{{위키데이터 속성 추적}}
[[파일:JADES-GS-z13-0.png|alt=Color composite JWST NIRCam image of distant galaxy JADES-GS-z13-0. An initial sample of four z>10 galaxies was spectroscopically confirmed by Curtis-Lake et al. at redshifts z~10.4-13.2. The most distant galaxies at z=13.20 and z=12.63 are newly discovered by JADES NIRCam imaging, while the z=10.38 and z=11.58 galaxies confirm previous photometric redshift estimates from the literature. The yellow-orange-red colours reflect the absorption of the F115W and F150W fluxes of these distant galaxies by the  intervening intergalactic medium.|섬네일|[[w:JADES-GS-z13-0|JADES-GS-z13-0]]은 한 원거리 [[은하]]이다.]]
이 문서에서는 지금까지 '''가장 멀리 있는 천체'''로 발견 및 확인된 천체들과 그 분류된 기간을 기재하고 있다.

아래에 나열된 천체들의 [[거리 측정 (우주론)|광행거리]]와 비교하기 위해 [[대폭발|대폭발(빅뱅)]] 이후 [[우주의 나이]]는 현재 13.787±0.020Gyr로 추정된다.<ref name="Planck 2018age">
{{저널 인용
 |author=Planck Collaboration
 |year=2020
 |title=Planck 2018 results. VI.&nbsp;Cosmological parameters
 |journal=Astronomy & Astrophysics
 |volume=641 |at=page&nbsp;A6 (see PDF page&nbsp;15, Table&nbsp;2: "Age/Gyr", last&nbsp;column)
 |doi=10.1051/0004-6361/201833910
 |arxiv=1807.06209 |bibcode=2020A&A...641A...6P
 |s2cid=119335614
}}
</ref>

가까운 은하에 있는 천체를 제외한 멀리 떨어진 천체까지의 거리는 거의 항상 빛의 [[허블-르메트르 법칙|우주적 적색편이]]의 측정으로부터 추론한다. 본질적으로, 매우 먼 물체는 매우 희미한 경향이 있으므로 이러한 거리 측정은 어렵고 오류가 발생할 수 있다. 천체까지의 거리를 [[분광학]]적으로 결정할 지 아니면 [[w:Photometric redshift|측광학적 적색편이(photometric redshift)]] 기술을 사용하여 결정할지의 구분은 중요하다. 전자는 일반적으로 더 정확하고 더 신뢰할 수 있다. 특이한 스펙트럼을 가진 더 낮은 적색편이 광원과의 혼동으로 인해 측광 적색편이가 더 잘못되기 쉽다는 의미이다. 이러한 이유로 [[적색편이|분광학적 적색편이]]는 일반적으로 물체의 거리가 확실히 알려진 것으로 하기 위하여 필요한 것으로 간주되는 반면에, 측광학적으로 결정된 적색편이에 의해서는 매우 먼거리 광원의 "후보"를 찾아낸다. 여기서는,이 구별은 측광학적 적색편이를 위해서 "p" 아래첨자로써 표시한다.

[[고유거리]]는 은하가 고정된 시점에 얼마나 멀리 떨어져 있는지를 측정한다. 현재 우주론적 [[척도인자]] 값은 1을 가지므로 고유거리는 [[공변거리]]와 같다: <math>a(t_0) = 1</math>. 고유거리는 마치 시간의 흐름을 멈출 수 있는 것처럼 얻은 거리를 나타낸다  ([[프리드만-르메트르-로버트슨-워커 계량]]에서 <math>dt = 0</math>로 설정), 계량 막대를 사용하면서 은하계까지 걸어간다고 가정한다.<ref>{{서적 인용|last=Guidry |first=Mike |title=Modern general relativity: black holes, gravitational waves, and cosmology |date=2019 |publisher=Cambridge university press |isbn=978-1-107-19789-3 |location=Cambridge New York}}</ref> 실용적인 이유로, 고유거리는 은하가 빛을 방출하는 시점부터 관측자(지구에 있는)가 빛 신호를 수신하는 시점까지의 빛이 이동한 거리로서 ([[프리드만-르메트르-로버트슨-워커 계량]]에서 <math>ds = 0 </math>로 설정) 계산된다. 고유거리는 우주의 팽창, 즉 빛이 통과할 때 공간이 팽창하는 것을 고려하기 때문에 "광행거리"와 다르며, 그 결과 [[w:Hubble volume|허블 구(Hubble sphere)]] 너머의 가장 먼 은하를 찾아내고 따라서 광속 ''c'' 보다 큰 [[후퇴 속도]]를 가진 수치를 산출한다.<ref>{{저널 인용|last1=Davis |first1=Tamara M. |last2=Lineweaver |first2=Charles H. |date=2004 |title=Expanding Confusion: Common Misconceptions of Cosmological Horizons and the Superluminal Expansion of the Universe |url=https://www.cambridge.org/core/product/identifier/S132335800000607X/type/journal_article |journal=Publications of the Astronomical Society of Australia |language=en |volume=21 |issue=1 |pages=97–109 |doi=10.1071/AS03040 |arxiv=astro-ph/0310808 |bibcode=2004PASA...21...97D |s2cid=13068122 |issn=1323-3580}}</ref>

== 분광학적으로 확인된 가장 먼 천체 ==
<!--'''NOTE: ToDo? (5 August 2022) =>''' May need to check values in the "light travel distance" ("[[Distance measure#Alternative terminology|lookback time]]") column based on the "[https://cosmocalc.icrar.org/ ICRAR Cosmological Calculator]",<ref name="ICRAR-2022" /> as well as the earlier "[http://www.astro.ucla.edu/~wright/ACC.html UCLA Cosmological Calculator]"<ref name="UCLA-2015" /> and "[https://www.kempner.net/cosmic.php KEMP Cosmology Calculator]"<ref name="KEMP-2022" /> (and compare these values with the [[Age of the universe|13.787 billion years]] since the [[Big Bang]]?) - some of the "light travel distance" values for earlier listed galaxies/objects seem off to some extent.<br /><br />
1 Gly (gigalight-year) = 1 billion [[light-years]]. -->

{| class="sortable wikitable"
|+ 분광학적 적색 편이가 측정된 가장 먼 천체들
|-
|-
! 이미지
! 명칭
! [[적색편이]] <br />(z)
! [[거리 측정 (우주론)|광행거리]]<sup>§</sup> <br />([[광년|Gly]])<ref name="UCLA-2015">{{웹 인용|author=Staff |title=UCLA Cosmological Calculator |url=http://www.astro.ucla.edu/~wright/ACC.html |date=2015 |work=[[UCLA]] |access-date=6 August 2022 }} Light travel distance was calculated from redshift value using the UCLA Cosmological Calculator, with parameters values as of 2015: H<sub>0</sub>=67.74 and Omega<sub>M</sub>=0.3089 (see Table/Planck2015 at "[[Lambda-CDM model#Parameters]]" )</ref><ref name="UCLA-2018">{{웹 인용|author=Staff |title=UCLA Cosmological Calculator |url=http://www.astro.ucla.edu/~wright/ACC.html |date=2018 |work=[[UCLA]] |access-date=6 August 2022 }} Light travel distance was calculated from redshift value using the UCLA Cosmological Calculator, with parameters values as of 2018: H<sub>0</sub>=67.4 and Omega<sub>M</sub>=0.315 (see Table/Planck2018 at "[[Lambda-CDM model#Parameters]]" )</ref><ref name="ICRAR-2022">{{웹 인용|author=Staff |title=ICRAR Cosmology Calculator |url=https://cosmocalc.icrar.org/ |date=2022 |work=[[International Centre for Radio Astronomy Research]] |access-date=6 August 2022 }} ICRAR Cosmology Calculator - Set H<sub>0</sub>=67.4 and Omega<sub>M</sub>=0.315 (see Table/Planck2018 at "[[Lambda-CDM model#Parameters]]")</ref><ref name="KEMP-2022">{{웹 인용|last=Kempner |first=Joshua |title=KEMPNER Cosmology Calculator |url=https://www.kempner.net/cosmic.php |date=2022 |work=Kempner.net |access-date=6 August 2022 }} KEMP Cosmology Calculator - Set H<sub>0</sub>=67.4, Omega<sub>M</sub>=0.315, and Omega<sub>Λ</sub>=0.6847 (see Table/Planck2018 at "[[Lambda-CDM model#Parameters]]")</ref>
![[고유거리]]
(Gly)
! 유형
! 노트
|-

