$. We have found that in the innermost gas there is a high velocity structure, most likely indicating the presence of an outflow from the AGN while our analysis of the cluster cool core using RGS data indicates that the velocity of the gas agrees with the M87 optical redshift. An overall gradient in the velocity is seen, with larger values as we move away from the cluster core. The hot gas located within the western radio flow is redshifted, moving with a velocity $\\sim 331$ km\u002Fs while the hot gas located within the eastern radio flow is blueshifted, with a velocity $\\sim 258$ km\u002Fs, suggesting the presence of backflows. Our results reveal the effects of both AGN outflows and gas sloshing, in the complex velocity field of the Virgo cluster. ","authors":[{"name":"Efrain Gatuzz"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"name":"K. Dennerl"},{"id":"53f9c6efdabfae7f97afb7a3","name":"C. Pinto"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f4745adabfaee43ed2d4c5","name":"T. Tamura"},{"id":"53f3a8f8dabfae4b34aeb000","name":"S. A. Walker"},{"name":"J. ZuHone"}],"id":"614164545244ab9dcb9dd803","lang":"en","num_citation":0,"order":4,"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F\u002F21\u002F2109\u002F2109.06213.pdf","title":"Measuring sloshing, merging and feedback velocities in the Virgo cluster","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2109.06213"],"versions":[{"id":"614164545244ab9dcb9dd803","sid":"2109.06213","src":"arxiv","year":2021}],"year":2021},{"abstract":"We present the first joint NuSTAR and NICER observations of the ultra-compact X-ray binary (UCXB) 4U 1543$-$624 obtained in 2020 April. The source was at a luminosity of $L_{0.5-50\\\\ \\\\mathrm{keV}} = 4.9 (D\u002F7\\\\ \\\\mathrm{kpc})^{2}\\\\times10^{36}$ ergs s$^{-1}$ and showed evidence of reflected emission in the form of an O VIII line, Fe K line, and Compton hump within the spectrum. We used a full reflection model, known as xillverCO, that is tailored for the atypical abundances found in UCXBs, to account for the reflected emission. We tested the emission radii of the O and Fe line components and conclude that they originate from a common disk radius in the innermost region of the accretion disk ($R_{\\\\rm in} \\\\leq1.07\\\\ R_{\\\\mathrm{ISCO}}$). By assuming that the position of the inner disk is the Alfv\\\\\\u0027{e}n radius, we placed an upper limit on the magnetic field strength to be $B\\\\leq0.7(D\u002F7\\\\ \\\\mathrm {kpc})\\\\times10^{8}$ G at the poles. Given the lack of pulsations detected and position of $R_{\\\\rm in}$, it was likely that a boundary layer region had formed between the neutron star (NS) surface and inner edge of the accretion disk with an extent of 1.2 km. This implies a maximum radius of the neutron star accretor of $R_{\\\\mathrm{NS}}\\\\leq 12.1$ km when assuming a canonical NS mass of 1.4 $M_{\\\\odot}$.","authors":[{"name":"R. M. Ludlam"},{"name":"A. D. Jaodand"},{"id":"562ebbd345cedb3399376cd0","name":"J. A. García"},{"id":"53f4a9a2dabfaedce5639cf8","name":"N. Degenaar"},{"id":"548580b0dabfaed7b5fa2301","name":"J. A. Tomsick"},{"id":"53f46a8adabfaec09f250028","name":"E. M. Cackett"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"5448ba8fdabfae87b7e6e9b2","name":"P. Gandhi"},{"name":"D. J. K. Buisson"},{"name":"A. W. Shaw"},{"id":"53f45edddabfaeb22f51fb77","name":"D. Chakrabarty"}],"doi":"10.3847\u002F1538-4357\u002FABEDB0","id":"5fe1b6ae91e0119a161edbc2","num_citation":0,"order":6,"pages":{"start":"123"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2012\u002F2012.10461.pdf","title":"Simultaneous NICER and NuSTAR Observations of the Ultra-compact X-ray Binary 4U 1543-624","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2012.10461","https:\u002F\u002Finspirehep.net\u002Fliterature\u002F1837692"],"venue":{"info":{"name":"The Astrophysical Journal"},"issue":"2","volume":"911"},"versions":[{"id":"5fe1b6ae91e0119a161edbc2","sid":"2012.10461","src":"arxiv","year":2020},{"id":"60b9a6b0e4510cd7c8ffa18b","sid":"3158908062","src":"mag","vsid":"1980519","year":2021}],"year":2021},{"abstract":"Motivated by the recent discoveries that six ultraluminous X-ray sources (ULXs) are powered by highly super-Eddington X-ray pulsars, we searched for additional pulsating ULX (PULX) candidates by identifying sources that exhibit long-term flux variability of at least an order of magnitude (a common feature seen in the six known PULXs, which may potentially be related to transitions to the propeller regime). Expanding on previous studies, we used the available fluxes from XMM-Newton, Swift, and Chandra, along with carefully computed upper limits in cases of a non-detection, to construct long-term light curves for a sample of 296 ULXs selected from the XMM-Newton archive. Among these 296, we find 25 sources showing flux variability larger than a factor of 10, of which 17 show some evidence for (or are at least consistent with) exhibiting bimodal flux distributions, as would be expected for sources undergoing propeller transitions. These sources are excellent candidates for continued monitoring programs to further test for this behaviour. There are three sources in our final sample with fluxes similar to NGC 5907 ULX1, currently the faintest known PULX, which would also be good targets for deeper observations with current facilities to search for pulsations. For the rest of the PULX candidates identified here, the next generation of X-ray telescopes (such as Athena) may be required to determine their nature owing to their lower peak fluxes.","authors":[{"name":"X Song"},{"id":"561e7ec745ce1e5964935785","name":"D J Walton"},{"name":"G B Lansbury"},{"name":"P A Evans"},{"id":"54068c09dabfae92b421034c","name":"A C Fabian"},{"name":"H Earnshaw"},{"id":"54053b63dabfae91d3fc9940","name":"T P Roberts"}],"doi":"10.1093\u002Fmnras\u002Fstz3036","id":"5e09a85adf1a9c0c41688b6e","num_citation":0,"order":4,"pages":{"end":"1277","start":"1260"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F19\u002F1910\u002F1910.11857.pdf","title":"The Hunt for Pulsating Ultraluminous X-ray Sources","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"1","volume":"491"},"versions":[{"id":"5e09a85adf1a9c0c41688b6e","sid":"2984764068","src":"mag","vsid":"195663288","year":2019},{"id":"5db6c73a3a55acec0731cee5","sid":"1910.11857","src":"arxiv","year":2019},{"id":"5fc9b047d83c7e914aa1a683","sid":"WOS:000512163600085","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020}],"year":2020},{"abstract":"We explore how X-ray reverberation around black holes may reveal the presence of the innermost stable circular orbit (ISCO), predicted by general relativity, and probe the dynamics of the plunging region between the ISCO and the event horizon. Being able to directly detect the presence of the ISCO and probe the dynamics of material plunging through the event horizon represents a unique test of general relativity in the strong field regime. X-ray reverberation off of the accretion disc and material in the plunging region is modelled using general relativistic ray tracing simulations. X-ray reverberation from the plunging region has a minimal effect on the time-averaged X-ray spectrum and the overall lag-energy spectrum, but is manifested in the lag in the highest frequency Fourier components, above 0.01 c(3) (GM)(-1) (scaled for the mass of the black hole) in the 2-4 keV energy band for a non-spinning black hole or the 1-2 keV energy band for a maximally spinning black hole. The plunging region is distinguished from disc emission not just by the energy shifts characteristic of plunging orbits, but by the rapid increase in ionization of material through the plunging region. Detection requires measurement of time lags to an accuracy of 20 per cent at these frequencies. Improving accuracy to 12 per cent will enable constraints to be placed on the dynamics of material in the plunging region and distinguish plunging orbits from material remaining on stable circular orbits, confirming the existence of the ISCO, a prime discovery space for future X-ray missions.","authors":[{"name":"Wilkins D. R."