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ALMA Observations of the Protostar L1527 IRS: Probing Details of the Disk and the Envelope Structures
We have recently observed the Class 0/I protostar L1527 IRS using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 1 in 220 GHz dust continuum and C18O ( J = 2 − 1 ) line emissions with a ∼2 times higher angular resolution ( ∼ 0 5 ) and ∼4 times better sensitivity than our AL...
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Published in: | The Astrophysical journal 2017-11, Vol.849 (1), p.56 |
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creator | Aso, Yusuke Ohashi, Nagayoshi Aikawa, Yuri Machida, Masahiro N. Saigo, Kazuya Saito, Masao Takakuwa, Shigehisa Tomida, Kengo Tomisaka, Kohji Yen, Hsi-Wei |
description | We have recently observed the Class 0/I protostar L1527 IRS using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 1 in 220 GHz dust continuum and C18O ( J = 2 − 1 ) line emissions with a ∼2 times higher angular resolution ( ∼ 0 5 ) and ∼4 times better sensitivity than our ALMA Cycle 0 observations. Continuum emission shows elongation perpendicular to the associated outflow, with a deconvolved size of 0 53 × 0 15 . C18O emission shows similar elongation, indicating that both emissions trace the disk and the flattened envelope surrounding the protostar. The velocity gradient of the C18O emission along the elongation due to rotation of the disk/envelope system is reanalyzed, identifying Keplerian rotation proportional to r − 0.5 more clearly than the Cycle 0 observations. The Keplerian-disk radius and the dynamical stellar mass are kinematically estimated to be ∼74 au and ∼ 0.45 M ☉ , respectively. The continuum visibility is fitted by models without any annulus averaging, revealing that the disk is in hydrostatic equilibrium. The best-fit model also suggests a density jump by a factor of ∼5 between the disk and the envelope, suggesting that disks around protostars can be geometrically distinguishable from the envelope from a viewpoint of density contrast. Importantly, the disk radius geometrically identified with the density jump is consistent with the kinematically estimated radius. Possible origin of the density jump due to the mass accretion from the envelope to the disk is discussed. C18O observations can be reproduced by the same geometrical structures derived from the dust observations, with possible C18O freeze-out and localized C18O desorption. |
doi_str_mv | 10.3847/1538-4357/aa8264 |
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Continuum emission shows elongation perpendicular to the associated outflow, with a deconvolved size of 0 53 × 0 15 . C18O emission shows similar elongation, indicating that both emissions trace the disk and the flattened envelope surrounding the protostar. The velocity gradient of the C18O emission along the elongation due to rotation of the disk/envelope system is reanalyzed, identifying Keplerian rotation proportional to r − 0.5 more clearly than the Cycle 0 observations. The Keplerian-disk radius and the dynamical stellar mass are kinematically estimated to be ∼74 au and ∼ 0.45 M ☉ , respectively. The continuum visibility is fitted by models without any annulus averaging, revealing that the disk is in hydrostatic equilibrium. The best-fit model also suggests a density jump by a factor of ∼5 between the disk and the envelope, suggesting that disks around protostars can be geometrically distinguishable from the envelope from a viewpoint of density contrast. Importantly, the disk radius geometrically identified with the density jump is consistent with the kinematically estimated radius. Possible origin of the density jump due to the mass accretion from the envelope to the disk is discussed. C18O observations can be reproduced by the same geometrical structures derived from the dust observations, with possible C18O freeze-out and localized C18O desorption.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aa8264</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Accretion disks ; Angular resolution ; Astrophysics ; circumstellar matter ; Continuum radiation ; Density ; Deposition ; Dust ; Elongation ; Emission ; Emissions ; Protostars ; Radio telescopes ; Rotating disks ; Rotation ; stars: individual (L1527 IRS) ; stars: low-mass ; stars: protostars ; Stellar mass ; Velocity gradient ; Visibility</subject><ispartof>The Astrophysical journal, 2017-11, Vol.849 (1), p.56</ispartof><rights>2017. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Nov 01, 2017</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c416t-f68d14dfffdfd585840c1b2b3282cfb5b5f4dc74d9c391375fb76211782c21073</citedby><cites>FETCH-LOGICAL-c416t-f68d14dfffdfd585840c1b2b3282cfb5b5f4dc74d9c391375fb76211782c21073</cites><orcidid>0000-0003-1412-893X ; 0000-0003-0769-8627 ; 0000-0003-2726-0892 ; 0000-0003-1549-6435 ; 0000-0003-3283-6884 ; 0000-0003-0998-5064 ; 0000-0002-0963-0872 ; 0000-0002-8238-7709 ; 0000-0001-8105-8113 ; 0000-0003-0845-128X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids></links><search><creatorcontrib>Aso, Yusuke</creatorcontrib><creatorcontrib>Ohashi, Nagayoshi</creatorcontrib><creatorcontrib>Aikawa, Yuri</creatorcontrib><creatorcontrib>Machida, Masahiro N.