EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Experience with combined Fe 55 / Vela SNR calibration Madrid, 2010 March EPIC Calibration & Operations Meeting NRCO 81

EPIC Calibration Meeting, Mallorca Experience with combined Fe 55 /Tycho SNR calibration K. Dennerl, 2008 April 8 Internal calibration source onboard XMM-Newton / EPIC-pn Al-K Mn-K

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March ks in 2000  210 ks in 2008  390 ks in 2010  1.4 Ms in ks in 2000  210 ks in 2008  390 ks in 2010  1.4 Ms in ks 30 ks half-life of Fe 55 : 2.7 yr  activity in 2010: 7.7% of activity in 2000 Motivation: decay of the internal calibration source

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 NRCO 81

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 NRCO 81 0) offset map calculation 1) cal-closed 2) thin (Vela SNR) 3) cal-thin (Vela SNR)

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 NRCO 81

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Strategy: 1.start with regular Fe 55 exposure 2.perform regular Vela observation 3.finish with Vela + Fe 55 observation Questions: 1.does Vela disturb the calibration exposure ? 2.does the internal calibration source disturb the Vela observation ? same offset map used in all exposures, all exposures performed in a contiguous mode, within one revolution sequence: cal-closed  thin  cal-thin NRCO 81

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 calclosed: T22:35: T09:46: thin: T09:54: T21:14: calthin: T21:21: T08:53: red: keV, 0 – 25 cts/px green: 1.2 – 1.8 keV, 0 – 5 cts/px blue: 5.0 – 7.0 keV, 0 – 4 cps/px Spectra and images, derived from singles cal-closedthincal-thin

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  comparison cal-closed cal-thin

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Method: compare line position in 30 subfields * for every quadrant *with sufficient photon statistics errors determined from the spread of the line energies

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 0cal-thin (Vela SNR), quadrant ± ± adu all singles

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 1cal-thin (Vela SNR), quadrant ± 1.9 all singles ± adu

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 2cal-thin (Vela SNR), quadrant ± 1.6 all singles ± adu

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 3cal-thin (Vela SNR), quadrant ± 3.2 all singles ± adu

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  comparison cal-closed cal-thin quadrant 0: +0.6 adu quadrant 1: +1.1 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu quadrant 0: +0.6 adu quadrant 1: +1.1 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu  yes, systematic shift of Mn-K α to higher energies:

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  comparison cal-closed cal-thin  yes, systematic shift of Mn-K α to higher energies: quadrant 0: +0.6 adu quadrant 1: +1.1 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu quadrant 0: +0.6 adu quadrant 1: +1.1 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu Main difference: presence of additional photons in cal-thin  could an inappropriate correction of precursor induced CTI changes cause the shift ?  same analysis with first singles..

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 0cal-thin (Vela SNR), quadrant 0 all first singles ± ± adu

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 1cal-thin (Vela SNR), quadrant 1 all first singles ± adu ± 1.8

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 2cal-thin (Vela SNR), quadrant 2 all first singles ± adu ± 1.6

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, quadrant 3cal-thin (Vela SNR), quadrant 3 all first singles ± adu ± 2.3

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  comparison cal-closed cal-thin  yes, systematic shift of Mn-K α to higher energies: quadrant 0: +0.6 adu quadrant 1: +1.1 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu quadrant 0: +0.6 adu quadrant 1: +1.1 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu singles Main difference: presence of additional photons in cal-thin: could an inappropriate correction of precursor induced CTI changes cause the shift ?  same analysis with first singles.. Main difference: presence of additional photons in cal-thin: could an inappropriate correction of precursor induced CTI changes cause the shift ?  same analysis with first singles..  energy shift not caused by (visible) precursors quadrant 0: +0.7 adu quadrant 1: +1.2 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu quadrant 0: +0.7 adu quadrant 1: +1.2 adu quadrant 2: +0.5 adu quadrant 3: +0.1 adu first singles

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  The systematic energy shift of Mn-K α when the Vela SNR is in the FOV is not due to imperfect modeling of (visible) precursors. Could this be a temporal effect due to, e.g., temperature changes ?  Splitting the exposures into pieces of the same length (~600s) and monitoring the line energy (from the whole detector) with XSPEC..

