광도 순 항성 목록

아래 목록은 광도 순서로 밝은 별부터 어두운 별까지 나열한 것이다. 절대등급은 어떤 별을 10파섹 거리에 두고 바라보았을 때의 밝기이다. 절대등급 순서로 별을 나열할 경우 높은 순위를 차지하는 것은 질량이 큰 초거성들이다. 이들은 매우 희귀하며 지구에서 멀리 떨어져 있기 때문에 정확한 자료를 도출하는 데 한계가 있다. 따라서 같은 별을 놓고 천문학자들이 제각기 다른 관측값을 내놓기도 한다. 표에 따르면 현재까지 관측된 별 중 가장 밝은 것은 태양광도의 794만 배로 빛나는 궁수자리 V4650이다. 그러나 외부은하 천체인 퀘이사(Quasar)를 포함시킬 경우 순위는 바뀐다. 현재 발견된 퀘이사 중 가장 밝은 것은 돛자리 구역에서 발견된 3C 273이다. 이 퀘이사의 겉보기 등급은 12.8로 맨눈으로 볼 수는 없으나, 절대등급은 -26.7에 달한다. 만약 이 퀘이사를 지구로부터 10파섹 떨어진 곳에 옮겨다 놓는다고 가정하면, 태양과 똑같은 밝기로 지구인들의 눈에 보일 것이다. 여기서 퀘이사는 태양보다 약 2조 배 더 밝다는 계산이 나온다. 이 정도 밝기는 우리 은하 전체 밝기의 약 100배에 해당하는 값이다. 그러나 퀘이사의 광도는 시간에 따라 차이를 보인다. 감마선 영역만 놓고 보면 SGR 1806-20이라는 마그네타(중성자 별의 일종)는 관측된 태양계 외부 천체 중에서 가장 밝았다. 2004년 12월 27일 이 별은 강력한 감마선 폭발을 일으켰다. 만약 인간이 감마선을 볼 수 있고, 이 별에서 32.6광년 떨어진 곳에 자리잡고 있다고 가정하면 폭발 순간의 밝기는 -29였을 것이다. 이는 태양보다 밝다. (3.2×10^15~1016 L☉) 1998년 관측된 GRB 971214 감마선 폭발의 경우 초신성 수백 개의 폭발과 맞먹는 빛을 발산했다. 이후 연구를 통해 이 에너지는 초신성 1개에서 지구를 향해 뿜어져 나온 것으로 알려졌다. M33-013406.63, LGGS J013406.63+304147.8 이라고도 불리는 별은 원래 태양의 8,000,000배 이상의 광도를 가진다고 생각되었으나 새 문헌이 M33-013406.63이 쌍성일 가능성을 제시했고 이 경우 광도는 태양의 약 4,500,000배로 감소한다. 쌍성계로 알려져 있다. 삼연성계일 가능성도 있다. 동반성의 광도도 태양의 1,000,000배에 달하지만 주성의 밝기에 묻힌다. Mercer 23은 은하면 근처의 산개성단이다. 머서 30은 드래곤피쉬 성운의 산개성단이다. 절대복사등급이 실수로 −11.5 대신 −10.5로 적혀있다. 쌍성계지만 동반성이 주성에 비해 매우 어둡다. VVV CL041는 산개성단이다. Cl 1813-178은 분자운 복합체 W33 복합체의 산개성단이다. VVV CL074는 산개성단이다. 변광성, 1994년 분출 당시에는 밝기가 5배 더 높았다.(태양의 10,000,000배) 밝은 청색변광성, 최고 광도 기준. G10.0-0.3은 은하중심의 전파 성운이다.. 머서 81은 분자운 G338.4+0.2의 산개성단이다. DBSB 179는 분자운 G347.6+0.2의 산개성단이다. 보훔 10은 용골자리 성운의 산개성단이다. 푸른 거품 성운은 Hen 3-519 주변의 볼프-레이에 성운이다. 엄밀히 말하면 MSX5C G358.5391+00.1305가 별의 이름이고 Wray 17-96이 성운의 이름이다. N135은 대마젤란 은하의 방출 성운이다. 이 매개변수는 이러한 별에 대한 광학적 적합만을 기반으로 한다. DEM S10은 소마젤란 은하의 H II 영역이다. FSR 1555은 성단이다. DEM S80은 소마젤란 은하의 H II 영역이다. SFC 27은 분자운 G291.27-0.71의 일부다. BSDL 2505은 대마젤란 은하의 성단이다. 돛자리 R2는 돛자리 분자 능선의 OB 성협이다. 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