Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: disc atmosphere or wind?
D. J. K. Buisson, D. Altamirano, M. Díaz Trigo, M. Mendez, M. Armas Padilla, N. Castro Segura, N. D. Degenaar, J. van den Eijnden, F. A. Fogantini, P. Gandhi, C… 展开作者
D. J. K. Buisson, D. Altamirano, M. Díaz Trigo, M. Mendez, M. Armas Padilla, N. Castro Segura, N. D. Degenaar, J. van den Eijnden, F. A. Fogantini, P. Gandhi, C. Knigge, T. Muñoz-Darias, M. Özbey Arabacı, F. M. Vincentelli
We find soft X-ray emission lines from the X-ray binary Swift J1858.6-0814 in data from XMM-Newton-RGS: N VII, O VII and O VIII, as well as notable residuals short of a detection at Ne IX and other higher ionisation transitions. These could be associated with the disc atmosphere, as in accretion disc corona sources, or with a wind, as has been detected in Swift J1858.6-0814 in emission lines at optical wavelengths. Indeed, the N VII line is redshifted, consistent with being the emitting component of a P-Cygni profile. We find that the emitting plasma has an ionisation parameter $\log(ξ)=1.35\pm0.2$ and a density $n>1.5\times10^{11}$ cm$^{-3}$. From this, we infer that the emitting plasma must be within $10^{13}$ cm of the ionising source, $\sim5\times10^{7}r_{\rm g}$ for a $1.4M_{\odot}$ neutron star, and from the line width that it is at least $10^4r_{\rm g}$ away ($2\times10^{9}(M/1.4M_{\odot})$ cm). We compare this with known classes of emission line regions in other X-ray binaries and active galactic nuclei.
Dynamics of X-Ray-Emitting Ejecta in the Oxygen-Rich Supernova Remnant Puppis A Revealed by the XMM-Newton RGS
利用XMM-牛顿号上反射光栅光谱仪（RGS）前所未有的光谱分辨率，我们揭示了富氧超新星遗迹船尾座A中发射X射线的喷出物的动力学。RGS光谱显示出突出的K壳层线，包括O VII He_alpha禁戒和共振，O VIII Ly_alpha，O VIII Ly_beta和Ne IX He_alpha共振，这些线来自与光学富氧细丝（遗迹东北部所谓的Omega细丝）位置一致的喷出物结。我们发现，线的质心蓝移了1480+/-140+/-60 km/s（第一和第二项误差分别是测量和校准不确定性），这是完全一致的光学欧米茄灯丝。在654 eV（对应于O VIII Ly_alpha）处获得的谱线展宽小于~0.9 eV，表明氧温度小于~30 keV。对XMM-牛顿MOS谱的分析表明，电子温度约为0.8 keV，电离时标约为2 e10 cm^-3 s。我们表明，氧和电子的温度以及电离时标可以调和，如果喷出物结被加热的碰撞冲击，其速度是~600-1200公里/秒，随后由于库仑相互作用平衡。RGS光谱还显示了位于残骸东北边缘附近的另一个喷出物特征的相对较弱的K壳层线，从中我们测量到650+/-70+/-60 km/s的向红多普勒速度。
XMM-Newton multi-year campaign on NGC 55 ULX-1: Resolving the wind and its variability with RGS
INAF – IASF Palermo（意大利国家天体物理研究所帕勒莫天文台）；Università degli Studi di Palermo, Dipartimento di Fisica e Chimica（巴勒莫大学物理与化学系）；Center for Astrophysics – Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；Department of Astronomy & Physics, Saint Mary’s University（圣玛丽大学天文与物理系）；Université de Toulouse, CNRS, IRAP（图卢兹大学，法国国家科学研究中心，天体物理研究所在）；INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano（意大利国家天体物理研究所米兰空间天体物理与宇宙物理研究所）；Institute of Space Sciences (ICE), CSIC（西班牙国家研究委员会空间科学研究所）；INAF – Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；Department of Physics, Centre for Extragalactic Astronomy, Durham University（杜伦大学物理系河外天文中心）
We present XMM-Newton observations of N132D, the X-ray brightest supernova remnant (SNR) in the Large Magellanic Cloud (LMC), using the Reflection Grating Spectrometer (RGS) that enables high-resolution spectroscopy in the soft X-ray band. A dozen emission lines from L-shell transitions of various elements at intermediate charge states are newly detected in the RGS data integrating the ~200-ks on-axis observations. The 0.3-2.0-keV spectra require at least three components of thermal plasmas with different electron temperatures and indicate clear evidence of non-equilibrium ionization (NEI). Ou…
Variability of the X-ray obscuring wind in Mrk 335 with XMM-Newton/RGS
