering thus simultaneously explains the existence of debris, the tilt of the discs, and the eccentricity of the planets they orbit.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140689875","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

Characterising Tidal Features Around Galaxies in Cosmological Simulations 描述宇宙学模拟中星系周围的潮汐特征

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-18 DOI: 10.1093/mnras/stae1064

Aman Khalid, S. Brough, Garreth Martin, Lucas C. Kimmig, C. Lagos, R. Remus, C. Martínez-Lombilla

{"title":"Characterising Tidal Features Around Galaxies in Cosmological Simulations","authors":"Aman Khalid, S. Brough, Garreth Martin, Lucas C. Kimmig, C. Lagos, R. Remus, C. Martínez-Lombilla","doi":"10.1093/mnras/stae1064","DOIUrl":"https://doi.org/10.1093/mnras/stae1064","url":null,"abstract":"\u0000 Tidal features provide signatures of recent mergers and offer a unique insight into the assembly history of galaxies. The Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST) will enable an unprecedentedly large survey of tidal features around millions of galaxies. To decipher the contributions of mergers to galaxy evolution it will be necessary to compare the observed tidal features with theoretical predictions. Therefore, we use cosmological hydrodynamical simulations NewHorizon, eagle, IllustrisTNG, and Magneticum to produce LSST-like mock images of z ∼ 0 galaxies (z ∼ 0.2 for NewHorizon) with $M_{scriptstyle star ,text{ 30 pkpc}}ge 10^{9.5}$ M$_{scriptstyle odot }$. We perform a visual classification to identify tidal features and classify their morphology. We find broadly good agreement between the simulations regarding their overall tidal feature fractions: $f_{small {rm NEWHORIZON}}=0.40pm 0.06$, $f_{small {rm EAGLE}}=0.37pm 0.01$, $f_{small {rm TNG}}=0.32pm 0.01$ and $f_{small {rm MAGNETICUM}}=0.32pm 0.01$, and their specific tidal feature fractions. Furthermore, we find excellent agreement regarding the trends of tidal feature fraction with stellar and halo mass. All simulations agree in predicting that the majority of central galaxies of groups and clusters exhibit at least one tidal feature, while the satellite members rarely show such features. This agreement suggests that gravity is the primary driver of the occurrence of visually-identifiable tidal features in cosmological simulations, rather than subgrid physics or hydrodynamics. All predictions can be verified directly with LSST observations.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 18","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140688086","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

Evidence for a nearly orthogonal rotator in GX 301–2 with phase-resolved cyclotron resonant scattering features 利用相位分辨回旋共振散射特征证明 GX 301-2 中存在近乎正交的旋转器

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-18 DOI: 10.1093/mnras/stae1071

Xiao Chen, Yuanze Ding, Wei Wang, Osamu Nishimura, Qi Liu, S. Zhang, Ming-Yu Ge, Fang-Jun Lu, Jinlu Qu, Li-pei Song, Shu Zhang

{"title":"Evidence for a nearly orthogonal rotator in GX 301–2 with phase-resolved cyclotron resonant scattering features","authors":"Xiao Chen, Yuanze Ding, Wei Wang, Osamu Nishimura, Qi Liu, S. Zhang, Ming-Yu Ge, Fang-Jun Lu, Jinlu Qu, Li-pei Song, Shu Zhang","doi":"10.1093/mnras/stae1071","DOIUrl":"https://doi.org/10.1093/mnras/stae1071","url":null,"abstract":"\u0000 Cyclotron resonant scattering features (CRSFs) are the absorption features in the X-ray spectra of strongly magnetized accretion neutron stars (NSs), which are probably the most reliable probe to the surface magnetic fields of NSs. The high mass X-ray binary GX 301–2 exhibits a very wide, variable and complicated CRSF in the average spectra, which should be two absorption lines based on NuStar and Insight-HXMT observations. With the Insight-HXMT frequent observations, we performed the phase-resolved spectroscopy and confirmed two cyclotron absorption lines in the phase-resolved spectra, with their centroid energy ratio ∼1.6 − 1.7 in the super-critical luminosity case. A major hindrance in understanding those CRSFs is the very poorly constrained magnetic inclination angle, which is also a fundamental property of a NS and key to understanding the emission characteristics of a pulsar. Comparing the phase-resolved CRSF with simulated X-ray spectra, the magnetic inclination angle is found to be ≳ 70○, i.e., nearly orthogonal between the NS’s spin and magnetic axies. The implications of an orthogonal rotator and magnetic structure evolution in the accreting X-ray binary are also discussed.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140686939","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

Modelling stochastic and quasi-periodic behaviour in stellar time-series: Gaussian process regression versus power-spectrum fitting 恒星时间序列中的随机和准周期行为建模：高斯过程回归与功率谱拟合

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-17 DOI: 10.1093/mnras/stae1059

