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1st INTEGRAL Data Analysis Workshop ISDC , October 5-8, 2004 Imaging extended sources with JEM-X

1st INTEGRAL Data Analysis Workshop ISDC , October 5-8, 2004 Imaging extended sources with JEM-X. N. Lund C. Budtz-Jorgensen N.J. Westergaard J. Chevenez Danish Space Research Institute. Imaging of extended sources with a coded mask instrument.

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1st INTEGRAL Data Analysis Workshop ISDC , October 5-8, 2004 Imaging extended sources with JEM-X

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  1. 1st INTEGRAL Data Analysis WorkshopISDC, October 5-8, 2004Imaging extended sources with JEM-X N. Lund C. Budtz-Jorgensen N.J. Westergaard J. Chevenez Danish Space Research Institute

  2. Imaging of extended sourceswith a coded mask instrument Coded mask instruments are good for point sources because the point spread function is simple and the source signal is concentrated in a few pixels of the image. It is therefore also relatively simple to estimate the background under the source. Imaging extended sources are more complex – particularly if the morphology of the source is to be studied without prejudices. The results obtained in an analysis of a 1 Msec observation of SN1006 have demonstrated that JEM-X can image an extended source, and have inspired us to look at other data which have become public lately.

  3. Imaging of extended sources by JEM-XCase I: SN 1006 SN 1006 is an X-ray bright, high-latitude supernova remnant, well studied in many wavelengths. Significant cosmic ray accelleration is expected to take place in the remnant. INTEGRAL has observed SN 1006 for 1 Msec. (PI: Steven Reynolds) Shown here is an ASCA (0.4-8 keV) image of the remnant showing two X-ray emission lobes concentrated in the regions of strong electron accelleration near the remnnant boundary.

  4. JEM-X images of SN 1006 ASCA 0.4-8 keV JEM-X 3-4 keV JEM-X 4-8 keV At energies above 8 keV we cannot yet reliably detect the source. We are working on reducing the background noise in our images. Only 75% of the available INTEGRAL data have been used up to now.

  5. JEM-X imaging of extended sources Case II: Coma cluster 3 to 4 keV 4 to 8 keV The cluster is not securely detected above 8 keV.

  6. JEM-X imaging of extended sourcesCase III: NGC 1275 Central radio jet Radio halo Optical filaments (H-alpha) 0.3-3 keV X-rays . 30 arcsec 5 arcmin 10 arcmin 5 arcmin . N-S aligned N-S aligned N-S aligned ? symmetric

  7. JEM-X images of NGC 1275 3-4 keV 4-8 keV The N-S alignment of the core jet of NGC 1275 apparently emerges again in hard X-rays JEM-X point spread function illustrated with an image of GRS1915+105 8-14 keV 14-35 keV

  8. Extended source caveats 1) The outer extensions of the JEM-X image of the X-ray halo of NGC 1275 do not match with the XMM image. (Inadequate flat fielding of JEM-X image?) White contours: XMM 2 to 7 keV Green contours: JEM-X 4 to 8 keV 2) The observation was disturbed by a varying background. More work is needed! 3) Be patient !

  9. Midisky background suppression experiments Local flat field No cleaning Global flat field

  10. Detection of faint sources by JEM-X The OSA 4.0 supplied image mosaicking tool does not work with the JEM-X images generated under OSA 4.0 An improved imaging software (Midisky) is available from DSRI together with a mosaicking tool (Mosaic_weight). Both of these packages can be downloaded via ftp from: DSRI.DK pub/jemx/mosaic_weight.tar.gz pub/jemx/midisky/midi_distribution_2.tar.gz Both packages will become part of the OSA 5.0.

  11. Galactic Center - 2003 GCDE

  12. Galactic Center - 2004 SgrA PI: A. Goldwurm

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