최원거리 천체 목록

이 문서에서는 지금까지 가장 멀리 있는 천체로 발견 및 확인된 천체들과 그 분류된 기간을 기재하고 있다. 아래에 나열된 천체들의 광행거리와 비교하기 위해 대폭발(빅뱅) 이후 우주의 나이는 현재 13.787±0.020Gyr로 추정된다. 가까운 은하에 있는 천체를 제외한 멀리 떨어진 천체까지의 거리는 거의 항상 빛의 우주적 적색편이의 측정으로부터 추론한다. 본질적으로, 매우 먼 물체는 매우 희미한 경향이 있으므로 이러한 거리 측정은 어렵고 오류가 발생할 수 있다. 천체까지의 거리를 분광학적으로 결정할 지 아니면 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 분광학적 적색편이는 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. 고유거리는 은하가 고정된 시점에 얼마나 멀리 떨어져 있는지를 측정한다. 현재 우주론적 척도인자 값은 1을 가지므로 고유거리는 공변거리와 같다: a ( t 0 ) = 1 {\displaystyle a(t_{0})=1} . 고유거리는 마치 시간의 흐름을 멈출 수 있는 것처럼 얻은 거리를 나타낸다 (프리드만-르메트르-로버트슨-워커 계량에서 d t = 0 {\displaystyle dt=0} 로 설정), 계량 막대를 사용하면서 은하계까지 걸어간다고 가정한다. 실용적인 이유로, 고유거리는 은하가 빛을 방출하는 시점부터 관측자(지구에 있는)가 빛 신호를 수신하는 시점까지의 빛이 이동한 거리로서 (프리드만-르메트르-로버트슨-워커 계량에서 d s = 0 {\displaystyle ds=0} 로 설정) 계산된다. 고유거리는 우주의 팽창, 즉 빛이 통과할 때 공간이 팽창하는 것을 고려하기 때문에 "광행거리"와 다르며, 그 결과 허블 구(Hubble sphere) 너머의 가장 먼 은하를 찾아내고 따라서 광속 c 보다 큰 후퇴 속도를 가진 수치를 산출한다. 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. 2012년 이전에는 2002년 중반부터 2012년 12월 사이에 관측된 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. 여기에 포함된 일부 천체는 분광학적으로 관측되었지만, 단지 한 방출선만이 잠정적으로 탐지되었으므로, 따라서 연구자들은 여전히 후보로 간주하고 있다. 이 목록의 천체는 거리를 결정하였을 때 가장 멀리 있는 천체로 확인되었다. 이것은 종종 천체의 발견 날짜와 동일하지 않다. 천체까지의 거리는 시차 측정, 세페이드 변광성 또는 Ia형 초신성과 같은 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. 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. 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