Discovery of X-rays from the supernova remnant G0.9+0.1 (original) (raw)
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2004
G266.2 1.2 (RX J0852.0 4622) is a member of the emerging class of Galactic supernova remnants (SNRs) which feature X-ray spectra dominated by non-thermal emission. This X-ray emission is believed to be synchrotron radiation produced by cosmic-ray electrons accelerated to TeV energies along the expanding shock fronts of SNRs. To explore this phenomenon of high energy X-ray emission from SNRs in more detail, we are conducting a broadband X-ray study of these sources using both new and archived observations. To illustrate this work, we present the results of our two observations made with Chandra (with a total effective exposure time of 73972 seconds) of the luminous northwestern rim of G266.2 1.2: this observation has revealed for the first time fine X-ray structure in this rim. A satisfactory fit to the spectrum of a sharply defined leading shock is derived using a power law model with a photon index = 2.41 0.06. Alternatively, this spectrum can be fit with the SRCUT model which lead...
An X-Ray Point Source and Synchrotron Nebula Candidate in the Supernova Remnant G292.0+1.8
2001
We present archival data from the Chandra X-Ray Observatory that reveal a bright point source to the southeast of the center of the young supernova remnant G292.0+1.8 that is coincident with the peak of highest radio surface brightness. The mostly featureless spectrum of the point source at coordinates (J2000) RA = 11 24 39.2, DEC = -59 16 19.8 is well fit by a three-parameter absorbed model with one power-law and two blackbody components. We also argue that the neutron star is surrounded by a synchrotron wind nebula based off of the source's hard emission and high radio and X-ray luminosities, each corresponding to a canonical wind nebula spin-down power, dE/dt ~ 10^36 erg/s.
The Astrophysical Journal, 2010
We present a detailed spatially-resolved spectroscopic analysis of two Xray observations (with a total integration time of 73280 seconds) made of the luminous northwestern rim complex of the Galactic supernova remnant (SNR) G266.2−1.2 (RX J0852.0−4622) with the Chandra X-ray Observatory. G266.2−1.2 is a member of a class of Galactic SNRs which feature X-ray spectra dominated by non-thermal emission: in the cases of these SNRs, the emission is believed to have a synchrotron origin and studies of the X-ray spectra of these SNRs can lend insights into how SNRs accelerate cosmic-ray particles. The Chandra observations have clearly revealed fine structure in this rim complex (including a remarkably well-defined leading shock) and the spectra of these features are dominated by non-thermal emission. We have measured the length scales of the upstream structures at eight positions along the rim and derive lengths of 0.02-0.08 pc (assuming a distance of 750 pc to G266.2−1.2). We have also extracted spectra from seven regions in the rim complex (as sampled by the ACIS-S2, -S3
Radio-continuum emission from the young galactic supernova remnant G1.9+0.3
Serbian Astronomical Journal, 2014
We present an analysis of a new Australia Telescope Compact Array (ATCA) radio-continuum observation of supernova remnant (SNR) G1.9+0.3, which at an age of ~181?25 years is the youngest known in the Galaxy. We analysed all available radio-continuum observations at 6-cm from the ATCA and Very Large Array. Using this data we estimate an expansion rate for G1.9+0.3 of 0.563%?0.078% per year between 1984 and 2009. We note that in the 1980's G1.9+0.3 expanded somewhat slower (0.484% per year) than more recently (0.641% per year). We estimate that the average spectral index between 20-cm and 6-cm, across the entire SNR is ?={0.72?0.26 which is typical for younger SNRs. At 6-cm, we detect an average of 6% fractionally polarised radio emission with a peak of 17%?3%. The polarised emission follows the contours of the strongest of X-ray emission. Using the new equipartition formula we estimate a magnetic field strength of B?273?G, which to date, is one of the highest magnetic field stren...
Discovery of thermal X-ray emission in the supernova remnant G337.8-0.1 (Kes 41)
Astronomy and Astrophysics, 2008
Aims. We report here on the first detection at X-ray wavelengths of the Supernova Remnant (SNR) G337.8−0.1, carried out with the XMM-Newton Observatory. Methods. Using the X-ray observations, we studied the X-ray morphology of the remnant at different energy ranges, analysed the spectral properties and investigated a possible variable behavior. Results. The SNR shows a diffuse filled-center structure in the X-ray region with an absence of a compact source in its center. We find a high column density of N H > 6.9×10 22 cm −2 , which supports a relatively distant location (d ≥ 7 kpc). The X-ray spectrum exhibits emission lines, indicating that the X-ray emission has a thin thermal plasma origin, and is well represented by a non-equilibrium ionization (NEI) plasma model. The X-ray characteristics and well-known radio parameters show that G337.8−0.1 belongs to the emerging class of mixed-morphology (MM) SNRs.
The Astrophysical Journal, 2001
PSR J1119−6127 is a recently discovered 1700-year-old radio pulsar that has a very high inferred surface dipolar magnetic field. We present a detailed analysis of a pointed ASCA observation and archival ROSAT data of PSR J1119−6127 and its surroundings. Both data sets reveal extended emission coincident with the newlydiscovered radio supernova remnant G292.2-0.5, reported in a companion paper by Crawford et al. A hard point source, offset ∼1. ′ 5 from the position of the radio pulsar, is seen with the ASCA GIS. No pulsations are detected at the radio period with a pulsed fraction upper limit of 61% (95% confidence). The limited statistics prevent a detailed spectral analysis, although a power-law model with photon index Γ ≈ 1 − 2 describes the data well. Both the spectral model and derived X-ray luminosity are consistent with those measured for other young radio pulsars, although the spatial offset renders an identification of the source as the X-ray counterpart of the pulsar uncertain.
