English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

With a high spatial resolution imaging instrument such as the  Chandra/ACIS, one can confidently identify an X-ray source with only a fewdetected counts. The detection threshold of such sources, however, variesstrongly across the field-of-view of the instrument. Furthermore, the lowdetection counting statistics, together with a typical steep source number-fluxrelation, causes more intrinsically faint sources to be detected at apparentlyhigher fluxes than the other way around. We quantify this ``X-ray Eddingtonbias'' as well as the detection threshold variation and devise simpleprocedures for their corrections. To illustrate our technique, we presentresults from our analysis of X-ray sources detected in the fields of thelarge-scale hierarchical complex Abell 2125 at $z = 0.247$ and the nearbygalaxy NGC 4594 (Sombrero). We show that the sources detected in the Abell 2125field, excluding 10 known complex members, have a number-flux relationconsistent with the expected from foreground or background objects. Incontrast, the number-flux relation of the NGC 4594 field is dominated by X-raysources associated with the galaxy. This galactic component of the relation iswell characterized by a broken power law.Comment: 19 pages. Accepted for publication in Ap

Correction for the Flux Measurement Bias in X‐Ray Source Detection