This article has an erratum: [https://doi.org/10.1051/0004-6361:20065478e]
Volume 458, Number 2, November I 2006
|Page(s)||541 - 552|
|Section||Stellar structure and evolution|
|Published online||12 September 2006|
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
Institut für Astrophysik, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany e-mail: firstname.lastname@example.org
2 MPI für Extraterrestrische Physik, 85748 Garching, Germany e-mail: email@example.com
3 Institut für Astronomie und Astrophysik, Sand 1, 72076 Tübingen, Germany e-mail: firstname.lastname@example.org
Accepted: 29 June 2006
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 white dwarfs HZ43 A and Sirius B and of the neutron star RX J185635-3754 with the aim of resolving current uncertainties in the soft X-ray spectral fluxes and photospheric parameters of the three stars. We apply the derived photon spectra to a cross-calibration of the LETG+HRC-S with the short-wavelength EUVE spectrometer and the ROSAT PSPC.
Methods.We tie HZ43 A to the flux of RX J1856 in the 44-48 Å range and perform a simultaneous least squares fit to the LETG+HRC spectra of the three stars. This allows us to determine an internally consistent set of spectral energy distributions and an empirically derived wavelength-dependent correction to the LETG+HRC-S effective area. We employ NLTE model atmospheres calculated with TMAP for the white dwarfs and a two-blackbody model for RX J1856, tied to the respective optical fluxes.
Results.The two-blackbody model for RX J1856 features a hot spot on a cooler star and yields eV and eV with a stellar angular radius as seen from infinity of km pc-1. For HZ43 A, our fit yields Teff = K and (cgs) with anti-correlated errors (1-σ) which include not only the statistical but also the systematic uncertainties of the fit. HZ43AB displays a previously detected bremsstrahlung component with a temperature keV. For Sirius B, we find Teff = K for fixed . The calibration of the short-wavelength EUVE spectrometer differs from that of the LETG+HRC-S by %. The ROSAT PSPC is found to be correctly calibrated within a few percent and reports of a major miscalibration are unfounded.
Conclusions.We have obtained improved parameters for RX J185635-3754, HZ43 A, and Sirius B which fit the observations from the optical to the soft X-ray regime. Our approach allows us to quote their absolute spectral fluxes at selected wavelengths which may aid the calibration of other space-borne instruments.
Key words: methods: data analysis / white dwarfs / stars: neutron / stars: fundamental parameters
© ESO, 2006
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