KMT-2019-BLG-2073: Fourth Free-floating Planet Candidate with θ E < 10 μas
We analyze the very short Einstein timescale ( t E ≃ 7 hr) event KMT-2019-BLG-2073. Making use of the pronounced finite-source effects generated by the clump giant source, we measure the Einstein radius θ E ≃ 4.8 μ as and so infer a mass M = 59 M ⊕ ( π rel / 16 μ as ) − 1 , where π rel is the lens-s...
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| Veröffentlicht in: | The Astronomical journal 2021-07, Vol.162 (1), p.15 |
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| creator | Kim, Hyoun-Woo Hwang, Kyu-Ha Gould, Andrew Yee, Jennifer C. Ryu, Yoon-Hyun Albrow, Michael D. Chung, Sun-Ju Han, Cheongho Kil Jung, Youn Lee, Chung-Uk Shin, In-Gu Shvartzvald, Yossi Zang, Weicheng Cha, Sang-Mok Kim, Dong-Jin Kim, Seung-Lee Lee, Dong-Joo Lee, Yongseok Park, Byeong-Gon Pogge, Richard W. |
| description | We analyze the very short Einstein timescale (
t
E
≃ 7 hr) event KMT-2019-BLG-2073. Making use of the pronounced finite-source effects generated by the clump giant source, we measure the Einstein radius
θ
E
≃ 4.8
μ
as and so infer a mass
M
=
59
M
⊕
(
π
rel
/
16
μ
as
)
−
1
, where
π
rel
is the lens-source relative parallax. We find no significant evidence for a host of this planetary-mass object, though one could be present at sufficiently wide separation. If so, it would be detectable after about 10 yr. This is the fourth isolated microlens with a measured Einstein radius
θ
E
< 10
μ
as, which we argue is a useful threshold for a “likely free-floating planet (FFP)” candidate. We outline a new approach to constructing a homogeneous sample of giant-star finite-source/point-lens (FSPL) events, within which the subsample of FFP candidates can be statistically analyzed. We illustrate this approach using 2019 KMTNet data and show that there appears to be a large
θ
E
gap between the two FFP candidates and the 11 other FSPL events. We argue that such sharp features are more identifiable in a sample selected on
θ
E
compared to the traditional approach of identifying candidates based on short
t
E
. |
| doi_str_mv | 10.3847/1538-3881/abfc4a |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_O3W</sourceid><recordid>TN_cdi_proquest_journals_2540807439</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2540807439</sourcerecordid><originalsourceid>FETCH-LOGICAL-c265a-5d38d44130b02b1231f853936d53f0c6f476781ac0a694d798d06a1f8a4ee403</originalsourceid><addsrcrecordid>eNp1kL9OwzAQhy0EEqWwM1pixfQc_4mDWKBqCyIIhu6WG9uQqiTFToV4Mwaeoc-EqyCYmO50-u53pw-hUwoXTPF8RAVThClFR2bhK2720OB3tI8GAMCJzIQ8REcxLgEoVcAHqLx_mJMMaEFuyllqcnaJp-0mdC94GpwjftWarm6e8dPKNK7DY9PY2prO4fc6MdtPPMFXmALefpl4jA68WUV38lOHaD6dzMe3pHyc3Y2vS1JlUhgiLFOWc8pgAdmCZox6JVjBpBXMQyU9z2WuqKnAyILbvFAWpEmQ4c5xYEN01seuQ_u2cbHTy_Rxky7qTHBQkPOUNkTQU1VoYwzO63WoX0340BT0Tpne-dE7P7pXllbO-5W6Xf9l_ot_A6VSaYQ</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2540807439</pqid></control><display><type>article</type><title>KMT-2019-BLG-2073: Fourth Free-floating Planet Candidate with θ E < 10 μas</title><source>IOP Publishing Free Content</source><creator>Kim, Hyoun-Woo ; Hwang, Kyu-Ha ; Gould, Andrew ; Yee, Jennifer C. ; Ryu, Yoon-Hyun ; Albrow, Michael D. ; Chung, Sun-Ju ; Han, Cheongho ; Kil Jung, Youn ; Lee, Chung-Uk ; Shin, In-Gu ; Shvartzvald, Yossi ; Zang, Weicheng ; Cha, Sang-Mok ; Kim, Dong-Jin ; Kim, Seung-Lee ; Lee, Dong-Joo ; Lee, Yongseok ; Park, Byeong-Gon ; Pogge, Richard W.