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{{short description|Astronomical objects of planetary size that did not form in orbit around a star }}
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[[Image:Sol Cha-110913-773444 Jupiter.jpg|thumb|A size comparison between the [[Sun]], a young sub-brown dwarf, and [[Jupiter]]. As the sub-brown dwarf ages, it will gradually cool and shrink.]]
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{{Use dmy dates|date=April 2020}}
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[[Image:Sol Cha-110913-773444 Jupiter.jpg|thumb|upright=1.2|Comparison: the [[Sun]] (yellow), a young sub-brown dwarf (red), and [[Jupiter]] (multi-colored). As the sub-brown dwarf ages, it will gradually cool and shrink.]]


A '''sub-brown dwarf''' or '''planetary-mass brown dwarf''' is an astronomical object formed in the same manner as [[star]]s and brown dwarfs (i.e. through the collapse of a [[nebula|gas cloud]]) but that has a [[planetary-mass object|mass below the limiting mass for thermonuclear fusion]] of [[deuterium]] (about {{Jupiter mass|13}}).<ref>[http://www.dtm.ciw.edu/boss/definition.html Working Group on Extrasolar Planets – Definition of a "Planet"] POSITION STATEMENT ON THE DEFINITION OF A "PLANET" (IAU)</ref>
A '''sub-brown dwarf''' or '''planetary-mass brown dwarf''' is an [[astronomical object]] that formed in the same manner as [[star]]s and [[brown dwarf]]s (i.e. through the collapse of a [[Nebula|gas cloud]]) but that has a [[Planetary-mass object|planetary mass]], therefore by definition below the [[Deuterium fusion#In sub-stellar objects|limiting mass]] for [[thermonuclear fusion]] of [[deuterium]] (about {{Jupiter mass|13}}).<ref>[http://www.dtm.ciw.edu/boss/definition.html Working Group on Extrasolar Planets – Definition of a "Planet"] {{webarchive|url=https://web.archive.org/web/20060916161707/http://www.dtm.ciw.edu/boss/definition.html |date=16 September 2006 }} POSITION STATEMENT ON THE DEFINITION OF A "PLANET" (IAU)</ref>
Some researchers call them free-floating planets<ref name="Delorme2012">{{cite journal|last=Delorme|first=P.|title=CFBDSIR2149-0403: a 4–7 Jupiter-mass free-floating planet in the young moving group AB Doradus ?|journal=Astronomy & Astrophysics|date=December 2012|arxiv =1210.0305 |doi = 10.1051/0004-6361/201219984 |bibcode = 2012A&A...548A..26D |display-authors=etal}}</ref> whereas others call them planetary-mass brown dwarfs.<ref name="Luhman20140421">{{cite journal |title=Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun |journal=[[The Astrophysical Journal Letters]] |first=K. L. |last=Luhman |volume=786 |issue=2 |page=L18 |date=21 April 2014 |doi=10.1088/2041-8205/786/2/L18|arxiv = 1404.6501 |bibcode = 2014ApJ...786L..18L }}</ref>
Some researchers include them in the category of [[rogue planet]]s<ref name="Delorme2012">{{cite journal|last=Delorme|first=P.|title=CFBDSIR2149-0403: a 4–7 Jupiter-mass rogue planet in the young moving group AB Doradus ?|journal=Astronomy & Astrophysics|volume=548|pages=A26|date=December 2012|arxiv =1210.0305 |doi = 10.1051/0004-6361/201219984 |bibcode = 2012A&A...548A..26D |s2cid=50935950|display-authors=etal}}</ref> whereas others call them planetary-mass brown dwarfs.<ref name="Luhman20140421">{{cite journal |title=Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun |journal=[[The Astrophysical Journal Letters]] |first=K. L. |last=Luhman |volume=786 |issue=2 |page=L18 |date=21 April 2014 |doi=10.1088/2041-8205/786/2/L18|arxiv = 1404.6501 |bibcode = 2014ApJ...786L..18L |s2cid=119102654 }}</ref>


