SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS JOHN R

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 • EXTENDED GENERALLY SHELL -LIKE OBJECT 0. 2 PC FOR 1987 A TO 158 PC FOR DEM L 203 (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 ke. V 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

= -0. 48 DEM L 81 = 0. 0

X-RAY SPECTRUM OF N 103 SNR (usually incorrectly called N 103 B) THIS SHOWS THERMAL NATURE OF THE EMISSION LEWIS, K. ET AL. 2003 Ap. J, 582, 770

SNR MCELS J 0521 -6542 3 COLOR [S II] H RATIO [S II]/H

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

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

N 157 B ANOTHER COMPOSITE Radio - contours are 2, 3, 4, 6, 7 n. Jy/beam X-ray - contours are 5, 10, 20, 30, 40, 100, 300, 6 00 counts from 0. 1 -10 ke. V 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 XRay contours and at the position of the cross in the radio

SPECTRUM OF N 157 B IT WILL BE VERY DIFFICULT TO MAKE ONE CONTINUOUS SPECTRUM FOR THIS OBJECT

X-RAY SPECTRUM OF N 103 SNR NOTE THE MANY LINES OF HIGHLY IONIZED INTERMEDIATE-MASS ELEMENTS LEWIS, K. ET AL. 2003 Ap. J, 582, 770

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, Ap. J, 375, 652

JY/BEAM N 19 AREA IN THE SMC RED: X-RAY CONTOURS GREYSCALE: 13 -CM RADIO

N 19 AREA IN THREE WAVELENGTHS H 22 cm Radio 1. 5 - 8 ke. V X-ray

SOME STATISTICS LMC TOTAL NUMBER OF SNRS CORE COLLAPSE TYPE Ia UNKNOWN 49 SMC 19 12 4 6 1 31 14 STANDARD STATISTICS EXPECTED IN IRREGULAR GALAXIES PREDICT ABOUT 10% TYPE Ia SNe.

RADIO LUMINOSITY vs DIAMETER FOR LMC SNRs slope -1. 13 corr coef 0. 08 1987 A DEM L 71 CONCLUSION: THERE IS NO CORRELATION OF LUMINOSITY WITH DIAMETER (IN AGREEMENT WITH PREVIOUS STUDIES)

X-RAY - RADIO LUMINOSITIES OF LMC SNRs DEM L 71 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

CHANDRA IMAGE OF CAS A 1. 1 ke. V 2 ke. V 5 ke. V

X-RAY IMAGE AND RADIO CONTOURS OF THE OXYGEN RICH SNR N 132 D, THE BRIGHTEST LMC RADIO SOURCE

SNR 1 E 0102 -72. 3 in the Small Magellanic Cloud radio X-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.

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 N 132 D AND 1 E 0102 -723. THE REWARD FOR DOING SO: A BOTTLE OF EITHER DICKEL TENNESSEE WHISKEY OR GRUET NEW MEXICO CHAMPAGNE

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