Massive neutrinos and galaxy formation

1981 ◽  
Vol 243 ◽  
pp. L1 ◽  
Author(s):  
F. R. Klinkhamer ◽  
C. A. Norman
Keyword(s):  
Galaxy Formation ◽  
Massive Neutrinos

Galaxy formation with cosmic strings and massive neutrinos

1988 ◽  
Vol 328 ◽  
pp. 23 ◽  
Author(s):  
Edmund Bertschinger ◽  
Paul N. Watts
Keyword(s):  
Galaxy Formation ◽  
Cosmic Strings ◽  
Massive Neutrinos

Erratum - Massive Neutrinos and Galaxy Formation

1981 ◽  
Vol 245 ◽  
pp. L97 ◽  
Author(s):  
F. R. Klinkhamer ◽  
C. A. Norman
Keyword(s):  
Galaxy Formation ◽  
Massive Neutrinos

Massive neutrinos and the pancake theory of galaxy formation

1984 ◽  
Vol 281 ◽  
pp. L13 ◽  
Author(s):  
R. Schaeffer ◽  
J. Silk
Keyword(s):  
Galaxy Formation ◽  
Massive Neutrinos

scholarly journals The BAHAMAS project: the CMB–large-scale structure tension and the roles of massive neutrinos and galaxy formation

2018 ◽  
Vol 476 (3) ◽  
pp. 2999-3030 ◽  
Author(s):  
Ian G McCarthy ◽  
Simeon Bird ◽  
Joop Schaye ◽  
Joachim Harnois-Deraps ◽  
Andreea S Font ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Bahamas ◽  
Massive Neutrinos

scholarly journals Cosmological Streaming Velocities & Large-Scale Density Maxima

1988 ◽  
Vol 130 ◽  
pp. 551-551
Author(s):  
J. A. Peacock ◽  
S.L. Lumsden ◽  
A.F. Heavens
Keyword(s):  
Galaxy Formation ◽  
Large Scale ◽  
Power Index ◽  
Density Variation ◽  
Statistical Testing ◽  
Microwave Background ◽  
Peculiar Velocities ◽  
Density Perturbations ◽  
Streaming Velocity ◽  
Massive Neutrinos

We consider the statistical testing of models for galaxy formation against the observed peculiar velocities on 10–100 Mpc scales (the Rubin-Ford effect). If we assume that observers are likely to be sited near maxima in the primordial field of density perturbations (Peacock & Heavens 1985: MNRAS 217, 805; Bardeen et al. 1986: Ap. J. 304, 15), then the observed filtered velocity field will be biased to low values by comparison with a point selected at random. The streaming-velocity data constrain models for galaxy formation with large-scale damping (adiabatic perturbations) to have a damping length close to the Rubin-Ford scale (rD ∼ 20 h−1 Mpc) and are mildly non-linear (Ω0.6 σo ∼1), where σo is the current fractional rms density variation. The Figure illustrates the regions of parameter space allowed at the 10,5,1 & 0.1% levels; the results are nearly independent of n, the power index of the primordial spectrum. Thus, both purely baryonic universes and universes dominated by massive neutrinos can account for the observed velocities, provided 0.1 ≲ Ω ≲ 1. In particular, the canonical Ω = 1 massive-neutrino model yields the required velocities quite naturally (in contradiction to the conclusion of Vittorio et al. 1986: Nature 323, 132), while not violating the constraints on the isotropy of the microwave background. For further details of this work, see Peacock, Lumsden & Heavens 1987: MNRAS in press.

The Metallicity Distribution in the Halo Stars of NGC 5128: Implications for Galaxy Formation

1999 ◽  
Vol 117 (2) ◽  
pp. 855-867 ◽  
Author(s):  
Gretchen L. H. Harris ◽  
William E. Harris ◽  
Gregory B. Poole
Keyword(s):  
Galaxy Formation ◽  
Halo Stars ◽  
Metallicity Distribution

scholarly journals Galaxy Formation: Some Comparisons between Theory and Observation

1983 ◽  
Vol 100 ◽  
pp. 391-399 ◽  
Author(s):  
S. Michael Fall
Keyword(s):  
Galaxy Formation ◽  
Total Mass ◽  
Virial Theorem ◽  
Velocity Dispersion ◽  
Rotation Velocity ◽  
Morphological Type ◽  
Fundamental Parameter ◽  
Mass Ratio ◽  
First Approximation ◽  
Type Form

