ADAPTIVE OPTICS IMAGING OF VY CANIS MAJORIS AT 2-5 μm WITH LBT/LMIRCam
We present adaptive optics images of the extreme red supergiant VY Canis Majoris in the K sub(s), L', and M bands (2.15-4.8 mu m) made with LMIRCam on the Large Binocular Telescope. The peculiar "Southwest Clump" previously imaged from 1 to 2.2 mu m appears prominently in all three fi...
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| Veröffentlicht in: | The Astronomical journal 2013-10, Vol.146 (4), p.1-7 |
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| creator | Shenoy, Dinesh P Jones, Terry J Humphreys, Roberta M Marengo, Massimo Leisenring, Jarron M Nelson, Matthew J Wilson, John C Skrutskie, Michael F Hinz, Philip M Hoffmann, William F Bailey, Vanessa Skemer, Andrew RODIGAS, TIMOTHY Vaitheeswaran, Vidhya |
| description | We present adaptive optics images of the extreme red supergiant VY Canis Majoris in the K sub(s), L', and M bands (2.15-4.8 mu m) made with LMIRCam on the Large Binocular Telescope. The peculiar "Southwest Clump" previously imaged from 1 to 2.2 mu m appears prominently in all three filters. We find its brightness is due almost entirely to scattering, with the contribution of thermal emission limited to at most 25%. We model its brightness as optically thick scattering from silicate dust grains using typical size distributions. We find a lower limit mass for this single feature of 5 x 10 super(-3) M sub([middot in circle]) to 2.5 x 10 super(-2) M sub([middot in circle]) depending on the assumed gas-to-dust ratio. The presence of the Clump as a distinct feature with no apparent counterpart on the other side of the star is suggestive of an ejection event from a localized region of the star and is consistent with VY CMa's history of asymmetric high-mass-loss events. |
| doi_str_mv | 10.1088/0004-6256/146/4/90 |
| format | Article |
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The peculiar "Southwest Clump" previously imaged from 1 to 2.2 mu m appears prominently in all three filters. We find its brightness is due almost entirely to scattering, with the contribution of thermal emission limited to at most 25%. We model its brightness as optically thick scattering from silicate dust grains using typical size distributions. We find a lower limit mass for this single feature of 5 x 10 super(-3) M sub([middot in circle]) to 2.5 x 10 super(-2) M sub([middot in circle]) depending on the assumed gas-to-dust ratio. 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The peculiar "Southwest Clump" previously imaged from 1 to 2.2 mu m appears prominently in all three filters. We find its brightness is due almost entirely to scattering, with the contribution of thermal emission limited to at most 25%. We model its brightness as optically thick scattering from silicate dust grains using typical size distributions. We find a lower limit mass for this single feature of 5 x 10 super(-3) M sub([middot in circle]) to 2.5 x 10 super(-2) M sub([middot in circle]) depending on the assumed gas-to-dust ratio. The presence of the Clump as a distinct feature with no apparent counterpart on the other side of the star is suggestive of an ejection event from a localized region of the star and is consistent with VY CMa's history of asymmetric high-mass-loss events.</description><subject>Adaptive optics</subject><subject>ASTRONOMY</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>ASYMMETRY</subject><subject>BRIGHTNESS</subject><subject>Clumps</subject><subject>COSMIC DUST</subject><subject>Ejection</subject><subject>FILTERS</subject><subject>Imaging</subject><subject>MASS TRANSFER</subject><subject>OPTICS</subject><subject>Scattering</subject><subject>SILICATES</subject><subject>Stars</subject><subject>STELLAR WINDS</subject><subject>TELESCOPES</subject><issn>0004-6256</issn><issn>1538-3881</issn><issn>1538-3881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNqN0b1OwzAUBWALgUQpvACTJRaWkGtfx3HGENo0qD-oDUVMlps6oqhtSpwOvBvPwDORqoiZ6UhXn-5wDiHXDO4YKOUDgPAkD6TPhPSFH8EJ6bAAlYdKsVPS-QPn5MK5dwDGFIgOSeOH-CnP5j06aSOZ0WwUp9k4pZM-nb_SJB5nMzqKHyfTNuOcci-g318b-pLlAzq8z_3hKJsmZnNJzkqzdvbqN7vkud_Lk4E3nKRZEg-9AlXQeIgQLkO7RLAMg1AginCBhjFjbSmXGJlFZCG0gnPbnhFZactIKhMujF0Cxy65Of6tXLPSrlg1tngrqu3WFo3mnIeIAbbq9qh2dfWxt67Rm5Ur7HpttrbaO82kBJCcyeAfNBBSMR6xlvIjLerKudqWelevNqb-1Az0YQZ9aFkfWtbtDFroCPAH0dVybg</recordid><startdate>20131001</startdate><enddate>20131001</enddate><creator>Shenoy, Dinesh P</creator><creator>Jones, Terry J</creator><creator>Humphreys, Roberta