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| caption = OTS 44 (orange crosshair) and surrounding nebulae |
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[[File:Brown dwarf OTS 44 with disc.jpg|thumb|An artist's concept of OTS 44's dust disk]] |
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'''OTS 44''' is a [[Free-floating planet|free-floating]] [[planetary-mass object]] or [[brown dwarf]] located at {{Convert|550|ly|pc}} in the [[constellation]] [[Chamaeleon]] near the [[reflection nebula]] [[IC 2631]]. It is among the lowest-mass free-floating substellar objects, with approximately 11.5 times the mass of [[Jupiter]], or approximately 1.1% that of the [[Sun]].<ref name=Bonnefoy2014_AA562/><ref>{{cite journal|last1=Luhmann|first1=K. L.|last2=Peterson|first2=D. E.|last3=Megeath|first3=S. T.|title=Spectroscopic Confirmation of the Least Massive Known Brown Dwarf in Chamaeleon|journal=The Astrophysical Journal|volume=617|issue=1|pages=565–568|date=2004|doi=10.1086/425228|arxiv = astro-ph/0411445 |bibcode = 2004ApJ...617..565L |s2cid=18157277 }}</ref> |
'''OTS 44''' is a [[Free-floating planet|free-floating]] [[planetary-mass object]] or [[brown dwarf]] located at {{Convert|550|ly|pc}} in the [[constellation]] [[Chamaeleon]] near the [[reflection nebula]] [[IC 2631]]. It is among the lowest-mass free-floating substellar objects, with approximately 11.5 times the mass of [[Jupiter]], or approximately 1.1% that of the [[Sun]].<ref name=Bonnefoy2014_AA562/><ref>{{cite journal|last1=Luhmann|first1=K. L.|last2=Peterson|first2=D. E.|last3=Megeath|first3=S. T.|title=Spectroscopic Confirmation of the Least Massive Known Brown Dwarf in Chamaeleon|journal=The Astrophysical Journal|volume=617|issue=1|pages=565–568|date=2004|doi=10.1086/425228|arxiv = astro-ph/0411445 |bibcode = 2004ApJ...617..565L |s2cid=18157277 }}</ref> |
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Its radius is not very well known and is estimated to be 23–57% that of the Sun.<ref name=apj620_1_L51/><ref name=joergens2013_AA558/> |
Its radius is not very well known and is estimated to be 23–57% that of the Sun.<ref name=apj620_1_L51/><ref name=joergens2013_AA558/> |
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OTS 44 was discovered in 1998 by Oasa, Tamura, and Sugitani as a member of the star-forming region Chamaeleon I.<ref name=oasa1998>{{cite journal|last1=Tamura|first1=M.|last2=Itoh|first2=Y.|last3=Oasa|first3=Y.|last4=Nakajima|first4=T.|title=Isolated and Companion Young Brown Dwarfs in the Taurus and Chamaeleon Molecular Clouds|journal=Science|volume=282|issue=5391|date=1998|pages=1095–7|doi=10.1126/science.282.5391.1095|pmid=9804541|bibcode = 1998Sci...282.1095T }}</ref><ref name=oasa1999>{{cite journal|last1=Oasa|first1=Y.|last2=Tamura|first2=M.|last3=Sugitani|first3=K.|title=A Deep Near-Infrared Survey of the Chamaeleon I Dark Cloud Core|journal=The Astrophysical Journal|volume=526|issue=1|pages=336–343|date=1999|doi=10.1086/307964|bibcode = 1999ApJ...526..336O |doi-access=free}}</ref> Based upon infrared observations with the [[Spitzer Space Telescope]] and the [[Herschel Space Observatory]], OTS 44 emits an [[infrared excess|excess of infrared radiation]] for an object of its type, suggesting it has a circumstellar disk of dust and particles of rock and ice.<ref name=apj620_1_L51/><ref name=joergens2013_AA558/><ref>{{cite web|title=Blurring the lines between stars and planets: Lonely planets offer clues to star formation|url=http://www.mpia.de/Public/menu_q2e.php?Aktuelles/PR/2013/PR_2013_09/PR_2013_09_en.html|website=MPIA Science Release 2013-09|access-date=1 September 2014}}</ref> This disk has a mass of at |
OTS 44 was discovered in 1998 by Oasa, Tamura, and Sugitani as a member of the star-forming region Chamaeleon I.<ref name=oasa1998>{{cite journal|last1=Tamura|first1=M.|last2=Itoh|first2=Y.|last3=Oasa|first3=Y.|last4=Nakajima|first4=T.|title=Isolated and Companion Young Brown Dwarfs in the Taurus and Chamaeleon Molecular Clouds|journal=Science|volume=282|issue=5391|date=1998|pages=1095–7|doi=10.1126/science.282.5391.1095|pmid=9804541|bibcode = 1998Sci...282.1095T }}</ref><ref name=oasa1999>{{cite journal|last1=Oasa|first1=Y.|last2=Tamura|first2=M.|last3=Sugitani|first3=K.|title=A Deep Near-Infrared Survey of the Chamaeleon I Dark Cloud Core|journal=The Astrophysical Journal|volume=526|issue=1|pages=336–343|date=1999|doi=10.1086/307964|bibcode = 1999ApJ...526..336O |doi-access=free}}</ref> Based upon infrared observations with the [[Spitzer Space Telescope]] and the [[Herschel Space Observatory]], OTS 44 emits an [[infrared excess|excess of infrared radiation]] for an object of its type, suggesting it has a circumstellar disk of dust and particles of rock and ice.<ref name=apj620_1_L51/><ref name=joergens2013_AA558/><ref>{{cite web|title=Blurring the lines between stars and planets: Lonely planets offer clues to star formation|url=http://www.mpia.de/Public/menu_q2e.php?Aktuelles/PR/2013/PR_2013_09/PR_2013_09_en.html|website=MPIA Science Release 2013-09|access-date=1 September 2014}}</ref> This disk (gas+dust) has a SED-fitted mass of at about 30 Earth masses.<ref name=joergens2013_AA558/> Observations with the SINFONI spectrograph at the [[Very Large Telescope]] show that the disk |