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  Splitting the exposures into pieces of the same length (~600s) and monitoring the line energy (from the whole detector) with XSPEC.. cal-closed, all singles cal-thin, all singles 1σ errors determined from Δχ 2 = +1 Mn-K

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  Splitting the exposures into pieces of the same length (~600s) and monitoring the line energy (from the whole detector) with XSPEC.. cal-closed, first singles cal-thin, first singles 1σ errors determined from Δχ 2 = +1 Mn-K

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, first singles cal-thin, first singles cal-closed, all singles cal-thin, all singles  the energy shift happens between the observations

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23  an energy shift happens also at Al-K cal-closed, all singles cal-thin, all singles Does the presence of the Vela SNR (and the different filter wheel position) affect the calibration measurements with the internal Fe 55 source ?  Splitting the exposures into pieces of the same length (~600s) and monitoring the line energy (from the whole detector) with XSPEC.. 1σ errors determined from Δχ 2 = +1 Al-K

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, all singles spectrum over the full detector and the whole time interval cal-thin, all singles spectrum over the full detector and the whole time interval E = ( / ) keVE = ( / ) keV from total exposures: + (5.0 ± 0.7) eV

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closed, all singles spectrum over the full detector and the whole time interval cal-thin, all singles spectrum over the full detector and the whole time interval from total exposures: E = ( / ) keVE = ( / ) keV + (4.5 ± 0.8) eV

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Does the presence of the internal Fe 55 source affect the calibration measurements with the Vela SNR ?  comparison thin cal-thin

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 thin, all singles spectrum over the full detector and the whole time interval cal-thin, all singles spectrum over the full detector and the whole time interval from total exposures: E = ( / ) keV E = ( / ) keV + (0.3 ± 0.6) eV

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23  no energy shift happens at OVII between thin and cal-thin thin, all singlescal-thin, all singles  Splitting the exposures into pieces of the same length (~600s) and monitoring the line energy (from the whole detector) with XSPEC.. 1σ errors determined from Δχ 2 = +1 Does the presence of the internal Fe 55 source affect the calibration measurements with the Vela SNR ? OVII

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 E = ( / ) keVE = ( / ) keV E = ( / ) keVE = ( / ) keVE = ( / ) keV E = ( / ) keVE = ( / ) keV Summary: line energies (all singles, whole detector) cal-closedthincal-thin + (0.3 ± 0.6) eV + (4.5 ± 0.8) eV + (5.0 ± 0.7) eV

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 cal-closedthincal-thin Summary of NRCO 81 Changing from cal-closed to cal-thin, with the Vela SNR in the FOV, increases the energies of Al-K and Mn-K by ~ 5 eV. No change in the line energy is observed at the OVII emission from the Vela SNR, if the detector is additionally irradiated with the internal calibration source.

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Conclusions from NRCO 81 The change observed between cal-closed and cal-thin is not caused by deficiencies in the code for the precursor correction. It is, however, possible that photons/particles penetrating the thin filter release additional charge in the CCDs which is below the low energy threshold and thus not transmitted, but still capable of reducing the charge transfer losses by trap saturation. Independent of its origin, the fact that an energy shift is observed between the cal-closed and cal-thin observation indicates that cal-thin conditions may be more appropriate for exposures with the internal calibration source. Cal-thin (and probably also cal-medium and cal-thick) observations of suitable targets offer promising opportunities for future calibration exposures. The Vela SNR is definitively suited for such a purpose.

EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Experience with combined Fe 55 / Vela SNR calibration Madrid, 2010 March EPIC Calibration & Operations Meeting NRCO 81