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Friday, July 31, 2020 | History

2 edition of ASCA observations of the Barnard 209 dark cloud and an intense X-ray flare on V773 Tauri found in the catalog.

ASCA observations of the Barnard 209 dark cloud and an intense X-ray flare on V773 Tauri

ASCA observations of the Barnard 209 dark cloud and an intense X-ray flare on V773 Tauri

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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:
  • Stellar flares.,
  • X ray astronomy.,
  • Magnetic clouds.,
  • Plasma decay.,
  • T Tauri stars.,
  • Astronomical models.,
  • Stellar coronas.

  • Edition Notes

    StatementStephen L. Skinner ... [et al.].
    Series[NASA contractor report] -- 207206, NASA contractor report -- NASA CR-207206.
    ContributionsSkinner, Stephen Lee., United States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL17132057M

    A comprehensive calibration of the ASCA X-ray pointing accuracy is given in Restoration of the ASCA Source Position Accuracy (ApJ Vol. , p. ), the primary reference for this web page. Here we provide the look-up table and software referred to therein. These can be used to easily correct the measured sky coordinates derived from any given. We discuss the importance of X-ray scattering and Compton reflection in type 2 Seyfert Galaxies, based upon the analysis of ASCA observations of 25 such sources. Consideration of the iron Kα complex, [O III] line, and X-ray variability suggest that NGC , NGC , NGC , Mrk 3, Mrk E, and Mrk are dominated by reprocessed examine the properties of these sources in more.

    CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): Abstract. SLX − is among the 10 persistent, high energy, SIGMA sources which contribute significantly to the last five year averaged γ/X-ray emission from the direction of the Galactic Center. Detailed study of the source has only been carried out recently from data collected by SIGMA in the keV range.   Central Alabama X-Ray would like to thank all the participants at the ASCA Convention and Exposition for another successful year! We were proud to introduce Chattanooga and Collagentex to our list of quality product vendors. We look forward to Central Alabama X-Ray's 20th Anniversary of attending the ASCA in See you there!

    As of April, there were observations of stars, 58 of cataclysmic variables, of X-ray binaries, of supernova remnants and diffuse Galactic emission, of normal galaxies, of active galactic nuclei, of clusters of galaxies, and "surveys and misc." observations (see the Legacy article for more on the status of. ASCA calibration database (CALDB) at HEASARC (High-Energy Astrophysics Archive, Goddard Space Flight Center) are only sup-plied in 1keVbandwidths from 1 to 10keV. Our methodology is to take the X-ray events from each cluster observation and divide them into broad spectral energy bands, cor-responding to the energy ranges of the PSF images. We.


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ASCA observations of the Barnard 209 dark cloud and an intense X-ray flare on V773 Tauri Download PDF EPUB FB2

ASCA (Advanced Satellite for Cosmology and Astrophysics) detected an intense X-ray flare on the weak-lined T Tauri star V Tau (=HD ) during a 30 ks observation of the Barnard dark cloud in September.

Get this from a library. ASCA observations of the Barnard dark cloud and an intense X-ray flare on V Tauri. [Stephen Lee Skinner; United States. National Aeronautics and Space Administration.;]. We present results of a ≈ 40 ks ASCA observation of the active weak-lined T Tauri star V Tau (HD ) and the surrounding Barnard dark cloud, obtained in February.

ASCA results of eight X-ray sources in the Chamaeleon II dark cloud are presented. Six sources were identified as low-mass young stellar objects, either Class II--III sources or T Tauri stars with X-ray temperatures and luminosities in the range of keV and 10() () erg s(-1), respectively.

Two of them showed time variability: one with typical flare profile and the other with Cited by: 6. ASCA obtained broad-band ( keV) images and spectra of the central region of the Rho Ophiuchi dark cloud in August.

The ks observation detected at least eleven sources (S/N >= 3), including the X-ray bright pre--main-sequence star DoAr 21 and embedded infrared sources with no optical counterparts. Hard X-rays up to ~ 8 keV were detected from DoAr 21 (whose light curve shows no Cited by: 1.

et al.Kamata et al.Ozawa et al. ); however, not all Class I protostars are X-ray emitters. Their spectra are harder than those of T Tauri Stars, and the X-ray emission sometimes shows time variability like solar flares. Class I objects detected with ASCA, for instance WL6 and EL29 in the ρ Ophiuchi dark cloud, indicate 2.

Important Keywords and Columns in ASCA FITS Events Files RAWX/Y, DETX/Y, X/Y Columns and RA/DEC_NOM Keywords TIME Column and TIMESYS, MJDREF, TSTART, TSTOP Keywords.