|-
| [[파일:JADES-GS-z13-0.png|100px]]
| [[JADES-GS-z13-0]]
| z = {{val|13.20|0.04|0.07}}
| 13.576<ref name="UCLA-2015" /> / 13.596<ref name="UCLA-2018" /> / 13.474<ref name="ICRAR-2022" /> / 13.473<ref name="KEMP-2022" />
|33.6
| 은하
| [[w:Lyman-break galaxy|라이먼 브레이크 은하]], JWST/근적외선 분광기로 라이먼 브레이크 탐지.<ref name="Robertson2022">{{저널 인용|display-authors = etal |first1 = B. E. |last1 = Robertson |title = Identification and properties of intense star-forming galaxies at redshifts z > 10 |journal = Nature Astronomy |year = 2023 |volume = 7 |issue = 5 |pages = 611–621 |doi = 10.1038/s41550-023-01921-1 |arxiv = 2212.04480|bibcode = 2023NatAs...7..611R |s2cid = 257968812 }}</ref> [[암흑물질성]]일 가능성.<ref name=":0">{{저널 인용|last1=Ilie |first1=Cosmin |last2=Paulin |first2=Jillian |last3=Freese |first3=Katherine |date=2023-07-25 |title=Supermassive Dark Star candidates seen by JWST |journal=Proceedings of the National Academy of Sciences |language=en |volume=120 |issue=30 |pages=e2305762120 |doi=10.1073/pnas.2305762120 |issn=0027-8424 |pmc=10372643 |pmid=37433001|arxiv=2304.01173 |bibcode=2023PNAS..12005762I }}</ref>
|-
|
|[[UNCOVER-z13]]
| z = {{val|13.079|0.014|0.001}}
| 13.51
|32.56<sup>†</sup>
| 은하
| 라이먼 브레이크 은하, JWST/근적외선 분광기로 라이먼 브레이크 탐지.<ref name="arxiv.org">{{저널 인용|last=Wang |first=Bingjie |display-authors=et al |date=2023-11-13 |title=UNCOVER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z &gt; 12 Galaxies |journal=The Astrophysical Journal Letters |volume=957 |issue=2 |pages=L34 |doi=10.3847/2041-8213/acfe07 |arxiv=2308.03745 |bibcode=2023ApJ...957L..34W |issn=2041-8205 |doi-access=free }}</ref>
|-
|
| [[JADES-GS-z12-0]]
| z = {{val|12.63|0.24|0.08}}
| 13.556<ref name="UCLA-2015" /> / 13.576<ref name="UCLA-2018" /> / 13.454<ref name="ICRAR-2022" /> / 13.453<ref name="KEMP-2022" />
|32.34<sup>†</sup>
| 은하
| 라이먼 브레이크 은하, JWST/근적외선 분광기로 라이먼 브레이크 탐지.<ref name="Robertson2022"/> 암흑물질성일 가능성.<ref name=":0" />
|-
|
| [[UNCOVER-z12]]
| z = {{val|12.393|0.004|0.001}}
| 13.48
|32.21<sup>†</sup>
| 은하
| 라이먼 브레이크 은하, JWST/근적외선 분광기로 라이먼 브레이크 탐지.<ref name="arxiv.org" />
|-
| [[파일:NASA-GLASS-z13-Context-JWST-20220722.jpg|100px]]
| [[GLASS-z12]]
| z = {{val|12.117|0.01|0.01}}
| 13.536<ref name="UCLA-2015" /> / 13.556<ref name="UCLA-2018" /> / 13.434<ref name="ICRAR-2022" /> / 13.433<ref name="KEMP-2022" />
|33.2
| 은하
|  JWST/근적외선 카메라로 발견된 라이먼 브레이크 은하. [O III] 방출의 ALMA의 탐지로 확인됨.<ref name="Bakx2022">{{저널 인용|title=Deep ALMA redshift search of a z~12 GLASS-JWST galaxy candidate|first=Tom J. L. C.|last=Bakx|display-authors=etal|arxiv=2208.13642|journal=Monthly Notices of the Royal Astronomical Society|doi=10.1093/mnras/stac3723|date=January 2023|volume=519 |issue=4 |pages=5076–5085 }}</ref>
|-
| [[파일:UDFj-39546284-hs-2011-05-c.jpg|100px]]
| [[UDFj-39546284]]
| z = {{val|11.58|0.05|0.05}}
| 13.512<ref name="UCLA-2015" /> / 13.532<ref name="UCLA-2018" /> / 13.410<ref name="ICRAR-2022" /> / 13.409<ref name="KEMP-2022" />
|31.77<sup>†</sup>
| 은하
| 라이먼 브레이크 은하, JWST/근적외선 분광기로 라이먼 브레이크의 탐지.<ref name="Robertson2022"/> 암흑물질성일 가능성.<ref name=":0" />
|-
|
| [[Maisie's Galaxy|CEERS J141946.36+525632.8]]<br/>([[Maisie's Galaxy]])
<ref>{{저널 인용|last1=Haro |first1=Pablo Arrabal |last2=Dickinson |first2=Mark |last3=Finkelstein |first3=Steven L. |last4=Kartaltepe |first4=Jeyhan S. |last5=Donnan |first5=Callum T. |last6=Burgarella |first6=Denis |last7=Carnall |first7=Adam |last8=Cullen |first8=Fergus |last9=Dunlop |first9=James S. |last10=Fernández |first10=Vital |last11=Fujimoto |first11=Seiji |last12=Jung |first12=Intae |last13=Krips |first13=Melanie |last14=Larson |first14=Rebecca L. |last15=Papovich |first15=Casey |date=2023-08-14 |title=Confirmation and refutation of very luminous galaxies in the early universe |journal=Nature |volume=622 |issue=7984 |pages=707–711 |doi=10.1038/s41586-023-06521-7 |pmid=37579792 |issn=0028-0836|arxiv=2303.15431 |bibcode=2023Natur.622..707A |s2cid=257766818 }}</ref>
| z {{=}} {{val|11.44|0.09|0.08}}
| 13.4
|31.69<sup>†</sup>
| 은하
| JWST로 발견된 라이먼 브레이크 은하.
|-
|
| [[CEERS2 588]]<br/>
<ref>{{ArXiv 인용|last1=Harikane |first1=Yuichi |last2=Nakajima |first2=Kimihiko |last3=Ouchi |first3=Masami |last4=Umeda |first4=Hiroya |last5=Isobe |first5=Yuki |last6=Ono |first6=Yoshiaki |last7=Xu |first7=Yi |last8=Zhang |first8=Yechi |display-authors=3 |title=Pure Spectroscopic Constraints on UV Luminosity Functions and Cosmic Star Formation History From 25 Galaxies at $z_\mathrm{spec}=8.61-13.20$ Confirmed with JWST/NIRSpec |eprint=2304.06658v3 |date=2023 |class=astro-ph.GA }}</ref>
| z {{=}} {{val|11.04}}
| 13.45
|31.45<sup>†</sup>
| 은하
| JWST로 발견된 라이먼 브레이크 은하.
|-
| [[파일:Distant galaxy GN-z11 in GOODS-N image by HST.jpg|100px]]
| [[GN-z11]]
| z = 10.6034 ± 0.0013
| 13.481<ref name="UCLA-2015" /> / 13.501<ref name="UCLA-2018" /> / 13.380<ref name="ICRAR-2022" /> / 13.379<ref name="KEMP-2022" />
|31.18<sup>†</sup>
| 은하
| 라이먼 브레이크 은하; HST가 5.5σ에서 탐지한 라이먼 브레이크.<ref name="Oesch2016">{{저널 인용|title=A Remarkably Luminous Galaxy at ''z''=11.1 Measured with ''Hubble Space Telescope'' Grism Spectroscopy |journal=[[The Astrophysical Journal]] |first1=P. A. |last1=Oesch |first2=G. |last2=Brammer |first3=P. |last3=van Dokkum |display-authors=etal |volume=819 |issue=2 |at=129 |date=March 2016 |arxiv=1603.00461 |bibcode=2016ApJ...819..129O |doi=10.3847/0004-637X/819/2/129|s2cid=119262750 |doi-access=free }}</ref> 그리고 켁/적외선 다중 분광기로  5.3σ에서 탄소 방출선의 탐지.<ref name="Jiang2021">{{저널 인용|title=Evidence for GN-z11 as a luminous galaxy at redshift 10.957|display-authors=etal|first1=Linhua|last1=Jiang|journal=Nature Astronomy|date=January 2021|volume=5|issue=3 |pages=256–261|doi=10.1038/s41550-020-01275-y|arxiv=2012.06936|bibcode=2021NatAs...5..256J|s2cid=229156468 }}</ref> 2023년 2월 JWST에 의한 결정적 적색편이<ref>{{저널 인용|title=JADES NIRSpec Spectroscopy of GN-z11: Lyman- ''α'' emission and possible enhanced nitrogen abundance in a ''z'' = 10.60 luminous galaxy |date=2023 |doi=10.1051/0004-6361/202346159 |arxiv=2302.07256 |last1=Bunker |first1=Andrew J. |last2=Saxena |first2=Aayush |last3=Cameron |first3=Alex J. |last4=Willott |first4=Chris J. |last5=Curtis-Lake |first5=Emma |last6=Jakobsen |first6=Peter |last7=Carniani |first7=Stefano |last8=Smit |first8=Renske |last9=Maiolino |first9=Roberto |last10=Witstok |first10=Joris |last11=Curti |first11=Mirko |last12=d'Eugenio |first12=Francesco |last13=Jones |first13=Gareth C. |last14=Ferruit |first14=Pierre |last15=Arribas |first15=Santiago |last16=Charlot |first16=Stephane |last17=Chevallard |first17=Jacopo |last18=Giardino |first18=Giovanna |last19=De Graaff |first19=Anna |last20=Looser |first20=Tobias J. |last21=Lützgendorf |first21=Nora |last22=Maseda |first22=Michael V. |last23=Rawle |first23=Tim |last24=Rix |first24=Hans-Walter |last25=Del Pino |first25=Bruno Rodríguez |last26=Alberts |first26=Stacey |last27=Egami |first27=Eiichi |last28=Eisenstein |first28=Daniel J. |last29=Endsley |first29=Ryan |last30=Hainline |first30=Kevin |journal=Astronomy & Astrophysics |volume=677 |pages=A88 |s2cid=256846361 |display-authors=1 }}</ref>
|-
| 
| JADES-GS-z10-0 [[UDFj-39546284]]
| z = {{val|10.38|0.07|0.06}}
| 13.449<ref name="UCLA-2015" /> / 13.469<ref name="UCLA-2018" /> / 13.348<ref name="ICRAR-2022" /> / 13.347<ref name="KEMP-2022" />
|31.04<sup>†</sup>
| 은하
| 라이먼 브레이크 은하, JWST/근적외선 분광기로 라이먼 브레이크의 탐지<ref name="Robertson2022"/>
|-
| [[파일:JD1-JWST-GLASS.pdf|100px]]
| JD1
| z = {{val|9.793|0.002}}
| 13.409<ref name="UCLA-2015" /> / 13.429<ref name="UCLA-2018" /> / 13.308<ref name="ICRAR-2022" /> / 13.307<ref name="KEMP-2022" />
|30.12<sup>†</sup>
| 은하
| 라이먼 브레이크 은하, JWST/근적외선 분광기로 라이먼 브레이크의 탐지<ref>{{저널 인용|last1=Roberts-Borsani |first1=Guido |last2=Treu |first2=Tommaso |last3=Chen |first3=Wenlei |last4=Morishita |first4=Takahiro |last5=Vanzella |first5=Eros |last6=Zitrin |first6=Adi |last7=Bergamini |first7=Pietro |last8=Castellano |first8=Marco |last9=Fontana |first9=Adriano |last10=Grillo |first10=Claudio |last11=Kelly |first11=Patrick L. |last12=Merlin |first12=Emiliano |last13=Paris |first13=Diego |last14=Rosati |first14=Piero |last15=Acebron |first15=Ana |title=A shot in the Dark (Ages): a faint galaxy at $z=9.76$ confirmed with JWST |journal = Nature Astronomy |year = 2023 |volume = 618 |issue=7965 |pages = 480–483 |doi = 10.1038/s41586-023-05994-w |pmid=37198479 |arxiv = 2210.15639|bibcode = 2023Natur.618..480R |s2cid=258741077 }}</ref>
|-
| [[파일:Hubble and ALMA image of MACS J1149.5+2223.jpg|100px]]
| [[MACS1149-JD1]]
| z = {{val|9.1096|0.0006}}
| 13.361<ref name="UCLA-2015" /> / 13.381<ref name="UCLA-2018" /> / 13.261<ref name="ICRAR-2022" /> / 13.260<ref name="KEMP-2022" />
|30.37
| 은하
| VLT로 수소 방출선 그리고 ALMA로 산소선의 탐지<ref>{{저널 인용|author=T. Hashimoto |author2=N. Laporte |author3=K. Mawatari |author4=R. S. Ellis |author5=A. K. Inoue |author6=E. Zackrisson |author7=G. Roberts-Borsani |author8=W. Zheng |author9=Y. Tamura |author10=F. E. Bauer |author11=T. Fletcher |author12=Y. Harikane |author13=B. Hatsukade |author14=N. H. Hayatsu |author15=Y. Matsuda |author16=H. Matsuo |author17=T. Okamoto |author18=M. Ouchi |author19=R. Pello |author20=C. Rydberg |author21=I. Shimizu |author22=Y. Taniguchi |author23=H. Umehata |author24=N. Yoshida | title=The Onset of Star Formation 250 Million Years After the Big Bang | journal=Nature | volume=557 | issue=7705 | pages=312–313 |arxiv=1805.05966 |bibcode=2018Natur.557..392H |doi=10.1038/s41586-018-0117-z | pmid=29765123 | year=2019 | s2cid=21702406 }}</ref>
|-
| [[파일:EGSY8p7 por el Hubble y Spitzer.jpg|100px]]
| [[EGSY8p7]]
| z = {{val|8.683|0.001|0.004}}
| 13.325<ref name="UCLA-2015" /> / 13.345<ref name="UCLA-2018" /> / 13.225<ref name="ICRAR-2022" /> / 13.224<ref name="KEMP-2022" />
|30.05
| 은하
| 라이먼 알파 방출체; 그리고 켁/적외선 다중 분광기로  7.5σ 신뢰도로 라이먼 알파의 탐지<ref>{{저널 인용|author=Adi Zitrin |author2=Ivo Labbe |author3=Sirio Belli |author4=Rychard Bouwens |author5=Richard S. Ellis |author6=Guido Roberts-Borsani |author7=Daniel P. Stark |author8=Pascal A. Oesch |author9=Renske Smit | title=Lyman-alpha Emission from a Luminous z = 8.68 Galaxy: Implications for Galaxies as Tracers of Cosmic Reionization | journal=The Astrophysical Journal | volume=810 | issue=1 | pages=L12 |arxiv=1507.02679 |bibcode=2015ApJ...810L..12Z |doi=10.1088/2041-8205/810/1/L12 | year=2015 |s2cid = 11524667}}</ref>
|-
|
| SMACS-4590
| z = 8.496
| 13.308<ref name="UCLA-2015" /> / 13.328<ref name="UCLA-2018" /> / 13.208<ref name="ICRAR-2022" /> / 13.207<ref name="KEMP-2022" />
|29.71<sup>†</sup>
| 은하
| JWST/근적외선 분광기로 수소, 산소 및 네온 방출선 탐지<ref name="Curti2023">{{저널 인용|title=The chemical enrichment in the early Universe as probed by JWST via direct metallicity measurements at z 8|first=Mirko |last=Curti|display-authors=etal|journal=Monthly Notices of the Royal Astronomical Society|date=January 2023|volume=518|issue=1|pages=425–438|doi=10.1093/mnras/stac2737|arxiv=2207.12375|bibcode=2023MNRAS.518..425C}}</ref><ref name="Carnall2023">{{저널 인용|title=A first look at the SMACS0723 JWST ERO: spectroscopic redshifts, stellar masses, and star-formation histories|first=A. C.|last=Carnall|display-authors=etal|journal=Monthly Notices of the Royal Astronomical Society: Letters|date=January 2023|volume=518|issue=1|pages=L45–L50|doi=10.1093/mnrasl/slac136|arxiv=2207.08778|bibcode=2023MNRAS.518L..45C}}</ref><ref name="Schaerer2022">{{저널 인용|title=First look with JWST spectroscopy: Resemblance among z ~ 8 galaxies and local analogs|first=D.|last=Schaerer|display-authors=etal|journal=Astronomy & Astrophysics|date=September 2022|volume=665|id=L4|page=6|doi=10.1051/0004-6361/202244556|arxiv=2207.10034 |bibcode=2022A&A...665L...4S|s2cid=252175886 }}</ref><ref name="Katz2023">{{저널 인용|title=AFirst insights into the ISM at z > 8 with JWST: possible physical implications of a high [O III] λ4363/[O III] λ5007|first=Harley|last=Katz|display-authors=etal|journal=Monthly Notices of the Royal Astronomical Society|date=January 2023|volume=518|issue=1|pages=592–603|doi=10.1093/mnras/stac2657|arxiv=2207.13693|bibcode=2023MNRAS.518..592K}}</ref>
|-
| 
| [[A2744 YD4]]
| z = 8.38
| 13.297<ref name="UCLA-2015" /> / 13.317<ref name="UCLA-2018" /> / 13.197<ref name="ICRAR-2022" /> / 13.196<ref name="KEMP-2022" />
|29.50<sup>†</sup>
| 은하
| ALMA로 4.0σ 신뢰도로 감지된 라이먼 알파와 [O III] 방출<ref>{{저널 인용|author1=Laporte, N. |author2=Ellis, R. S. |author3=Boone, F. |author4=Bauer, F. E. |author5=Quénard, D. |author6=Roberts-Borsani, G. W. |author7=Pelló, R. |author8=Pérez-Fournon, I. |author9=Streblyanska, A. | title=Dust in the Reionization Era: ALMA Observations of a z = 8.38 Gravitationally Lensed Galaxy | journal=The Astrophysical Journal | volume=832 | issue=2 | pages=L21 |arxiv=1703.02039 |bibcode=2017ApJ...837L..21L |doi=10.3847/2041-8213/aa62aa | year=2017 |s2cid = 51841290 |doi-access=free }}</ref>
|-
| 
| [[MACS0416 Y1]]
| z = {{val|8.3118|0.0003}}
| 13.290<ref name="UCLA-2015" /> / 13.310<ref name="UCLA-2018" /> / 13.190<ref name="ICRAR-2022" /> / 13.189<ref name="KEMP-2022" />
|29.44<sup>†</sup>
| 은하
| ALMA로 6.3σ 신뢰도로 감지된 라이먼 알파와 [O III] 방출<ref>{{저널 인용|author1=Tamura, Y. |author2=Mawatari, K. |author3=Hashimoto, T. |author4=Inoue, A. K. |author5=Zackrisson, E. |author6=Christensen, L. |author7=Binggeli, C |author8=Matsuda, Y. |author9=Matsuo, H. |author10=Takeuchi, T. T. |author11=Asano, R. S. |author12=Sunaga, K. |author13=Shimizu, I. |author14=Okamoto, T. |author15=Yoshida, N. |author16=Lee, M. |author17=Shibuya, T. |author18=Taniguchi, Y. |author19=Umehata, H. |author20=Hatsukade, B. |author21=Kohno, K. |author22=Ota, K. | title=Detection of the Far-infrared [O III] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era | journal=The Astrophysical Journal | volume=874 | issue=1 | page=27 |arxiv=1806.04132 |bibcode=2019ApJ...874...27T |doi=10.3847/1538-4357/ab0374 | year=2017 | s2cid=55313459 |doi-access=free }}</ref>
|-
| 
| [[GRB 090423]]
| z = {{val|8.23|0.06|0.07}}
| 13.282<ref name="UCLA-2015" /> / 13.302<ref name="UCLA-2018" /> / 13.182<ref name="ICRAR-2022" /> / 13.181<ref name="KEMP-2022" />
|30
| [[감마선 폭발]]
| 탐지된 라이먼 알파 브레이크<ref name="Tanvir2009">{{저널 인용|bibcode=2009Natur.461.1254T |title=A gamma-ray burst at a redshift of z~8.2 |journal=Nature |volume=461 |issue=7268 |pages=1254–7 |last1=Tanvir |first1=N. R. |last2=Fox |first2=D. B. |last3=Levan |first3=A. J. |last4=Berger |first4=E. |last5=Wiersema |first5=K. |last6=Fynbo |first6=J. P. U. |last7=Cucchiara |first7=A. |last8=Krühler |first8=T. |last9=Gehrels |first9=N. |last10=Bloom |first10=J. S. |last11=Greiner |first11=J. |last12=Evans |first12=P. A. |last13=Rol |first13=E. |last14=Olivares |first14=F. |last15=Hjorth |first15=J. |last16=Jakobsson |first16=P. |last17=Farihi |first17=J. |last18=Willingale |first18=R. |last19=Starling |first19=R. L. C. |last20=Cenko |first20=S. B. |last21=Perley |first21=D. |last22=Maund |first22=J. R. |last23=Duke |first23=J. |last24=Wijers |first24=R. A. M. J. |last25=Adamson |first25=A. J. |last26=Allan |first26=A. |last27=Bremer |first27=M. N. |last28=Burrows |first28=D. N. |last29=Castro-Tirado |first29=A. J. |last30=Cavanagh |first30=B. |display-authors=29 |year=2009 |doi=10.1038/nature08459 |pmid=19865165|arxiv = 0906.1577 |s2cid=205218350 }}</ref>
|-
| 
| [[RXJ2129-11002]]
| z = {{val|8.16|0.01}}
| 13.175<ref name="UCLA-2015" />
|29.31<sup>†</sup>
| 은하
| JWST/근적외선 분광기 프리즘으로 탐지된 라이먼 알파 브레이크와 함께 [O III] 이중선, Hβ 및 [O II] 이중선<ref name="Langeroodi2022">{{저널 인용|author1=Langeroodi, Danial |author2=Hjorth, Jens |author3=Chen, Wenlei |author4=Kelly, Patrick L. |author5=Williams, Hayley |author6=Lin, Yu-Heng |author7=Scarlata, Claudia |author8=Zitrin, Adi |author9=Broadhurst, Tom |author10=Diego, Jose M. |author11=Huang, Xiaosheng |author12=Filippenko, Alexei V. |author13=Foley, Ryan J. |author14=Jha, Saurabh |author15=Koekemoer, Anton M. |author16=Oguri, Masamune |author17=Perez-Fournon, Ismael |author18=Pierel, Justin |author19=Poidevin, Frederick |author20=Strolger, Lou | title=Evolution of the Mass-Metallicity Relation from Redshift z≈8 to the Local Universe | journal=The Astrophysical Journal |arxiv=2212.02491 |bibcode=2015ApJ...804L..30O | year=2022| volume=804 | issue=2 | doi=10.1088/2041-8205/804/2/L30 | s2cid=55115344 }}</ref>
|-
| 
| [[RXJ2129-11022]]
| z = {{val|8.15|0.01}}
| 13.174<ref name="UCLA-2015" />
|29.30<sup>†</sup>
| 은하
| JWST/근적외선 분광기 프리즘으로 탐지된 라이먼 알파 브레이크와 함께 [O III] 이중선, Hβ 및 [O II] 이중선<ref name="Langeroodi2022"/>
|-
| [[파일:Galaxy-EGS-zs8-1-20150505.jpg|100px]]
| [[EGS-zs8-1]]
| z = {{val|7.7302|0.0006}}
| 13.228<ref name="UCLA-2015" /> / 13.248<ref name="UCLA-2018" /> / 13.129<ref name="ICRAR-2022" /> / 13.128<ref name="KEMP-2022" />
|29.5
| 은하
| 라이먼 브레이크 은하<ref>{{저널 인용|author=P. A. Oesch |author2=P. G. van Dokkum |author3=G. D. Illingworth |author4=R. J. Bouwens |author5=I. Momcheva |author6=B. Holden |author7=G. W. Roberts-Borsani |author8=R. Smit |author9=M. Franx |author10=I. Labbe |author11=V. Gonzalez |author12=D. Magee | title=A Spectroscopic Redshift Measurement for a Luminous Lyman Break Galaxy at z = 7.730 using Keck/MOSFIRE |arxiv=1502.05399 |bibcode=2015ApJ...804L..30O |doi=10.1088/2041-8205/804/2/L30 |volume=804 | issue=2 |journal=The Astrophysical Journal |pages=L30 | year=2015 |s2cid = 55115344}}</ref>
|-
|
| SMACS-6355
| z = 7.665
| 13.221<ref name="UCLA-2015" /> / 13.241<ref name="UCLA-2018" /> / 13.121<ref name="ICRAR-2022" /> / 13.120<ref name="KEMP-2022" />
|28.83
| 은하
| JWST/근적외선 분광기로 수소, 산소 및 네론 방출선의 탐지<ref name="Curti2023"/><ref name="Carnall2023"/><ref name="Schaerer2022"/><ref name="Katz2023"/>
|-
|
| z7_GSD_3811
| z = {{val|7.6637|0.0011}}
| 13.221<ref name="UCLA-2015" /> / 13.240<ref name="UCLA-2018" /> / 13.121<ref name="ICRAR-2022" /> / 13.120<ref name="KEMP-2022" />
|28.83<sup>†</sup>
| 은하
| 라이먼 알파 방출체<ref>{{저널 인용| first1=M. |last1=Song |first2=S. L. |last2=Finkelstein |first3=R. C. |last3=Livermore |first4=P. L. |last4=Capak |first5=M. |last5=Dickinson |first6=A. |last6=Fontana
| title=Keck/MOSFIRE Spectroscopy of z = 7–8 Galaxies: Lyman-alpha Emission from a Galaxy at z = 7.66 |journal=The Astrophysical Journal |volume=826 |issue=2 |page=113 |arxiv=1602.02160 | year=2016 |doi=10.3847/0004-637X/826/2/113 |bibcode=2016ApJ...826..113S |s2cid=51806693 |doi-access=free }}</ref>
|-
|
| SMACS-10612
| z = 7.658
| 13.221<ref name="UCLA-2015" /> / 13.241<ref name="UCLA-2018" /> / 13.120<ref name="ICRAR-2022" /> / 13.119<ref name="KEMP-2022" />
|28.83<sup>†</sup>
| 은하
| JWST/근적외선 분광기로 수소, 산소 및 네론 방출선의 탐지<ref name="Curti2023"/><ref name="Carnall2023"/><ref name="Schaerer2022"/>><ref name="Katz2023"/>
|-
| 
| [[QSO J0313–1806]]
| z = {{val|7.6423|0.0013}}
| 13.218<ref name="UCLA-2015" /> / 13.238<ref name="UCLA-2018" /> / 13.119<ref name="ICRAR-2022" /> / 13.118<ref name="KEMP-2022" />
|30
| [[퀘이사]]
| 탐지된 라이먼 알파 브레이크<ref>{{저널 인용|arxiv=2101.03179 |doi=10.3847/2041-8213/abd8c6 |title=A Luminous Quasar at Redshift 7.642 |year=2021 |last1=Wang |first1=Feige |last2=Yang |first2=Jinyi |last3=Fan |first3=Xiaohui |last4=Hennawi |first4=Joseph F. |last5=Barth |first5=Aaron J. |last6=Banados |first6=Eduardo |last7=Bian |first7=Fuyan |last8=Boutsia |first8=Konstantina |last9=Connor |first9=Thomas |last10=Davies |first10=Frederick B. |last11=Decarli |first11=Roberto |last12=Eilers |first12=Anna-Christina |last13=Farina |first13=Emanuele Paolo |last14=Green |first14=Richard |last15=Jiang |first15=Linhua |last16=Li |first16=Jiang-Tao |last17=Mazzucchelli |first17=Chiara |last18=Nanni |first18=Riccardo |last19=Schindler |first19=Jan-Torge |last20=Venemans |first20=Bram |last21=Walter |first21=Fabian |last22=Wu |first22=Xue-Bing |last23=Yue |first23=Minghao |author3-link=Xiaohui Fan |journal=The Astrophysical Journal |volume=907 |issue=1 |pages=L1 |bibcode=2021ApJ...907L...1W |s2cid=231572944 |doi-access=free }}</ref>
|-
| 
| [[ULAS J1342+0928]]
| z = {{val|7.5413|0.0007}}
| 13.206<ref name="UCLA-2015" /> / 13.226<ref name="UCLA-2018" /> / 13.107<ref name="ICRAR-2022" /> / 13.106<ref name="KEMP-2022" />
|29.36
| 퀘이사
| [C II] 방출로부터 추정된 적색편이<ref name="NAT-20171206">{{저널 인용|author=Bañados, Eduardo|display-authors=etal|title=An 800-million-solar-mass black hole in a significantly neutral Universe at a redshift of 7.5 |date=6 December 2017 |journal=[[Nature (journal)|Nature]] |volume=553|issue=7689|pages=473–476|doi=10.1038/nature25180 |pmid=29211709|arxiv=1712.01860 |bibcode=2018Natur.553..473B |s2cid=205263326 }}</ref>
|-
| [[파일:Z8 GND 5296.jpg|100px]]
| [[z8_GND_5296]]
| z = 7.51
| 13.202<ref name="UCLA-2015" /> / 13.222<ref name="UCLA-2018" /> / 13.103<ref name="ICRAR-2022" /> / 13.102<ref name="KEMP-2022" />
|30.01
| 은하
| 라이먼 알파 방출체<ref>{{저널 인용|author=S. L. Finkelstein |author2=C. Papovich |author3=M. Dickinson |author4=M. Song |author5=V. Tilvi |author6=A. M. Koekemoer |author7=K. D. Finkelstein |author8=B. Mobasher |author9=H. C. Ferguson |author10=M. Giavalisco |author11=N. Reddy |author12=M. L. N. Ashby |author13=A. Dekel |author14=G. G. Fazio |author15=A. Fontana |author16=N. A. Grogin |author17=J.-S. Huang |author18=D. Kocevski |author19=M. Rafelski |author20=B. J. Weiner |author21=S. P. Willner | title=A galaxy rapidly forming stars 700 million years after the Big Bang at redshift 7.51 |arxiv=1310.6031 |journal=[[Nature (journal)|Nature]] |date=2013 |volume=502 |issue=7472 |pages=524–527 |doi=10.1038/nature12657 |bibcode=2013Natur.502..524F |pmid=24153304| s2cid=4448085 }}</ref>
|-
| [[파일:A1689-zD1.jpg|100px]]
| [[A1689-zD1]]
| z = {{val|7.5|0.2}}
| 13.201<ref name="UCLA-2015" /> / 13.221<ref name="UCLA-2018" /> / 13.102<ref name="ICRAR-2022" /> / 13.101<ref name="KEMP-2022" />
|30
| 은하
| 라이먼 알파 방출체<ref>{{저널 인용|last1=Watson |first1=Darach |last2=Christensen |first2=Lise |author3-link=Kirsten Kraiberg Knudsen |last3=Knudsen |first3=Kirsten Kraiberg |last4=Richard |first4=Johan |last5=Gallazzi |first5=Anna |last6=Michałowski |first6=Michał Jerzy |title=A dusty, normal galaxy in the epoch of reionization |journal=Nature |volume=519 |issue=7543 |pages=327–330 |doi=10.1038/nature14164 |pmid=25731171 |arxiv=1503.00002 |bibcode=2015Natur.519..327W |year=2015|s2cid=2514879 }}</ref>
|-
|
| GS2_1406
| z = {{val|7.452|0.003}}
| 13.195<ref name="UCLA-2015" /> / 13.215<ref name="UCLA-2018" /> / 13.096<ref name="ICRAR-2022" /> / 13.095<ref name="KEMP-2022" />
|28.62<sup>†</sup>
| 은하
| 라이먼 알파 방출체<ref>{{저널 인용| first1=R. L. |last1=Larson |first2=S. L. |last2=Finkelstein |first3=N. |last3=Pirzkal |first4=R. |last4=Ryan |first5=V. |last5=Tilvi |first6=S. |last6=Malhotra |first7=J. |last7=Rhoads |first8=K. |last8=Finkelstein | first9=I. |last9=Jung |first10=L. |last10=Christensen |first11=A. |last11=Cimatti |first12=I. |last12=Ferreras |first13=N. |last13=Grogin |first14=A. M. |last14=Koekemoer |first15=N. |last15=Hathi |first16=R. |last16=O'Connell |first17=G. |last17=Östlin |first18=A. |last18=Pasquali |first19=J. |last19=Pharo |first20=B. |last20=Rothberg |first21=R. A. |last21=Windhorst | title=Discovery of a z = 7.452 High Equivalent Width Lyman alpha Emitter from the Hubble Space Telescope Faint Infrared Grism Survey |journal=The Astrophysical Journal |volume=858 |issue=2 |page=113 |arxiv=1712.05807 | year=2018 |doi=10.3847/1538-4357/aab893 |bibcode=2018ApJ...858...94L  |s2cid=119257857 |doi-access=free }}</ref>
|-
| [[파일:GN-108036.jpg|100px]]
| [[GN-108036]]
| z = 7.213
| 13.164<ref name="UCLA-2015" /> / 13.184<ref name="UCLA-2018" /> / 13.065<ref name="ICRAR-2022" /> / 13.064<ref name="KEMP-2022" />
|29
| 은하
| 라이먼 알파 방출체<ref name="Ono2012"/>
|-
| [[파일:SXDF-NB1006-2.jpeg|100px]]
| [[SXDF-NB1006-2]]
| {{nowrap|z {{=}} {{val|7.2120|0.0003}}}}
| 13.164<ref name="UCLA-2015" /> / 13.184<ref name="UCLA-2018" /> / 13.065<ref name="ICRAR-2022" /> / 13.064<ref name="KEMP-2022" />
|29
| 은하
| 탐지된 [O III] 방출<ref>{{저널 인용|title=Detection of an oxygen emission line from a high redshift galaxy in the reionization epoch|url=https://www.eso.org/public/archives/releases/sciencepapers/eso1620/eso1620a.pdf|first1=Akio K.|last1=Inoue|display-authors=etal|journal=Science|volume=352|issue=6293|pages=1559–1562|doi=10.1126/science.aaf0714|arxiv=1606.04989|bibcode=2016Sci...352.1559I|date=June 2016|pmid=27312046|s2cid=206646433 }}</ref>
|-
| [[파일:ALMA witnesses assembly of galaxy in early Universe (annotated).jpg|100px]]
| [[BDF-3299]]
| z = {{val|7.109|0.002}}
| 13.149<ref name="UCLA-2015" /> / 13.169<ref name="UCLA-2018" /> / 13.051<ref name="ICRAR-2022" /> / 13.050<ref name="KEMP-2022" />
|28.25
| 은하
| 라이먼 브레이크 은하<ref name="Vanzella et al.">{{저널 인용|last=Vanzella |display-authors=etal |date=2011 |title=Spectroscopic Confirmation of Two Lyman Break Galaxies at Redshift Beyond 7 |journal=[[The Astrophysical Journal Letters]] |volume=730 |issue=2 |pages=L35 |doi=10.1088/2041-8205/730/2/L35 |bibcode=2011ApJ...730L..35V |arxiv=1011.5500 |s2cid=53459241 }}</ref>
|-
| [[파일:ULAS J1120+0641.jpg|100px]]
| [[ULAS J1120+0641]]
| z = {{val|7.085|0.003}}
| 13.146<ref name="UCLA-2015" /> / 13.166<ref name="UCLA-2018" /> / 13.048<ref name="ICRAR-2022" /> / 13.047<ref name="KEMP-2022" />
|29.85
| 퀘이사
| Si III]+C III] 및 Mg II 방출선들로부터 추정된 적색편이<ref>{{저널 인용|title=A luminous quasar at a redshift of z = 7.085 |author=Daniel J. Mortlock |author2=Stephen J. Warren |author3=Bram P. Venemans|display-authors=etal |journal=Nature |volume=474 |issue=7353 |pages=616–619 |date=2011 |doi=10.1038/nature10159|arxiv=1106.6088 |bibcode = 2011Natur.474..616M |pmid=21720366|s2cid=2144362 }}
</ref>
|-
| [[파일:A1703 zD6.jpg|100px]]
| [[A1703 zD6]]
| z = {{val|7.045|0.004}}
| 13.140<ref name="UCLA-2015" /> / 13.160<ref name="UCLA-2018" /> / 13.042<ref name="ICRAR-2022" /> / 13.041<ref name="KEMP-2022" />
|29
| 은하
| 중력렌즈 현상의 라이먼 알파 방출체<ref>{{저널 인용|bibcode=2012ApJ...744..179S|doi= 10.1088/0004-637X/744/2/179|title=Keck Spectroscopy of Faint 3 < z < 8 Lyman Break Galaxies: Evidence for a Declining Fraction of Emission Line Sources in the Redshift Range 6 < z < 8|journal=The Astrophysical Journal|volume=744|issue=2|page=7|date=January 2012|last1=Schenker|first1=Matthew A.|display-authors=etal|arxiv=1107.1261|s2cid= 119244384}}</ref>
|-
| 
| [[BDF-521]]
| z = {{val|7.008|0.002}}
| 13.135<ref name="UCLA-2015" /> / 13.155<ref name="UCLA-2018" /> / 13.037<ref name="ICRAR-2022" /> / 13.036<ref name="KEMP-2022" />
|28.43<sup>†</sup>
| 은하
| 라이먼 알파 은하<ref name="Vanzella et al." />
|-
|
| G2_1408
| z = {{val|6.972|0.002}}
| 13.130<ref name="UCLA-2015" /> / 13.150<ref name="UCLA-2018" /> / 13.032<ref name="ICRAR-2022" /> / 13.030<ref name="KEMP-2022" />
|28.10<sup>†</sup>
| 은하
| 라이먼 알파 방출체<ref>{{저널 인용|arxiv=1010.2754 |last1=Fontana |first1=A. |title=The lack of intense Lyman~alpha in ultradeep spectra of z = 7 candidates in GOODS-S: Imprint of reionization? |journal=The Astrophysical Journal |volume=725 |issue=2 |pages=L205 |last2=Vanzella |first2=E. |last3=Pentericci |first3=L. |last4=Castellano |first4=M. |last5=Giavalisco |first5=M. |last6=Grazian |first6=A. |last7=Boutsia |first7=K. |last8=Cristiani |first8=S. |last9=Dickinson |first9=M. |last10=Giallongo |first10=E. |last11=Maiolino |first11=M. |last12=Moorwood |first12=A. |last13=Santini |first13=P. |year=2010 |doi=10.1088/2041-8205/725/2/L205 |bibcode=2010ApJ...725L.205F|s2cid=119270473 }}</ref>
|-
| [[파일:IOK-1.jpg|100px]]
| [[IOK-1]]
| z = 6.965
| 13.129<ref name="UCLA-2015" /> / 13.149<ref name="UCLA-2018" /> / 13.030<ref name="ICRAR-2022" /> / 13.029<ref name="KEMP-2022" />
|28.09<sup>†</sup>
| 은하
| 라이먼 알파 방출체<ref name="Ono2012">{{저널 인용|arxiv=1107.3159 |title=Spectroscopic Confirmation of Three z-Dropout Galaxies at z = 6.844 – 7.213: Demographics of Lyman-Alpha Emission in z ~ 7 Galaxies |journal=The Astrophysical Journal |volume=744 |issue=2 |page=83 |last1=Ono |first1=Yoshiaki |last2=Ouchi |first2=Masami |last3=Mobasher |first3=Bahram |last4=Dickinson |first4=Mark |last5=Penner |first5=Kyle |last6=Shimasaku |first6=Kazuhiro |last7=Weiner |first7=Benjamin J. |last8=Kartaltepe |first8=Jeyhan S. |last9=Nakajima |first9=Kimihiko |last10=Nayyeri |first10=Hooshang |last11=Stern |first11=Daniel |last12=Kashikawa |first12=Nobunari |last13=Spinrad |first13=Hyron |year=2011 |doi=10.1088/0004-637X/744/2/83 |bibcode=2012ApJ...744...83O|s2cid = 119306980}}</ref>
|-
| [[파일:LAE J095950.99+021219.1.jpg|100px]]
| [[LAE J095950.99+021219.1]]
| z = 6.944
| 13.126<ref name="UCLA-2015" /> / 13.146<ref name="UCLA-2018" /> / 13.028<ref name="ICRAR-2022" /> / 13.027<ref name="KEMP-2022" />
|28.07<sup>†</sup>
| 은하
| 라이먼 알파 방출체<ref>{{저널 인용|arxiv=1205.3161 |last1=Rhoads |first1=James E. |title=A Lyman Alpha Galaxy at Redshift z = 6.944 in the COSMOS Field |journal=The Astrophysical Journal |volume=752 |issue=2 |pages=L28 |last2=Hibon |first2=Pascale |last3=Malhotra |first3=Sangeeta |last4=Cooper |first4=Michael |last5=Weiner |first5=Benjamin |year=2012 |doi=10.1088/2041-8205/752/2/L28 |bibcode=2012ApJ...752L..28R|s2cid=118383532 }}</ref>
|-
| 
| SDF-46975
| z = 6.844
| 13.111<ref name="UCLA-2015" /> / 13.131<ref name="UCLA-2018" /> / 13.013<ref name="ICRAR-2022" /> / 13.012<ref name="KEMP-2022" />
|27.95<sup>†</sup>
| 은하<br/> .......................
| 라이먼 알파 방출체<ref name="Ono2012"/>
|-
|
| [[PSO J172.3556+18.7734]]
|''z'' = {{val|6.823|0.003|0.001}}
| 13.107<ref name="UCLA-2015" /> / 13.127<ref name="UCLA-2018" /> / 13.010<ref name="ICRAR-2022" /> / 13.009<ref name="KEMP-2022" />
|27.93<sup>†</sup>
| 퀘이사<br/>([[제트 (천문학)|천체물리학적 제트]])
| Mg II 방출로부터 추정된 적색편이<ref>{{저널 인용|title=The Discovery of a Highly Accreting, Radio-loud Quasar at z = 6.82 |journal=The Astrophysical Journal |publisher=Harvard University |bibcode=2021ApJ...909...80B |last1=Bañados |first1=Eduardo |last2=Mazzucchelli |first2=Chiara |last3=Momjian |first3=Emmanuel |last4=Eilers |first4=Anna-Christina |last5=Wang |first5=Feige |last6=Schindler |first6=Jan-Torge |last7=Connor |first7=Thomas |last8=Andika |first8=Irham Taufik |last9=Barth |first9=Aaron J. |last10=Carilli |first10=Chris |last11=Davies |first11=Frederick B. |last12=Decarli |first12=Roberto |last13=Fan |first13=Xiaohui |last14=Farina |first14=Emanuele Paolo |last15=Hennawi |first15=Joseph F. |last16=Pensabene |first16=Antonio |last17=Stern |first17=Daniel |last18=Venemans |first18=Bram P. |last19=Wenzl |first19=Lukas |last20=Yang |first20=Jinyi |year=2021 |volume=909 |issue=1 |page=80 |doi=10.3847/1538-4357/abe239 |arxiv=2103.03295 |s2cid=232135300 |doi-access=free }}</ref>
|-
| colspan="7" |
<small>
§ 표에 표시된 거리는 광행거리로, 물리적으로 직접적인 의미는 없다. [[거리 측정]] 및 [[관측 가능한 우주]]에서 논의를 참조하라.
</small>

