We present Chandra HETGS spectroscopy of the Be/X-ray binary 1A 0535+262 obtained during the 2009/2010 giant outburst. These are the first CCD grating spectra of this type of system during a giant outburst. Our spectra reveal a number of lines including a narrow Fe K_alpha emission line with a FWHM of ~ 5000 km s^-1. For the first time, we detect the presence of a highly ionized outflow in a Be/X-ray binary. Assuming that the line is He-like Fe XXV, fits with a simple Gaussian imply an outflow velocity of ~ 1500 km s^-1. However, self-consistent photoionization modeling with XSTAR suggests that Fe XXIII-XXIV must also contribute. In this case, an outflow velocity of ~ 3000 km s^-1 is implied. These results are discussed in the context of the accretion flow in Be-star, neutron star, and black hole X-ray binaries.
We present a study of the narrow Fe K$α$ line in seven bright, nearby AGN that have been observed extensively with the Chandra High Energy Transmission Grating (HETG). The HETG data reveal a wider Fe K$α$ line in the first order spectrum than in the second and third order spectra, which we interpret as the result of spatially extended Fe K$α$ emission. We utilize these differences in narrow Fe K$α$ line widths in the multi-order Chandra HETG spectra to determine the spatial extent and intrinsic velocity width of the emitting material in each object. We find that there is modest evidence for sp…
We present a uniform analysis of six examples of embedded wind shock (EWS) O star X-ray sources observed at high resolution with the Chandra grating spectrometers. By modeling both the hot plasma emission and the continuum absorption of the soft X-rays by the cool, partially ionized bulk of the wind we derive the temperature distribution of the shock-heated plasma and the wind mass-loss rate of each star. We find a similar temperature distribution for each star's hot wind plasma, consistent with a power-law differential emission measure, $\frac{d\log EM}{d\log T}$, with a slope a little steepe…
Analysis of the 3C445 Soft X-ray Spectrum as Observed by Chandra high-energy gratings
我们提出了一个详细的分析软X射线发射的3C 445使用档案钱德拉HETG光谱。高电离的H-和He-类Mg，Si和S线，以及一个解决的低电离Si K $α$线，在高分辨率光谱检测。类氦三重态的Mg和Si被分解成单独的线，并且计算出的R比表明发射极的高密度。低的G值表明谱线来自碰撞电离等离子体。然而，在光谱中的一个解决窄Ne X RRC功能的检测似乎更喜欢一个光电离环境。光谱随后建模与光电离模型，并与碰撞模型的结果进行了比较。通过对光谱的详细分析，我们排除了这些发射线的碰撞起源。一个单组分光电离模型提供了一个很好的适合的发射功能。最佳拟合参数为log $ξ$ = $3.3^{+0.4}_{-0.3}$ erg cm s $^{-1}$、$n_{H}$ = $5^{+15}_{-4.5}\times10^{10}$ cm $^{-3}$和$N_{H}$ = $2.5^{+3.8}_{-1.7}\times10^{20}$ cm $^{-2}$。根据计算的发射体高密度、测量的发射谱线速度宽度和推断的径向距离（6 $\times$ $10^{14}$ - 8 $\times$ $10^{15}$ cm），我们认为发射谱线来自物质，位于宽线区（BLR）。
Axion-Like Particles (ALPs) are predicted by several Beyond the Standard Model theories, in particular, string theory. In the presence of an external magnetic field perpendicular to the direction of propagation, ALPs can couple to photons. Therefore, if an X-ray source is viewed through a magnetised plasma, such as a luminous quasar in a galaxy cluster, we may expect spectral distortions that are well described by photon-ALP oscillations. We present a $571 \ \mathrm{ks}$ combined High and Low Energy Transmission Grating (HETG/LETG) Chandra observation of the powerful radio-quiet quasar H1821+6…
