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3 edition of Absorption of the X-ray background by the Large Magellanic Cloud found in the catalog.

Absorption of the X-ray background by the Large Magellanic Cloud

Absorption of the X-ray background by the Large Magellanic Cloud

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Absorption spectra.,
  • X-ray spectroscopy.

  • Edition Notes

    StatementThomas T. Hamilton.
    SeriesNASA contractor report -- NASA CR-189462.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL18060300M

    We present Suzaku spectra of X-ray emission in the fields just off the LMC X-3 sight line. O VII, O VIII, and Ne IX emission lines are clearly detected, suggesting the presence of an optically thin thermal plasma with an average temperature of × K. This temperature is significantly higher than that inferred from existing X-ray absorption line data obtained with Chandra grating. M. Orio et al.: A transient supersoft X-ray source in the Large Magellanic Cloud L3 Table 1. The ROSAT PSPC count rate. The distance from the center of the detector, the lowest blackbody temperature with Lbol = ergs/s and the highest blackbody temperature and lowest bolometric luminosity in ergs/s admitted at the 2 ˙ con dence level.

    2. Information for the supernova remnants listed in number 1(a through e) in the Extensions Section. OBS ID (W49B) - Type II; though hard to tell from the spectrum perhaps due to interstellar absorption of lines less than keV (so you can't see O, Me and Mg lines). From this spectrum it is very difficult to classify the supernova type. Catalogue of Be/X-ray binary systems in the Small Magellanic Cloud: X-ray, optical & IR properties M. J. Coe & J. Kirk Physics and Astronomy, University of Southampton, SO17 1BJ, UK. June 3 ABSTRACT This is a catalogue of ∼70 X-ray emitting binary systems in the Small Magellanic.

      The Large Magellanic Cloud (LMC) is a dwarf irregular galaxy located on the border between the constellations Dorado and Mensa. The galaxy is believed to be a satellite of the Milky Way and a member of the Local Group of galaxies, which includes about 30 galaxies that are loosely bound together by their gravitation. Absorption spectroscopy can be used to detect diffuse gas between the observer and a bright background object. Each cloud of diffuse gas shows up as a narrow absorption line in the spectrum of the background object and, thanks to the expansion of the universe, the redshift of each absorber corresponds to its distance from us.


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Absorption of the X-ray background by the Large Magellanic Cloud Download PDF EPUB FB2

Get this from a library. Absorption of the X-ray background by the Large Magellanic Cloud. [Thomas T Hamilton; United States. National Aeronautics and Space Administration.].

Soft x ray flux of extragalactic origin should be partially absorbed during passage through the Large Magellanic Cloud. Past attempts to measure this absorption have been frustrated by the LMC's intrinsic x ray emission. New calibration techniques were developed to enable precise (within 5 pct.) measurement of the flux and spectrum of diffuse x rays detected by the Einstein Observatory : Thomas T.

Hamilton. Absorption of the x ray background by the large magellanic cloud. By Thomas T. Hamilton. Abstract. Soft x ray flux of extragalactic origin should be partially absorbed during passage through the Large Magellanic Cloud.

Past attempts to measure this absorption have been frustrated by the LMC's intrinsic x ray : Thomas T. Hamilton.

A soft X-ray survey ( keV) of the Large Magellanic Cloud (LMC) during a sounding rocket flight, reveals possible emission from the centrally located barlike structure.

No evidence was seen for absorption of the soft X-ray 'background' in the direction of the LMC. Both of these observations support the hypothesis of a local production of the soft X-ray by: 7.

A soft X-ray survey ( keV) of the Large Magellanic Cloud (LMC) during a sounding rocket flight, reveals possible emission from the centrally located barlike structure. No evidence was seen for absorption of the soft X-ray 'background' in the direction of the LMC.

Then the fact that the intensity did not go to zero in the galactic plane where the absorption optical depth is very large demonstrated that they were at least partly galactic. In the last few years, several experiments have attempted to measure the X-ray shadows of the Small Magellanic Cloud, M31, and the Large Magellanic Cloud.

X-ray sources in the Magellanic Clouds are of great astrophysical interest. The Small and Large Clouds are the nearest extragalactic star systems, and individual X-ray sources with rather low luminosities can be de-tected and compared with a large sample of Milky Way X-ray sources.

