scholarly journals Predictions forHerschelfrom Λ-cold dark matter: unveiling the cosmic star formation history

2010 ◽  
Author(s):  
C. G. Lacey ◽  
C. M. Baugh ◽  
C. S. Frenk ◽  
A. J. Benson ◽  
A. Orsi ◽  
...  
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Cold Dark Matter ◽  
Star Formation History ◽  
Formation History

Star Formation History and Stellar Metallicity Distribution in a Cold Dark Matter Universe

2001 ◽  
Vol 558 (2) ◽  
pp. 497-504 ◽  
Author(s):  
Kentaro Nagamine ◽  
Masataka Fukugita ◽  
Renyue Cen ◽  
Jeremiah P. Ostriker
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Cold Dark Matter ◽  
Star Formation History ◽  
Formation History ◽  
Metallicity Distribution

scholarly journals Origin of the galaxy morphology

2003 ◽  
Vol 208 ◽  
pp. 431-432
Author(s):  
N. Nakasato
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
High Resolution ◽  
Cold Dark Matter ◽  
Star Formation History ◽  
The Galaxy ◽  
Particle Hydrodynamics ◽  
History Of ◽  
Analytic Models ◽  
Galaxy Morphology

In the current most plausible Cold Dark Matter (CDM) cosmology, larger halos increase their mass by the progressive mergers of smaller clumps. Due to these progressive merger events, galaxies have formed and evolved. Such merger events could trigger star bursts depending on mass of a merging object. In other words, star formation history reflects the strength of the interaction between a galaxy and merging objects. Also, a several merger events strongly affect the development of the morphology of galaxies as assumed in semi-analytic models. In the most advanced semi-analytic models, N-body simulations of dark matter particles are used to obtain the merging history of halos. By combining the description of radiative cooling, hydrodynamics and star formation with the obtained merging history, such models successfully have explained the various qualitative predictions. Here, we show the results of similar approach but using a fullly numerical model. In contrast to the semi-analytic models, we use our high resolution Smoothed Particle Hydrodynamics (SPH) models. With our SPH code, we try to tackle the problem of the galaxy morphology. We have done a several handful high-resolution SPH simulations and analyzed the merging history of such models. Accordingly, we can see the relation between the obtained morphology and the merging history or other physical properties of the model.

scholarly journals Star formation history from the cosmic infrared background anisotropies

2018 ◽  
Vol 614 ◽  
pp. A39 ◽  
Author(s):  
A. S. Maniyar ◽  
M. Béthermin ◽  
G. Lagache
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Star Formation History ◽  
Dark Matter Halo ◽  
Model Parameters ◽  
Formation History ◽  
Infrared Background ◽  
Cosmic Infrared Background

We present a linear clustering model of cosmic infrared background (CIB) anisotropies at large scales that is used to measure the cosmic star formation rate density up to redshift 6, the effective bias of the CIB, and the mass of dark matter halos hosting dusty star-forming galaxies. This is achieved using the Planck CIB auto- and cross-power spectra (between different frequencies) and CIB × CMB (cosmic microwave background) lensing cross-spectra measurements, as well as external constraints (e.g. on the CIB mean brightness). We recovered an obscured star formation history which agrees well with the values derived from infrared deep surveys and we confirm that the obscured star formation dominates the unobscured formation up to at least z = 4. The obscured and unobscured star formation rate densities are compatible at 1σ at z = 5. We also determined the evolution of the effective bias of the galaxies emitting the CIB and found a rapid increase from ~0.8 at z = 0 to ~8 at z = 4. At 2 < z < 4, this effective bias is similar to that of galaxies at the knee of the mass functions and submillimetre galaxies. This effective bias is the weighted average of the true bias with the corresponding emissivity of the galaxies. The halo mass corresponding to this bias is thus not exactly the mass contributing the most to the star formation density. Correcting for this, we obtained a value of log(Mh/M⊙) = 12.77−0.125+0.128 for the mass of the typical dark matter halo contributing to the CIB at z = 2. Finally, using a Fisher matrix analysis we also computed how the uncertainties on the cosmological parameters affect the recovered CIB model parameters, and find that the effect is negligible.

scholarly journals An empirical model for the star formation history in dark matter haloes

2014 ◽  
Vol 439 (2) ◽  
pp. 1294-1312 ◽  
Author(s):  
Zhankui Lu ◽  
H. J. Mo ◽  
Yu Lu ◽  
Neal Katz ◽  
Martin D. Weinberg ◽  
...  
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Empirical Model ◽  
Star Formation History ◽  
Formation History

scholarly journals Star Formation History of Dwarf Galaxies in Cosmological Hydrodynamic Simulations

2010 ◽  
Vol 2010 ◽  
pp. 1-5 ◽  
Author(s):  
Kentaro Nagamine
Keyword(s):  
Star Formation ◽  
Large Scale ◽  
Cold Dark Matter ◽  
Dwarf Galaxies ◽  
Star Formation History ◽  
Hydrodynamic Simulations ◽  
Cosmological Context ◽  
Cold Dark Matter Model ◽  
Formation History ◽  
History Of

