Method of wave equations exact solutions in studies of neutrinos
... and cosmology, where strong electromagnetic fields and dense matter may play an important role. The aim of this paper is to present a rather powerful method in investigations of different phenomena that can appear when neutrinos are moving in the background matter [1, 2]. In addition, we also demons ...
... and cosmology, where strong electromagnetic fields and dense matter may play an important role. The aim of this paper is to present a rather powerful method in investigations of different phenomena that can appear when neutrinos are moving in the background matter [1, 2]. In addition, we also demons ...
Galaxies
... underlying dark matter. We have started to understand how baryonic gas within the dark matter halos cools and collapses to form stars, and how the energy from star formation can feed back into the surrounding gas and regulate subsequent star formation. However, at a fundamental level we still lack a ...
... underlying dark matter. We have started to understand how baryonic gas within the dark matter halos cools and collapses to form stars, and how the energy from star formation can feed back into the surrounding gas and regulate subsequent star formation. However, at a fundamental level we still lack a ...
Module 11.1.1: Galaxies: Morphology and the Hubble Sequence
... actually older, are called early types, according to Hubble. And spiral galaxies, which on average are younger, are called late types. It's a little confusing but it's just the way ...
... actually older, are called early types, according to Hubble. And spiral galaxies, which on average are younger, are called late types. It's a little confusing but it's just the way ...
The VLT LEGA-C Spectroscopic Survey: The Physics of Galaxies at
... stellar content of galaxies and their mass, ongoing star formation, internal structure, environment, and nuclear activity can be explored at large look-back time for the first time by the LEGA-C dataset. The LEGA-C survey can play a crucial and unique role in the context of previous, current, and up ...
... stellar content of galaxies and their mass, ongoing star formation, internal structure, environment, and nuclear activity can be explored at large look-back time for the first time by the LEGA-C dataset. The LEGA-C survey can play a crucial and unique role in the context of previous, current, and up ...
distance
... to understand them? (lessons learned from stars about this?) – measure properties • If you know distance and you measure flux you can figure out total luminosity • Distance measurements that work to other galaxies: Cepheids — BRIGHT! Can see them out to ~40 Mpc ...
... to understand them? (lessons learned from stars about this?) – measure properties • If you know distance and you measure flux you can figure out total luminosity • Distance measurements that work to other galaxies: Cepheids — BRIGHT! Can see them out to ~40 Mpc ...
Clusters as laboratories for the study of galaxy evolution
... formation. From the lack of evolution in the shape of the bright end of the K-band LF we can however deduce that if the massive ellipticals in clusters formed through merging, it took place at higher redshifts (z >> 1 ) than is predicted by current semianalytical models.” p.s. van Dokkum and Stanfor ...
... formation. From the lack of evolution in the shape of the bright end of the K-band LF we can however deduce that if the massive ellipticals in clusters formed through merging, it took place at higher redshifts (z >> 1 ) than is predicted by current semianalytical models.” p.s. van Dokkum and Stanfor ...
Properties of simulated Milky Way-mass galaxies in loose group and
... findings (Balogh et al. 2004a; Martínez et al. 2008). The independence of metallicity on large-scale environment is perhaps refuted by the findings of Ellison et al. (2009) where a residual metallicity-environment effect is found observationally even after the dependence on luminosity and colour have ...
... findings (Balogh et al. 2004a; Martínez et al. 2008). The independence of metallicity on large-scale environment is perhaps refuted by the findings of Ellison et al. (2009) where a residual metallicity-environment effect is found observationally even after the dependence on luminosity and colour have ...
Effects of color superconductivity on the nucleation of quark matter in
... in the value of Nc is expected to be within one or two orders of magnitude. In any case, all the qualitative features of our scenario will be not affected by the uncertainty in the value of Nc . In order to explore the astrophysical implications of the nucleation, we introduce the concept of critical ...
... in the value of Nc is expected to be within one or two orders of magnitude. In any case, all the qualitative features of our scenario will be not affected by the uncertainty in the value of Nc . In order to explore the astrophysical implications of the nucleation, we introduce the concept of critical ...
Building galaxies Hunt, Leslie Kipp
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...
The effect of the environment on the HI scaling relations
... Arecibo SDSS Survey (GASS; Catinella et al. 2010), a targeted survey of a volume-limited sample of ∼1000 massive galaxies (M∗ >1010 M⊙ ). Catinella et al. (2010) used the first GASS data release to quantify the main scaling relations linking the Hi-to-stellar mass ratio to stellar mass, stellar mass ...
