The present work is devoted to the study of the supernova remnant and its neutron star XMMU J172054. 5-372652. The paper analyzes observations in 2009 and 2018, data for this system obtained by the Chandra x ray observatory. The analysis showed that the neutron star G350. 1-0. 3 with M = 1, 4 Msun, R = 13 MS, dist = 4, 5 KPC, the author also measured its temperature in two groups: the first group, including observations made in 2009, and the second group, including 5 observations made at different times of the year 2018.
In addition, in this work, the author studies all important aspects of the supernova remnants of G350. 1-0. 3, and obtain their spectra using the collided plasma, nonequilibrium, constant temperature (VNEI) model, which assumes a constant temperature and a single ionization parameter. It gives a characteristic of the spectrum, but is not a physical model, the author will precede the spectra obtained using this model.
ABSTRACT
The present work is devoted to the study of the supernova remnant and its neutron star XMMU J172054. 5-372652. The paper analyzes observations in 2009 and 2018, data for this system obtained by the Chandra x ray observatory. The analysis showed that the neutron star G350. 1-0. 3 with M = 1, 4 Msun, R = 13 MS, dist = 4, 5 KPC, we also measured its temperature in two groups: the first group, including observations made in 2009, and the second group, including 5 observations made at different times of the year 2018.
In addition, in this work, we study all important aspects of the supernova remnants of G350. 1-0. 3, and obtain their spectra using the collided plasma, nonequilibrium, constant temperature (VNEI) model, which assumes a constant temperature and a single ionization parameter. It gives a characteristic of the spectrum, but is not a physical model, we will precede the spectra obtained using this model.
Key words: X-rays: stars - neutrinos - stars: neutron - supernovae: individual (G350.1-0.3)
1 INTRODUCTION
Supernovae play an important role in modern astrophysics. They are vital for the chemical evolution of the universe, and are also one of the most important sources of energy for the interstellar medium. Part of this energy is in the form of cosmic rays, which have an energy density of 1-2 eV cm 1 in the Galaxy, which is thus about a third of the total energy density of the interstellar medium. Finally, supernovae, especially Type Ia supernovae, play a central role in modern cosmology, since their brightness allows them to be detected at high redshifts(Paolo & Heavens 2007). their use led to the recognition that the expansion of the universe is accelerating, not slowing down (Riess & Filippenko 2007).
G350. 1-0. 3 is a bright radio source in our Galaxy. Its linear polarization and non-thermal spectrum initially led to its classification as SNR (Canizares & Neighbours 1975), but the high-resolution image revealed a distorted and elongated morphology, very different from the shell structure usually observed in such sources.
It was later shown that G350. 1-0. 3 is a very young and bright SNR expanding into a dense surrounding gas. An associated neutron star has been discovered in it, which is probably an addition to the growing class of "central compact objects" (CCOs) in the remnants of supernovae.
Many supernova remnants (SNRs) expand into complex environments formed by molecular clouds and strong winds from OB associations. If our understanding of SNR is to progress, we must strive to identify and understand these complex systems.
The subject of the study is to obtain the spectra of observations of Chandra G350. 1-0.3, to analyze the models most suitable for their study, using the tools xspec, sherpa.
The aim of the work is to analyze the X-ray observations of the Chandra Observatory conducted in 2009-2018 and to choose a spectral model that best describes the spectrum of the CCO.
2 CHANDRAOBSERVATIONS
G350. 1-0. 3 is a supernova remnant located in the constellation Scorpio. It is located in the Milky Way and is possibly associated with a neutron star (XMMU J172054.5-372652) formed as a result of the same supernova explosion. Previously, this object was mistakenly classified as a distant galaxy (Witt A. 2002).
G350. 1-0. 3, a bright radio source inside the Milky Way, was initially identified by comparing observations from the Molonglo Observatory Synthesis Telescope and the Parks Radio Telescope and classified as a supernova remnant in publications in 1973 and 1975.
However, later higher-resolution images in the mid-80s revealed an unexpected irregular morphology that was significantly different from other sources of supernova remnants. Then it was claimed that G350. 1-0. 3 was a radio galaxy or galaxy cluster, which led to a reclassification, as a result of which the catalogs of supernova remnants downgraded the object to a "candidate for a supernova remnant" or completely excluded it; G350.1-0.3 was subsequently "forgotten"(Borkowski & Miltich 2020).