Niamh K. O'Sullivan, S. Aigrain

{"title":"Modelling stochastic and quasi-periodic behaviour in stellar time-series: Gaussian process regression versus power-spectrum fitting","authors":"Niamh K. O'Sullivan, S. Aigrain","doi":"10.1093/mnras/stae1059","DOIUrl":"https://doi.org/10.1093/mnras/stae1059","url":null,"abstract":"\u0000 As the hunt for an Earth-like exoplanets has intensified in recent years, so has the effort to characterise and model the stellar signals that can hide or mimic small planetary signals. Stellar variability arises from a number of sources, including granulation, supergranulation, oscillations and activity, all of which result in quasi-periodic or stochastic behaviour in photometric and/or radial velocity observations. Traditionally, the characterisation of these signals has mostly been done in the frequency domain. However, the recent development of scalable Gaussian process regression methods makes direct time-domain modelling of stochastic processes a feasible and arguably preferable alternative, obviating the need to estimate the power spectral density of the data before modelling it. In this paper, we compare the two approaches using a series of experiments on simulated data. We show that frequency domain modelling can lead to inaccurate results, especially when the time sampling is irregular. By contrast, Gaussian process regression results are often more precise, and systematically more accurate, in both the regular and irregular time sampling regimes. While this work was motivated by the analysis of radial velocity and photometry observations of main sequence stars in the context of planet searches, we note that our results may also have applications for the study of other types of astrophysical variability such as quasi-periodic oscillations in X-ray binaries and active galactic nuclei variability.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140690586","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 S-PLUS fornax project (S+FP): SExtractor detection and measurement of nearby galaxies in large photometric surveys S-PLUS fornax 项目（S+FP）：在大型测光巡天中对附近星系进行 SExtractor 探测和测量

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-16 DOI: 10.1093/mnras/stae1053

R. F. Haack, A. V. S. Castelli, C. M. de Oliveira, F. Almeida-Fernandes, F. Faifer, A. Lopes, Y. Jaffe, R. Demarco, C. Lima-Dias, L. Lomel'i-Nunez, G. P. Montaguth, W. Schoenell, T. Ribeiro, A. Kanaan

{"title":"The S-PLUS fornax project (S+FP): SExtractor detection and measurement of nearby galaxies in large photometric surveys","authors":"R. F. Haack, A. V. S. Castelli, C. M. de Oliveira, F. Almeida-Fernandes, F. Faifer, A. Lopes, Y. Jaffe, R. Demarco, C. Lima-Dias, L. Lomel'i-Nunez, G. P. Montaguth, W. Schoenell, T. Ribeiro, A. Kanaan","doi":"10.1093/mnras/stae1053","DOIUrl":"https://doi.org/10.1093/mnras/stae1053","url":null,"abstract":"\u0000 All-sky multi-band photometric surveys represent a unique opportunity of exploring rich nearby galaxy clusters up to several virial radii, reaching the filament regions where pre-processing is expected to occur. These projects aim to tackle a large number of astrophysical topics, encompassing both the galactic and extragalactic fields. In that sense, generating large catalogues with homogeneous photometry for both resolved and unresolved sources that might be interesting to achieve specific goals, imposes a compromise when choosing the set of parameters to automatically detect and measure such a plethora of objects. In this work we present the acquired experience on studying the galaxy content of the Fornax cluster using large catalogues obtained by the Southern Photometric Local Universe Survey (S-PLUS). We realized that some Fornax bright galaxies are missed in the S-PLUS iDR4 catalogues. In addition, Fornax star-forming galaxies are included as multiple detections due to over-deblending. To solve those issues, we performed specific SExtractor runs to identify the proper set of parameters to recover as many Fornax galaxies as possible with confident photometry and avoiding duplications. From that process, we obtained new catalogs containing 12-band improved photometry for ∼3 × 106 resolved and unresolved sources in an area of ∼208 deg2 in the direction of the Fornax cluster. Together with identifying the main difficulties to carry out the study of nearby groups and clusters of galaxies using S-PLUS catalogs, we also share possible solutions to face issues that seem to be common to other ongoing photometric surveys.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"5 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140696822","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

Correction to: VLBI astrometry of radio stars to link radio and optical celestial reference frames: observing strategies 更正为射电恒星的 VLBI 天体测量以连接射电和光学天体参照系：观测策略

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-13 DOI: 10.1093/mnras/stae935

引用次数: 0

Doppler tomography as a tool for characterising exoplanet atmospheres II: an analysis of HD 179949 b 作为系外行星大气特征描述工具的多普勒层析成像 II：对 HD 179949 b 的分析

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-08 DOI: 10.1093/mnras/stae906

S. M. Matthews, C. A. Watson, E. D. de Mooij, T. R. Marsh, M. Brogi, S. R. Merritt, K. W. Smith, D. Steeghs

{"title":"Doppler tomography as a tool for characterising exoplanet atmospheres II: an analysis of HD 179949 b","authors":"S. M. Matthews, C. A. Watson, E. D. de Mooij, T. R. Marsh, M. Brogi, S. R. Merritt, K. W. Smith, D. Steeghs","doi":"10.1093/mnras/stae906","DOIUrl":"https://doi.org/10.1093/mnras/stae906","url":null,"abstract":"\u0000 High-resolution Doppler spectroscopy provides an avenue to study the atmosphere of both transiting and non-transiting planets. This powerful method has also yielded some of the most robust atmospheric detections to date. Currently, high-resolution Doppler spectroscopy detects atmospheric signals by cross-correlating observed data with a model atmospheric spectrum. This technique has been successful in detecting various molecules such as H2O, CO, HCN and TiO, as well as several atomic species. Here we present an alternative method of performing high-resolution Doppler spectroscopy, using a technique known as Doppler tomography. We present an analysis of HD 179949 b using Doppler tomography and provide Doppler tomograms confirming previous detections of CO at 2.3 μm and H2O at both 2.3 μm and 3.5 μmwithin the atmosphere of HD 179949 b, showing significantly lower background noise levels when compared to cross-correlation methods applied to the same data. We also present a novel detection of H2O at 2.1 μm as well as a tentative detection of CO on the night side of the planet at 2.3 μm. This represents the first observational evidence for molecular absorption in the night-side emission spectrum of an exoplanet using Doppler spectroscopy.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"237 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140730654","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

Correction to: The invisible black widow PSR J1720–0534: implications for the electron density towards the North Polar Spur 更正：看不见的黑寡妇PSR J1720-0534：对北极刺电子密度的影响

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-05 DOI: 10.1093/mnras/stae879

引用次数: 0