We examine the past and current work on the star formation (SF) histories of dwarf galaxies in cosmological hydrodynamic simulations. The results obtained from different numerical methods are still somewhat mixed, but the differences are understandable if we consider the numerical and resolution effects. It remains a challenge to simulate the episodic nature of SF history in dwarf galaxies at late times within the cosmological context of a cold dark matter model. More work is needed to solve the mysteries of SF history of dwarf galaxies employing large-scale hydrodynamic simulations on the next generation of supercomputers.

scholarly journals Galaxy Interactions, Star Formation History, and Bulgeless Galaxies

2008 ◽  
Vol 4 (S254) ◽  
pp. 67-72 ◽  
Author(s):  
Shardha Jogee
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Hierarchical Models ◽  
Star Formation History ◽  
Galaxy Interactions ◽  
Formation History ◽  
History Of ◽  
Interaction History ◽  
The Impact

AbstractHierarchical ΛCDM models provide a successful paradigm for the growth of dark matter on large scales, but they face important challenges in predicting how the baryonic components of galaxies evolve. I present constraints on two aspects of this evolution: (1) The interaction history of galaxies over the last 7 Gyr and the impact of interactions on their star formation properties, based on Jogeeet al. (2008a, b); (2) Constraints on the origin of bulges in hierarchical models and the challenge posed in accounting for galaxies with low bulge-to-total ratios, based on Weinzirl, Jogee, Khochar, Burkert, & Kormendy (2008, hereafter WJKBK08).

scholarly journals The chemical evolution of dwarf starburst galaxies

1999 ◽  
Vol 193 ◽  
pp. 679-691
Author(s):  
Francesca Matteucci ◽  
Annibale D'Ercole
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Chemical Evolution ◽  
Starburst Galaxies ◽  
Star Formation History ◽  
H Ii Regions ◽  
Dark Matter Halos ◽  
Star Formation Activity ◽  
Irregular Galaxies ◽  
Formation History

We will review the most popular models for the chemical evolution of some starburst galaxies, in particular dwarf irregular galaxies. These galaxies are relatively simple and unevolved objects with low metallicities and large gas contents, suggesting that they are either young or have undergone discontinuous star formation activity. Some dwarf irregulars are starburst galaxies currently experiencing an intense star formation event and they are known as blue compact galaxies or extragalactic H II regions. We will discuss the effects of the presence of dark matter halos together with stellar energetics (stellar winds and supernovae) on the development of a galactic wind in these systems. Particular emphasis will be given to the role of massive stars in driving the thermal and chemical evolution of the gas, in particular to type II supernovae. A comparison between different model predictions for abundances and abundance ratios will be used to impose constraints on the star formation history and on the amount of dark matter, which we found to be extremely important in these systems.

scholarly journals No cores in dark matter-dominated dwarf galaxies with bursty star formation histories

2019 ◽  
Vol 486 (4) ◽  
pp. 4790-4804 ◽  
Author(s):  
Sownak Bose ◽  
Carlos S Frenk ◽  
Adrian Jenkins ◽  
Azadeh Fattahi ◽  
Facundo A Gómez ◽  
...  
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Cold Dark Matter ◽  
Dwarf Galaxies ◽  
Local Environment ◽  
Temporal Variations ◽  
Star Formation History ◽  
Constant Density ◽  
Core Formation ◽  
Star Formation Histories

ABSTRACT Measurements of the rotation curves of dwarf galaxies are often interpreted as requiring a constant density core at the centre, at odds with the ‘cuspy’ inner profiles predicted by N-body simulations of cold dark matter (CDM) haloes. It has been suggested that this conflict could be resolved by fluctuations in the inner gravitational potential caused by the periodic removal of gas following bursts of star formation. Earlier work has suggested that core formation requires a bursty and extended star formation history (SFH). Here we investigate the structure of CDM haloes of dwarf galaxies ($M_{{\rm DM}} \sim 10^9\!-\!5\times 10^{10}\, {\rm M}_\odot$) formed in the apostle (‘A Project of Simulating the Local Environment’) and auriga cosmological hydrodynamic simulations. Our simulations have comparable or better resolution than others that make cores ($M_{{\rm gas}} \sim 10^4\, {\rm M}_\odot$, gravitational softening ∼150 pc). Yet, we do not find evidence of core formation at any mass or any correlation between the inner slope of the DM density profile and temporal variations in the SFH. apostle and auriga dwarfs display a similar diversity in their cumulative SFHs to available data for Local Group dwarfs. Dwarfs in both simulations are DM-dominated on all resolved scales at all times, likely limiting the ability of gas outflows to alter significantly the central density profiles of their haloes. We conclude that recurrent bursts of star formation are not sufficient to cause the formation of cores, and that other conditions must also be met for baryons to be able to modify the central DM cusp.

Sign in / Sign up

Export Citation Format

Share Document