A study published in 2008 combined archived data and new images from the European Space Agency's XMM-Newton orbiting X-ray telescope to demonstrate that G350. 1-0.3 is a supernova remnant. The researchers determined that the strange shape of the object arose as a result of an explosion near a dense gas cloud, about 15,000 light-years from Earth, which prevented uniform expansion and led to its elongated shape.
The researchers also determined that the nearby thermal X-ray source XMMU J172054. 5-372652 is a central compact supernova object (Borkowski & Miltich 2020).
G350. 1-0. 3 is eight light-years across and about 900-1000 years old, making it one of the youngest and brightest supernova remnants in the Milky Way. It is unlikely that people would have seen a supernova explosion, because the intermediate interstellar dust would probably have prevented its observation from Earth.
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Fig 1. Supernova remnant G350. 1-0. 3 and neutron star XMMU J172054. 5372652
The Chandra X-Ray Observatory observed G350. 1-0.3 on May 21, 2009 and July 5, 2018. The total time of the two observations is 82.97 kps and 189.24 kps, respectively. More detailed information about individual observations can be seen in Table 1. The data is processed using chandra repro in CIAO 4.13, and the images are obtained using Ds9 provided by the Chandra X-ray center.
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Table 1. Chandra Observation for G350. 1-0. 3
The ACIS-S tool is designed for detecting spectra and worked in the standard mode and continuous data accumulation.
G350. 1-0. 3 was observed on May 21, 2009 at 05: 11: 23, and five segments in July 2018 for a total of 189. The average distance between the two epochs is 9.126 years. In all observations, G350.1-0.3 was placed on an advanced ACIS S3 CCD spectrometer that operated in the weak source mode.
Looking at the X-ray image of G350. 1-0. 3 taken in 2009, we see in Figure 2. there is practically no X-ray radiation to the West, and XMMU J172054.5-372652 is observed, which is our neutron star, our CCO. The intensity of X-rays is higher in the eastern region than in the Northern and Southern regions. XMMU J172054. 5-372652 is located in the western region, which is about 20 times weaker than the eastern one.
According to the results of the work (Borkowski &Miltich 2020), it can be said that some weaker areas have more or less sunny abundance. The proper motions of the expansion show that G350. 10.3 is eight light-years wide and about 600 years old, regardless of the distance. This is the third youngest known supernova remnant in the Galaxy and one of the most asymmetric.
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Fig 2. Chandra ACIS-S image taken in 2009. The energy range is 0.5-7.0 keV.
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Fig 3. Images of Chandra G350. 1-0. 3, on the left we see a supernova remnant in 2009, on the right we see a supernova remnant in 2018. The figures are not shown to the same scales along the flow.
Corresponding areas of motion analysis, using the maximum likelihood method. The arrows indicate the relative value of the 2D velocities and the direction of movement of the emissions.
Next, we will analyze the spectra of the selected areas, we can do this using specextract. To select the spectrum of the southern region, we use the manual and perform the processing as shown below.
(ciao-4.13) G350.1-0.3/10102/repro/Regionl$ pset specextract infile="acisfl0102_repro_evt2.fits[sky=region(src.reg)]"
(ciao-4.13) G350.1-0.3/10102/repro/Regionl$ pset specextract bkgfile="acisfl0102_repro_evt2.fits [sky=region(bkg.reg]]"
(ciao-4.13) G350.1-0.3/10102/repro/Regionl$ pset specextract outroot=10102
(ciao-4.13) Desktop/G350.1-0.3/10102/repro/Regionl$ pset specextract correctpsf=yes
(ciao-4.13) Desktop/G350.1-0.3/10102/repro/Regionl$ pset specextractweight=no
(ciao-4.13) Desktop/G350.1-0.3/10102/repro/Regionl$ specextract
Now we can get the spectrum using Sherpa as follows:
Sherpa 4.13.0
Python 3.8.2 (default, Mar 25 2020,17:03:02)
IPython profile: sherpa
Using matplotlib backend: Qt5Agg
sherpa In 1: load_pha("10102.pi")
sherpa In 2: plot_data()
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Fig 4. The spectrum of the northern region, we used the data process in specextract and Sherpa to obtain this spectrum.