High resolution radio study of the pulsar wind nebula within the supernova remnant G0.9+0.1
Astronomy and Astrophysics, 2008
Aims. We have conducted a study in radio wavelengths and in X-rays of the pulsar wind nebula (PWN) in the supernova remnant (SNR) G0.9+0.1 with the goal of investigating in detail its morphology and to accurately determine its characteristic parameters. Method. To carry out this research we have observed the PWN at λ 3.6 and 6 cm using the Australia Telescope Compact Array (ATCA) and combined these data with existing multiconfiguration VLA data and single dish observations in order to recover information at all spatial scales. We have also reprocessed VLA archival data at λ 20 cm. From all these observational data we have produced high-fidelity images at the three radio frequencies with angular resolution better than 3 ′′ . The radio data were compared to X-ray data obtained with Chandra and in two different observing runs with XMM-Newton. Results. The new observations revealed that the morphology and symmetry suggested by Chandra observations (torus and jet-like features) are basically preserved in the radio range in spite of the rich structure observed in the radio emission of this PWN, including several arcs, bright knots, extensions and filaments. The reprocessed X-ray images show for the first time that the X-ray plasma fills almost the same volume as the radio PWN.
The Astrophysical Journal, 2005
We present the discovery of non-thermal radio and X-ray emission positionally coincident with the TeV γray source HESS J1813-178. We demonstrate that the non-thermal radio emission is due to a young shell-type supernova remnant (SNR) G12.8-0.0, and constrain its distance to be greater than 4 kpc. The X-ray emission is primarily non-thermal and is consistent with either an SNR shell or unidentified pulsar/pulsar wind nebula origin; pulsed emission is not detected in archival ASCA data. A simple synchrotron+inverse Compton model for the broadband emission assuming that all of the emission arises from the SNR shell implies maximum energies of (30 − 450)(B/10µ G) −0.5 TeV. Further observations are needed to confirm that the broadband emission has a common origin and better constrain the X-ray spectrum. Subject headings: acceleration of particles -supernova remnants -radio:ISM -Xrays:ISM -ISM: individual (G12.8-0.0, HESS J1813-178)
G337.2+0.1: A new X-ray supernova remnant?
Astronomy and Astrophysics, 2005
We present evidence supporting a SNR origin for the radio source G337.2+0.1, which was discovered along the line of sight to the Norma spiral arm in the MOST 843-MHz radio survey. The radio source is spatially superposed to the unidentified ASCA source AX J1635.9-4719. An analysis of this latter source reveals that its X-ray spectrum, extended nature, and non-variable flux are consistent with what is expected for a SNR. In addition, we have used HI-line observations of the region to look for any effect of the presumed remnant on the ISM. We have found a well-defined minimum centered at the position of the radio source in the velocity range of ∼ −25 to −19 km s −1 . This feature appears as a sharp absorption dip in the spectrum that might be produced when the continuum emission from the SNR candidate is absorbed by foreground gas. Hence we have used it to constrain the distance to the source, which seems to be a young (age ∼ a few 10 3 yr) and distant (d ∼ 14 kpc) SNR. G337.2+0.1 and AX J1635.9-4719 would be the radio/X-ray manifestations of this remnant.
The X-Ray Properties of Five Galactic Supernova Remnants Detected by the Spitzer Glimpse Survey
The Astronomical Journal, 2014
We present a study of the X-ray properties of five Galactic supernova remnants (SNRs)-Kes 17 (G304.6+0.1), G311.5−0.3, G346.6−0.2, CTB 37A (G348.5+0.1) and G348.5−0.0-that were detected in the infrared by Reach et al. (2006) in an analysis of data from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) that was conducted by the Spitzer Space Telescope. We present and analyze archival ASCA observations of Kes 17, G311.5−0.3 and G346.6−0.2, archival XMM-Newton observations of Kes 17, CTB 37A and-2-G348.5−0.0 and an archival Chandra observation of CTB 37A. All of the SNRs are clearly detected in the X-ray possibly except for G348.5−0.0. Our study reveals that the four detected SNRs all feature center-filled X-ray morphologies and that the observed emission from these sources is thermal in all cases. We argue that these SNRs should be classified as mixed-morphology SNRs (MM SNRs): our study strengthens the correlation between MM SNRs and SNRs interacting with molecular clouds and suggests that the origin of mixed-morphology SNRs may be due to the interactions between these SNRs and adjacent clouds. Our ASCA analysis of G311.5−0.3 reveals for the first time X-ray emission from this SNR: the X-ray emission is center-filled within the radio and infrared shells and thermal in nature (kT ∼ 0.98 keV), thus motivating its classification as an MM SNR. We find considerable spectral variations in the properties associated with the plasmas of the other X-ray-detected SNRs, such as a possible overabundance of magnesium in the plasma of Kes 17. Our new results also include the first detailed spatially-resolved spectroscopic study of CTB 37A using Chandra as well as a spectroscopic study of the discrete X-ray source CXOU J171428.5−383601, which may be a neutron star associated with CTB 37A. Finally, we also estimate such properties as electron density n e , radiative age t rad and swept-up mass M X for each of the four X-ray-detected SNRs. Each of these values are comparable to archetypal mixed-morphology SNRs like 3C 391 and W44. In an analysis of the spectrum of Kes 17, we did not find evidence of over-ionization unlike other archetypal mixed-morphology SNRs like W28 and W44.