Origin of the Hubble sequence

Nature ◽  
1989 ◽  
Vol 337 (6208) ◽  
pp. 600-601 ◽  
Author(s):  
M. G. Edmunds
Keyword(s):  
Hubble Sequence

scholarly journals A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations

2019 ◽  
Vol 489 (1) ◽  
pp. 842-854 ◽  
Author(s):  
Dandan Xu ◽  
Ling Zhu ◽  
Robert Grand ◽  
Volker Springel ◽  
Shude Mao ◽  
...  
Keyword(s):  
Observational Data ◽  
Mass Range ◽  
Stellar Mass ◽  
Model Uncertainties ◽  
Massive Galaxies ◽  
Hubble Sequence ◽  
Galaxy Sample ◽  
The Mean ◽  
Stellar Orbit

ABSTRACT Motivated by the recently discovered kinematic ‘Hubble sequence’ shown by the stellar orbit-circularity distribution of 260 CALIFA galaxies, we make use of a comparable galaxy sample at z = 0 with a stellar mass range of $M_{*}/\mathrm{M}_{\odot }\in [10^{9.7},\, 10^{11.4}]$ selected from the IllustrisTNG simulation and study their stellar orbit compositions in relation to a number of other fundamental galaxy properties. We find that the TNG100 simulation broadly reproduces the observed fractions of different orbital components and their stellar mass dependences. In particular, the mean mass dependences of the luminosity fractions for the kinematically warm and hot orbits are well reproduced within model uncertainties of the observed galaxies. The simulation also largely reproduces the observed peak and trough features at $M_{*}\approx 1\rm {-}2\times 10^{10}\, \mathrm{M}_{\odot }$ in the mean distributions of the cold- and hot-orbit fractions, respectively, indicating fewer cooler orbits and more hotter orbits in both more- and less-massive galaxies beyond such a mass range. Several marginal disagreements are seen between the simulation and observations: the average cold-orbit (counter-rotating) fractions of the simulated galaxies below (above) $M_{*}\approx 6\times 10^{10}\, \mathrm{M}_{\odot }$ are systematically higher than the observational data by $\lesssim 10{{\ \rm per\ cent}}$ (absolute orbital fraction); the simulation also seems to produce more scatter for the cold-orbit fraction and less so for the non-cold orbits at any given galaxy mass. Possible causes that stem from the adopted heating mechanisms are discussed.

scholarly journals Molecular Gas Distribution in Barred and Nonbarred Galaxies along the Hubble Sequence

2008 ◽  
Vol 178 (2) ◽  
pp. 225-246 ◽  
Author(s):  
S. Komugi ◽  
Y. Sofue ◽  
K. Kohno ◽  
H. Nakanishi ◽  
S. Onodera ◽  
...  
Keyword(s):  
Molecular Gas ◽  
Gas Distribution ◽  
Hubble Sequence

Hubble Sequence: New Light on Galaxy Evolution

Nature ◽  
1970 ◽  
Vol 226 (5251) ◽  
pp. 1091-1092
Author(s):  
Keyword(s):  
Galaxy Evolution ◽  
Hubble Sequence

Clues on the Hubble Sequence Formation from Self-Consistent Hydrodynamical Simulations

2003 ◽  
pp. 103-106
Author(s):  
R. Domínguez-Tenreiro ◽  
A. Serna ◽  
A. Sáiz ◽  
M. M. Sierra-Glez. De Buitrago
Keyword(s):  
Hubble Sequence ◽  
Self Consistent ◽  
Hydrodynamical Simulations

scholarly journals 9.18. Galactic winds in active galaxies

1998 ◽  
Vol 184 ◽  
pp. 417-418 ◽  
Author(s):  
S. Veilleux ◽  
J. Bland-Hawthorn ◽  
G. Cecil ◽  
P. Shopbell
Keyword(s):  
Absorption Line ◽  
Galaxy Formation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Active Galaxies ◽  
Large Scale Circulation ◽  
X Ray ◽  
Hubble Sequence ◽  
Galactic Winds ◽  
X Ray Background

The effects of large-scale galactic winds in active galaxies may be far-reaching. It has been suggested that the Hubble sequence can be understood in terms of a galaxy's greater ability to sustain winds with increasing bulge-to-disk ratio. The large-scale circulation of gas associated with these galactic winds might help explain the mass-metallicity relation between galaxies and the metallicity-radius relation within galaxies. Galactic winds probably contribute non-negligibly to the cosmic X-ray background and may be involved in the quasar absorption-line phenomenon. The cosmological implications of the wind phenomenon have been widely explored in the context of proto-galaxies and quasars. The extremely energetic galactic winds that were likely associated with galaxy formation almost certainly played a key role in heating and ionizing the intergalactic medium at high redshifts and may have created the seeds for the large-scale structure we see today.

scholarly journals A comprehensive examination of the optical morphologies of 719 isolated galaxies in the AMIGA sample