† Wright (2006)<ref name="UCLA-2018" />를 사용하여 얻은 숫자 값: <math>H_{0}  </math> = 70, <math>\Omega_{CM}</math> = 0.30, <math>\Omega_{DE}</math> = 0.70.
|}

== 가장 먼 천체 후보 ==
2022년 6월 [[제임스 웹 우주망원경]](JWST)의 과학 작업이 시작된 이래, 적외선을 멀리까지 볼 수 있는 JWST의 능력 덕분에 [[허블 우주망원경]](z = 11)으로 볼 수 있는 것보다 훨씬 더 먼 수많은 은하가 발견되었다.<ref name="Adams2022"/><ref name="Yan2023">{{저널 인용|title=First Batch of z ≈ 11–20 Candidate Objects Revealed by the James Webb Space Telescope Early Release Observations on SMACS 0723-73|first=Haojing|last=Yan|display-authors=etal|journal=The Astrophysical Journal Letters|date=January 2023|volume=942|issue=L9|page=20|doi-access=free|doi=10.3847/2041-8213/aca80c|arxiv=2207.11558|bibcode=2023ApJ...942L...9Y}}</ref>  2012년 이전에는 2002년 중반부터 2012년 12월 사이에 관측된 [[w:Hubble eXtreme Deep Field|허블 익스트림 딥 필드(Hubble eXtreme Deep Field)]](XDF) 프로젝트에서 발표한 측광학적 적색편이 추정치를 기반으로 z = 8 이상의 천체 약 50개와 z = 7의 후보 천체 100개가 있었다.<ref name=fg>{{웹 인용|url=http://www.firstgalaxies.org/the-latest-results |title=Our Latest Results |author1=Garth Illingworth |author2=Rychard Bouwens |author3=Pascal Oesch |author4=Ivo Labbe |author5=Dan Magee |website=FirstGalaxies |date=December 2012 |access-date=March 10, 2016}}</ref> 여기에 포함된 일부 천체는 분광학적으로 관측되었지만, 단지 한 방출선만이 잠정적으로 탐지되었으므로, 따라서 연구자들은 여전히 후보로 간주하고 있다.<ref name="Harikane2022b">{{저널 인용|title=A Comprehensive Study of Galaxies at z ~ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch|first=Yuichi|last=Harikane|journal=The Astrophysical Journal Supplement Series |year=2023 |volume=265 |issue=1 |page=5 |display-authors=etal|arxiv=2208.01612|doi=10.3847/1538-4365/acaaa9 |bibcode=2023ApJS..265....5H |s2cid=251253150 |doi-access=free }}</ref><ref name="Fujimoto2022"/>

