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Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://xmm.vilspa.esa.es/docs/documents/Appendix/Summary.html
Äàòà èçìåíåíèÿ: Tue Jan 9 10:52:07 2001
Äàòà èíäåêñèðîâàíèÿ: Sat Dec 22 02:35:34 2007
Êîäèðîâêà:
Ïîèñêîâûå ñëîâà: carl sagan

· Summary of open items

Do we need an OCR on the system which provides the CD-ROMs of ERME data ? The time data seem suspect. (CLOSED)

Urgently need to review the rejection efficiency to cosmic ray primaries maybe from diagnostic or similar data. This should allow to confirm the distribution of fluorescent background components. (Action PF to summarise MOS findings already reported briefly. MPE and SRON to make similar findings available by March 2001)

Gather revised data for configurations etc. that went into the XMM modeling. (Action ED to contact CHANDRA for their inputs. SSD and WMA check what is available from PX)

Convert ERME count rate data into fluences and subsequently into focal plane received dose. (Action WMA)

Update AE8 models into operational altitude limits. Furthermore review incorporation of improved CHANDRA models. (Action XMM-SOC Vilspa review CHANDRA updates in 2001)

The EPIC gain data is affected by the RGS temperature excursions.

What to include for the SAS public release?

Complete actions from splinter to confirm update in RGS procedures to minimize temperature excursions. (Action JdH confirm mode)

Complete analysis to provide gain correction model. (Action EPIC)

Review what can be learnt wrt. the micro-meteorite model. Any tests we should investigate ? (Action LS report back to XMM SOC ca. March 2001)

Determine telescope orientation for the micro-meteorite event. (Action XMM-Newton SOC Check attitude history Jan 2001 ).

Calculate and maintain relevant data for knowing where XMM-Newton is wrt. the magnetotail. Compare data to CTI history curves and soft proton flare history. (Action XMM-Newton SOC March 2001)

Use the PN data to determine the accumulated MOS soft proton dose. (Action EK to provide conversion data for XMM-Newton SOC to correlate)

Review the allowable MOS soft proton dose and decide if we can institute an orbit allowed fluence in addition to our current monitoring levels. (Action EPIC and XMM-Newton SOC March 2001)

Review the CHANDRA and EPIC soft proton fluences and damage coefficients to understand if the current levels are too conservative. (Action EPIC and XMM-Newton SOC March 2001)

Implement more prompt bad pixel monitoring at VILSPA (Action XMM-Newton SOC Jan 2001)

Implement regular 3 by 3 Diagnostic data as part of the MOS cycle of internal calibration exposures. (Action XMM-Newton SOC Jan 2001)

Compare the 30% changes in vignetted background rate with ERME count rate trends. (Action S Molendi provide times for XMM-Newton SOC to correlate)

Check the energy dependence in the modelled vignetting (GEANT4). (Check CHANDRA model, if interested). (Action ESTEC WMA)

Provide vignetting as fn(E) data so that we can update/validate the scattering models (Action S Molendi, JdHerder, K Dennerl supply data to E Daly Feb 2001)

Provide collection of meeting papers on-line (Closed)

Provide URL for WMA site at ESTEC. (http://www.estec.esa.nl/wmwww/WMA/)

Check the soft p+ induced oxide dose versus the flatband shift that would induce operational changes (Action EPIC and XMM-Newton SOC Mar 2001)

Full discarded lines + RGS above threshold counts history for all flares (Action XMM-Newton SOC Mar 2001 )

Compare the CCD1 vs. CCD9 RGS above threshold counts for all flares (Action RGS Mar 2001)

Plot a distribution of the peaks (/cm**2/s) of soft p+ flares for XMM-Newton and Chandra. The shift required to normalise the two distributions should give you the relative transmission efficiency ? (Take care with normalisation for filters, HETG etc.) (Action XMM-SOC and contact with CXC Mar 2001)