... Arecibo SDSS Survey (GASS; Catinella et al. 2010), a targeted survey of a volume-limited sample of ∼1000 massive galaxies (M∗ >1010 M⊙ ). Catinella et al. (2010) used the first GASS data release to quantify the main scaling relations linking the Hi-to-stellar mass ratio to stellar mass, stellar mass ...
Satellite galaxies in hydrodynamical simulations of Milky Way sized
... Collisionless simulations of the CDM cosmology predict a plethora of dark matter substructures in the halos of Milky Way sized galaxies, yet the number of known luminous satellites galaxies is very much smaller, a discrepancy that has become known as the ‘missing satellite problem’. The most massive ...
... Collisionless simulations of the CDM cosmology predict a plethora of dark matter substructures in the halos of Milky Way sized galaxies, yet the number of known luminous satellites galaxies is very much smaller, a discrepancy that has become known as the ‘missing satellite problem’. The most massive ...
the inclination of the dwarf irregular galaxy
... Since the rotation velocity depends on the adopted inclination as 1/ sin i, uncertainties in the inclination are more important in galaxies with low inclinations (i.e. more face-on galaxies). In this paper, we suggest an indirect method to provide upper limits on i in galaxies with low inclinations, ...
... Since the rotation velocity depends on the adopted inclination as 1/ sin i, uncertainties in the inclination are more important in galaxies with low inclinations (i.e. more face-on galaxies). In this paper, we suggest an indirect method to provide upper limits on i in galaxies with low inclinations, ...
Chapter 7 in the LSST Science Book
... This is one of the most pressing problems of galaxy formation today, and any formulation of galaxy formation must account for this tension. Indeed there are a number of competing suggestions aimed at explaining how thin disks may survive and/or emerge from the expected bombardment. To first order, t ...
... This is one of the most pressing problems of galaxy formation today, and any formulation of galaxy formation must account for this tension. Indeed there are a number of competing suggestions aimed at explaining how thin disks may survive and/or emerge from the expected bombardment. To first order, t ...
Dark matter
Dark matter is a hypothetical kind of matter that cannot be seen with telescopes but would account for most of the matter in the universe. The existence and properties of dark matter are inferred from its gravitational effects on visible matter, on radiation, and on the large-scale structure of the universe. Dark matter has not been detected directly, making it one of the greatest mysteries in modern astrophysics.Dark matter neither emits nor absorbs light or any other electromagnetic radiation at any significant level. According to the Planck mission team, and based on the standard model of cosmology, the total mass–energy of the known universe contains 4.9% ordinary matter, 26.8% dark matter and 68.3% dark energy. Thus, dark matter is estimated to constitute 84.5% of the total matter in the universe, while dark energy plus dark matter constitute 95.1% of the total mass–energy content of the universe.Astrophysicists hypothesized the existence of dark matter to account for discrepancies between the mass of large astronomical objects determined from their gravitational effects, and their mass as calculated from the observable matter (stars, gas, and dust) that they can be seen to contain. Their gravitational effects suggest that their masses are much greater than the observable matter survey suggests. Dark matter was postulated by Jan Oort in 1932, albeit based upon insufficient evidence, to account for the orbital velocities of stars in the Milky Way. In 1933, Fritz Zwicky was the first to use the virial theorem to infer the existence of unseen matter, which he referred to as dunkle Materie 'dark matter'. More robust evidence from galaxy rotation curves was discovered by Horace W. Babcock in 1939, but was not attributed to dark matter. The first hypothesis to postulate ""dark matter"" based upon robust evidence was formulated by Vera Rubin and Kent Ford in the 1960s–1970s, using galaxy rotation curves. Subsequently, many other observations have indicated the presence of dark matter in the universe, including gravitational lensing of background objects by galaxy clusters such as the Bullet Cluster, the temperature distribution of hot gas in galaxies and clusters of galaxies and, more recently, the pattern of anisotropies in the cosmic microwave background. According to consensus among cosmologists, dark matter is composed primarily of a not yet characterized type of subatomic particle.The search for this particle, by a variety of means, is one of the major efforts in particle physics today.Although the existence of dark matter is generally accepted by the mainstream scientific community, some alternative theories of gravity have been proposed, such as MOND and TeVeS, which try to account for the anomalous observations without requiring additional matter. However, these theories cannot account for the properties of galaxy clusters.