</creatorcontrib><creatorcontrib>Saigo, Kazuya</creatorcontrib><creatorcontrib>Saito, Masao</creatorcontrib><creatorcontrib>Takakuwa, Shigehisa</creatorcontrib><creatorcontrib>Tomida, Kengo</creatorcontrib><creatorcontrib>Tomisaka, Kohji</creatorcontrib><creatorcontrib>Yen, Hsi-Wei</creatorcontrib><title>ALMA Observations of the Protostar L1527 IRS: Probing Details of the Disk and the Envelope Structures</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We have recently observed the Class 0/I protostar L1527 IRS using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 1 in 220 GHz dust continuum and C18O ( J = 2 − 1 ) line emissions with a ∼2 times higher angular resolution ( ∼ 0 5 ) and ∼4 times better sensitivity than our ALMA Cycle 0 observations. Continuum emission shows elongation perpendicular to the associated outflow, with a deconvolved size of 0 53 × 0 15 . C18O emission shows similar elongation, indicating that both emissions trace the disk and the flattened envelope surrounding the protostar. The velocity gradient of the C18O emission along the elongation due to rotation of the disk/envelope system is reanalyzed, identifying Keplerian rotation proportional to r − 0.5 more clearly than the Cycle 0 observations. The Keplerian-disk radius and the dynamical stellar mass are kinematically estimated to be ∼74 au and ∼ 0.45 M ☉ , respectively. The continuum visibility is fitted by models without any annulus averaging, revealing that the disk is in hydrostatic equilibrium. The best-fit model also suggests a density jump by a factor of ∼5 between the disk and the envelope, suggesting that disks around protostars can be geometrically distinguishable from the envelope from a viewpoint of density contrast. Importantly, the disk radius geometrically identified with the density jump is consistent with the kinematically estimated radius. Possible origin of the density jump due to the mass accretion from the envelope to the disk is discussed. C18O observations can be reproduced by the same geometrical structures derived from the dust observations, with possible C18O freeze-out and localized C18O desorption.</description><subject>Accretion disks</subject><subject>Angular resolution</subject><subject>Astrophysics</subject><subject>circumstellar matter</subject><subject>Continuum radiation</subject><subject>Density</subject><subject>Deposition</subject><subject>Dust</subject><subject>Elongation</subject><subject>Emission</subject><subject>Emissions</subject><subject>Protostars</subject><subject>Radio telescopes</subject><subject>Rotating disks</subject><subject>Rotation</subject><subject>stars: individual (L1527 IRS)</subject><subject>stars: low-mass</subject><subject>stars: protostars</subject><subject>Stellar mass</subject><subject>Velocity gradient</subject><subject>Visibility</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNp1kN1LwzAUxYMoOKfvPgZ8ta75alLfxjZ1UJk4Bd9C2ibaOZuapAP_e1sr88mny7n3nHPhB8A5iq-IoHyCGBERJYxPlBI4oQdgtF8dglEcxzRKCH85Bifeb3qJ03QE9DS7n8JV7rXbqVDZ2kNrYHjT8MHZYH1QDmaIYQ6Xj-vrfplX9Suc66Cq7d47r_w7VHX5Ixb1Tm9to-E6uLYIrdP-FBwZtfX67HeOwfPN4ml2F2Wr2-VsmkUFRUmITCJKREtjTGlKJpigcYFynBMscGFyljNDy4LTMi1IighnJucJRoh3Z4xiTsbgYuhtnP1stQ9yY1tXdy8lJgkTWIhEdK54cBXOeu-0kY2rPpT7kiiWPUzZk5M9OTnA7CKXQ6SyzV_nv_ZvbVxzkA</recordid><startdate>20171101</startdate><enddate>20171101</enddate><creator>Aso, Yusuke</creator><creator>Ohashi, Nagayoshi</creator><creator>Aikawa, Yuri</creator><creator>Machida, Masahiro N.</creator><creator>Saigo, Kazuya</creator><creator>Saito, Masao</creator><creator>Takakuwa, Shigehisa</creator><creator>Tomida, Kengo</creator><creator>Tomisaka, Kohji</creator><creator>Yen, Hsi-Wei</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0003-1412-893X</orcidid><orcidid>https://orcid.org/0000-0003-0769-8627</orcidid><orcidid>https://orcid.org/0000-0003-2726-0892</orcidid><orcidid>https://orcid.org/0000-0003-1549-6435</orcidid><orcidid>https://orcid.org/0000-0003-3283-6884</orcidid><orcidid>https://orcid.org/0000-0003-0998-5064</orcidid><orcidid>https://orcid.org/0000-0002-0963-0872</orcidid><orcidid>https://orcid.org/0000-0002-8238-7709</orcidid><orcidid>https://orcid.org/0000-0001-8105-8113</orcidid><orcidid>https://orcid.org/0000-0003-0845-128X</orcidid></search><sort><creationdate>20171101</creationdate><title>ALMA Observations of the Protostar L1527 IRS: Probing Details of the Disk and the Envelope Structures</title><author>Aso, Yusuke ; Ohashi, Nagayoshi ; Aikawa, Yuri ; Machida, Masahiro N. ; Saigo, Kazuya ; Saito, Masao ; Takakuwa, Shigehisa ; Tomida, Kengo ; Tomisaka, Kohji ; Yen, Hsi-Wei</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c416t-f68d14dfffdfd585840c1b2b3282cfb5b5f4dc74d9c391375fb76211782c21073</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Accretion disks</topic><topic>Angular resolution</topic><topic>Astrophysics</topic><topic>circumstellar matter</topic><topic>Continuum radiation</topic><topic>Density</topic><topic>Deposition</topic><topic>Dust</topic><topic>Elongation</topic><topic>Emission</topic><topic>Emissions</topic><topic>Protostars</topic><topic>Radio telescopes</topic><topic>Rotating disks</topic><topic>Rotation</topic><topic>stars: individual (L1527 IRS)</topic><topic>stars: low-mass</topic><topic>stars: protostars</topic><topic>Stellar mass</topic><topic>Velocity gradient</topic><topic>Visibility</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aso, Yusuke</creatorcontrib><creatorcontrib>Ohashi, Nagayoshi</creatorcontrib><creatorcontrib>Aikawa, Yuri</creatorcontrib><creatorcontrib>Machida, Masahiro N.</creatorcontrib><creatorcontrib>Saigo, Kazuya</creatorcontrib><creatorcontrib>Saito, Masao</creatorcontrib><creatorcontrib>Takakuwa, Shigehisa</creatorcontrib><creatorcontrib>Tomida, Kengo</creatorcontrib><creatorcontrib>Tomisaka, Kohji</creatorcontrib><creatorcontrib>Yen, Hsi-Wei</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</fulltext></delivery><addata><au>Aso, Yusuke</au><au>Ohashi, Nagayoshi</au><au>Aikawa, Yuri</au><au>Machida, Masahiro N.</au><au>Saigo, Kazuya</au><au>Saito, Masao</au><au>Takakuwa, Shigehisa</au><au>Tomida, Kengo</au><au>Tomisaka, Kohji</au><au>Yen, Hsi-Wei</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>ALMA Observations of the Protostar L1527 IRS: Probing Details of the Disk and the Envelope Structures</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2017-11-01</date><risdate>2017</risdate><volume>849</volume><issue>1</issue><spage>56</spage><pages>56-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We have recently observed the Class 0/I protostar L1527 IRS using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 1 in 220 GHz dust continuum and C18O ( J = 2 − 1 ) line emissions with a ∼2 times higher angular resolution ( ∼ 0 5 ) and ∼4 times better sensitivity than our ALMA Cycle 0 observations. Continuum emission shows elongation perpendicular to the associated outflow, with a deconvolved size of 0 53 × 0 15 . C18O emission shows similar elongation, indicating that both emissions trace the disk and the flattened envelope surrounding the protostar. The velocity gradient of the C18O emission along the elongation due to rotation of the disk/envelope system is reanalyzed, identifying Keplerian rotation proportional to r − 0.5 more clearly than the Cycle 0 observations. The Keplerian-disk radius and the dynamical stellar mass are kinematically estimated to be ∼74 au and ∼ 0.45 M ☉ , respectively. The continuum visibility is fitted by models without any annulus averaging, revealing that the disk is in hydrostatic equilibrium. The best-fit model also suggests a density jump by a factor of ∼5 between the disk and the envelope, suggesting that disks around protostars can be geometrically distinguishable from the envelope from a viewpoint of density contrast. Importantly, the disk radius geometrically identified with the density jump is consistent with the kinematically estimated radius. Possible origin of the density jump due to the mass accretion from the envelope to the disk is discussed. C18O observations can be reproduced by the same geometrical structures derived from the dust observations, with possible C18O freeze-out and localized C18O desorption.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/aa8264</doi><tpages>15</tpages><orcidid>https://orcid.org/0000-0003-1412-893X</orcidid><orcidid>https://orcid.org/0000-0003-0769-8627</orcidid><orcidid>https://orcid.org/0000-0003-2726-0892</orcidid><orcidid>https://orcid.org/0000-0003-1549-6435</orcidid><orcidid>https://orcid.org/0000-0003-3283-6884</orcidid><orcidid>https://orcid.org/0000-0003-0998-5064</orcidid><orcidid>https://orcid.org/0000-0002-0963-0872</orcidid><orcidid>https://orcid.org/0000-0002-8238-7709</orcidid><orcidid>https://orcid.org/0000-0001-8105-8113</orcidid><orcidid>https://orcid.org/0000-0003-0845-128X</orcidid><oa>free_for_read</oa></addata></record> |
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subjects | Accretion disks Angular resolution Astrophysics circumstellar matter Continuum radiation Density Deposition Dust Elongation Emission Emissions Protostars Radio telescopes Rotating disks Rotation stars: individual (L1527 IRS) stars: low-mass stars: protostars Stellar mass Velocity gradient Visibility |
title | ALMA Observations of the Protostar L1527 IRS: Probing Details of the Disk and the Envelope Structures |
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