</creator><creatorcontrib>Kim, Hyoun-Woo ; Hwang, Kyu-Ha ; Gould, Andrew ; Yee, Jennifer C. ; Ryu, Yoon-Hyun ; Albrow, Michael D. ; Chung, Sun-Ju ; Han, Cheongho ; Kil Jung, Youn ; Lee, Chung-Uk ; Shin, In-Gu ; Shvartzvald, Yossi ; Zang, Weicheng ; Cha, Sang-Mok ; Kim, Dong-Jin ; Kim, Seung-Lee ; Lee, Dong-Joo ; Lee, Yongseok ; Park, Byeong-Gon ; Pogge, Richard W.</creatorcontrib><description>We analyze the very short Einstein timescale (
t
E
≃ 7 hr) event KMT-2019-BLG-2073. Making use of the pronounced finite-source effects generated by the clump giant source, we measure the Einstein radius
θ
E
≃ 4.8
μ
as and so infer a mass
M
=
59
M
⊕
(
π
rel
/
16
μ
as
)
−
1
, where
π
rel
is the lens-source relative parallax. We find no significant evidence for a host of this planetary-mass object, though one could be present at sufficiently wide separation. If so, it would be detectable after about 10 yr. This is the fourth isolated microlens with a measured Einstein radius
θ
E
< 10
μ
as, which we argue is a useful threshold for a “likely free-floating planet (FFP)” candidate. We outline a new approach to constructing a homogeneous sample of giant-star finite-source/point-lens (FSPL) events, within which the subsample of FFP candidates can be statistically analyzed. We illustrate this approach using 2019 KMTNet data and show that there appears to be a large
θ
E
gap between the two FFP candidates and the 11 other FSPL events. We argue that such sharp features are more identifiable in a sample selected on
θ
E
compared to the traditional approach of identifying candidates based on short
t
E
.</description><identifier>ISSN: 0004-6256</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/1538-3881/abfc4a</identifier><language>eng</language><publisher>Madison: The American Astronomical Society</publisher><subject>Astronomy ; Candidates ; Extrasolar planets ; Giant stars ; Gravitational microlensing exoplanet detection ; Microlenses ; Parallax ; Planets ; Rogue planets</subject><ispartof>The Astronomical journal, 2021-07, Vol.162 (1), p.15</ispartof><rights>2021. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Jul 2021</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c265a-5d38d44130b02b1231f853936d53f0c6f476781ac0a694d798d06a1f8a4ee403</citedby><cites>FETCH-LOGICAL-c265a-5d38d44130b02b1231f853936d53f0c6f476781ac0a694d798d06a1f8a4ee403</cites><orcidid>0000-0003-1525-5041 ; 0000-0003-0043-3925 ; 0000-0001-8263-1006 ; 0000-0003-1435-3053 ; 0000-0002-6982-7722 ; 0000-0002-2641-9964 ; 0000-0002-9241-4117 ; 0000-0001-9823-2907 ; 0000-0002-0314-6000 ; 0000-0001-9481-7123 ; 0000-0003-3316-4012 ; 0000-0002-4355-9838 ; 0000-0003-0562-5643 ; 0000-0001-6285-4528 ; 0000-0001-6000-3463</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/abfc4a/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>314,776,780,27901,27902,38845,38867,53815,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/abfc4a$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc></links><search><creatorcontrib>Kim, Hyoun-Woo</creatorcontrib><creatorcontrib>Hwang, Kyu-Ha</creatorcontrib><creatorcontrib>Gould, Andrew</creatorcontrib><creatorcontrib>Yee, Jennifer C.</creatorcontrib><creatorcontrib>Ryu, Yoon-Hyun</creatorcontrib><creatorcontrib>Albrow, Michael D.