Locating the TeV gamma-rays from the shell regions of Cassiopeia A

Download

index.pdf

Date

2014-01-01

Author

Saha, Lab
Ergin, Tülün
Majumdar, Pratik
Bozkurt, Mustafa

Metadata

Show full item record

This work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.

Item Usage Stats

146
views

0
downloads

We have analyzed Chandra X-ray data from different parts of the shell of young supernova remnant (SNR) in the energy range of 0.7 - 8 keV. We observed that X-ray flux level varies over different shell regions of the source. Implications of X-ray observation will be discussed here. We also analyzed Fermi-LAT data in the energy range 0.5 - 50 GeV for the source. The differential spectrum obtained in this way fits with simple power-law. We also present here multi-wavelength modeling of the source considering archival radio and TeV data along with Chandra and Fermi-LAT data.

Subject Keywords

Cassiopeia A, X-rays, Observations

URI

https://hdl.handle.net/11511/32851

DOI

https://doi.org/10.1017/s1743921313009927

Collections

Department of Physics, Conference / Seminar

Suggestions

OpenMETU
Core

Recent Spin Rate Measurements of 4U 1907+09 Sahiner, S.; İNAM, SITKI ÇAĞDAŞ; Baykal, Altan (2010-08-06) In this study, X-ray spectral and pulse timing analysis of the high mass X-ray binary (HMXB) pulsar 4U 1907+09, based on the observations with RXTE are presented. Spin rate measurements indicate a new spin-down episode with a rate close to the previous steady spin-down rate. Orbital phase resolved spectroscopy reveals that the Hydrogen column density varies through the orbit reaching to its maximum value just after periastron. A slight spectral softening with increasing luminosity is aslo observed.
X-ray and optical observations of high mass x-ray binaries Beklen, Elif; Baykal, Altan; İnam, Çağdaş; Department of Physics (2010) In this thesis, X-ray and optical observations of accretion powered pulsars are presented. By using archival RXTE observations we work on the X-ray spectral and pulse timing analysis of 4U 1538-52, 4U 1907+09, SMC X-1 to have more detailed information about their orbital and spin parameters. For 4U 1538-52 and SMC X-1, we determined new orbital epochs. By using long term pulse history of 4U 1907+09, we were able to work spin-down trend of the system and also calculate the change in the spin-down rate. Using...
Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9 Sezer, A.; Ergin, Tülün; Yamazaki, R.; Sano, H.; Fukui, Y. (2019-11-01) We present the results from the Suzaku X-ray Imaging Spectrometer observation of the mixed-morphology supernova remnant (SNR) HB9 (G160.9+2.6). We discovered recombining plasma (RP) in the western Suzaku observation region and the spectra here are well described by a model having collisional ionization equilibrium (CIE) and RP components. On the other hand, the X-ray spectra from the eastern Suzaku observation region are best reproduced by the CIE and non-equilibrium ionization model. We discuss possible sc...
Investigating the region of 3C 397 in High Energy Gamma rays Bhattacharjee, Pooja; Majumdar, Pratik; Ergin, Tülün; Saha, Lab; Joarder, Partha S. (2017-02-24) We investigate the supernova remnant (SNR) 3C 397 and its neighboring pulsar PSR J1906+0722 in high energy gamma rays by using nearly six years of archival data of Large Area Telescope on board Fermi Gamma Ray Space Telescope (Fermi-LAT). The off-pulse analysis of gamma-ray flux from the location of PSR J1906+0722 reveals an excess emission which is found to be very close to the radio location of 3C 397. Here, we present the preliminary results of this gamma-ray analysis of 3C 397 and PSR J1906+0722.
DETECTION OF EXTENDED VHE GAMMA RAY EMISSION FROM G106.3+2.7 WITH VERITAS Acciari, V. A.; et. al. (IOP Publishing, 2009-09-20) We report the detection of very-high-energy (VHE) gamma-ray emission from supernova remnant (SNR) G106.3+2.7. Observations performed in 2008 with the VERITAS atmospheric Cherenkov gamma-ray telescope resolve extended emission overlapping the elongated radio SNR. The 7.3 sigma (pre-trials) detection has a full angular extent of roughly 0 degrees.6 by 0 degrees.4. Most notably, the centroid of the VHE emission is centered near the peak of the coincident (CO)-C-12 (J = 1-0) emission, 0 degrees.4 away from the ...

Citation Formats

L. Saha, T. Ergin, P. Majumdar, and M. Bozkurt, “Locating the TeV gamma-rays from the shell regions of Cassiopeia A,” 2014, vol. 9, Accessed: 00, 2020. [Online]. Available: https://hdl.handle.net/11511/32851.