&lt;title&gt;Preliminary test results on spectral resolution of the Low Energy Transmission Grating Spectrometer on board of AXAF&lt;/title&gt;

Brinkman, A. C.; Gunsing, C. J. T.; Kaastra, J. S.; Braeuninger, Heinrich W.; Hartner, Gisela; Predehl, P.; Drake, J. J.; Juda, Jiahong Zhang; Juda, M.; Dewey, Daniel; Flanagan, Kathryn A.; Marshall, Herman L.

doi:10.1117/12.278846

Cited by 20 publications

(3 citation statements)

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“…The XMM‐Newton and Chandra X‐ray satellites are provided with spectrometers that have a high ( E /Δ E ∼ 100 − 1,000) energy spectral resolution and are, therefore, able to resolve spectral features narrower than 1,000 km s − 1 (Brinkman et al ; Canizares et al ; den Herder et al ). Despite their high resolving power, the gratings are often ignored because they have a much lower effective area than the CCD spectrometers, provide only 1D spectroscopy (along their cross‐dispersion direction), and require a careful data reduction, particularly for extended and/or multiple sources in the field of view.…”

Section: Soft X‐ray Spectral Features Of Ulxsmentioning

confidence: 99%

Ultrafast outflows in ultraluminous X‐ray sources

Pinto¹,

Fabian²,

Middleton

et al. 2017

Astron Nachr

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Ultraluminous X-ray sources (ULXs) are bright extragalactic sources with X-ray luminosities above 10 39 erg/s powered by accretion onto compact objects. According to the first studies performed with XMM-Newton ULXs seemed to be excellent candidates to host intermediate-mass black holes (10 2−4 M⊙). However, in the last years the interpretation of super-Eddington accretion onto stellar-mass black holes or neutron stars for most ULXs has gained a strong consensus. One critical missing piece to confirm the super-Eddington scenario was the direct detection of the massive, radiativelydriven winds expected as atomic emission/absorption lines in ULX spectra. The first evidence for winds was found as residuals in the soft X-ray spectra of ULXs. Most recently we have been able to resolve these residuals into rest-frame emission and blueshifted (∼ 0.2c) absorption lines arising from highly ionized gas in the deep high-resolution XMMNewton spectra of two ultraluminous X-ray sources. The compact object is therefore surrounded by powerful ultrafast winds as predicted by models of hyper-Eddington accretion. Here we discuss the relevance of these discoveries and the importance of further, deep, XMM-Newton observations of powerful winds in many other ultraluminous X-ray sources to estimate the energetics of the wind, the geometry of the system, and the masses of the central accretors.

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Section: Soft X‐ray Spectral Features Of Ulxsmentioning

confidence: 99%

Ultrafast outflows in ultraluminous X‐ray sources

Pinto¹,

Fabian²,

Middleton

et al. 2017

Astron Nachr

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“…In addition to the Calibration Reports, some of the results appear in these 11,12,13,14,15,16,17,18,19,20,5 and previous 21,22,23,24,25,26,27,28,29,30,31,32,33,34,35,9,10 proceedings.…”

Section: Science Calibration Web Pages (See A)mentioning

confidence: 92%

The Chandra X-Ray Observatory (CXO)

Weisskopf¹

2001

The Neutron Star—Black Hole Connection

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The Chandra X-Ray Observatory (CXO), the x-ray component of NASA's Great Observatories, was launched early in the morning of 1999, July 23 by the Space Shuttle Columbia. The Shuttle launch was only the first step in placing the observatory in orbit. After release from the cargo bay, the Inertial Upper Stage performed two firings, and separated from the observatory as planned. Finally, after five firings of Chandra's own Integral Propulsion System -the last of which took place 15 days after launch -the observatory was placed in its highly elliptical orbit of ∼140,000 km apogee and ∼10,000 km perigee. After activation, the first x-rays focussed by the telescope were observed on 1999, August 12. Beginning with these initial observations one could see that the telescope had survived the launch environment and was operating as expected. The month following the opening of the sunshade door was spent adjusting the focus for each set of instrument configurations, determining the optical axis, calibrating the star camera, establishing the relative response functions, determining energy scales, and taking a series of "publicity" images. Each observation proved to be far more revealing than was expected. Finally, and despite an initial surprise and setback due to the discovery that the Chandra x-ray telescope was far more efficient for concentrating low-energy protons than had been anticipated, the observatory is performing well and is returning superb scientific data. Together with other space observatories, most notably the recently activated XMM-Newton, it is clear that we are entering a new era of discovery in high-energy astrophysics.

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“…The relevant instruments are the Chandra High-Energy Transmission Grating Spectrometer (HETGS; C.R. Canizares et al, in preparation), the Chandra Low-Energy Transmission Grating Spectrometer (LETGS;Brinkman et al 1997), and the XMM-Newton Reflection Grating Spectrometer (RGS; denHerder et al 2001). …”

mentioning

confidence: 99%

Grating X-ray Spectroscopy of High-Velocity Outflows from Active Galaxies

Brandt

Kaspi²

2002

AIP Conference Proceedings

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X-ray absorption and emission lines now serve as powerful diagnostics of the outflows from active galaxies. Detailed X-ray line studies of outflows have recently been enabled for a significant number of active galaxies via the grating spectrometers on Chandra and XMM-Newton. We will review some of the recent X-ray findings on active galaxy outflows from an observational perspective. We also describe some future prospects.X-ray absorption lines from H-like and He-like ions of C, N, O, Ne, Mg, Al, Si, and S are often seen. A wide range of ionization parameter appears to be present in the absorbing material, and inner-shell absorption lines from lower ionization ions, Fe L-shell lines, and Fe M-shell lines have also been seen. The X-ray absorption lines are typically blueshifted relative to the systemic velocity by a few hundred km s −1 , and they often appear kinematically consistent with UV absorption lines of C IV, N V, and H I. The X-ray absorption lines can have complex profiles with multiple kinematic components present as well as filling of the absorption lines by emission-line photons. A key remaining uncertainty is the characteristic radial location of the outflowing gas; only after this quantity is determined will it be possible to calculate reliably the amount of outflowing gas and the kinetic luminosity of the outflow.

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<title>Preliminary test results on spectral resolution of the Low Energy Transmission Grating Spectrometer on board of AXAF</title>

Cited by 20 publications

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Ultrafast outflows in ultraluminous X‐ray sources

Ultrafast outflows in ultraluminous X‐ray sources

The Chandra X-Ray Observatory (CXO)

Grating X-ray Spectroscopy of High-Velocity Outflows from Active Galaxies

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