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SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS

SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS. JOHN R. DICKEL UNIVERSITY OF NEW MEXICO AND ROSA MURPHY WILLIAMS COLUMBUS STATE UNIVERSITY. Preliminary SNR tables at: http://hoth.ccssc.org/mcsnr/test.php. SNR IDENTIFICATION.

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SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS

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  1. SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS JOHN R. DICKEL UNIVERSITY OF NEW MEXICO AND ROSA MURPHY WILLIAMS COLUMBUS STATE UNIVERSITY Preliminary SNR tables at: http://hoth.ccssc.org/mcsnr/test.php

  2. SNR IDENTIFICATION • EXTENDED GENERALLY SHELL -LIKE OBJECT - 0.2 PC FOR 1987A TO 158 PC FOR DEM L203 (1 PC IS 4 ARCSEC AT THE LMC AND 3.4 ARCSEC AT THE SMC) • NON THERMAL RADIO SPECTRA - TYPICAL SPECTRAL INDICES,  = -0.5, WHERE Sf = const f • THERMAL X-RAYS - TYPICAL TEMP ~ 1 keV WITH A LARGE SPREAD • CAVEAT - PULSAR WIND NEBULAE HAVE FLATTER RADIO SPECTRA AND NON-THERMAL HIGH ENERGY X-RAY TAILS • [S II]/ Ha > 0.4

  3. = -0.48 DEM L81 = 0.0

  4. X-RAY SPECTRUM OF N103 SNR(usually incorrectly called N103B) THIS SHOWS THE THERMAL NATURE OF THE EMISSION LEWIS, K. ET AL. 2003 ApJ, 582, 770

  5. SNR MCELS J0521-6542 3 COLOR RATIO [S II] H [S II]/H

  6. TYPE CLASSIFICATION OF MAGELLANIC CLOUD SNRS CORE COLLAPSE: PRESENCE OF A PULSAR OR OTHER COMPACT REMAINS IN A REGION OF YOUNG STARS OXYGEN RICH TYPE Ia: XRAY SPECTRA SHOW LINES OF HIGHLY IONIZED INTERMEDIATE MASS ELEMENTS BALMER DOMINATED IN OPTICAL

  7. 0540-693 - A PROTOTYPE COMPOSITE SNR 50-MSEC PULSAR, PWN, O-RICH SHELL, ORGANIZED POLARIZATION IN THE PWN 6-CM RADIO IMAGE

  8. N157B ANOTHER COMPOSITE Radio - contours are 2,3,4,6,7 nJy/beam X-ray - contours are 5,10,20,30,40,100,300,600 counts from 0.1-10 keV The shell can be seen faintly on the southern part of the radio image. The 16-msec X-Ray pulsar is at the center of the bright X-Ray contours and at the position of the cross in the radio image.

  9. SPECTRUM OF N157B IT WILL BE VERY DIFFICULT TO MAKE ONE CONTINUOUS SPECTRUM FOR THIS OBJECT

  10. X-RAY SPECTRUM OF N103 SNRNOTE THE MANY LINES OF HIGHLY IONIZED INTERMEDIATE-MASS ELEMENTS LEWIS, K. ET AL. 2003 ApJ, 582, 770

  11. H LINE PROFILE TOWARD THE TYPE Ia BALMER-DOMINATED SNR 0519-675 UNEQUILIBRATED VELOCITY 1180 KM/S EQUILIBRATED 1580 KM/S SMITH, R. C. ET AL. 1991, ApJ, 375, 652

  12. N19 AREA IN THE SMC JY/BEAM RED: X-RAY CONTOURS GREYSCALE: 13-CM RADIO

  13. N19 AREA IN THREE WAVELENGTHS H22cm Radio 1.5 - 8 keV X-ray

  14. SOME STATISTICS LMCSMC TOTAL NUMBER OF SNRS4919 CORE COLLAPSE 12 4 TYPE Ia 61 UNKNOWN 3114 STANDARD STATISTICS EXPECTED IN IRREGULAR GALAXIESPREDICT ABOUT 10% TYPE Ia SNe.

  15. RADIO LUMINOSITY vs DIAMETER FOR LMC SNRs slope -1.13 corr coef 0.08 1987A DEM L71 CONCLUSION: THERE IS NO CORRELATION OF LUMINOSITY WITH DIAMETER (IN AGREEMENT WITH PREVIOUS STUDIES)

  16. X-RAY - RADIO LUMINOSITIES OF LMC SNRs DEM L71 DEM L71 slope 0.77 corr. coeff 0.41 CONCLUSION: BRIGHTER X-RAY EMISSION MAY, IN GENERAL, CORRESPOND TO BRIGHTER RADIO BUT THERE IS NO CLEAR CORRELATION

  17. CHANDRA IMAGE OF CAS A 1.1 keV 2keV 5 keV

  18. X-RAY IMAGE AND RADIO CONTOURS OF THE OXYGEN RICH SNR N132D, THE BRIGHTEST LMC RADIO SOURCE

  19. SNR 1E0102-72.3 in the Small Magellanic Cloud radioX-ray optical in the light of [O III] characteristic of oxygen rich SNRs Note that the radio shell lies outside the X-ray one – an unusual condition in shell SNRs.

  20. THE MAGELLANIC CLOUD CANDIDATES ARE ABOUT 20 TIMES FURTHER AWAY THAN CAS A SO THE REQUIRED SENSITIVITY NEEDS TO BE INCREASED BY A FACTOR OF 400.THE INTERNATIONAL X-RAY OBSERVATORY (IXO) WILL BE ABOUT 100 TIMES MORE SENSITIVE THAN CHANDRA THEREFORE WITH MODESTLY LONGER EXPOSURES THE FIRST TASK FOR IXO SHOULD BE TO FIND THE COOLING NEUTRON STARS IN N132D AND 1E0102-723. THE REWARD FOR DOING SO: A BOTTLE OF EITHER DICKEL TENNESSEE WHISKEY OR GRUET NEW MEXICO CHAMPAGNE

  21. Preliminary SNR tables at:http://hoth.ccssc.org/mcsnr/test.phpPlease send us references, new data, etc.We will eventually get proper pages for each SNR.

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