{"title":"天琴座RR星的绝对星等","authors":"T. Tsujimoto, M. Miyamoto, Y. Yoshii","doi":"10.1017/S1539299600022383","DOIUrl":null,"url":null,"abstract":"The present determination of the absolute magnitude .M v (RR) of RR Lyrae stars is twofold, relying upon Hipparcos proper motions and trigonometric parallaxes separately. First, applying the statistical parallax method to the proper motions, we find v (RR)>= 0.69 ± 0.10 for 99 halo RR Lyraes with = -1.58. Second, applying the Lutz-Kelker correction to the RR Lyrae HIP95497 with the most accurately measured parallax, we obtain M v (RR) = 0.57-0.74 at [Fe/H]=-1.6. Furthermore, allowing full use of low accuracy and negative parallaxes as well for 125 RR Lyraes with - 2.49≤[Fe/H]≤0.07, the maximum likelihood estimation yields the relation, M v (RR)= (0.59±0.37)+(0.20±0.63)([Fe/H]+1.60), which formally agrees with the recent preferred relation. The same estimation yields again My (RR) = 0.65 ± 0.33 for the 99 halo RR Lyraes. Although the formal errors in the latter two estimates are rather large, all of the four results suggest the fainter absolute magnitude, My(RR)=0.6-0.7 at [Fe/H]=-1.6. The present results still provide the lower limit on the age of the universe which is inconsistent with a fiat, matter-dominated universe and current estimates of the Hubble constant.","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"15 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"1997-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"The Absolute Magnitude Of RR Lyrae Stars\",\"authors\":\"T. Tsujimoto, M. Miyamoto, Y. Yoshii\",\"doi\":\"10.1017/S1539299600022383\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The present determination of the absolute magnitude .M v (RR) of RR Lyrae stars is twofold, relying upon Hipparcos proper motions and trigonometric parallaxes separately. First, applying the statistical parallax method to the proper motions, we find v (RR)>= 0.69 ± 0.10 for 99 halo RR Lyraes with = -1.58. Second, applying the Lutz-Kelker correction to the RR Lyrae HIP95497 with the most accurately measured parallax, we obtain M v (RR) = 0.57-0.74 at [Fe/H]=-1.6. Furthermore, allowing full use of low accuracy and negative parallaxes as well for 125 RR Lyraes with - 2.49≤[Fe/H]≤0.07, the maximum likelihood estimation yields the relation, M v (RR)= (0.59±0.37)+(0.20±0.63)([Fe/H]+1.60), which formally agrees with the recent preferred relation. The same estimation yields again My (RR) = 0.65 ± 0.33 for the 99 halo RR Lyraes. Although the formal errors in the latter two estimates are rather large, all of the four results suggest the fainter absolute magnitude, My(RR)=0.6-0.7 at [Fe/H]=-1.6. The present results still provide the lower limit on the age of the universe which is inconsistent with a fiat, matter-dominated universe and current estimates of the Hubble constant.\",\"PeriodicalId\":422890,\"journal\":{\"name\":\"Highlights of Astronomy\",\"volume\":\"15 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"1997-08-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Highlights of Astronomy\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1017/S1539299600022383\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Highlights of Astronomy","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1017/S1539299600022383","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
摘要
目前对天琴座RR星的绝对星等m.v (RR)的测定是双重的,分别依靠依巴谷固有运动和三角视差。首先,将统计视差方法应用于固有运动,我们发现99晕RR Lyraes的v (RR)>= 0.69±0.10,= -1.58。其次,对视差测量精度最高的RR Lyrae HIP95497进行Lutz-Kelker校正,得到[Fe/H]=-1.6时的M v (RR) = 0.57-0.74。此外,在充分考虑低精度和负视差的情况下,对于- 2.49≤[Fe/H]≤0.07的125 RR Lyraes,最大似然估计得到的关系为M v (RR)=(0.59±0.37)+(0.20±0.63)([Fe/H]+1.60),与最近的优选关系正式一致。同样的估计也得出了99晕天琴座RR的My (RR) = 0.65±0.33。虽然后两种估计的形式误差相当大,但所有四种结果都表明绝对星等较弱,在[Fe/H]=-1.6时,My(RR)=0.6-0.7。目前的结果仍然提供了宇宙年龄的下限,这与固定的、物质主导的宇宙和目前对哈勃常数的估计不一致。
The present determination of the absolute magnitude .M v (RR) of RR Lyrae stars is twofold, relying upon Hipparcos proper motions and trigonometric parallaxes separately. First, applying the statistical parallax method to the proper motions, we find v (RR)>= 0.69 ± 0.10 for 99 halo RR Lyraes with = -1.58. Second, applying the Lutz-Kelker correction to the RR Lyrae HIP95497 with the most accurately measured parallax, we obtain M v (RR) = 0.57-0.74 at [Fe/H]=-1.6. Furthermore, allowing full use of low accuracy and negative parallaxes as well for 125 RR Lyraes with - 2.49≤[Fe/H]≤0.07, the maximum likelihood estimation yields the relation, M v (RR)= (0.59±0.37)+(0.20±0.63)([Fe/H]+1.60), which formally agrees with the recent preferred relation. The same estimation yields again My (RR) = 0.65 ± 0.33 for the 99 halo RR Lyraes. Although the formal errors in the latter two estimates are rather large, all of the four results suggest the fainter absolute magnitude, My(RR)=0.6-0.7 at [Fe/H]=-1.6. The present results still provide the lower limit on the age of the universe which is inconsistent with a fiat, matter-dominated universe and current estimates of the Hubble constant.