</creatorcontrib><creatorcontrib>Chung, Sun-Ju</creatorcontrib><creatorcontrib>Han, Cheongho</creatorcontrib><creatorcontrib>Kil Jung, Youn</creatorcontrib><creatorcontrib>Lee, Chung-Uk</creatorcontrib><creatorcontrib>Shin, In-Gu</creatorcontrib><creatorcontrib>Shvartzvald, Yossi</creatorcontrib><creatorcontrib>Zang, Weicheng</creatorcontrib><creatorcontrib>Cha, Sang-Mok</creatorcontrib><creatorcontrib>Kim, Dong-Jin</creatorcontrib><creatorcontrib>Kim, Seung-Lee</creatorcontrib><creatorcontrib>Lee, Dong-Joo</creatorcontrib><creatorcontrib>Lee, Yongseok</creatorcontrib><creatorcontrib>Park, Byeong-Gon</creatorcontrib><creatorcontrib>Pogge, Richard W.</creatorcontrib><title>KMT-2019-BLG-2073: Fourth Free-floating Planet Candidate with θ E < 10 μas</title><title>The Astronomical journal</title><addtitle>AJ</addtitle><addtitle>Astron. J</addtitle><description>We analyze the very short Einstein timescale (
t
E
≃ 7 hr) event KMT-2019-BLG-2073. Making use of the pronounced finite-source effects generated by the clump giant source, we measure the Einstein radius
θ
E
≃ 4.8
μ
as and so infer a mass
M
=
59
M
⊕
(
π
rel
/
16
μ
as
)
−
1
, where
π
rel
is the lens-source relative parallax. We find no significant evidence for a host of this planetary-mass object, though one could be present at sufficiently wide separation. If so, it would be detectable after about 10 yr. This is the fourth isolated microlens with a measured Einstein radius
θ
E
< 10
μ
as, which we argue is a useful threshold for a “likely free-floating planet (FFP)” candidate. We outline a new approach to constructing a homogeneous sample of giant-star finite-source/point-lens (FSPL) events, within which the subsample of FFP candidates can be statistically analyzed. We illustrate this approach using 2019 KMTNet data and show that there appears to be a large
θ
E
gap between the two FFP candidates and the 11 other FSPL events. We argue that such sharp features are more identifiable in a sample selected on
θ
E
compared to the traditional approach of identifying candidates based on short
t
E
.</description><subject>Astronomy</subject><subject>Candidates</subject><subject>Extrasolar planets</subject><subject>Giant stars</subject><subject>Gravitational microlensing exoplanet detection</subject><subject>Microlenses</subject><subject>Parallax</subject><subject>Planets</subject><subject>Rogue planets</subject><issn>0004-6256</issn><issn>1538-3881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNp1kL9OwzAQhy0EEqWwM1pixfQc_4mDWKBqCyIIhu6WG9uQqiTFToV4Mwaeoc-EqyCYmO50-u53pw-hUwoXTPF8RAVThClFR2bhK2720OB3tI8GAMCJzIQ8REcxLgEoVcAHqLx_mJMMaEFuyllqcnaJp-0mdC94GpwjftWarm6e8dPKNK7DY9PY2prO4fc6MdtPPMFXmALefpl4jA68WUV38lOHaD6dzMe3pHyc3Y2vS1JlUhgiLFOWc8pgAdmCZox6JVjBpBXMQyU9z2WuqKnAyILbvFAWpEmQ4c5xYEN01seuQ_u2cbHTy_Rxky7qTHBQkPOUNkTQU1VoYwzO63WoX0340BT0Tpne-dE7P7pXllbO-5W6Xf9l_ot_A6VSaYQ</recordid><startdate>20210701</startdate><enddate>20210701</enddate><creator>Kim, Hyoun-Woo</creator><creator>Hwang, Kyu-Ha</creator><creator>Gould, Andrew</creator><creator>Yee, Jennifer C.</creator><creator>Ryu, Yoon-Hyun</creator><creator>Albrow, Michael D.