{{위키데이터 속성 추적}}
아래 목록은 관측된 별들 중 '''[[유효온도]]가 낮은 별'''과 [[갈색 왜성]]들을 순서대로 정렬한 것으로 단위는 [[켈빈]]이다. 유효온도가 2,000[[K]]보다 낮은 별이 포함된다.

Kirkpatrick et al. 2021<ref name=":0" />에 근처의 온도 2,400K 미만인 천체의 더 완전한 목록이 있고 이 논문에 나온 온도가 500K 미만인 물체가 이 목록에 포함되어있다.

==목록==
{{미완성 목록|date=October 2016}}

{| class="wikitable sortable"
|-
! 항성 이름
! width="100" | [[유효온도]]
([[켈빈|K]])
! [[항성분류|분광형]]
! width="120" |대략 태양계로부터의 거리 {{nowrap|([[광년]])}}
! 주석
|-
|[[WISE J0855-0714]]
|225–260<ref name="NASA20140425">{{뉴스 인용|url=http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425/ |title=NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun |work=[[NASA]].gov |first1=Whitney |last1=Clavin |first2=J. D. |last2=Harrington |date=25 April 2014 |archive-url=https://web.archive.org/web/20140426004939/http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425 |archive-date=26 April 2014 |url-status=live}}</ref>
|Y4
|{{val|7.27|0.13}}
|
|-
|[[WISE J0336−0143|WISE 0336-0143B]]<ref name=":1">{{저널 인용 |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 |arxiv=2303.16923 |bibcode=2023ApJ...947L..30C |issn=0004-637X|doi-access=free }}</ref>
|{{Val|295|10}}<ref name="Leggett+Tremblin">{{저널 인용 |last1=Leggett |first1=S. K. |last2=Tremblin |first2=Pascal |date=25 Sep 2023 |title=The First Y Dwarf Data From JWST Show That Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres |journal=ApJ |arxiv=2309.14567 }}</ref>
|Y1?
|32.7<ref name=":0" />
|스펙트럼 유형은 아직 게시되지 않았지만 MIRI F480M이 W2와 유사하고 Kirkpatrick et al. 2012<ref>{{저널 인용 |last1=Kirkpatrick |first1=J. Davy |last2=Gelino |first2=Christopher R. |last3=Cushing |first3=Michael C. |last4=Mace |first4=Gregory N. |last5=Griffith |first5=Roger L. |last6=Skrutskie |first6=Michael F. |last7=Marsh |first7=Kenneth A. |last8=Wright |first8=Edward L. |last9=Eisenhardt |first9=Peter R. |last10=McLean |first10=Ian S. |last11=Mainzer |first11=Amanda K. |last12=Burgasser |first12=Adam J. |last13=Tinney |first13=C. G. |last14=Parker |first14=Stephen |last15=Salter |first15=Graeme |date=2012-07-01 |title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function |journal=The Astrophysical Journal |volume=753 |issue=2 |pages=156 |doi=10.1088/0004-637X/753/2/156 |arxiv=1205.2122 |bibcode=2012ApJ...753..156K |issn=0004-637X|doi-access=free }}</ref>의 figure 13을 사용한다고 가정하면 Y1 정도여야 한다. 이 이후의 분광형일 수도 있다.
|-
|[[Backyard Worlds#WISE J0830+2837|WISEA 0830+2837]]
|300-350<ref>{{저널 인용 |last1=Bardalez Gagliuffi |first1=Daniella C. |last2=Faherty |first2=Jacqueline K. |last3=Schneider |first3=Adam C. |last4=Meisner |first4=Aaron |last5=Caselden |first5=Dan |last6=Colin |first6=Guillaume |last7=Goodman |first7=Sam |last8=Kirkpatrick |first8=J. Davy |last9=Kuchner |first9=Marc |last10=Gagné |first10=Jonathan |last11=Logsdon |first11=Sarah E. |last12=Burgasser |first12=Adam J. |last13=Allers |first13=Katelyn |last14=Debes |first14=John |last15=Wisniewski |first15=John |date=2020-06-01 |title=WISEA J083011.95+283716.0: A Missing Link Planetary-mass Object |journal=The Astrophysical Journal |volume=895 |issue=2 |pages=145 |doi=10.3847/1538-4357/ab8d25 |arxiv=2004.12829 |bibcode=2020ApJ...895..145B |issn=0004-637X|doi-access=free }}</ref>
|>Y1<ref name=":0" />
|26.87<ref name=":0" />
|연주시차가 불확실하며 분광형은 추정치다.
