{"id":3265,"date":"2024-04-09T09:11:00","date_gmt":"2024-04-09T07:11:00","guid":{"rendered":"https:\/\/x-ifu.irap.omp.eu\/?p=3265"},"modified":"2024-04-09T14:47:38","modified_gmt":"2024-04-09T12:47:38","slug":"instrument-response-files","status":"publish","type":"post","link":"https:\/\/x-ifu.irap.omp.eu\/fr\/science\/instrument-response-files","title":{"rendered":"Instrument response files have been updated"},"content":{"rendered":"

Figure:<\/strong> Effective area (cm\u00b2) of the X-IFU over the energy bandpass (keV) for its different optical configurations<\/em><\/p>\n

The X-IFU has recently undergone several changes in its design. An important work ahead of the launch is to analyse, verify and understand the X-IFU capabilities when observing celestial sources. This is mostly performed through simulations, using as inputs typical spectra and shapes of the observed objects (derived from previous missions) and folding in our current understanding of the instrument. The latter is encapsulated \u2013 in a simplistic albeit accurate way \u2013 in what is called the “instrument response files”, used as inputs by our simulators of X-ray observations (XSPEC, SPEX, SIXTE, SIXSA…). These responses provide a representative view of the spatial, spectral and temporal response of the instrument, alongside several important effects needed to estimate the final X-IFU performances (crosstalk, vignetting, grading). Following the consolidation of the new X-IFU design, the most up-to-date responses are now available for the community on this page<\/a>. These will allow scientist to understand the true potential of the X-IFU, prepare its observation plan and pave the way for future new discoveries.<\/p>\n

–<\/p>\n

Le X-IFU a r\u00e9cemment travers\u00e9 une phase de profond changement dans son architecture. Une partie importante du travail avant le lancement consiste \u00e0 analyser, v\u00e9rifier et comprendre les capacit\u00e9s d’un tel instrument lors de l’observation de sources c\u00e9lestes. Cela passe essentiellement par la simulation d’observations, au travers d’entr\u00e9es comme les spectres et formes des sources connues (issues de missions pr\u00e9c\u00e9dentes) convolu\u00e9es par notre connaissance actuelle de l’instrument. Cette derni\u00e8re est contenue \u2013 de mani\u00e8re simpliste mais pr\u00e9cise \u2013 au sein de ce que l’on appelle des \u00ab matrices de r\u00e9ponse instrumentale \u00bb, qui servent de point de d\u00e9part pour tous nos simulateurs d’observations rayon X (XSPEC, SPEX, SIXTE, SIXSA…). Ces matrices de r\u00e9ponses donnent aux utilisateurs une id\u00e9e des capacit\u00e9s spectrales, spatiales et temporelles de l’instrument, tout en incluant des effets instrumentaux fondamentaux pour les performances du X-IFU (diaphonie, vignettage, effet de notation). Suite \u00e0 la consolidation de la nouvelle architecture instrument, les matrices de r\u00e9ponse les plus \u00e0 jour sont d\u00e9sormais disponibles pour la communaut\u00e9 sur cette page<\/a>. Ces matrices de r\u00e9ponse permettront aux scientifiques de comprendre le potentiel du X-IFU, de pr\u00e9parer le plan d’observations et de poser les jalons de futures nouvelles d\u00e9couvertes.<\/p>","protected":false},"excerpt":{"rendered":"

The X-IFU has recently undergone several changes in its design architecture. An important work ahead of the launch is to analyse, verify and understand the X-IFU capabilities when observing. That’s why the instrument response files have been updated.<\/p>","protected":false},"author":5,"featured_media":3267,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"inline_featured_image":false,"footnotes":""},"categories":[10],"tags":[55,15,42,13],"acf":[],"yoast_head":"\nInstrument response files have been updated - Athena X-IFU<\/title>\n<meta name=\"description\" content=\"An important work ahead of the launch is to analyse the X-IFU capabilities when observing. 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