THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR
We present a chemical abundance analysis of 300S-1, the brightest likely member star of the 300 km s[superscript –1] stream near the faint satellite galaxy Segue 1. From a high-resolution Magellan/MIKE spectrum, we determine a metallicity of [Fe/H] = –1.46 ± 0.05 ± 0.23 (random and systematic uncert...
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| 语言: | en_US |
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IOP Publishing
2015
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| 在线阅读: | http://hdl.handle.net/1721.1/94536 https://orcid.org/0000-0002-2139-7145 |
| _version_ | 1826188860515680256 |
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| author | Lunnan, Ragnhild Casey, Andrew R. Norris, John E. Wyse, Rosemary F. G. Gilmore, Gerard Frebel, Anna L. |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Lunnan, Ragnhild Casey, Andrew R. Norris, John E. Wyse, Rosemary F. G. Gilmore, Gerard Frebel, Anna L. |
| author_sort | Lunnan, Ragnhild |
| collection | MIT |
| description | We present a chemical abundance analysis of 300S-1, the brightest likely member star of the 300 km s[superscript –1] stream near the faint satellite galaxy Segue 1. From a high-resolution Magellan/MIKE spectrum, we determine a metallicity of [Fe/H] = –1.46 ± 0.05 ± 0.23 (random and systematic uncertainties) for star 300S-1, and find an abundance pattern similar to typical halo stars at this metallicity. Comparing our stellar parameters to theoretical isochrones, we estimate a distance of 18 ± 7 kpc. Both the metallicity and distance estimates are in good agreement with what can be inferred from comparing the Sloan Digital Sky Survey photometric data of the stream stars to globular cluster sequences. While several other structures overlap with the stream in this part of the sky, the combination of kinematic, chemical, and distance information makes it unlikely that these stars are associated with either the Segue 1 galaxy, the Sagittarius Stream, or the Orphan Stream. Streams with halo-like abundance signatures, such as the 300 km s[superscript –1] stream, present another observational piece for understanding the accretion history of the Galactic halo. |
| first_indexed | 2024-09-23T08:06:09Z |
| format | Article |
| id | mit-1721.1/94536 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T08:06:09Z |
| publishDate | 2015 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/945362022-09-30T07:29:13Z THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR Lunnan, Ragnhild Casey, Andrew R. Norris, John E. Wyse, Rosemary F. G. Gilmore, Gerard Frebel, Anna L. Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Frebel, Anna L. Casey, Andrew R. We present a chemical abundance analysis of 300S-1, the brightest likely member star of the 300 km s[superscript –1] stream near the faint satellite galaxy Segue 1. From a high-resolution Magellan/MIKE spectrum, we determine a metallicity of [Fe/H] = –1.46 ± 0.05 ± 0.23 (random and systematic uncertainties) for star 300S-1, and find an abundance pattern similar to typical halo stars at this metallicity. Comparing our stellar parameters to theoretical isochrones, we estimate a distance of 18 ± 7 kpc. Both the metallicity and distance estimates are in good agreement with what can be inferred from comparing the Sloan Digital Sky Survey photometric data of the stream stars to globular cluster sequences. While several other structures overlap with the stream in this part of the sky, the combination of kinematic, chemical, and distance information makes it unlikely that these stars are associated with either the Segue 1 galaxy, the Sagittarius Stream, or the Orphan Stream. Streams with halo-like abundance signatures, such as the 300 km s[superscript –1] stream, present another observational piece for understanding the accretion history of the Galactic halo. Smithsonian Astrophysical Observatory (Clay Mathematics Institute) 2015-02-13T19:58:36Z 2015-02-13T19:58:36Z 2013-06 2012-12 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/94536 Frebel, Anna, Ragnhild Lunnan, Andrew R. Casey, John E. Norris, Rosemary F. G. Wyse, and Gerard Gilmore. “THE 300 Km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR.” The Astrophysical Journal 771, no. 1 (July 1, 2013): 39. © The American Astronomical Society https://orcid.org/0000-0002-2139-7145 en_US http://dx.doi.org/10.1088/0004-637X/771/1/39 The Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf IOP Publishing American Astronomical Society |
| spellingShingle | Lunnan, Ragnhild Casey, Andrew R. Norris, John E. Wyse, Rosemary F. G. Gilmore, Gerard Frebel, Anna L. THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR |
| title | THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR |
| title_full | THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR |
| title_fullStr | THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR |
| title_full_unstemmed | THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR |
| title_short | THE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR |
| title_sort | 300 km s superscript 1 stellar stream near segue 1 insights from high resolution spectroscopy of its brightest star |
| url | http://hdl.handle.net/1721.1/94536 https://orcid.org/0000-0002-2139-7145 |
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