</creator><creator>Chung, Sun-Ju</creator><creator>Han, Cheongho</creator><creator>Kil Jung, Youn</creator><creator>Lee, Chung-Uk</creator><creator>Shin, In-Gu</creator><creator>Shvartzvald, Yossi</creator><creator>Zang, Weicheng</creator><creator>Cha, Sang-Mok</creator><creator>Kim, Dong-Jin</creator><creator>Kim, Seung-Lee</creator><creator>Lee, Dong-Joo</creator><creator>Lee, Yongseok</creator><creator>Park, Byeong-Gon</creator><creator>Pogge, Richard W.</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/0000-0003-1525-5041</orcidid><orcidid>https://orcid.org/0000-0003-0043-3925</orcidid><orcidid>https://orcid.org/0000-0001-8263-1006</orcidid><orcidid>https://orcid.org/0000-0003-1435-3053</orcidid><orcidid>https://orcid.org/0000-0002-6982-7722</orcidid><orcidid>https://orcid.org/0000-0002-2641-9964</orcidid><orcidid>https://orcid.org/0000-0002-9241-4117</orcidid><orcidid>https://orcid.org/0000-0001-9823-2907</orcidid><orcidid>https://orcid.org/0000-0002-0314-6000</orcidid><orcidid>https://orcid.org/0000-0001-9481-7123</orcidid><orcidid>https://orcid.org/0000-0003-3316-4012</orcidid><orcidid>https://orcid.org/0000-0002-4355-9838</orcidid><orcidid>https://orcid.org/0000-0003-0562-5643</orcidid><orcidid>https://orcid.org/0000-0001-6285-4528</orcidid><orcidid>https://orcid.org/0000-0001-6000-3463</orcidid></search><sort><creationdate>20210701</creationdate><title>KMT-2019-BLG-2073: Fourth Free-floating Planet Candidate with θ E < 10 μas</title><author>Kim, Hyoun-Woo ; Hwang, Kyu-Ha ; Gould, Andrew ; Yee, Jennifer C. ; Ryu, Yoon-Hyun ; Albrow, Michael D. ; Chung, Sun-Ju ; Han, Cheongho ; Kil Jung, Youn ; Lee, Chung-Uk ; Shin, In-Gu ; Shvartzvald, Yossi ; Zang, Weicheng ; Cha, Sang-Mok ; Kim, Dong-Jin ; Kim, Seung-Lee ; Lee, Dong-Joo ; Lee, Yongseok ; Park, Byeong-Gon ; Pogge, Richard W.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c265a-5d38d44130b02b1231f853936d53f0c6f476781ac0a694d798d06a1f8a4ee403</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Astronomy</topic><topic>Candidates</topic><topic>Extrasolar planets</topic><topic>Giant stars</topic><topic>Gravitational microlensing exoplanet detection</topic><topic>Microlenses</topic><topic>Parallax</topic><topic>Planets</topic><topic>Rogue planets</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kim, Hyoun-Woo</creatorcontrib><creatorcontrib>Hwang, Kyu-Ha</creatorcontrib><creatorcontrib>Gould, Andrew</creatorcontrib><creatorcontrib>Yee, Jennifer C.</creatorcontrib><creatorcontrib>Ryu, Yoon-Hyun</creatorcontrib><creatorcontrib>Albrow, Michael D.</creatorcontrib><creatorcontrib>Chung, Sun-Ju</creatorcontrib><creatorcontrib>Han, Cheongho</creatorcontrib><creatorcontrib>Kil Jung, Youn</creatorcontrib><creatorcontrib>Lee, Chung-Uk</creatorcontrib><creatorcontrib>Shin, In-Gu</creatorcontrib><creatorcontrib>Shvartzvald, Yossi</creatorcontrib><creatorcontrib>Zang, Weicheng</creatorcontrib><creatorcontrib>Cha, Sang-Mok</creatorcontrib><creatorcontrib>Kim, Dong-Jin</creatorcontrib><creatorcontrib>Kim, Seung-Lee</creatorcontrib><creatorcontrib>Lee, Dong-Joo</creatorcontrib><creatorcontrib>Lee, Yongseok</creatorcontrib><creatorcontrib>Park, Byeong-Gon</creatorcontrib><creatorcontrib>Pogge, Richard W.</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 Astronomical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Kim, Hyoun-Woo</au><au>Hwang, Kyu-Ha</au><au>Gould, Andrew</au><au>Yee, Jennifer C.</au><au>Ryu, Yoon-Hyun</au><au>Albrow, Michael D.