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Fig 5. The spectrum of the Eastern A region.
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Figure 6. The spectrum of the Eastern B region.
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Figure 7. Spectrum of the Southern region.
After obtaining the spectra of the selected regions, we can conclude that the most intense spectra belong to the eastern regions, in addition, analyzing the spectra selected in 2009 and 2018.
3 DATA PROCESSINDG AND MODELS
In this chapter, we present an original result of analyzing the spectra of a Central Compact Object in the supernova remnant G350.1-0.3. Due to the fact that the supernova remnant is a young object, we can assume that the SSO may be cooling. To verify this, we analyzed Chandra's data for 2009 and 2018.
For the object of research G350. 1-0. 3, it was decided to use the data provided by the Chandra x-ray observatory, below we can see the steps necessary for selecting data, obtaining images of 2009 and 2018. To get the observations of Chandra, we must first have downloaded the files from the Chandra Data Archive. For our particular case G350. 1-0. 3, we find 6 observations (Table 1).
Let's continue downloading all 6 files to study, from the Ubuntu terminal, we need to open the files individually.
Conda is an open source package management system and environment management system that runs on Windows, macOS and Linux. Conda quickly installs, launches, and updates packages and their dependencies. Conda easily creates, saves, loads, and switches between environments on your local computer. It was created for Python programs, but it can package and distribute software for any language.
The Chandra_repro processing command automates the recommended data processing steps presented in the CIAO analysis streams. The command reads the primary data and creates a new bad pixel file, a new level=2 event file, and a new fits file. Chandra_repro can be used to re-process any ACIS and HRC images or grid data. For the 2009 and 2018 observations, we receive files after processing using chandra_repro, which will serve us to select the desired spectra.
After obtaining the spectra and analyzing the data process, now let's study 3 different spectral models for our neutron star, we will describe each model, and also look at the process in xspec, data input and the final result. The selected models are as follows:
- The XSPEC bbodyrad model: a blackbody spectrum, a normalized region.
- The XSPEC carbatm model: The non-magnetic carbon atmosphere of a neutron star.
- The XSPEC nsx model: a neutron star with a nonmagnetic atmosphere.
The carbatm model
Carbatm: The non-magnetic carbon atmosphere of a neutron star. The model provides the spectra emitted by the non-magnetic carbon atmosphere of a neutron star. The spectra of the model in the range from 0 to 20 keV of photon energy (displacement) are calculated in the grid of accelerations of the gravity of the surface log (g) = 13.7 - 14.9 (in CGS units) and effective temperatures T = 1 - 4 MK. For a given set of parameters, the gravity of the surface gy with a volume up to the Red gravitational z results in the mass M and radius R of the star. The test spectra are calculated by linear interpolation between the spectra of the nearest model in the T-log (g) grid and the boundaries of energy deposits. The number of photons in each container is divided by (1 + z).
Parameters:
- Effective temperature T (MK)
- Neutron star mass M
- Neutron star radius R (km)
- Normalization
- Of the source in units of 10 kpc, and A characterizes the fraction of the surface emitting radiation (A = 1 corresponds to the case when radiation comes from the entire surface).
XSPEC is a command-driven interactive program for approximating the X-ray spectrum, designed to be completely independent of the detector, so it can be used with any spectrometer. XSPEC was used to analyze data from HEAO- 1 A2, the Einstein Observatory, EXOSAT, Ginga, ROSAT, BBXRT, ASCA, CGRO, IUE, RXTE, Chandra, XMM- Newton, Integral / SPI, Fermi, Swift, Suzaku, NuSTAR, and Hitomi. Now there are more than 9300 articles in ADS that mention XSPEC.
Now, once the model is defined, and having hidden parameters, we can use the sxpec tool to get the model applied to our case, we choose the following:
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When setting up the carbatm model, it is necessary to fix the mass and radius of the neutron star, as well as the distance to it. In our case, this is M = 1.4 Msun, R = 13 km, dist = 4.5 KPC.
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Fig 8. Carbatm graph for a neutron star
[...]
- Quote paper
- Jose Alfredo Collazos Rozo (Author), 2021, X-Ray Studies of Radio-Silent Neutron Stars in the Remnants of Supernova Explosions, Munich, GRIN Verlag, https://www.hausarbeiten.de/document/1064418
