This image shows the dusty Galaxy NGC 4526, the galaxy that was host of a brilliant supernova in 1994. It has a central dust disc in the middle of the galaxy, and the fact that it seems dusty on the one hand more than the other allows us to learn which edge is closer to us. (Suggestion: It is the most dusty advantage). (Credit: ESA/HUBBLE AND NASA, PROCESSING: JUDY SCHMIDT)
When we see spiral galaxies, some are frequent, others are addressed, but most are inclined at angle. But what side is it closer to us?
Throughout the universe, spiral galaxies are extremely common.
The spirals, initially registered as weak and diffuse objects without a discernible structure through more primitive telescopes, were clearly observed since mid -1800 prevail in the night sky. We now understand that spirals are galaxies such as our own Milky Way, with central planes rich in dust and spiral arms that can be identified more easily depending on the inclination of the galaxy. (Credit: That/p. Grosbøl)
The NGC 772 spiral galaxy does not have a central bar, but exhibits huge levels of star formation and an unequal dust distribution: evidence of large populations of bright stars on the farthest side of the dusty galaxy. Large spiral and elliptical galaxies, although they are not as abundant as low dwarf galaxies, host most of the stars that have been formed throughout the history of the universe. (Credit: Gemini International Observatory/Noirlab/NSF/Aura; Image processing: TA Rector (University of Alask
Most of the spirals observed do not appear on the edge or face, but are inclined: inclined at angle.
When identifying the spiral components (disc) and elliptical (halo type) of the shadow galaxy, one can subtract the elliptical portion of the optical image data, leaving only the component similar to the disk. This view, created with Hubble data, reveals our best optical views of the album -shaped portion. Although the shadow galaxy is seen almost on the edge, like most spiral galaxies, it leans at an angle with respect to us. (Credit: Vicent Peris (OUV / PTEAM), Mast, STSCI, Aura, NASA)
Like many inclined or inclined spiral galaxies, NGC 7331, which is shown in the foreground of this image, exhibits a much more duosa screen on one side compared to the other. The prominence of this “unilateral” dust gives us important clues about the inclination of the galaxy with respect to our perspective. (Credit: Fort Lewis College Observatory)
Unlocking the answer requires together only two pieces of key information.
Located at approximately 44 million light years away, Galaxy NGC 5866, also known as Messier 102, is a practically perfectly perfect spiral galaxy that is sometimes called the spindle galaxy. Its dust lane, although slightly deformed by what the observations suggest is a recent interaction with a complementary galaxy, almost perfectly divides the plane of the galaxy itself. (Credit: NASA, ESA and the Hubble Heritage team (STSCI/Aura))))
A stars density map on the Milky Way and the surrounding sky, which clearly shows the Milky Way, large and small Magellanic clouds, and if you look more closely, NGC 104 to the left of the SMC, NGC 6205 slightly above and the left of the galactic nucleus, and NGC 7078 slightly below. In total, the Milky Way contains about 200–400 billion stars in its extension in the form of a disc. There are many galaxies to discover, but within 10 degrees above and below the galactic plane, visible light is a lousy tool to reveal them. (Credit: ESA/GAIA)
We can observe this directly examining the spiral galaxies views of edge, including ours.
Seeing the Milky Way in infrared wavelengths of light, we can see through large quantities of the galactic dust and see the distribution of stars and stars forming regions behind them. As revealed by the 2 microns survey All-Scy (2Mass), the densest galactic dust collections can be seen tracking our spiral arms, but the center of the Milky Way plane is where the dust is dense. The views of infrared and visible light show this, but in very different ways. (Credit: 2MASS/IPAC/CALTECH & UMASS)