We observed the Galactic black hole X-ray binary V4641 Sgr with the high resolution transmission gratings on Chandra during the source's 2020 outburst. Over two epochs of Chandra gratings observations, we see numerous highly ionized metal lines, superimposed on a hot, disc-dominated X-ray continuum. The measured inner disc temperatures and luminosities imply an unfeasibly small inner disc radius, such that we suggest that the central engine of V4641 Sgr is obscured, and we are viewing scattered X-rays. We find that the emission lines in the Chandra spectra cannot be constrained by a single pho…
The Cores of the Fe K$α$ Lines in Active Galactic Nuclei: an Extended Chandra High Energy Grating Sample
利用钱德拉高能光栅（HEG）观测到的较大样本，对Yaqoob & Padmanabhan（2004）报道的Seyfert星系中\sim 6.4 keV的Fe K $α$发射线核心的研究进行了扩展。虽然严重模糊的活动星系核（AGN）被排除在样本之外，这些数据提供了一些最高精度的测量的峰值能量的Fe K $α$线，和最高的光谱分辨率测量的核心的宽度的线在unobscured和适度模糊（$N_{H}<10^{23} \ \rm cm^{-2}$）塞弗特星系的日期。在33个源中检测到Fe K $α$线，并在32个源中约束其质心能量。在27个数据源中，数据的统计质量足以产生FWHM的测量值。我们发现，线质心能量的分布在中性Fe的值附近有很强的峰值，超过80%的观测值在6.38- 6.43keV范围内。包括统计误差，32个源中的30个（$\sim 94%$）具有在6.35- 6.47 keV范围内的线质心能量。在可以测量非零下限的观测值中，平均等效宽度为$53 \pm 3eV. The mean FWHM from the subsample of 27 sources was $ 2060 \pm 230 \ \rm km \ s^{-1} $. The mean EW and FWHM are somewhat higher when multiple observations for a…
Axions/axion-like particles (ALPs) are a well motivated extension of the Standard Model and are generic within String Theory. The X-ray transparency of the intracluster medium (ICM) in galaxy clusters is a powerful probe of light ALPs (with mass $<10^{-11}\,{\rm eV}$); as X-ray photons from an embedded or background source propagate through the magnetized ICM, they may undergo energy-dependent quantum mechanical conversion into ALPs (and vice versa), imprinting distortions on the X-ray spectrum. We present Chandra data for the active galactic nucleus NGC1275 at the center of the Perseus cluste…
CHEERS Results from NGC 3393, III: Chandra X-ray Spectroscopy of the Narrow Line Region
我们提出了空间分辨钱德拉窄带成像和成像光谱的NGC 3393。这个星系拥有一个康普顿厚度的塞弗特2活动星系核，其亚千秒差距的双极外流与环核气体强烈相互作用。我们确定了窄带过量发射与Ne IX 0.905千电子伏的过渡（可能的贡献，由于中间态铁排放），指向强烈的冲击驱动的活动星系核反馈。成像光谱解析流出ISM相互作用网站和周围的ISM在~100 pc的规模，并建议存在一个热AGN风以上的平面在半径超过冲击网站。交叉锥显示的证据，已通过在环面的间隙，并为碰撞激发的等离子体可能是由冲击约束的赤道流出的光电离的再加工。亚角秒分辨率的深X射线观测（例如Lynx可以非常有效地执行，这也将有力地解决复杂的线发射）是必要的，以消除模型退化和减少局部反馈特性的不确定性。
RT Cru belongs to the rare class of hard X-ray emitting symbiotics, whose origin is not yet fully understood. In this work, we have conducted a detailed spectroscopic analysis of X-ray emission from RT Cru based on observations taken by the Chandra Observatory using the Low Energy Transmission Grating (LETG) on the High-Resolution Camera Spectrometer (HRC-S) in 2015 and the High Energy Transmission Grating (HETG) on the Advanced CCD Imaging Spectrometer S-array (ACIS-S) in 2005. Our thermal plasma modeling of the time-averaged HRC-S/LETG spectrum suggests a mean temperature of $kT \sim 1.3$ ke…
High-resolution X-ray spectroscopy of the low and high states of the Seyfert 1 galaxy NGC 4051 with Chandra LETGS
方法.本文分析了Chandra低能透射光栅光谱仪的两个观测结果。我们研究了光谱响应突然通量减少的一个因素，这发生在第二次观察。结果我们检测到一个高度电离的吸收组件的流出速度为-4670公里/秒，在塞弗特1星系中观察到的最高流出速度的组件之一。该光谱包含一个相对论O VIII Ly α线，和四个吸收组件跨越范围的电离参数XI在0.07和3.19之间。在低态出现了产生CVI和CV辐射复合连续谱的发射分量。黑体温度随着第二次观测中观测到的通量的下降而下降。结论.对于所有的吸收器组件，我们排除了电离参数线性响应通量的减少了5倍。吸收体的可变性表明，四个检测到的组分中至少有三个位于0.02-1 pc的范围内。删节