==Description==
==Sub-brown dwarf or free-floating planet==
Sub-brown dwarfs are formed in the manner of [[star]]s, through the collapse of a [[nebula|gas cloud]] (perhaps with the help of [[photo-erosion]]) but there is no consensus amongst astronomers on whether the formation process should be taken into account when classifying an object as a planet.<ref>[http://www.space.com/scienceastronomy/solarsystem/planet_confusion_001101-1.html What is a Planet? Debate Forces New Definition], by Robert Roy Britt, 02 November 2000</ref> Free-floating sub-brown dwarfs can be observationally indistinguishable from [[rogue planet]]s that originally formed around a star and were ejected from orbit, and on the other hand a sub-brown dwarf formed free-floating in a star cluster may get captured into orbit around a star. A definition for the term "sub-brown dwarf" was put forward by the IAU Working Group on Extra-Solar Planets (WGESP), which defined it as a free-floating body found in young star clusters below the lower mass cut-off of brown dwarfs.<ref>IAU WGESP, [http://www.dtm.ciw.edu/boss/definition.html 'Position Statement on the Definition of "Planet"'], 28 February 2003</ref>
Sub-brown dwarfs are formed in the manner of [[star]]s, through the collapse of a [[nebula|gas cloud]] (perhaps with the help of [[photo-erosion]]) but there is no consensus amongst astronomers on whether the formation process should be taken into account when classifying an object as a planet.<ref>[https://web.archive.org/web/20010502150203/http://www.space.com/scienceastronomy/solarsystem/planet_confusion_001101-1.html What is a Planet? Debate Forces New Definition], by Robert Roy Britt, 2 November 2000</ref> Free-floating sub-brown dwarfs can be observationally indistinguishable from rogue planets, which originally formed around a star and were ejected from orbit. Similarly, a sub-brown dwarf formed free-floating in a star cluster may be captured into orbit around a star, making distinguishing sub-brown dwarfs and large planets also difficult. A definition for the term "sub-brown dwarf" was put forward by the [[IAU Working Group on Extra-Solar Planets]] (WGESP), which defined it as a free-floating body found in young star clusters below the lower mass cut-off of brown dwarfs.<ref>IAU WGESP, [http://www.astro.iag.usp.br/~dinamica/WGEP.html 'Position Statement on the Definition of "Planet"'], 28 February 2003</ref>


