&lt;title&gt;Imaging performance of the XMM-Newton x-ray telescopes&lt;/title&gt;

Aschenbach, B.; Briel, U. G.; Haberl, F.; Braeuninger, Heinrich W.; Burkert, Wolfgang; Oppitz, Andreas; Gondoin, P.; Lumb, D.

doi:10.1117/12.391615

Cited by 73 publications

(41 citation statements)

References 7 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…based on MOS (EPIC-MOS1 and -MOS2, Turner et al 2001) and PN CCD X-ray detectors (EPIC-PN, Strüder et al 2001) which are mounted behind the three telescopes (Aschenbach et al 2000). The background in the EPIC detectors was low during the whole observation with the exception of a short interval of ∼400 s when it increased from 1-2 cts s −1 to about 10 cts s −1 per PN CCD.…”

Section: Xmm-newton Broad Band X-ray Observationsmentioning

confidence: 99%

X-ray and optical observations of : A new intermediate polar with soft X-ray emission

Haberl

Motch

Zickgraf

2002

A&A

View full text Add to dashboard Cite

Abstract.We report the identification of the ROSAT all-sky survey source 1RXS J154814.5-452845 as new intermediate polar and present the results from follow-up optical and X-ray observations. The source shows pulsations with a period of 693 s both in the optical and X-ray light curves and the detection of a synodic frequency strongly suggests that this is the rotation period of the white dwarf. Although the one day aliasing and the sparse optical data coverage does not allow to unambiguously identify the orbital period, the most likely values of 9.37 h and 6.72 h add 1RXS J154814.5-452845 to the intermediate polars with the longest orbital periods known. The optical spectrum displays features from the late type secondary and shows the presence of broad absorption lines at Hβ and higher order Balmer lines which may be a signature of the white dwarf atmosphere, very similar to V 709 Cas (RX J0028.8+5917 Bonnet-Bidaud et al. 2001). The average X-ray spectra as obtained by the EPIC instruments on board XMM-Newton show hard emission typical for this class of objects but also the presence of soft blackbody-like emission similar to that seen from soft intermediate polars and thought to arise from the white dwarf surface heated by the hard X-rays. The best fit model comprises thermal emission from multi-temperature plasma in collisional ionization equilibrium with a continuous temperature distribution up to a maximum of ∼60 keV, an Fe fluorescence line at 6.4 keV and with equivalent width of 260 eV and a blackbody component with kT of 86 eV. The hard X-ray emission is absorbed by matter covering 47% of the X-ray source with an equivalent hydrogen density of ∼10 23 cm −2 . The remaining hard emission is absorbed by a much reduced column density of 1.5 × 10 21 cm −2 as is the soft blackbody emission. Pulse-phase spectroscopy around spin maximum and minimum reveals that the flux variations are mainly caused by a change in the temperature distribution with higher intensity (a factor of ∼3 in the 1 keV emission) seen from the lower temperature plasma during spin maximum. The absorption in the high column density matter only decreases marginally during spin maximum. The emission characteristics are consistent with the accretion curtain scenario and features in the X-ray pulse profiles indicate that we observe one pole of the white dwarf and our line of sight is nearly parallel to the curtain at spin minimum while at maximum we have a more direct view to the cooling post shock accretion flow.

show abstract

Section: Xmm-newton Broad Band X-ray Observationsmentioning

confidence: 99%

X-ray and optical observations of : A new intermediate polar with soft X-ray emission

Haberl

Motch

Zickgraf

2002

A&A

View full text Add to dashboard Cite

show abstract

“…Here we report on the analysis of the data collected with the European Photon Imaging Cameras (EPICs) based on MOS (EPIC-MOS1 and -MOS2, Turner et al 2001) and pn (EPIC-pn, Strüder et al 2001) CCD detectors which are mounted behind the three X-ray telescopes (Aschenbach et al 2000). All cameras were operated in the Full-Frame mode (FF) providing data over a field of view of ∼13 radius.…”

Section: The Xmm-newton Observationmentioning

confidence: 99%

XMM-Newton observations of the isolated neutron star RX J0806.4-4123

Haberl

Zavlin

2002

A&A

View full text Add to dashboard Cite

Abstract. The isolated neutron star RX J0806.4-4123 was observed with XMM-Newton in November 2000. The data from the three EPIC instruments allowed us (i) to derive an improved X-ray position to an accuracy of 2-3 , (ii) to accumulate the first medium-resolution soft X-ray spectra of high statistical quality and (iii) to find a candidate for the neutron star rotation period. Although this period of 11.3714 s is formally detected at a 3.5σ level in the EPIC-pn data, the similar pulse profiles deduced from all three EPIC instruments increase the confidence that the period is real. The pulsed fraction of ∼6% would then be the weakest X-ray flux modulation detected from dim isolated neutron stars. We fitted the X-ray spectra with blackbody and neutron star atmosphere models and discuss the results with respect to the brightness limit placed by optical images. The reduced size of the error circle on the X-ray position should allow deeper searches for an optical counterpart.

show abstract

“…XMM-Newton has three nested Wolter I-type X-ray telescopes (Aschenbach et al 2000) with the European Photon Imaging Camera (EPIC) CCD detectors (pn, MOS1 and MOS2) in their focal planes (Strüder et al 2001;Turner et al 2001). They achieve a spatial resolution of 17″ half energy width and an energy resolution of 13 150eV at 6.4 keV.…”

Section: Observationsmentioning

confidence: 99%

ETA CARINAE’S THERMAL X-RAY TAIL MEASURED WITH XMM-NEWTON AND NuSTAR

Hamaguchi

Corcoran

Gull

et al. 2016

ApJ

View full text Add to dashboard Cite

The evolved, massive highly eccentric binary system, ηCar, underwent a periastron passage in the summer of 2014. We obtained two coordinated X-ray observations with XMM-Newton and NuSTAR during the elevated X-ray flux state and just before the X-ray minimum flux state around this passage. These NuSTAR observations clearly detected X-ray emission associated with ηCar extending up to ∼50 keV for the first time. The NuSTAR spectrum above 10 keV can be fit with the bremsstrahlung tail from a kT∼6 keV plasma. This temperature is ΔkT∼2 keV higher than those measured from the iron K emission line complex, if the shocked gas is in collisional ionization equilibrium. This result may suggest that the companion starʼs pre-shock wind velocity is underestimated. The NuSTAR observation near the X-ray minimum state showed a gradual decline in the X-ray emission by 40% at energies above 5 keV in a day, the largest rate of change of the X-ray flux yet observed in individual ηCar observations. The column density to the hardest emission component, N H ∼10 24 H cm −2 , marked one of the highest values ever observed for η Car, strongly suggesting increased obscuration of the wind-wind colliding X-ray emission by the thick primary stellar wind prior to superior conjunction. Neither observation detected the power-law component in the extremely hard band that INTEGRAL and Suzaku observed prior to 2011. If the nondetection by NuSTAR is caused by absorption, the power-law source must be small and located very near the windwind collision apex. Alternatively, it may be that the power-law source is not related to either ηCar or the GeV γ-ray source.

show abstract

<title>Imaging performance of the XMM-Newton x-ray telescopes</title>

Cited by 73 publications

References 7 publications

X-ray and optical observations of : A new intermediate polar with soft X-ray emission

X-ray and optical observations of : A new intermediate polar with soft X-ray emission

XMM-Newton observations of the isolated neutron star RX J0806.4-4123

ETA CARINAE’S THERMAL X-RAY TAIL MEASURED WITH XMM-NEWTON AND NuSTAR

Contact Info

Product

Resources

About