{"title":"平面宇宙论中SWIRE的对数正态光度函数","authors":"L. Zaninetti","doi":"10.22606/adap.2018.34003","DOIUrl":null,"url":null,"abstract":"The evaluation of the physical parameters or effects such as the luminosity function (LF) or the photometric maximum (PM) for galaxies is routinely modeled by their spectroscopic redshift. Here, we model LF and PM for galaxies by the photometric redshift as given by the Spitzer Wide-Area Infrared Extragalactic (SWIRE) catalog in the framework of a lognormal LF. In addition, we compare our model with the Schechter LF for galaxies. The adopted cosmological framework is that of the flat cosmology.","PeriodicalId":131060,"journal":{"name":"Advances in Astrophysics","volume":"63 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2018-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"1","resultStr":"{\"title\":\"A Lognormal Luminosity Function for SWIRE in Flat Cosmology\",\"authors\":\"L. Zaninetti\",\"doi\":\"10.22606/adap.2018.34003\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The evaluation of the physical parameters or effects such as the luminosity function (LF) or the photometric maximum (PM) for galaxies is routinely modeled by their spectroscopic redshift. Here, we model LF and PM for galaxies by the photometric redshift as given by the Spitzer Wide-Area Infrared Extragalactic (SWIRE) catalog in the framework of a lognormal LF. In addition, we compare our model with the Schechter LF for galaxies. The adopted cosmological framework is that of the flat cosmology.\",\"PeriodicalId\":131060,\"journal\":{\"name\":\"Advances in Astrophysics\",\"volume\":\"63 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2018-11-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"1\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Advances in Astrophysics\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.22606/adap.2018.34003\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Advances in Astrophysics","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.22606/adap.2018.34003","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
A Lognormal Luminosity Function for SWIRE in Flat Cosmology
The evaluation of the physical parameters or effects such as the luminosity function (LF) or the photometric maximum (PM) for galaxies is routinely modeled by their spectroscopic redshift. Here, we model LF and PM for galaxies by the photometric redshift as given by the Spitzer Wide-Area Infrared Extragalactic (SWIRE) catalog in the framework of a lognormal LF. In addition, we compare our model with the Schechter LF for galaxies. The adopted cosmological framework is that of the flat cosmology.
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