NGC 2622 is a Seyfert 1 Galaxy located in the constellation of Cancer in the northern hemisphere. NGC 2622 is called NGC 2622 in the New General Catalogue (NGC). This catalogue is a list of deep space objects compiled by John Louis Emil Dreyer in 1888 to …

NGC 2622 is a Barred Spiral Galaxy in the Cancer constellation. NGC 2622 is situated close to the celestial equator and, as such, it is at least partly visible from both hemispheres in certain times of the year.

2020年6月8日 · Physical Information: The recessional velocity of NGC 2622 is 8580 km/sec, but it is obviously interacting with PGC 24266 (each has extended regions of gas, stars and clusters of stars strewn into intergalactic space by their interaction), so the pair must be at the same distance from us and their average recessional velocity should be used to ...

2017年3月14日 · The main target in this image is NGC 2622, which is a slightly distorted barred spiral galaxy (~14 magnitude). NGC 2622 is classified as a Seyfert I galaxy which means that it hosts a supermassive black hole at its core surrounded by an active accretion disk that is emitting massive amounts of UV and X-ray radiat...

Media in category "NGC 2622" The following 4 files are in this category, out of 4 total.

NGC 2622 este o seyfert 1 galaxy⁠ (d) situată în constelația Racul. [7][8][9] A fost descoperită în 1865 de către Albert Marth. [10] Se află la o distanță de 120,29 de megaparseci de Pământ. [11]

NGC 262 (also known as Markarian 348) is the largest known spiral galaxy, [5] located in the constellation Andromeda. [1] It is a Seyfert 2 spiral galaxy located 287 million light years away. [2]

NGC 2623 (also known as ARP 243) is an interacting galaxy located around 263 million light-years away in the constellation Cancer. It was discovered on 19 January 1885 by French astronomer Édouard Jean-Marie Stephan.

NGC 2623 是一個在天球上位於 巨蟹座 的星系 [1]。 這個星系因為是由兩個星系之間強烈碰撞後 合併 而擁有特殊形態 [1]。 星系之間的劇烈碰撞使作用星系內的氣體雲被壓縮與氣體動能大幅增強，使 恆星形成 率急遽升高 [1]。 恆星形成中的區域即為影像中的亮藍色斑點。 這樣的區域在星系中心以及沿著由塵埃和氣體組成的NGC 2623的大半徑曲線（即 潮汐尾）中呈現星團狀分布 [1]。 這些潮汐尾結構延伸約5萬光年 [1]，許多年輕高溫新生恆星在其中聚集形成星團，在NGC …

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