Investigation into the strong residuals seen

Slides:



Advertisements
Similar presentations
EPIC Calibration Meeting, Mallorca Low energy calibration with the Vela SNR K. Dennerl, 2009 March 31 Low energy calibration with the Vela SNR Mallorca,
Advertisements

XMM EPIC MOS Jenny Carter EPIC Background, Operations and Calibration Mallorca, March/April 09 Jenny Carter, University of Leicester.
XMM EPIC MOS Jenny Carter 4 th EPIC BG WG Meeting Mallorca, 25/10/06 BGWG blank sky data analysis Jenny Carter, University of Leicester.
Solar flare hard X-ray spikes observed by RHESSI: a statistical study Jianxia Cheng Jiong Qiu, Mingde Ding, and Haimin Wang.
Dennis Bodewits 1, Damian Christian 2, Casey Lisse 3, Scott Wolk 4, Konrad Dennerl 5, Jenny Carter 6, Andy Read 6, and Susan Lepri 7 (1) Univ. Maryland,
Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal April ACIS Calibration: Recent Updates, Planned Updates, & Future Issues 2.E0102: Joint.
XMM-Newton 1 Michael Smith, ESAC PN Monitoring MPE, May 2006.
XMM EPIC MOS Steve Sembay ESAC 04/10/05 Implementation of the MOS spatial/temporal DRM: Does it work ? Zeta Puppis: Checking the line.
Chandra Calibration Status Calibration Updates Since Last CUC Meeting ACIS 1. New tgain files were released for epochs 23 and 24 (May 2005 – Nov 2005)
XMM-Newton 1 Michael Smith, ESAC PN Monitoring Palermo, April 2007.
XMM-Newton 1 M.Stuhlinger/M.Smith, ESAC PN Monitoring Mallorca, November 2007.
Experience with combined Fe55/Vela SNR calibration - MOS Andrea Tiengo INAF, IASF-Milano In collaboration with: Mariachiara Rossetti (IASF-Milano) Martin.
EPIC Calibration Meeting, MPE K. Dennerl, 2006 May 04 EPIC pn at low energies: LW mode Properties of EPIC pn at low energies: LW mode.
6 November 2007Cal-Ops Meeting Mallorca Recent Results from EPIC MOS Life Test Facility Tony Abbey and Craig Brown University of Leicester Space Research.
XMM-Newton 1 M.Stuhlinger/P.Calderon, ESAC Re-appearance of the MOS1 CCD1 meteorite column during revs Madrid, 23. March 2010.
Energy Calibration using SNRs: preliminary results Andrea Tiengo INAF, IASF-Milano Mallorca, 6 November 2007 EPIC Calibration Meeting.
XMM EPIC MOS Steve Sembay MPE 04/05/06 The Effective Area of EPIC A comparison of MOS1, MOS2 and PN derived fluxes of 17 on-axis AGN.
MOS 3x3 mode slow slew survey Richard Saxton October 2006.
EPIC Calibration Meeting, Mallorca K. Dennerl, 2006 October 26 EPIC pn: Jumps in the energy scale Sudden jumps in the absolute energy scale and their origin.
The EPIC-pn spectral response Frank Haberl EPIC Cal meeting, Tübingen, February 2003 Status of the pn spectral response in SAS5.4.1 Latest developments.
Mallorca EPIC Cal Meeting - February 2005 Darren Baskill: XMM project: MOS monitoring.
Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Nov ACIS Calibration: Planned Updates & Future Issues 2.ACIS Operations: Controlling the.
EPIC Calibration Meeting, Mallorca K. Dennerl, 2006 October 26 CTI.. update for EPIC pn EPIC pn: Update on the CTI, the absolute energy scale and the energy.
High-Resolution X-ray Spectroscopy of AGN Warm Absorbers Rebecca Smith MSSL, UCL with G. Branduardi-Raymont and M. Page.
Photons of Light The smallest unit of light is a photon A photon is often called a particle of light The Energy of an individual photon depends on its.
Chandra Calibration Status CUC Meeting Oct. 13, 2011.
EPIC Calibration Meeting, Mallorca K. Dennerl, 2006 October 26 Suppression of the low-energy noise Suppression of the low-energy noise: an improved approach.
XMM-Newton 1 Michael Smith, ESAC PN Monitoring Mallorca, October 2006.
The EPIC-PN response matrix - update Frank Haberl EPIC Cal meeting, VILSPA, March 2004 Known problems in PN6.6 / SAS6.0.
Capture of electrons in traps photon pixel time = trap = occupied trap.
XMM 1 EPIC MOS Monitoring CAL/OPS Meeting Mallorca
Marcus Kirsch, XMM-Newton European Space Astronomy Center Page 1 EPIC ESAC Energy calibration refinement of the EPIC-pn Burst mode M.G.F. Kirsch 1, E.
Column rejection in the MOS  The core of soft sources is removed by the standard emchain.  Due to very large fluctuations in count rate from one column.
XMM EPIC MOS Steve Sembay Mallorca 02/02/05 Temporal and spatial variability of the MOS RMF 1.Introduction and brief history of the.
EPIC Calibration Meeting, Madrid Correcting spatial inhomogeneities of the absolute energy scale K. Dennerl, 2010 March 23 Correcting spatial inhomogeneities.
EPIC Calibration Meeting, Mallorca Origin of gain offsets K. Dennerl, 2008 April 8 Origin of gain offsets: new insights from eROSITA calibration Mallorca,
J.Vaitkus et al., WOEDAN Workshop, Vilnius, The steady and transient photoconductivity, and related phenomena in the neutron irradiated Si.
(Deep Level Transient Spectroscopy) II. Advanced Techniques
Optical Characterization of GaN-based Nanowires : From Nanometric Scale to Light Emitting Devices A-L. Bavencove*, E. Pougeoise, J. Garcia, P. Gilet, F.
XIS FM sensors cal. report Hiroshi Nakajima XIS
NEEP 541 Ionization in Semiconductors - II Fall 2002 Jake Blanchard.
Thermally Stimulated Currents Method Ioana Pintilie a) National Institute of Materials Physics, Bucharest-Magurele, P.O.Box MG-7, Romania b) Institute.
Suzaku Study of X-ray Emission from the Molecular Clouds in the Galactic Center M. Nobukawa, S. G. Ryu, S. Nakashima, T. G. Tsuru, K. Koyama (Kyoto Univ.),
Development of CCDs for the SXI We have developed 2 different types of CCDs for the SXI in parallel.. *Advantage =>They are successfully employed for current.
J.Vaitkus. RD50 Workshop, Liverool, May, 2011 Deep level system Gaussian approximation according the extrinsic photoconductivity in irradiated Si.
Electron Energy Loss Spectroscopy (EELS) Suggested Reading: Used electron spectrometer Used TEM Review of theory for elastic + inelastic scattering Examples.
A Brief Review of “Matter”. Atom nucleus electron e-e- (proton,neutrons) p+p+ n ● 10,000,000 atoms can fit across a period in your textbook. ● The nucleus.
3 May 2007 Suzaku Users mwb MIT/MKI XIS Update Mark Bautz, MIT Kavli Institute XIS-2 Anomaly Contamination.
EPIC Calibration Meeting, Madrid Experience with combined Fe 55 /Vela SNR calibration K. Dennerl, 2010 March 23 Experience with combined Fe 55 / Vela SNR.
The onboard calibration for the spaced-row charge injection of the Suzaku XIS Hideki Uchiyama, Yoshiaki Hyodo, Hiroya Yamaguchi, Hideyuki Mori, Takeshi.
Application of a Charge Transfer Model to Space Telescope Data Paul Bristow Dec’03
XMM-Newton 1 Michael Smith, ESAC PN Monitoring Mallorca, April 2008.
Boron and Phosphorus Implantation Induced Electrically Active Defects in p-type Silicon Jayantha Senawiratne 1,a, Jeffery S. Cites 1, James G. Couillard.
CCD Calibrations Eliminating noise and other sources of error.
Experience with combined Fe55 / Tycho SNR calibration
Dong Li Purple Mountain Observatory, CAS
Ioana Pintilie, 11 th RD50 Workshop, November 2007, Geneve
Nature of the Band Gap in the Transparent Conducting Oxide In2O3
The RGS view of Markarian 421 Lights Shadows And
Revision CHAPTER 6.
A large XMM-Newton project on SN 1006
Deep Level Transient Spectroscopy (DLTS)
Trap Pumping Method Importance of inter-phase trapping
Infrared study of a star forming region, L1251B
EPIC Calibration & Operations Meeting
Temporal &Spatial Dependency of the MOS RMF
Calibration Activities – the MOS perspective
Long-term trends in EPIC pn energy response
-Short Talk- The soft X-ray characteristics of solar flares, both with and without associated CMEs Kay H.R.M., Harra L.K., Matthews S.A., Culhane J.L.,
Fig. 6 PL study showing the lower energetic states at the layer edges.
Presentation transcript:

Investigation into the strong residuals seen near the Oxygen edge in MOS spectra of bright continuum sources. Rate Dependent CTI effect ? Steve Sembay

Event 1 Readout direction Event 2 Trap

Emission timescales for filled traps (Holland et al. 1993, NIMS, A326, 335) σn electron capture cross section Xn entropy factor υth electron thermal velocity Ncdensity of states in conduction band E energy level of trap T temperature

Level (eV) te (-90°C) (-100°C) (-120°C) 0.17 0.44 Emission timescales for filled traps (Holland et al. 1993, NIMS, A326, 335) Level (eV) te (-90°C) (-100°C) (-120°C) 0.17 0.07 µs 0.19 µs 1.1 µs 0.44 3.8 s 22.9 s 1.4 x 103 s c.f. row transfer time of MOS = 15 µs

Around O edge χ2 -> 3.90 – 2.13 with gain offset = 8.7±1.0 eV

Around Si and Au edge: χ2 -> 1.025 – 0.998 Offset ~ 12.5 eV

MOS v RGS Line Energy: N line ~ 432 eV J. Carter (Mallorca 06) Most MOS Large Window Mode SW Obs.

Closed Cal Al line in small window mode

Closed Cal Al line in small window mode

Is there a “possible” gain shift at O: CTI dependent on rate? Method 1: Analyse spectra from different regions

Sample of bright AGN/BL Lacs: The “Usual Suspects” MKN 421 0165 MKN 421 0171 3C 273 0277 H1426+428 0278 PKS2155-304 0362 PKS2155-304 0450 ARK 120 0679 H1426+428 0852 PKS2155-304 1095 PKS2155-304 1266 3C 273 1299 MKN 421 1357

MOS1 Count Rate v Offset In Boxes Before/After Cooling

MOS2 Count Rate v Offset In Boxes Before/After Cooling

Is there a “possible” gain shift at O: CTI dependent on rate? Method 2: Flag precursor events from event file

Flag Bad Readout direction Flag Bad

Flagged events

|Summary: Observed offset is not affected by removal of precursor events in CCD RAWY direction This suggests offset is not caused by incorrect application of CTI measurement due to trap filling in CCD.