===Lower mass limit===
===Lower mass limit===
The smallest mass of gas cloud that could collapse to form a sub-brown dwarf is about 1 [[Jupiter mass]] (M<sub>J</sub>).<ref>{{citation|bibcode=2003IAUS..211..529B|title=Nomenclature: Brown Dwarfs, Gas Giant Planets, and ?|author1=Boss|first1=Alan P.|last2=Basri|first2=Gibor|last3=Kumar|first3=Shiv S.|last4=Liebert|first4=James|last5=Martín|first5=Eduardo L.|last6=Reipurth|first6=Bo|last7=Zinnecker|first7=Hans|volume=211|year=2003|pages=529|journal=Brown Dwarfs }}</ref> This is because to collapse by [[gravity|gravitational]] contraction requires radiating away energy as heat and this is limited by the opacity of the gas.<ref>{{citation|arxiv=0907.2243v1|doi= 10.1088/0004-637X/702/1/805|title=Substellar Objects in Nearby Young Clusters (Sonyc): The Bottom of the Initial Mass Function in Ngc 1333|year=2009|last1=Scholz|first1=Alexander|last2=Geers|first2=Vincent|last3=Jayawardhana|first3=Ray|last4=Fissel|first4=Laura|last5=Lee|first5=Eve|last6=Lafreniere|first6=David|last7=Tamura|first7=Motohide|journal=The Astrophysical Journal|volume=702|pages=805|bibcode = 2009ApJ...702..805S }}</ref> A 3 M<sub>J</sub> candidate is described in the paper.<ref>{{citation|arxiv=0711.2510v1|
The smallest mass of gas cloud that could collapse to form a sub-brown dwarf is about 1 [[Jupiter mass]] (M<sub>J</sub>).<ref>{{citation|bibcode=2003IAUS..211..529B|title=Nomenclature: Brown Dwarfs, Gas Giant Planets, and ?|last1=Boss|first1=Alan P.|last2=Basri|first2=Gibor|last3=Kumar|first3=Shiv S.|last4=Liebert|first4=James|last5=Martín|first5=Eduardo L.|last6=Reipurth|first6=Bo|last7=Zinnecker|first7=Hans|volume=211|year=2003|pages=529|journal=Brown Dwarfs }}</ref> This is because to collapse by [[gravity|gravitational]] contraction requires radiating away energy as heat and this is limited by the opacity of the gas.<ref>{{citation|arxiv=0907.2243v1|doi= 10.1088/0004-637X/702/1/805|title=Substellar Objects in Nearby Young Clusters (Sonyc): The Bottom of the Initial Mass Function in Ngc 1333|year=2009|last1=Scholz|first1=Alexander|last2=Geers|first2=Vincent|last3=Jayawardhana|first3=Ray|last4=Fissel|first4=Laura|last5=Lee|first5=Eve|author5-link=Eve Lee|last6=Lafreniere|first6=David|last7=Tamura|first7=Motohide|journal=The Astrophysical Journal|volume=702|issue= 1|pages=805–822|bibcode = 2009ApJ...702..805S |s2cid= 5102383}}</ref> A 3 M<sub>J</sub> candidate is described in a 2007 paper.<ref>{{citation|arxiv=0711.2510v1|
title=Dusty disks at the bottom of the IMF
title=Dusty disks at the bottom of the IMF
| first1=Aleks |last1=Scholz|first2= Ray|last2= Jayawardhana|year=2007|doi=10.1086/526340|journal=The Astrophysical Journal|volume=672|pages=L49|url=http://iopscience.iop.org/1538-4357/672/1/L49/fulltext/22162.text.html
| first1=Aleks |last1=Scholz|first2= Ray|last2= Jayawardhana|year=2007|doi=10.1086/526340|journal=The Astrophysical Journal|volume=672|issue = 1|pages=L49–L52|bibcode = 2008ApJ...672L..49S }}</ref>
|bibcode = 2008ApJ...672L..49S }}</ref>


== List of possible sub-brown dwarfs ==
== List of possible sub-brown dwarfs ==
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===Orbiting one or more stars===
===Orbiting one or more stars===
There is no consensus whether these companions of stars should be considered sub-brown dwarfs or planets.
There is no consensus whether these companions of stars should be considered sub-brown dwarfs or planets.
* [[2MASS J0441+2301|2MASS J0441+2301 Bb]]
* [[WD 0806-661]] B
* [[DT Virginis]] c
* [[FW Tauri]] b
* [[ROXs 42b]] b


===Orbiting a brown dwarf===
===Orbiting a brown dwarf===
At around 2022 the IAU working definition of an exoplanet excludes these objects as planets.<ref name=":0">{{Cite journal |last1=Etangs |first1=A. Lecavelier des |last2=Lissauer |first2=Jack J. |date=2022-03-17 |title=The IAU Working Definition of an Exoplanet |journal=New Astronomy Reviews |volume=94 |pages=101641 |arxiv=2203.09520 |doi=10.1016/j.newar.2022.101641|bibcode=2022NewAR..9401641L }}</ref> The only fitting label would be as sub-brown dwarfs, but they are more often referred as [[Planetary-mass object|planetary mass objects]]. Other definitions, like from the [[NASA Exoplanet Archive]] or the [[Extrasolar Planets Encyclopaedia]] would include these as exoplanets. There is no consensus whether these companions of brown dwarfs should be considered sub-brown dwarfs or planets.
There is no consensus whether these companions of brown dwarfs should be considered sub-brown dwarfs or planets.