},{"id":"54853b27dabfaed7b5fa1fad","name":"Reynolds C. S."},{"id":"54068c09dabfae92b421034c","name":"Fabian A. C."}],"doi":"10.1093\u002Fmnras\u002Fstaa628","id":"5e5f7c3d91e011df604ec6cc","num_citation":0,"order":2,"pages":{"end":"5550","start":"5532"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2003\u002F2003.00019.pdf","title":"Venturing beyond the ISCO: Detecting X-ray emission from the plunging regions around black holes","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2003.00019","http:\u002F\u002Fwww.webofknowledge.com\u002F","https:\u002F\u002Farxiv.org\u002Fpdf\u002F2003.00019.pdf","http:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020MNRAS.493.5532W\u002Fabstract","http:\u002F\u002Fexport.arxiv.org\u002Fpdf\u002F2003.00019","https:\u002F\u002Fit.arxiv.org\u002Fabs\u002F2003.00019","https:\u002F\u002Fau.arxiv.org\u002Fabs\u002F2003.00019","https:\u002F\u002Ffr.arxiv.org\u002Fabs\u002F2003.00019","https:\u002F\u002Fru.arxiv.org\u002Fabs\u002F2003.00019","https:\u002F\u002Fexport.arxiv.org\u002Fabs\u002F2003.00019"],"venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"4","volume":"493"},"versions":[{"id":"5e5f7c3d91e011df604ec6cc","sid":"2003.00019","src":"arxiv","year":2020},{"id":"5fc9b011d83c7e914aa17c46","sid":"WOS:000539094400070","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020},{"id":"60741bfde4510cd7c86ef094","sid":"3007979212","src":"mag","vsid":"195663288","year":2020}],"year":2020},{"abstract":"Hercules X-1 is one of the best-studied highly magnetized neutron star X-ray binaries with a wealth of archival data. We present the discovery of an ionized wind in its X-ray spectrum when the source is in the high state. The wind detection is statistically significant in most of the XMM-Newton observations, with velocities ranging from 200 to 1000 km s(-1). Observed features in the iron K band can be explained by both wind absorption and a forest of iron emission lines. However, we also detect nitrogen, oxygen, and neon absorption lines at the same systematic velocity in the high-resolution Reflection Grating Spectrometer grating spectra. The wind must be launched from the accretion disc, and could be the progenitor of the ultraviolet absorption features observed at comparable velocities, but the latter likely originate at significantly larger distances from the compact object. We find strong correlations between the ionization level of the outflowing material and the ionizing luminosity as well as the superorbital phase. If the luminosity is driving the correlation, the wind could be launched by a combination of Compton heating and radiation pressure. If instead the superorbital phase is the driver for the variations, the observations are likely scanning the wind at different heights above the warped accretion disc. If this is the case, we can estimate the wind mass outflow rate, corrected for the limited launching solid angle, to be roughly 70 per cent of the mass accretion rate.","authors":[{"name":"P Kosec"},{"id":"54068c09dabfae92b421034c","name":"A C Fabian"},{"id":"53f9c6efdabfae7f97afb7a3","name":"C Pinto"},{"id":"561e7ec745ce1e5964935785","name":"D J Walton"},{"name":"S Dyda"},{"id":"54853b27dabfaed7b5fa1fad","name":"C S Reynolds"}],"doi":"10.1093\u002Fmnras\u002Fstz3200","id":"5e09a797df1a9c0c41678d8a","num_citation":0,"order":1,"pages":{"end":"3750","start":"3730"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F19\u002F1910\u002F1910.08337.pdf","title":"An ionised accretion disc wind in Hercules X-1","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"3","volume":"491"},"versions":[{"id":"5e09a797df1a9c0c41678d8a","sid":"2983054376","src":"mag","vsid":"195663288","year":2020},{"id":"5dad81bd3a55acd0ec6ebcfe","sid":"1910.08337","src":"arxiv","year":2019},{"id":"5fc9b046d83c7e914aa1a5eb","sid":"WOS:000512306500043","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020}],"year":2020},{"abstract":"A variety of large-scale diffuse radio structures have been identified in many clusters with the advent of new state-of-the-art facilities in radio astronomy. Among these diffuse radio structures, radio mini-halos are found in the central regions of cool core clusters. Their origin is still unknown and they are challenging to discover; less than 30 have been published to date. Based on new VLA observations, we confirmed the mini-halo in the massive strong cool core cluster PKS 0745-191 (z = 0.1028) and discovered one in the massive cool core cluster MACS J1447.4+0827 (z = 0.3755). Furthermore, using a detailed analysis of all known mini-halos, we explore the relation between mini-halos and active galactic nucleus (AGN) feedback processes from the central galaxy. We find evidence of strong, previously unknown correlations between mini-halo radio power and X-ray cavity power, and between mini-halo and the central galaxy radio power related to the relativistic jets when spectrally decomposing the AGN radio emission into a component for past outbursts and one for ongoing accretion. Overall, our study indicates that mini-halos are directly connected to the central AGN in clusters, following previous suppositions. We hypothesize that AGN feedback may be one of the dominant mechanisms giving rise to mini-halos by injecting energy into the intra-cluster medium and reaccelerating an old population of particles, while sloshing motion may drive the overall shape of mini-halos inside cold fronts. AGN feedback may therefore not only play a vital role in offsetting cooling in cool core clusters, but may also play a fundamental role in re-energizing non-thermal particles in clusters.","authors":[{"name":"A. Richard-Laferrière"},{"id":"53f47460dabfaeee22a87ad3","name":"J. Hlavacek-Larrondo"},{"name":"R. S. Nemmen"},{"name":"C. L. Rhea"},{"name":"G. B. Taylor"},{"name":"M. Prasow-Émond"},{"name":"M. Gendron-Marsolais"},{"name":"M. Latulippe"},{"id":"53f4347ddabfaedce551ce3a","name":"A. C. Edge"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f4374cdabfaedf435878e9","name":"J. S. Sanders"},{"name":"M. T. Hogan"},{"name":"G. Demontigny"}],"doi":"10.1093\u002Fmnras\u002Fstaa2877","id":"5f02e86391e011ee5e0257c0","num_citation":0,"order":9,"pages":{"end":"2958","start":"2934"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2007\u002F2007.01306.pdf","title":"On