{| class="wikitable"
|+ 가장 먼 천체 후보로 주목할 만한 천체
|-
|-
! 명칭
! [[적색편이]] <br />(z)
! [[거리 측정 (우주론)|광행거리]]<sup>§</sup> <br />([[광년|Gly]])
! 유형
! 노트
|-
| [[F200DB-045]]
| z<sub>p</sub> = {{val|20.4|0.3|0.3}}<ref name="Yan2023"/><br/>or {{val|0.70|0.19|0.55}}<ref name="Adams2022"/> or {{val|0.40|0.15|0.26}}<ref name="MorishitaStiavelli2022"/>
| 13.725<ref name="UCLA-2015" /> / 13.745<ref name="UCLA-2018" />  / 13.623<ref name="ICRAR-2022"/> / 13.621<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/><br />'''노트:''' 한 연구에서 절차에 의해 제시된 은하의 적색편이 값은<ref name="Adams2022"/> 다른 절차를 사용하는 다른 연구에서 제시된 값과 다를 수 있다.<ref name="Yan2023" /><ref name="ARX-20221209">{{저널 인용|arxiv=2208.01612v3|last1=Harikane |first1=Yuichi |last2=Ouchi |first2=Masami |last3=Oguri |first3=Masamune |last4=Ono |first4=Yoshiaki |last5=Nakajima |first5=Kimihiko |last6=Isobe |first6=Yuki |last7=Umeda |first7=Hiroya |last8=Mawatari |first8=Ken |last9=Zhang |first9=Yechi |title=A Comprehensive Study of Galaxies at z ~ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch |journal=The Astrophysical Journal Supplement Series |year=2023 |volume=265 |issue=1 |page=5 |doi=10.3847/1538-4365/acaaa9 |bibcode=2023ApJS..265....5H |s2cid=251253150 |doi-access=free }}</ref><ref name="MorishitaStiavelli2022">{{저널 인용|arxiv=2207.11671v2|last1=Morishita |first1=Takahiro |last2=Stiavelli |first2=Massimo |title=Physical Characterization of Early Galaxies in the Webb's First Deep Field SMACS J0723.3-7323 |journal=The Astrophysical Journal Letters |year=2023 |volume=946 |issue=2 |pages=L35 |doi=10.3847/2041-8213/acbf50 |bibcode=2023ApJ...946L..35M |s2cid=254220684 |doi-access=free }}</ref>
|-
| [[F200DB-175]]
| z<sub>p</sub> = {{val|16.2|0.3|0.0}}
| 13.657<ref name="UCLA-2015" /> / 13.677<ref name="UCLA-2018" />  / 13.555<ref name="ICRAR-2022"/> / 13.554<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[S5-z17-1]]
| {{nowrap|z {{=}} {{val|16.0089|0.0004}}}}<br/>or {{val|4.6108|0.0001}}
| 13.653<ref name="UCLA-2015" /> / 13.673<ref name="UCLA-2018" />  / 13.551<ref name="ICRAR-2022"/> / 13.550<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하; [C II] (z = {{val|4.6108|0.0001}}) 또는 [O III] (z = {{val|16.0089|0.0004}}) 중 하나에 기인한 것으로 추정되는 단일 방출선에 대한 잠정적 (5.1σ) ALMA 탐지. [C II] (z = {{val|4.6108|0.0001}}) or [O III] (z = {{val|16.0089|0.0004}}).<ref name="Harikane2022b"/><ref name="Fujimoto2022">{{저널 인용|title=ALMA FIR View of Ultra High-redshift Galaxy Candidates at z ~ 11-17: Blue Monsters or Low- z Red Interlopers?|first=Seiji|last=Fujimoto|journal=The Astrophysical Journal |display-authors=etal|arxiv=2211.03896|date=2023|volume=955 |issue=2 |page=130 |doi=10.3847/1538-4357/aceb67 |bibcode=2023ApJ...955..130F |doi-access=free }}</ref>
|-
| [[F150DB-041]]
| z<sub>p</sub> = {{val|16.0|0.2|0.2}}<ref name="Yan2023"/><br/>or {{val|3.70|0.02|0.59}}<ref name="Adams2022"/>
| 13.653<ref name="UCLA-2015" /> / 13.673<ref name="UCLA-2018" />  / 13.551<ref name="ICRAR-2022"/> / 13.549<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/><ref name="Adams2022"/>
|-
| [[SMACS-z16a]]
| z<sub>p</sub> = {{val|15.92|0.17|0.15}}<ref name="Hakim2022"/><br/>or {{val|2.96|0.73|0.21}}<ref name="Adams2022"/>
| 13.651<ref name="UCLA-2015" /> / 13.671<ref name="UCLA-2018" />  / 13.549<ref name="ICRAR-2022"/> / 13.548<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Hakim2022">{{저널 인용|title=Revealing galaxy candidates out to z 16 with JWST observations of the lensing cluster SMACS0723|first=Atek|last=Hakim|display-authors=etal|journal=Monthly Notices of the Royal Astronomical Society|doi=10.1093/mnras/stac3144|arxiv=2207.12338|bibcode=2023MNRAS.519.1201A|date=November 2022|volume=519 |issue=1 |pages=1201–1220 }}</ref><ref name="Adams2022">{{저널 인용|title=Discovery and properties of ultra-high redshift galaxies (9 < z < 12) in the JWST ERO SMACS 0723 Field|first=N. J.|last=Adams|display-authors=etal|journal=Monthly Notices of the Royal Astronomical Society|doi=10.1093/mnras/stac3347|arxiv=2207.11217|bibcode=2023MNRAS.518.4755A|date=November 2022|volume=518 |issue=3 |pages=4755–4766 }}</ref>
|-
| [[F200DB-015]]
| z<sub>p</sub> = {{val|15.8|3.4|0.1}}
| 13.648<ref name="UCLA-2015" /> / 13.668<ref name="UCLA-2018" />  / 13.546<ref name="ICRAR-2022"/> / 13.545<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F200DB-181]]
| z<sub>p</sub> = {{val|15.8|0.5|0.3}}
| 13.648<ref name="UCLA-2015" /> / 13.668<ref name="UCLA-2018" />  / 13.546<ref name="ICRAR-2022"/> / 13.545<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F200DB-159]]
| z<sub>p</sub> = {{val|15.8|4.0|15.2}}
| 13.648<ref name="UCLA-2015" /> / 13.668<ref name="UCLA-2018" />  / 13.546<ref name="ICRAR-2022"/> / 13.545<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F200DB-086]]
| z<sub>p</sub> = {{val|15.4|0.6|14.6}}<ref name="Yan2023"/><br/>or {{val|3.53|10.28|1.84}}<ref name="Adams2022"/>
| 13.639<ref name="UCLA-2015" /> / 13.659<ref name="UCLA-2018" />  / 13.537<ref name="ICRAR-2022"/> / 13.536<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/><ref name="Adams2022"/>
|-
| [[SMACS-z16b]]
| z<sub>p</sub> = {{val|15.32|0.16|0.13}}<ref name="Hakim2022"/><br/>or {{val|15.39|0.18|0.26}}<ref name="Adams2022"/>
| 13.637<ref name="UCLA-2015" /> / 13.657<ref name="UCLA-2018" />  / 13.535<ref name="ICRAR-2022"/> / 13.534<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Hakim2022"/><ref name="Adams2022"/>
|-
| [[F150DB-048]]
| z<sub>p</sub> = {{val|15.0|0.2|0.8}}
| 13.629<ref name="UCLA-2015" /> / 13.649<ref name="UCLA-2018" />  / 13.527<ref name="ICRAR-2022"/> / 13.526<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DB-007]]
| z<sub>p</sub> = {{val|14.6|0.4|0.4}}
| 13.619<ref name="UCLA-2015" /> / 13.639<ref name="UCLA-2018" />  / 13.517<ref name="ICRAR-2022"/> / 13.516<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DB-004]]
| z<sub>p</sub> = {{val|14.0|0.4|2.0}}
| 13.602<ref name="UCLA-2015" /> / 13.622<ref name="UCLA-2018" />  / 13.500<ref name="ICRAR-2022"/> / 13.499<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DB-079]]
| z<sub>p</sub> = {{val|13.8|0.5|1.9}}
| 13.596<ref name="UCLA-2015" /> / 13.616<ref name="UCLA-2018" />  / 13.494<ref name="ICRAR-2022"/> / 13.493<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-007]]
| z<sub>p</sub> = {{val|13.4|0.6|2.0}}
| 13.583<ref name="UCLA-2015" /> / 13.603<ref name="UCLA-2018" />  / 13.481<ref name="ICRAR-2022"/> / 13.480<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-053]]
| z<sub>p</sub> = {{val|13.4|0.3|2.3}}
| 13.583<ref name="UCLA-2015" /> / 13.603<ref name="UCLA-2018" />  / 13.481<ref name="ICRAR-2022"/> / 13.480<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-050]]
| z<sub>p</sub> = {{val|13.4|0.6|10.0}}
| 13.583<ref name="UCLA-2015" /> / 13.603<ref name="UCLA-2018" />  / 13.481<ref name="ICRAR-2022"/> / 13.480<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-058]]
| z<sub>p</sub> = {{val|13.4|0.6|12.5}}<ref name="Yan2023"/><br/>{{val|3.42|0.30|0.20}}<ref name="Adams2022"/>
| 13.583<ref name="UCLA-2015" /> / 13.603<ref name="UCLA-2018" />  / 13.481<ref name="ICRAR-2022"/> / 13.480<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/><ref name="Adams2022"/>
|-
| [[F150DA-038]]
| z<sub>p</sub> = {{val|13.4|0.4|13.2}}
| 13.583<ref name="UCLA-2015" /> / 13.603<ref name="UCLA-2018" />  / 13.481<ref name="ICRAR-2022"/> / 13.480<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[HD1 (galaxy)|HD1]]
| z = {{val|13.27}}
| 13.579<ref name="UCLA-2015" /> / 13.599<ref name="UCLA-2018" />  / 13.477<ref name="ICRAR-2022"/> / 13.476<ref name="KEMP-2022" />
| 은하
| 아직 분광학적으로 확인되지 않았다. 가장 먼 거리에서 확인된 은하 기네스 세계 기록
라이먼 브레이크 은하(5σ 신뢰도)에 이어 ALMA에서 [[금지선|[O III]]] 방출선 하나만 잠정적으로 탐지(4σ 신뢰도)<ref name="Harikane2022a">{{저널 인용|display-authors = etal |first1 = Y. |last1 = Harikane |title = A Search for H-Dropout Lyman Break Galaxies at z ~ 12–16 |journal=The Astrophysical Journal | volume=929 | issue=1 | page=1 |bibcode=2022ApJ...929....1H |doi=10.3847/1538-4357/ac53a9 |date = April 2022 |arxiv = 2112.09141|s2cid = 246823511 |doi-access = free }}</ref>
|-
| [[F150DA-010]]
| z<sub>p</sub> = {{val|12.8|0.6|1.5}}
| 13.562<ref name="UCLA-2015" /> / 13.582<ref name="UCLA-2018" />  / 13.460<ref name="ICRAR-2022"/> / 13.459<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[S5-z12-1]]
| z<sub>p</sub> = {{val|12.57|1.23|0.46}}
| 13.553<ref name="UCLA-2015" /> / 13.573<ref name="UCLA-2018" />  / 13.452<ref name="ICRAR-2022"/> / 13.451<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Harikane2022b"/>
|-
| [[CEERS-27535 4]]
| z<sub>p</sub> = {{val|12.56|1.75|0.27}}
| 13.553<ref name="UCLA-2015" /> / 13.573<ref name="UCLA-2018" />  / 13.452<ref name="ICRAR-2022"/> / 13.451<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022">{{저널 인용|last=Donnan|first=C. T.|display-authors=et al. |title=The evolution of the galaxy UV luminosity function at redshifts z ≃ 8 - 15 from deep JWST and ground-based near-infrared imaging|journal=Monthly Notices of the Royal Astronomical Society|doi=10.1093/mnras/stac3472|arxiv=2207.12356|bibcode=2023MNRAS.518.6011D|date=November 2022|volume=518 |issue=4 |pages=6011–6040 }}</ref>
|-
| [[SMACS-1566]]
| z<sub>p</sub> = {{val|12.29|1.50|0.44}}
| 13.542<ref name="UCLA-2015" /> / 13.562<ref name="UCLA-2018" />  / 13.441<ref name="ICRAR-2022"/> / 13.440<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[SMACS-z12b]]<br/>(F150DA-077)
| z<sub>p</sub> = {{val|12.26|0.17|0.16}}<ref name="Hakim2022"/><ref name="Adams2022"/><br/>or {{val|13.4|0.4|1.7}}<ref name="Yan2023"/>
| 13.541<ref name="UCLA-2015" /> / 13.561<ref name="UCLA-2018" />  / 13.440<ref name="ICRAR-2022"/> / 13.439<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Hakim2022"/><ref name="Adams2022"/><ref name="Yan2023"/>
|-
| [[SMACS-z12a]]
| z<sub>p</sub> = {{val|12.20|0.21|0.12}}
| 13.539<ref name="UCLA-2015" /> / 13.559<ref name="UCLA-2018" />  / 13.437<ref name="ICRAR-2022"/> / 13.436<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Hakim2022"/><ref name="Adams2022"/>
|-
| [[CR2-z12-4]]
| z<sub>p</sub> = {{val|12.08|2.11|1.25}}
| 13.534<ref name="UCLA-2015" /> / 13.554<ref name="UCLA-2018" />  / 13.432<ref name="ICRAR-2022"/> / 13.431<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Harikane2022b"/>
|-
| [[SMACS-10566]]
| z<sub>p</sub> = {{val|12.03|0.57|0.26}}
| 13.532<ref name="UCLA-2015" /> / 13.552<ref name="UCLA-2018" />  / 13.430<ref name="ICRAR-2022"/> / 13.429<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[XDFH-2395446286]]
| z<sub>p</sub> = {{val|12.0|0.1|0.2}}
| 13.530<ref name="UCLA-2015" /> / 13.550<ref name="UCLA-2018" />  / 13.429<ref name="ICRAR-2022"/> / 13.428<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Bouwens2022">{{저널 인용|title=Evolution of the UV LF from z ~ 15 to z ~ 8 using new JWST NIRCam medium-band observations over the HUDF/XDF|first=Rychard J.|last=Bouwens|journal=Monthly Notices of the Royal Astronomical Society |year=2023 |volume=523 |pages=1036–1055 |display-authors=etal|arxiv=2211.02607|doi=10.1093/mnras/stad1145 }}</ref>
|-
| [[CR2-z12-2]]
| z<sub>p</sub> = {{val|11.96|1.44|0.87}}
| 13.529<ref name="UCLA-2015" /> / 13.549<ref name="UCLA-2018" />  / 13.427<ref name="ICRAR-2022"/> / 13.426<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Harikane2022b"/>
|-
| [[9-BUSCAR]]
| z<sub>p</sub> = {{val|11.91|0.10|0.22}}
| 13.527<ref name="UCLA-2015" /> / 13.547<ref name="UCLA-2018" />  / 13.425<ref name="ICRAR-2022"/> / 13.424<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Rodighiero2022">{{저널 인용|first1=Giulia|last1=Rodighiero|author1-link=Giulia Rodighiero|display-authors=etal|title=JWST unveils heavily obscured (active and passive) sources up to z 13|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=518|issue=1|pages=L19–L24|date=January 2023|doi=10.1093/mnrasl/slac115 |arxiv=2208.02825|bibcode=2023MNRAS.518L..19R}}</ref>
|-
| [[SMACS-8347]]
| z<sub>p</sub> = {{val|11.90|0.27|0.39}}
| 13.526<ref name="UCLA-2015" /> / 13.546<ref name="UCLA-2018" />  / 13.425<ref name="ICRAR-2022"/> / 13.424<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[CEERS-26409 4]]
| z<sub>p</sub> = {{val|11.90|1.60|0.70}}
| 13.526<ref name="UCLA-2015" /> / 13.546<ref name="UCLA-2018" />  / 13.425<ref name="ICRAR-2022"/> / 13.424<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[F150DB-069]]
| z<sub>p</sub> = {{val|11.8|1.7|0.2}}
| 13.522<ref name="UCLA-2015" /> / 13.542<ref name="UCLA-2018" />  / 13.420<ref name="ICRAR-2022"/> / 13.419<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[XDFH-2334046578]]
| z<sub>p</sub> = {{val|11.8|0.4|0.5}}
| 13.522<ref name="UCLA-2015" /> / 13.542<ref name="UCLA-2018" />  / 13.420<ref name="ICRAR-2022"/> / 13.419<ref name="KEMP-2022" />
| 은하
| JWST와 허블우주망원경에 의해 발견된 라이먼 브레이크 은하<ref name="Bouwens2022"/>
|-
| [[CR2-z12-3]]
| z<sub>p</sub> = {{val|11.66|0.69|0.71}}
| 13.515<ref name="UCLA-2015" /> / 13.535<ref name="UCLA-2018" />  / 13.414<ref name="ICRAR-2022"/> / 13.413<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Harikane2022b"/>
|-
| [[CR2-z12-1]]
| z<sub>p</sub> = {{val|11.63|0.51|0.53}}
| 13.514<ref name="UCLA-2015" /> / 13.534<ref name="UCLA-2018" />  / 13.413<ref name="ICRAR-2022"/> / 13.412<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Harikane2022b"/>
|-
| [[F150DB-088]]
| z<sub>p</sub> = {{val|11.6|0.3|0.2}}
| 13.513<ref name="UCLA-2015" /> / 13.533<ref name="UCLA-2018" />  / 13.411<ref name="ICRAR-2022"/> / 13.410<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DB-084]]
| z<sub>p</sub> = {{val|11.6|0.4|0.4}}
| 13.513<ref name="UCLA-2015" /> / 13.533<ref name="UCLA-2018" />  / 13.411<ref name="ICRAR-2022"/> / 13.410<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DB-044]]
| z<sub>p</sub> = {{val|11.4|0.4|11.3}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[XDFH-2404647339]]
| z<sub>p</sub> = {{val|11.4|0.4|0.5}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST와 허블우주망원경에 의해 발견된 라이먼 브레이크 은하<ref name="Bouwens2022"/>
|-
| [[F150DB-075]]
| z<sub>p</sub> = {{val|11.4|0.4|0.1}}<ref name="Yan2023"/><br/>{{val|0.04|0.01|0.01}}<ref name="Adams2022"/>
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/><ref name="Adams2022"/>
|-
| [[F150DA-062]]
| z<sub>p</sub> = {{val|11.4|0.3|0.3}}<ref name="Yan2023"/><br/>{{val|1.78|0.20|0.08}}<ref name="Adams2022"/>
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/><ref name="Adams2022"/>
|-
| [[CEERS-127682]]
| z<sub>p</sub> = {{val|11.40|0.59|0.51}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[CEERS-5268 2]]
| z<sub>p</sub> = {{val|11.40|0.30|1.11}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[F150DA-060]]
| z<sub>p</sub> = {{val|11.4|0.6|8.2}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-031]]
| z<sub>p</sub> = {{val|11.4|1.0|8.2}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-052]]
| z<sub>p</sub> = {{val|11.4|0.8|10.6}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DB-054]]
| z<sub>p</sub> = {{val|11.4|0.5|10.8}}
| 13.503<ref name="UCLA-2015" /> / 13.523<ref name="UCLA-2018" />  / 13.402<ref name="ICRAR-2022"/> / 13.401<ref name="KEMP-2022" />
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[SMACS-z11d]]
| z<sub>p</sub> = {{val|11.28|0.32}}<br/>or {{val|2.35|0.30|0.67}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Adams2022"/>
|-
| [[CEERS-77241]]
| z<sub>p</sub> = {{val|11.27|0.39|0.70}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[CEERS-6647]]
| z<sub>p</sub> = {{val|11.27|0.58|0.28}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[CEERS-622 4]]
| z<sub>p</sub> = {{val|11.27|0.48|0.60}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[SMACS-z11c]]
| z<sub>p</sub> = {{val|11.22|0.32}}<br/>or {{val|3.84|0.05|0.04}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Adams2022"/>
|-
| [[SMACS-z11b]]
| z<sub>p</sub> = {{val|11.22|0.56}}<br/>or {{val|6.94|0.07|0.07}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Adams2022"/>
|-
| [[F150DA-005]]
| z<sub>p</sub> = {{val|11.2|0.4|0.3}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-020]]
| z<sub>p</sub> = {{val|11.2|0.2|7.9}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[CEERS-61486]]
| z<sub>p</sub> = {{val|11.15|0.37|0.35}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Donnan2022"/>
|-
| [[SMACS-z11e]]<br/>(F150DA-081)
| z<sub>p</sub> = {{val|11.10|0.21|0.34}}<ref name="Adams2022"/><br/>or {{val|13.4|0.6|2.2}}<ref name="Yan2023"/>
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Adams2022"/><ref name="Yan2023"/>
|-
| [[SMACS-z11a]]
| z<sub>p</sub> = {{val|11.05|0.09|0.08}}<ref name="Hakim2022"/><br/>or {{val|1.73|0.18|0.04}}<ref name="Adams2022"/>
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Hakim2022"/><ref name="Adams2022"/>
|-
| [[CR3-z12-1]]
| z<sub>p</sub> = {{val|11.05|2.24|0.47}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Harikane2022b"/>
|-
| [[F150DA-026]]
| z<sub>p</sub> = {{val|11.0|0.5|0.3}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[F150DA-036]]
| z<sub>p</sub> = {{val|11.0|0.4|7.8}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[SMACS-z10e]]
| z<sub>p</sub> = {{val|10.89|0.16|0.14}}<ref name="Hakim2022"/><br/>or {{val|1.38|1.37|0.24}}<ref name="Adams2022"/>
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Hakim2022"/><ref name="Adams2022"/>
|-
| [[F150DB-040]]
| z<sub>p</sub> = {{val|10.8|0.3|0.2}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Yan2023"/>
|-
| [[EGS-14506]]
| z<sub>p</sub> = {{val|10.71|0.34|0.62}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Whitler2022">{{저널 인용|first1=Lily|last1=Whitler|display-authors=etal|title=On the ages of bright galaxies 500 Myr after the Big Bang: insights into star formation activity at z ≳ 15 with JWST|journal=Monthly Notices of the Royal Astronomical Society|date=December 2022|volume=519 |issue=1 |pages=157–171 |doi=10.1093/mnras/stac3535|arxiv=2208.01599|bibcode=2023MNRAS.519..157W}}</ref>
|-
| [[MACS0647-JD]]
| z<sub>p</sub> = {{val|10.6|0.3}}
| 
| 은하
| 한 [[은하단]]에 의해 세 이미지로 나타난 [[중력렌즈|중력렌즈 현상]]; JWST와 허블우주망원경으로 발견됨.<ref>{{저널 인용| bibcode = 2013ApJ...762...32C | title=CLASH: Three Strongly Lensed Images of a Candidate z ~ 11 Galaxy | journal=The Astrophysical Journal | volume=762 | issue=1 | page=32 | year=2013 | doi=10.1088/0004-637x/762/1/32|arxiv = 1211.3663 | last1=Coe | first1=Dan | last2=Zitrin | first2=Adi | last3=Carrasco | first3=Mauricio | last4=Shu | first4=Xinwen | last5=Zheng | first5=Wei | last6=Postman | first6=Marc | last7=Bradley | first7=Larry | last8=Koekemoer | first8=Anton | last9=Bouwens | first9=Rychard | last10=Broadhurst | first10=Tom | last11=Monna | first11=Anna | last12=Host | first12=Ole | last13=Moustakas | first13=Leonidas A. | last14=Ford | first14=Holland | last15=Moustakas | first15=John | last16=Van Der Wel | first16=Arjen | last17=Donahue | first17=Megan | last18=Rodney | first18=Steven A. | last19=Benítez | first19=Narciso | last20=Jouvel | first20=Stephanie | last21=Seitz | first21=Stella | last22=Kelson | first22=Daniel D. | last23=Rosati | first23=Piero | s2cid=119114237 }}</ref><ref name="Hsiao2022">{{저널 인용|title=JWST Reveals a Possible z ~ 11 Galaxy Merger in Triply Lensed MACS0647–JD|first=Tiger Yu-Yang|last=Hsiao|journal=The Astrophysical Journal Letters |year=2023 |volume=949 |issue=2 |pages=L34 |display-authors=etal|arxiv=2210.14123|doi=10.3847/2041-8213/acc94b |bibcode=2023ApJ...949L..34H |s2cid=253107903 |doi-access=free }}</ref>
|-
| [[GLASS-z10]]<br/>(GLASS-1698)<ref name="Donnan2022"/>
| z = 10.38
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하;  [O III] 방출선 만의 잠적적 (4.4σ) ALMA 탐지<ref name="Naidu2022">{{저널 인용|title=Two Remarkably Luminous Galaxy Candidates at z ≈ 10 − 12 Revealed by JWST|first=Rohan P.|last=Naidu|display-authors=etal|journal=The Astrophysical Journal Letters|volume=940|issue=1|id=L14|page=11|doi=10.3847/2041-8213/ac9b22|arxiv=2207.09434|bibcode=2022ApJ...940L..14N|date=November 2022|s2cid=250644267 |doi-access=free }}</ref><ref name="Yoon2022">{{저널 인용|title=ALMA Observation of a z ≳ 10 Galaxy Candidate Discovered with JWST|first=Ilsang|last=Yoon|journal=The Astrophysical Journal |display-authors=etal|arxiv=2210.08413|date=2023|volume=950 |issue=1 |page=61 |doi=10.3847/1538-4357/acc94d |bibcode=2023ApJ...950...61Y |doi-access=free }}</ref>
|-
| [[EGS-7860]]
| z<sub>p</sub> = {{val|10.11|0.60|0.82}}
| 
| 은하
| JWST에 의해 발견된 라이먼 브레이크 은하<ref name="Whitler2022"/>
|-
| [[SPT0615-JD]]
| z<sub>p</sub> = {{val|9.9|0.8|0.6}}
| 13.419<ref name="UCLA-2015" />
| 은하
|<ref>{{저널 인용|arxiv=1801.03103 |title= A Candidate z~10 Galaxy Strongly Lensed into a Spatially Resolved Arc|journal= The Astrophysical Journal|volume= 864|pages= L22|last1= Salmon|first1= Brett|last2= Coe|first2= Dan|last3= Bradley|first3= Larry|last4= Bradač|first4= Marusa|last5= Huang|first5= Kuang-Han|last6= Strait|first6= Victoria|last7= Oesch|first7= Pascal|last8= Paterno-Mahler|first8= Rachel|last9= Zitrin|first9= Adi|last10= Acebron|first10= Ana|last11= Cibirka|first11= Nathália|last12= Kikuchihara|first12= Shotaro|last13= Oguri|first13= Masamune|last14= Brammer|first14= Gabriel B|last15= Sharon|first15= Keren|last16= Trenti|first16= Michele|last17= Avila|first17= Roberto J|last18= Ogaz|first18= Sara|last19= Andrade-Santos|first19= Felipe|last20= Carrasco|first20= Daniela|last21= Cerny|first21= Catherine|last22= Dawson|first22= William|last23= Frye|first23= Brenda L|last24= Hoag|first24= Austin|last25= Jones|first25= Christine|last26= Mainali|first26= Ramesh|last27= Ouchi|first27= Masami|last28= Rodney|first28= Steven A|last29= Stark|first29= Daniel|last30= Umetsu|first30= Keiichi|year= 2018|doi= 10.3847/2041-8213/aadc10|s2cid= 78087820|doi-access= free}}</ref>
|-
| [[A2744-JD]]
| z<sub>p</sub>≅9.8
| 13.412<ref name="UCLA-2015" />
| 은하<BR/>...............................
| 은하가 확대되고 또한 세 다중 이미지로의 중력렌즈 현상.<ref>{{웹 인용|url=http://www.nasa.gov/press/2014/october/nasa-s-hubble-finds-extremely-distant-galaxy-through-cosmic-magnifying-glass/#.VJBxQmTF_fY |title=Hubble Finds Distant Galaxy Through Cosmic Magnifying Glass |work=NASA|date=23 April 2015 }}</ref><ref>{{저널 인용| doi=10.1088/2041-8205/793/1/L12 | volume=793 | issue=1 | title=A Geometrically Supported z ~ 10 Candidate Multiply Imaged by the Hubble Frontier Fields Cluster A2744 | journal=The Astrophysical Journal | pages=L12 |arxiv=1407.3769 |bibcode=2014ApJ...793L..12Z | year=2014 | last1=Zitrin | first1=Adi | last2=Zheng | first2=Wei | last3=Broadhurst | first3=Tom | last4=Moustakas | first4=John | last5=Lam | first5=Daniel | last6=Shu | first6=Xinwen | last7=Huang | first7=Xingxing | last8=Diego | first8=Jose M. | last9=Ford | first9=Holland | last10=Lim | first10=Jeremy | last11=Bauer | first11=Franz E. | last12=Infante | first12=Leopoldo | last13=Kelson | first13=Daniel D. | last14=Molino | first14=Alberto | s2cid=43853349 | url=http://hub.hku.hk/bitstream/10722/206809/1/content.pdf }}</ref>
|-
| [[MACS1149-JD1]]
| z<sub>p</sub>≅9.6
| 13.398<ref name="UCLA-2015" /><ref>{{웹 인용|url=http://www.nasa.gov/mission_pages/spitzer/news/spitzer20120919.html |title=NASA Telescopes Spy Ultra-Distant Galaxy|publisher=NASA }}</ref>
| 후보 은하 또는 원시은하
|<ref name="zheng2012">{{저널 인용| last1=Zheng | first1=W. | last2=Postman | first2=M. | last3=Zitrin | first3=A. | last4=Moustakas | first4=J. | last5=Shu | first5=X. | last6=Jouvel | first6=S. | last7=Høst | first7=O. | last8=Molino | first8=A. | last9=Bradley | first9=L. | last10=Coe | doi=10.1038/nature11446 | first10=D. | last11=Moustakas | first11=L. A. | last12=Carrasco | first12=M. | last13=Ford | first13=H. | last14=Benítez | first14=N. | last15=Lauer | first15=T. R. | last16=Seitz | first16=S. | last17=Bouwens | first17=R. | author-link17 = Rychard Bouwens| last18=Koekemoer | first18=A. | last19=Medezinski | first19=E. | last20=Bartelmann | first20=M. | last21=Broadhurst | first21=T. | last22=Donahue | first22=M. |author22-link= Megan Donahue | last23=Grillo | first23=C. | last24=Infante | first24=L. | last25=Jha | first25=S. W. | last26=Kelson | first26=D. D. | last27=Lahav | first27=O. | last28=Lemze | first28=D. | last29=Melchior | first29=P. | last30=Meneghetti | first30=M. | title=A magnified young galaxy from about 500 million years after the Big Bang | journal=Nature | volume=489 | issue=7416 | pages=406–408 | year=2012 | pmid=22996554 |arxiv=1204.2305 |bibcode=2012Natur.489..406Z | s2cid=4415218 }}</ref>
|-
| [[GRB 090429B]]
| z<sub>p</sub>≅9.4
| 13.383<ref name="UCLA-2015" /><ref name=PennState-2011-05-25>Penn State Science, [http://science.psu.edu/news-and-events/2011-news/Fox5-2011 "Cosmic Explosion is New Candidate for Most Distant Object in the Universe"], Derek. B. Fox, Barbara K. Kennedy, 25 May 2011</ref>
| [[감마선 폭발]]
|<ref name=SD-2011-05-27>Space Daily, [http://www.spacedaily.com/reports/Explosion_Helps_Researcher_Spot_Universe_Most_Distant_Object_999.html Explosion Helps Researcher Spot Universe's Most Distant Object], 27 May 2011</ref> 이 경우 측광학적 적색편이는 불확실성이 상당히 크며, 적색편이의 하한은 z>7이다.
|-
| [[UDFy-33436598]]
| z<sub>p</sub>≅8.6
| 13.317<ref name="UCLA-2015" />
| 후보 은하 또는 원시은하
|<ref name=eso>{{웹 인용|url=http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=50876 |title=ESA Science & Technology: The Hubble eXtreme Deep Field (annotated) }}</ref>
|-
| [[UDFy-38135539]]
| z<sub>p</sub>≅8.6
| 13.317<ref name="UCLA-2015" />
| 후보 은하 또는 원시은하
| 2010년 이 광원에 z=8.55 의 분광학적 적색편이가 주장되었다.<ref name=UDFy-38135539>{{웹 인용|url=https://www.newscientist.com/article/dn19603-dim-galaxy-is-most-distant-object-yet-found.html |title=Dim galaxy is most distant object yet found |author=David Shiga |work=New Scientist}}</ref> 그러나 이후 잘못된 것으로 밝혀졌다.<ref name="Bunker2013">{{저널 인용|bibcode=2013MNRAS.430.3314B |title=VLT/XSHOOTER and Subaru/MOIRCS spectroscopy of HUDF.YD3: no evidence for Lyman & |journal=Monthly Notices of the Royal Astronomical Society |volume=430 |issue=4 |page=3314 |last1=Bunker |first1=Andrew J. |last2=Caruana |first2=Joseph |last3=Wilkins |first3=Stephen M. |last4=Stanway |first4=Elizabeth R. |last5=Lorenzoni |first5=Silvio |last6=Lacy |first6=Mark |last7=Jarvis |first7=Matt J. |last8=Hickey |first8=Samantha |year=2013 |doi=10.1093/mnras/stt132|arxiv = 1301.4477 }}</ref>
|-
| [[BoRG-58]]
| z<sub>p</sub>≅8
| 13.258<ref name="UCLA-2015" />
| [[은하단]] 또는<BR/> 원시은하단
| 원시은하단 후보<ref name="Trenti2012">{{저널 인용|title=Overdensities of Y-dropout Galaxies from the Brightest-of-Reionizing Galaxies Survey: A Candidate Protocluster at Redshift z ≈ 8|journal=The Astrophysical Journal |volume=746 |issue=1 |page=55 |last1=Trenti |first1=M. |last2=Bradley |first2=L. D. |last3=Stiavelli |first3=M. |last4=Shull |first4=J. M. |last5=Oesch |first5=P. |last6=Bouwens |first6=R. J. | author-link6 = Rychard Bouwens|last7=Munoz |first7=J. A. |last8=Romano-Diaz |first8=E. |last9=Treu |first9=T. |last10=Shlosman |first10=I. |last11=Carollo |first11=C. M. | author-link11 = C. Marcella Carollo| year=2011 |arxiv=1110.0468 |doi=10.1088/0004-637X/746/1/55 |bibcode=2012ApJ...746...55T |s2cid=119294290 }}</ref>
|-
|colspan=5|
<small>
§ 표에 기재된 거리는 광행거리인데 직접적인 물리적 의의는 없다. [[거리 측정]] 및 [[관측 가능한 우주]]에 대한 토론 참조
</small>
|}