* The 5–10M<sub>J</sub> companion of [[2MASS J04414489+2301513]]
==== WISE J0336−0143B ====
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* [[2M1207b]]
{{Main|WISE J0336−0143}}
WISE J0336−0143B, orbits a brown dwarf or sub-brown dwarf. The primary has a mass of 8.5 to 18 {{Jupiter mass}} and secondary has a mass of 5-11.5 {{Jupiter mass}}. This object does not fit the IAU working definition of an [[exoplanet]].<ref name=":0" /> This definition requires a mass ratio of about q<0.04, but the mass ratio of WISE J0336−0143AB is q=0.61±0.05.<ref>{{Cite journal |last1=Calissendorff |first1=Per |last2=De Furio |first2=Matthew |last3=Meyer |first3=Michael |last4=Albert |first4=Loïc |last5=Aganze |first5=Christian |last6=Ali-Dib |first6=Mohamad |last7=Bardalez Gagliuffi |first7=Daniella C. |last8=Baron |first8=Frederique |last9=Beichman |first9=Charles A. |last10=Burgasser |first10=Adam J. |last11=Cushing |first11=Michael C. |last12=Faherty |first12=Jacqueline Kelly |last13=Fontanive |first13=Clémence |last14=Gelino |first14=Christopher R. |last15=Gizis |first15=John E. |date=2023-04-01 |title=JWST/NIRCam Discovery of the First Y+Y Brown Dwarf Binary: WISE J033605.05-014350.4 |journal=The Astrophysical Journal |volume=947 |issue=2 |pages=L30 |doi=10.3847/2041-8213/acc86d |issn=0004-637X |doi-access=free|arxiv=2303.16923 |bibcode=2023ApJ...947L..30C }}</ref> It also does not fit the definition of a [[rogue planet]], because it is gravitationally bound to a brown dwarf (or possibly sub-brown dwarf). Therefore it only fits the definition of sub-brown dwarf.

==== 2M1207b ====
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{{Main|2M1207b}}
2M1207b orbits around a young brown dwarf with a circumstellar disk and itself is likely surrounded by a circumstellar disk. The mass ratio is well above the upper limit of q=0.04 for exoplanets.<ref>{{Cite journal |last1=Luhman |first1=K. L. |last2=Tremblin |first2=P. |last3=Birkmann |first3=S. M. |last4=Manjavacas |first4=E. |last5=Valenti |first5=J. |last6=Alves de Oliveira |first6=C. |last7=Beck |first7=T. L. |last8=Giardino |first8=G. |last9=Lützgendorf |first9=N. |last10=Rauscher |first10=B. J. |last11=Sirianni |first11=M. |date=2023-06-01 |title=JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B |journal=The Astrophysical Journal |volume=949 |issue=2 |pages=L36 |doi=10.3847/2041-8213/acd635 |issn=0004-637X |doi-access=free|arxiv=2305.18603 |bibcode=2023ApJ...949L..36L }}</ref>

====Others====
Other examples of planetary-mass objects orbiting brown dwarfs and with M<sub>B</sub><13 {{Jupiter mass}} and q>0.04:

* [[CFHTWIR-Oph 98|CFHTWIR-Oph 98B]], with M<sub>B</sub>={{Val|11.6|0.4|0.8}} {{Jupiter mass}} and q={{Val|0.509|0.017|0.023}}<ref>{{Cite journal |last1=Fontanive |first1=Clémence |last2=Allers |first2=Katelyn N. |last3=Pantoja |first3=Blake |last4=Biller |first4=Beth |last5=Dubber |first5=Sophie |last6=Zhang |first6=Zhoujian |last7=Dupuy |first7=Trent |last8=Liu |first8=Michael C. |last9=Albert |first9=Loïc |date=2020-12-01 |title=A Wide Planetary-mass Companion to a Young Low-mass Brown Dwarf in Ophiuchus |journal=The Astrophysical Journal |volume=905 |issue=2 |pages=L14 |doi=10.3847/2041-8213/abcaf8 |issn=0004-637X |doi-access=free|arxiv=2011.08871 |bibcode=2020ApJ...905L..14F }}</ref>
* [[2MASS J04414489+2301513|2MASS J04414489+2301513Bb]], with M<sub>Bb</sub>={{Val|9.8|1.8}} {{Jupiter mass}} and <math>q={M_{Bb} \over M_{Ba}}>0.36</math><ref>{{Cite journal |last1=Bowler |first1=Brendan P. |last2=Hillenbrand |first2=Lynne A. |date=2015-10-01 |title=Near-infrared Spectroscopy of 2M0441+2301 AabBab: A Quadruple System Spanning the Stellar to Planetary Mass Regimes |journal=The Astrophysical Journal |volume=811 |issue=2 |pages=L30 |doi=10.1088/2041-8205/811/2/L30 |issn=0004-637X |doi-access=free|arxiv=1509.01658 |bibcode=2015ApJ...811L..30B }}</ref>
* [[2MASS J0249-0557|2MASS J0249-0557ABc]], with M<sub>c</sub>={{Val|11.6|1.3|1.0}} {{Jupiter mass}} and <math>q={M_{c} \over M_{AB}}=0.13</math><ref>{{Cite journal |last1=Dupuy |first1=Trent J. |last2=Liu |first2=Michael C. |last3=Allers |first3=Katelyn N. |last4=Biller |first4=Beth A. |last5=Kratter |first5=Kaitlin M. |last6=Mann |first6=Andrew W. |last7=Shkolnik |first7=Evgenya L. |last8=Kraus |first8=Adam L. |last9=Best |first9=William M. J. |date=2018-08-01 |title=The Hawaii Infrared Parallax Program. III. 2MASS J0249-0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group |journal=The Astronomical Journal |volume=156 |issue=2 |pages=57 |doi=10.3847/1538-3881/aacbc2 |issn=0004-6256|doi-access=free |arxiv=1807.05235 |bibcode=2018AJ....156...57D }}</ref>


