The Reflection Grating Spectrometer on board XMM-Newton

Herder, J. W. den; Brinkman, A. C.; Kahn, S. M.; Branduardi‐Raymont, G.; Thomsen, K.; Aarts, H.; Audard, M.; Bixler, J.; Boggende, A. J. den; Cottam, J.; Decker, Todd A.; Dubbeldam, L.; Erd, C.; Goulooze, H.; Güdel, M.; Guttridge, P.; Hailey, Charles J.; Janabi, K. Al; Kaastra, J. S.; Korte, P. A. J. de; Leeuwen, B. J. van; Mauche, C. W.; McCalden, A. J.; Mewe, R.; Naber, A.; Paerels, F. B. S.; Peterson, J. R.; Rasmussen, A. P.; Rees, K.; Sakelliou, I.; Šako, M.; Spodek, Joshua; Stern, Marcela; Tamura, Takayuki; Tandy, J. A.; Vries, C. P. de; Welch, S; Zehnder, A.

doi:10.1051/0004-6361:20000058

Cited by 833 publications

(240 citation statements)

References 12 publications

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“…The Chandra observatory provides two different grating instruments; the Low-Energy Transmission Grating (LETG, 0.1-10 keV; Brinkman et al 2000) and the High-Energy Transmission Grating (HETG, 0.4-10 keV; Marshall et al 2004). The XMM-Newton satellite carries two Reflection Grating Spectrometers (RGS1 and RGS2, 0.35-2.5 keV; den Herder et al 2001). …”

Section: X-ray Missions Used Most For X-ray Burst/accretion Flow Intementioning

confidence: 99%

Accretion Disks and Coronae in the X-Ray Flashlight

et al. 2017

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Plasma accreted onto the surface of a neutron star can ignite due to unstable thermonuclear burning and produce a bright flash of X-ray emission called a Type-I X-ray burst. Such events are very common; thousands have been observed to date from over a hundred accreting neutron stars. The intense, often Eddington-limited, radiation generated in these thermonuclear explosions can have a discernible effect on the surrounding accretion flow that consists of an accretion disk and a hot electron corona. Type-I X-ray bursts can there- fore serve as direct, repeating probes of the internal dynamics of the accretion process. In this work we review and interpret the observational evidence for the impact that Type-I X-ray bursts have on accretion disks and coronae. We also provide an outlook of how to make further progress in this research field with prospective experiments and analysis techniques, and by exploiting the technical capabilities of the new and concept X-ray missions ASTROSAT, NICER, Insight-HXMT, eXTP, and STROBE-X.

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Section: X-ray Missions Used Most For X-ray Burst/accretion Flow Intementioning

confidence: 99%

Accretion Disks and Coronae in the X-Ray Flashlight

et al. 2017

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“…Two of the telescopes have Multi-Object Spectrometer (MOS) CCDs (Turner et al 2001) and the last one uses pn CCDs (Strüder et al 2001) for data recording. There are two Reflection Grating Spectrometers (RGS) (den Herder et al 2001). The Optical Monitor (OM), a photon counting instrument, is a coaligned 30-cm optical/UV telescope, providing for the first time the possibility to observe simultaneously in the X-ray and optical/UV regime from a single platform (Mason et al 2001).…”

