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An image of NGC 45, a low surface brightness spiral galaxy, by GALEX. UGC 477 is located over 110 million light-years away in the constellation of Pisces. [1]A low-surface-brightness galaxy, or LSB galaxy, is a diffuse galaxy with a surface brightness that, when viewed from Earth, is at least one magnitude lower than the ambient night sky.
UGC 6614 is classified as a low surface brightness (LSB) galaxy. [3] [4] [5] The galaxy is nearly face-on and has a ring-like feature around its bulge, [6] with distinctive extended spiral arms. [7] The bulge of UGC 6614 is found to be red, similar to those of S0 and other elliptical galaxies, hinting at the existence of an old star population. [8]
A truly dark sky has a surface brightness of 2 × 10 −4 cd m −2 or 21.8 mag arcsec −2. [9] [clarification needed] The peak surface brightness of the central region of the Orion Nebula is about 17 Mag/arcsec 2 (about 14 milli nits) and the outer bluish glow has a peak surface brightness of 21.3 Mag/arcsec 2 (about 0.27 millinits). [10]
The fundamental plane is a set of bivariate correlations connecting some of the properties of normal elliptical galaxies.Some correlations have been empirically shown. The fundamental plane is usually expressed as a relationship between the effective radius, average surface brightness and central velocity dispersion of normal elliptical galaxies.
First low surface brightness galaxy: Malin 1: Coma Berenices: 1986 Malin 1 was the first verified LSB galaxy. LSB galaxies had been first theorized in 1976. [26] First superluminal jet from a Seyfert III Zw 2: Pisces [27] 2000 [28]
In visible light, the galaxy exhibits an overall bluish color and as it is relatively dim for a galaxy of its size, it is classified as a low surface brightness galaxy (LSB). [ 2 ] [ 3 ] NGC 5866B is located relatively close in the sky to the more well-known NGC 5907 (Splinter Galaxy) and NGC 5866 (Spindle Galaxy).
For example, all observations seem to indicate that Type Ia supernovae that are of known distance have the same brightness, corrected by the shape of the light curve. The basis for this closeness in brightness is discussed below; however, the possibility exists that the distant Type Ia supernovae have different properties than nearby Type Ia ...
Tuning-fork-style diagram of the Hubble sequence Galaxy morphological classification is a system used by astronomers to divide galaxies into groups based on their visual appearance. There are several schemes in use by which galaxies can be classified according to their morphologies, the most famous being the Hubble sequence , devised by Edwin ...