the relation between mini-halos and AGN feedback in clusters of galaxies","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2007.01306","http:\u002F\u002Fwww.webofknowledge.com\u002F","https:\u002F\u002Farxiv.org\u002Fpdf\u002F2007.01306","https:\u002F\u002Fexport.arxiv.org\u002Fabs\u002F2007.01306","https:\u002F\u002Fexport.arxiv.org\u002Fpdf\u002F2007.01306","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020MNRAS.499.2934R\u002Fabstract","https:\u002F\u002Fjp.arxiv.org\u002Fpdf\u002F2007.01306","https:\u002F\u002Fuk.arxiv.org\u002Fpdf\u002F2007.01306","https:\u002F\u002Fza.arxiv.org\u002Fabs\u002F2007.01306","https:\u002F\u002Fuk.arxiv.org\u002Fabs\u002F2007.01306"],"venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"2","volume":"499"},"versions":[{"id":"5f02e86391e011ee5e0257c0","sid":"2007.01306","src":"arxiv","year":2020},{"id":"5fd57f43a4e4c3c831a59ffe","sid":"WOS:000587762900100","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020},{"id":"60741de3e4510cd7c870866c","sid":"3039503757","src":"mag","vsid":"195663288","year":2020}],"year":2020},{"abstract":"Chandra X-ray observations are analyzed for five galaxy clusters whose atmospheric cooling times, entropy parameters, and ratios of cooling time to freefall time within the central galaxies lie below 1 Gyr, below 30 keV cm(2), and between 20 less than or similar to min(t(cool)\u002Ft(ff)) less than or similar to 50, respectively. These thermodynamic properties are commonly associated with molecular clouds, bright H alpha emission, and star formation in central galaxies. However, all have H alpha luminosities below 10(40)erg s(-1)in the ACCEPT database. Star formation and molecular gas are absent at the levels seen in other central galaxies with similar atmospheric properties. Only RBS 0533 may host a radio\u002FX-ray bubble, which are commonly observed in cooling atmospheres. Signatures of uplifted, high-metallicity atmospheric gas are absent. Their atmospheres are apparently thermodynamically stable despite the absence of strong nuclear feedback. We suggest that extended filaments of nebular emission and associate molecular clouds are absent at appreciable levels because their central radio sources have failed to lift low-entropy atmospheric gas to an altitude where the ratio of the cooling time to the freefall time falls below unity and the gas becomes thermally unstable.","authors":[{"name":"Martz C. G."},{"id":"53f4353bdabfaeb22f467922","name":"McNamara B. R."},{"id":"54315157dabfae8f291441ce","name":"Nulsen P. E. J."},{"name":"Vantyghem A. N."},{"name":"Gingras M-J."},{"name":"Babyk Iu. V."},{"id":"53f4352cdabfaedce552496a","name":"Russell H. R."},{"id":"53f4347ddabfaedce551ce3a","name":"Edge A. C."},{"id":"5406e79bdabfae92b4228f5f","name":"McDonald M."},{"name":"Tamhane P. D."},{"id":"54068c09dabfae92b421034c","name":"Fabian A. C."},{"name":"Hogan M. T."}],"doi":"10.3847\u002F1538-4357\u002Fab96cd","id":"5e7c7d3c91e011f07751bba6","num_citation":0,"order":10,"pages":{"start":"57"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2003\u002F2003.11104.pdf","title":"Thermally Unstable Cooling Stimulated by Uplift: The Spoiler Clusters","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2003.11104","https:\u002F\u002Fiopscience.iop.org\u002Farticle\u002F10.3847\u002F1538-4357\u002Fab96cd\u002Fpdf","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020ApJ...897...57M\u002Fabstract","https:\u002F\u002Fdro.dur.ac.uk\u002F31484\u002F","https:\u002F\u002Fresearch-repository.uwa.edu.au\u002Fen\u002Fpublications\u002Fthermally-unstable-cooling-stimulated-by-uplift-the-spoiler-clust","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"1","volume":"897"},"versions":[{"id":"5e7c7d3c91e011f07751bba6","sid":"2003.11104","src":"arxiv","year":2020},{"id":"5fae6f66d4150a363cef28e3","sid":"3038190972","src":"mag","vsid":"1980519","year":2020},{"id":"5ff68bbad4150a363cd02e47","sid":"3100157207","src":"mag","vsid":"1980519","year":2020},{"id":"5fc6f8aed75e2ac63d58ec44","sid":"WOS:000549984300001","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2020}],"year":2020},{"abstract":"We report on the first simultaneous Neutron Star Interior Composition Explore (NICER) and Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the neutron star (NS) low-mass X-ray binary 4U 1735-44, obtained in 2018 August. The source was at a luminosity of similar to 1.8 (D\u002F5.6 kpc)(2) x 10(37) erg s(-1) in the 0.4-30 keV band. We account for the continuum emission with two different continuum descriptions that have been used to model the source previously. Despite the choice in continuum model, the combined passband reveals a broad Fe K line indicative of reflection in the spectrum. In order to account for the reflection spectrum we utilize a modified version of the reflection model relxill that is tailored for thermal emission from accreting NSs. Alternatively, we also use the reflection convolution model of rfxconv to model the reflected emission that would arise from a Comptonized thermal component for comparison. We determine that the innermost region of the accretion disk extends close to the innermost stable circular orbit (R-ISCO) at the 90% confidence level regardless of reflection model. Moreover, the current flux calibration of NICER is within 5% of the NuSTAR\u002FFPMA(B).","authors":[{"name":"Ludlam R. M."},{"id":"53f46a8adabfaec09f250028","name":"Cackett E. M."},{"id":"562ebbd345cedb3399376cd0","name":"García J. A."},{"id":"53f47182dabfaefedbb9abea","name":"Miller J. M."},{"id":"53f47720dabfaefedbbb10ef","name":"Bult P. M."},{"id":"5487f892dabfae8a11fb3f8d","name":"Strohmayer T. E."},{"id":"53f435acdabfaee43ec29e87","name":"Guillot S."},{"name":"Jaisawal G. K."},{"name":"Malacaria C."},{"id":"54068c09dabfae92b421034c","name":"Fabian A. C."},{"id":"53f4290fdabfaeb2acfb557a","name":"Markwardt C. B."}],"doi":"10.3847\u002F1538-4357\u002Fab89a6","id":"5e982cc591e0119e8a952437","num_citation":0,"order":9,"pages":{"start":"45"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2004\u002F2004.06723.pdf","title":"NICER-NuSTAR Observations of the Neutron Star Low-Mass X-ray Binary 4U 1735-44","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2004.06723","http:\u002F\u002Fwww.webofknowledge.com\u002F","http:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020ApJ...895...45L\u002Fabstract","https:\u002F\u002Fiopscience.iop.org\u002Farticle\u002F10.3847\u002F1538-4357\u002Fab89a6"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"1","volume":"895"},"versions":[{"id":"5e982cc591e0119e8a952437","sid":"2004.06723","src":"arxiv","year":2020},{"id":"5fc6f8b0d75e2ac63d58ede7","sid":"WOS:000536905900001","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2020},{"id":"6075428ce4510cd7c832077f","sid":"3026841424","src":"mag","vsid":"1980519","year":2020}],"year":2020},{"abstract":"We present simple XSPEC models for fitting excess variance spectra of active galactic nuclei. Using