{"title":"Cyg X-3红外发射模型与UKIRT IRCAM3点扩散函数","authors":"R.N. Ogley , S.J.Bell Burnell , R.P. Fender","doi":"10.1016/S0083-6656(96)00064-5","DOIUrl":null,"url":null,"abstract":"<div><p>Modelling of the point spread function of the UKIRT IRCAM3 array was conducted in order to test for any extended emission around the X-ray binary Cyg X-3. We found that the point spread function cannot be represented by a simple Gaussian, but modelling of the stars required additional functions, namely Lorentzian and exponential components. After modelling for the PSF, we found that Cyg X-3 could be represented by two stellar-type profiles, 0.56″ apart.</p></div>","PeriodicalId":101275,"journal":{"name":"Vistas in Astronomy","volume":"41 1","pages":"Pages 65-70"},"PeriodicalIF":0.0000,"publicationDate":"1997-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.1016/S0083-6656(96)00064-5","citationCount":"2","resultStr":"{\"title\":\"Modelling of infrared emission from Cyg X-3 and the UKIRT IRCAM3 point spread function\",\"authors\":\"R.N. Ogley , S.J.Bell Burnell , R.P. Fender\",\"doi\":\"10.1016/S0083-6656(96)00064-5\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><p>Modelling of the point spread function of the UKIRT IRCAM3 array was conducted in order to test for any extended emission around the X-ray binary Cyg X-3. We found that the point spread function cannot be represented by a simple Gaussian, but modelling of the stars required additional functions, namely Lorentzian and exponential components. After modelling for the PSF, we found that Cyg X-3 could be represented by two stellar-type profiles, 0.56″ apart.</p></div>\",\"PeriodicalId\":101275,\"journal\":{\"name\":\"Vistas in Astronomy\",\"volume\":\"41 1\",\"pages\":\"Pages 65-70\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"1997-01-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"https://sci-hub-pdf.com/10.1016/S0083-6656(96)00064-5\",\"citationCount\":\"2\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Vistas in Astronomy\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://www.sciencedirect.com/science/article/pii/S0083665696000645\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Vistas in Astronomy","FirstCategoryId":"1085","ListUrlMain":"https://www.sciencedirect.com/science/article/pii/S0083665696000645","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
Modelling of infrared emission from Cyg X-3 and the UKIRT IRCAM3 point spread function
Modelling of the point spread function of the UKIRT IRCAM3 array was conducted in order to test for any extended emission around the X-ray binary Cyg X-3. We found that the point spread function cannot be represented by a simple Gaussian, but modelling of the stars required additional functions, namely Lorentzian and exponential components. After modelling for the PSF, we found that Cyg X-3 could be represented by two stellar-type profiles, 0.56″ apart.
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