OVII and OVIII line emission in the diffuse soft X-ray background: heliospheric and galactic contributions^*

¹ UMR 7620, IPSL/Service d'Aéronomie, CNRS, Université Pierre et Marie Curie, Université Versailles-Saint-Quentin, Verrières-le-Buisson, France e-mail: dimitra.koutroumpa@aerov.jussieu.fr
² UMR 7158, DSM/DAPNIA/SAp, CEA Saclay, 91191 Gif-sur-Yvette, France
³ Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA

Received: 13 July 2007
Accepted: 10 September 2007

Abstract

Aims.We study the 0.57 keV (O VII triplet) and 0.65 keV (O VIII) diffuse emission generated by charge transfer collisions between solar wind (SW) oxygen ions and interstellar H and He neutral atoms in the inner Heliosphere. These lines which dominate the 0.3-1.0 keV energy interval are also produced by hot gas in the galactic halo (GH) and possibly the Local Interstellar Bubble (LB).

Methods.We developed a time-dependent model of the Solar Wind Charge-Exchange (SWCX) X-ray emission, based on the localization of the Solar Wind Parker spiral at each instant. We include input SW conditions affecting three selected fields, as well as shadowing targets observed with XMM-Newton, Chandra and Suzaku satellites and calculate X-ray emission in the oxygen lines O VII and O VIII in order to determine the SWCX contamination and the residual emission to attribute to the galactic soft X-ray background. We obtain ground level intensities and/or simulated lightcurves for each target and compare to X-ray data from the three instruments mentioned.

Results.The local 3/4 keV emission (due essentially to O VII and O VIII) detected in front of shadowing clouds is found to be entirely explained by the CX heliospheric emission. No emission from the LB is needed at these energies. The observed and modeled range of the foreground oxygen emission is 0.3-4.6 LU (Line Units = photons cm^-2 s^-1 sr^-1) for OVII and 0.02-2.1 LU for OVIII depending on directions and conditions.
Using the model predictions we subtract the heliospheric contribution to the measured emission and derive the halo contribution. We also correct for an error in the preliminary analysis of the Hubble Deep Field North (HDFN). We find intensities of 4.9 LU, 6.25 LU, 11.15 LU for OVII and 1.41 LU, 1.62 LU, 1.97 LU for OVIII towards the Marano Field, the Hubble Deep Field-North, and the Lockman Hole respectively.