SMASHing the LMC: Mapping a Ring-like Stellar Overdensity in the LMC Disk
We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ∼6° (∼5.2 kpc at the LMC distance) that is conti...
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| Veröffentlicht in: | The Astrophysical journal 2018-12, Vol.869 (2), p.125 |
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| creator | Choi, Yumi Nidever, David L. Olsen, Knut Besla, Gurtina Blum, Robert D. Zaritsky, Dennis Cioni, Maria-Rosa L. van der Marel, Roeland P. Bell, Eric F. Johnson, L. Clifton Vivas, A. Katherina Walker, Alistair R. de Boer, Thomas J. L. Noël, Noelia E. D. Monachesi, Antonela Gallart, Carme Monelli, Matteo Stringfellow, Guy S. Massana, Pol Martinez-Delgado, David Muñoz, Ricardo R. |
| description | We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ∼6° (∼5.2 kpc at the LMC distance) that is continuous over ∼270° in position angle and is only limited by the current data coverage. The overdensity shows an amplitude up to 2.5 times higher than that of the underlying smooth disk. This structure might be related to the multiple arms found by de Vaucouleurs. We find that the overdensity shows spatial correlation with intermediate-age star clusters, but not with young ( |
| doi_str_mv | 10.3847/1538-4357/aaed1f |
| format | Article |
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Clifton ; Vivas, A. Katherina ; Walker, Alistair R. ; de Boer, Thomas J. L. ; Noël, Noelia E. D. ; Monachesi, Antonela ; Gallart, Carme ; Monelli, Matteo ; Stringfellow, Guy S. ; Massana, Pol ; Martinez-Delgado, David ; Muñoz, Ricardo R.</creator><creatorcontrib>Choi, Yumi ; Nidever, David L. ; Olsen, Knut ; Besla, Gurtina ; Blum, Robert D. ; Zaritsky, Dennis ; Cioni, Maria-Rosa L. ; van der Marel, Roeland P. ; Bell, Eric F. ; Johnson, L. Clifton ; Vivas, A. Katherina ; Walker, Alistair R. ; de Boer, Thomas J. L. ; Noël, Noelia E. D. ; Monachesi, Antonela ; Gallart, Carme ; Monelli, Matteo ; Stringfellow, Guy S. ; Massana, Pol ; Martinez-Delgado, David ; Muñoz, Ricardo R.</creatorcontrib><description>We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ∼6° (∼5.2 kpc at the LMC distance) that is continuous over ∼270° in position angle and is only limited by the current data coverage. The overdensity shows an amplitude up to 2.5 times higher than that of the underlying smooth disk. This structure might be related to the multiple arms found by de Vaucouleurs. We find that the overdensity shows spatial correlation with intermediate-age star clusters, but not with young (<1 Gyr) main-sequence stars, indicating the stellar populations associated with the overdensity are intermediate in age or older. Our findings on the LMC overdensity can be explained by either of two distinct formation mechanisms of a ring-like overdensity: (1) the overdensity formed out of an asymmetric one-armed spiral wrapping around the LMC main body, which is induced by repeated encounters with the Small Magellanic Cloud (SMC) over the last Gyr, or (2) the overdensity formed very recently as a tidal response to a direct collision with the SMC. Although the measured properties of the overdensity alone cannot distinguish between the two candidate scenarios, the consistency with both scenarios suggests that the ring-like overdensity is likely a product of tidal interaction with the SMC, but not with the Milky Way halo.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aaed1f</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Dark energy ; galaxies: dwarf ; galaxies: interactions ; galaxies: structure ; Magellanic Clouds ; Main sequence stars ; Mapping ; Milky Way ; Sky surveys (astronomy) ; Spiral wrapping ; Star clusters ; Stellar age ; Stellar populations ; Stellar structure ; Tidal interaction</subject><ispartof>The Astrophysical journal, 2018-12, Vol.869 (2), p.125</ispartof><rights>2018. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Dec 20, 2018</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c380t-72d32f312cc29e080163f887324622a98f49d5511e32e242f74f84452f81f7f23</citedby><cites>FETCH-LOGICAL-c380t-72d32f312cc29e080163f887324622a98f49d5511e32e242f74f84452f81f7f23</cites><orcidid>0000-0003-2325-9616 ; 0000-0002-7123-8943 ; 0000-0003-4341-6172 ; 0000-0002-1793-3689 ; 0000-0002-8622-4237 ; 0000-0001-6421-0953 ; 0000-0003-3835-2231 ; 0000-0002-5564-9873 ; 0000-0002-6797-696X ; 0000-0002-5177-727X ; 0000-0001-5292-6380 ; 0000-0002-7134-8296 ; 0000-0003-1680-1884 ; 0000-0001-6728-806X ; 0000-0001-7827-7825 ; 0000-0003-1479-3059</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aaed1f/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>314,776,780,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aaed1f$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc></links><search><creatorcontrib>Choi, Yumi</creatorcontrib><creatorcontrib>Nidever, David L.</creatorcontrib><creatorcontrib>Olsen, Knut</creatorcontrib><creatorcontrib>Besla, Gurtina</creatorcontrib><creatorcontrib>Blum, Robert D.</creatorcontrib><creatorcontrib>Zaritsky, Dennis</creatorcontrib><creatorcontrib>Cioni, Maria-Rosa L.</creatorcontrib><creatorcontrib>van der Marel, Roeland P.</creatorcontrib><creatorcontrib>Bell, Eric F.</creatorcontrib><creatorcontrib>Johnson, L. Clifton</creatorcontrib><creatorcontrib>Vivas, A. Katherina</creatorcontrib><creatorcontrib>Walker, Alistair R.</creatorcontrib><creatorcontrib>de Boer, Thomas J. L.</creatorcontrib><creatorcontrib>Noël, Noelia E. D.</creatorcontrib><creatorcontrib>Monachesi, Antonela</creatorcontrib><creatorcontrib>Gallart, Carme</creatorcontrib><creatorcontrib>Monelli, Matteo</creatorcontrib><creatorcontrib>Stringfellow, Guy S.</creatorcontrib><creatorcontrib>Massana, Pol</creatorcontrib><creatorcontrib>Martinez-Delgado, David</creatorcontrib><creatorcontrib>Muñoz, Ricardo R.</creatorcontrib><title>SMASHing the LMC: Mapping a Ring-like Stellar Overdensity in the LMC Disk</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ∼6° (∼5.2 kpc at the LMC distance) that is continuous over ∼270° in position angle and is only limited by the current data coverage. The overdensity shows an amplitude up to 2.5 times higher than that of the underlying smooth disk. This structure might be related to the multiple arms found by de Vaucouleurs. We find that the overdensity shows spatial correlation with intermediate-age star clusters, but not with young (<1 Gyr) main-sequence stars, indicating the stellar populations associated with the overdensity are intermediate in age or older. Our findings on the LMC overdensity can be explained by either of two distinct formation mechanisms of a ring-like overdensity: (1) the overdensity formed out of an asymmetric one-armed spiral wrapping around the LMC main body, which is induced by repeated encounters with the Small Magellanic Cloud (SMC) over the last Gyr, or (2) the overdensity formed very recently as a tidal response to a direct collision with the SMC. Although the measured properties of the overdensity alone cannot distinguish between the two candidate scenarios, the consistency with both scenarios suggests that the ring-like overdensity is likely a product of tidal interaction with the SMC, but not with the Milky Way halo.</description><subject>Astrophysics</subject><subject>Dark energy</subject><subject>galaxies: dwarf</subject><subject>galaxies: interactions</subject><subject>galaxies: structure</subject><subject>Magellanic Clouds</subject><subject>Main sequence stars</subject><subject>Mapping</subject><subject>Milky Way</subject><subject>Sky surveys (astronomy)</subject><subject>Spiral wrapping</subject><subject>Star clusters</subject><subject>Stellar age</subject><subject>Stellar populations</subject><subject>Stellar structure</subject><subject>Tidal interaction</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp9kM9LwzAcxYMoOKd3jwHxZl3yTdok3sambrAxcAreQmgT7VbbmnTC_ntb6o-LeHp8H5_3vvAQOqfkmkkuRjRmMuIsFiNjbEbdARr8WIdoQAjhUcLE8zE6CWHTnaDUAM3Xy_F6lpcvuHm1eLGc3OClqevOMPihlajItxavG1sUxuPVh_WZLUPe7HFefmfwNA_bU3TkTBHs2ZcO0dPd7eNkFi1W9_PJeBGlTJImEpAxcIxCmoKyRBKaMCelYMATAKOk4yqLY0otAwscnOBOch6Dk9QJB2yILvre2lfvOxsaval2vmxfamBJLDhIRVqK9FTqqxC8dbr2-Zvxe02J7gbT3Tq6W0f3g7WRqz6SV_Vv5z_45R-4qTdaJkqDphDrOnPsExMXdgc</recordid><startdate>20181220</startdate><enddate>20181220</enddate><creator>Choi, Yumi</creator><creator>Nidever, David L.