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Suzaku study on the Ejecta of the Supernova Remnant G272.2$-$3.2  [PDF]
Fumiyoshi Kamitsukasa,Katsuji Koyama,Hiroshi Nakajima,Kiyoshi Hayashida,Koji Mori,Satoru Katsuda,Hiroyuki Uchida,Hiroshi Tsunemi
Physics , 2015, DOI: 10.1093/pasj/psv114
Abstract: We report re-analyses of the Suzaku observations of the Galactic supernova remnant (SNR), G272.2$-$3.2, for which the previous studies were limited below 3 keV. With careful data reduction and background subtraction, we discover the K-shell lines of Ar, Ca, and Fe above 3 keV. The X-ray spectrum of G272.2$-$3.2 consists of two components, a low-temperature collisional ionization equilibrium (CIE) plasma ($kT_{\rm e} \sim 0.2$ keV) and a high-temperature non-equilibrium ionization (NEI) plasma ($kT_{\rm e} = 0.6$-$3$ keV). The CIE plasma has solar abundances over the entire area, hence it would originate from the interstellar medium. On the other hand, the abundances of the NEI plasma increase toward the inner region, suggesting the ejecta origin. The line center energy of the Fe K-shell emission ($\sim 6.4$ keV) suggests that the ejecta are recently heated by the reverse shock, a common feature in Type Ia SNRs.
A New ASCA and ROSAT Study of the Supernova Remnant: G272.2-3.2  [PDF]
I. M. Harrus,P. O. Slane,R. Smith,J. P. Hughes
Physics , 2001, DOI: 10.1086/320577
Abstract: G272.2-3.2 is a supernova remnant (SNR) characterized by an apparent centrally brightened X-ray morphology and thermally dominated X-ray emission. Because of this combination of Sedov-type (thermal emission) and non-Sedov type (non-shell like morphology) features, the remnant is classified as a ``thermal composite'' SNR. This class of remnant is still poorly understood due in part to the difficulties in modeling accurately all the physical conditions which shape the emission morphology. In this paper we present a combined analysis of data from the ASCA and ROSAT satellites coupled with previous results at other wavelengths. We find that the X-ray emission from G272.2-3.2 is best described by a non-equilibrium ionization (NEI) model with a temperature around 0.70 keV, an ionization timescale of 3200 cm^-3 yr and a relatively high column density (NH about 10^22 atoms/cm^2). We look into the possible explanations for the apparent morphology of G272.2-3.2 using several models (among which both cloud evaporation and thermal conduction models). For each of the models considered we examine all the implications on the evolution of G272.2-3.2.
XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region  [PDF]
E. Sánchez-Ayaso,J. A. Combi,F. Bocchino,J. F. Albacete-Colombo,J. López-Santiago,J. Martí,E. Castro
Physics , 2013, DOI: 10.1051/0004-6361/201219709
Abstract: We aim to study the spatial distribution of the physical and chemical properties of the X-ray emitting plasma of the supernova remnant G272.2-3.2, in order to get important constraints on its ionization stage, on the progenitor supernova explosion, and the age of the remnant. We report combined XMM-Newton and Chandra images, median photon energy map, silicon and sulfur equivalent width maps, and a spatially resolved spectral analysis for a set of regions of the remnant. Complementary radio and H{\alpha} observations, available in the literature, are also used to study the multi-wavelength connection of all detected emissions. The X-ray morphology of the remnant displays an overall structure with an almost circular appearance, a centrally brightened hard region, with a peculiar elongated hard structure oriented along the northwest-southeast direction of the central part. The X-ray spectral study of the regions shows distinct K{\alpha} emission-line features of metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by an absorbed VNEI thermal plasma model, which produces elevated abundances of Si, S, and Fe in the circular central region, typical of ejecta material. The values of abundances found in the central region of the SNR favor a Type Ia progenitor for this remnant. The outer region shows abundances below the solar value, as expected if the emission arises from the shocked ISM. The relatively low ionization timescales suggests non-equilibrium ionization. We identify the location of the contact discontinuity. Its distance to the outer shock is higher than expected for expansion in a uniform media, what suggests that the remnant spent most of its time in a more dense medium.
G272.2--3.2: A centrally filled and possibly young SNR discovered by ROSAT  [PDF]
J. Greiner,R. Egger,B. Aschenbach
Physics , 1994,
Abstract: We report the discovery of a new SNR in the \ros All-Sky-Survey data. The SNR has a nearly circular shape with a diameter of about 15 arcmin. The surface brightness is rather uniform over the remnant. The observed interstellar absorption suggests a distance of about 1.8$^{+1.4}_{-0.8}$ kpc. The X-ray emission appears to be of thermal origin with a plasma temperature of about 10$^7$ K. The Sedov model leads to an age of only 1800 years. We find no spectral evidence of non-thermal emission in the center of the remnant. The two most likely explanations for the centrally filled structure are evaporation of shock heated clouds in the interior of the remnant or a reverse shock heating the ejecta of the SNR explosion.