Before theoretical ideas in this subject can be compared with observational data, it is necessary to consider the properties of galaxies that are likely to be relics of their formation. Most astronomers would agree that the list of important parameters should be headed by the total mass M, energy E and angular momentum J. Next on the list should probably be the relative contributions to these quantities from the disc and bulge components of galaxies and denoted D/B for the mass ratio. They can be estimated from the median (i.e. half-mass) radius R, velocity dispersion σ and rotation velocity v of each component, either through the virial theorem or through the luminosity L and an assumed value of M/L. As a first approximation, it is reasonable to suppose that galaxies of a given disc-to-bulge ratio or morphological type form a sequence with mass as the fundamental parameter. The comparison of theory with data is further simplified by considering the extreme cases of ellipticals, with D/B << 1, and late-type spirals, with D/B >> 1. The approach outlined below is to explore the consequences of relaxing in succession the constraints that E, J and M be conserved during the collapse of proto-galaxies. In this article I concentrate on theories that are based on some form of hierarchical clustering because the pancake and related theories are not yet refined enough for a detailed confrontation with observations.

scholarly journals Detecting Cold Dark Matter Candidates

1987 ◽  
Vol 117 ◽  
pp. 490-490
Author(s):  
A. K. Drukier ◽  
K. Freese ◽  
D. N. Spergel
Keyword(s):  
Dark Matter ◽  
Cold Dark Matter ◽  
Galactic Halo ◽  
Dark Matter Particle ◽  
Low Energy ◽  
The Sun ◽  
Background Rate ◽  
System Noise ◽  
Weakly Interacting ◽  
Massive Neutrinos

We consider the use of superheated superconducting colloids as detectors of weakly interacting galactic halo candidate particles (e.g. photinos, massive neutrinos, and scalar neutrinos). These low temperature detectors are sensitive to the deposition of a few hundreds of eV's. The recoil of a dark matter particle off of a superheated superconducting grain in the detector causes the grain to make a transition to the normal state. Their low energy threshold makes this class of detectors ideal for detecting massive weakly interacting halo particles.We discuss realistic models for the detector and for the galactic halo. We show that the expected count rate (≈103 count/day for scalar and massive neutrinos) exceeds the expected background by several orders of magnitude. For photinos, we expect ≈1 count/day, more than 100 times the predicted background rate. We find that if the detector temperature is maintained at 50 mK and the system noise is reduced below 5 × 10−4 flux quanta, particles with mass as low as 2 GeV can be detected. We show that the earth's motion around the Sun can produce a significant annual modulation in the signal.

scholarly journals Is there enough star formation in simulated protoclusters?

2020 ◽  
Vol 501 (2) ◽  
pp. 1803-1822
Author(s):  
Seunghwan Lim ◽  
Douglas Scott ◽  
Arif Babul ◽  
David J Barnes ◽  
Scott T Kay ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Formation ◽  
Star Formation History ◽  
Test Case ◽  
Numerical Resolution ◽  
Formation History ◽  
Order Of Magnitude ◽  
History Of ◽  
Hydrodynamical Simulations ◽  
Formation Efficiency

ABSTRACT As progenitors of the most massive objects, protoclusters are key to tracing the evolution and star formation history of the Universe, and are responsible for ${\gtrsim }\, 20$ per cent of the cosmic star formation at $z\, {\gt }\, 2$. Using a combination of state-of-the-art hydrodynamical simulations and empirical models, we show that current galaxy formation models do not produce enough star formation in protoclusters to match observations. We find that the star formation rates (SFRs) predicted from the models are an order of magnitude lower than what is seen in observations, despite the relatively good agreement found for their mass-accretion histories, specifically that they lie on an evolutionary path to become Coma-like clusters at $z\, {\simeq }\, 0$. Using a well-studied protocluster core at $z\, {=}\, 4.3$ as a test case, we find that star formation efficiency of protocluster galaxies is higher than predicted by the models. We show that a large part of the discrepancy can be attributed to a dependence of SFR on the numerical resolution of the simulations, with a roughly factor of 3 drop in SFR when the spatial resolution decreases by a factor of 4. We also present predictions up to $z\, {\simeq }\, 7$. Compared to lower redshifts, we find that centrals (the most massive member galaxies) are more distinct from the other galaxies, while protocluster galaxies are less distinct from field galaxies. All these results suggest that, as a rare and extreme population at high z, protoclusters can help constrain galaxy formation models tuned to match the average population at $z\, {\simeq }\, 0$.

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