</creator><creator>Olsen, Knut</creator><creator>Besla, Gurtina</creator><creator>Blum, Robert D.</creator><creator>Zaritsky, Dennis</creator><creator>Cioni, Maria-Rosa L.</creator><creator>van der Marel, Roeland P.</creator><creator>Bell, Eric F.</creator><creator>Johnson, L. 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Clifton ; Vivas, A. Katherina ; Walker, Alistair R. ; de Boer, Thomas J. L. ; Noël, Noelia E. 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D.</creatorcontrib><creatorcontrib>Monachesi, Antonela</creatorcontrib><creatorcontrib>Gallart, Carme</creatorcontrib><creatorcontrib>Monelli, Matteo</creatorcontrib><creatorcontrib>Stringfellow, Guy S.</creatorcontrib><creatorcontrib>Massana, Pol</creatorcontrib><creatorcontrib>Martinez-Delgado, David</creatorcontrib><creatorcontrib>Muñoz, Ricardo R.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Choi, Yumi</au><au>Nidever, David L.</au><au>Olsen, Knut</au><au>Besla, Gurtina</au><au>Blum, Robert D.</au><au>Zaritsky, Dennis</au><au>Cioni, Maria-Rosa L.</au><au>van der Marel, Roeland P.</au><au>Bell, Eric F.</au><au>Johnson, L. Clifton</au><au>Vivas, A. Katherina</au><au>Walker, Alistair R.</au><au>de Boer, Thomas J. L.</au><au>Noël, Noelia E. D.</au><au>Monachesi, Antonela</au><au>Gallart, Carme</au><au>Monelli, Matteo</au><au>Stringfellow, Guy S.</au><au>Massana, Pol</au><au>Martinez-Delgado, David</au><au>Muñoz, Ricardo R.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>SMASHing the LMC: Mapping a Ring-like Stellar Overdensity in the LMC Disk</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2018-12-20</date><risdate>2018</risdate><volume>869</volume><issue>2</issue><spage>125</spage><pages>125-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ∼6° (∼5.2 kpc at the LMC distance) that is continuous over ∼270° in position angle and is only limited by the current data coverage. The overdensity shows an amplitude up to 2.5 times higher than that of the underlying smooth disk. This structure might be related to the multiple arms found by de Vaucouleurs. We find that the overdensity shows spatial correlation with intermediate-age star clusters, but not with young (<1 Gyr) main-sequence stars, indicating the stellar populations associated with the overdensity are intermediate in age or older. Our findings on the LMC overdensity can be explained by either of two distinct formation mechanisms of a ring-like overdensity: (1) the overdensity formed out of an asymmetric one-armed spiral wrapping around the LMC main body, which is induced by repeated encounters with the Small Magellanic Cloud (SMC) over the last Gyr, or (2) the overdensity formed very recently as a tidal response to a direct collision with the SMC. 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| ispartof | The Astrophysical journal, 2018-12, Vol.869 (2), p.125 |
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| source | IOP Publishing Free Content |
| subjects | Astrophysics Dark energy galaxies: dwarf galaxies: interactions galaxies: structure Magellanic Clouds Main sequence stars Mapping Milky Way Sky surveys (astronomy) Spiral wrapping Star clusters Stellar age Stellar populations Stellar structure Tidal interaction |
| title | SMASHing the LMC: Mapping a Ring-like Stellar Overdensity in the LMC Disk |
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