Multi-wavelength analysis of the Galactic supernova remnant MSH 11-61A  [PDF]
Katie Auchettl,Patrick Slane,Daniel Castro,Adam R. Foster,Randall K. Smith
Physics , 2015, DOI: 10.1088/0004-637X/810/1/43
Abstract: Due to its centrally bright X-ray morphology and limb brightened radio profile, MSH 11-61A (G290.1-0.8) is classified as a mixed morphology supernova remnant (SNR). H$\textsc{i}$ and CO observations determined that the SNR is interacting with molecular clouds found toward the north and southwest regions of the remnant. In this paper we report on the detection of $\gamma$-ray emission coincident with MSH 11-61A, using 70 months of data from the Large Area Telescope on board the \textit{Fermi Gamma-ray Space Telescope}. To investigate the origin of this emission, we perform broadband modelling of its non-thermal emission considering both leptonic and hadronic cases and concluding that the $\gamma$-ray emission is most likely hadronic in nature. Additionally we present our analysis of a 111 ks archival \textit{Suzaku} observation of this remnant. Our investigation shows that the X-ray emission from MSH 11-61A arises from shock-heated ejecta with the bulk of the X-ray emission arising from a recombining plasma, while the emission towards the east arises from an ionising plasma.
X-ray Emission from the Galactic Supernova Remnant G272.2-3.2  [PDF]
Randall L. McEntaffer,Nolan Grieves,Thomas Brantseg
Physics , 2013,
Abstract: We present analysis of Chandra X-ray Observatory data detailing a galactic supernova remnant, G272.2-3.2. A clear shell of emission has been resolved for the first time as a series of filaments and knots around the entire rim of the remnant. Spectral analysis of these features show that they are consistent with shock heating of interstellar material in a clumpy medium. Spatially separated from this shell we see a central diffuse region dominated by harder, hotter emission. Spatial spectroscopy shows a clear enhancement of metals consistent with a Type Ia explosion, namely S, Si, and Fe. We find no clear evidence for a compact object or pulsar wind nebula and argue for a Type Ia origin. Consideration of the ionization timescales suggest an age of 8700 years for G272.2-3.2.
On identities in centrally nilpotent Moufang loops and centrally nilpotent A-loops  [PDF]
N. I. Sandu
Mathematics , 2014,
Abstract: This paper proves that the variety generated by a centrally nilpotent Moufang loop (or centrally nilpotent A-loop) is finitely based.
Some Centrally Symmetric Manifolds  [PDF]
Dipendu Maity,Ashish Kumar Upadhyay
Mathematics , 2014,
Abstract: We show existence of centrally symmetric maps on surfaces all of whose faces are quadrangles and pentagons for each orientable genus $g \geq 0$. We also show existence of centrally symmetric maps on surfaces all of whose faces are hexagons for each orientable genus $g = 2k-1$, $k\in \mathbb{N}$. We enumerate centrally symmetric triangulated manifolds of dimensions 2 and 3 with few vertices.
Investigation of CTA 1 with Suzaku Observation  [PDF]
Lupin C. C. Lin,Jumpei Takata,Albert K. H. Kong,C. Y. Hui,Teruaki Enoto,H. K. Chang,Regina H. H. Huang,J. S. Liang,Shinpei Shibata,C. Y. Hwang
Physics , 2012, DOI: 10.1111/j.1365-2966.2012.21832.x
Abstract: We report on an 105 ks Suzaku observation of the supernova remnant CTA 1 (G119.5+10.2). The Suzaku soft X-ray observation was carried out with both timing mode and imaging mode. A ~ 10' extended feature, which is interpreted as a bow-shock component of the pulsar wind nebula (PWN), is revealed in this deep observation for the first time. The nebular spectrum can be modelled by a power-law with a photon index of ~ 1.8 which suggests a slow synchrotron cooling scenario. The photon index is approximately constant across this extended feature. We compare and discuss our observations of this complex nebula with previous X-ray investigations. We do not obtain any significant pulsation from the central pulsar in the soft (0.2-12 keV) and hard (10-60 keV) X-ray data. The non-detection is mainly due to the loss of the precise imaging ability to accurately determine the source contribution. The spectra of XIS and HXD can be directly connected without a significant spectral break according to our analysis. Future observations of NuSTAR and Astro-H would be able to resolve the contamination and provide an accurate hard X-ray measurement of CTA 1.
Centrally symmetric configurations of integer matrices  [PDF]
Hidefumi Ohsugi,Takayuki Hibi
Mathematics , 2011, DOI: 10.1215/00277630-2857555
Abstract: The concept of centrally symmetric configurations of integer matrices is introduced. We study the problem when the toric ring of a centrally symmetric configuration is normal as well as is Gorenstein. In addition, Gr\"obner bases of toric ideals of centrally symmetric configurations will be discussed. Special attentions will be given to centrally symmetric configurations of unimodular matrices and those of incidence matrices of finite graphs.
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