University of Chicago（芝加哥大学）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；Saint Mary’s University（圣玛丽大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；The Ohio State University（俄亥俄州立大学）；Technion（以色列理工学院）
We present a 140ks observation of NGC 4593 with XMM-Newton providing simultaneous and continuous PN X-ray and OM UV (UVW1 2910Å) lightcurves which sample short-timescale variations better than previous observations. These observations were simultaneous with 22d of Swift X-ray and UV/optical monitoring, reported previously, and 4d of AstroSat X-ray (SXT), far (FUV 1541Å), and near (NUV 2632Å) UV allowing lag measurements between them and the highly-sampled XMM. From the XMM we find that UVW1 lags behind the X-rays by 29.5$\pm$1.3ks, $\sim$half the lag previously determined from the Swift monito…
We report on the XMM-Newton observation of HP Cet and Swift J0820.6-2805, two X-ray photon sources that are candidates to be members of the intermediate polar class of cataclysmic variables. If the historical optical light curve of HP Cet shows a periodic feature at $\simeq 96$ minutes, a clear identification of such a signature in the high energy band (apart for a variability on a time scale of $\simeq 8$ minutes as detected by the ROSAT satellite) is lacking. By using XMM-Newton archive data, we clearly identify a feature (at $\simeq 88$ minutes) which is marginally consistent with one of th…
A spectral and timing study of MAXI J1535-571, based on Swift/XRT, XMM-Newton and NICER observations obtained in fall 2017
我们对2017年秋季新探测到的X射线瞬态MAXI J1535-571进行了光谱定时分析。在我们的研究中，我们包括38个Swift/XRT窗口定时模式观测，3个XMM-牛顿观测和31个NICER观测。计算了黑洞瞬变过程中常用的基本图，拟合了功率密度和能谱，研究了谱参数和时间参数的演化。观测到的性质与明亮的黑洞X射线双星（$F_{\mathrm{0.6-10 keV}}^{\mathrm{max}}=3.71\pm0.02\times10^{-7}$ erg cm $^{-2}$ s $^{-1}$）一致，该双星从低硬态演化到高软态，再回到低硬态。在一些观测中，功率密度谱显示出C型准周期振荡，这进一步证明了MAXI J1535-571在这些观测中处于硬态。不到10天的软状态持续时间非常短，2018年春季的观测表明，MAXI J1535-571进入了第二个（更长）软状态。
Probing the physics of the accretion flow around active galactic nuclei (AGN) is crucial to understanding their emission mechanisms as well as being able to constrain the geometrical and variability properties of the different regions around them. The soft X-ray excess -- usually observed below $\sim2\,\mathrm{keV}$ in excess of the dominant X-ray powerlaw continuum -- is one prominent feature that is commonly seen in type 1 Seyfert AGN and therefore readily provides a useful diagnostic of the accretion flow mechanism around these systems. NGC 5940 is a Seyfert 1 AGN which reveals strong, prom…
The {\it Fermi} satellite has detected $\sim$60 radio galaxies (RGs). In this study, we investigate the difference in the properties of X-ray spectra between GeV-loud RGs and GeV-quiet RGs. Our sample comprises 68 objects: 36 RGs detected with {\it Fermi} and 32 RGs not detected with gamma rays. We analyzed the X-ray spectra of these 68 objects using data from the {\it XMM-Newton}, {\it Chandra}, {\it NuSTAR}, and {\it Swift} satellites. Our results show that most GeV-loud RGs do not exhibit significant absorption, while $\sim$50\% of the GeV-quiet RGs exhibit significant absorption. This sugg…
We present results from {\it XMM-Newton/RGS} observations of prominent knots in the southest portion of Tycho's supernova remnant, known to be the remnant of a Type Ia SN in 1572 C.E. By dispersing the photons from these knots out of the remnant with very little emission in front of or behind them, we obtained the nearly uncontaminated spectra of the knots. In the southernmost knot, the RGS successfully resolved numerous emission lines from Si, Ne, O He$α$ and Ly$α$, and Fe L-shell. This is the first clear detection of O lines in Tycho's SNR. Line broadening was measured to be $\sim 3$ eV for …