===Free-floating===
===Free-floating===
Also called [[rogue planet]]s:
*[[WISE 0855–0714]] 3–10 M<sub>J</sub> about 7 light years away
*[[WISE 0855–0714]] 3–10 M<sub>J</sub> about 7 light years away
*[[S Ori 52]]
*[[S Ori 52]]
*[[UGPS J072227.51-054031.2]] 10–25 M<sub>J</sub> 13 light years away
*[[UGPS J0722−0540|UGPS 0722-05]] 10–25 M<sub>J</sub> 13 light years away
*[[Cha 110913-773444]] 5–15 M<sub>J</sub> 163 light years away
*[[Cha 110913-773444]] 5–15 M<sub>J</sub> 163 light years away
*[[CFBDSIR2149-0403]] 4–7 M<sub>J</sub> 130 light years away
*[[CFBDSIR 2149−0403]] 4–7 M<sub>J</sub> 130 light years away
*[[OTS 44]] 11.5 M<sub>J</sub> 550 light years away
*[[OTS 44]] 11.5 M<sub>J</sub> 550 light years away
*[[PSO J318.5-22]] 6.5 M<sub>J</sub> 80 light years away
*[[PSO J318.5−22]] 6–8 M<sub>J</sub> about 80 light years away


== See also ==
== See also ==
{{wiktionary}}
{{wiktionary}}
* [[Brown dwarf]]
* [[Brown dwarf]]
* [[Fusor (astronomy)]]
* [[Giant planet]]
* [[Giant planet]]
* [[Hot Jupiter]]
* [[Hot Jupiter]]
* [[Red dwarf]]
* [[Red dwarf]]
* [[Rogue planet]]
* [[Rogue planet]]
* [[Substellar object]]
* [[Shiv S. Kumar]] (theorist who predicted the existence of brown dwarfs)
* [[List of planet types]]
* [[Lists of astronomical objects]]


== References ==
== References ==
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{{Star}}
{{Star}}
{{Exoplanet}}
{{Exoplanet}}
{{Portal bar|Astronomy|Spaceflight|Outer space|Solar System}}
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{{Use dmy dates|date=August 2011}}

{{DEFAULTSORT:Sub-Brown Dwarf}}
{{DEFAULTSORT:Sub-Brown Dwarf}}
[[Category:Brown dwarfs]]
[[Category:Brown dwarfs|+]]
[[Category:Types of planet]]
[[Category:Types of planet]]
[[Category:Star types]]
[[Category:Planetary-mass objects]]
[[Category:Planemos]]
[[Category:Free-floating substellar objects]]
[[Category:Free-floating substellar objects]]

Latest revision as of 15:08, 20 November 2024

Comparison: the Sun (yellow), a young sub-brown dwarf (red), and Jupiter (multi-colored). As the sub-brown dwarf ages, it will gradually cool and shrink.

