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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >SiO and H2O Maser Observations of Red Supergiants in Star Clusters Embedded in the Galactic Disk
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SiO and H2O Maser Observations of Red Supergiants in Star Clusters Embedded in the Galactic Disk

机译：银河星盘内星团中红色超巨星的SiO和H2O Maser观测

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Wepresenttheresultsofradioobservationsofredsupergiantsinastarcluster,Stephenson(1990,AJ,99,1867)a€?s#2,andofcandidatesforredsupergiantsinthreestarclusters,Merceretal.(2005,ApJ,635,560)a€?s#4,#8,and#13,intheSiOandH$$_2$$Omaserlines.TheStephensona€?s#2clusterandnearbyaggregationatthesouthwestcontainmorethan15redsupergiants.WedetectedoneredsupergiantatthecenterofStephensona€?s#2andthreeinasouthwestaggregationintheSiOmaserline;threeoutofthesefourwerealsodetectedintheH$$_2$$Omaserline.Theaverageradialvelocityofthefourdetectedobjectsis97kms$$^{-1}$$,givingakinematicdistanceof5.5kpc,whichlocatesthisclusternearthebaseoftheScutuma€“Cruxspiralarm.WealsodetectedsixSiOemittingobjectsassociatedwithotherstarclusters.Inaddition,mappingobservationsintheCO$$J=$$1a€“0linetowardtheseclustersrevealedthatanappreciableamountofmoleculargasstillremainsaroundtheStephensona€?s#2clusterincontrasttotheprototypicalred-supergiantcluster,Bicaetal.(2003,Aamp;A,404,223)a€?s#122.Thisindicatesthatthetimescaleofgasexpulsiondiffersconsiderablyinindividualclusters.
机译：我们介绍了红色超巨星在星团中的无线电观测结果，斯蒂芬森（1990，AJ，99,1867）一个第二名，以及在三个星团中的红色超巨星的候选者。（2005，ApJ，635,560）一个在硅中的＃4，＃8和H $$ _ 2。 ？Omaserlines.TheStephensona€小号＃2clusterandnearbyaggregationatthesouthwestcontainmorethan15redsupergiants.WedetectedoneredsupergiantatthecenterofStephensona€小号＃2andthreeinasouthwestaggregationintheSiOmaserline; threeoutofthesefourwerealsodetectedintheH $$ _ 2 $$ Omaserline.Theaverageradialvelocityofthefourdetectedobjectsis97kms $$ ^ { - 1} $$，givingakinematicdistanceof5.5kpc，whichlocatesthisclusternearthebaseoftheScutuma€“Cruxspiralarm.WealsodetectedsixSiOemittingobjectsassociatedwithotherstarclusters.Inaddition，mappingobservationsintheCO $ $ J = $ 1a”向着簇的0行表明，在Stephensona的s＃2簇与典型的红色超级巨型簇Bicaetal相比，仍有相当数量的分子气体残留。（2003年，Aamp; A，404,223）表明气体量为＃122。各个离子的差异很大。

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