2019 ◽  
Vol 488 (2) ◽  
pp. 2175-2189 ◽  
Author(s):  
Ronald J Buta ◽  
Lourdes Verdes-Montenegro ◽  
Ancor Damas-Segovia ◽  
Michael Jones ◽  
Javier Blasco ◽  
...  
Keyword(s):  
Local Environment ◽  
Far Infrared ◽  
Point Of View ◽  
Sloan Digital Sky Survey ◽  
Infrared Excess ◽  
Hubble Sequence ◽  
Isolated Galaxies ◽  
Grand Design ◽  
Kolmogorov Smirnov ◽  
Variety Classification

Abstract Using images from Sloan Digital Sky Survey Data Release 8, we have re-examined the morphology of 719 galaxies from the Analysis of the interstellar Medium in Isolated GAlaxies (AMIGA) project, a sample consisting of the most isolated galaxies that have yet been identified. The goal is to further improve the classifications of these galaxies by examining them in the context of the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system, which includes recognition of features that go beyond the original de Vaucouleurs point of view. Our results confirm previous findings that isolated galaxies are found across the complete revised Hubble sequence, with intermediate- to late-type (Sb-Sc) spirals being relatively more common. Elmegreen Arm Classifications are also presented, and show that more than 50 per cent of the 514 spirals in the sample for which an arm class (AC) could be judged are grand design (AC 8,9,12). The visual bar fraction for the sample is ≈50 per cent, but only 16 per cent are classified as strongly barred (SB). The dominant family classification is SA (non-barred), the dominant inner variety classification is (s) (pure spiral), and the dominant outer variety classification is no outer ring, pseudo-ring, or lens. The Kolmogorov–Smirnov test is used to check for potential biases in the morphological interpretations, and for any possible relation between rings, bars, and ACs with local environment and far-infrared excess. The connection between morphology and stellar mass is also examined for a subset of the sample.

scholarly journals Photometric and kinematic properties of disky elliptical galaxies

1993 ◽  
Vol 153 ◽  
pp. 425-426
Author(s):  
Cecilia Scorza
Keyword(s):  
Fourier Expansion ◽  
Major Axis ◽  
Elliptical Galaxies ◽  
Continuous Transition ◽  
X Ray ◽  
Hubble Sequence ◽  
Kinematic Properties

New insights in the structure of elliptical galaxies have been obtained indicating the presence of faint stellar disks in some of these systems. Clear correlations between the isophotal shapes, the kinematic, radio and X-ray properties of disky E's were found, suggesting that these galaxies form together with SO's a continuous transition of D/B ratio in the Hubble sequence (Bender et al. 1989). The isophotal shapes of these galaxies have been quantified by the fourth cosine coefficient a4 of the Fourier expansion of the deviations from perfect ellipses, which yields positive values when the isophotes are pointed along the major axis (Carter 1987, Lauer 1985, Jedrzewski 1987, Bender and Möllenhoff 1987).

scholarly journals Hubble Sequence as a Temporal Evolution Sequence

1999 ◽  
Vol 186 ◽  
pp. 491-491
Author(s):  
Xiaolei Zhang
Keyword(s):  
Spiral Galaxies ◽  
Temporal Evolution ◽  
Natural Question ◽  
Late Type ◽  
Present Epoch ◽  
Hubble Sequence ◽  
Deep Survey ◽  
Deep Fields ◽  
The Universe ◽  
Evolution Sequence

The results from Hubble Space Telescope's Medium Deep Survey and Deep Fields indicate that there exists far more blue spiral galaxies at the intermediate and high redshifts than at the present epoch. A natural question therefore is: what have become of these excess late type galaxies as the Universe aged?

scholarly journals Structural diversity of disc galaxies originating in the cold gas inflow from cosmic webs

2020 ◽  
Vol 494 (1) ◽  
pp. L37-L41
Author(s):  
Masafumi Noguchi
Keyword(s):  
High Redshift ◽  
Morphological Diversity ◽  
Structural Diversity ◽  
High Mass ◽  
Cold Flow ◽  
Hubble Sequence ◽  
The Galaxy ◽  
Gas Accretion ◽  
Disc Galaxies ◽  
Cold Gas

ABSTRACT Disc galaxies show a large morphological diversity with varying contribution of three major structural components: thin discs, thick discs, and central bulges. Dominance of bulges increases with the galaxy mass (Hubble sequence), whereas thick discs are more prominent in lower mass galaxies. Because galaxies grow with the accretion of matter, this observed variety should reflect diversity in accretion history. On the basis of the prediction by the cold-flow theory for galactic gas accretion and inspired by the results of previous studies, we put a hypothesis that associates different accretion modes with different components. Namely, thin discs form as the shock-heated hot gas in high-mass haloes gradually accretes to the central part, thick discs grow by the direct accretion of cold gas from cosmic webs when the halo mass is low, and finally bulges form by the inflow of cold gas through the shock-heated gas in high-redshift massive haloes. We show that this simple hypothesis reproduces the mean observed variation of galaxy morphology with the galaxy mass. This scenario also predicts that thick discs are older and poorer in metals than thin discs, in agreement with the currently available observations.

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