A sub-brown dwarf or planetary-mass brown dwarf is an astronomical object that formed in the same manner as stars and brown dwarfs (i.e. through the collapse of a gas cloud) but that has a planetary mass, therefore by definition below the limiting mass for thermonuclear fusion of deuterium (about 13 MJ).[1] Some researchers include them in the category of rogue planets[2] whereas others call them planetary-mass brown dwarfs.[3]

Description

[edit]

Sub-brown dwarfs are formed in the manner of stars, through the collapse of a gas cloud (perhaps with the help of photo-erosion) but there is no consensus amongst astronomers on whether the formation process should be taken into account when classifying an object as a planet.[4] Free-floating sub-brown dwarfs can be observationally indistinguishable from rogue planets, which originally formed around a star and were ejected from orbit. Similarly, a sub-brown dwarf formed free-floating in a star cluster may be captured into orbit around a star, making distinguishing sub-brown dwarfs and large planets also difficult. A definition for the term "sub-brown dwarf" was put forward by the IAU Working Group on Extra-Solar Planets (WGESP), which defined it as a free-floating body found in young star clusters below the lower mass cut-off of brown dwarfs.[5]

Lower mass limit

[edit]

The smallest mass of gas cloud that could collapse to form a sub-brown dwarf is about 1 Jupiter mass (MJ).[6] This is because to collapse by gravitational contraction requires radiating away energy as heat and this is limited by the opacity of the gas.[7] A 3 MJ candidate is described in a 2007 paper.[8]

List of possible sub-brown dwarfs

[edit]

Orbiting one or more stars

[edit]

There is no consensus whether these companions of stars should be considered sub-brown dwarfs or planets.

Orbiting a brown dwarf

[edit]

At around 2022 the IAU working definition of an exoplanet excludes these objects as planets.[9] The only fitting label would be as sub-brown dwarfs, but they are more often referred as planetary mass objects. Other definitions, like from the NASA Exoplanet Archive or the Extrasolar Planets Encyclopaedia would include these as exoplanets. There is no consensus whether these companions of brown dwarfs should be considered sub-brown dwarfs or planets.

WISE J0336−0143B

[edit]
Main article: WISE J0336−0143

WISE J0336−0143B, orbits a brown dwarf or sub-brown dwarf. The primary has a mass of 8.5 to 18 MJ and secondary has a mass of 5-11.5 MJ. This object does not fit the IAU working definition of an exoplanet.[9] This definition requires a mass ratio of about q<0.04, but the mass ratio of WISE J0336−0143AB is q=0.61±0.05.[10] It also does not fit the definition of a rogue planet, because it is gravitationally bound to a brown dwarf (or possibly sub-brown dwarf). Therefore it only fits the definition of sub-brown dwarf.

2M1207b

[edit]
Main article: 2M1207b

2M1207b orbits around a young brown dwarf with a circumstellar disk and itself is likely surrounded by a circumstellar disk. The mass ratio is well above the upper limit of q=0.04 for exoplanets.[11]

Others

[edit]

Other examples of planetary-mass objects orbiting brown dwarfs and with MB<13 MJ and q>0.04:

Free-floating

[edit]

Also called rogue planets:

See also

[edit]
Look up sub-brown dwarf in Wiktionary, the free dictionary.

