View source for Astronomy:IM Lupi

{{Short description|Pre-main-sequence star in the constellation Lupus}}
{{Starbox begin
|name=IM Lupi
}}
{{Starbox image
|image=[[File:Eso1811c(1).jpg|250px]]
|caption=VLT/SPHERE scattered light image of the disk around IM Lupi. The gray circle shows the position of the star.
|credit=ESO/H. Avenhaus et al./DARTT-S collaboration
}}
{{Starbox observe
| epoch = J2000
| constell = [[Astronomy:Lupus (constellation)|Lupus]]
| ra = {{RA|15|56|09.2067}}<ref name="Gaia DR3">{{Cite journal |last=Gaia Collaboration |date=2020-11-01 |title=VizieR Online Data Catalog: Gaia EDR3 (Gaia Collaboration, 2020) |url=https://ui.adsabs.harvard.edu/abs/2020yCat.1350....0G |journal=VizieR Online Data Catalog |pages=I/350|bibcode=2020yCat.1350....0G }}</ref> 
| dec = {{DEC|-37|56|06.1261}}<ref name="Gaia DR3"/>
| appmag_v = 11.93
}}
{{Starbox character
| type = Young Stellar Object
| class = M0<ref name="Salyk"/>
| variable = [[Astronomy:Orion variable|Orion variable]] of [[Astronomy:T Tauri star|T Tauri type]] (INT)<ref>{{Cite journal |last1=Watson |first1=C. L. |last2=Henden |first2=A. A. |last3=Price |first3=A. |date=2006-05-01 |title=The International Variable Star Index (VSX) |url=https://ui.adsabs.harvard.edu/abs/2006SASS...25...47W |journal=Society for Astronomical Sciences Annual Symposium |volume=25 |pages=47|bibcode=2006SASS...25...47W }}</ref>
}}
{{Starbox astrometry
| radial_v = 
| prop_mo_ra = -12.059<ref name="Gaia DR3"/>
| prop_mo_dec =  -23.727<ref name="Gaia DR3"/>
| parallax = 6.4175
| p_error = 0.022
| parallax_footnote = <ref name="Gaia DR3"/>
}}
{{Starbox detail
| source =<ref name="Cleeves"/>
| mass = 1
| radius = 
| temperature = 
| luminosity = 0.9
| gravity = 
| metal_fe = 
| rotation = 
| rotational_velocity = 
| age_myr = 0.5 - 1
}}
{{Starbox catalog
}}
{{Starbox reference
| Simbad = IM+Lup
}}
{{Starbox end}}

IM Lupi is a young stellar object with a surrounding [[Astronomy:Protoplanetary disk|protoplanetary disk]]. The young star is suspected to host a still forming [[Astronomy:Protoplanet|protoplanet]] at a distance of 110 [[Astronomy:Astronomical unit|astronomical units]] (AU) and a mass of 2-3 {{Jupiter mass|link=true}}.<ref name="Hensley">{{Cite web |last=Hensley |first=Kerry |date=2022-08-01 |title=Evidence for a Hidden Planet in IM Lupi's Disk |url=https://aasnova.org/2022/08/01/evidence-for-a-hidden-planet-in-im-lupis-disk/ |access-date=2023-05-27 |website=AAS Nova |language=en-US}}</ref><ref name="Verrios">{{Cite journal |last1=Verrios |first1=Harrison J. |last2=Price |first2=Daniel J. |last3=Pinte |first3=Christophe |last4=Hilder |first4=Thomas |last5=Calcino |first5=Josh |date=2022-07-01 |title=Kinematic Evidence for an Embedded Planet in the IM Lupi Disk |journal=The Astrophysical Journal |volume=934 |issue=1 |pages=L11 |doi=10.3847/2041-8213/ac7f44 |arxiv=2207.02869 |bibcode=2022ApJ...934L..11V |s2cid=250334752 |issn=0004-637X |doi-access=free }}</ref> IM Lupi is 508 [[Astronomy:Light-year|light-years]] (156 [[Astronomy:Parsec|parsec]]) distant.<ref name="Verrios" />

