RR Pic (1925): A Chandra X-ray view

Pekoen, Y.
Balman, Şölen
We present the Chandra ACIS-S3 data of the old classical nova RR Pic (1925). The source has a count rate of 0.067 +/- 0.002 count s(-1) in the 0.3 - 5.0 keV energy range. We detect the orbital period of the underlying binary system in the X- ray wavelengths. We also find that the neutral hydrogen column density differs for orbital minimum and orbital maximum spectra with values 0.25(-0.18)(+0.23) x 10(22) and 0.64(-0.14)(+ 0.13) x 10(22) cm(-2) at 3 sigma confidence level. The X- ray spectrum of RR Pic can be represented by a composite model of bremsstrahlung with a photoelectric absorption, two absorption lines centered around 1.1 - 1.4 keV and five Gaussian lines centered at emission lines around 0.3 - 1.1 keV corresponding to various transitions of S, N, O, C, Ne and Fe. The bremsstrahlung temperature derived from the fits ranges from 0.99 to 1.60 keV and the unabsorbed X-ray flux is found to be 2.5(-1.2)(+0.4) x 10(-13) erg cm(-2) s(-1) in the 0.3 - 5.0 keV range with a luminosity of 1.1 +/- 0.2 10(31) erg s(-1) at 600 pc. We also detect excess emission in the spectrum possibly originating from the reverse shock in the ejecta. A fit with a cooling flow plasma emission model shows enhanced abundances of He, C, N, O and Ne in the X- ray emitting region indicating existence of diffusive mixing.


Chandra observation of the shell of Nova Persei 1901 (GK Persei): Detection of localized nonthermal X-ray emission from a miniature supernova remnant
Balman, Şölen (IOP Publishing, 2005-07-10)
I present data on the shell of classical Nova Persei (1901) obtained by the Advanced CCD Imaging Spectrometer S3 detector on board the Chandra X-Ray Observatory. The X-ray nebula is affected mostly by the complex interstellar medium around the nova and has not developed a regular shell. The X-ray nebula is lumpy and asymmetric, with the bulk of the emission coming from the southwestern quadrant. The brightest X-ray emission is detected as an arc that covers the region from the west to the south of the centr...
RXTE and Swift Observations of SWIFT J0513.4-6547
Sahiner, S.; Serim, Muhammed Miraç; Baykal, Altan; İNAM, SITKI ÇAĞDAŞ (Oxford University Press (OUP), 2016-02-11)
We present timing and spectral analysis of Swift-XRT (X-ray Telescope) and RXTE-PCA (Rossi X-ray Timing Explorer-proportional Counter Array) observations of the transient Be/X-ray pulsar SWIFT J0513.4-6547 during its outburst in 2009 and its rebrightening in 2014. From 2009 observations, short-term spin-up rate of the source after the peak of the outburst is found to have about half of the value measured at the peak of the outburst by Coe et al. When the source is quiescent between 2009 and 2014, average sp...
Avdan, H.; Avdan, S.; AKYÜZ, AYSUN; Balman, Şölen; AKSAKER, NAZIM; AKKAYA ORALHAN, Inci (American Astronomical Society, 2016-09-10)
We study the X-ray and optical properties of the ultraluminous X-ray source (ULX) X-6 in the nearby galaxy NGC 4258 (M106) based on the archival XMM-Newton, Chandra, Swift, and Hubble Space Telescope (HST) observations. The source has a peak luminosity of L-X similar to 2 x 10(39) erg s(-1) in the XMM-Newton observation of 2004 June. Consideration of the hardness ratios and the spectral model parameters shows that the source seems to exhibit possible spectral variations throughout the X-ray observations. In...
RXTE-PCA observations of XMMU J054134.7-682550
İNAM, SITKI ÇAĞDAŞ; Townsend, L. J.; McBride, V. A.; Baykal, Altan; Coe, M. J.; Corbet, R. H. D. (Oxford University Press (OUP), 2009-05-21)
We analysed Rossi X-ray Timing Explorer Proportional Counter Array observations of a recent outburst of the X-ray pulsar XMMU J054134.7-682550. We calculated the pulse frequency history of the source. We found no sign of a binary companion. The source spins up when the X-ray flux is higher, with a correlation between the spin-up rate and X-ray flux, which may be interpreted as a sign of an accretion disc. On the other hand, the source was found to have an almost constant spin frequency when the X-ray flux i...
AKYÜZ, AYSUN; Kayaci, S.; Avdan, H.; Ozel, M. E.; SONBAŞ, EDA; Balman, Şölen (IOP Publishing, 2013-03-01)
We present the results of a study of non-nuclear discrete sources in a sample of three nearby spiral galaxies (NGC 4395, NGC 4736, and NGC 4258) based on XMM-Newton archival data supplemented with Chandra data for spectral and timing analyses. A total of 75 X-ray sources have been detected within the D-25 regions of the target galaxies. The large collecting area of XMM-Newton makes the statistics sufficient to obtain spectral fitting for 16 (about 20%) of these sources. Compiling the extensive archival expo...
Citation Formats
Y. Pekoen and Ş. Balman, “RR Pic (1925): A Chandra X-ray view,” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, pp. 921–926, 2008, Accessed: 00, 2020. [Online]. Available: https://hdl.handle.net/11511/57371.