1 / 16

XMM-Newton Observation of the composite SNR G0.9+0.1 and the discovery of a new transient source

XMM-Newton Observation of the composite SNR G0.9+0.1 and the discovery of a new transient source. Lara Sidoli (IASF Milano) Fabrizio Bocchino (Oss. Palermo) Sandro Mereghetti (IASF Milano) Rino Bandiera (Oss. Arcetri). Overview. Preliminary XMM results on the SNR G0.9+0.1

tejana
Download Presentation

XMM-Newton Observation of the composite SNR G0.9+0.1 and the discovery of a new transient source

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. XMM-Newton Observation of the composite SNR G0.9+0.1 and the discovery of a new transient source Lara Sidoli (IASF Milano) Fabrizio Bocchino (Oss. Palermo) Sandro Mereghetti (IASF Milano) Rino Bandiera (Oss. Arcetri)

  2. Overview • Preliminary XMM results on the SNR G0.9+0.1 • X-ray emission from the Pulsar Wind Nebula • X-ray emission from the radio shell ? • Discovery of a new X-ray Transient in the Galactic Center region

  3. The Composite SNS G0.9+0.1: radio vs X-rays • Radio polarized core (2'diameter) and a radio shell (8' diameter) • Galactic Center region: the high absorption hampered the discovery at soft X-rays • BeppoSAX discovery of X-rays from the PWN (Mereghetti, Sidoli, Israel 1998)

  4. XMM-Newton Observation

  5. XMM-Newton vs Chandra • Expanded view of the central part of the XMM-Newton PN image (2-10 keV) • Comparison with the differentsubstructures resolved with Chandra inside the PWN

  6. Radial profile • Comparison of the G0.9+0.1 radial profile with the LMC X-3 profile taken as reference for the PSF • --- 2-5 keV • --- 2-10 keV • --- 5-10 keV

  7. Spectral Analysis: the entire PWN • We extracted PN and both MOS counts from within 1' from the PWN peak and corrected with a local background

  8. PWN spectral results

  9. Spectral Softening at larger distance • Analysis of 3 spectra extracted from 3 annular regions centered on the PWN shows a spectral softening • Powerlaw fits performed fixing the column density at the entire PWN spectrum best fit

  10. Preliminary results on the X-ray emission from the radio shell • Net rate from the radio shell region 0.0097 +/- 0.0011 counts/s (3-6 keV)

  11. X-rays from the shell region

  12. Discovery of a NEW TRANSIENT Source in the Galactic Center region • A new X-ray source at R.A.=17h 47m 16.0s Dec= -28deg 10' 45'' • Comparison between a GC survey observation performed on Sept.23, 2000 (Porquet et al. 2003) and our observation performed on March 12, 2003

  13. Spectral Analysis of the New Transient

  14. Powerlaw model fit to the X-ray Transient Spectrum: • Absorption Column Density ~ 8 E22 cm-2 • Photon Index = 2.1 +/- 0.1 • Unabs. Flux = 6.8 E-12 erg/cm2/s • Luminosity (2-10 keV) ~ 7 E34 erg/s (@ 10 kpc) • It's likely a transient LMXB located in the GC region

  15. Conclusions • Preliminary results on the Composite SNR G0.9+0.1: • Entire PWN spectrum well fit with a power law with typical parameters of other PWNs • No hardness variations inside the nebula, with respect to XMM 2000 observation • Spectral Softening of the X-ray emission in the PWN with increasing distance from its brightness peak • Possible detection of X-rays from the radio shell (confirming Porquet et al. 2003 discovery), maybe of non-thermal origin

  16. Conclusions 2 • Discovery of a New X-ray Transient source • High absorption • Spectrum well fit with a single powerlaw • Change in the observed flux of at least a factor of 80 between 2000 and 2003 XMM-Newton observation • It is likely a transient LMXB in the GC region

More Related