</au><au>Chung, Sun-Ju</au><au>Han, Cheongho</au><au>Kil Jung, Youn</au><au>Lee, Chung-Uk</au><au>Shin, In-Gu</au><au>Shvartzvald, Yossi</au><au>Zang, Weicheng</au><au>Cha, Sang-Mok</au><au>Kim, Dong-Jin</au><au>Kim, Seung-Lee</au><au>Lee, Dong-Joo</au><au>Lee, Yongseok</au><au>Park, Byeong-Gon</au><au>Pogge, Richard W.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>KMT-2019-BLG-2073: Fourth Free-floating Planet Candidate with θ E < 10 μas</atitle><jtitle>The Astronomical journal</jtitle><stitle>AJ</stitle><addtitle>Astron. J</addtitle><date>2021-07-01</date><risdate>2021</risdate><volume>162</volume><issue>1</issue><spage>15</spage><pages>15-</pages><issn>0004-6256</issn><eissn>1538-3881</eissn><abstract>We analyze the very short Einstein timescale (
t
E
≃ 7 hr) event KMT-2019-BLG-2073. Making use of the pronounced finite-source effects generated by the clump giant source, we measure the Einstein radius
θ
E
≃ 4.8
μ
as and so infer a mass
M
=
59
M
⊕
(
π
rel
/
16
μ
as
)
−
1
, where
π
rel
is the lens-source relative parallax. We find no significant evidence for a host of this planetary-mass object, though one could be present at sufficiently wide separation. If so, it would be detectable after about 10 yr. This is the fourth isolated microlens with a measured Einstein radius
θ
E
< 10
μ
as, which we argue is a useful threshold for a “likely free-floating planet (FFP)” candidate. We outline a new approach to constructing a homogeneous sample of giant-star finite-source/point-lens (FSPL) events, within which the subsample of FFP candidates can be statistically analyzed. We illustrate this approach using 2019 KMTNet data and show that there appears to be a large
θ
E
gap between the two FFP candidates and the 11 other FSPL events. We argue that such sharp features are more identifiable in a sample selected on
θ
E
compared to the traditional approach of identifying candidates based on short
t
E
.</abstract><cop>Madison</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-3881/abfc4a</doi><tpages>19</tpages><orcidid>https://orcid.org/0000-0003-1525-5041</orcidid><orcidid>https://orcid.org/0000-0003-0043-3925</orcidid><orcidid>https://orcid.org/0000-0001-8263-1006</orcidid><orcidid>https://orcid.org/0000-0003-1435-3053</orcidid><orcidid>https://orcid.org/0000-0002-6982-7722</orcidid><orcidid>https://orcid.org/0000-0002-2641-9964</orcidid><orcidid>https://orcid.org/0000-0002-9241-4117</orcidid><orcidid>https://orcid.org/0000-0001-9823-2907</orcidid><orcidid>https://orcid.org/0000-0002-0314-6000</orcidid><orcidid>https://orcid.org/0000-0001-9481-7123</orcidid><orcidid>https://orcid.org/0000-0003-3316-4012</orcidid><orcidid>https://orcid.org/0000-0002-4355-9838</orcidid><orcidid>https://orcid.org/0000-0003-0562-5643</orcidid><orcidid>https://orcid.org/0000-0001-6285-4528</orcidid><orcidid>https://orcid.org/0000-0001-6000-3463</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 0004-6256 |
| ispartof | The Astronomical journal, 2021-07, Vol.162 (1), p.15 |
| issn | 0004-6256 1538-3881 |
| language | eng |
| recordid | cdi_proquest_journals_2540807439 |
| source | IOP Publishing Free Content |
| subjects | Astronomy Candidates Extrasolar planets Giant stars Gravitational microlensing exoplanet detection Microlenses Parallax Planets Rogue planets |
| title | KMT-2019-BLG-2073: Fourth Free-floating Planet Candidate with θ E < 10 μas |
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