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8 results for โsupernova remnantsโ
First Study of the Supernova Remnant Population in the Large Magellanic Cloud with eROSITA
<p>Aims. The all-sky survey carried out by the extended Roentgen Survey with an Imaging Telescope Array (eROSITA) on board Spektrum-Roentgen-Gamma (Spektr-RG, SRG) has provided us with spatially and spectrally resolved X-ray data of the entire Large Magellanic Cloud (LMC) and its immediate surroundings in the soft X-ray band down to 0.2 keV with an average angular resolution</p> <p>of 26′′ in the field of view. In this work, we have studied the supernova remnants (SNRs) and candidates in the LMC using data from the first four all-sky surveys (eRASS:4). From the X-ray data in combination with results at other wavelengths, we obtain information about the SNRs, their progenitors, and the surrounding interstellar medium (ISM). The study of the entire population of SNRs in a galaxy helps us to understand the underlying stellar populations, the environments, in which the SNRs are evolving, and the stellar feedback on the ISM.</p> <p>Methods. The eROSITA telescopes are the best instruments currently available for the study of extended soft sources like SNRs in an entire galaxy due to their large field of view and high sensitivity in the softer part of the X-ray band. We applied the Gaussian gradient magnitude (GGM) filter to the eROSITA images of the LMC to highlight the edges of the shocked gas in order to find new SNRs. We visually compared the X-ray images with those of their optical and radio counterparts to investigate the true nature of the extended emission. The X-ray emission is evaluated using the contours with respect to the background, while for the optical we used line ratio</p> <p>diagnostics, and non-thermal emission in the radio images. We used the Magellanic Cloud Emission Line Survey (MCELS) for the optical data. For the radio comparison, we used data from the Australian Square Kilometre Array Pathfinder (ASKAP) survey of the LMC. Using the star formation history (SFH) derived from the near-IR photometry of the VISTA survey of the Magellanic Clouds (VMC) we have investigated the possible progenitor type of the new SNRs and SNR candidates in our sample. Results. We present the most updated catalogue of SNRs in the LMC. Previously known SNRs and candidates were detected with 1σ significance down to a surface brightness of Σ [0.2–5.0 keV] = 3.0 × 10−15 erg s−1 cm−2 arcmin−2 and were examined. The eROSITA data have allowed us to confirm one of the previous candidates as an SNR. We confirm three newly detected extended sources as new SNRs, while we propose 13 extended sources as new X-ray SNR candidates. We also present the analysis of the follow-up</p> <p>XMM-Newton observation of MCSNR J0456–6533 discovered with eROSITA. Among the new candidates, we propose J0614–7251 (4eRASSU J061438.1−725112) as the first X-ray SNR candidate in the outskirts of the LMC.</p>
spherical harmonics analysis of the wavefronts of a young supernova remnant
<p>This repository complements the upcoming ApJ paper "From supernova to supernova remnant: comparison of thermonuclear explosion models". The plots represent the surface of the three wavefronts of a young SNR: CD = contact discontinuity (edge of the ejecta), RS = reverse shock, FS = forward shock (outer blast wave). Radial fluctuations from the explosion center are mapped in spherical projection, and expanded in spherical harmonics to obtain the power spectrum = distribution of angular scales. Four supernova models are compared: N100ddt, N5ddt, N100def, N5def. The repository contains 3 folders: </p> <ul> <li><strong>maps_spectra</strong> (64 files, 16 MB) contains all the plots for the 4 models, for 4 fields: CD, FS, RS, FS-RS, as a function of time: as movies from 1 yr to 500 yr, and as snapshots at 3 selected times 1 yr, 100 yr, 500 yr.</li> <li><strong>SH_expansion</strong> (1059 files, 310 MB) contains a pedagogical example of the full expansion in spherical harmonics, for one map: the CD of N100ddt at 1 yr. It includes the basis functions Y๐๐ up to ๐=16 for each ๐, the individual components of the expansion up to ๐max=383, and the progressively reconstructed signal at each ๐.</li> <li><strong>SH_residuals</strong> (192 files, 90 MB) contains all the residuals plots to assess the quality of the reconstruction, for the 4 models, for the 4 fields, as a function of time.</li> </ul>
Einstein Observatory - Supernova Remnant Images
<p>This archive contains 72 Supernova Remnant Images from the Einstein Observatory (from Seward, F.D. 1990, ApJS 73, 781). einstein__supernova_remnant_descriptions.csv contains descriptions of each image. This file uses a pipe (|) as the delimiter.</p> <p>From https://www.cfa.harvard.edu/about/history/einstein/:</p> <p>The Einstein Observatory (High Energy Astronomical Observatory 2, HEAO-2; known as HEAO-B prior to launch) was a pioneering space astronomy mission which flew from 1978 to 1981. It was the first imaging X-ray telescope in orbit to be used for extrasolar astronomy, following the success of the Skylab solar X-ray telescope. Together with IUE, it was one of the first NASA missions with a guest observer program, helping create today's broad community of space scientists. The HEAO-B X-ray telescope was designed by SAO's Leon van Speybroeck, and the mission was conceived by Riccardo Giacconi and operated by the former American Science and Engineering group at CfA in collaboration with the managing NASA center, Marshall Space Flight Center in Huntsville, Alabama.</p> <p>We hope to put historical materials from the HEAO-2/Einstein mission in this area. To start off with, we have digitized the Einstein Slide Collection, used for talks and presentations by Einstein staff during and after the mission. Early results, with some exceptions, are in the first slides. Most captions accurately describe content of the slide. Some do not. We have corrected obvious problems but a few captions remain mysterious. You are welcome to browse or extract and use any of these images. Be aware that large color images (made by photographing a monitor display) are sometimes distorted. Also, the digitization was a batch job and the focus and/or exposure was sometimes not optimum. Many of the black and white slides were dirty or damaged. Most of the original slides are available from the SAO High Energy Division and for presentation or publication some could be greatly improved by cleaning and redigitization.