{{동적 목록}}

== 최원거리 천체의 유형별 목록 ==
{| class="wikitable"
|+ 유형별 최원거리 천체
|-
! 유형
! 천체
! 적색편이<br/>(거리)
! 노트
|-
| 유형에 관계없이 모든 [[천체]]
|rowspan=2 |[[JADES-GS-z13-0]]
|rowspan=2 |z = 13.20
|rowspan=2 |2022년 12월 현재 분광학적으로 적색편이가 확인된 가장 먼 은하<ref name="Robertson2022"/> 이는 2022년 12월 9일 현재 진행 중인 웹 과학의 데이터로, 아직 동료 검토 과정을 거치지 않은 데이터이다. 광행거리는 약 136억 광년(현재 우리가 관측하는 빛이 약 136억 년 전에 지구를 떠난 이후 우주의 팽창으로 인해 지구로부터 약 336억 광년(103억 파섹)의 고유거리)으로 추정된다.<ref name="UCLA-2018"/>{{참고|en:List of galaxies}}
|-
| [[은하]] 또는 [[원시은하]]
|-
| [[은하단]]
| [[CL J1001+0220]]
| z ≅ 2.506
| 2016년 기준<ref name=AJ-828-1>{{저널 인용|arxiv=1604.07404 |doi= 	10.3847/0004-637X/828/1/56 |title=Discovery of a galaxy cluster with a violently starbursting core at z=2.506 |journal=The Astrophysical Journal |volume=828 |number=1 |year=2016 |last1=Wang |first1=Tao |last2=Elbaz |first2=David |last3=Daddi |first3=Emanuele |last4=Finoguenov |first4=Alexis |last5=Liu |first5=Daizhong |last6=Schrieber |first6=Corenin |last7=Martin |first7=Sergio |last8=Strazzullo |first8=Veronica |last9=Valentino |first9=Francesco |last10=van Der Burg |first10=Remco |last11=Zanella |first11=Anita |last12=Cisela |first12=Laure |last13=Gobat |first13=Raphael |last14=Le Brun |first14=Amandine |last15=Pannella |first15=Maurilio |last16=Sargent |first16=Mark |last17=Shu |first17=Xinwen |last18=Tan |first18=Qinghua |last19=Cappelluti |first19=Nico | last20=Li |first20=Xanxia |page=56|bibcode = 2016ApJ...828...56W |s2cid= 	8771287 |doi-access= 	free }}</ref>{{참고|en:List of galaxy clusters}}
|-
| [[초은하단]]
| [[Hyperion proto-supercluster]]
| z = 2.45
| 2018년 발견 당시 이 초은하단은 지금까지 발견된 초은하단 중 가장 빠르고 가장 큰 원시 초은하단이였다.<ref>{{저널 인용|arxiv=1806.06073|title=The progeny of a Cosmic Titan: a massive multi-component proto-supercluster in formation at z=2.45 in VUDS|last1=Cucciati|first1=O.|last2=Lemaux|first2=B. C.|last3=Zamorani|first3=G.|last4=Le Fevre|first4=O.|last5=Tasca|first5=L. A. M.|last6=Hathi|first6=N. P.|last7=Lee|first7=K-G.|last8=Bardelli|first8=S.|last9=Cassata|first9=P.|last10=Garilli|first10=B.|last11=Le Brun|first11=V.|last12=Maccagni|first12=D.|last13=Pentericci|first13=L.|last14=Thomas|first14=R.|last15=Vanzella|first15=E.|last16=Zucca|first16=E.|last17=Lubin|first17=L. M.|last18=Amorin|first18=R.|last19=Cassara'|first19=L. P.|last20=Cimatti|first20=A.|last21=Talia|first21=M.|last22=Vergani|first22=D.|last23=Koekemoer|first23=A.|last24=Pforr|first24=J.|last25=Salvato|first25=M.|journal = [[Astronomy & Astrophysics]]|year=2018|volume = 619|pages = A49|doi = 10.1051/0004-6361/201833655|bibcode = 2018A&A...619A..49C|s2cid = 119472428}}</ref> {{참고|en:List of superclusters}}
|-
| [[은하단|원시은하단]]
| [[A2744z7p9OD]]
| z = 7.88
| 2023년 발견 당시 이 원시은하단은 지금까지 발견되어 분광학적으로 확인된 원시은하단 중 가장 멀리 떨어져 있다.<ref name=arXiv-2211.09097>{{저널 인용|title= Early results from GLASS-JWST. XVIII: A spectroscopically confirmed protocluster 650 million years after the Big Bang|author1=Morishita, Takahiro  |author2=Roberts-Borsani, Guido  |author3=Treu, Tommaso  |author4=Brammer, Gabriel  |author5=Mason, Charlotte A.  |author6=Trenti, Michele  |author7=Vulcani, Benedetta  |author8=Wang, Xin  |author9=Acebron, Ana  |author10=Bahé, Yannick  |author11=Bergamini, Pietro  |author12=Boyett, Kristan  |author13=Bradac, Marusa  |author14=Calabrò, Antonello  |author15=Castellano, Marco  |author16=Chen, Wenlei  |author17=De Lucia, Gabriella  |author18=Filippenko, Alexei V.  |author19=Fontana, Adriano  |author20=Glazebrook, Karl  |author21=Grillo, Claudio  |author22=Henry, Alaina  |author23=Jones, Tucker  |author24=Kelly, Patrick L.  |author25=Koekemoer, Anton M.  |author26=Leethochawalit, Nicha  |author27=Lu, Ting-Yi  |author28=Marchesini, Danilo  |author29=Mascia, Sara  |author30=Mercurio, Amata  |author31=Merlin, Emiliano  |author32=Metha, Benjamin  |author33=Nanayakkara, Themiya  |author34=Nonino, Mario  |author35=Paris, Diego  |author36=Pentericci, Laura  |author37=Santini, Paola  |author38=Strait, Victoria  |author39=Vanzella, Eros  |author40=Windhorst, Rogier A.  |author41=Rosati, Piero  |author42=Xie, Lizhi |date= 30 January 2023|arxiv= 2211.09097|journal= Astrophysical Journal Letters |volume=947 |issue=2 |doi=10.3847/2041-8213/acb99e |bibcode=2023ApJ...947L..24M |s2cid=253553396 |doi-access=free }}</ref> {{참고|en:List of galaxy groups and clusters}}
|-
| [[퀘이사]]
|rowspan=2 |[[UHZ1]]
|rowspan=2 |z ~ 10.0
|<ref name=Bogdan2023/>{{참고|en:List of quasars}}
|-
| [[블랙홀]]
|<ref name=Bogdan2023>{{인용|journal=[[Nature Astronomy]]|title=Evidence for heavy-seed origin of early supermassive black holes from a z≈10 x-ray quasar|date=November 6, 2023 |author=[[Akos Bogdan]] |volume=8 |pages=126–133 |display-authors=etal |doi=10.1038/s41550-023-02111-9 |arxiv=2305.15458 |bibcode= |s2cid=258887541 }}</ref>
|-
| [[별]] 또는 [[원시별]] 또는 항성 이후의 시체 <br /> <small>(사건으로 탐지)</small>
| [[Gamma-ray burst progenitor|Progenitor]] of [[GRB 090423]]
| z = 8.2
|<ref name="NASA-2009-04-28">NASA, [https://science.nasa.gov/science-news/science-at-nasa/2009/28apr_grbsmash/ "New Gamma-Ray Burst Smashes Cosmic Distance Record"] {{웨이백|url=https://science.nasa.gov/science-news/science-at-nasa/2009/28apr_grbsmash/ |date=20110310193130 }}, 28 April 2009</ref><ref name="Tanvir2009" /> 참고로, [[w:GRB 090429B|GRB 090429B]]는 측광학적 적색편차 zp≅9.4,<ref name=SC-2011-05-27>Science Codex, [http://www.sciencecodex.com/nasas_swift_finds_most_distant_gammaray_burst_yet "GRB 090429B – most distant gamma-ray burst yet"] {{Webarchive|url=https://web.archive.org/web/20110531000312/http://www.sciencecodex.com/nasas_swift_finds_most_distant_gammaray_burst_yet |date=2011-05-31 }}, ''NASA/Goddard'', 27 May 2011</ref> 따라서 GRB 090423보다 더 멀리 떨어져 있을 가능성이 높지만, 분광학적 확인이 부족하다. {{참고|en:List of gamma-ray bursts}} 지구에서 약 130억 광년 떨어진 거리로 추정됨
|-
| [[별]] 또는 [[원시별]] 또는 항성 이후의 시체 <br /> <small>(사건으로 탐지)</small></small>
| [[WHL0137-LS|WHL0137-LS (Earendel)]]
| {{nowrap|1=z = 6.2 ± 0.1}} <br/>(12.9 [[기가|G]][[광년|ly]])
| [[w:List of most distant stars|가장 멀리 떨어진 개별]] 별 발견 (2022년 3월)<ref>{{저널 인용|author=Welch, Brian |display-authors=et al. |title=A highly magnified star at redshift 6.2 |url=https://www.nature.com/articles/s41586-022-04449-y |date=30 March 2022 |journal=[[Nature (journal)|Nature]] |volume=603 |issue=7903 |pages=815–818 |doi=10.1038/s41586-022-04449-y |pmid=35354998 |arxiv=2209.14866 |bibcode=2022Natur.603..815W |s2cid=247842625 |access-date=30 March 2022 }}</ref><ref name="NASA-20220330">{{뉴스 인용|last1=Gianopoulos |first1=Andrea |title=Record Broken: Hubble Spots Farthest Star Ever Seen |url=https://www.nasa.gov/feature/goddard/2022/record-broken-hubble-spots-farthest-star-ever-seen |date=30 March 2022 |work=[[NASA]] |access-date=30 March 2022 }}</ref>
이전 기록으로는 [[SDSS J1229+1122]]<ref>{{잡지 인용|author=Camille M. Carlisle |url=http://www.skyandtelescope.com/astronomy-news/the-most-distant-star-everseen/ |title=The Most Distant Star Ever Seen? |magazine=Sky and Telescope |date=12 April 2013}}</ref> 및 [[MACS J1149 Lensed Star 1]].<ref>{{저널 인용| doi=10.1038/s41550-018-0430-3 | title=Extreme magnification of an individual star at redshift 1.5 by a galaxy-cluster lens | year=2018 | last1=Kelly | first1=Patrick L. | last2=Diego | first2=Jose M. | last3=Rodney | first3=Steven | last4=Kaiser | first4=Nick | last5=Broadhurst | first5=Tom | last6=Zitrin | first6=Adi | last7=Treu | first7=Tommaso | last8=Pérez-González | first8=Pablo G. | last9=Morishita | first9=Takahiro | last10=Jauzac | first10=Mathilde | last11=Selsing | first11=Jonatan | last12=Oguri | first12=Masamune | last13=Pueyo | first13=Laurent | last14=Ross | first14=Timothy W. | last15=Filippenko | first15=Alexei V. | last16=Smith | first16=Nathan | last17=Hjorth | first17=Jens | last18=Cenko | first18=S. Bradley | last19=Wang | first19=Xin | last20=Howell | first20=D. Andrew | last21=Richard | first21=Johan | last22=Frye | first22=Brenda L. | last23=Jha | first23=Saurabh W. | last24=Foley | first24=Ryan J. | last25=Norman | first25=Colin | last26=Bradac | first26=Marusa | last27=Zheng | first27=Weikang | last28=Brammer | first28=Gabriel | last29=Benito | first29=Alberto Molino | last30=Cava | first30=Antonio | journal=Nature Astronomy | volume=2 | issue=4 | pages=334–342 | arxiv=1706.10279 | bibcode=2018NatAs...2..334K | s2cid=119412560 | display-authors=1 }}</ref>이 있다.
|-
| [[성단]]
|rowspan=2 | [[The Sparkler]]
|rowspan=2 | z = 1.378<br/>(13.9 [[기가|G]][[광년|ly]])
|rowspan=2 | [[SMACS J0723.3-7327]]<ref name="Mowla2022">{{저널 인용|first=Lamiya|last=Mowla|display-authors=etal|title=The Sparkler: Evolved High-redshift Globular Cluster Candidates Captured by JWST|journal=The Astrophysical Journal Letters|date=October 2022|volume=937|issue=2|id=L35|page=9|doi-access=free|doi=10.3847/2041-8213/ac90ca|arxiv=2208.02233|bibcode=2022ApJ...937L..35M}}</ref>에 중력 렌즈가 있는 구상성단이 있는 은하계.
|-
| 성단의 시스템
|-
| 엑스레이 제트
| [[PJ352–15]] quasar jet
| z = 5.831 <br />(12.7 [[기가|G]][[광년|ly]])<ref>{{저널 인용|arxiv = 2103.03879|doi = 10.3847/1538-4357/abe710|title = Enhanced X-Ray Emission from the Most Radio-powerful Quasar in the Universe's First Billion Years|year = 2021|last1 = Connor|first1 = Thomas|last2 = Bañados|first2 = Eduardo|last3 = Stern|first3 = Daniel|last4 = Carilli|first4 = Chris|last5 = Fabian|first5 = Andrew|last6 = Momjian|first6 = Emmanuel|last7 = Rojas-Ruiz|first7 = Sofía|last8 = Decarli|first8 = Roberto|last9 = Farina|first9 = Emanuele Paolo|last10 = Mazzucchelli|first10 = Chiara|last11 = Earnshaw|first11 = Hannah P.|journal = The Astrophysical Journal|volume = 911|issue = 2|page = 120|bibcode = 2021ApJ...911..120C|s2cid = 232148026 | doi-access=free }}</ref>
| 이전 기록 보유체는 12.4Gl였다.<ref>[https://www.nasa.gov/mission_pages/chandra/images/gigantic-jet-spied-from-black-hole-in-early-universe.html NASA.gov]</ref><ref name=SpaceDaily-2012-11-30>SpaceDaily, [http://www.spacedaily.com/reports/Record_Setting_X_ray_Jet_Discovered_999.html "Record-Setting X-ray Jet Discovered"], 30 November 2012 (accessed 4 December 2012)</ref>
|-
| [[w:Microquasar|마이크로퀘이사]]
| [[XMMU J004243.6+412519]]
| (2.5 Mly)
| 최초로 발견된 은하계 밖의 마이크로 퀘이사.<ref>ESA, [http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=51225 "Artist's impression of the X-ray binary XMMU J004243.6+412519"], 12 December 2012 (accessed 18 December 2012)</ref><ref>e! Science News, [http://esciencenews.com/sources/scientific.blogging/2012/12/12/xmmu.j004243.6412519.black.hole.binary.at.the.eddington.limit "XMMU J004243.6+412519: Black-Hole Binary At The Eddington Limit"], 12 December 2012 (accessed 18 December 2012)</ref><ref>SpaceDaily, [http://www.spacedaily.com/reports/Microquasar_found_in_neighbor_galaxy_tantalizing_scientists_999.html "Microquasar found in neighbor galaxy, tantalizing scientists"], 17 December 2012 (accessed 18 December 2012)</ref>
|-
| 유사 [[성운]] 천체
| [[Himiko (Lyman-alpha blob)|Himiko]]
| z = 6.595
| 아마도 초기 우주에서 가장 큰 천체 중 하나.<ref>{{저널 인용|last1=Ouchi |first1=Masami |last2=Ono |first2=Yoshiaki |last3=Egami |first3=Eiichi |last4=Saito |first4=Tomoki |last5=Oguri |first5=Masamune |last6=McCarthy |first6=Patrick J. |last7=Farrah |first7=Duncan |last8=Kashikawa |first8=Nobunari |last9=Momcheva |first9=Ivelina |last10=Shimasaku |first10=Kazuhiro |last11=Nakanishi |first11=Kouichiro |last12=Furusawa |first12=Hisanori |last13=Akiyama |first13=Masayuki |last14=Dunlop |first14=James S. |last15=Mortier |first15=Angela M. J. |date=2009-05-01 |title=Discovery of a Giant Lyα Emitter Near the Reionization Epoch |url=https://ui.adsabs.harvard.edu/abs/2009ApJ...696.1164O |journal=The Astrophysical Journal |volume=696 |issue=2 |pages=1164–1175 |doi=10.1088/0004-637X/696/2/1164 |arxiv=0807.4174 |bibcode=2009ApJ...696.1164O |s2cid=15246638 |issn=0004-637X}}</ref><ref>{{뉴스 인용|url=http://www.space.com/scienceastronomy/090422-space-blob.html|title=Giant Mystery Blob Discovered Near Dawn of Time|last=Hsu|first=Jeremy|date=2009-04-22|publisher=[[SPACE.com]]|access-date=2009-04-24}}</ref>
|-
|[[자기장]]
|[[9io9]]
|z = 2.554 (11.1 Gly)
|ALMA로부터의 관측은 (중력)렌즈 효과의 은하 9io9에는 자기장이 포함하고 있음을 보여준다.
|-
| [[행성]]<br/>...............................
| [[SWEEPS-11]] / [[SWEEPS-04]]
| (27,710 ly)
|<ref name=USA-2006-01-25>USA Today, [https://www.usatoday.com/tech/science/space/2006-01-25-exoplanet-discovery_x.htm "Smallest, most distant planet outside solar system found"], '''Malcolm Ritter''', ''25 January 2006'' (accessed 5 August 2010)</ref>
* 마이크로렌즈 사건 [[PA-99-N2]]의 광도 곡선을 분석한 결과, [[안드로메다 은하]]에서 별 궤도를 도는 행성이 존재한다는 사실이 밝혀졌다.<ref>{{백과사전 인용|url=http://exoplanet.eu/star.php?st=PA-99-N2 |archive-url=https://web.archive.org/web/20100206051747/http://exoplanet.eu/star.php?st=PA-99-N2 |url-status=dead |archive-date=February 6, 2010 |title=Notes for star PA-99-N2 |author=Schneider, J. |encyclopedia=[[Extrasolar Planets Encyclopaedia]] |access-date=2010-08-06}}</ref>
* 논란이 되고 있는 이중 중력렌즈 효과의 [[Q0957+561]]의 로브(lobe) A의 마이크로렌즈 사건은 렌즈 효과의 은하에 적색편차 0.355(3.7Gly)에 놓인 한 행성이 있음을 시사한다.<ref>Exoplaneten.de, [http://www.exoplaneten.de/Q0957+561/english.html "The Microlensing Event of Q0957+561"] {{Webarchive|url=https://web.archive.org/web/20120211130721/http://www.exoplaneten.de/Q0957+561/english.html |date=2012-02-11 }} (accessed 5 August 2010)</ref><ref>{{저널 인용| last1=Schild | first1=R.E. | year=1996 | title=Microlensing Variability of the Gravitationally Lensed Quasar Q0957+561 A, B | journal=Astrophysical Journal | volume=464 | page=125 | doi=10.1086/177304 | bibcode=1996ApJ...464..125S}}</ref>
|-
|}

{| class="wikitable"
|+ 유형별 원거리 사건
|-
! 유형
! 사건
! 적색편이
! 노트
|-
| [[감마선 폭발]]
| [[GRB 090423]]
| z = 8.2
|<ref name="NASA-2009-04-28" /><ref name="Tanvir2009" /> 참고로, [[GRB 090429B]]는 측광학적 적색편이 z<sub>p</sub>≅9.4,<ref name="SC-2011-05-27" /> 따라서 GRB 090423보다 더 멀리 떨어져 있을 가능성이 높지만, 분광학적 확인이 부족하다.{{참고|en:List of gamma-ray bursts}}
|-
| [[초신성|중심핵붕괴 초신성]]
| [[SN 1000+0216]]
| z = 3.8993
|<ref>{{저널 인용|bibcode=2012Natur.491..228C |title=Superluminous supernovae at redshifts of 2.05 and 3.90 |journal=Nature |volume=491 |issue=7423 |pages=228–31 |last1=Cooke |first1=Jeff |last2=Sullivan |first2=Mark |last3=Gal-Yam |first3=Avishay |last4=Barton |first4=Elizabeth J. |last5=Carlberg |first5=Raymond G. |last6=Ryan-Weber |first6=Emma V. |last7=Horst |first7=Chuck |last8=Omori |first8=Yuuki |last9=Díaz |first9=C. Gonzalo |year=2012 |doi=10.1038/nature11521 |pmid=23123848|arxiv = 1211.2003 |s2cid=4397580 }}</ref>
{{참고|en:List of most distant supernovae}}
|-
| [[Ia형 초신성]]
| [[SN UDS10Wil]]
|z = 1.914
|<ref>{{웹 인용 |url=http://www.spacetelescope.org/images/heic1306d/ |title=Record-breaking supernova in the CANDELS Ultra Deep Survey: before, after, and difference |work=www.spacetelescope.org |확인날짜=2021-10-11 |archive-date=2017-12-03 |archive-url=https://web.archive.org/web/20171203153849/http://www.spacetelescope.org/images/heic1306d/ |url-status= }}</ref>
{{참고|en:List of supernovae}}
|-
| [[Ia형 초신성]]<br/>......................
| [[SN SCP-0401]] <br /> ([[Mingus (supernova)|Mingus]])
| z = 1.71
| 2004년에 처음 관측되었지만, 2013년이 되어서야 Ia형 초신성으로 확인될 수 있었다.<ref>Science Newsline, [http://www.sciencenewsline.com/articles/2013010923190007.html "The Farthest Supernova Yet for Measuring Cosmic History"] {{Webarchive|url=https://web.archive.org/web/20130521070143/http://www.sciencenewsline.com/articles/2013010923190007.html |date=2013-05-21 }}, Lawrence Berkeley National Laboratory, 9 January 2013 (accessed 10 January 2013)</ref><ref>Space.com, [http://www.space.com/19198-most-distant-supernova-hubble-discovery-aas221.html "Most Distant 'Standard Candle' Star Explosion Found"], Mike Wall, 9 January 2013 (accessed 10 January 2013)</ref>
{{참고|en:List of supernovae}}
|-
| [[재결합|우주적<br/> 디커플링]]
| [[우주배경복사]]의 생성
| z~1000 to 1089
|<ref>{{저널 인용|journal=Astrophysical Journal Supplement |title=Five-Year Wilkinson Microwave Anisotropy Probe Observations: Data Processing, Sky Maps, and Basic Results |volume=180 |issue=2 |pages=225–245 |date=2009 |doi=10.1088/0067-0049/180/2/225 |bibcode=2009ApJS..180..225H |arxiv=0803.0732 |s2cid=3629998 |last1=Hinshaw |first1=G. |last2=Weiland |first2=J. L. |last3=Hill |first3=R. S. |last4=Odegard |first4=N. |last5=Larson |first5=D. |last6=Bennett |first6=C. L. |last7=Dunkley |first7=J. |last8=Gold |first8=B. |last9=Greason |first9=M. R. |last10=Jarosik |first10=N. |last11=Komatsu |first11=E. |last12=Nolta |first12=M. R. |last13=Page |first13=L. |last14=Spergel |first14=D. N. |last15=Wollack |first15=E. |last16=Halpern |first16=M. |last17=Kogut |first17=A. |last18=Limon |first18=M. |last19=Meyer |first19=S. S. |last20=Tucker |first20=G. S. |last21=Wright |first21=E. L. }}</ref><ref>[[Redshift]] states the [[Cosmic microwave background]] radiation as having a redshift of z = 1089</ref>
|-
|}

<!--{| class="wikitable"
|+유형별 최원거리 천체
! 유형
! 천체
! 적색편이
!주
|-
| 유형에 관계없이 모든 [[천체]]
| rowspan="2" | [[GN-z11]]
| rowspan="2" | z = 11.09
| rowspan="2" | 약 134억 광년의 광행거리 (그리고 [[공변거리|고유거리]]는 우리가 지금 관측하는 빛이 약 134억년 전에 출발한 이후에 우주의 팽창에 의하여 지구로부터 약 {{단위 변환|32|e9ly|e9pc}} 임)를 가지고 있어, 천문학자들은 2016년 3월 현재 알려진 천체 중 가장 먼 은하로 발표했다.<ref name="GN-z11">{{웹 인용|url=http://www.nationalgeographic.com/science/phenomena/2016/03/03/astronomers-spot-most-distant-galaxy-yet-at-least-for-now/|제목=Astronomers Spot Most Distant Galaxy—At Least For Now|성=Drake|이름=Nadia|날짜=March 3, 2016|출판사=[[National Geographic (magazine)|National Geographic]]|확인날짜=April 13, 2019}}</ref> {{참고태그|1광년이 1년 동안 빛이 이동하는 거리이고 빛의 속도보다 빠르게 이동할 수 있는 것은 없으므로 얼핏 보면 나이가 138억년에 불과한 우주에서 320억 광년이라는 거리는 불가능하게 먼 것으로 볼일 수 있다. 그러나 빛이 방출될 당시 GN-z11과 우리은하 사이의 거리인 26억 6천만 광년이 우주의 팽창으로 인해 (z+1)에 해당하는 12.1배 증가하여 빛이 우리에게 도달하는 134억 년 동안 322억 광년의 거리로 증가하였다. [[관측 가능한 우주의 크기]], [[관측 가능한 우주의 크기에 대한 오해]], [[팽창하는 공간에서의 거리 측정]] 및 [[고무줄 위의 개미]] 기사 참조}}{{참고|은하 목록}}
|-
|[[은하]] 또는 [[원시은하]]
|-
| [[은하단]]
| CL J1001+0220
| z≅2.506
| 2016년 현재<ref name="AJ-828-1">{{저널 인용|제목=Discovery of a galaxy cluster with a violently starbursting core at z=2.506|저널=The Astrophysical Journal|성=Wang|이름=Tao|성2=Elbaz|이름2=David|연도=2016|권=828|쪽=56|arxiv=1604.07404|bibcode=2016ApJ...828...56W|doi=10.3847/0004-637X/828/1/56|성3=Daddi|이름3=Emanuele|성4=Finoguenov|이름4=Alexis|성5=Liu|이름5=Daizhong|성6=Schrieber|이름6=Corenin|성7=Martin|이름7=Sergio|성8=Strazzullo|이름8=Veronica|성9=Valentino|이름9=Francesco}}</ref>{{참고|은하단 목록}}
|-
|[[초은하단|은하초은하단]]
| 코마 초은하단
|
|
|-
| [[퀘이사]]
| rowspan="2" | J0313-1806
| rowspan="2" | z = 7.64
|<ref name="AAAS2021"/>{{참고|퀘이사 목록}}
|-
|[[블랙홀]]
|<ref name="AAAS2021" />
|-
| [[항성|별]] 또는 [[원시별|원시성]] 또는 사후 항성 시체 <small>(이벤트에 의해 감지됨)</small>
| [[GRB 090423]]의 원형
| z = 8.2
|<ref name="NASA-2009-04-28"/><ref name="Tanvir2009"/> GRB 090429B는 측광 적색편이 z <sub>p</sub> ≅9.4,<ref name="SC-2011-05-27">Science Codex, [http://www.sciencecodex.com/nasas_swift_finds_most_distant_gammaray_burst_yet "GRB 090429B – most distant gamma-ray burst yet"] {{웹아카이브|url=https://web.archive.org/web/20110531000312/http://www.sciencecodex.com/nasas_swift_finds_most_distant_gammaray_burst_yet}}, ''NASA/Goddard'', 27 May 2011</ref>를 가지므로 GRB 090423보다 더 멀리 떨어져 있을 가능성이 높지만 분광학적 확인이 부족하다.{{참고|감마선 버스트 목록}}추정거리는 지구에서 약 130억 광년
|-
| [[항성|별]] 또는 [[원시별|원시성]] 또는 사후 항성 시체<br /><small>(별으로 감지)</small>
| SDSS J1229+1122
| {{단위 변환|55|Mly|Mpc}}
| 이 청색의 추거성은 은하 IC 3418 의 조석 꼬리에 있는 성운을 비추고 있다.<ref>Sky and Telescope, [http://www.skyandtelescope.com/astronomy-news/the-most-distant-star-everseen/ "The Most Distant Star Ever Seen?"], '''Camille M. Carlisle''', ''12 April 2013''</ref> 이 기록은 은하단 MACS J1149.5+2223에 의하여 렌즈 현상이 되고 있는 적색편이 z=1.5(4.4Gpc)의 별에 의하여 갱신되었다.<ref>Paper, [http://adsabs.harvard.edu/abs/2017arXiv170610279K "An individual star at redshift 1.5 extremely magnified by a galaxy-cluster lens"], '''P. Kelly, J.M. Diego et al''', ''June 2017''</ref>
|-
| [[항성|별]]
| WHL0137-LS(Earendel)
| z = 6.2<br /> 27.8 [[기가|Gly]]
| 가장 멀리 있는 개별의 [[항성|별]]이 발견됨(2022년 3월 30일)<ref name="NA-20180402">{{저널 인용|제목=Extreme magnification of an individual star at redshift 1.5 by a galaxy-cluster lens|저널=[[Nature (journal)|Nature]]|성=Kelly, Patrick L.|날짜=2 April 2018|권=2|호=4|쪽=334–342|arxiv=1706.10279|bibcode=2018NatAs...2..334K|doi=10.1038/s41550-018-0430-3|저자표시=etal}}</ref><ref name="SPC-20180402">{{웹 인용|url=https://www.space.com/40171-cosmic-alignment-reveals-most-distant-star-yet.html|제목=Rare Cosmic Alignment Reveals Most Distant Star Ever Seen|성=Howell|이름=Elizabeth|날짜=2 April 2018|웹사이트=[[Space.com]]|확인날짜=2 April 2018}}</ref><ref name="BN-20180402">{{뉴스 인용|url=http://news.berkeley.edu/2018/04/02/cosmic-lens-helps-hubble-capture-most-distant-star-ever-seen/|제목=Hubble peers through cosmic lens to capture most distant star ever seen|성=Sanders|이름=Robert|날짜=2 April 2018|뉴스=[[University of California, Berkeley|Berkeley News]]|확인날짜=2 April 2018}}</ref><ref name="AM-20180402">{{웹 인용|url=http://www.astronomy.com/news/2018/04/hubble-images-farthest-star-ever-seen|제목=Hubble spots farthest star ever seen|성=Parks|이름=Jake|날짜=2 April 2018|웹사이트=[[Astronomy (magazine)|Astronomy]]|확인날짜=2 April 2018}}</ref>
|-
| [[성단]]
|
|
|
|-
| 성단의 체계
|  [[NGC 6397]] 뒤 [[타원은하|타원 은하]] 내의 [[구상성단|구상 성단]] 시스템
| 1.2 Gly
|<ref>New Scientist, [https://www.newscientist.com/article/dn14283-lucky-hubble-find-raises-star-cluster-mystery.html "Lucky Hubble find raises star cluster mystery"], Rachel Courtland, 8 July 2008 (accessed 18 December 2012)</ref><ref>Astronomy Magazine, [http://www.astronomy.com/News-Observing/News/2007/01/A%20star%20cluster%20hides%20star%20clusters.aspx "A star cluster hides star clusters"] {{웨이백|url=http://www.astronomy.com/News-Observing/News/2007/01/A%20star%20cluster%20hides%20star%20clusters.aspx |date=20170416125902 }}, Francis Reddy, 10 January 2007 (accessed 18 December 2012)</ref><ref>Space.com, [http://www.space.com/3341-faraway-galaxy-plays-peekaboo.html "Faraway Galaxy Plays Peekaboo"], Ker Than, 10 January 2007 (accessed 18 December 2012)</ref><ref>ScienceDaily, [https://www.sciencedaily.com/releases/2007/01/070110181358.htm "Astronomers Find The Most Distant Star Clusters Hidden Behind A Nearby Cluster"], 14 January 2007 (accessed 18 December 2012)</ref><ref>Kalirai, Jason S.; Richer, H.; Anderson, J.; Strader, J.; Forde, K.; "Globular Clusters in a Globular Cluster", 2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #228.02; Bulletin of the American Astronomical Society, Vol. 38, p.1214, December 2006; {{Bibcode|2006AAS...20922802K}}</ref>
|-
| 엑스레이 제트
| PJ352–15 퀘이사 제트
| z = 5.831<br />12.7 [[광년|Gly]]<ref>https://arxiv.org/abs/2103.03879</ref>
| 이전 기록 보유자는 12.4Gly에 있었다.<ref>[https://www.nasa.gov/mission_pages/chandra/images/gigantic-jet-spied-from-black-hole-in-early-universe.html NASA.gov]</ref><ref name="SpaceDaily-2012-11-30">SpaceDaily, [http://www.spacedaily.com/reports/Record_Setting_X_ray_Jet_Discovered_999.html "Record-Setting X-ray Jet Discovered"], 30 November 2012 (accessed 4 December 2012)</ref>
|-
| 마이크로퀘이사
| XMMU J004243.6+412519
| 2.5Mly
| 최초로 발견된은하외 마이크로퀘이사<ref>ESA, [http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=51225 "Artist's impression of the X-ray binary XMMU J004243.6+412519"], 12 December 2012 (accessed 18 December 2012)</ref><ref>e! Science News, [http://esciencenews.com/sources/scientific.blogging/2012/12/12/xmmu.j004243.6412519.black.hole.binary.at.the.eddington.limit "XMMU J004243.6+412519: Black-Hole Binary At The Eddington Limit"], 12 December 2012 (accessed 18 December 2012)</ref><ref>SpaceDaily, [http://www.spacedaily.com/reports/Microquasar_found_in_neighbor_galaxy_tantalizing_scientists_999.html "Microquasar found in neighbor galaxy, tantalizing scientists"], 17 December 2012 (accessed 18 December 2012)</ref>
|-
| [[행성]]
| [[SWEEPS-11]] / [[SWEEPS-04]]
| 27,710 ly
|<ref name="USA-2006-01-25">USA Today, [https://www.usatoday.com/tech/science/space/2006-01-25-exoplanet-discovery_x.htm "Smallest, most distant planet outside solar system found"], '''Malcolm Ritter''', ''25 January 2006'' (accessed 5 August 2010)</ref>

