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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]
Malin 1B is located 46,000 light-years (14,000 pc) away from the high surface brightness central spiral of Malin 1, which may be responsible for the formation of the galaxy's central bar. Meanwhile, SDSS J123708.91+142253.2 is located within the huge, faint halo of Malin 1 and might have caused the formation of the extended low surface ...
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]
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).
By defining R e as the radius of the isophote containing half of the total luminosity of the galaxy, the half-light radius, de Vaucouleurs profile may be expressed as: = + [() /] or = [() /] where I e is the surface brightness at R e.
The luminosity is calculated by multiplying the galaxy's apparent brightness by , where is its distance from Earth, and the spectral-line width is measured using long-slit spectroscopy. A series of collaborative catalogs of galaxy peculiar velocity values called CosmicFlow uses Tully–Fisher analysis; the Cosmicflow-4 catalog has reached 10000 ...
Sky Quality Meter model SQM-L. A sky quality meter (SQM) is an instrument used to measure the luminance of the night sky, more specifically the Night Sky Brightness (NSB) at the zenith, with a bandwidth ranging from 390 nm to 600 nm. [1]
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