Radio and X-ray Properties of Magellanic Cloud - Chandra X-Ray ...
Transcript of Radio and X-ray Properties of Magellanic Cloud - Chandra X-Ray ...
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SUPERNOVA REMNANTS IN THE
MAGELLANIC CLOUDS
JOHN R. DICKELJOHN R. DICKELUNIVERSITY OF NEW MEXICOUNIVERSITY OF NEW MEXICO
ANDAND
ROSA MURPHY WILLIAMSROSA MURPHY WILLIAMSCOLUMBUS STATE UNIVERSITYCOLUMBUS STATE UNIVERSITY
Preliminary SNR tables at:http://hoth.ccssc.org/mcsnr/test.php
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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
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= -0.48
DEM L81
= 0.0
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X-RAY SPECTRUM OF N103 SNR
(usually incorrectly called N103B)
LEWIS, K. ET AL. 2003 ApJ, 582, 770
THIS SHOWS THE THERMAL NATURE OF THE EMISSION
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SNR MCELS J0521-6542
[S II] H
[S II]/H
RATIO3 COLOR
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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
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0540-693 - A PROTOTYPE COMPOSITE SNR 50-MSEC PULSAR, PWN, O-RICH SHELL,ORGANIZED POLARIZATION IN THE PWN
6-CM RADIO IMAGE
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N157B ANOTHER COMPOSITE
X-ray - contours are 5,10,20,30,40,100,300,600 counts from 0.1-10 keV
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.
Radio - contours are2,3,4,6,7 nJy/beam
The shell can be seen faintly on the southern part of the radio image.
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SPECTRUM OF N157B
IT WILL BE VERY DIFFICULT TO MAKE ONE CONTINUOUS SPECTRUM FOR THIS OBJECT
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X-RAY SPECTRUM OF N103 SNRNOTE THE MANY LINES OF HIGHLY
IONIZED INTERMEDIATE-MASS ELEMENTS
LEWIS, K. ET AL. 2003 ApJ, 582, 770
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H LINE PROFILE TOWARD THE TYPE Ia BALMER-DOMINATED SNR 0519-
675
UNEQUILIBRATED VELOCITY 1180 KM/SEQUILIBRATED 1580 KM/S
SMITH, R. C. ET AL. 1991, ApJ, 375, 652
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N19 AREA IN THE SMC
RED: X-RAY CONTOURS GREYSCALE: 13-CM RADIO
JY/B
EA
M
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N19 AREA IN THREE WAVELENGTHS
H22cm Radio 1.5 - 8 keV X-ray
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SOME STATISTICS
LMC SMC
TOTAL NUMBER OF SNRS 49 19
CORE COLLAPSE 12 4
TYPE Ia 6 1
UNKNOWN 31 14
STANDARD STATISTICS EXPECTED IN IRREGULAR
GALAXIES PREDICT ABOUT 10% TYPE Ia SNe.
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RADIO LUMINOSITY vs DIAMETER FOR LMC SNRs
CONCLUSION: THERE IS NO CORRELATION OF LUMINOSITY WITH DIAMETER
(IN AGREEMENT WITH PREVIOUS STUDIES)
1987A
DEM L71
slope -1.13corr coef 0.08
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X-RAY - RADIO LUMINOSITIES OF LMC SNRs
CONCLUSION: BRIGHTER X-RAY EMISSION MAY, IN GENERAL, CORRESPOND TO BRIGHTER RADIO BUT THERE IS NO CLEAR CORRELATION
DEM L71
slope 0.77corr. coeff 0.41
DEM L71
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1.1 keV 2keV 5 keV
CHANDRA IMAGE OF CAS A
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X-RAY IMAGE AND RADIO CONTOURS OF THE OXYGEN RICH SNR N132D,
THE BRIGHTEST LMC RADIO SOURCE
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radio X-ray optical in the light of [O III] characteristic of oxygen rich SNRsNote that the radio shell lies outside the X-ray one – an unusual
condition in shell SNRs.
SNR 1E0102-72.3 in the Small Magellanic Cloud
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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
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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.