Wind-fed supergiant X-ray binaries are precious laboratories not only to study accretion under extreme gravity and magnetic field conditions, but also to probe still highly debated properties of massive star winds. These includes the so-called clumps, originated from the inherent instability of line driven winds, and larger structures. In this paper, we report on the results of the last (and not yet published) monitoring campaigns that our group has been carrying out since 2007 with both XMM-Newton and the Swift Neil Gehrels observatory. Data collected with the EPIC cameras on-board XMM-Newton…
XMM-Newton and Swift Unveil Another X-Ray Transient in NGC 4945, XMM J130514.64-493311.27
Oak Ridge Associated Universities（橡树岭联合大学）；X-ray Astrophysics Laboratory, NASA Goddard Space Flight Center（X射线天体物理实验室，NASA戈达德太空飞行中心）；Cahill Center for Astrophysics, California Institute of Technology（加州理工学院卡希尔天体物理学中心）；Southeastern Universities Research Association（东南部大学研究协会）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/GSFC空间科学与技术研究与探索中心）
研究利用 XMM-牛顿卫星和雨燕卫星在 NGC 4945 中发现 X 射线瞬变源 XMM J130514.64-493311.27，分析其特性并通过多种波段观测寻找对应体，最终提出该源是处于活跃阶段的 X 射线双星。
Compton-thick AGNs in the NuSTAR era. V: Joint NuSTAR and XMM-Newton spectral analysis of three "soft-Gamma" candidate CT-AGNs in the Swift-BAT 100-month catalog
IGR J17091-3624 is a low mass X-ray binary (LMXB) which received wide attention from the community thanks to its similarities with the bright black hole system GRS 1915+105. Both systems exhibit a wide range of highly structured X-ray variability during outburst, with time scales from few seconds to tens of minutes, which make them unique in the study of mass accretion in LMXBs. In this work we present a general overview into the long-term evolution of IGR J17091-3624, using Swift/XRT observations from the onset of the 2011-2013 outburst in February 2011 to the end of the last bright outburst …
The neutron star low-mass X-ray binary SWIFT J1749.4-2807 is the only known eclipsing accreting millisecond X-ray pulsar. In this manuscript we perform a spectral characterization of the system throughout its 2021, two-week-long outburst, analyzing 11 NICER observations and quasi-simultaneous XMM-Newton and NuSTAR single observations at the outburst peak. The broadband spectrum is well-modeled with a black body component with a temperature of $\sim$0.6 keV, most likely consistent with a hot spot on the neutron star surface, and a Comptonisation spectrum with power-law index $Γ\sim 1.9$, arisin…
Probing spectral variability in NGC 4490 ULX-8 over 24 years of XMM-Newton, Chandra and Swift-XRT observations
Indian Institute of Science Education and Research (IISER) Mohali（印度科学教育研究所）；University of Southampton（南安普顿大学）；Indian Institute of Astrophysics（印度天体物理研究所）；Inter-University Centre for Astronomy and Astrophysics（大学间天文学与天体物理学中心）；Raman Research Institute（拉曼研究所）
Context. Serendipitous X-ray surveys have proven to be an efficient way to find rare objects, for example tidal disruption events, changing-look active galactic nuclei (AGN), binary quasars, ultraluminous X-ray sources (ULXs), and intermediate mass black holes. With the advent of very large X-ray surveys, an automated classification of X-ray sources becomes increasingly valuable.Aims. This work proposes a revisited naive Bayes classification of the X-ray sources in the Swift-XRT and XMM-Newton catalogs into four classes -- AGN, stars, X-ray binaries (XRBs) and cataclysmic variables (CVs) -- ba…