a simple Monte Carlo approach, we simulate a range of spectra corresponding to physical parameters varying, then calculate the resulting variance spectra. Starting from a variable power law, we build up a set of models corresponding to the different physical processes that can affect the final excess variance spectrum. We show that the complex excess variance spectrum of IRAS 13224-3809 can be well described by such an intrinsic variability model, where the power-law variability is damped by relativistic reflection and enhanced by an ultra-fast outflow. The reflection flux is correlated with that of the power law, but not perfectly. We argue that this correlation is stronger at high frequencies, where reverberation lags are detected, while excess variance spectra are typically dominated by low-frequency variability.","authors":[{"name":"M L Parker"},{"name":"W N Alston"},{"name":"Z Igo"},{"id":"54068c09dabfae92b421034c","name":"A C Fabian"}],"doi":"10.1093\u002Fmnras\u002Fstz3470","id":"5e5e18cf93d709897ce31e85","num_citation":0,"order":3,"pages":{"end":"1369","start":"1363"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F19\u002F1910\u002F1910.12808.pdf","title":"Modelling X-ray RMS spectra I: intrinsically variable AGNs","urls":["http:\u002F\u002Facademic.oup.com\u002Fmnras\u002Fadvance-article-pdf\u002Fdoi\u002F10.1093\u002Fmnras\u002Fstz3470\u002F31489484\u002Fstz3470.pdf","https:\u002F\u002Farxiv.org\u002Fabs\u002F1910.12808","http:\u002F\u002Fwww.webofknowledge.com\u002F","http:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020MNRAS.492.1363P\u002Fabstract","https:\u002F\u002Facademic.oup.com\u002Fmnras\u002Farticle-abstract\u002F492\u002F1\u002F1363\u002F5672646","http:\u002F\u002Facademic.oup.com\u002Fmnras\u002Farticle-abstract\u002F492\u002F1\u002F1363\u002F5672646","https:\u002F\u002Farxiv.org\u002Fpdf\u002F1910.12808"],"venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"1","volume":"492"},"versions":[{"id":"5e5e18cf93d709897ce31e85","sid":"2995921224","src":"mag","vsid":"195663288","year":2020},{"id":"5db80dc83a55acd5c14a2717","sid":"1910.12808","src":"arxiv","year":2019},{"id":"5fc9b02ed83c7e914aa192b6","sid":"WOS:000512329900104","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020},{"id":"607419d2e4510cd7c86cf929","sid":"2982142804","src":"mag","vsid":"195663288","year":2020}],"year":2020},{"abstract":"We present Atacama Large Millimetre\u002Fsubmillimetre Array observations of the brightest cluster galaxy Hydra-A, a nearby (z = 0.054) giant elliptical galaxy with powerful and extended radio jets. The observations reveal CO(1-0), CO(2-1), (CO)-C-13(2-1), CN(2-1), SiO(5-4), HCO+(1-0), HCO+(2-1), HCN(1-0), HCN(2-1), HNC(1-0), and H2CO(3-2) absorption lines against the galaxy's bright and compact active galactic nucleus. These absorption features are due to at least 12 individual molecular clouds that lie close to the centre of the galaxy and have velocities of approximately -50 to +10 km s(-1) relative to its recession velocity, where positive values correspond to inward motion. The absorption profiles are evidence of a clumpy interstellar medium within brightest cluster galaxies composed of clouds with similar column densities, velocity dispersions, and excitation temperatures to those found at radii of several kpc in the Milky Way. We also show potential variation in a similar to 10 km s(-1) wide section of the absorption profile over a 2 yr time-scale, most likely caused by relativistic motions in the hot spots of the continuum source that change the background illumination of the absorbing clouds.","authors":[{"name":"Rose Tom"},{"id":"53f4347ddabfaedce551ce3a","name":"Edge A. C."},{"id":"53f431d0dabfaec22ba50ab9","name":"Combes F."},{"id":"53f42e6edabfaedd74d44558","name":"Hamer S."},{"id":"53f4353bdabfaeb22f467922","name":"McNamara B. R."},{"id":"53f4352cdabfaedce552496a","name":"Russell H."},{"id":"53f83ff8dabfae9060b1eaf6","name":"Gaspari M."},{"id":"53f7bb04dabfae9060ae2114","name":"Salomé P."},{"id":"54053ce4dabfae91d3fca2ab","name":"Sarazin C."},{"id":"53f4423fdabfaee43ec70158","name":"Tremblay G. R."},{"id":"543256d4dabfaeb4c6a7f40e","name":"Baum S. A."},{"id":"53f462ecdabfaeee22a46c56","name":"Bremer M. N."},{"id":"53f4396cdabfaec22ba9dfae","name":"Donahue M."},{"id":"54068c09dabfae92b421034c","name":"Fabian A. C."},{"id":"53f42e56dabfaee0d9b09481","name":"Ferland G."},{"id":"53f470d7dabfaeee22a7a435","name":"Nesvadba N."},{"id":"5484a1e8dabfae8a11fb2174","name":"O'Dea C."},{"id":"53f451d1dabfaeee22a231d9","name":"Oonk J. B. R."},{"id":"53f36e43dabfae4b349b7b65","name":"Peck A. B."}],"doi":"10.1093\u002Fmnras\u002Fstaa1474","id":"5ec7a32791e0118397f3eda5","num_citation":0,"order":13,"pages":{"end":"380","start":"364"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2005\u002F2005.10252.pdf","title":"A molecular absorption line survey toward the AGN of Hydra-A","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2005.10252","https:\u002F\u002Fresearch-information.bris.ac.uk\u002Fen\u002Fpublications\u002Fa-molecular-absorption-line-survey-toward-the-agn-of-hydra-a","http:\u002F\u002Fexport.arxiv.org\u002Fabs\u002F2005.10252","http:\u002F\u002Fexport.arxiv.org\u002Fpdf\u002F2005.10252","http:\u002F\u002Farxiv.org\u002Fpdf\u002F2005.10252.pdf","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"1","volume":"496"},"versions":[{"id":"5ec7a32791e0118397f3eda5","sid":"2005.10252","src":"arxiv","year":2020},{"id":"5fae67f9d4150a363ce15d5c","sid":"3026733908","src":"mag","vsid":"195663288","year":2020},{"id":"5fd57f78a4e4c3c831a5cfee","sid":"WOS:000560784700027","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020}],"year":2020},{"abstract":"The black hole candidate and X-ray binary MAXI J1535-571 was discovered in 2017 September. During the decay of its discovery outburst, and before returning to quiescence, the source underwent at least four reflaring events, with peak luminosities of similar to 10(35-36) erg s(-1) (d\u002F4.1 kpc)(2). To investigate the nature of these flares, we analysed a sample of NICER (Neutron star Interior Composition Explorer) observations taken with almost daily cadence. In this work, we present the detailed spectral and timing analysis of the evolution of the four reflares. The higher sensitivity of NICER at lower energies, in comparison with other X-ray detectors, allowed us to constrain the disc component of the spectrum at similar to 0.5 keV. We found that during each reflare the source appears to trace out a q-shaped track in the hardness-intensity diagram similar to those observed in black hole binaries during full outbursts. MAXI J1535 -571 transits between the hard state (valleys) and softer states (peaks) during these flares. Moreover, the Comptonized component is undetected at the peak of the first reflare, while the disc component is undetected during the valleys. Assuming the most likely distance of 4.1 kpc, we find that the hard-to-soft transitions take place at the lowest luminosities ever observed in a black hole transient, while the soft-to-hard transitions occur at some of the lowest luminosities ever reported for such systems.","authors":[{"name":"Cúneo V. A."