The search for absorption of 1 keV x-rays by the Small Magellanic Cloud

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National Aeronautics and Space Administration , [Washington, D.C.?
X-ray astro
Statementprepared by Brad Marazas.
SeriesNASA CR -- 185348., NASA contractor report -- NASA CR-185348.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
Pagination1 v.
ID Numbers
Open LibraryOL15274041M

Get this from a library. The search for absorption of 1 keV x-rays by the Small Magellanic Cloud. [Brad Marazas; United States. National Aeronautics and Space Administration.]. 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 by: 3.

RXTE () observations of the Small Magellanic Cloud (SMC), spanning The resulting observational library provides a comprehensive view of the physical, temporal and statistical properties of the SMC pulsar population across the luminosity range of L X = { erg s 1.

From a sampleFile Size: KB. Refraction of X-rays X-rays can be treated like light when interaction with a medium. However, unlike visible light, the index of refraction of x-rays in matter is very close to unity: a a' n = 1 + i with ˘10 5 Snell’s Law cos = n cos 0 where 0.

AN X-RAY INVESTIGATION OF THE NGC FIELD IN THE SMALL MAGELLANIC CLOUD I. THE LUMINOUS BLUE VARIABLE HD AND THE NGC CLUSTER ´1 Institutd’AstrophysiqueetdeGe´ophysique,Universite´ deLie`ge,Alle´edu6Aouˆt17,Bat.B5c,BLie`ge,Belgium;[email protected] Magellanic Cloud and the link of the sup ergiant B [e] star LHA S 18 with an X-ray source G.

Maravelias, 1 ⋆ A. Zezas, 1, 2, 3 V. Antoniou, 3, 4 D.

Details The search for absorption of 1 keV x-rays by the Small Magellanic Cloud PDF

Hatzidimitriou 5. Abstract: We report the discovery of extended X-ray emission within the young star cluster NGC in the Wing of the Small Magellanic Cloud (SMC) based on observations obtained with the Chandra X-ray Observatory. X-ray emission is detected from the cluster core area with the highest stellar density and from a dusty ridge surrounding the HII by: Y.

Naz´e10, R. Hainich1, J. Reyes-Iturbide11 Draft version Janu ABSTRACT We report the discovery of extended X-ray emission within the young star cluster NGCa in the Wing of the Small Magellanic Cloud (SMC) based on observations obtained with the ChandraX-ray Observatory.


and Slane, Patrick O. and Güver, Tolga and Özel, Feryal}, abstractNote = {We present a comprehensive study of interstellar X-ray extinction. XMM-Newton archival data for the Small Magellanic Cloud have been examined for the presence of previously undetected X-ray pulsars.

One such pulsar, with a period of s, is detected. For isotropic X-rays in 1 keV – 1 MeV, superposition theories involving clusters of galaxies, Seyfert galaxies, etc. over a cosmological path length are now roughly viable.

Simple ‘metagalactic’ Compton theories seem excluded if the break at 40 keV Cited by: 3. Complex computer-image processing of the relative absorption of the X-rays, in different directions, can produce a highly detailed three-dimensional X-ray image of the body.

X-rays can also be used to probe the structures of atoms and molecules. Consider X-rays incident on the surface of a crystalline : Samuel J. Ling, Jeff Sanny, William Moebs.

The Magellanic Clouds (MCs) have been mapped at soft X-rays (– keV) with ROSAT during an all-sky survey and numerous pointed observations. A distinct class of supersoft X-ray sources (SSS) was discovered radiating with blackbody temperatures of a few times 10 5 K and with bolometric luminosities ∼ 10 4 times solar.

A detailed study of these sources in X-rays, UV and Author: P. Kahabka, P. Kahabka. We investigate the mechanism that reproduced notable spectral features at the ignition phase of the nova explosion observed for a super-Eddington X-ray transient source MAXI J– in the Small Magellanic Cloud.

These features include a strong Ne IX emission line at keV. X-rays transmitted without interaction contribute to _____ Compton interactions, photoelectric absorption, and transmitted x-rays all contribue to _____. differential absorption. High kVp techniques reduce _____.

patient dose. At energies below 40 keV, the predominant x-ray interaction in soft tissue and bone is _____. X-rays are absorbed as they pass through materials according to the exponential law: I = I 0 e -μt where I 0 is the incident intensity, I is the (reduced) intensity after travelling a distance t through the material and μ is the absorption coefficient (sometimes also referred to as the photoelectric absorption (coefficient) due to photo.

