Last edited by Salkis
Tuesday, July 28, 2020 | History

2 edition of Broad band X-ray spectra of cosmic sources found in the catalog.

Broad band X-ray spectra of cosmic sources

COSPAR. Scientific Commission E. E1.1 Symposium

Broad band X-ray spectra of cosmic sources

proceedings of the E1.1 symposium of COSPAR Scientific Commission E which was held during the thirty-second COSPAR scientific assembly, Nagoya, Japan, 12-19 July, 1998

by COSPAR. Scientific Commission E. E1.1 Symposium

  • 65 Want to read
  • 3 Currently reading

Published by Published for the Committee on Space Research [by] Pergamon in Oxford, New York .
Written in English

    Subjects:
  • Astrophysics -- Congresses.,
  • Cosmic rays -- Congresses.,
  • X-ray sources, Galactic -- Congresses.,
  • X-ray spectroscopy -- Congresses.

  • Edition Notes

    Includes bibliographical references and index.

    Statementedited by K. Makishima, L. Piro and T. Takahashi.
    GenreCongresses.
    SeriesAdvances in space research -- v. 25, no. 3/4
    ContributionsMakishima, K., Piro, L., Takahashi, T., COSPAR. Scientific Assembly, COSPAR. Scientific Commission E.
    Classifications
    LC ClassificationsQB472.A1 C688 1998
    The Physical Object
    Paginationxii, p. 351-918 :
    Number of Pages918
    ID Numbers
    Open LibraryOL19484163M

      4 Latex pages, 6 figures, uses Accepted for publication in Advances in Space Research, in Proceedings of 32nd Sci. Ass. of COSPAR, "Broad-Band X-ray Spectroscopy of Cosmic Sources" Subjects: Astrophysics (astro-ph) DOI: /S(99) Cite as: arXiv:astro-ph/ (or arXiv:astro-ph/v1 for this version)   Abstract: The X-ray telescopes on board BeppoSAX are an optimal set of instruments to observe bright galactic binary pulsars. These sources emit very hard and quite complex X-ray spectra that can be accurately measured with BeppoSAX between and keV. A prototype of this complexity, the source Her X-1, shows at least seven different components in its ://

    K. Pottschmidt's research works with 4, citations and 6, reads, including: Dust and gas absorption in the high mass X-ray binary IGR J   spectra. - "Origin of the Hard X-ray/Soft -y-ray Background The spectra of a significant sample of AGN will test the AGN origin of the cosmic x-ray background (CXB) for the poorly explored hard x-ray band. With a total sample of _ AGN, at least half of which will have been measured at keV with ABRIXAS, the spectral distributions of a

    The derived fraction of the X-ray emission resolved into point sources is shown as a function of energy in Fig. the narrow energy band – keV that contains the iron emission line, 84 When the X-ray spectra of optically identified and unidentified X-ray sources are stacked together by optical type, we find that the summed spectra are best fit by (i) a spectral photon index of for Type I AGN, (ii) a spectral index of for Type II AGN, and (iii) a harder index of for (non-ROSAT) unidentified sources selected in the


Share this book
You might also like
Schizophrenia

Schizophrenia

Safe tree climbing in forest management

Safe tree climbing in forest management

F-16 multinational staged improvement program

F-16 multinational staged improvement program

Examining changes in self-concept and other selected variables in seventh and eighth grade students participating in a creative and performing arts magnet middle school program

Examining changes in self-concept and other selected variables in seventh and eighth grade students participating in a creative and performing arts magnet middle school program

Development and evaluation of teaching situations involving role playing in science teacher education

Development and evaluation of teaching situations involving role playing in science teacher education

Turnips and swedes for human consumption.

Turnips and swedes for human consumption.

XVII Brazilian Symposium on Computer Graphics and Image Processing: Proceedings

XVII Brazilian Symposium on Computer Graphics and Image Processing: Proceedings

Ceramics

Ceramics

Medieval treatises on estate management.

Medieval treatises on estate management.

Macroeconomics

Macroeconomics

Architects of ideas

Architects of ideas

poets of the nineteenth century

poets of the nineteenth century

Byzantine year 6562

Byzantine year 6562

Free-grace alone exalted in mans conversion, or, A sermon preached in Pauls on Aug. 23, 1657

Free-grace alone exalted in mans conversion, or, A sermon preached in Pauls on Aug. 23, 1657

Broad band X-ray spectra of cosmic sources by COSPAR. Scientific Commission E. E1.1 Symposium Download PDF EPUB FB2

Broad Band X-Ray Spectra of Cosmic Sources July • Nagoya, Japan. Makishima, L. Piro, T. Takahashi. Vol Issues 3–4, Pages () Previous vol/issue.

Next vol/issue. Actions for selected articles. Select all / Deselect all. Download PDFs Export ://   Get this from a library. Broad band X-ray spectra of cosmic sources: proceedings of the E symposium of COSPAR Scientific Commission E which was held during the thirty-second COSPAR scientific assembly, Nagoya, Japan, July, [K Makishima; L Piro; T Takahashi; COSPAR.

Scientific Assembly; COSPAR. Scientific Commission E.] Broad band X-ray spectra of cosmic sources. Proceedings. E Symposium of COSPAR Scientific Commission E held during the 32nd COSPAR Scientific Assembly, Nagoya (Japan), 12 - 19 Jul Makishima, K.