== Star ==
The star IM Lupi was classified as a [[Astronomy:Young stellar object|class II]] YSO with a [[Astronomy:Stellar classification#Class M|spectral type M0]].<ref name="Salyk">{{Cite journal |last1=Salyk |first1=Colette |last2=Herczeg |first2=Gregory J. |last3=Brown |first3=Joanna M. |last4=Blake |first4=Geoffrey A. |last5=Pontoppidan |first5=Klaus M. |last6=van Dishoeck |first6=Ewine F. |date=2013-05-01 |title=Measuring Protoplanetary Disk Accretion with H I Pfund β |url=https://ui.adsabs.harvard.edu/abs/2013ApJ...769...21S |journal=The Astrophysical Journal |volume=769 |issue=1 |pages=21 |doi=10.1088/0004-637X/769/1/21 |arxiv=1303.4804 |bibcode=2013ApJ...769...21S |s2cid=43905871 |issn=0004-637X}}</ref> The star is probably not actively accreting, but there is evidence that the accretion is variable around IM Lupi. The young star is associated with the Lupus 2 Molecular Cloud.<ref name="Cleeves">{{Cite journal |last1=Cleeves |first1=L. Ilsedore |last2=Öberg |first2=Karin I. |last3=Wilner |first3=David J. |last4=Huang |first4=Jane |last5=Loomis |first5=Ryan A. |last6=Andrews |first6=Sean M. |last7=Czekala |first7=Ian |date=2016-12-01 |title=The Coupled Physical Structure of Gas and Dust in the IM Lup Protoplanetary Disk |journal=The Astrophysical Journal |volume=832 |issue=2 |pages=110 |doi=10.3847/0004-637X/832/2/110 |arxiv=1610.00715 |bibcode=2016ApJ...832..110C |s2cid=118347827 |issn=0004-637X |doi-access=free }}</ref> 

== Protoplanetary Disk ==
Many features at different wavelengths have been observed in this disk, which is very massive (0.17 {{Solar mass}}).<ref name="Hensley" /><ref name="Cleeves" /> The disk has a gas and a dust component. The gas component reaches out to 751 AU and the smaller dust component reaches out to 334 AU.  In a scattered light image from [[Astronomy:Spectro-Polarimetric High-Contrast Exoplanet Research|SPHERE]] the upper surface and part of the lower surface was imaged.<ref name="Avenhaus" /> Dust observations with [[Astronomy:Atacama Large Millimeter Array|ALMA]] shows two rings and with SPHERE  2 additional rings were detected.<ref name="Cleeves" /><ref name="Avenhaus">{{Cite journal |last1=Avenhaus |first1=Henning |last2=Quanz |first2=Sascha P. |last3=Garufi |first3=Antonio |last4=Perez |first4=Sebastian |last5=Casassus |first5=Simon |last6=Pinte |first6=Christophe |last7=Bertrang |first7=Gesa H. -M. |last8=Caceres |first8=Claudio |last9=Benisty |first9=Myriam |last10=Dominik |first10=Carsten |date=2018-08-01 |title=Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks |journal=The Astrophysical Journal |volume=863 |issue=1 |pages=44 |doi=10.3847/1538-4357/aab846 |arxiv=1803.10882 |bibcode=2018ApJ...863...44A |s2cid=119260968 |issn=0004-637X |doi-access=free }}</ref> ALMA observations at 1.25 mm shows a spiral pattern,<ref>{{Cite journal |last1=Andrews |first1=Sean M. |last2=Huang |first2=Jane |last3=Pérez |first3=Laura M. |last4=Isella |first4=Andrea |last5=Dullemond |first5=Cornelis P. |last6=Kurtovic |first6=Nicolás T. |last7=Guzmán |first7=Viviana V. |last8=Carpenter |first8=John M. |last9=Wilner |first9=David J. |last10=Zhang |first10=Shangjia |last11=Zhu |first11=Zhaohuan |last12=Birnstiel |first12=Tilman |last13=Bai |first13=Xue-Ning |last14=Benisty |first14=Myriam |last15=Hughes |first15=A. Meredith |date=2018-12-01 |title=The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview |journal=The Astrophysical Journal |volume=869 |issue=2 |pages=L41 |doi=10.3847/2041-8213/aaf741 |arxiv=1812.04040 |bibcode=2018ApJ...869L..41A |s2cid=118934372 |issn=0004-637X |doi-access=free }}</ref> which is also imprinted on the surface of the dusty part as seen by SPHERE.<ref name="Hensley" /> ALMA also observed the molecule [[Chemistry:Carbon monoxide|<sup>12</sup>CO]], which traces the gas component of the disk. The CO observations show several deviations from [[Astronomy:Kepler orbit|Keplerian motion]] in the form of 16 kinks. The kinks and spirals could be caused by an undetected [[Astronomy:Exoplanet|planet]] with a mass of 2-3 {{Jupiter mass}} orbiting at about 110 AU. It is also possible that [[Physics:Gravitational instability|gravitational instability]] causes the patterns in this disk.<ref name="Verrios" />

== References ==
<references />

[[Category:Protoplanets]]
[[Category:Circumstellar disks]]

{{Sourceattribution|IM Lupi}}