* 미세렌즈 현상 PA-99-N2의 광곡선을 분석한 결과 [[안드로메다 은하]]<ref>{{백과사전 인용|url=http://exoplanet.eu/star.php?st=PA-99-N2 |title=Notes for star PA-99-N2 |encyclopedia=The Extrasolar Planets Encyclopaedia |author=Schneider, J. |access-date=2010-08-06}}</ref>에 있는 별 주위를 도는 행성이 존재함을 알 수 있다.
* 이중 중력렌즈 현상에 의한 [[이중준성|Q0957+561]]의 엽 A에서 논란이 되고 있는 미세 렌즈 현상은 렌즈 은하내에 적색편이 0.355(3.7 Gly)에 있는 행성이 있음을 시사한다.<ref>Exoplaneten.de, [http://www.exoplaneten.de/Q0957+561/english.html "The Microlensing Event of Q0957+561"] {{웹아카이브|url=https://web.archive.org/web/20120211130721/http://www.exoplaneten.de/Q0957+561/english.html}} (accessed 5 August 2010)</ref><ref>{{저널 인용|제목=Microlensing Variability of the Gravitationally Lensed Quasar Q0957+561 A,B|저널=Astrophysical Journal|성=Schild|이름=R.E.|연도=1996|권=464|쪽=125|bibcode=1996ApJ...464..125S|doi=10.1086/177304}}</ref>
|-
|}
{| class="wikitable"
|+유형별 원거리 사건
! 유형
! 사건
! 적색편이
! 주
|-
| [[감마선 폭발|감마선 버스트]]
| [[GRB 090423]]
| z = 8.2
|<ref name="NASA-2009-04-28">NASA, [https://science.nasa.gov/science-news/science-at-nasa/2009/28apr_grbsmash/ "New Gamma-Ray Burst Smashes Cosmic Distance Record"] {{웨이백|url=https://science.nasa.gov/science-news/science-at-nasa/2009/28apr_grbsmash/ |date=20110310193130 }}, 28 April 2009</ref><ref name="Tanvir2009"/> GRB 090429B는 측광학적 적색편이 z <sub>p</sub> ≅9.4를 가지고 있으므로,<ref name="SC-2011-05-27"/> GRB 090423보다 더 멀리 떨어져 있을 가능성이 높지만 분광학적 확인이 부족하다.{{참고|감마선 버스트 목록}}
|-
|[[초신성|핵붕괴 초신성]]
| SN 1000+0216
| z = 3.8993
|<ref>{{저널 인용|제목=Superluminous supernovae at redshifts of 2.05 and 3.90|저널=Nature|성=Cooke|이름=Jeff|성2=Sullivan|이름2=Mark|연도=2012|권=491|호=7423|쪽=228–31|arxiv=1211.2003|bibcode=2012Natur.491..228C|doi=10.1038/nature11521|pmid=23123848|성3=Gal-Yam|이름3=Avishay|성4=Barton|이름4=Elizabeth J.|성5=Carlberg|이름5=Raymond G.|성6=Ryan-Weber|이름6=Emma V.|성7=Horst|이름7=Chuck|성8=Omori|이름8=Yuuki|성9=Díaz|이름9=C. Gonzalo}}</ref>{{참고|최원거리 초신성 목록}}
|-
|[[Ia형 초신성]]
| SN UDS10Wil
| z = 1.914
|<ref>{{웹 인용|url=http://www.spacetelescope.org/images/heic1306d/|제목=Record-breaking supernova in the CANDELS Ultra Deep Survey: before, after, and difference|성=information@eso.org|웹사이트=www.spacetelescope.org}}</ref>{{참고|초신성 목록}}
|-
|[[Ia형 초신성]]
| SN SCP-0401<br />( 밍구스 )
| z = 1.71
| 2004년에 처음 관측되었으며 2013년이 되어서야 Ia형 초신성으로 식별될 수 있었다.<ref>Science Newsline, [http://www.sciencenewsline.com/articles/2013010923190007.html "The Farthest Supernova Yet for Measuring Cosmic History"] {{웹아카이브|url=https://web.archive.org/web/20130521070143/http://www.sciencenewsline.com/articles/2013010923190007.html}}, Lawrence Berkeley National Laboratory, 9 January 2013 (accessed 10 January 2013)</ref><ref>Space.com, [http://www.space.com/19198-most-distant-supernova-hubble-discovery-aas221.html "Most Distant 'Standard Candle' Star Explosion Found"], Mike Wall, 9 January 2013 (accessed 10 January 2013)</ref>{{참고|초신성 목록}}
|-
|[[재결합|우주적 분리]]
| 우주 배경 방사선 생성
| z~1000 ~ 1089
|<ref>{{저널 인용|제목=Five-Year Wilkinson Microwave Anisotropy Probe Observations: Data Processing, Sky Maps, and Basic Results|저널=Astrophysical Journal Supplement|저자=Hinshaw, G.|저자2=Weiland, J. L.|저자3=Hill, R. S.|저자4=Odegard, N.|저자5=Larson, D.|저자6=Bennett, C. L.|저자7=Dunkley, J.|저자8=Gold, B.|저자9=Greason, M. R.|저자10=Jarosik, N.|저자11=Komatsu, E.|저자12=Nolta, M. R.|저자13=Page, L.|저자14=Spergel, D. N.|저자15=Wollack, E.|저자16=Halpern, M.|저자17=Kogut, A.|저자18=Limon, M.|저자19=Meyer, S. S.|저자20=Tucker, G. S.|저자21=Wright, E. L.|날짜=2009|권=180|호=2|쪽=225–245|arxiv=0803.0732|bibcode=2009ApJS..180..225H|doi=10.1088/0067-0049/180/2/225}}</ref><ref>[[Redshift]] states the [[Cosmic microwave background]] radiation as having a redshift of z = 1089</ref>
|-
|}
-->

== 최원거리 천체 기록 보유자의 연대표 ==
이 목록의 천체는 거리를 결정하였을 때 가장 멀리 있는 천체로 확인되었다. 이것은 종종 천체의 발견 날짜와 동일하지 않다.