M</creator><creator>Marengo, Massimo</creator><creator>Leisenring, Jarron M</creator><creator>Nelson, Matthew J</creator><creator>Wilson, John C</creator><creator>Skrutskie, Michael F</creator><creator>Hinz, Philip M</creator><creator>Hoffmann, William F</creator><creator>Bailey, Vanessa</creator><creator>Skemer, Andrew</creator><creator>RODIGAS, TIMOTHY</creator><creator>Vaitheeswaran, Vidhya</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20131001</creationdate><title>ADAPTIVE OPTICS IMAGING OF VY CANIS MAJORIS AT 2-5 μm WITH LBT/LMIRCam</title><author>Shenoy, Dinesh P ; Jones, Terry J ; Humphreys, Roberta M ; Marengo, Massimo ; Leisenring, Jarron M ; Nelson, Matthew J ; Wilson, John C ; Skrutskie, Michael F ; Hinz, Philip M ; Hoffmann, William F ; Bailey, Vanessa ; Skemer, Andrew ; RODIGAS, TIMOTHY ; Vaitheeswaran, Vidhya</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c385t-3307d7ed30e135743347b3a11aeef6d39ab9e07e422e3a1331fef968a7baed023</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>Adaptive optics</topic><topic>ASTRONOMY</topic><topic>ASTROPHYSICS</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>ASYMMETRY</topic><topic>BRIGHTNESS</topic><topic>Clumps</topic><topic>COSMIC DUST</topic><topic>Ejection</topic><topic>FILTERS</topic><topic>Imaging</topic><topic>MASS TRANSFER</topic><topic>OPTICS</topic><topic>Scattering</topic><topic>SILICATES</topic><topic>Stars</topic><topic>STELLAR WINDS</topic><topic>TELESCOPES</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Shenoy, Dinesh P</creatorcontrib><creatorcontrib>Jones, Terry J</creatorcontrib><creatorcontrib>Humphreys, Roberta M</creatorcontrib><creatorcontrib>Marengo, Massimo</creatorcontrib><creatorcontrib>Leisenring, Jarron M</creatorcontrib><creatorcontrib>Nelson, Matthew J</creatorcontrib><creatorcontrib>Wilson, John C</creatorcontrib><creatorcontrib>Skrutskie, Michael F</creatorcontrib><creatorcontrib>Hinz, Philip M</creatorcontrib><creatorcontrib>Hoffmann, William F</creatorcontrib><creatorcontrib>Bailey, Vanessa</creatorcontrib><creatorcontrib>Skemer, Andrew</creatorcontrib><creatorcontrib>RODIGAS, TIMOTHY</creatorcontrib><creatorcontrib>Vaitheeswaran, Vidhya</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astronomical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Shenoy, Dinesh P</au><au>Jones, Terry J</au><au>Humphreys, Roberta M</au><au>Marengo, Massimo</au><au>Leisenring, Jarron M</au><au>Nelson, Matthew J</au><au>Wilson, John C</au><au>Skrutskie, Michael F</au><au>Hinz, Philip M</au><au>Hoffmann, William F</au><au>Bailey, Vanessa</au><au>Skemer, Andrew</au><au>RODIGAS, TIMOTHY</au><au>Vaitheeswaran, Vidhya</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>ADAPTIVE OPTICS IMAGING OF VY CANIS MAJORIS AT 2-5 μm WITH LBT/LMIRCam</atitle><jtitle>The Astronomical journal</jtitle><date>2013-10-01</date><risdate>2013</risdate><volume>146</volume><issue>4</issue><spage>1</spage><epage>7</epage><pages>1-7</pages><issn>0004-6256</issn><issn>1538-3881</issn><eissn>1538-3881</eissn><abstract>We present adaptive optics images of the extreme red supergiant VY Canis Majoris in the K sub(s), L', and M bands (2.15-4.8 mu m) made with LMIRCam on the Large Binocular Telescope. The peculiar "Southwest Clump" previously imaged from 1 to 2.2 mu m appears prominently in all three filters. We find its brightness is due almost entirely to scattering, with the contribution of thermal emission limited to at most 25%. We model its brightness as optically thick scattering from silicate dust grains using typical size distributions. We find a lower limit mass for this single feature of 5 x 10 super(-3) M sub([middot in circle]) to 2.5 x 10 super(-2) M sub([middot in circle]) depending on the assumed gas-to-dust ratio. The presence of the Clump as a distinct feature with no apparent counterpart on the other side of the star is suggestive of an ejection event from a localized region of the star and is consistent with VY CMa's history of asymmetric high-mass-loss events.</abstract><cop>United States</cop><doi>10.1088/0004-6256/146/4/90</doi><tpages>7</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Adaptive optics ASTRONOMY ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ASYMMETRY BRIGHTNESS Clumps COSMIC DUST Ejection FILTERS Imaging MASS TRANSFER OPTICS Scattering SILICATES Stars STELLAR WINDS TELESCOPES |
| title | ADAPTIVE OPTICS IMAGING OF VY CANIS MAJORIS AT 2-5 μm WITH LBT/LMIRCam |
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