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| ⚫ | is accreting matter at the rate of approximately 10<sup>−11</sup> of the mass of the Sun per year.<ref name=joergens2013_AA558/> It could eventually develop into a [[planetary system]]. Observations with [[Atacama Large Millimeter Array|ALMA]] detected the disk in [[millimeter]] wavelengths. The observations constrained the dust mass of the disk between 0.07 and 0.63 {{Earth mass|link=true}}, but these mass estimates are limited by assumptions on poorly constrained parameters.<ref>{{Cite journal|last1=Bayo|first1=Amelia|last2=Joergens|first2=Viki|last3=Liu|first3=Yao|last4=Brauer|first4=Robert|last5=Olofsson|first5=Johan|last6=Arancibia|first6=Javier|last7=Pinilla|first7=Paola|author7-link= Paola Pinilla |last8=Wolf|first8=Sebastian|last9=Ruge|first9=Jan Philipp|last10=Henning|first10=Thomas|last11=Natta|first11=Antonella|date=May 2017|title=First Millimeter Detection of the Disk around a Young, Isolated, Planetary-mass Object|journal=Astrophysical Journal Letters|language=en|volume=841|issue=1|pages=L11|doi=10.3847/2041-8213/aa7046|bibcode=2017ApJ...841L..11B|issn=0004-637X|hdl=10150/624481|s2cid=73605838 |hdl-access=free |doi-access=free }}</ref> |
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Observations with the SINFONI spectrograph at the [[Very Large Telescope]] show that the disk |
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| ⚫ | is accreting matter at the rate of approximately 10<sup>−11</sup> of the mass of the Sun per year.<ref name=joergens2013_AA558/> It could eventually develop into a [[planetary system]]. Observations with [[Atacama Large Millimeter Array|ALMA]] detected the disk in [[millimeter]] wavelengths. The observations constrained the dust mass of the disk between 0.07 and 0.63 {{Earth mass|link=true}}, but these mass estimates are limited by assumptions on poorly constrained parameters.<ref>{{Cite journal|last1=Bayo|first1=Amelia|last2=Joergens|first2=Viki|last3=Liu|first3=Yao|last4=Brauer|first4=Robert|last5=Olofsson|first5=Johan|last6=Arancibia|first6=Javier|last7=Pinilla|first7=Paola|last8=Wolf|first8=Sebastian|last9=Ruge|first9=Jan Philipp|last10=Henning|first10=Thomas|last11=Natta|first11=Antonella|date=May 2017|title=First Millimeter Detection of the Disk around a Young, Isolated, Planetary-mass Object|journal=Astrophysical Journal Letters|language=en|volume=841|issue=1|pages=L11|doi=10.3847/2041-8213/aa7046|bibcode=2017ApJ...841L..11B|issn=0004-637X|hdl=10150/624481|s2cid=73605838 |hdl-access=free}}</ref> |
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==See also== |
==See also== |
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* [[SCR 1845-6357]], a binary |
* [[SCR 1845-6357]], a binary system comprising a red dwarf and a brown dwarf |
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* [[Cha 110913-773444]], an astronomical object that may be a free-floating planet surrounded by what appears to be a protoplanetary disk |
* [[Cha 110913-773444]], an astronomical object that may be a free-floating planet surrounded by what appears to be a protoplanetary disk |
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==References== |
==References== |
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| |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Chamaeleon |
| Right ascension | 11h10m 11.5s |
| Declination | −76° 32′ 13″ |
| Characteristics | |
| Spectral type | M9.5[1] |
| Astrometry | |
| Distance | 554 ly (170 pc) |
| Details | |
| Mass | 0.011[2] M☉ |
| Radius | 0.23[1]–0.57[3] R☉ |
| Luminosity | 0.0013[1]–0.0024[3] L☉ |
| Temperature | 1,700[2][3]–2,300[1] K |
| Database references | |
| SIMBAD | data |
OTS 44 is a free-floating planetary-mass objectorbrown dwarf located at 550 light-years (170 pc) in the constellation Chamaeleon near the reflection nebula IC 2631. It is among the lowest-mass free-floating substellar objects, with approximately 11.5 times the mass of Jupiter, or approximately 1.1% that of the Sun.[2][4] Its radius is not very well known and is estimated to be 23–57% that of the Sun.[1][3]
OTS 44 was discovered in 1998 by Oasa, Tamura, and Sugitani as a member of the star-forming region Chamaeleon I.[5][6] Based upon infrared observations with the Spitzer Space Telescope and the Herschel Space Observatory, OTS 44 emits an excess of infrared radiation for an object of its type, suggesting it has a circumstellar disk of dust and particles of rock and ice.[1][3][7] This disk (gas+dust) has a SED-fitted mass of at about 30 Earth masses.[3] Observations with the SINFONI spectrograph at the Very Large Telescope show that the disk is accreting matter at the rate of approximately 10−11 of the mass of the Sun per year.[3] It could eventually develop into a planetary system. Observations with ALMA detected the disk in millimeter wavelengths. The observations constrained the dust mass of the disk between 0.07 and 0.63 ME, but these mass estimates are limited by assumptions on poorly constrained parameters.[8]
