The calibration of eROSITA on SRG

Dennerl, K.; Andritschke, Robert; Bräuninger, H.; Burkert, Wolfgang; Burwitz, V.; Emberger, Valentin; Freyberg, M. J.; Friedrich, Péter; Gaida, Roland; Granato, Stefanie; Hartner, Gisela; Kienlin, A. von; Meidinger, Norbert; Menz, Benedikt; Predehl, P.

doi:10.1117/12.2562330

Cited by 10 publications

(12 citation statements)

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“…These images are the basis for modelling the PSF. More details are presented in Dennerl et al (2020).…”

Section: Discussionmentioning

confidence: 99%

“…Comparisons between the measured values and the modelled vignetting curves are shown in Fig. 7 of Dennerl et al (2020).…”

Section: Appendix A: Esass Data Analysis Software Package Appendix B:...mentioning

confidence: 99%

“…This method was also applied to the other three valid pattern types (doubles, triples, and quadruples) by using the same generic function and modifying only some parameters. This re-sulted in four initial RMFs, one for each pattern size (Dennerl et al 2020). These are the RMFs that are currently used for all TMs.…”

Section: Appendix A: Esass Data Analysis Software Package Appendix B:...mentioning

confidence: 99%

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The eROSITA Final Equatorial Depth Survey (eFEDS)

Brunner

Liu

Lamer

et al. 2022

A&A

240

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Context. The eROSITA X-ray telescope on board the Spectrum-Poentgen-Gamma (SPG) observatory combines a large field of view and a large collecting area in the energy range between ~0.2 and ~8.0 keV. This gives the telescope the capability to perform uniform scanning observations of large sky areas. Aims. SRG/eROSITA performed scanning observations of the ~140 square degree eROSITA Final Equatorial Depth Survey field (the eFEDS field) as part of its performance verification phase ahead of the planned four year of all-sky scanning operations. The observing time of eFEDS was chosen to slightly exceed the depth expected in an equatorial field after the completion of the all-sky survey. While verifying the capability of eROSITA to perform large-area uniform surveys and saving as a test and training dataset to establish calibration and data analysis procedures, the eFEDS survey also constitutes the largest contiguous soft X-ray survey at this depth to date, supporting a range of early eROSITA survey science investigations. Here we (i) present a catalogue of detected X-ray sources in the eFEDS field providing information about source positions and extent, as well as fluxes in multiple energy bands, and (ii) document the suite of tools and procedures developed for eROSITA data processing and analysis, which were validated and optimised by the eFEDS work. Methods. The data were fed through a standard data processing pipeline, which appltes X-ray event calibration and provides a set of standard calibrated data products. A mutiti-stage source detection procedure, building in part on experience from XMM-Newton, was optimised and calibrated by performing realistic simulations of the eROSITA eFEDS observations. Source fluxes were computed in multiple standard energy bands by forced point source fitting and aperture photometry. We cross-matched the eROSITA eFEDS source catalogue with previous XMM-ATLAS observations, which confirmed the excellentt agreement of the eROSITA and XMM-ATLAS source fluxes. Astrometric corrections were performed by cross-matching the eROSITA source positions with an optical reference catalogue of quasars. Results. We present a primary catalogue of 27 910 X-ray sources (542 of which are significantly spatially extended) detected in the 0.2–2.3 keV energy range with detection likelihoods ≥6, corresponding to a (point source) flux limit of 6.5 × 10–15 erg cm–2 s–1 in the 0.5–2.0 keV energy band (80% completeness). A supplementary catalogue contains 4774 low-significance source candidates with detection likelihoods between 5 and 6. In addition, a hard-band sample of 246 sources detected in the energy range 22.3–5.0 keV above a detection likelihood of 10 is provided. In an appendix, we finally describe the dedicated data analysis software package, the eROSITA calibration database, and the standard calibrated data products.

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“…These images are the basis for modelling the PSF. More details are presented in Dennerl et al (2020).…”

Section: Discussionmentioning

confidence: 99%

“…Comparisons between the measured values and the modelled vignetting curves are shown in Fig. 7 of Dennerl et al (2020).…”

Section: Appendix A: Esass Data Analysis Software Package Appendix B:...mentioning

confidence: 99%

Section: Appendix A: Esass Data Analysis Software Package Appendix B:...mentioning

confidence: 99%

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The eROSITA Final Equatorial Depth Survey (eFEDS)

Brunner

Liu

Lamer

et al. 2022

A&A

240

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“…Further details of the calibration can be found in Ref. 13. Only TM7 showed one single bad pixel during ground calibration, whereas all other six cameras were free of any bad pixels.…”

Section: Camera Calibration On Groundmentioning

confidence: 99%

“…Analysis showed that this effect was caused by four Table 6 Energy resolution including the one sigma error of the seven eROSITA cameras in space. 13 The values were obtained from onboard calibration source measurements in November and December 2019. The operating temperature was −85°C.…”

Section: Micrometeoroid Damagementioning

confidence: 99%

eROSITA camera array on the SRG satellite

Meidinger

Andritschke

Dennerl

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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The Spectrum-Roentgen-Gamma satellite with the extended roentgen survey with an imaging telescope array (eROSITA) x-ray telescope as scientific payload was successfully launched on July 13, 2019 and deployed in a 6-month halo orbit around the second Lagrange point of the Sun-Earth system. The telescope comprises an array of seven mirror systems with seven focal plane cameras. The spectroscopic CCD cameras are a further development of the very successful EPIC-PN camera on the XMM-Newton satellite, which is still operating after more than 20 years in space. The key component of the camera is the detector, which matches the large field of view of 1 deg to permit an all-sky survey in the energy range from 0.2 to 8 keV with state-of-the-art energy resolution. The image area of the PN-junction charge coupled device comprises 384 × 384 pixels. The pixel size of 75 × 75 μm 2 each matches the angular resolution of the mirror system. Readout of the full frame is achieved in 9.18 ms but for thermal and onboard event preprocessing reasons, the time resolution is slowed down to 50 ms. The photon entrance window of five of the seven CCDs is equipped with an optical blocking filter, which proved to be advantageous. The improved concept and design of the eROSITA cameras will be explained as well as their operation and performance in space.

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