E. Ladd, J. Deane, J. Goldader, D. Sanders, C. Wynn-Williams
{"title":"W51的亚毫米图像","authors":"E. Ladd, J. Deane, J. Goldader, D. Sanders, C. Wynn-Williams","doi":"10.1063/1.43982","DOIUrl":null,"url":null,"abstract":"We report on submillimeter observations of the star forming region W51 on 11 pc size scales with 0.7 pc resolution. These observations show at least nine emission centers, each of which has enough luminosity to be a potential site for massive star formation. We also detect a region of extended emission surrounding these emission centers. This extended emission component has a steeper submillimeter spectrum, suggesting that it is warmer than the star forming cores.","PeriodicalId":310353,"journal":{"name":"Back to the Galaxy","volume":"22 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2008-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Submillimeter images of W51\",\"authors\":\"E. Ladd, J. Deane, J. Goldader, D. Sanders, C. Wynn-Williams\",\"doi\":\"10.1063/1.43982\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"We report on submillimeter observations of the star forming region W51 on 11 pc size scales with 0.7 pc resolution. These observations show at least nine emission centers, each of which has enough luminosity to be a potential site for massive star formation. We also detect a region of extended emission surrounding these emission centers. This extended emission component has a steeper submillimeter spectrum, suggesting that it is warmer than the star forming cores.\",\"PeriodicalId\":310353,\"journal\":{\"name\":\"Back to the Galaxy\",\"volume\":\"22 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2008-05-29\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Back to the Galaxy\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1063/1.43982\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Back to the Galaxy","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1063/1.43982","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
We report on submillimeter observations of the star forming region W51 on 11 pc size scales with 0.7 pc resolution. These observations show at least nine emission centers, each of which has enough luminosity to be a potential site for massive star formation. We also detect a region of extended emission surrounding these emission centers. This extended emission component has a steeper submillimeter spectrum, suggesting that it is warmer than the star forming cores.
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