</p> <p>A set was made for the Smithsonian institution and is included here as E672-E730. These make a nice presentation of Einstein results for several classes of objects and are all very good reproductions. As an extension of this, later results can be found in slides E860, E887-E894, E899-E905, E919, and E1081. First Light for the Observatory is in E778.</p> <p>Acknowledgements: Digital materials were prepared by Alaalden Ibrahim and Jonathan McDowell. Fred Seward has checked the collection and would be pleased to discuss any problems found in the slide labels.</p>
Reproduction package for the paper "Completing the X-ray view of the recently discovered supernova remnant G54.41+0.03"
<p>This is a basic reproduction package for the paper "Completing the X-ray view of the recently discovered supernova remnant G54.41+0.03" by V. Domฤek et al. (2021). It provides raw, intermediate and final data sets, including figures and scripts to allow the reproduction of the work performed in this paper. It also lists software used and data archives containing the public observational data. </p> <p>An open access version of the paper can be found at https://arxiv.org/abs/</p>
Positive and Negative Feedback from the Supernova remnant IC443: first results from SHREC
<p>Supernova remnants (SNRs) drive large-scale shocks that locally enhance the density of the surrounding material but also inject vast amounts of energy and momentum that largely perturb and disperse the Interstellar Medium (ISM). The interplay between these two effects is considered paramount in regulating the star formation efficiency in galaxies. However, how SNRs affect the conditions of density and temperature of the ISM is not well constrained from an observational point of view. In this poster, I present our exploratory large single-dish observing program SHREC, aimed to observe the molecular shock tracer SiO(2-1) toward a sample of โ30 SNRs known to be interacting with molecular clouds. I introduce the aim and technical aspects of SHREC and present the first results obtained toward the SNRs IC443. IC443 is a well known SNR, expanding into and interacting with a nearby toroidal molecular cloud. Toward the major site of interaction, known as clump G, we estimate the mass of the shocked gas to be 100 Msun. The shock driven by IC443 into this material enhances its density by a factor >10, to value consistent with those required to ignite star formation. Finally, we estimate that between 35-50% of the momentum injected by IC443 is transferred to the nearby molecular material. Our work therefore indicates that the molecular ISM is an important carrier of the SNR momentum and that the SNR-molecular cloud interaction play a crucial role in the regulating star formation in galaxies.</p>
Animations for "Remnants of Subdwarf Helium Donor Stars Ejected from Close Binaries with Thermonuclear Supernovae"
<p>Movies showing time evolution of the density in the z=0 plane for each of the seven Athena++ models in the paper. Each movie file corresponds to one model, labeled according to donor model number and the kinetic energy of the explosion in units of 10<sup>51</sup> ergs.</p>
Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog
A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees <= galactic longitude l_II <= 355 degrees, galactic latitude |b_II| <~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR. This table was created by the HEASARC in March 2007 based on the CDS table J/A+AS/118/329, file msc.dat. This is a service provided by NASA HEASARC .
M 33 XMM-Newton Supernova Remnants Catalog
The authors of this catalog carried out a study of the X-ray properties of the supernova remnant (SNR) population in M 33 with XMM-Newton, comprising deep observations of eight fields in M 33 covering all of the area within the D<sub>25</sub> contours, and with a typical luminosity of 7.1 x 10<sup>34</sup> erg/s (0.2-2.0keV). With their deep observations and large field of view they have detected 105 SNRs at the 3-sigma level, of which 54 SNRs are newly detected in X-rays, and three are newly discovered SNRs. Combining XMM-Newton data with deep Chandra survey data allowed detailed spectral fitting of 15 SNRs, for which they have measured temperatures, ionization time-scales and individual abundances. This large sample of SNRs allowed the authors to construct an X-ray luminosity function, and compare its shape to luminosity functions from host galaxies of differing metallicities and star formation rates to look for environmental effects on SNR properties. They concluded that while metallicity may play a role in SNR population characteristics, differing star formation histories on short time-scales, and small-scale environmental effects appear to cause more significant differences between X-ray luminosity distributions. In addition, they analyze the X-ray detectability of SNRs, and find that in M 33 SNRs with higher [SII]/H-alpha ratios, as well as those with smaller galactocentric distances, are more detectable in X-rays. This catalog utilized data from a deep survey of M 33 using an 8 field XMM-Newton mosaic that extends out to the D25 isophote. The point source catalog from this survey was published by W15 (Williams+2015, J/ApJS/218/9). In addition to the catalog of W15, the authors utilized high-resolution observations from the Chandra ACIS Survey of M 33 (ChASeM33, Tullmann+2011, J/ApJS/193/31) for the purposes of obtaining X-ray spectral fits. This table was ingested by the HEASARC in October 2019 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/472/308">CDS Catalog J/MNRAS/472/308</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
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