A luminous supersoft X-ray source (SSXS, or SSS) is an astronomical source that emits only low energy (i.e., soft) X-rays have energies in the to keV range, whereas hard X-rays are in the 1–20 keV range.

SSSs emit few or no photons with energies above 1 keV, and most have effective temperature below eV. This means that the radiation they emit is. Small Magellanic Cloud: ¡, ¡, and ¡ The ROSAT/HRI images of these SNRs indicate that the most of the X-ray emissions are concentrated in the center region.

Only from ¡ are faint X-rays along the radio shell also detected. The ASCA/SIS spectra of ¡ and ¡Cited by: 6. X rays: Their origin, dosage, and practical application [Schall, W.

E] on *FREE* shipping on qualifying offers. X rays: Their origin, dosage, and practical applicationAuthor: W. E Schall. First astronomical X-ray source is a lecture for the advanced course on X-ray are free to take this quiz based on the lecture at any time.

Once you’ve read and studied the lecture itself, the links contained within the lecture, listed under See also, External links and in the {{principles of radiation astronomy}} template, you should have adequate background to.

Abstract Only X-ray-bright superbubbles have been reported in the past. ROSA T provides an excellent opportunity to study X-ray-dim superbubbles We have analyzed the ROSAT Position Sensitive Proportional Counter observations of four superbubbles in the Large Magellanic Cloud DEMDEMand DEM   AsianScientist (Feb.

9, ) – Researchers from Tohoku University now know what happens in the million billionth of a second after x-rays hit matter. Their findings have been published in Nature Communications.

X-rays are one of the most important diagnostic tools in medicine, biology and the material sciences, as they may penetrate deep into material which is. X-Ray Absorption X-rays (light with wavelength λ. 12 A or energy 1˚. keV) are absorbed by all matter through the photo-electric effect: An x-ray is absorbed by an atom when the energy of the x-ray is transferred to a core-level elec-tron (K, L, or M shell) which is ejected from the atom.

The atom is left in an excited. This page contains materials for the session on x-ray emission and absorption. It features a 1-hour lecture video, and also presents the prerequisites, learning objectives, reading assignment, lecture slides, homework with solutions, and resources for further study.

Soft X-rays have energies in the to keV range, whereas hard X-rays are in the keV range. SSXSs are in most cases only detected below keV, so that within our own galaxy they are usually hidden by interstellar absorption in the galactic disk.

We know more than 80 Be/X-ray binaries in the Small Magellanic Cloud (SMC), about two dozen in the Large Magellanic Cloud (LMC) and over one hundred in the Milky Way.

Description The search for absorption of 1 keV x-rays by the Small Magellanic Cloud PDF

Given that the mass of the SMC is 50 to times smaller than that of the Milky Way Be/X-ray binaries are extremely abundant in this irregular dwarf galaxy. At 50% survival, the OER for cells treated with 8 keV X rays was compared with for (60)Co gamma rays. The numbers of H2AX foci per Gy after treatment with 8 keV X rays and (60)Co gamma rays were similar; however, the size of the foci generated at 8 keV was significantly larger, possibly indicating more complex DNA by: 7.

X-rays with photon energies above 5–10 keV (below – nm wavelength) are called hard X-rays, while those with lower energy are called soft X-rays.[4] Due to their penetrating ability, hard X-rays are widely used to image the inside of objects, e.g., in.

The relationship among transmitted x-rays, photoelectrically absorbed x-ray, and Compton scattered x-rays resulting in the x-ray image differential absorption Scattering of very low energy x-rays with no loss of energy; also called coherent or Thompson scattering.

Aims. We report the discovery of three faint, super-soft X-ray sources in LMC fields observed with XMM-Newton. Methods. We analyse the three new sources together with RX J and RX J, both known since ROSAT.


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We identify XMMU J with the LMC planetary nebula LHA N = LMC SMP The EPIC-pn spectrum of XMMU J Cited by: 8. A star is an astronomical object consisting of a luminous spheroid of plasma held together by its own nearest star to Earth is the other stars are visible to the naked eye from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth.

Historically, the most prominent stars were grouped into .X-rays having an energy of keV undergo Compton scattering from a target. The scattered rays are detected at relative to the incident rays. Find(a)the Compton shift at this angle,(b)the energy of the scattered x-ray, and(c)the energy of the recoiling electron.The primary interactions of x-rays with isolated atoms from Z = 1 (hydrogen) to Z = 92 (uranium) are described and computed within a self-consistent Dirac-Hartree-Fock framework.

The results are provided over the energy range from either 1 eV or 10 eV to keV, depending on the atom.