Because the distance is known, the abso. AN X-RAY image of the field surrounding the supernova SNA, derived from the Einstein Observatory Large Magellanic Cloud (LMC) Survey, has allowed us to constrain the properties of the hot.

The X-ray shadow in the south-east of the Large Magellanic Cloud Fig. The grey-scale maps represent the ROSAT R4{R7 band brightness distribution of the area south of 30Dor. The X-ray bright region of diffuse X-ray emission is called \wedge" in this paper due to its shape.

The X-ray dark region on the western side of the wedge is the X-ray. X-RAY AND ULTRAVIOLET SPECTROSCOPY OF GALACTIC DIFFUSE HOT GAS ALONG THE LARGE MAGELLANIC CLOUD X-3 SIGHT LINE Y. Yao1,2,3, T.

Hagihara 4,a, D. McCammon5, from existing X-ray absorption line data obtained with Chandra grating groups have attempted to study the background emission with X-ray CCDs aboard Suzaku X-ray.

Exploiting the good coverage obtained with sensitive XMM-Newton observations, we have undertaken a search for highly absorbed X-ray sources in the Small Magellanic Cloud (SMC), which is known to contain a large number of HMXRBs.

Due to the low Galactic foreground absorption, X-ray binary systems in the Magellanic Clouds are well suited for studies of the soft component in their X-ray spectrum. Fig. 1 and Fig. 2 show the X-ray light curves of the two novae and the unforeseen, intriguing variability within time scales of hours.

Fig. 1 shows large aperiodic variability for N LMC a: the count rate varied by an order of magnitude on and by a factor of about 3 in the other exposures, with somewhat lower amplitude on day –, the last exposure. Mon.

Not. Astron. Soc.() Printed 3 November (MN LATEX style file v) Survey of O VI absorption in the Large Magellanic Cloud A. Pathak⋆, A. Pradhan, N. Sujatha and J.

Murthy Indian Institute of Astrophysics, Koramangala II Block, BangaloreIndia. An illustration of an open book. Books. An illustration of two cells of a film strip. Video. An illustration of an audio speaker. Audio. An illustration of a " floppy disk. Survey of O VI absorption in the Large Magellanic Cloud Item Preview remove-circle Share or Embed This Item.

The Large Magellanic Cloud (LMC) is a satellite galaxy of the Milky Way. At a distance of around 50 kiloparsecs (≈, light-years), the LMC is the second- or third-closest galaxy to the Milky Way, after the Sagittarius Dwarf Spheroidal (~16 kpc) and the possible dwarf irregular galaxy known as the Canis Major on readily visible stars and a mass of approximately New research shows that the energy was so pervasive that it illuminated gas associated with two satellite galaxies of our own: the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC).

We have presented the first observations of the far ultraviolet diffuse radiation in the Magellanic Clouds and have shown that it is predominantly due to scattering of starlight from interstellar dust grains. We have also presented a survey of OVI absorption in the Large Magellanic Cloud (LMC), a tracer of hot gas in the interstellar medium (ISM).

We have used Far Ultraviolet Spectroscopic Explorer (FUSE) observations of the Large Magellanic Cloud (LMC) to determine the O vi column densities in. In the course of the first all-sky survey (eRASS1), the eROSITA instrument on board the Russian/German Spektrum-Roentgen-Gamma (SRG) mission has nearly finished scanning the Large Magellanic Cloud (LMC).

A source with supersoft X-ray spectrum was detected at the following position (after preliminary astrometrical corrections). Gruber D.in Proceedings of the International Workshop on the X-Ray Background, edited by X.

Barcons and A. Fabian (Cambridge University Press, Cambridge), p. 44 Google Scholar Iwan D. et al.ApJ,ADS CrossRef Google Scholar.ratios are found only when X-ray luminosities are statistically well measured and corrected by the interstellar absorption, not by the total absorption.

It should also be emphasized that 30 Dor is an extreme environment, more akin to starbursts than a good representative of the Large Magellanic Cloud (LMC) population.the Large Magellanic Cloud (MIT and Caltech) and measuring emission from the Small Magellanic Cloud (Wisconsin), their ability to make definitive statements about the effect of absorption was hampered by the difficulty of eliminating the effects of X-ray emission from within the clouds themselves.

These experiments.