Section: Observations and Analysismentioning

confidence: 99%

XMM-NEWTONOBSERVATIONS OF THE DWARF NOVA RU Peg IN QUIESCENCE: PROBE OF THE BOUNDARY LAYER

Balman

Godon

Sion

et al. 2011

ApJ

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We present an analysis of X-ray and UV data obtained with the XMM-Newton Observatory of the long period dwarf nova RU Peg. RU Peg contains a massive white dwarf, possibly the hottest white dwarf in a dwarf nova, it has a low inclination, thus optimally exposing its X-ray emitting boundary layer, and has an excellent trigonometric parallax distance.We modeled the X-ray data using XSPEC assuming a multi-temperature plasma emission model built from the MEKAL code (i.e., CEVMKL). We obtained a maximum temperature of 31.7 keV, based on the EPIC MOS1, 2 and pn data, indicating that RU Peg has an X-ray spectrum harder than most dwarf novae, except U Gem. This result is consistent with and indirectly confirms the large mass of the white dwarf in RU Peg. The X-ray luminosity we computed corresponds to a boundary layer luminosity for a mass accretion rate of 2 × 10 −11 M ⊙ /yr (assuming M wd = 1.3M ⊙ ), in agreement with the expected quiescent accretion rate. The modeling of the O viii emission line at 19Å as observed by the RGS implies a projected stellar rotational velocity v rot sin i =695 km s −1 , i.e. the line is emitted from material rotating at ∼936-1245 km s −1 (i ∼ 34 • − 48 • ) or about 1/6 of the Keplerian speed; this velocity is much larger than the rotation speed of the white dwarf inferred from the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum. Cross-correletion analysis yielded an undelayed (time lag ∼ 0) component and a delayed component of 116±17 sec where the X-ray variations/fluctuations lagged the UV variations. This indicates that the UV fluctuations in the inner disk are propagated into the X-ray emitting region in about 116 sec. The undelayed component may be related to irradiation effects.

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“…MCG À6-30-15 was observed during the Guaranteed Time Observations phase on 2000 July 10-11. The instrument modes for the Reflection Grating Spectrometer (RGS; den Herder et al 2001), the European Photon Imaging Cameras (EPIC) MOS (Turner et al 2001a) and PN (Strü der et al 2001), and the Optical Monitor (OM; Mason et al 2001), as well as the associated exposure times for both observations, are summarized in Table 1.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Can a Dusty Warm Absorber Model Reproduce the Soft X‐Ray Spectra of MCG −6‐30‐15 and Markarian 766?

Šako¹,

Kahn²,

Branduardi‐Raymont³

et al. 2003

ApJ

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XMM-Newton RGS spectra of MCG À6-30-15 and Mrk 766 exhibit complex discrete structure, which was interpreted in a paper by Branduardi-Raymont and coworkers as evidence for the existence of relativistically broadened Ly emission from carbon, nitrogen, and oxygen, produced in the innermost regions of an accretion disk around a Kerr black hole. This suggestion was subsequently criticized in a paper by Lee and coworkers, who argued that for MCG À6-30-15, the Chandra HETG spectrum, which is partially overlapping the RGS in spectral coverage, is adequately fitted by a dusty warm absorber model, with no relativistic line emission. We present a reanalysis of the original RGS data sets in terms of the model by Lee and coworkers. Specifically, we show that (1) the explicit model given by Lee and coworkers differs markedly from the RGS data, especially at longer wavelengths, beyond the region sampled by the HETG; (2) generalizations of the Lee and coworkers model, with all parameters left free, do provide qualitatively better fits to the RGS data, but are still incompatible with the detailed spectral structure; (3) the ionized oxygen absorption-line equivalent widths are well measured with the RGS for both sources, and place very tight constraints on both the column densities and turbulent velocity widths of O vii and O viii. The derived column densities are well below those posited by Lee and coworkers and are insufficient to play any role in explaining the observed edge-like feature near 17.5 Å ; (4) the lack of a significant neutral oxygen edge near 23 Å places very strong limits on any possible contribution of absorption to the observed structure by dust embedded in a warm medium; and (5) the original relativistic line model with warm absorption proposed by BranduardiRaymont and coworkers provides a superior fit to the RGS data, both in the overall shape of the spectrum and in the discrete absorption lines. We also discuss a possible theoretical interpretation for the putative relativistic Ly line emission in terms of the photoionized surface layers of the inner regions of an accretion disk. While there are still a number of outstanding theoretical questions about the viability of such a model, it is interesting to note that simple estimates of key parameters are roughly compatible with those derived from the observed spectra.

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The Reflection Grating Spectrometer on board XMM-Newton

Cited by 833 publications

References 12 publications

Accretion Disks and Coronae in the X-Ray Flashlight

Accretion Disks and Coronae in the X-Ray Flashlight

XMM-NEWTONOBSERVATIONS OF THE DWARF NOVA RU Peg IN QUIESCENCE: PROBE OF THE BOUNDARY LAYER

Can a Dusty Warm Absorber Model Reproduce the Soft X‐Ray Spectra of MCG −6‐30‐15 and Markarian 766?

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