Abstract. The following topics were dealt with: broad-band X-ray spectroscopy of compact objects, emission line diagnostics of cosmic plasmas The X-ray telescopes on board BeppoSAX are an optimal set of instruments to observe bright galactic binary pulsars.

These sources emit very hard and quite complex X-ray spectra that can be accurately measured with BeppoSAX between and   The cosmic X-ray sources that will be observed with these detectors range from the nearby solar-mass Galactic X-ray binaries to the largest structures in the universe, the clusters of galaxies.

Download: Download full-size image; Fig. Simulated wide band X-ray spectrum from the Coma :// We present the X-ray spectral analysis of the brightest extragalactic sources in the Chandra-Cosmic Evolution Survey catalogue, showing at least 70 net counts in the keV band. This sample has a per cent completeness in optical-infrared identification, with ∼75 per cent of the sample having a spectroscopic redshift and ∼25 per cent a photometric :// During the last days of Ginga, we tried to make simultaneous observations with Ginga and ROSAT of several low-mass x-ray binaries.

We succeeded in the case of The simultaneous observations took place in the period Sept. Due to the broad energy range covered jointly by both observatories, some interesting new features were :// L/abstract. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A The discovery of a diffuse background of cosmic X-radiation accompanied the birth of the field of X-ray astronomy, yet the exact origin of this radiation remains unexplained more than thirty years hence.

Subsequent research has demonstrated that the X-ray background (XRB) arises from the integrated emission of individual sources. The principal weakness of the discrete-source explanation for 9M/abstract.

The X-ray spectrum in Figure 2 can be identified as coming from a very specific region of the thin-foil specimen imaged in the AEM and can be quantified in a straightforward manner. Typical energy-dispersive X-ray spectra display the number of X-ray counts detected at a given energy.

The Gaussian characteristic peaks are superimposed on a slowly varying bremsstrahlung :// 6 hours ago  We also investigate the X-ray spectral curvature of blazar H and found that six of our observations are well described by the log parabolic model with α = – and β = – Three of our observations are well described by power law model.

The break energy of the X-ray spectra varies between – :// We review some theoretical models, which are used to explain some X-ray and gamma-ray data from rotation powered pulsars emitted from regions within and beyond the light cylinder.

In particular, the high energy emission resulting from the interactions between The X-ray source catalog comprises X-ray point sources detected down to a maximum likelihoo d threshold detml = 8 3 in at least one band (,or keV).

Finally, our observation allows us to associate the presence of an hard tail with a low luminosity X-ray state ( keV luminosity of 10^37 erg/s at kpc).Comment: Submitted for publication in Advances in Space Research, Proc. of the 32nd COSPAR Meeting held in Nagoya, July,"Broad band Spectra of Cosmic X-ray sources", 6 pages The Broad Band X-ray Telescope (BBXRT) was flown on the space shuttle Columbia (STS) on December 2-Decem as part of the ASTRO-1 payload.

The flight of BBXRT marked the first opportunity for performing X-ray observations over a broad energy range ( keV) with a moderate energy resolution (typically 90 eV and eV at 1 and 6 Abstract.

We will present some results on the broad--band observations of BeppoSAX of the bright Seyfert galaxies NGC and NGC Comment: 5 pages, 4 figures, Proc. of the 32 COSPAR Ass., Session E "Broad Band X-Ray Spectra of Cosmic Sources, ed.s K.

Makishima, L. Piro, T. Takahashi, Advances in Space Research, in pres X-ray concentrators, energy sensitive broad-band imaging detectors and wavelength dispersive gratings and crystals can be combined to provide powerful tools for performing diagnostic measurements on cosmic X-ray plasmas.

A selection of these devices is ://   wherein broad-band emission from low-luminosity sources appears to be dominated by detected X-ray sources in the Fermi-LAT localization circles, thus enabling identification, blazars and GRBs with hard gamma-ray spectra, and consider the effects of cosmic X-ray spectra of XMM-Newton serendipitous medium flux sources Article (PDF Available) in Astronomy and Astrophysics (3) December with 38 Reads How we measure 'reads' They are therefore typical of sources dominating the X-ray Background in that band.

12 of the 15 targets for which we have optical spectra show emission lines at a range of line luminosities, and. The task of ME module is to provide measurements of X-ray sources in 5 − 40 keV and, together with the measurements with the Low Energy X-ray Telescope (LE, Chen et al., ) and the High Energy X-ray Telescope (HE, Liu et al., ), to study these sources in a rather broad energy band of 1 − keV.

It contains three detector boxes and   HETE-2 Mission Goals The primary goal of HETE-2 is to determine the origin and nature of cosmic gamma-ray bursts (GRBs).

This is accomplished through the simultaneous, broad-band observation in the soft X-ray, medium X-ray, and gamma-ray energy ranges, and the precise localization and identification of cosmic gamma-ray burst sources (GRBs). The cosmic X-ray background (CXB) is a broad band di use emission discovered since the early era of X-ray astronomy (Gi-acconi et al.

). It is known today that in the X-ray do-main the CXB is the integrated emission of many faint point-like extragalactic sources, most of them being Seyfert galaxies or ://