},{"name":"Alabarta K."},{"id":"542ed5badabfaea2e89f6731","name":"Zhang L."},{"id":"53f43221dabfaec22ba54bd2","name":"Altamirano D."},{"id":"5630ede745ce1e59687ba319","name":"Méndez M."},{"id":"53f476c7dabfaeecd6a4bf0f","name":"Padilla M. Armas"},{"id":"53f43ae8dabfaee1c0ac9221","name":"Remillard R."},{"id":"5410450edabfae44f0891e91","name":"Homan J."},{"id":"5434ce9bdabfaebba58695d5","name":"Steiner J. F."},{"id":"5485e1bcdabfaed7b5fa25ef","name":"Combi J. A."},{"name":"Muñoz-Darias T."},{"id":"53f42d58dabfaec22ba17483","name":"Gendreau K. C."},{"id":"53f443f6dabfaeb22f4b5d1d","name":"Arzoumanian Z."},{"name":"Stevens A. L."},{"name":"Loewenstein M."},{"id":"53f453e6dabfaeb22f4f7157","name":"Tombesi F."},{"id":"53f47720dabfaefedbbb10ef","name":"Bult P."},{"id":"54068c09dabfae92b421034c","name":"Fabian A. C."},{"name":"Buisson D. J. K."},{"name":"Neilsen J."}],"doi":"10.1093\u002Fmnras\u002Fstaa1606","id":"5ede11fa91e0116152461aba","num_citation":0,"order":17,"pages":{"end":"1012","start":"1001"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fupload\u002Fpdf\u002F106\u002F1441\u002F1615\u002F5ede11fa91e0116152461aba_0.pdf","title":"A NICER look at the state transitions of the black hole candidate MAXI J1535-571 during its reflares","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2006.03074","http:\u002F\u002Fwww.webofknowledge.com\u002F","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020MNRAS.496.1001C\u002Fabstract","https:\u002F\u002Farxiv.org\u002Fabs\u002F2006.03074v1","https:\u002F\u002Facademic.oup.com\u002Fmnras\u002Farticle\u002F496\u002F2\u002F1001\u002F5855052","https:\u002F\u002Fwww.narcis.nl\u002Fpublication\u002FRecordID\u002Foai%3Apure.rug.nl%3Apublications%2F3104eecf-e924-46f3-a43b-1ec224b48ef6","https:\u002F\u002Farxiv.org\u002Fpdf\u002F2006.03074v2","https:\u002F\u002Finspirehep.net\u002Fliterature\u002F1799651","http:\u002F\u002Fexport.arxiv.org\u002Fpdf\u002F2006.03074","http:\u002F\u002Facademic.oup.com\u002Fmnras\u002Farticle-abstract\u002F496\u002F2\u002F1001\u002F5855052","http:\u002F\u002Fexport.arxiv.org\u002Fabs\u002F2006.03074"],"venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"2","volume":"496"},"versions":[{"id":"5ede11fa91e0116152461aba","sid":"2006.03074","src":"arxiv","year":2020},{"id":"5fc9b081d83c7e914aa1d856","sid":"WOS:000561118000001","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020},{"id":"60741d86e4510cd7c87039e3","sid":"3033832622","src":"mag","vsid":"195663288","year":2020}],"year":2020},{"abstract":" Galactic outflows are known to consist of several gas phases, however, so far the connection between these multiple phases has been investigated little and only in a few objects. In this paper, we analyse MUSE\u002FVLT data of 26 local (U)LIRGs and study their ionised and neutral atomic phases. We also include objects from the literature to obtain a total sample of 31 galaxies with spatially resolved multi-phase outflow information. We find that the ionized phase of the outflows has on average an electron density three times higher than the disc ($n_{\\rm e, disc}$ $\\sim$ 150 cm$^{-3}$ vs $n_{\\rm e, outflow}$ $\\sim$ 500 cm$^{-3}$), suggesting that cloud compression in the outflow is more important that cloud dissipation. We find that the difference in extinction between outflow and disc correlates with the outflow gas mass. Together with the analysis of the outflow velocities, this suggests that at least some of the outflows are associated with the ejection of dusty clouds from the disc. The presence of dust in outflows is relevant for potential formation of molecules inside them. We combine our data with millimetre data to investigate the molecular phase. We find that the molecular phase accounts for more than 60 $\\%$ of the total mass outflow rate in most objects and this fraction is higher in AGN-dominated systems. The neutral atomic phase contributes of the order of 10 $\\%$, while the ionized phase is negligible. The ionized-to-molecular mass outflow rate declines slightly with AGN luminosity, although with a large scatter. ","authors":[{"name":"A. Fluetsch"},{"id":"548719c2dabfae8a11fb3604","name":"R. Maiolino"},{"name":"S. Carniani"},{"id":"53f4cba3dabfaee57778172d","name":"S. Arribas"},{"name":"F. Belfiore"},{"name":"E. Bellocchi"},{"name":"S. Cazzoli"},{"name":"C. Cicone"},{"id":"53f44d53dabfaefedbb2ed70","name":"G. Cresci"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f47983dabfaefedbbb8580","name":"R. Gallagher"},{"name":"W. Ishibashi"},{"id":"53f43964dabfaee1c0ab9b3e","name":"F. Mannucci"},{"id":"53f42eaddabfaee0d9b0da50","name":"A. Marconi"},{"id":"53f43500dabfaeb2ac046ae8","name":"M. Perna"},{"id":"53f438abdabfaee02acdfd1e","name":"E. Sturm"},{"id":"53f42d2cdabfaedd74d33932","name":"G. Venturi"}],"doi":"10.1093\u002Fmnras\u002Fstab1666","id":"5ef476b691e01165a63bba61","num_citation":0,"order":9,"title":"Properties of the Multiphase Outflows in Local (Ultra)luminous Infrared Galaxies","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2006.13232"],"versions":[{"id":"5ef476b691e01165a63bba61","sid":"2006.13232","src":"arxiv","year":2021}],"year":2020},{"abstract":"We continue the analysis of NuSTAR data from the recent discovery outburst of MAXI J1820+070 (optical counterpart ASASSN-18ey), focussing on an observation including unusual flaring behaviour during the hard to soft state transition, which is a short phase of outbursts and so comparatively rarely observed. Two plateaus in flux are separated by a variable interval lasting ∼10 ks, which shows dipping then flaring stages. The variability is strongest (with fractional variability up to F Var ∼10 per cent FVar∼10 per cent) at high energies and reduces as the contribution from disc emission becomes stronger. Flux-resolved spectra show that the variability is primarily due to the power-law flux changing. We also find a long soft lag of the thermal behind the power-law emission, which is 20 +1.6 −1.2 20−1.2+1.6  s during the flaring phase. The lag during the dipping stage has a different lag–energy spectrum, which may be due to a wave passing outwards through the disc. Time-resolved spectral fitting suggests that the lag during the flaring stage may be due to the disc re-filling after being disrupted to produce the power-law flare, perhaps related to the system settling after the jet ejection which occurred around 1 d before. The time-scales of these phenomena imply a low viscosity parameter, α ∼ 10−3, for the inner region of the disc.","authors":[{"name":"D. J. K. Buisson"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f435c5dabfaeb1a7beee99","name":"P. Gandhi"},{"id":"53f45766dabfaedf4360f7d4","name":"E. Kara"},{"name":"M. L. Parker"},{"name":"A. W. Shaw"},{"id":"548580b0dabfaed7b5fa2301","name":"J. A. Tomsick"},{"id":"53f472a6dabfaefedbb9f1f2","name":"D. J. Walton"},{"id":"53f43a99dabfaee4dc7aa8ad","name":"J. Wang"}],"doi":"10.1093\u002FMNRAS\u002FSTAA3510","id":"5fa4007991e011a6939b82bb","num_citation":0,"order":1,"pages":{"end":"3986","start":"3976"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2011\u002F2011.02472.pdf","title":"MAXI