When Slipher noticed inclined absorption lines in the nuclear spectra of the M31 and the Sombrero galaxy he made the discovery that the galaxies rotate in 1914. (Read, Iorio, Agertz, and Fraternali 2016).
Wolf therefore also identified the M81's likely atomic range lines in the same year (McGaugh, Lelli , and Schombert 2016).
Following these findings in 1918, Pease used the Mt. Wilson 60-inch telescope to look into the rotation of the massive Andromeda nebula (Bouché, Murphy, Kacprzak, Péroux, Contini, Martin, and Dessauges-Zavadsky 2013).
Courteau, Cappellari, de Jong, Dutton, Emsellem, Hoekstra, Koopmans, Mamon, Maraston, Treu, and Widrow 2014,
suggests that to do this, he had to obtain a minor axis alit spectrum of the m13, which had an exposure of 84 hours.
Primarily, the rotation curves describe the concept on how the velocity of objects in the galaxy changes according to the function of the object distance in the center.
For instance, considering the central mass as a star or a black hole with objects moving circular way around the rotational velocity than can be determined by the newton’s centripetal force and gravitational equations.
Rotational Curves of Distant Galaxies
The understanding of the evolution and information of the galaxies has improved significantly over the past few decades (Lelli , McGaugh, and Schombert 2016).
The improvement has been by space-based facilities and the larger ground-based telescopes that are leading the multiwavelength surveys accumulating study of more massive galaxies over the increasing range of redshifts.
Importantly, much of the knowledge information and knowledge about the distant galaxies rest on the relatively crude information that is rarely on integrated spectra (Truong, Newman, Simon, Blitz, Ellis, and Bolatto 2017).
The results of shapes of the rotational curves of distant galaxies have shown similar characteristics similar to the rotational curves of near galaxies (Wheeler, Pace, Bullock, Boylan-Kolchin, Oñorbe, Elbert, Fitts, Hopkins, and Kereš 2016).
Primarily, the high-redshift rotational curves of distant galaxies shoe a solid-body rise within the turnover and inner regions of the constant circular velocity in the outer parts.
Moreover, the idea of dark matter does not affect or modify the gravitational laws within the distant and near galaxies.
A study by several astronomers in Western Australia indicated they have come to a stumbling conclusion that a murder mystery of cosmic proportions (Kirby, Bullock, Boylan-Kolchin, Kaplinghat, and Cohen 2014).
This can be backed up by several surveys of far-off galaxies that revealed that the process of the massive celestial objects of their gas is common than scientists think (Di Teodoro, Fraternali, and Miller 2016).
Even though scientists are yet to make studies and observations on the topic of dark matter, its existence if often inferred trough is examining their influence on movement and the effects that occur around the galaxies (Oman, Marasco, Navarro, Frenk, Schaye, and Benítez-Llambay 2017).
Moreover, an astronomer in International Center for Radio Astronomy Research (ICRAR) surveyed both the rotational curves of both distant and near galaxies discovering a phenomenon where the galaxies gases are stripped away a way that the scientist could not believe.
Furthermore, a study conducted in 2015 indicated that distant galaxies have little dark matter compared to near galaxies (Anglés-Alcázar, Davé, Özel, and Oppenheimer 2014).
The stars in the distant galaxies have also been found to move much slower than the stars in near galaxies.
This can be attributed to the lack of dark matter to the far-off galaxies (Maiolino, Russell, Fabian, Carniani, Gallagher, Cazzoli, Arribas, Belfiore, Bellocchi, Colina, and Cresci 2017).
In contrast to the distant galaxies, the stars that orbit near the Milky Way and other near galaxies are argued to move much faster as their velocities result from the gravity of stars and gas that is closer to the galactic center (Lelli, McGaugh, and Schombert 2016).
Importantly, the rotation curves of these distant galaxies fall off as turbulent gas bring more material to the inner regions of the galaxies.
The gas and stuff pile up while the dark matter concentrates on the outskirts of the galaxy (McGaugh and Schombert 2015).
Further, winds flowing and explosions of stars from the black holes may drive dark matter from the inner regions of the galaxy.
The dark matter in these distant galaxies can be distributed to a scale of more than hundreds of thousand light-years while the stars and gas in the near galaxies interact in a near scale of tens of thousands light-years (Lelli, McGaugh, Schombert, and Pawlowski 2016).
This explains the reason why astronomers can detect the gas but not the dark matter.
Importantly, the current models of the galaxy formation indicate that ordinary and dark matter intermixed during the early years of the universe (Contini, Epinat, Bouché, Brinchmann, Boogaard, Ventou, Bacon, Richard, Weilbacher, Wisotzki, and Krajnoviç 2016).
This observation led to the belief that dark matter should tug on the regular matter therefore resulting in rotation curves that are flat for distant galaxies (Leisman, Haynes, Janowiecki, Hallenbeck, Józsa, Giovanelli, Adams, Neira, Cannon, Janesh, and Rhode 2017).
The way gas and stars move in distant galaxies is similar to the way gas and stars move in near galaxies.
During his studies scientist, Vera Rubin noticed some anomalies in 1976 (Ho, Martin, Kacprzak, and Churchill).
She identified that at the observable edges of the galaxies there was there would be much less staff.
This implied that there was more matter that what she saw.
Observations have indicated that distant galaxies behave differently compared to the near galaxies.
Much of the difference can be attributed to the difference in the dark matter.
The mass distribution in the near and distant galaxies is determined by the photometric and dynamical methods.
The rotation curves are the primary objects for determining the distribution and dynamical mass in the spiral and Milky Way (Graham, Janz, Penny, Chilingarian, Ciambur, Forbes, and Davies 2016).
Importantly, a study conducted in 2016 has revealed a strong relationship between the amount of visible mass and the motion of the stars in the galaxies (Izotov, Orlitová, Schaerer, Thuan, Verhamme, Guseva, and Worseck 2016).
The study has some contradicting results as it indicated that the stars orbiting and the outer regions of the galaxy move at the same speed as the ones near the center.
Moreover, the study suggested that the gravitational glue that is provided by the dark matter plays a crucial role in keeping the stars together (Oman, Marasco, Navarro, Frenk, Schaye, and Benítez-Llambay 2017).
These results were consistent for both near and distant galaxies.
Results from a study conducted by Foot 2016 in 153 galaxies indicated that varying rotations, brightness, and sizes and found that the acceleration can be expressed as a simple function of visible matter within the galaxies (Gazak, Kudritzki, Evans, Patrick, Davies, Bergemann, Plez, Bresolin, Bender, Wegner, and Bonanos 2015).
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