|-
|CWISEP 0238-1332<ref name=":0" />
|{{Val|367|79}}
|>Y1
|58.66
|연주시차가 불확실하며 분광형은 추정치다.
|-
|CWISEP 0402-2651<ref name=":0" />
|{{Val|367|79}}
|>Y1
|39.53
|연주시차가 불확실하며 분광형은 추정치다.
|-
|WISEU 0503-5648<ref name=":0" />
|{{Val|367|79}}
|>Y1
|33.18
|분광형은 추정치다.
|-
|CWISEP 0940+5233<ref name=":0" />
|{{Val|367|79}}
|>Y1
|43.49
|연주시차가 불확실하며 분광형은 추정치다.
|-
|WISEA 1257+7153<ref name=":0" />
|{{Val|367|79}}
|>Y1
|54.18
|분광형은 추정치다.
|-
|CWISEP 1446-2317<ref name=":0" />
|{{Val|367|79}}
|>Y1
|37.75
|연주시차가 불확실하며 분광형은 추정치다.
|-
|WISEA 1930-2059<ref name=":0" />
|{{Val|367|79}}
|>Y1
|30.67
|분광형은 추정치다.
|-
|CWISEP 1935-1546<ref name=":0" />
|{{Val|367|79}}
|>Y1
|47.06
|분광형은 추정치다.
|-
|CWISEP 2230+2549<ref name=":0" />
|{{Val|367|79}}
|>Y1
|52.44
|연주시차가 불확실하며 분광형은 추정치다.
|-
|CWISEP 2256+4002<ref name=":0" />
|{{Val|367|79}}
|>Y1
|32.04
|분광형은 추정치다.
|-
|[[CFBDSIR 1458+10B]]
|370
|Y0
|104
|
|-
|WISE 0825+2805<ref name=":0" />
|{{Val|376|88}}
|Y0.5
|21.37
|
|-
|[[WD 0806−661|WD 0806-661B]]<ref name=":0" />
|{{Val|377|88}}
|Y1
|62.80
|분광형은 추정치다.
|-
|[[WISE 0350−5658|WISE 0350-5658]]<ref name=":0" />
|{{Val|388|88}}
|Y1
|18.49
|
|-
|WISEA 2354+0240<ref name=":0" />
|{{Val|388|88}}
|Y1
|24.97
|
|-
|[[WISE J2209+2711|WISE 2209+2711]]<ref name=":0" />
|{{Val|389|88}}
|Y0:
|20.17
|
|-
|[[WISE 0647−6232|WISE 0647-6232]]<ref name=":0" />
|{{Val|393|88}}
|Y1
|32.78
|
|-
|[[WISE 1541−2250|WISEPA 1541-2250]]<ref name=":0" />
|{{Val|395|88}}
|Y1
|19.54
|
|-
|[[WISE 1828+2650]]
|{{Val|406|88}}<ref name=":0">{{저널 인용 |last1=Kirkpatrick |first1=J. Davy |last2=Gelino |first2=Christopher R. |last3=Faherty |first3=Jacqueline K. |last4=Meisner |first4=Aaron M. |last5=Caselden |first5=Dan |last6=Schneider |first6=Adam C. |last7=Marocco |first7=Federico |last8=Cayago |first8=Alfred J. |last9=Smart |first9=R. L. |last10=Eisenhardt |first10=Peter R. |last11=Kuchner |first11=Marc J. |last12=Wright |first12=Edward L. |last13=Cushing |first13=Michael C. |last14=Allers |first14=Katelyn N. |last15=Gagliuffi |first15=Daniella C. Bardalez |date=2021-03-01 |title=The Field Substellar Mass Function Based on the Full-sky 20-pc Census of 525 L, T, and Y Dwarfs |journal=The Astrophysical Journal Supplement Series |volume=253 |issue=1 |pages=7 |doi=10.3847/1538-4365/abd107 |arxiv=2011.11616 |bibcode=2021ApJS..253....7K |s2cid=227126954 |issn=0067-0049 |doi-access=free }}</ref>
|Y2V<ref>{{저널 인용 |last1=Beichman |first1=Charles A. |last2=Gelino |first2=Christopher R. |last3=Kirkpatrick |first3=J. Davy |last4=Barman |first4=Travis S. |last5=Marsh |first5=Kenneth A. |last6=Cushing |first6=Michael C. |last7=Wright |first7=E. L. |date=2013-01-29 |title=The Coldest Brown Dwarf (Or Free Floating Planet)?: The Y Dwarf WISE 1828+2650 |journal=The Astrophysical Journal |volume=764 |issue=1 |pages=101 |doi=10.1088/0004-637X/764/1/101 |arxiv=1301.1669 |bibcode=2013ApJ...764..101B |s2cid=118575478 |issn=0004-637X}}</ref>
|32.5
|온도가 더 낮을 수 있으며 쌍성계라면 구성원은 275-350 K 정도로 차가울 수 있다.<ref>{{저널 인용 |last1=Cushing |first1=Michael C. |last2=Schneider |first2=Adam C. |last3=Kirkpatrick |first3=J. Davy |last4=Morley |first4=Caroline V. |last5=Marley |first5=Mark S. |last6=Gelino |first6=Christopher R. |last7=Mace |first7=Gregory N. |last8=Wright |first8=Edward L. |last9=Eisenhardt |first9=Peter R. |last10=Skrutskie |first10=Michael F. |last11=Marsh |first11=Kenneth A. |date=2021-10-01 |title=An Improved Near-infrared Spectrum of the Archetype Y Dwarf WISEP J182831.08+265037.8 |journal=The Astrophysical Journal |volume=920 |issue=1 |pages=20 |doi=10.3847/1538-4357/ac12cb |arxiv=2107.00506 |bibcode=2021ApJ...920...20C |issn=0004-637X|doi-access=free }}</ref>
|-
|[[WISE 0535−7500|WISE 0535-7500]]<ref name=":0" />
|{{Val|410|88}}
|>=Y1:
|47.48
|
|-
|[[WISE 1405+5534]]
|{{Val|411|88}}<ref name=":0" />
|Y0.5(pec?)<ref name=":0" />
|20.62
|
|-
|CWISEP 0321+6932<ref name=":0" />
|{{Val|412|79}}
|Y0.5
|47.61
|분광형은 추정치다.
|-
|[[WISE 1639−6847|WISE 1639-6847]]<ref name=":0" />
|{{Val|412|88}}
|Y0pec
|14.85
|
|-
|CWISEP 2356-4814<ref name=":0" />
|{{Val|412|79}}
|Y0.5
|56.62
|분광형은 추정치다.