We analyzed ASCA data, including the reflection nebula NGCand discovered two X-ray flares from an Hα emission-line star, Kiso A–, located at ∼ 30′ to the southwest of NGC X-ray peak is shifted from the cloud core to the south by 1′.2, which is significantly larger than the X-ray position errors.

Spatial extent of the keV line and the contin-uum X-ray images are examined with the SIS data, because spatial resolution of the SIS is better. The Advanced Satellite for Cosmology and Astrophysics (ASCA), is Japan’s fourth cosmic X-ray astronomy mission, and the second for which the United States is providing part of the scientific satellite was successfully launched on Febru ASCA operated successfully till July 15 when it was tranferred into a safe-hold mode.

The X-ray shadows in the DXB as detected with mosaics of the ROSAT PSPC pointed observations in the Galactic plane have recently revealed the existence of a highly enhanced X-ray emitting region around the Galactic center: a Galactic X-ray bulge (GXB) (Park et al.

; Almy et al. ; Park et al. P98 hereafter). The derived X-ray. ASCA Archive. ASCA public archive complete. (Oct 5, ) Archive Access.

GIS gain update - more accurately calibrated data are available for some recent sequences outside the normal supersedes the earlier ( April) reprocessing and affects more sequences. ASCA archive via Browse. We therefore carried out a target of opportunity (TOO) observation using the ASCA satellite on 12 December 2 OBSERVATIONS AND ANALYSIS ASCA observed the SMC X-3 region from to on 12 December centered on the position of SMC X-3 with the two SIS detectors operated in "1CCD" mode providing a time resolution o4 by: 1.

To illustrate this work, we examine the X-ray spectrum of the northwestern rim of an SNR suspected to have a non-thermal component to its X-ray emission, G+ (RX J+), over the energy range ≈– keV using observations made by the ASCA GIS and the RXTE by: 5.

New Horizon of X-Ray Astronomy. First Results from ASCA. Proceedings of the International Conference on X-ray Astronomy, held March, at Tokyo Metropolitan University, Tokyo, Japan. Frontiers Science Series No.

12 (FSS). Edited by Fumiyoshi Makino and Takaya Ohashi. Published by Universal Academy Press, Inc., Tokyo, Japan,p 41) A large gas cloud in the interstellar medium that contains several type O and B stars would appear to us as A) a dark nebula.

B) an emission nebula. C) bright blue. D) a reflection nebula. E) a dark patch against a bright background. the evolution of the X-ray spectrum from SN J observed with three years of ASCA observations. We found that the X-ray emission in the early phase consists of two thermal components with diƒerent absorptions in agree-mentwiththetwo-shockscheme.

OBSERVATIONS AND RESULTS Observation ASCA (Tanaka, Inoue, & Holt ) observed M81 10Cited by: Mon. Not. Astron. Soc.– () ASCA spectroscopy of the hard X-ray emission from the colliding wind interaction in g2 Velorum G.

Rauw,1,2w† I. Stevens,2w J. Pittard2,3w and M. Corcoran4w 1Institut d’Astrophysique & Ge ´ophysique, Universite de Lie `ge, 5, Avenue de Cointe, B Liege, Belgium 2School of Physics & Astronomy, University of Birmingham, Edgbaston.

Start studying Astronomy Chapter Learn vocabulary, terms, and more with flashcards, games, and other study tools. Pierre et al.: ASCA observations of massive medium-distant clusters of galaxies.

Table 2. Cluster data Cluster z ˙ v L X [{] N H km s −1 erg s−1 cm 2 A 18 (PSPC) A (HRI) Velocity dispersions and luminosities are from L emonon et al. N H is a 21cm value from Cited by: 6. Abstract. X-ray emissions from clusters are most likely originated from a thin hot plasma in a collisional ionization equilibrium.

The optical depth of continuum component is order of 10 −3, whereas that of emission lines is around t emission models used for spectral fitting can not estimate this effect, so that the determination of elemental abundances seems to include large Author: Koujun Yamashita.X; in comparing the previous observations with the ASCA data, we have recalculated the previously-published source luminosities for a new fiducial distance of kpc.

2. Observation The region of the sky containing NGC was observed with the Japanese X-ray satellite, ASCA (Tanaka et al ) bet_en Apr 6 UT and Apr 7   This paper presents the properties of X-ray sources in the regions of NGC and NGC observed with ASCA.

We found 14 point-like sources in the NGC field. In the NGC field, on the other hand, we found extended X-ray emission in the central dust lane of NGCand resolved 5 point-like sources around the by: 4.