J1820+070 with NuSTAR II. Flaring during the hard to soft state transition with a long soft lag","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2011.02472","https:\u002F\u002Farxiv.org\u002Fpdf\u002F2011.02472","https:\u002F\u002Feprints.soton.ac.uk\u002F446230\u002F","https:\u002F\u002Facademic.oup.com\u002Fmnras\u002Farticle\u002F500\u002F3\u002F3976\u002F5979788","http:\u002F\u002Fexport.arxiv.org\u002Fpdf\u002F2011.02472","http:\u002F\u002Fexport.arxiv.org\u002Fabs\u002F2011.02472","http:\u002F\u002Farxiv.org\u002Fpdf\u002F2011.02472.pdf"],"venue":{"info":{"name":"Monthly Notices of the Royal Astronomical Society"},"issue":"3","volume":"500"},"versions":[{"id":"5fa4007991e011a6939b82bb","sid":"2011.02472","src":"arxiv","year":2020},{"id":"60741f7de4510cd7c871f464","sid":"3095421815","src":"mag","vsid":"195663288","year":2020}],"year":2020},{"abstract":"We present a deep XMM-Newton observation of the extremely massive, rapidly rotating, relativistic-jet-launching spiral galaxy 2MASX J23453268-0449256. Diffuse X-ray emission from the hot gaseous halo around the galaxy is robustly detected out to a radius of 160 kpc, corresponding roughly to 35 per cent of the virial radius ($\\\\approx 450$ kpc). We fit the X-ray emission with the standard isothermal $\\\\beta$ model, and it is found that the enclosed gas mass within 160 kpc is $1.15_{-0.24}^{+0.22} \\\\times 10^{11} \\\\, \\\\rm{M}_{\\\\odot}$. Extrapolating the gas mass profile out to the virial radius, the estimated gas mass is $8.25_{-1.77}^{+1.62} \\\\times 10^{11} \\\\, \\\\rm{M}_{\\\\odot}$, which makes up roughly 65 per cent of the total baryon mass content of the galaxy. When the stellar mass is considered and accounting for the statistical and systematic uncertainties, the baryon mass fraction within the virial radius is $0.121_{-0.043}^{+0.043}$, in agreement with the universal baryon fraction. The baryon mass fraction is consistent with all baryons falling within $r_{200}$, or with only half of the baryons falling within $r_{200}$. Similar to the massive spiral galaxies NGC 1961 and NGC 6753, we find a low value for the metal abundance of $\\\\approx 0.1 {\\\\rm{Z}}_{\\\\odot}$, which appears uniform with radius. We also detect diffuse X-ray emission associated with the northern and southern lobes, possibly attributed to inverse Compton scattering of cosmic microwave background photons. The estimated energy densities of the electrons and magnetic field in these radio lobes suggest that they are electron-dominated by a factor of 10$-$200, depending on the choice of the lower cut-off energy of the electron spectrum.","authors":[{"name":"M. S. Mirakhor"},{"id":"53f3a8f8dabfae4b34aeb000","name":"S. A. Walker"},{"id":"53f4d56ddabfaeedd37834c2","name":"J. Bagchi"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"5484a253dabfaed7b5fa1a87","name":"A. J. Barth"},{"id":"53f431d0dabfaec22ba50ab9","name":"F. Combes"},{"name":"P. Dabhade"},{"id":"5433f08ddabfaebba58306a0","name":"L. C. Ho"},{"name":"M. B. Pandge"}],"doi":"10.1093\u002FMNRAS\u002FSTAA3404","id":"5f9bd74691e011dcf482d7d5","num_citation":0,"order":3,"pages":{"end":"2513","start":"2503"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2010\u002F2010.15131.pdf","title":"Exploring the hot gaseous halo around an extremely massive and relativistic jet launching spiral galaxy with XMM-Newton","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2010.15131","https:\u002F\u002Fscholarlypublications.universiteitleiden.nl\u002Fhandle\u002F1887\u002F3146866\u002F","https:\u002F\u002Fhal.archives-ouvertes.fr\u002Fhal-03034754","https:\u002F\u002Fwww.mysciencework.com\u002Fpublication\u002Fshow\u002Fexploring-hot-gaseous-halo-around-extremely-massive-relativistic-jet-launching-spiral-galaxy-xmmnewton-343c2644"],"venue":{"info":{"name":"Monthly Notices of the Royal Astronomical Society"},"issue":"2","volume":"500"},"versions":[{"id":"5f9bd74691e011dcf482d7d5","sid":"2010.15131","src":"arxiv","year":2020},{"id":"60741f7de4510cd7c871f498","sid":"3095607707","src":"mag","vsid":"195663288","year":2020}],"year":2020},{"abstract":"We present new broadband X-ray observations of the type-I Seyfert galaxy IRAS 09149-6206, taken in 2018 with $XMM$-$Newton$, $NuSTAR$ and $Swift$. The source is highly complex, showing a classic \\u0027warm\\u0027 X-ray absorber, additional absorption from highly ionised iron, strong relativistic reflection from the innermost accretion disc and further reprocessing by more distant material. By combining X-ray timing and spectroscopy, we have been able to fully characterise the supermassive black hole in this system, constraining both its mass and - for the first time - its spin. The mass is primarily determined by X-ray timing constraints on the break frequency seen in the power spectrum, and is found to be $\\\\log[M_{\\\\rm{BH}}\u002FM_{\\\\odot}] = 8.0 \\\\pm 0.6$ (1$\\\\sigma$ uncertainties). This is in good agreement with previous estimates based on the H$\\\\alpha$ and H$\\\\beta$ line widths, and implies that IRAS 09149-6206 is radiating at close to (but still below) its Eddington luminosity. The spin is constrained via detailed modelling of the relativistic reflection, and is found to be $a^* = 0.94^{+0.02}_{-0.07}$ (90% confidence), adding IRAS 09149-6206 to the growing list of radio-quiet AGN that host rapidly rotating black holes. The outflow velocities of the various absorption components are all relatively modest ($v_{\\\\rm{out}} \\\\lesssim 0.03c$), implying these are unlikely to drive significant galaxy-scale AGN feedback.","authors":[{"id":"53f472a6dabfaefedbb9f1f2","name":"D. J. Walton"},{"name":"W. N. Alston"},{"name":"P. Kosec"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f42da9dabfaee02ac64b4f","name":"L. C. Gallo"},{"id":"562ebbd345cedb3399376cd0","name":"J. A. Garcia"},{"id":"53f47182dabfaefedbb9abea","name":"J. M. Miller"},{"id":"561e7ec745ce1e596493576f","name":"E. Nardini"},{"id":"53f31fb1dabfae9a8444e947","name":"M. T. Reynolds"},{"id":"5406ede4dabfae450f3f7518","name":"C. Ricci"},{"id":"561e7ec745ce1e596493579c","name":"D. Stern"},{"name":"T. Dauser"},{"id":"53f436b8dabfaeee229adee1","name":"F. A. Harrison"},{"id":"54853b27dabfaed7b5fa1fad","name":"C. S. Reynolds"}],"doi":"10.1093\u002FMNRAS\u002FSTAA2961","id":"5f6c61a891e0119671e8575f","num_citation":0,"order":3,"pages":{"end":"1498","start":"1480"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2009\u002F2009.10734.pdf","title":"A Full Characterisation of the Supermassive Black Hole in IRAS 09149-6206","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2009.10734","https:\u002F\u002Farxiv.org\u002Fpdf\u002F2009.10734","http:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020MNRAS.499.1480W\u002Fabstract","https:\u002F\u002Facademic.oup.com\u002Fmnras\u002Farticle\u002F499\u002F1\u002F1480\u002F5917086","http:\u002F\u002Fexport.arxiv.org\u002Fpdf\u002F2009.10734"],"venue":{"info":{"name":"Monthly Notices of the Royal Astronomical