|-
|[[WISE J0336−0143|WISE 0336-0143A]]<ref name=":1" />
|{{Val|440|24}}<ref name="Leggett+Tremblin3">{{저널 인용 |last1=Leggett |first1=S. K. |last2=Tremblin |first2=Pascal |date=25 Sep 2023 |title=The First Y Dwarf Data From JWST Show That Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres |journal=ApJ |arxiv=2309.14567 }}</ref>
|Y0<ref name=":0" />
|32.7<ref name=":0" />
|
|-
|[[WISEPA J173835.53+273258.9|WISEPA 1738+2732]]<ref name=":0" />
|{{Val|450|88}}
|Y0
|24.92
|
|-
|[[WISEPA J041022.71+150248.5|WISEPA 0410+1502]]<ref name=":0" />
|{{Val|451|88}}
|Y0
|21.56
|
|-
|[[WISE 2220−3628|WISE 2220-3628]]<ref name=":0" />
|{{Val|452|88}}
|Y0
|34.15
|
|-
|[[WISE 1534–1043|WISE 1534-1043]]
|{{Val|453|77}}<ref>{{저널 인용 |last1=Meisner |first1=Aaron M. |last2=Leggett |first2=S. K. |last3=Logsdon |first3=Sarah E. |last4=Schneider |first4=Adam C. |last5=Tremblin |first5=Pascal |last6=Phillips |first6=Mark |date=2023-08-01 |title=Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs |journal=The Astronomical Journal |volume=166 |issue=2 |pages=57 |doi=10.3847/1538-3881/acdb68 |arxiv=2301.09817 |bibcode=2023AJ....166...57M |issn=0004-6256|doi-access=free }}</ref>
|sdY?
|53
|[[은하헤일로|헤일로]]의 갈색왜성일 가능성이 있다.
|-
|WISE 1206+8401<ref name=":0" />
|{{Val|454|88}}
|Y0
|38.51
|
|-
|[[WISE 0146+4234|WISE 0146+4234B]]<ref name=":0" />
|{{Val|460|79}}
|Y0
|63.09
|
|-
|WISEA 0302-5817<ref name=":0" />
|{{Val|460|79}}
|Y0:
|54.45
|
|-
|CWISEP 0634+5049<ref name=":0" />
|{{Val|460|79}}
|Y0
|52.61
|분광형은 추정치다.
|-
|CWISEP 0859+5349<ref name=":0" />
|{{Val|460|79}}
|Y0
|60.62
|분광형은 추정치다.
|-
|CWISE 0925-4720<ref name=":0" />
|{{Val|460|79}}
|Y0
|34.96
|분광형은 추정치다.
|-
|CWISEP 0938+0634<ref name=":0" />
|{{Val|460|79}}
|Y0
|61.31
|연주시차가 불확실하며 분광형은 추정치다.
|-
|CWISEP 1047+5457<ref name=":0" />
|{{Val|460|79}}
|Y0
|43.37
|분광형은 추정치다.
|-
|CWISE 1121-6232<ref name=":0" />
|{{Val|460|79}}
|Y0
|33.69
|분광형은 추정치다.
|-
|WISEA 1141-3326<ref name=":0" />
|{{Val|460|79}}
|Y0
|31.36
|
|-
|[[WISE 1217+1626|WISE 1217+1626 B]]
|{{Val|460|79}}<ref name=":0" />
|Y0-0.5
|33
|
|-
|CWISE 1531-3306<ref name=":0" />
|{{Val|460|79}}
|Y0
|55.37
|분광형은 추정치다.
|-
|WISENF 1936+0408<ref name=":0" />
|{{Val|460|79}}
|Y0
|28.64
|분광형은 추정치다.
|-
|CWISEP 2011-4812<ref name=":0" />
|{{Val|460|79}}
|Y0
|45.94
|분광형은 추정치다.
|-
|WISEA 2243-1458<ref name=":0" />
|{{Val|460|79}}
|Y0
|47,75
|분광형은 추정치다.
