A dimensional study of disc galaxies

Hernández, X.; Cervantes-Sodi, B.

doi:10.1111/j.1365-2966.2006.10115.x

Cited by 44 publications

(60 citation statements)

References 65 publications

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“…It is important to note that Kregel et al (2002) did not present the correlation between the disc thickness and the galaxy type for the updated analysis. It was done by Hernandez & Cervantes-Sodi (2006) and is shown in their fig. 7.…”

Section: Discussionmentioning

confidence: 99%

“…Careful examination of fig. 7 in Hernandez & Cervantes-Sodi (2006) shows that the trend is supported by only one point (a galaxy of Sa type). Therefore, we can conclude that the reported correlation is rather poor.…”

Section: Introductionmentioning

confidence: 99%

“…However, Kregel et al (2002) did not use the revised data to discuss the dependence of the ratio z0/h on the morphological type found earlier by de Grijs (1998) on the base of the same sample. It was done by Hernandez & Cervantes-Sodi (2006), who analyzed the data by Kregel et al (2002) and confirmed a diminishing trend of the ratio z0/h while going from the early to late types: the late-type galaxies at the Sc end have thinner discs than the earlier types, on average. Careful examination of fig.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Does the stellar disc flattening depend on the galaxy type?

Mosenkov

Sotnikova

Решетников

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We analyze the dependence of the stellar disc flatness on the galaxy morphological type using 2D decomposition of galaxies from the reliable subsample of the Edge-on Galaxies in SDSS (EGIS) catalogue. Combining these data with the retrieved models of the edge-on galaxies from the Two Micron All Sky Survey (2MASS) and the Spitzer Survey of Stellar Structure in Galaxies (S 4 G) catalogue, we make the following conclusions:(1) The disc relative thickness z 0 /h in the near-and mid-infrared passbands correlates weakly with morphological type and does not correlate with the bulge-to-total luminosity ratio B/T in all studied bands.(2) Applying an 1D photometric profile analysis overestimates the disc thickness in galaxies with large bulges making an illusion of the relationship between the disc flattening and the ratio B/T .(3) In our sample the early-type disc galaxies (S0/a) have both flat and "puffed" discs. The early spirals and intermediate-type galaxies have a large scatter of the disc flatness, which can be caused by the presence of a bar: barred galaxies have thicker stellar discs, on average. On the other hand, the late-type spirals are mostly thin galaxies, whereas irregular galaxies have puffed stellar discs.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Does the stellar disc flattening depend on the galaxy type?

Mosenkov

Sotnikova

Решетников

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…It is possible to estimate λ using the observed characteristics of the disk. Following the method outlined by Hernandez & Cervantes-Sodi (2006), λ can be estimated using:…”

Section: Appendix A: Spin Parameter Of the Halosmentioning

confidence: 99%

3D spectroscopy with VLT/GIRAFFE

Puech¹,

Hammer²,

Lehnert

et al. 2007

A&A

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Context. One of the most outstanding problems related to numerical models of galaxy formation is the so-called "angular momentum catastrophe", i.e., the inability to theoretically explain the high angular momentum observed in local disk galaxies. Aims. We study the evolution of the angular momentum from z ∼ 0.6 to z = 0 to better understand the mechanisms responsible for the large angular momenta of disk galaxies observed today. This study is based on a complete sample of 32, 0.4 ≤ z ≤ 0.75 galaxies observed with FLAMES/GIRAFFE at the VLT. Their kinematics had been classified as rotating disks (11 galaxies), perturbed rotators (7 galaxies), or complex kinematics (14 galaxies). Methods. We have computed the specific angular momentum of disks ( j disk ) and the dynamical support of rotating disks through the V/σ ratio. To study how angular momentum can be acquired dynamically, we compared the properties of distant and local galaxies, as a function of their kinematical class. Results. We find that distant rotating disks have essentially the same properties ( j disk and R d ) as local disks, while distant galaxies with more complex kinematics have a significantly higher scatter in the j disk -V max and R d -V max planes. On average, distant galaxies show lower values of V/σ than local galaxies, the lowest V/σ values being reached by distant galaxies showing perturbed rotation. This can probably be attributed to heating mechanisms at work in distant disks. Conclusions. We found observational evidence for a non-linear random-walk evolution of the angular momentum in galaxies during the past 8 Gyr. The evolution related to galaxies with complex kinematics can be attributed to mergers, but not to (smooth) gas accretion alone. If galaxies observed at intermediate redshift are related to present-day spirals, then our results match the "spiral rebuilding" scenario proposed by Hammer et al. (2005) quite closely.

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“…They confirmed observationally that the mass and angular momentum are strongly correlated with the morphology of galaxies. Hernandez & Cervantes-Sodi (2006) calculated the λ-parameter for two galaxy samples with a total of 337 observed spirals and found that with decreasing bulge-to-disk ratio the spirals have increasing λ-values. In a further study Hernandez et al (2007) investigated a sample of 11,597 spiral and elliptical galaxies from the Sloan Digital Sky Survey (SDSS) and found that ellipticals on average have lower λ-values than spiral galaxies.…”

Section: Introductionmentioning

confidence: 99%

Connecting Angular Momentum and Galactic Dynamics: The Complex Interplay Between Spin, Mass, and Morphology

Teklu

Remus

Dolag

et al. 2015

ApJ

251

253

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The evolution and distribution of the angular momentum of dark matter (DM) halos have been discussed in several studies over the past decades. In particular, the idea arose that angular momentum conservation should allow us to infer the total angular momentum of the entire DM halo from measuring the angular momentum of the baryonic component, which is populating the center of the halo, especially for disk galaxies. To test this idea and to understand the connection between the angular momentum of the DM halo and its galaxy, we use a state-of-the-art, hydrodynamical cosmological simulation taken from the set of Magneticum Pathfinder simulations. Thanks to the inclusion of the relevant physical processes, the improved underlying numerical methods, and high spatial resolution, we successfully produce populations of spheroidal and disk galaxies self-consistently. Thus, we are able to study the dependence of galactic properties on their morphology. We find that(1) the specific angular momentum of stars in disk and spheroidal galaxies as a function of their stellar mass compares well with observational results; (2) the specific angular momentum of the stars in disk galaxies is slightly smaller compared to the specific angular momentum of the cold gas, in good agreement with observations; (3) simulations including the baryonic component show a dichotomy in the specific stellar angular momentum distribution when splitting the galaxies according to their morphological type(this dichotomy can also be seen in the spin parameter, where disk galaxies populate halos with slightly larger spin compared to spheroidal galaxies); (4) disk galaxies preferentially populate halos in which the angular momentum vector of the DM component in the central part shows a better alignment to the angular momentum vector of the entire halo; and (5) the specific angular momentum of the cold gas in disk galaxies is approximately 40% smaller than the specific angular momentum of the total DM halo and shows a significant scatter.

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A dimensional study of disc galaxies

Cited by 44 publications

References 65 publications

Does the stellar disc flattening depend on the galaxy type?

Does the stellar disc flattening depend on the galaxy type?

3D spectroscopy with VLT/GIRAFFE

Connecting Angular Momentum and Galactic Dynamics: The Complex Interplay Between Spin, Mass, and Morphology

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