Nora Salem, Karen L. Masters, David V. Stark, Anubhav Sharma
{"title":"Finding Passive Galaxies in H i-MaNGA: The Impact of Star Formation Rate Indicator","authors":"Nora Salem, Karen L. Masters, David V. Stark, Anubhav Sharma","doi":"10.3847/2515-5172/ad676f","DOIUrl":null,"url":null,"abstract":"H <sc>i</sc>-rich galaxies typically have high star formation rates (SFRs), but there exist interesting H <sc>i</sc>-rich and low star-forming galaxies. Previous work on a sample of these galaxies identified from H <sc>i</sc>-Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) (H <sc>i</sc> follow-up to the MaNGA survey) using an infrared indicator of specific-SFR (sSFR; namely W2 − W3 < 2) could find no single physical process to explain their unusual behavior. The method by which galaxies are identified as low sSFR may be important in this conclusion. In this Research Note, we explore how an H <sc>i</sc>-rich, low sSFR sample of H <sc>i</sc>-MaNGA galaxies differs using H<italic toggle=\"yes\">α</italic>, single stellar population, and ultraviolet estimators of SFR. We find that samples are statistically similar to each other so long as W2 − W3 < 2 is interpreted as corresponding to sSFR < 10<sup>−11.15</sup> yr<sup>−1</sup>.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"34 1","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-07-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Research notes of the AAS","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.3847/2515-5172/ad676f","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
Abstract
H i-rich galaxies typically have high star formation rates (SFRs), but there exist interesting H i-rich and low star-forming galaxies. Previous work on a sample of these galaxies identified from H i-Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) (H i follow-up to the MaNGA survey) using an infrared indicator of specific-SFR (sSFR; namely W2 − W3 < 2) could find no single physical process to explain their unusual behavior. The method by which galaxies are identified as low sSFR may be important in this conclusion. In this Research Note, we explore how an H i-rich, low sSFR sample of H i-MaNGA galaxies differs using Hα, single stellar population, and ultraviolet estimators of SFR. We find that samples are statistically similar to each other so long as W2 − W3 < 2 is interpreted as corresponding to sSFR < 10−11.15 yr−1.
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