|-
|WISE 1112-3857<ref name=":0" />
|{{Val|461|88}}
|T9
|31.79
|
|-
|[[WISE 0734−7157|WISE 0734-7157]]<ref name=":0" />
|{{Val|462|88}}
|Y0
|43.78
|
|-
|[[WISE 0713−2917|WISE 0713-2917]]<ref name=":0" />
|{{Val|464|88}}
|Y0
|29.84
|
|-
|[[WISEPC J205628.90+145953.3|WISEPC 2056+1459]]<ref name=":0" />
|{{Val|464|88}}
|Y0
|23.16
|
|-
|WISE 0304-2705<ref name=":0" />
|{{Val|465|88}}
|Y0~pec
|44.62
|
|-
|[[WISE 0359−5401|WISE 0359-5401]]
|{{Val|467|16|18}}<ref>{{저널 인용 |last1=Beiler |first1=Samuel A. |last2=Cushing |first2=Michael C. |last3=Kirkpatrick |first3=J. Davy |last4=Schneider |first4=Adam C. |last5=Mukherjee |first5=Sagnick |last6=Marley |first6=Mark S. |date=2023-07-01 |title=The First JWST Spectral Energy Distribution of a Y Dwarf |journal=The Astrophysical Journal |volume=951 |issue=2 |pages=L48 |doi=10.3847/2041-8213/ace32c |arxiv=2306.11807 |bibcode=2023ApJ...951L..48B |issn=0004-637X|doi-access=free }}</ref>
|Y0<ref name=":0" />
|44.31<ref name=":0" />
|
|-
|WISE 0943+3607<ref name=":0" />
|{{Val|468|88}}
|T9.5
|33.59
|
|-
|WISE 0833+0052<ref name=":0" />
|{{Val|472|88}}
|(sd)T9
|40.92
|[[준왜성]]일 가능성이 있다.
|-
|[[WISE 1542+2230]]<ref name=":0" />
|{{Val|472|88}}
|T9.5
|38.69
|
|-
|[[WISE 0811-8051]]<ref name=":0" />
|{{Val|479|88}}
|T9.5:
|32.91
|
|-
|[[WISE 2134-7137|WISEPA 2134-7137]]<ref name=":0" />
|{{Val|481|88}}
|T9~pec
|29.73
|준왜성일 가능성이 있다.
|-
|WISE 2212-6931<ref name=":0" />
|{{Val|487|88}}
|T9
|40.47
|
|-
|[[WISE 0751-7634|WISEPA 0751-7634]]<ref name=":0" />
|{{Val|492|88}}
|T9
|33.32
|
|-
|[[WISE 0335+4310]]<ref name=":0" />
|{{Val|492|88}}
|T9
|38.46
|
|-
|[[WISE 1217+1626|WISE 1217+1626 A]]
|575
|T8.5-9
|33
|
|-
|[[UGPS J0521+3640]]
|600–650
|T8.5
|26.7
|
|-
|[[2MASS 0939-2448]] A/B
|650<ref name="Leggett2009">{{저널 인용 |doi=10.1088/0004-637X/695/2/1517 |last1=Leggett |first1=Sandy K. |last2=Cushing |first2=Michael C. |last3=Saumon |first3=Didier |last4=Marley |first4=Mark S. |last5=Roellig |first5=Thomas L. |last6=Warren |first6=Stephen J. |last7=Burningham |first7=Ben |last8=Jones |first8=Hugh R. A. |last9=Kirkpatrick |first9=J. Davy |last10=Lodieu |first10=Nicolas |last11=Lucas |first11=Philip W. |last12=Mainzer |first12=Amy K. |last13=Martín |first13=Eduardo L. |last14=McCaughrean |first14=Mark J. |last15=Pinfield |first15=David J. |last16=Sloan |first16=Gregory C. |last17=Smart |first17=Richard L. |last18=Tamura |first18=Motohide |last19=Van Cleve |first19=Jeffrey E. |title=The Physical Properties of Four ~600 K T Dwarfs |date=2009 |journal=[[The Astrophysical Journal]] |volume=695 |issue=2 |pages=1517–1526 |arxiv=0901.4093 |bibcode=2009ApJ...695.1517L |s2cid=44050900 }}</ref>
|T8
|{{val|17.4|0.4}}
|
|-
|[[2MASS 0415-0935]]
|764
|T8V
|{{val|18.6|0.2}}
|
|-
|[[54 Piscium]] B
|810 ± 50