천체까지의 거리는 [[시차 (천문학)|시차]] 측정, [[세페이드 변광성]] 또는 [[Ia형 초신성]]과 같은 [[우주 거리 사다리|표준 참조의]] 사용 또는 [[적색편이]] 측정을 통해 결정할 수 있다. 분광학적 적색편이 측정이 선호되는 반면, 측광학적 적색편이 측정도 높은 적색편이 광원의 후보를 식별하기 위하여는 사용된다. 기호 ''z'' 는 적색편이를 나타낸다.
{| class="wikitable"
|+최원거리 천체 기록 보유자 (측광학적 적색편이에 기초한 후보 제외)
!천체
!유형
!일자
!거리<br /> <small> (z = [[적색편이]]) </small>
!주
|-
| [[JADES-GS-z13-0]]
| 은하
| 2022 - 현재
| z = 13.20
|<ref name="Robertson2022" />
|-
|[[GN-z11]]
|은하
|2016&nbsp;−&nbsp;2022
|z = 11.09
|<ref name="BBC-2016-03-03">{{웹 인용|url=https://www.bbc.com/news/science-environment-35721734|제목=Hubble sets new cosmic distance record|성=Jonathan Amos|날짜=3 March 2016|출판사=BBC News}}</ref>
|-
|EGSY8p7
| 은하
|2015&nbsp;−&nbsp;2016
|z = 8.68
|<ref name="BBC-2016-03-03" /><ref name="Space.com-2015-08-05">{{뉴스 인용|url=http://www.space.com/30170-most-distant-galaxy-discovered.html|제목=Ancient Galaxy Is Most Distant Ever Found|성=Mike Wall|날짜=5 August 2015|출판사=Space.com}}</ref><ref name="AstronomyNow-2015-08-06">{{뉴스 인용|url=http://astronomynow.com/2015/08/06/a-new-record-keck-observatory-measures-most-distant-galaxy/|제목=A new record: Keck Observatory measures most distant galaxy|성=W. M. Keck Observatory|날짜=6 August 2015|출판사=Astronomy Now}}</ref><ref name="HuffPost-2015-07-15">{{뉴스 인용|url=http://www.huffingtonpost.com/mario-de-leo-winkler/the-farthest-object-in-th_b_7795982.html|제목=The Farthest Object in the Universe|성=Mario De Leo Winkler|날짜=15 July 2015|출판사=Huffington Post}}</ref>
|-
|Progenitor of [[GRB 090423]] / Remnant of [[GRB 090423]]
|감마선 폭발<br/> 조상<br/>/ [[감마선 폭발|감마선 폭발 잔해]]
|2009&nbsp;−&nbsp;2015
|z = 8.2
|<ref name="Tanvir2009"/><ref name=NS-2009-04-27>''[[New Scientist]]'', [https://www.newscientist.com/article/dn17035-most-distant-object-in-the-universe-spotted.html "Most distant object in the universe spotted"], ''Rachel Courtland'', 22:32 27 April 2009 . Retrieved 2009-11-11.</ref>
|-
|[[IOK-1]]
|[[은하]]
|2006&nbsp;−&nbsp;2009
|z = 6.96
|<ref name="NS-2009-04-27" /><ref>''New Scientist'', [https://www.newscientist.com/article/dn10069-first-generation-of-galaxies-glimpsed-forming.html "First generation of galaxies glimpsed forming"], 'David Shiga ', 19:01 13 September 2006 (accessed 2009/11/11)</ref><ref>{{저널 인용|doi=10.1038/nature05104 |pmid=16971942 |year=2006 |last1=Iye |first1=M |title=A galaxy at a redshift z = 6.96 |journal=Nature |volume=443 |issue=7108 |pages=186–8 |last2=Ota |first2=K |last3=Kashikawa |first3=N |last4=Furusawa |first4=H |last5=Hashimoto |first5=T |last6=Hattori |first6=T |last7=Matsuda |first7=Y |last8=Morokuma |first8=T |last9=Ouchi |first9=M |last10=Shimasaku |first10=K |bibcode=2006Natur.443..186I|arxiv = astro-ph/0609393 |s2cid=2876103 }}</ref><ref name="z.gt.5">{{저널 인용|제목=Star Forming Galaxies at z > 5|저널=Proceedings of the International Astronomical Union|성=Taniguchi|이름=Yoshi|날짜=23 June 2008|권=3|호=S250|쪽=429–436|arxiv=0804.0644|bibcode=2008IAUS..250..429T|doi=10.1017/S1743921308020796}}</ref>
|-
|SDF J132522.3+273520
| 은하
|2005&nbsp;−&nbsp;2006
|z = 6.597
|<ref name="z.gt.5" /><ref name="SDFz6.6">{{저널 인용|제목=The SUBARU Deep Field Project: Lymanα Emitters at a Redshift of 6.6|저널=Publications of the Astronomical Society of Japan|성=Taniguchi|이름=Yoshiaki|성2=Ajiki|이름2=Masaru|url=http://pasj.asj.or.jp/v57/n1/570114/57012649.pdf|연도=2005|권=57|쪽=165–182|arxiv=astro-ph/0407542|bibcode=2005PASJ...57..165T|doi=10.1093/pasj/57.1.165|성3=Nagao|이름3=Tohru|성4=Shioya|이름4=Yasuhiro|성5=Murayama|이름5=Takashi|성6=Kashikawa|이름6=Nobunari|성7=Kodaira|이름7=Keiichi|성8=Kaifu|이름8=Norio|성9=Ando|이름9=Hiroyasu}}</ref>
|-
|SDF J132418.3+271455
| 은하
|2003&nbsp;−&nbsp;2005
|z = 6.578
|<ref name="SDFz6.6" /><ref name=BBC-2003-03-25>BBC News, [http://news.bbc.co.uk/2/hi/science/nature/2884411.stm Most distant galaxy detected], Tuesday, 25 March 2003, 14:28 GMT</ref><ref name=SpaceRef-2003-03-24>SpaceRef, [http://www.spaceref.com/news/viewpr.html?pid=11046 Subaru Telescope Detects the Most Distant Galaxy Yet and Expects Many More] {{웹아카이브|url=https://archive.today/20121209015117/http://www.spaceref.com/news/viewpr.html?pid=11046 |날짜=2012-12-09 }}, Monday, March 24, 2003</ref><ref>{{저널 인용|arxiv=astro-ph/0301096 |last1=Kodaira |first1=K. |title=The Discovery of Two Lyman$α$ Emitters Beyond Redshift 6 in the Subaru Deep Field |journal=Publications of the Astronomical Society of Japan |volume=55 |issue=2 |pages=L17 |last2=Taniguchi |first2=Y. |last3=Kashikawa |first3=N. |last4=Kaifu |first4=N. |last5=Ando |first5=H. |last6=Karoji |first6=H. |last7=Ajiki |first7=Masaru |last8=Akiyama |first8=Masayuki |last9=Aoki |first9=Kentaro |last10=Doi |first10=Mamoru |last11=Fujita |first11=Shinobu S. |last12=Furusawa |first12=Hisanori |last13=Hayashino |first13=Tomoki |last14=Imanishi |first14=Masatoshi |last15=Iwamuro |first15=Fumihide |last16=Iye |first16=Masanori |last17=Kawabata |first17=Koji S. |last18=Kobayashi |first18=Naoto |last19=Kodama |first19=Tadayuki |last20=Komiyama |first20=Yutaka |last21=Kosugi |first21=George |last22=Matsuda |first22=Yuichi |last23=Miyazaki |first23=Satoshi |last24=Mizumoto |first24=Yoshihiko |last25=Motohara |first25=Kentaro |last26=Murayama |first26=Takashi |last27=Nagao |first27=Tohru |last28=Nariai |first28=Kyoji |last29=Ohta |first29=Kouji |last30=Ohyama |first30=Youichi |year=2003 |doi=10.1093/pasj/55.2.L17 |bibcode = 2003PASJ...55L..17K }}</ref>
|-
|HCM-6A
|은하
|2002&nbsp;−&nbsp;2003
|z = 6.56
|이 은하는 은하단 Abell 370에 의해 렌즈화되었다. 이것은 적색편이 6을 초과하는 것으로 발견된 최초의 비퀘이사 은하이다. 이것은 퀘이사 SDSSp J103027.10+052455.0의 적색편이 z = 6.28을 초과하였다.<ref name="BBC-2003-03-25" /><ref name="SpaceRef-2003-03-24" /><ref>''New Scientist,'' [https://www.newscientist.com/article/dn2046-new-record-for-universes-most-distant-object.html New record for Universe's most distant object], 17:19 14 March 2002</ref><ref>BBC News, [http://news.bbc.co.uk/2/hi/science/nature/1871043.stm Far away stars light early cosmos], Thursday, 14 March 2002, 11:38 GMT</ref><ref>{{저널 인용| doi = 10.1086/340424 | volume=568 | title=A Redshift [CLC][ITAL]z[/ITAL][/CLC] = 6.56 Galaxy behind the Cluster Abell 370 | year=2002 | journal=The Astrophysical Journal | pages=L75–L79 | last1 = Hu | first1 = E. M. | issue=2 | arxiv=astro-ph/0203091 | bibcode=2002ApJ...568L..75H| doi-access=free }}</ref><ref>{{웹 인용|url=http://hera.ph1.uni-koeln.de/~heintzma/U/Lens.htm |title=K2.1 HCM 6A&nbsp;— Discovery of a redshift z = 6.56 galaxy lying behind the cluster Abell 370 |publisher=Hera.ph1.uni-koeln.de |date=2008-04-14 |access-date=2010-10-22 |url-status=dead |archive-url=https://web.archive.org/web/20110518140741/http://hera.ph1.uni-koeln.de/~heintzma/U/Lens.htm |archive-date=2011-05-18 }}</ref>
|-
|SDSS J1030+0524 (SDSSp J103027.10+052455.0)
|[[퀘이사]]
|2001&nbsp;−&nbsp;2002
|z = 6.28
|<ref name="VLT z = 6.28">{{저널 인용|arxiv=astro-ph/0112075 |last1=Pentericci |first1=L. |title=VLT observations of the z = 6.28 quasar SDSS 1030+0524 |journal=The Astronomical Journal |volume=123 |issue=5 |pages=2151 |last2=Fan |first2=X. |last3=Rix |first3=H. W. |last4=Strauss |first4=M. A. |last5=Narayanan |first5=V. K. |last6=Richards |first6=G T. |last7=Schneider |first7=D. P. |last8=Krolik |first8=J. |last9=Heckman |first9=T. |last10=Brinkmann |first10=J. |last11=Lamb |first11=D. Q. |last12=Szokoly |first12=G. P. |year=2002 |doi=10.1086/340077 |bibcode=2002AJ....123.2151P}}</ref><ref name="SDSS1030+0524">''[[The Astrophysical Journal]]'', 578:702–707, 20 October 2002, A Constraint on the Gravitational Lensing Magnification and Age of the Redshift z = 6.28 Quasar SDSS 1030+0524</ref><ref name="REIONz.gt.6">{{저널 인용|doi=10.1086/375547 |title=Probing the Ionization State of the Universe atz>6 |journal=The Astronomical Journal |volume=126 |issue=1 |pages=1–14 |year=2003 |last1=White |first1=Richard L. |last2=Becker |first2=Robert H. |last3=Fan |first3=Xiaohui |last4=Strauss |first4=Michael A. |bibcode=2003AJ....126....1W|arxiv = astro-ph/0303476 |s2cid=51505828 }}</ref><ref name="Xray z = 6.30">{{저널 인용|bibcode=2004ApJ...611L..13F |doi=10.1086/423669 |title=The X-Ray Spectrum of the z = 6.30 QSO SDSS J1030+0524 |journal=The Astrophysical Journal |volume=611 |issue=1 |pages=L13–L16 |year=2004 |last1=Farrah |first1=D. |last2=Priddey |first2=R. |last3=Wilman |first3=R. |last4=Haehnelt |first4=M. |last5=McMahon |first5=R.|arxiv = astro-ph/0406561 |s2cid=14854831 }}</ref><ref name=PSU2001 /><ref name=SDSS2001 />
|-
|SDSS 1044-0125 J104433.04-012502.2)
|퀘이사
|2000&nbsp;−&nbsp;2001
|z = 5.82
|<ref name=Summer2000>PennState – Eberly College of Science – Science Journal – Summer 2000 – Vol. 17, No. 1 [http://www.science.psu.edu/journal/Sum2000/DistObj.htm International Team of Astronomers Finds Most Distant Object] {{Webarchive|url=https://web.archive.org/web/20090912024541/http://www.science.psu.edu/journal/Sum2000/DistObj.htm |date=2009-09-12 }}</ref><ref name="z = 5.74">The Astrophysical Journal Letters, 522:L9–L12, 1999 September 1, An Extremely Luminous Galaxy at z = 5.74</ref><ref name=PSU2001>PennState Eberly College of Science, [http://www.science.psu.edu/alert/Schneider6-2001.htm Discovery Announced of Two Most Distant Objects] {{webarchive|url=https://web.archive.org/web/20071121093952/http://www.science.psu.edu/alert/Schneider6-2001.htm |date=2007-11-21 }}, June 2001</ref><ref name=SDSS2001>SDSS, [http://www.sdss.org/news/releases/20010605.edr.html Early results from the Sloan Digital Sky Survey: From under our nose to the edge of the universe], June 2001</ref><ref>PennState Eberly College of Science, [http://www.science.psu.edu/alert/Brandt12-2000.htm X-rays from the Most Distant Quasar Captured with the XMM-Newton Satellite] {{webarchive|url=https://web.archive.org/web/20071121231510/http://www.science.psu.edu/alert/Brandt12-2000.htm |date=2007-11-21 }}, Dec 2000</ref><ref name=10Feb2005>UW-Madison Astronomy, [http://www.astro.wisc.edu/~stanway/research/highzobj.html Confirmed High Redshift (z > 5.5) Galaxies – (Last Updated 10th February 2005)] {{webarchive|url=https://web.archive.org/web/20070618233852/http://www.astro.wisc.edu/~stanway/research/highzobj.html |date=2007-06-18 }}</ref><ref>SPACE.com, [http://www.space.com/scienceastronomy/astronomy/distant_object_001201.html Most Distant Object in Universe Comes Closer], 01 December 2000</ref>
|-
|SSA22-HCM1
|은하
|1999&nbsp;−&nbsp;2000
|z>=5.74
|<ref>''The Astrophysical Journal Letters'', 522:L9–L12, September 1, 1999, An Extremely Luminous Galaxy at z = 5.74</ref><ref name="Stern04Sept" />
|-
|HDF 4-473.0
|은하
|1998&nbsp;−&nbsp;1999
|z = 5.60
|<ref name=Stern04Sept>''[[Publications of the Astronomical Society of the Pacific]]'', 111: 1475–1502, 1999 December; Search Techniques for Distant Galaxies; [http://nedwww.ipac.caltech.edu/level5/Sept04/Stern/Stern1.html Introduction]</ref>
|-
|RD1 (0140+326 RD1)
|은하
|1998
|z = 5.34
|<ref name=NYT-1998-10-20>''New York Times,'' [https://query.nytimes.com/gst/fullpage.html?res=9B0DEFDD123DF933A15753C1A96E958260&sec=&spon=&pagewanted=3 Peering Back in Time, Astronomers Glimpse Galaxies Aborning], October 20, 1998</ref><ref name=APOD-1998-03-24>Astronomy Picture of the Day, [http://apod.nasa.gov/apod/ap980324.html A Baby Galaxy], March 24, 1998</ref><ref name="z = 5.34">{{저널 인용|제목=A Galaxy at z = 5.34|저널=The Astrophysical Journal|성=Dey|이름=Arjun|성2=Spinrad|이름2=Hyron|연도=1998|권=498|호=2|쪽=L93|arxiv=astro-ph/9803137|bibcode=1998ApJ...498L..93D|doi=10.1086/311331|성3=Stern|이름3=Daniel|성4=Graham|이름4=James R.|성5=Chaffee|이름5=Frederic H.}}</ref><ref name="Stern04Sept" /><ref name="UCLA">{{웹 인용|url=http://www.astro.ucla.edu/~wright/old_new_cosmo.html#12Mar98|제목=A New Most Distant Object: z = 5.34|출판사=Astro.ucla.edu|확인날짜=2010-10-22}}</ref>
|-
|CL 1358+62 G1 & CL 1358+62 G2
|은하
|1997&nbsp;−&nbsp;1998
|z = 4.92
|이들은 발견 당시 가장 멀리 떨어진 천체였다. 이 한 쌍의 은하는 은하단 CL1358+62(z = 0.33)에 의한 렌즈 현상에 의한 것으로 밝혀졌다. 우주에서 가장 멀리 떨어진 천체의 기록을 [[퀘이사]]가 아닌 천체가 세운 것은 1964년 이후 처음이었다.<ref name=APOD-1998-03-24 /><ref>Astronomy Picture of the Day, [http://apod.nasa.gov/apod/ap970731.html Behind CL1358+62: A New Farthest Object], July 31, 1997</ref><ref>{{저널 인용|bibcode=1997ApJ...486L..75F |doi=10.1086/310844 |title=A Pair of Lensed Galaxies at [CLC][ITAL]z[/ITAL][/CLC]=4.92 in the Field of CL 1358+62 |journal=The Astrophysical Journal |volume=486 |issue=2 |pages=L75 |year=1997 |last1=Franx |first1=Marijn |last2=Illingworth |first2=Garth D. |last3=Kelson |first3=Daniel D. |last4=Van Dokkum |first4=Pieter G. |last5=Tran |first5=Kim-Vy|arxiv = astro-ph/9704090 |s2cid=14502310 }}</ref><ref name="z = 5.34" /><ref name=Stern04Sept /><ref name=Illingworth>{{저널 인용| doi = 10.1023/a:1017052809781 | url = http://nedwww.ipac.caltech.edu/level5/Illingworth/Ill8.html | bibcode=1999Ap&SS.269..165I | volume=269/270 | year=1999 | journal=Astrophysics and Space Science | pages=165–181  | last1 = Illingworth | first1 = Garth | title = Galaxies at High Redshift | arxiv = astro-ph/0009187 | s2cid = 119363931 }}</ref>
|-
|PC 1247-3406
|퀘이사
|1991&nbsp;−&nbsp;1997
|z = 4.897
|<ref name="Summer2000" /><ref>{{저널 인용|제목=Multicolor detection of high-redshift quasars, 2: Five objects with Z greater than or approximately equal to 4|저널=The Astronomical Journal|성=Smith|이름=J. D.|성2=Djorgovski|이름2=S.|연도=1994|권=108|쪽=1147|bibcode=1994AJ....108.1147S|doi=10.1086/117143|성3=Thompson|이름3=D.|성4=Brisken|이름4=W. F.|성5=Neugebauer|이름5=G.|성6=Matthews|이름6=K.|성7=Meylan|이름7=G.|성8=Piotto|이름8=G.|성9=Suntzeff|이름9=N. B.}}</ref><ref>''New Scientist,'' issue 1842, 10 October 1992, page 17, [https://www.newscientist.com/article/mg13618423.200-science-infant-galaxys-light-show-.html Science: Infant galaxy's light show]</ref><ref>FermiLab [http://www.princeton.edu/pr/news/98/q4/1208-skysur.htm Scientists of Sloan Digital Sky Survey Discover Most Distant Quasar] {{웹아카이브|url=https://web.archive.org/web/20090912194951/http://www.princeton.edu/pr/news/98/q4/1208-skysur.htm}} December 8, 1998</ref><ref name="472QSR401">{{저널 인용|제목=Discovery of radio-loud quasars with z = 4.72 and z = 4.01|저널=Monthly Notices of the Royal Astronomical Society|성=Hook|이름=Isobel M.|성2=McMahon|이름2=Richard G.|연도=1998|권=294|호=1|쪽=L7–L12|arxiv=astro-ph/9801026|bibcode=1998MNRAS.294L...7H|doi=10.1046/j.1365-8711.1998.01368.x}}</ref>
|-
|PC 1158+4635
|퀘이사
|1989&nbsp;−&nbsp;1991
|z = 4.73
|<ref name=Summer2000 /><ref name=472QSR401 /><ref name="z.gt.4">{{저널 인용|bibcode=1991AJ....101....5T |title=Quasars and galaxy formation. I – the Z greater than 4 objects |journal=Astronomical Journal |volume=101 |pages=5 |last1=Turner |first1=Edwin L. |year=1991 |doi=10.1086/115663}}</ref><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=PC+1158%2B4635 Object query : PC 1158+4635], QSO B1158+4635 -- Quasar</ref><ref>{{저널 인용|doi=10.1111/j.1749-6632.1991.tb32157.x |title=Young Galaxies |journal=Annals of the New York Academy of Sciences |volume=647 |issue=1 Texas/ESO–Cer |pages=31–41 |year=1991 |last1=Cowie |first1=Lennox L. |bibcode=1991NYASA.647...31C|s2cid=222074763 }}</ref><ref name=20NOV1989>''New York Times,'' [https://query.nytimes.com/gst/fullpage.html?res=950DE0DB153AF933A15752C1A96F948260&scp=11&sq=most+distant+quasar&st=nyt Peering to Edge of Time, Scientists Are Astonished], November 20, 1989</ref>
|-
|Q0051-279
|퀘이사
|1987&nbsp;−&nbsp;1989
|z = 4.43
|<ref name="z = 4.43">{{저널 인용|bibcode=1987Natur.330..453W |doi=10.1038/330453a0 |title=Quasars of redshift z = 4.43 and z = 4.07 in the South Galactic Pole field |journal=Nature |volume=330 |issue=6147 |pages=453 |year=1987 |last1=Warren |first1=S. J. |last2=Hewett |first2=P. C. |last3=Osmer |first3=P. S. |last4=Irwin |first4=M. J.|s2cid=4352819 }}</ref><ref name="z.gt.4" /><ref name=20NOV1989 /><ref>{{저널 인용|bibcode=1988Ap.....29..657L |doi=10.1007/BF01005972 |title=Absorption spectra of quasars |journal=Astrophysics |volume=29 |issue=2 |pages=657–671 |year=1989 |last1=Levshakov |first1=S. A.|s2cid=122978350 }}</ref><ref>''[[New York Times]],'' [https://query.nytimes.com/gst/fullpage.html?res=940DE3DF143CF937A25752C0A96E948260&sec=&spon=&pagewanted=all Objects Detected in Universe May Be the Most Distant Ever Sighted], January 14, 1988</ref><ref>''New York Times,'' [https://query.nytimes.com/gst/fullpage.html?res=940DE7D8113CF933A25756C0A96E948260&sec=&spon=&pagewanted=all Astronomers Peer Deeper Into Cosmos], May 10, 1988</ref>
|-
|Q0000-26 <br /><br /> (QSO B0000-26)
|퀘이사
|1987
|z = 4.11
|<ref name="z = 4.43" /><ref name="z.gt.4" /><ref>[[SIMBAD]], [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Q0000-26 Object query : Q0000-26], QSO B0000-26 – Quasar</ref>
|-
|PC 0910+5625 <br /><br /> (QSO B0910+5625)
|퀘이사
|1987
|z = 4.04
|이것은 4 이상의 적색편이를 가진 것으로 밝혀진 두번째 퀘이사이다.<ref name="Summer2000" /><ref name="z.gt.4" /><ref name="PC0910+5625">{{저널 인용|제목=PC 0910 + 5625 – an optically selected quasar with a redshift of 4.04|저널=Astrophysical Journal|성=Schmidt|이름=Maarten|성2=Schneider|이름2=Donald P.|연도=1987|권=321|쪽=L7|bibcode=1987ApJ...321L...7S|doi=10.1086/184996|성3=Gunn|이름3=James E.}}</ref><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=PC+0910%2B5625&submit=SIMBAD+search Object query : PC 0910+5625], QSO B0910+5625 -- Quasar</ref>
|-
|Q0046–293 <br /><br /> (QSO J0048-2903)
|퀘이사
|1987
|z = 4.01
|<ref name="z = 4.43" /><ref name="z.gt.4" /><ref name="PC0910+5625" /><ref>{{저널 인용|제목=First observation of a quasar with a redshift of 4|저널=Nature|성=Warren|이름=S. J.|성2=Hewett|이름2=P. C.|연도=1987|권=325|호=6100|쪽=131|bibcode=1987Natur.325..131W|doi=10.1038/325131a0|성3=Irwin|이름3=M. J.|성4=McMahon|이름4=R. G.|성5=Bridgeland|이름5=M. T.|성6=Bunclark|이름6=P. S.|성7=Kibblewhite|이름7=E. J.}}</ref><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Q0046-293 Object query : Q0046-293], QSO J0048-2903 -- Quasar</ref>
|-
|Q1208+1011 <br /><br /> (QSO B1208+1011)
|퀘이사
|1986&nbsp;−&nbsp;1987
|z = 3.80
|이것은 중력 렌즈화된 이중 이미지 퀘이사로 발견 당시부터 1991년까지 이미지 사이 각도 간격으로 최소값인 0.45 초를 보유하고 있었다.<ref name="PC0910+5625" /><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Q1208%2B1011 Object query : Q1208+1011], QSO B1208+1011 – Quasar</ref><ref>''New Scientist,'' [https://www.newscientist.com/article/mg13217953.100-science-quasar-doubles-help-to-fix-the-hubble-constant.html Quasar doubles help to fix the Hubble constant], 16 November 1991</ref>
|-
|PKS 2000-330 <br /><br /> (QSO J2003-3251, Q2000-330)
|퀘이사
|1982&nbsp;−&nbsp;1986
|z = 3.78
|<ref name="PC0910+5625" /><ref>Orwell Astronomical Society (Ipswich) – OASI ; [http://www.ast.cam.ac.uk/~ipswich/Miscellaneous/Archived_astro_news.htm Archived Astronomy News Items, 1972–1997] {{웹아카이브|url=https://web.archive.org/web/20090912004912/http://www.ast.cam.ac.uk/~ipswich/Miscellaneous/Archived_astro_news.htm}}</ref><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=PKS+2000-330 Object query : PKS 2000-330], QSO J2003-3251 – Quasar</ref>
|-
|OQ172 <br /><br /> (QSO B1442+101)
|퀘이사
|1974&nbsp;−&nbsp;1982
|z = 3.53
|<ref name="BigEarHist" /><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=OQ172 Object query : OQ172], QSO B1442+101 – Quasar</ref><ref name="Q3Y" />
|-
|OH471 <br /><br /> (QSO B0642+449)
|퀘이사
|1973&nbsp;−&nbsp;1974
|z = 3.408
|별명이 "우주의 끝을 표시하는 불꽃"(the blaze marking the edge of the universe)이었다.<ref name=BigEarHist>OSU Big Ear, [http://www.bigear.org/ohsmarkr/History_OSURO.htm History of the OSU Radio Observatory]</ref><ref name=Q3Y /><ref>''[[Time Magazine]]'', [https://web.archive.org/web/20081214071937/http://www.time.com/time/magazine/article/0,9171,945213,00.html The Edge of Night], Monday, Apr. 23, 1973</ref><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=OH471 Object query : OH471], QSO B0642+449 – Quasar</ref><ref>{{저널 인용|bibcode=1990RPPh...53.1095W |doi=10.1088/0034-4885/53/8/003 |title=The detection of high-redshift quasars |journal=Reports on Progress in Physics |volume=53 |issue=8 |pages=1095 |year=1990 |last1=Warren |first1=S J |last2=Hewett |first2=P C}}</ref>
|-
|4C 05.34
|퀘이사
|1970&nbsp;−&nbsp;1973
|z = 2.877
|그것의 적색편이는 이전 기록보다 훨씬 더 커서 잘못된 것으로 여겨졌다.<ref name="Q3Y">{{웹 인용|url=http://www.reciprocalsystem.com/ce/q3y.htm|제목=QUASARS – THREE YEARS LATER|확인날짜=2021-10-11|archive-date=2017-01-18|archive-url=https://web.archive.org/web/20170118162311/http://www.reciprocalsystem.com/ce/q3y.htm|url-status=}}</ref><ref name="UoM23">The Structure of the Physical Universe, Volume III – The Universe of Motion,
[http://library.rstheory.com/books/uom/23.html CHAPTER 23 – Quasar Redshifts] {{웹아카이브|url=https://web.archive.org/web/20080619085211/http://library.rstheory.com/books/uom/23.html}}, by Dewey Bernard Larson, Library of Congress Catalog Card No. 79-88078, {{ISBN|0-913138-11-8}} , Copyright © 1959, 1971, 1984</ref><ref>{{저널 인용|제목=Some Inferences from Spectrophotometry of Quasi-Stellar Sources|저널=Astrophysical Journal|성=Bahcall|이름=John N.|성2=Oke|이름2=J. B.|연도=1971|권=163|쪽=235|bibcode=1971ApJ...163..235B|doi=10.1086/150762}}</ref><ref name="4C05.34" />
|-
|5C 02.56 <br /><br /> (7C 105517.75+495540.95)
|퀘이사
|1968&nbsp;−&nbsp;1970
|z = 2.399
|<ref name="Illingworth" /><ref name="4C05.34">{{저널 인용|제목=The Unusually Large Redshift of 4C 05.34|저널=Nature|성=Lynds|이름=R.|성2=Wills|이름2=D.|연도=1970|권=226|호=5245|쪽=532|bibcode=1970Natur.226..532L|doi=10.1038/226532a0|pmid=16057373}}</ref><ref>SIMBAD, [http://simbad.harvard.edu/simbad/sim-id?Ident=5C+02.56+&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Object query : 5C 02.56], 7C 105517.75+495540.95 – Quasar</ref>
|-
|4C 25.05 <br /><br /> (4C 25.5)
|퀘이사
|1968
|z = 2.358
|<ref name="Illingworth" /><ref name="4C05.34" /><ref name="zQSOg">{{저널 인용|제목=The Distribution of Redshifts in Quasi-Stellar Objects, N-Systems and Some Radio and Compact Galaxies|저널=Astrophysical Journal|성=Burbidge|이름=Geoffrey|연도=1968|권=154|쪽=L41|bibcode=1968ApJ...154L..41B|doi=10.1086/180265}}</ref>
|-
|PKS 0237-23 <br /><br /> (QSO B0237-2321)
|퀘이사
|1967&nbsp;−&nbsp;1968
|z = 2.225
|<ref name="UoM23" /><ref name="zQSOg" /><ref>''Time Magazine,'' [https://web.archive.org/web/20081215131450/http://www.time.com/time/magazine/article/0,9171,843526,00.html A Farther-Out Quasar], Friday, Apr. 07, 1967</ref><ref>SIMBAD, [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=%401251167&Name=QSO%20B0237-2321 Object query : QSO B0237-2321], QSO B0237-2321 – Quasar</ref><ref name="lambdaQSO">{{저널 인용|제목=On the Wavelengths of the Absorption Lines in Quasi-Stellar Objects|저널=Astrophysical Journal|성=Burbidge|이름=Geoffrey|연도=1967|권=147|쪽=851|bibcode=1967ApJ...147..851B|doi=10.1086/149072}}</ref>
|-
|4C 12.39 <br /><br /> (Q1116+12, PKS 1116+12)
|퀘이사
|1966&nbsp;−&nbsp;1967
|z = 2.1291
|<ref name="Illingworth" /><ref name="lambdaQSO" /><ref name="ManOnMnt" /><ref>SIMBAD, [http://simbad.harvard.edu/simbad/sim-id?Ident=Q1116%2B12&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Object query : Q1116+12], 4C 12.39 – Quasar</ref>
|-
|4C 01.02 <br /><br /> (Q0106+01, PKS 0106+1)
|퀘이사
|1965&nbsp;−&nbsp;1966
|z = 2.0990
|<ref name="Illingworth" /><ref name="lambdaQSO" /><ref name=ManOnMnt>''Time Magazine,'' [https://web.archive.org/web/20090911161032/http://www.time.com/time/magazine/article/0,9171,899107-1,00.html The Man on the Mountain], Friday, Mar. 11, 1966</ref><ref>SIMBAD, [http://simbad.harvard.edu/simbad/sim-id?Ident=Q0106%2B01&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Object query : Q0106+01], 4C 01.02 – Quasar</ref>
|-
|3C 9
|퀘이사
|1965
|z = 2.018
|<ref name="lambdaQSO" /><ref name=TowardEdgeUniverse>''Time Magazine,'' [https://web.archive.org/web/20080220093047/http://www.time.com/time/magazine/article/0,9171,901720,00.html Toward the Edge of the Universe], Friday, May. 21, 1965</ref><ref name=Quasi-Quasars>Time Magazine, [https://web.archive.org/web/20080423044527/http://www.time.com/time/magazine/article/0,9171,898892,00.html The Quasi-Quasars], Friday, Jun. 18, 1965</ref><ref>''The Cosmic Century: A History of Astrophysics and Cosmology'' [https://archive.org/details/cosmiccenturyhis0000long/page/379 p. 379] by Malcolm S. Longair – 2006</ref><ref>{{저널 인용|bibcode=1965ApJ...141.1295S |title=Large Redshifts of Five Quasi-Stellar Sources |journal=Astrophysical Journal |volume=141 |pages=1295 |last1=Schmidt |first1=Maarten |year=1965 |doi=10.1086/148217}}</ref><ref>[http://www.astro.caltech.edu/~george/ay21/qso.txt The Discovery of Radio Galaxies and Quasars], 1965</ref>
|-
|3C 147
|퀘이사
|1964&nbsp;−&nbsp;1965
|z = 0.545
|<ref>{{저널 인용|제목=Redshifts of the Quasi-Stellar Radio Sources 3c 47 and 3c 147|저널=Quasi-Stellar Sources and Gravitational Collapse|성=Schmidt|이름=Maarten|성2=Matthews|이름2=Thomas A.|연도=1965|쪽=269|bibcode=1965qssg.conf..269S}}</ref><ref>{{저널 인용|제목=Radio properties of optically selected high-redshift quasars. I – VLA observations of 22 quasars at 6 CM|저널=Astronomical Journal|성=Schneider|이름=Donald P.|성2=Van Gorkom|이름2=J. H.|연도=1992|권=103|쪽=1451|bibcode=1992AJ....103.1451S|doi=10.1086/116159|성3=Schmidt|이름3=Maarten|성4=Gunn|이름4=James E.}}</ref><ref>''Time Magazine, ''[http://aolsvc.timeforkids.kol.aol.com/time/magazine/article/0,9171,875737,00.html Finding the Fastest Galaxy: 76,000 Miles per Second]{{깨진 링크|date=January 2018}}, Friday, Apr. 10, 1964</ref><ref name="3C47">{{저널 인용|제목=Redshift of the Quasi-Stellar Radio Sources 3c 47 and 3c 147|저널=Astrophysical Journal|성=Schmidt|이름=Maarten|성2=Matthews|이름2=Thomas A.|연도=1964|권=139|쪽=781|bibcode=1964ApJ...139..781S|doi=10.1086/147815}}</ref>
|-
|[[3C 295]]
|[[전파은하]]
|1960&nbsp;−&nbsp;1964
|z = 0.461
|<ref name="Stern04Sept" /><ref name="Illingworth" /><ref>{{웹 인용|url=http://www.astro.caltech.edu/~george/ay21/qso.txt|제목=The Discovery of Radio Galaxies and Quasars|확인날짜=2010-10-22}}</ref><ref>{{저널 인용|제목=High Redshift Radio Galaxies|저널=Annual Review of Astronomy and Astrophysics|성=McCarthy|이름=Patrick J.|연도=1993|권=31|쪽=639–688|bibcode=1993ARA&A..31..639M|doi=10.1146/annurev.aa.31.090193.003231}}</ref><ref name="200in">{{저널 인용|제목=The Ability of the 200-INCH Telescope to Discriminate Between Selected World Models|저널=Astrophysical Journal|성=Sandage|이름=Allan|연도=1961|권=133|쪽=355|bibcode=1961ApJ...133..355S|doi=10.1086/147041}}</ref>
|-
|LEDA 25177 (MCG+01-23-008)
|[[가장 밝은 은하단 은하]]
|1951&nbsp;−&nbsp;1960
|z = 0.2 <br /><br /> (V = 61000&nbsp;km/s)
|이 은하는 [[바닷뱀자리-센타우루스 초은하단]](Hydra Supercluster)에 있다. 그것은 [[역기점|B1950.0]] {{적경|08|55|4}} {{적위|+03|21}}에 있으며 더 희미한 히드라 성단 Cl 0855+0321(ACO 732)의 BCG이다.<ref name="Stern04Sept" /><ref name="200in" /><ref>{{저널 인용|제목=The law of red shifts (George Darwin Lecture)|저널=Monthly Notices of the Royal Astronomical Society|성=Hubble|이름=E. P.|연도=1953|권=113|호=6|쪽=658–666|bibcode=1953MNRAS.113..658H|doi=10.1093/mnras/113.6.658}}</ref><ref>{{저널 인용|제목=Observational Tests of World Models: 6.1. Local Tests for Linearity of the Redshift-Distance Relation|저널=Annu. Rev. Astron. Astrophys.|성=Sandage|이름=Allan|url=http://nedwww.ipac.caltech.edu/level5/Sept01/Sandage/Sand6.html|권=1988|호=26|쪽=561–630}}</ref><ref>{{저널 인용|제목=Redshifts and magnitudes of extragalactic nebulae|저널=Astronomical Journal|성=Humason|이름=M. L.|성2=Mayall|이름2=N. U.|연도=1956|권=61|쪽=97|bibcode=1956AJ.....61...97H|doi=10.1086/107297|성3=Sandage|이름3=A. R.}}</ref><ref name="RAS-1954-05-08">{{저널 인용|제목=1053 May 8 meeting of the Royal Astronomical Society|저널=The Observatory|연도=1953|권=73|쪽=97|bibcode=1953Obs....73...97.}}</ref><ref>{{저널 인용|제목=From Atoms to Galaxies|저널=Astronomical Society of the Pacific Leaflets|성=Merrill|이름=Paul W.|연도=1958|권=7|호=349|쪽=393|bibcode=1958ASPL....7..393M}}</ref>
|-
|LEDA 51975 (MCG+05-34-069)
|가장 밝은 은하단 은하
|1936 –
|z = 0.13 <br /><br /> (V = 39000&nbsp;km/s)
|[[역기점|B1950.0]] {{적경|14|30|6}}{{적위|+3|46}} [[겉보기등급]] 17.8의 타원형 은하로 Bootes Cluster (ACO 1930)의 [[가장 밝은 은하단]]은  1936년 [[밀턴 휴메이슨]](Milton L. Humason)에 의해 40,000km/s의 후퇴 적색편이 속도를 갖는 것으로 밝혀졌다.<ref name="RAS-1954-05-08" /><ref name="z1936">{{저널 인용|제목=The Apparent Radial Velocities of 100 Extra-Galactic Nebulae|저널=The Astrophysical Journal|성=Humason|이름=M. L.|날짜=January 1936|권=83|쪽=10|bibcode=1936ApJ....83...10H|doi=10.1086/143696}}</ref><ref>"The First 50 Years At Palomar: 1949–1999 ; The Early Years of Stellar Evolution, Cosmology, and High-Energy Astrophysics'; [http://nedwww.ipac.caltech.edu/level5/Sept03/Sandage/Sandage5_2.html 5.2.1. The Mount Wilson Years] ; ''Annu. Rev. Astron. Astrophys.'' 1999. 37: 445–486</ref>
|-
|LEDA 20221 (MCG+06-16-021)
|가장 밝은 은하단 은하
|1932 –
|z = 0.075 <br /><br /> (V = 23000&nbsp;km/s)
|이것은 [[쌍둥이자리]] [[은하단]] (ACO 568)의 [[BCG]]이며 [[역기점|B1950.0]] {{적경|07|05|0}}} {{적위|+35|04}}에 위치한다.<ref name="z1936" /><ref name="RASC-26">{{저널 인용|제목=Notes and Queries (Doings at Mount Wilson-Ritchey's Photographic Telescope-Infra-red Photographic Plates)|저널=Journal of the Royal Astronomical Society of Canada|성=Chant|이름=C. A.|날짜=1 April 1932|권=26|쪽=180|bibcode=1932JRASC..26..180C}}</ref>
|-
|BCG of WMH Christie's Leo Cluster
|가장 밝은 은하단 은하
|1931&nbsp;−&nbsp;1932
|z = <br /><br /> (V = 19700&nbsp;km/s)
|<ref name="RASC-26" /><ref>{{저널 인용|제목=Apparent Velocity-Shifts in the Spectra of Faint Nebulae|저널=The Astrophysical Journal|성=Humason|이름=Milton L.|날짜=July 1931|권=74|쪽=35|bibcode=1931ApJ....74...35H|doi=10.1086/143287}}</ref><ref>{{저널 인용|제목=The Velocity-Distance Relation among Extra-Galactic Nebulae|저널=The Astrophysical Journal|성=Hubble|이름=Edwin|성2=Humason|이름2=Milton L.|날짜=July 1931|권=74|쪽=43|bibcode=1931ApJ....74...43H|doi=10.1086/143323}}</ref><ref name="ASPL-1">{{저널 인용|제목=The Large Apparent Velocities of Extra-Galactic Nebulae|저널=Leaflet of the Astronomical Society of the Pacific|성=Humason|이름=M. L.|날짜=1 January 1931|권=1|호=37|쪽=149|bibcode=1931ASPL....1..149H}}</ref>
|-
|BCG of Baede's Ursa Major Cluster
|가장 밝은 은하단 은하
|1930&nbsp;−&nbsp;1931
|z = <br /><br /> (V = 11700&nbsp;km/s)
|<ref name="ASPL-1" /><ref name="Rayton">{{저널 인용|제목=The Rayton short-focus spectrographic objective|저널=Astrophysical Journal|성=Humason|이름=M. L.|연도=1930|권=71|쪽=351|bibcode=1930ApJ....71..351H|doi=10.1086/143255}}</ref>
|-
|NGC 4860
|은하
|1929&nbsp;−&nbsp;1930
|z = 0.026 <br /><br /> (V = 7800&nbsp;km/s)
|<ref name="Rayton" /><ref name="H0" /><ref>{{저널 인용|제목=The Berkeley Meeting of the Astronomical Society of the Pacific, June 20–21, 1929|저널=Publications of the Astronomical Society of the Pacific|연도=1929|권=41|호=242|쪽=244|bibcode=1929PASP...41..244.|doi=10.1086/123945}}</ref>
|- style="background:#c0c0e0;"
|NGC 7619
|은하
|1929
|z = 0.012 <br /><br /> (V = 3779&nbsp;km/s)
|적색편이 측정을 사용하여 NGC 7619가 측정 당시 가장 큰 값이었다. 발표 당시에 이는 거리에 대한 일반적인 지침으로 아직 받아들여지지 않았지만, 그해 말 에드윈 허블이 적색편이를 거리와 관련하여 설명한 후 추론된 거리로 널리 받아들여졌다.<ref name="H0" /><ref name=Humason-1929-03-15>From the ''Proceedings of the National Academy of Sciences''; Volume 15 : March 15, 1929 : Number 3 ; [http://antwrp.gsfc.nasa.gov/diamond_jubilee/d_1996/hum_1929.html The Large Radial Velocity of N. G. C. 7619] ; January 17, 1929</ref><ref>''The Journal of the Royal Astronomical Society of Canada / Journal de la Société Royale D'astronomie du Canada;'' Vol. 83, No.6 December 1989 Whole No. 621 ; [http://antwrp.gsfc.nasa.gov/diamond_jubilee/d_1996/sandage_hubble.html EDWIN HUBBLE 1889–1953]</ref>
|- style="background:#e0e0c0;"
|[[NGC 584]] <br /><br /> (Dreyer nebula 584)
|은하
|1921&nbsp;−&nbsp;1929
|z = 0.006 <br /><br /> (V = 1800&nbsp;km/s)
|당시 성운은 아직 독립된 은하로 받아들여지지 않았다. 그러나 1923년에 은하는 일반적으로 우리은하 외부에 있는 것으로 인식되었다.<ref name="RAS-1954-05-08" /><ref name="H0">{{저널 인용|제목=H_0: The Incredible Shrinking Constant, 1925–1975|저널=Publications of the Astronomical Society of the Pacific|성=Trimble|이름=Virginia|url=https://escholarship.org/content/qt0tg0q2qx/qt0tg0q2qx.pdf?t=nlq2m6|연도=1996|권=108|쪽=1073|bibcode=1996PASP..108.1073T|doi=10.1086/133837}}</ref><ref name="Humason-1929-03-15" /><ref name="Bio52" /><ref>{{저널 인용|제목=Comet Skjellerup|저널=Harvard College Observatory Bulletin|성=Bailey|이름=S. I.|연도=1920|권=739|쪽=1|bibcode=1920BHarO.739....1B}}</ref>><ref>New York Times, [https://query.nytimes.com/gst/abstract.html?res=9906E2DA153CE533A2575AC1A9679C946095D6CF DREYER NEBULA NO. 584 Inconceivably Distant; Dr. Slipher Says the Celestial Speed Champion Is 'Many Millions of Light Years' Away.] ; January 19, 1921, Wednesday</ref><ref name=NYT-1921-01-18>''New York Times,'' [https://query.nytimes.com/gst/abstract.html?res=9F06E1DB153CE533A2575BC1A9679C946095D6CF Nebula Dreyer Breaks All Sky Speed Records; Portion of the Constellation of Cetus Is Rushing Along at Rate of 1,240 Miles a Second.] ; January 18, 1921, Tuesday</ref>
|- style="background:#e0e0c0;"
|[[솜브레로 은하|M104]] ([[솜브레로 은하|NGC 4594]])
|은하
|1913&nbsp;−&nbsp;1921
|z = 0.004 <br /><br /> (V = 1180&nbsp;km/s)
|이것은 적색편이가 결정된 두 번째 은하인데 첫 번째는 안드로메다로 이는 우리에게 접근하고 있으므로 거리를 추론하는 데 적색편이를 사용할 수 없다. 둘 다 [[베스토슬라이퍼]](Vesto Melvin Slipher)에 의해 측정되었다. 이때 성운은 아직 독립 은하로 받아들여지지 않았다. NGC 4594는 원래 1000km/s로 측정되었다가 1916년에 1100으로, 그리고 1916년에 1180으로 개선되었다.<ref name="H0" /><ref name="Bio52">National Academy of Sciences; [https://books.google.com/books?id=h9xnzIV_zQYC Biographical Memoirs: V. 52] – Vesto Melvin Slipher; {{ISBN|0-309-03099-4}}</ref><ref name="NYT-1921-01-18" />
|- style="background:#e0c0c0;"
|[[아크투루스]] <br /><br /> (목동자리 알파)
|[[항성]]
|1891&nbsp;−&nbsp;1910
|160 [[광년|ly]] <br /><br /> (18 mas) <br /><br /> <small>(this is very inaccurate, true=37 ly)</small>
|이 숫자는 오류로 원래 1891년에 발표된 수치가 1910년에 40 광년(60 mas)로 수정되었다. 1891년부터 1910년까지 이 별은 시차가 가장 작은 것으로 알려진 별이며 따라서 거리가 가장 먼것으로 알려진 별이라고 여겨졌다. 1891년 이전에는 Arcturus가 127 mas의 시차를 갖는 것으로 기록되었다.<ref>''Hawera & Normanby Star'', [http://paperspast.natlib.govt.nz/cgi-bin/paperspast?a=d&d=HNS19101229.2.10 "Items of Interest"], 29 December 1910, Volume LX, page 3 . Retrieved 25 March 2010.</ref><ref>''[[Evening Star (San Jose)|Evening Star]]'' (San Jose), [https://news.google.com/newspapers?id=VvQxAAAAIBAJ&sjid=T-MFAAAAIBAJ&pg=984,6069796&dq=parallax+star&hl=en "Colossal Arcturus"], ''Pittsburgh Dispatch'', 10 June 1910 . Retrieved 25 March 2010.</ref><ref>''[[Nelson Evening Mail]]'', [http://paperspast.natlib.govt.nz/cgi-bin/paperspast?a=d&d=NEM18911102.2.16 "British Bloodthirstiness"], 2 November 1891, Volume XXV, Issue 230, Page 3 . Retrieved 25 March 2010.</ref><ref>"Handbook of astronomy", ''Dionysius Lardner & Edwin Dunkin'', Lockwood & Co. (1875), [https://archive.org/details/handbookastrono00lardgoog/page/n171 p.121]</ref>
|-
|[[카펠라]] <br /><br /> (마차부자리 알파,)
|[[항성]]
|1849&nbsp;-&nbsp;
|72 ly <br /><br /> (46 mas)
|<ref>"The Three Heavens", ''Josiah Crampton'', William Hunt and Company (1876), [https://archive.org/details/threeheavens00cramgoog/page/n215 <!-- pg=163 --> p.164]</ref><ref>{{언어링크|de}} ''[[Kosmos: Entwurf einer physischen Weltbeschreibung]]'', Volume 4, [[Alexander von Humboldt]], J. G. Cotta (1858), [https://books.google.com/books?ei=58vkTZKCEcKugQfhxfGsBg&ct=result&id=MbYqAQAAIAAJ p.195]</ref><ref>"Outlines of Astronomy", ''John F. W. Herschel'', Longman & Brown (1849), ch. 'Parallax of Stars', [https://books.google.com/books?id=cvY0AAAAcAAJ&pg=PA552 p.551 (section 851)]</ref>
|-
|[[폴라리스]] <br /><br /> ([[폴라리스|작은곰자리 알파]])
|항성
|1847&nbsp;-&nbsp;1849
|50 ly <br /><br /> (80 mas) <br /><br /> <small>(this is very inaccurate, true=~375 ly)</small>
|<ref name="Pulkowa-1849" /><ref name=Sidereal-1847-04>The Sidereal Messenger, "Of the Precession of the Equinoxes, Nutation of the Earth's Axis, And Aberration of Light", Vol.1, No.12, ''April'' 1847: 'Derby, Bradley, & Co.' Cincinnati</ref>
|-
|[[베가]] <br /><br /> (거문고자리 알파)
|항성 ([[이중성]] 짝의 부분)
|1839&nbsp;-&nbsp;1847
|7.77 pc <br /><br /> (125 mas)
|<ref name=Pulkowa-1849>''The North American Review'', "The Observatory at Pulkowa", ''FGW Struve'', Volume 69 Issue 144 (July 1849)</ref>
|-
|[[백조자리 61]]
|[[쌍성]]<br/>...............................
|1838&nbsp;−&nbsp;1839
|3.48 [[파섹|pc]] <br /><br /> (313.6 mas)
|이는 태양 이외에 그 거리가 측정된 최초의 항성이다.<ref name="Pulkowa-1849" /><ref>''SEDS'', [http://messier.seds.org/xtra/Bios/bessel.html "Friedrich Wilhelm Bessel (July 22, 1784 – March 17, 1846)"] {{웹아카이브|url=https://web.archive.org/web/20120204150631/http://messier.seds.org/xtra/Bios/bessel.html}} . Retrieved 11 November 2009.</ref><ref>''[[Harper's New Monthly Magazine]]'', [http://digital.library.cornell.edu/cgi/t/text/pageviewer-idx?c=harp;cc=harp;idno=harp0049-6;node=harp0049-6%3A1;size=l;frm=frameset;seq=837;view=image;page=root "Some Talks of an Astronomer"], ''Simon Newcomb'', Volume 0049 Issue 294 (November 1874), pp.827 (accessed 2009-Nov-11)</ref>
|- style="background:#e0e0c0;"
|[[천왕성]]
|태양계의 [[행성]]
|1781&nbsp;−&nbsp;1838
|18 [[AU]]
|이것은 항성의 시차를 최초로 성공적으로 측정하기 전에 발견된 마지막 행성이었습니다. 별들이 행성들보다 훨씬 더 멀리 떨어져 있다는 것이 확인되었다.
|- style="background:#c0c0e0;"
|[[토성]]
|태양계의 행성
|1619&nbsp;−&nbsp;1781
|10 AU
|[[케플러의 제3법칙]]에 의하여 마침내 토성이 고전적 행성의 가장 바깥쪽에 있는 것으로 결정되었고 그 거리가 구하여졌다. 그것은 가장 긴 궤도 주기와 가장 느린 궤도 운동을 가졌기 때문에 이전에는 가장 바깥쪽에 있는 것으로 추측되었다. 항성들이 행성들보다 훨씬 더 멀리 떨어져 있다는 것이 확인되었다.
|- style="background:#e0c0e0;"
|[[화성]]
|태양계의 행성
|1609&nbsp;−&nbsp;1619
|2.6 AU when Mars is diametrically opposed to Earth
|케플러는 그의 출판물 [[신천문학]](Astronomia nova)에서 화성과 지구의 궤도를 특성을 정확하게 밝혔다. 항성은 행성보다 훨씬 더 멀리 떨어져 있다고 추측하였다.
|- style="background:#e0c0e0;"
|[[태양]]
|항성
|3rd century BC — 1609
|380 Earth radii <small> (very inaccurate, true=16000 Earth radii) </small>
|[[사모스의 아리스타쿠스]](Aristarchus of Samos)는 지구에서 달까지의 거리에 관련하여 지구에서 태양까지의 거리를 측정했다. 달까지의 거리는 지구 반지름으로 설명되었다(20, 역시 부정확함). 지구의 지름은 이전에 계산되었다. 당시에는 일부 행성이 더 멀리 떨어져 있다고 가정했지만 거리는 측정할 수 없었다. 케플러가 지구가 아닌 알려진 5개의 행성 중 태양으로부터의 거리를 결정할 때까지 행성의 순서는 추측이었다. 고정된 항성은 행성보다 훨씬 더 멀리 떨어져 있다고 추측되었다.
|- style="background:#e0c0e0;"
|[[달]]
|행성의 [[위성]]
|3rd century BC
|20 Earth radii <small> (very inaccurate, true=64 Earth radii) </small>
|[[사모스의 아리스타르코스]]가 지구로부터 달까지의 거리를 측정하였다. 지구의 반지름은 이전에 계산되었다.
|-
| colspan="5" |