Society"},"issue":"1","volume":"499"},"versions":[{"id":"5f6c61a891e0119671e8575f","sid":"2009.10734","src":"arxiv","year":2020},{"id":"607543ade4510cd7c834b465","sid":"3088252398","src":"mag","vsid":"195663288","year":2020}],"year":2020},{"abstract":"We study reflected X-ray emission that returns to the accretion disc in the strong gravitational fields around black holes using General Relativistic ray-tracing and radiative transfer calculations. Reflected X-rays that are produced when the inner regions of the disc are illuminated by the corona are subject to strong gravitational light bending, causing up to 47 per cent of the reflected emission to be returned to the disc around a rapidly spinning black hole, depending upon the scale height of the corona. The iron K alpha line is enhanced relative to the continuum by 25 per cent, and the Compton hump by up to a factor of 3. Additional light traveltime between primary and secondary reflections increases the reverberation time lag measured in the iron K band by 49 per cent, while the soft X-ray lag is increased by 25 per cent and the Compton hump response time is increased by 60 per cent. Measured samples of X-ray reverberation lags are shown to be consistent with X-rays returning to the accretion disc in strong gravity. Understanding the effects of returning radiation is important in interpreting reverberation observations to probe black holes. Reflected X-rays returning to the disc can be uniquely identified by blueshifted returning iron K line photons that are Compton scattered from the inner disc, producing excess, delayed emission in the 3.5-4.5 keV energy range that will be detectable with forthcoming X-ray observatories, representing a unique test of General Relativity in the strong field limit.","authors":[{"name":"D. R. Wilkins"},{"id":"562ebbd345cedb3399376cd0","name":"J. A. García"},{"name":"T. Dauser"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"}],"doi":"10.1093\u002Fmnras\u002Fstaa2566","id":"5f3e3c3891e011c0de1c28fe","num_citation":0,"order":3,"pages":{"end":"3319","start":"3302"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2008\u002F2008.08083.pdf","title":"Returning radiation in strong gravity around black holes: Reverberation from the accretion disc","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2008.08083","https:\u002F\u002Farxiv.org\u002Fpdf\u002F2008.08083.pdf","http:\u002F\u002Fexport.arxiv.org\u002Fpdf\u002F2008.08083","http:\u002F\u002Fexport.arxiv.org\u002Fabs\u002F2008.08083","https:\u002F\u002Fjp.arxiv.org\u002Fpdf\u002F2008.08083","https:\u002F\u002Fjp.arxiv.org\u002Fabs\u002F2008.08083","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"3","volume":"498"},"versions":[{"id":"5f3e3c3891e011c0de1c28fe","sid":"2008.08083","src":"arxiv","year":2020},{"id":"5ff68400d4150a363cbc7d65","sid":"3079765146","src":"mag","vsid":"195663288","year":2020},{"id":"5fd57f44a4e4c3c831a5a085","sid":"WOS:000587752500017","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020}],"year":2020},{"abstract":"We present results of temporal and spectral analyses on four XMM-Newton EPIC pn observations of IRAS 17020+4544, a narrow-line Seyfert 1 galaxy with evidence of a radio jet. Analysis of the light curves reveals that this radio-loud source does not behave like the bulk population of its radio-quiet counterparts. A trend of spectral hardening with increased flux is found. Variability is found to increase with energy, though it decreases as the spectrum hardens. The first 40 ks of the most recent observation behave uniquely among the epochs, exhibiting a softer spectral state than at any other time. Possible non-stationarity at low energies is found, with no such effect present at higher energies, suggesting at least two distinct spectral components. A reverberation signature is confirmed, with the lag-frequency, lag-energy, and covariance spectra changing significantly during the soft-state epoch. The temporal analysis suggests a variable power law in the presence of a reflection component, thus motivating such a fit for the 0.3-10 keV EPIC pn spectra from all epochs. We find an acceptable spectral fit using the timing-motivated parameters and report the detection of a broad Fe K emission line, requiring an additional model component beyond the reflection spectrum. We discuss links between this source and other narrow-line Seyfert 1 sources that show evidence of jet activity, finding similarities among this currently very limited sample of interesting objects.","authors":[{"name":"Gonzalez A. G."},{"id":"53f42da9dabfaee02ac64b4f","name":"Gallo L. C."},{"name":"Kosec P."},{"id":"54068c09dabfae92b421034c","name":"Fabian A. C."},{"name":"Alston W. N."},{"name":"Berton M."},{"name":"Wilkins D. R."}],"doi":"10.1093\u002Fmnras\u002Fstaa1735","id":"5ee9f15b91e01152af022f07","num_citation":0,"order":3,"pages":{"end":"3724","start":"3708"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fupload\u002Fpdf\u002F988\u002F926\u002F1316\u002F5ee9f15b91e01152af022f07_0.pdf","title":"Characterising continuum variability in the radio-loud narrow-line Seyfert 1 galaxy IRAS 17020+4544","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2006.09330","http:\u002F\u002Farxiv.org\u002Fpdf\u002F2006.09330.pdf","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"3","volume":"496"},"versions":[{"id":"5ee9f15b91e01152af022f07","sid":"2006.09330","src":"arxiv","year":2020},{"id":"5fae6dafd4150a363cec0f93","sid":"3035103275","src":"mag","vsid":"195663288","year":2020},{"id":"5fd57f77a4e4c3c831a5ced2","sid":"WOS:000574919300070","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2020}],"year":2020},{"abstract":"The launch of the Nuclear Spectroscopic Telescope Array (NuSTAR) heralded a new era of sensitive high-energy X-ray spectroscopy for X-ray binaries (XRBs). In this paper we show how multiple physical parameters can be measured from the accretion disc spectrum when the high-energy side of the disc spectrum can be measured precisely using NuSTAR. This immediately makes two exciting developments possible. If the mass and distance of the source are known, the continuum fitting method can be used to calculate the spin and inner disc inclination independently of the iron line fitting method. If the mass and distance are unknown, the two methods can be combined to constrain these values to a narrow region of parameter space. In this paper we perform extensive simulations to establish the reliability of these techniques. We find that with high-quality spectra, spin and inclination can indeed be simultaneously measured using the disc spectrum. These measurements are much more precise at higher spin values, where the relativistic effects are stronger. The inclusion of a soft X-ray snapshot observation alongside the NuSTAR data significantly improves the reliability, particularly for lower temperature discs, as it gives a greatly improved measurement of the disc peak. High signal-to-noise data are not necessary for this, as measuring the peak temperature is relatively easy. We discuss the impact of systematic effects on this technique, and the implications of our results such as robust measurements of accretion disc warps and XRB mass