|T7.5V
|{{val|36.32|0.02}}
|<ref>{{저널 인용|last1=Luhman |first1=K. L. |last2=Patten |first2=B. M. |last3=Marengo |first3=M. |last4=Schuster |first4=M. T. |last5=Hora |first5=J. L. |last6=Ellis |first6=R. G. |last7=Stauffer |first7=J. R. |last8=Sonnett |first8=S. M. |last9=Winston |first9=E. |last10=Gutermuth |first10=R. A. |last11=Megeath |first11=S. T. |last12=Backman |first12=D. E. |last13=Henry |first13=T. J. |last14=Werner |first14=M. W. |last15=Fazio |first15=G. G. |date=January 2007 |title=Discovery of Two T Dwarf Companions with the Spitzer Space Telescope |journal=The Astrophysical Journal |volume=654 |issue=1 |pages=570–579 |doi=10.1086/509073 |arxiv=astro-ph/0609464 |issn=0004-637X|doi-access=free }}</ref>
|-
|[[2M 1237+6526]]
| 850<ref name="Liebert & Burgasser">{{저널 인용 | arxiv=astro-ph/0609793| author=Liebert| author2=Burgasser| name-list-style=amp| title=On the Nature of the Unique Hα-emitting T Dwarf 2MASS J12373919+6526148| journal=[[Astronomy & Astrophysics]]| volume=655|issue=1|pages=522–527 |date=2007|bibcode=2007ApJ...655..522L|doi = 10.1086/509882 | s2cid=18852560}}</ref>
|T6.5
|46
|
|-
|[[2MASS J0348−6022]]
|880
|T7<ref>{{저널 인용 |last1=Tannock |first1=Megan E. |last2=Metchev |first2=Stanimir |last3=Heinze |first3=Aren |last4=Miles-Páez |first4=Paulo A. |last5=Gagné |first5=Jonathan |last6=Burgasser |first6=Adam |last7=Marley |first7=Mark S. |last8=Apai |first8=Dániel |last9=Suárez |first9=Genaro |last10=Plavchan |first10=Peter |date=2021-05-01 |title=Weather on Other Worlds. V. The Three Most Rapidly Rotating Ultra-Cool Dwarfs |journal=The Astronomical Journal |volume=161 |issue=5 |pages=224 |doi=10.3847/1538-3881/abeb67 |arxiv=2103.01990 |bibcode=2021AJ....161..224T |s2cid=232105126 |issn=0004-6256 |doi-access=free }}</ref>
|27.2
|
|-
|[[SCR 1845-6357B]]
|950
|T6
|{{val|13.050|0.008}}
|
|-
|[[인디언자리 엡실론]] Bb
|993
|T6
|12.05
|
|-
|[[2MASS 0243-2453]]
|1,050
|T6
|{{val|35|1}}
|
|-
|[[카멜레온자리 110913-773444]]
|1,350
|M9.5
|529
|
|-
|[[인디언자리 엡실론]] Ba
|1,353
|T1-1.5
|12.05
|
|-
|[[2MASS 0036+1821]]
|1,650
|L3.5
|{{val|28.51|0.05}}
|
|-
|[[2MASS 1507-1627]]
|1,650
|L5
|{{val|24.12|0.06}}
|
|-
|[[OTS 44]]
|1,700
|M9.5
|554
|
|-
|[[GD 165]] B
|1,755<ref>{{저널 인용 |last1=Filippazzo |first1=Joseph C. |last2=Rice |first2=Emily L. |last3=Faherty |first3=Jacqueline |last4=Cruz |first4=Kelle L. |last5=Van Gordon |first5=Mollie M. |last6=Looper |first6=Dagny L. |date=2015-09-10 |title=Fundamental Parameters and Spectral Energy Distributions of Young and Field Age Objects with Masses Spanning the Stellar to Planetary Regime |journal=The Astrophysical Journal |volume=810 |issue=2 |pages=158 |doi=10.1088/0004-637X/810/2/158 |arxiv=1508.01767 |bibcode=2015ApJ...810..158F |s2cid=89611607 |issn=1538-4357}}</ref>
