The angular momentum-mass relation: a fundamental law from dwarf irregulars to massive spirals

Posti, Lorenzo; Fraternali, Filippo; Teodoro, Enrico M. Di; Pezzulli, Gabriele

doi:10.1051/0004-6361/201833091

Cited by 98 publications

(243 citation statements)

References 48 publications

Supporting

Mentioning

205

Contrasting

Order By: Relevance

“…In this case the observed scatter in R e would drive the one in j st ar , making the argument above circular. However, the constraints on the scatter in j st ar by Posti et al (2018b) quoted above, are found by direct integration of the observed rotation curves in the SPARC sample (Lelli et al 2016). It is also intriguing that, to first order, eq.…”

Section: Is the Mmw Model Consistent With Observed Ltgs Scaling Relatmentioning

confidence: 83%

Galaxy sizes and the galaxy–halo connection – I. The remarkable tightness of the size distributions

Zanisi

Shankar

Lapi

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The mass and structural assembly of galaxies is a matter of intense debate. Current theoretical models predict the existence of a linear relationship between galaxy size (R e ) and the host dark matter halo virial radius (R h ). By making use of semi-empirical models compared to the size distributions of central galaxies from the Sloan Digital Sky Survey, we provide robust constraints on the normalization and scatter of the R e − R h relation. We explore the parameter space of models in which the R e − R h relation is mediated by either the spin parameter or the concentration of the host halo, or a simple constant the nature of which is in principle unknown. We find that the data require extremely tight relations for both early-type and latetype galaxies (ETGs,LTGs), especially for more massive galaxies. These constraints challenge models based solely on angular momentum conservation, which predict significantly wider distributions of galaxy sizes and no trend with stellar mass, if taken at face value. We discuss physically-motivated alterations to the original models that bring the predictions into better agreement with the data. We argue that the measured tight size distributions of SDSS disk galaxies can be reproduced by semi-empirical models in which the R e − R h connection is mediated by the stellar specific angular momenta j st ar . We find that current cosmological models of galaxy formation broadly agree with our constraints for LTGs, and justify the strong link between R e and j st ar that we propose, however the tightness of the R e − R h relation found in such ab-initio theoretical models for ETGs is in tension with our semi-empirical findings.

show abstract

Section: Is the Mmw Model Consistent With Observed Ltgs Scaling Relatmentioning

confidence: 83%

Galaxy sizes and the galaxy–halo connection – I. The remarkable tightness of the size distributions

Zanisi

Shankar

Lapi

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Note that, for this plot, we do not compute the true specific stellar angular momentum from individual stellar particles, but rather estimate it exactly as for observations (Posti et al 2018). The magenta area with the dashed line shows the best fit of the observational data from Posti et al (2018), while the black line shows the best fit for the data of the models. The same functions as used by Posti et al (2018) are here applied to calculate j star and fit the data,…”

Section: Stellar Angular Momentum and Disk Vs Halo Populations Thin mentioning

confidence: 99%

“…The magenta area with the dashed line shows the best fit of the observational data from Posti et al (2018), while the black line shows the best fit for the data of the models. The same functions as used by Posti et al (2018) are here applied to calculate j star and fit the data,…”

Section: Stellar Angular Momentum and Disk Vs Halo Populations Thin mentioning

confidence: 99%

“…23 and 24 are Eq. 1 and 4 of Posti et al (2018), where Σ star is the stellar surface mass density, V star,rot the stellar rotation curve of the galaxy and α, β are the fit parameters. Posti et al (2018) find their best fit with α = 0.55 ± 0.02 and β = 3.34 ± 0.03, while the best fit for the models here is α = 0.51 ± 0.04 and β = 3.05 ± 0.04.…”

Section: Stellar Angular Momentum and Disk Vs Halo Populations Thin mentioning

confidence: 99%

“…Relation between the specific stellar angular momentum, jstar, of all models with their respective stellar mass, Mstar (Fall relation, computed here as for observations). The magenta area with the dashed line shows the observed data from Posti et al (2018), the symbols for the different models are shown in the legend and the black line (Eq. 24) shows the best fit to the models.…”

Section: 7mentioning

confidence: 99%

See 2 more Smart Citations

The Formation of Exponential Disk Galaxies in MOND

Wittenburg

Kroupa

Famaey

2020

ApJ

View full text Add to dashboard Cite

The formation and evolution of galaxies is highly dependent on the dynamics of stars and gas, which is governed by the underlying law of gravity. To investigate how the formation and evolution of galaxies takes place in Milgromian gravity (MOND), we present full hydrodynamical simulations with the Phantom of Ramses (POR) code. These are the first-ever galaxy formation simulations done in MOND with detailed hydrodynamics, including star formation, stellar feedback, radiative transfer and supernovae. These models start from simplified initial conditions, in the form of isolated, rotating gas spheres in the early Universe. These collapse and form late-type galaxies obeying several scaling relations, which was not a priori expected. The formed galaxies have a compact bulge and a disk with exponentially decreasing surface mass density profiles and scale lengths consistent with observed galaxies, and vertical stellar mass distributions with distinct exponential profiles (thin and thick disk). This work thus shows for the first time that disk galaxies with exponential profiles in both gas and stars are a generic outcome of collapsing gas clouds in MOND. These models have a slight lack of stellar angular momentum because of their somewhat compact stellar bulge, which is connected to the simple initial conditions and the negligible later gas accretion. We also analyse how the addition of more complex baryonic physics changes the main resulting properties of the models and find this to be negligibly so in the Milgromian framework.

show abstract

Probing galaxy evolution through Hi 21-cm emission and absorption: current status and prospects with square kilometre array

et al. 2022

View full text Add to dashboard Cite

One of the major science goals of square kilometre array (SKA) is to understand the role played by atomic hydrogen (Hi) gas in the evolution of galaxies throughout cosmic time. The hyperfine transition line of the hydrogen atom at 21-cm is one of the best tools to detect and study the properties of Hi gas associated with galaxies. In this paper, we review our current understanding of Hi gas and its relationship with galaxies through observations of the 21-cm line both in emission and absorption. In addition, we provide an overview of the Hi science that will be possible with SKA and its precursors and pathfinders, i.e., Hi 21-cm emission and absorption studies of galaxies from nearby to high redshifts that will trace various processes governing galaxy evolution.

show abstract

The angular momentum-mass relation: a fundamental law from dwarf irregulars to massive spirals

Cited by 98 publications

References 48 publications

Galaxy sizes and the galaxy–halo connection – I. The remarkable tightness of the size distributions

Galaxy sizes and the galaxy–halo connection – I. The remarkable tightness of the size distributions

The Formation of Exponential Disk Galaxies in MOND

Probing galaxy evolution through Hi 21-cm emission and absorption: current status and prospects with square kilometre array

Contact Info

Product

Resources

About