References

[edit]
  1. ^ Working Group on Extrasolar Planets – Definition of a "Planet" Archived 16 September 2006 at the Wayback Machine POSITION STATEMENT ON THE DEFINITION OF A "PLANET" (IAU)
  2. ^ Delorme, P.; et al. (December 2012). "CFBDSIR2149-0403: a 4–7 Jupiter-mass rogue planet in the young moving group AB Doradus ?". Astronomy & Astrophysics. 548: A26. arXiv:1210.0305. Bibcode:2012A&A...548A..26D. doi:10.1051/0004-6361/201219984. S2CID 50935950.
  3. ^ Luhman, K. L. (21 April 2014). "Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun". The Astrophysical Journal Letters. 786 (2): L18. arXiv:1404.6501. Bibcode:2014ApJ...786L..18L. doi:10.1088/2041-8205/786/2/L18. S2CID 119102654.
  4. ^ What is a Planet? Debate Forces New Definition, by Robert Roy Britt, 2 November 2000
  5. ^ IAU WGESP, 'Position Statement on the Definition of "Planet"', 28 February 2003
  6. ^ Boss, Alan P.; Basri, Gibor; Kumar, Shiv S.; Liebert, James; Martín, Eduardo L.; Reipurth, Bo; Zinnecker, Hans (2003), "Nomenclature: Brown Dwarfs, Gas Giant Planets, and ?", Brown Dwarfs, 211: 529, Bibcode:2003IAUS..211..529B
  7. ^ Scholz, Alexander; Geers, Vincent; Jayawardhana, Ray; Fissel, Laura; Lee, Eve; Lafreniere, David; Tamura, Motohide (2009), "Substellar Objects in Nearby Young Clusters (Sonyc): The Bottom of the Initial Mass Function in Ngc 1333", The Astrophysical Journal, 702 (1): 805–822, arXiv:0907.2243v1, Bibcode:2009ApJ...702..805S, doi:10.1088/0004-637X/702/1/805, S2CID 5102383
  8. ^ Scholz, Aleks; Jayawardhana, Ray (2007), "Dusty disks at the bottom of the IMF", The Astrophysical Journal, 672 (1): L49–L52, arXiv:0711.2510v1, Bibcode:2008ApJ...672L..49S, doi:10.1086/526340
  9. ^ a b Etangs, A. Lecavelier des; Lissauer, Jack J. (17 March 2022). "The IAU Working Definition of an Exoplanet". New Astronomy Reviews. 94: 101641. arXiv:2203.09520. Bibcode:2022NewAR..9401641L. doi:10.1016/j.newar.2022.101641.
  10. ^ Calissendorff, Per; De Furio, Matthew; Meyer, Michael; Albert, Loïc; Aganze, Christian; Ali-Dib, Mohamad; Bardalez Gagliuffi, Daniella C.; Baron, Frederique; Beichman, Charles A.; Burgasser, Adam J.; Cushing, Michael C.; Faherty, Jacqueline Kelly; Fontanive, Clémence; Gelino, Christopher R.; Gizis, John E. (1 April 2023). "JWST/NIRCam Discovery of the First Y+Y Brown Dwarf Binary: WISE J033605.05-014350.4". The Astrophysical Journal. 947 (2): L30. arXiv:2303.16923. Bibcode:2023ApJ...947L..30C. doi:10.3847/2041-8213/acc86d. ISSN 0004-637X.
  11. ^ Luhman, K. L.; Tremblin, P.; Birkmann, S. M.; Manjavacas, E.; Valenti, J.; Alves de Oliveira, C.; Beck, T. L.; Giardino, G.; Lützgendorf, N.; Rauscher, B. J.; Sirianni, M. (1 June 2023). "JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B". The Astrophysical Journal. 949 (2): L36. arXiv:2305.18603. Bibcode:2023ApJ...949L..36L. doi:10.3847/2041-8213/acd635. ISSN 0004-637X.
  12. ^ Fontanive, Clémence; Allers, Katelyn N.; Pantoja, Blake; Biller, Beth; Dubber, Sophie; Zhang, Zhoujian; Dupuy, Trent; Liu, Michael C.; Albert, Loïc (1 December 2020). "A Wide Planetary-mass Companion to a Young Low-mass Brown Dwarf in Ophiuchus". The Astrophysical Journal. 905 (2): L14. arXiv:2011.08871. Bibcode:2020ApJ...905L..14F. doi:10.3847/2041-8213/abcaf8. ISSN 0004-637X.
  13. ^ Bowler, Brendan P.; Hillenbrand, Lynne A. (1 October 2015). "Near-infrared Spectroscopy of 2M0441+2301 AabBab: A Quadruple System Spanning the Stellar to Planetary Mass Regimes". The Astrophysical Journal. 811 (2): L30. arXiv:1509.01658. Bibcode:2015ApJ...811L..30B. doi:10.1088/2041-8205/811/2/L30. ISSN 0004-637X.
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