SUMMARY OF PROPOSAL 51078

MR HIDEHIRO KANEDA
KANEDA@MIRANDA.PHYS.S.U-TOKYO.AC.JP

UNIVERSITY OF TOKYO
TOKYO JAPAN 113
BUNKYO-KU
7-3-1 HONGO
Tel: 03-3812-2111 EX4173 Fax: 03-3812-6938
Medium: 2.5GB8MM
Subject: SUPERNOVA REMNANTS AND GALACTIC DIFFUSE EMISSION

X-RAY EMISSIONS AT THE EDGE OF THE GALACTIC RIDGE (L


ABSTRACT

We propose to observe the edge of the galactic ridge at l = 60 deg. From the past observations with ASCA, we get an evidence that a softer (kT = 0.8 keV) component exists in the Galactic ridge emission in addition to the well-known harder (kT = 7 keV) component. This soft component requires a Galactic absorption with a column density of N_H = 0.7*10^22, which implies that it is located at an effective distance of 2 kps away from us. Then, how far does this soft component extend? What is its origin? Is there any relation with the 7 keV hard component? Such a soft component has also been discovered in many other spiral galaxies, therefore, this would be an our Galaxy version. By observing the edge of the Galactic ridge, we will get information about the behavior of this soft component.

CO-INVESTIGATORS
CO-I NAME INSTITUTE COUNTRY
KAZUO MAKISHIMAUNIVERSITY OF TOKYOJAPAN
KEIICHI MATSUZAKIUNIVERSITY OF TOKYOJAPAN
SHIGEO YAMAUCHIIWATE UNIVERSITYJAPAN
NORIKO YAMASAKITOKYO METROPOLITAN UJAPAN

TARGETS

TARGET NAMEPRIRADECTIMETCOFFGISSIS CNTOBS
1)RIDGE EDGE #1
2
295.1579 22.5858 10 ksN
Y
P
0.02000
1
2)RIDGE EDGE #2
2
295.4804 23.1072 10 ksN
Y
P
0.02000
1
3)RIDGE EDGE #3
2
295.8050 23.6279 10 ksN
Y
P
0.02000
1
4)RIDGE EDGE #4
2
296.1325 24.1479 10 ksN
Y
P
0.02000
1
5)RIDGE EDGE #5
2
296.4625 24.6673 10 ksN
Y
P
0.02000
1
6)RIDGE EDGE #6
2
296.7950 25.1859 10 ksN
Y
P
0.02000
1
7)RIDGE EDGE #7
2
297.1304 25.7037 10 ksN
Y
P
0.02000
1
8)RIDGE EDGE #8
2
297.4692 26.2208 10 ksN
Y
P
0.02000
1