Effective area calibration of the reflection grating spectrometers of XMM-Newton - II. X-ray spectroscopy of DA white dwarfs

@article{Kaastra2009EffectiveAC,
  title={Effective area calibration of the reflection grating spectrometers of XMM-Newton - II. X-ray spectroscopy of DA white dwarfs},
  author={Jelle S. Kaastra and Thierry M. Lanz and I. Hubeny and Frits B. S. Paerels},
  journal={Astronomy and Astrophysics},
  year={2009},
  volume={497},
  pages={311-323}
}
Context. White dwarf spectra have been widely used as a calibration source for X-ray and EUV instruments. The in-flight effective area calibration of the reflection grating spectrometers (RGS) of XMM-Newton depend upon the availability of reliable calibration sources. Aims. We investigate how well these white dwarf spectra can be used as standard candles at the lowest X-ray energies in order to gauge the absolute effective area scale of X-ray instruments. Methods. We calculate a grid of model… 
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References

SHOWING 1-10 OF 42 REFERENCES
Effective area calibration of the Reflection Grating Spectrometers of XMM-Newton. I. X-ray spectroscopy of the Crab nebula
The Crab nebula and pulsar have been widely used as a calibration source for X-ray instruments. The in-flight effective area calibration of the Reflection Grating Spectrometers (RGS) of XMM-Newton
In-flight effective area calibration of the Chandra low-energy transmission grating spectrometer
We present the in-flight effective area calibration of the Low Energy Transmission Grating Spectrometer (LETGS), which comprises the High Resolution Camera Spectroscopic readout (HRC-S) and the Low
Low-energy effective area of the Chandra low-energy transmission grating spectrometer
The Chandra X-ray Observatory was successfully launched on July 23, 1999, and subsequently began an intensive calibration phase. We present preliminary results from in- flight calibration of the low
Establishing HZ43 A, Sirius B, and RX J185635-3754 as soft X-ray standards: a cross-calibration between the Chandra LETG+HRC-S, the EUVE spectrometer, and the ROSAT PSPC
Context. The absolute calibration of space-borne instruments in the soft X-ray regime rests strongly on model spectra of hot white dwarfs. Aims. We analyze the Chandra LETG+HRC observations of the
On the relevance of Compton scattering for the soft X-ray spectra of hot DA white dwarfs
Aims. We re-examine the effects of Compton scattering on the emergent spectra of hot DA white dwarfs in the soft X-ray range. Earlier studies have implied that sensitive X-ray observations at
X-ray spectroscopy of NGC 5548
We analyze the high-resolution X-ray spectrum of the Seyfert 1 galaxy NGC 5548, for the full 0:1{10 keV band, using improved calibration results of the Chandra-LETGS instrument. The warm absorber
The Extreme Ultraviolet Explorer Stellar Spectral Atlas
We present an atlas of extreme ultraviolet (EUV) spectra of 95 bright stellar sources observed between 1992 July and 1996 June with the Extreme Ultraviolet Explorer (EUVE) spectrometers. These data
Comparison of White Dwarf Models with STIS Spectrophotometry
Computed flux distributions for four white dwarf (WD) stars with nearly pure hydrogen atmospheres are tied to the Vega flux scale with V-band Landolt photometry. With broadband photometric precision
Calibration of Synthetic Photometry Using DA White Dwarfs
We have calibrated four major ground-based photometric systems with respect to the Hubble Space Telescope (HST) absolute flux scale, which is defined by Vega and four fundamental DA white dwarfs.
Hubble Space Telescope spectroscopy of the Balmer lines in Sirius B
Sirius B is the nearest and brightest of all white dwarfs, but it is very difficult to observe at visible wavelengths due to the overwhelming scattered light contribution from Sirius A. However, from
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