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[Date Prev][Date Next][Thread Prev][Thread Next][Search] [Main Index] [Thread Index] [HEASARC Archives] GSFC XMM-Newton GOF Status Report #385: XMM-NEWTON NEWS #242
News #242, 12 April 2021
CONTENTS
[1]NEW PIPELINE VERSION RELEASED
[2]A DATABASE OF UPPER LIMITS created and made accessible from the XMM-Newton Science Archive
[3]XSA v13.1 RELEASE WITH ACCESS TO THE UPPER LIMITS DATABASE
NEWS
New Pipeline version released
A new version of the Pipeline Processing System (PPS) based on SASv19.0
has been released. Most important changes are aimed to facilitate the
estimate of pile-up effects in EPIC-pn spectra of bright X-rays sources
and to ease the combined spectral analysis of EPIC and OM sources.
A number of spectral products for different selection criteria are now
provided for bright sources in EPIC-pn camera.
OM fluxes are converted into PHA OGIP compliant format for individual
sources so that they can be loaded into X-rays standard spectral model
fitting packages. These OM PHA spectra are provided for OM sources
located close to some EPIC source.
In addition, the lightcurves obtained from different OM exposures in
Fast Mode are merged into a single file that covers the whole duration
of the observation.
A DATABASE OF UPPER LIMITS created and made accessible from the XMM-Newton
Science Archive
Upper limits, from the three EPIC cameras, have been pre-calculated and
stored in a database for slew observations and pointed observations
which are public. This is an on-going process with new observations
being added as they become available.
They have been calculated at 1,2 and 3-sigma significance using 1-sided
Bayesian statistics, which correspond to confidence probabilities of
84.13, 97.72 and 99.87% that the true count-rate value lies below the
respective upper limit. Values are available for soft (0.2-2 keV), hard
(2-12 keV) and total (0.2-12 keV) energy bands. Upper limit records are
shown when the input position lies within the field-of-view of a
pointed or slew observation and is not close to a detected source, is
not close to a chip gap or the edge of the field and where, for pointed
observations, the background is non-zero.
Upper limits are calculated from pipeline images using aperture
photometry. Source counts are extracted from a circle of radius of 15"
(pointed) and 30" (slew). Background counts for pointed data are
extracted from pipeline background maps, with a circle of radius 60".
For slew observations, background counts are extracted from an annulus
of inner radius 60" and outer radius 120".
The upper limit database can be searched via the XMM-Newton Science
Archive (XSA) interface. More details are provided [4]in this web page.
The database has been constructed by Planetek Hellas and the National
Observatory of Athens under an ESA-financed contract, in collaboration
with the XMM-Newton SOC and the ESAC Science Data Centre.
.
XSA V13.1 RELEASE WITH ACCESS TO THE Upper Limits DATABASE
A new version of the XMM-Newton Science Archive (XSA v13.1) is
available at
[5]https://www.cosmos.esa.int/web/xmm-newton/xsa
XSA v13.1 provides access to the new Upper Limits Database. SED
products generated by CDS have been updated to new files based on
4XMM-DR10.
XMM-Newton Science Operations Centre at
ESA's European Space Astronomy Centre,
Villanueva de la Ca�, Madrid, Spain
[6]SOC Home [7]Helpdesk Web Interface [8]Contact Helpdesk [9]Newsletter
Archive
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References
4. http://www.cosmos.esa.int/web/xmm-newton/epic-upper-limits
5. https://www.cosmos.esa.int/web/xmm-newton/xsa
6. https://www.cosmos.esa.int/web/xmm-newton
7. https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
8. mailto:xmmhelp@sciops.esa.int
9. https://www.cosmos.esa.int/web/xmm-newton/newsletter
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