DOPPLER-BROADENED IRON X-RAY LINES FROM TYCHO'S SUPERNOVA REMNANT

We use Suzaku observations to measure the spatial variation of the Fe Kα line with radius in the Tycho supernova remnant. The Fe line widths show a significant decrease from a FWHM value of 210 eV at the center to 130 eV at the rim. Over the same radial range the line center energy remains nearly constant. These observations are consistent with a scenario in which the shell of Fe-emitting ejecta in Tycho is expanding at speeds of 2800-3350 km s–1. The minimum line width we measure is still a factor of two larger than expected from a single component plasma emission model. If thermal Doppler broadening is the dominant additional source of broadening, we infer an ion temperature of (1-3) × 1010 K.

[1]  P. P. Plucinsky,et al.  Cosmic-Ray Acceleration at the Forward Shock in Tycho’s Supernova Remnant: Evidence from Chandra X-Ray Observations , 2005, astro-ph/0507478.

[2]  P. Ruiz-Lapuente.  Tycho Brahe’s Supernova: Light from Centuries Past , 2003, astro-ph/0309009.

[3]  Hideyuki Mori,et al.  New CTI Correction Method for Spaced-Row Charge Injection of the Suzaku X-Ray Imaging Spectrometer , 2008, 0810.0873.

[4]  T. Tanaka,et al.  In-Orbit Performance of the Hard X-Ray Detector on Board Suzaku , 2006, astro-ph/0611233.

[5]  H. Murakami,et al.  Energy-Scale Calibration of the Suzaku X-Ray Imaging Spectrometer Using the Checker Flag Charge-Injection Technique in Orbit , 2008, 0809.3665.

[6]  R. Smith,et al.  Balmer-dominated Spectra of Nonradiative Shocks in the Cygnus Loop, RCW 86, and Tycho Supernova Remnants , 2000, astro-ph/0010496.

[7]  Shunsaku Okada,et al.  The X-Ray Telescope onboard Suzaku , 2007 .

[8]  J. Hughes.  To Appear in the Astrophysical Journal Letters Preprint typeset using L ATEX style emulateapj THE EXPANSION OF THE X-RAY REMNANT OF TYCHO’S SUPERNOVA (SN1572) , 2000 .

[9]  John P. Hughes,et al.  The Blast Wave of Tycho’s Supernova Remnant , 2007, astro-ph/0703239.

[10]  U. Hwang,et al.  X-Ray Emission-Line Imaging and Spectroscopy of Tycho's Supernova Remnant , 1996, astro-ph/9608048.

[11]  Ryuichi Fujimoto,et al.  The X-Ray Observatory Suzaku , 2007 .

[12]  Motohide Kokubun,et al.  Suzaku Observations of Tycho's Supernova Remnant , 2008, 0805.3377.

[13]  R. Yamazaki,et al.  A Spatial and Spectral Study of Nonthermal Filaments in Historical Supernova Remnants: Observational Results with Chandra , 2004, astro-ph/0411326.

[14]  R. Kirshner,et al.  Six Balmer-dominated supernova remnants , 1991 .

[15]  Tuneyoshi Kamae,et al.  Hard X-Ray Detector (HXD) on Board Suzaku , 2006, astro-ph/0611232.

[16]  NasaGsfc,et al.  RADIOACTIVE SCANDIUM IN THE YOUNGEST GALACTIC SUPERNOVA REMNANT G1.9+0.3 , 2010, 1006.3552.

[17]  E. Reynoso,et al.  A VLA Study of the Expansion of Tycho's Supernova Remnant , 1997 .

[18]  R. Kirshner,et al.  The optical emission from a fast shock wave with application to supernova remnants , 1980 .

[19]  J. A. Gregory,et al.  X-Ray Imaging Spectrometer (XIS) on Board Suzaku , 2007 .

[20]  John P. Hughes,et al.  Constraints on the physics of type ia supernovae from the x-ray spectrum of the tycho supernova remnant , 2006 .

[21]  S. Gull,et al.  Neutral hydrogen towards 3C 10, the remnant of Tycho's supernova , 1986 .