surveys.","authors":[{"name":"M. L. Parker"},{"name":"D. J. K. Buisson"},{"id":"548580b0dabfaed7b5fa2301","name":"J. A. Tomsick"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"name":"K. K. Madsen"},{"id":"561e7ec745ce1e5964935785","name":"D. J. Walton"},{"id":"53f428b2dabfaeb22f3d1305","name":"F. Furst"}],"doi":"10.1093\u002Fmnras\u002Fstz045","id":"5ce2d0e7ced107d4c63cdb00","lang":"en","num_citation":0,"order":3,"pages":{"end":"1212","start":"1202"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F19\u002F1901\u002F1901.00683.pdf","title":"XRB continuum fitting with sensitive high-energy X-ray detectors","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"1","volume":"484"},"versions":[{"id":"5ce2d0e7ced107d4c63cdb00","sid":"2907456482","src":"mag","vsid":"195663288","year":2019},{"id":"5c615f57e1cd8eae1501b3a0","sid":"1901.00683","src":"arxiv","year":2019},{"id":"5fc9afadd83c7e914aa13d92","sid":"WOS:000462293100084","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2019}],"year":2019},{"abstract":"We report the discovery with the Neutron Star Interior Composition Explorer (NICER) of narrow emission and absorption lines during photospheric radius expansion (PRE) X-ray bursts from the ultracompact binary 4U 1820-30. NICER observed 4U 1820-30 in 2017 August during a low-flux, hard spectral state, accumulating about 60 ks of exposure. Five thermonuclear X-ray bursts were detected, of which four showed clear signs of PRE. We extracted spectra during the PRE phases and fit each to a model that includes a Comptonized component to describe the accretion-driven emission, and a blackbody for the burst thermal radiation. The temperature and spherical emitting radius of the fitted blackbody are used to assess the strength of PRE in each burst. The two strongest PRE bursts (burst pair 1) had blackbody temperatures of approximate to 0.6 keV and emitting radii of approximate to 100 km (at a distance of 8.4 kpc). The other two bursts (burst pair 2) had higher temperatures (approximate to 0.67 keV) and smaller radii (approximate to 75 km). All of the PRE bursts show evidence of narrow line emission near 1 keV. By coadding the PRE phase spectra of burst pairs 1 and, separately, 2, we find, in both coadded spectra, significant, narrow, spectral features near 1.0 (emission), 1.7, and 3.0 keV (both in absorption). Remarkably, all the fitted line centroids in the coadded spectrum of burst pair 1 appear systematically blueshifted by a factor of 1.046 +\u002F- 0.006 compared to the centroids of pair 2, strongly indicative of a gravitational shift, a wind-induced blueshift, or more likely some combination of both effects. The observed shifts are consistent with this scenario in that the stronger PRE bursts in pair 1 reach larger photospheric radii, and thus have weaker gravitational redshifts, and they generate faster outflows, yielding higher blueshifts. We discuss possible elemental identifications for the observed features in the context of recent burst-driven wind models.","authors":[{"id":"53f42e40dabfaeb22f413be3","name":"T. E. Strohmayer"},{"id":"53f43221dabfaec22ba54bd2","name":"D. Altamirano"},{"id":"5487bcd4dabfaed7b5fa32a6","name":"Z. Arzoumanian"},{"id":"53f47720dabfaefedbbb10ef","name":"P. M. Bult"},{"id":"53f3669ddabfae4b3499c48c","name":"D. Chakrabarty"},{"id":"53f42c9edabfaec09f1097cd","name":"J. Chenevez"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f3b101dabfae4b34b1c0d7","name":"K. C. Gendreau"},{"id":"53f435acdabfaee43ec29e87","name":"S. Guillot"},{"id":"54055e1ddabfae8faa5c83ed","name":"J. J. M. In 't Zand"},{"name":"G. K. Jaisawal"},{"id":"53f4d035dabfaeedd977dca0","name":"L. Keek"},{"name":"P. Kosec"},{"name":"R. M. Ludlam"},{"name":"S. Mahmoodifar"},{"name":"Christian Malacaria"},{"id":"53f47182dabfaefedbb9abea","name":"J. M. Miller"}],"doi":"10.3847\u002F2041-8213\u002Fab25eb","id":"5d9ed3b347c8f76646f971f1","num_citation":0,"order":6,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F19\u002F1906\u002F1906.00974.pdf","title":"NICER Discovers Spectral Lines during Photospheric Radius Expansion Bursts from 4U 1820−30: Evidence for Burst-driven Winds","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL LETTERS"},"issue":"2","volume":"878"},"versions":[{"id":"5d9ed3b347c8f76646f971f1","sid":"2951426188","src":"mag","vsid":"1980519","year":2019},{"id":"5cf828233a55ac460c40a863","sid":"1906.00974","src":"arxiv","year":2019},{"id":"5fc6fa3ed75e2ac63d59a8b7","sid":"WOS:000471732800001","src":"wos","vsid":"ASTROPHYSICAL JOURNAL LETTERS","year":2019}],"year":2019},{"abstract":"We present recent Chandra X-ray observations of the RX J0821.0+0752 galaxy cluster, in addition to ALMA observations of the CO(1-0) and CO(3-2) line emission tracing the molecular gas in its central galaxy. All of the CO line emission, originating from a 10(10) M-circle dot molecular gas reservoir, is located several kiloparsecs away from the nucleus of the central galaxy. The cold gas is concentrated into two main clumps surrounded by a diffuse envelope. They form a wide filament coincident with a plume of bright X-ray emission emanating from the cluster core. This plume encompasses a putative X-ray cavity that is only large enough to have uplifted a small percent of the molecular gas. Unlike other brightest cluster galaxies, stimulated cooling, where X-ray cavities lift low-entropy cluster gas until it becomes thermally unstable, cannot have produced the observed gas reservoir. Instead, the molecular gas has likely formed as a result of sloshing motions in the intracluster medium induced by a nearby galaxy. Sloshing can emulate uplift by dislodging gas from the galactic center. This gas has the shortest cooling time, so it will condense if disrupted for long enough.","authors":[{"name":"A. N. Vantyghem"},{"id":"53f4353bdabfaeb22f467922","name":"B. R. McNamara"},{"id":"53f4352cdabfaedce552496a","name":"H. R. Russell"},{"id":"53f4347ddabfaedce551ce3a","name":"A. C. Edge"},{"id":"54315157dabfae8f291441ce","name":"P. E. J. Nulsen"},{"id":"53f431d0dabfaec22ba50ab9","name":"F. Combes"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"5406e79bdabfae92b4228f5f","name":"M. McDonald"},{"id":"53f7bb04dabfae9060ae2114","name":"P. Salome"}],"doi":"10.3847\u002F1538-4357\u002Faaf1b4","id":"5ce2d03dced107d4c635a0c8","lang":"en","num_citation":0,"order":6,"pages":{"end":"","start":"57"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F18\u002F1811\u002F1811.09653.pdf","title":"An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"870"},"versions":[{"id":"5ce2d03dced107d4c635a0c8","sid":"2901098887","src":"mag","vsid":"1980519","year":2019},{"id":"5c615f12e1cd8eae1501a7aa","sid":"1811.09653","src":"arxiv","year":2018},{"id":"5ff68b77d4150a363ccf602d","sid":"3099286198","src":"mag","vsid":"1980519","year":2019},{"id":"5fc6f84fd75e2ac63d58a6a0","sid":"WOS:000455820100003","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2019}],"year":2019}],"profilePubsTotal":1247,"profilePatentsPage":1,"profilePatents":[],"profilePatentsTotal":0,"profilePatentsEnd":true,"profileProjectsPage":0,"profileProjects":null,"profileProjectsTotal":null,"newInfo":null,"checkDelPubs":[]}};