|
Alter: pages. Add: bibcode, pmid, pages. Removed URL that duplicated unique identifier. Removed parameters. Formatted dashes. | You can use this bot yourself. Report bugs here. | Activated by Headbomb | via #UCB_webform
|
m task, replaced: journal=ApJL → journal=Astrophysical Journal Letters
|
||
| Line 46: | Line 46: | ||
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|accessdate=1 September 2014}}</ref> This disk has a mass of at least 10 Earth masses.<ref name=joergens2013_AA558/> |
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|accessdate=1 September 2014}}</ref> This disk has a mass of at least 10 Earth masses.<ref name=joergens2013_AA558/> |
||
Observations with the SINFONI spectrograph at the [[Very Large Telescope]] show that the disk |
Observations with the SINFONI spectrograph at the [[Very Large Telescope]] show that the disk |
||
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|last=Bayo|first=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= |
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|last=Bayo|first=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|hdl-access=free}}</ref> |
||
==See also== |
==See also== |
||
| Line 72: | Line 72: | ||
[[Category:Astronomical objects discovered in 1998]] |
[[Category:Astronomical objects discovered in 1998]] |
||
{{Brown-dwarf |
{{Brown-dwarf-stub}} |
||
{{Exoplanet-stub}} |
|||
| |
| 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 has a mass of at least 10 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]
{{cite journal}}: CS1 maint: unflagged free DOI (link)
 | This brown dwarf-related article is a stub. You can help Wikipedia by expanding it. |
 | This extrasolar-planet-related article is a stub. You can help Wikipedia by expanding it. |