|L4<ref>{{저널 인용 |last1=Kirkpatrick |first1=J. Davy |last2=Reid |first2=I. Neill |last3=Liebert |first3=James |last4=Cutri |first4=Roc M. |last5=Nelson |first5=Brant |last6=Beichman |first6=Charles A. |last7=Dahn |first7=Conard C. |last8=Monet |first8=David G. |last9=Gizis |first9=John E. |last10=Skrutskie |first10=Michael F. |date=1999-07-01 |title=Dwarfs Cooler than ''M'': The Definition of Spectral Type ''L'' Using Discoveries from the 2 Micron All-Sky Survey (2MASS) |journal=The Astrophysical Journal |volume=519 |issue=2 |pages=802–833 |doi=10.1086/307414 |bibcode=1999ApJ...519..802K |s2cid=73569208 |issn=0004-637X|doi-access=free }}</ref>
|109
|
|-
|[[카시오페아자리 S]]
|1,800
|S3,4–S5,8
|{{val|3100|300|fmt=commas}}
|
|-
|[[페르세우스자리 V384]]
|1,820<ref name="Bergeat">{{저널 인용|author1=Bergeat, J.|author2=Chevallier, L.|date=2005|title=The mass loss of C-rich giants|journal=Astronomy and Astrophysics|volume=429|pages=235–246|bibcode=2005A&A...429..235B|arxiv=astro-ph/0601366|doi=10.1051/0004-6361:20041280|s2cid=56424665 }}</ref>
|N
|
|
|-
|[[DENIS-P J1058.7−1548]]
|1,850<ref>{{저널 인용 |last1=Heinze |first1=Aren N. |last2=Metchev |first2=Stanimir |last3=Apai |first3=Daniel |last4=Flateau |first4=Davin |last5=Kurtev |first5=Radostin |last6=Marley |first6=Mark |last7=Radigan |first7=Jacqueline |last8=Burgasser |first8=Adam J. |last9=Artigau |first9=Étienne |last10=Plavchan |first10=Peter |date=2013-04-08 |title=Weather on Other Worlds I: Detection of Periodic Variability in the L3 Dwarf DENIS-P J1058.7-1548 with Precise Multi-Wavelength Photometry |journal=The Astrophysical Journal |volume=767 |issue=2 |pages=173 |doi=10.1088/0004-637X/767/2/173 |arxiv=1303.2948 |bibcode=2013ApJ...767..173H |s2cid=29406867 |issn=0004-637X}}</ref>
|L3
|49
|
|-
|[[용자리 T]]
|1,850<ref name="Bergeat" />
|C6,2e
|
|
|-
|[[고물자리 V346]]
|1,875<ref name="Bergeat" />
|C
|
|
|-
|[[2MASS J0523-1403]]
|1,939<ref>{{저널 인용 |last=Filippazzo |first=Joseph C. |last2=Rice |first2=Emily L. |last3=Faherty |first3=Jacqueline |last4=Cruz |first4=Kelle L. |last5=Van Gordon |first5=Mollie M. |last6=Looper |first6=Dagny L. |date=2015-09-10 |title=Fundamental Parameters and Spectral Energy Distributions of Young and Field Age Objects with Masses Spanning the Stellar to Planetary Regime |url=http://arxiv.org/abs/1508.01767 |journal=The Astrophysical Journal |volume=810 |issue=2 |pages=158 |doi=10.1088/0004-637X/810/2/158 |issn=1538-4357|arxiv=1508.01767 }}</ref>
|L2.5V
|41.62
|2023년 기준으로 알려진 가장 차가운 [[주계열성]]이다.
|-
|[[마차부자리 S]]
|1,940<ref name="Bergeat" />
|C-N5+
|
|
|-
|[[백조자리 V1426]]
|1,975<ref name="Bergeat" />
|C7,2e
|
|
|}

== 같이 보기 ==
* [[반지름순 항성 목록]]
* [[유효온도가 높은 항성 목록]]
* [[질량이 큰 항성 목록]]

== 각주 ==
{{각주}}

{{항성}}
{{포털 막대|천문학|우주 개발|우주 공간|태양계}}

[[분류:항성 목록]]