* <small>''z''는 [[우주팽창|우주의 팽창]]에 의한 '''후퇴속도'''와 '''추정 거리'''를 나타내는 [[적색편이]]이다.</small>
* <small>''mas''는 '각도'의 측정값을 나타내는 [[시차 (천문학)|'''시차''']]이고, [[삼각측량법]]을 이용하여 천체까지의 거리를 결정할 수 있다.</small>

|}

== 발견 연도에 따른 최원거리 천체 목록 ==
이 목록에는 거리 결정이 아니라 천체를 발견한 연도별로 가장 멀리 있는 천체의 목록이 포함되어 있다. 천체는 거리 측정 없이 발견되었을 수 있으며, 나중에 그 당시 알려진 것 중 가장 멀리 있는 것으로 밝혀졌다. 그러나 천체의 이름이 지정되거나 설명되어 있어야 한다. [[OJ 287]]과 같은 천체는 이미 1891년에 사진판을 사용하여 탐지되었음에도 불구하고 전파망원경이 출현할 때까지 무시되었다.
{| class="wikitable"
|+예
! 기록 연도
! 현대의<br />광행거리 [[광년|(Mly)]]
! 천체
! 유형
! 탐지된 방법
! 최초 발견자<sup>(1)</sup>
|-
| 964
| 2.5<ref name="jensenetal2003">{{저널 인용|제목=Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations|저널=Astrophysical Journal|성=Jensen, Joseph B.|성2=Tonry, John L.|날짜=February 2003|권=583|호=2|쪽=712–726|arxiv=astro-ph/0210129|bibcode=2003ApJ...583..712J|doi=10.1086/345430|성3=Barris, Brian J.|성4=Thompson, Rodger I.|성5=Liu, Michael C.|성6=Rieke, Marcia J.|성7=Ajhar, Edward A.|성8=Blakeslee, John P.}}</ref>
| [[안드로메다 은하]]
| [[나선은하]]
| 맨눈
| [[압드 알라흐만 알수피]]<ref name="NSOG">{{서적 인용|제목=The Night Sky Observer's Guide, Volume 1|성=Kepple|이름=George Robert|성2=Glen W. Sanner|날짜=1998|출판사=Willmann-Bell, Inc.|쪽=18|isbn=978-0-943396-58-3}}</ref>
|-
| 1654
| 3
| [[삼각형자리 은하]]
| [[나선은하]]
| 굴절 망원경
| [[w:Giovanni Battista Hodierna|조반니 바티스타 호디에르나]]<ref>{{저널 인용|제목=Hodierna's Observations of Nebulae and his Cosmology|저널=Journal for the History of Astronomy|성=Fodera-Serio, G.|성2=Indorato, L.|날짜=February 1985|권=16|호=1|쪽=1–36|bibcode=1985JHA....16....1F|doi=10.1177/002182868501600101|성3=Nastasi, P.}}</ref>
|-
| 1779년
| 68<ref name="Gavazzietal1999">{{저널 인용|제목=The 3D structure of the Virgo cluster from ''H''-band Fundamental Plane and Tully-Fisher distance determinations|저널=Monthly Notices of the Royal Astronomical Society|성=G. Gavazzi|성2=A. Boselli|날짜=1999|권=304|호=3|쪽=595–610|arxiv=astro-ph/9812275|bibcode=1999MNRAS.304..595G|doi=10.1046/j.1365-8711.1999.02350.x|성3=M. Scodeggio|성4=D. Pierini|성5=E. Belsole}}</ref>
| [[메시에 58]]
| [[막대나선은하]]
| [[굴절 망원경]]
| [[샤를 메시에]]<ref name="burnham">{{서적 인용|url=https://archive.org/details/burnhamscelestia03burn/page/2086|제목=Burnham's Celestial Handbook: Volume Three, Pavo Through Vulpecula|성=Burnham|이름=Robert Jr|저자링크=Robert Burnham Jr|날짜=1978|출판사=Dover|쪽=[https://archive.org/details/burnhamscelestia03burn/page/2086 2086–2088]|isbn=978-0-486-23673-5}}</ref>
|-
| 1785년
| 76.4<ref>{{웹 인용|url=http://www.astro.yale.edu/obey/cgi-bin/catalog.cgi?n584|제목=The OBEY Survey – NGC 584}}</ref>
| [[NGC 584]]
| [[은하]]
|
| [[윌리엄 허셜]]
|-
| 1880년대
| 206 ± 29<ref name="ned-ngc1">{{웹 인용|url=http://nedwww.ipac.caltech.edu/cgi-bin/nDistance?name=NGC+0001|제목=Distance Results for NGC 0001|웹사이트=NASA/IPAC Extragalactic Database|확인날짜=2010-05-03}}</ref>
| [[NGC 1]]
| [[나선은하]]
|
| [[욘 드레위에르|드레이어]], [[윌리엄 허셜|허셜]]
|-
| 1959년
| 2,400<ref>{{저널 인용|제목=On the Mass and Distance of the Quasi-Stellar Object 3C 273|저널=Astrophysics and Space Science|성=Falla|이름=D. F.|성2=Evans|이름2=A.|연도=1972|권=15|호=3|쪽=395|bibcode=1972Ap&SS..15..395F|doi=10.1007/BF00649767}}</ref>
| [[3C 273]]
| [[퀘이사]]
| [[파크스 천문대|파크스 전파 망원경]]
| [[마르턴 스밋]], [[w:John Beverley Oke|베브 오케]]<ref>[http://www.aavso.org/vstar/vsots/spring05.shtml Variable Star Of The Season] {{웹아카이브|url=https://web.archive.org/web/20090123191313/http://www.aavso.org/vstar/vsots/spring05.shtml}}</ref>
|-
| 1960년
| 5,000<ref>{{저널 인용|제목=A New Distant Cluster of Galaxies|저널=Astrophysical Journal|성=Minkowski|이름=R.|연도=1960|권=132|쪽=908|bibcode=1960ApJ...132..908M|doi=10.1086/146994}}</ref>
| [[3C 295]]
| [[전파은하]]
| [[팔로마 천문대]]
| [[w:Rudolph Minkowski|루돌프 민코프스키]]
|-
| colspan="6" |<center> ''테이블에서 누락된 데이터''</center>
|-
| 2009년
| 13,000<ref>{{뉴스 인용|url=http://www.cnn.com/2009/TECH/04/29/gamma.ray.burst.space/index.html|제목=Exploding star is oldest object seen in universe|날짜=2009-04-29|출판사=Cnn.com|확인날짜=2010-10-22}}</ref>
| [[GRB 090423]]
| [[w:Gamma-ray burst progenitors|감마선 폭발 선조]]
| [[스위프트 감마선 폭발 임무|스위프트 감마선 버스트 미션]]
| H. 크림<sub>H. Krimm</sub> 등<ref>{{저널 인용|제목=GRB 090423: Swift detection of a burst|저널=GCN Circulars|성=Krimm, H.|url=http://gcn.gsfc.nasa.gov/gcn3/9198.gcn3|날짜=2009|권=9198|쪽=1|bibcode=2009GCN..9198....1K|저자표시=etal}}</ref>
|}

== 같이 보기 ==
* [[우주의 나이]]
* [[W:List of largest cosmic structures|가장 큰 우주 구조 목록(List of largest cosmic structures)]]
* [[극단적인 외계 행성 목록]]
* [[w:Lists of astronomical objects|천체 목록Lists of astronomical objects)]]
* [[w:List of most distant stars|최원거리 항성 목록(List of most distant stars)]]

== 각주 ==
{{각주|3}}
{{은하}}
{{항성}}
{{Portal bar|천문학|우주 개발|우주 공간|태양계}}

[[분류:천체]]