HyperLEDA. III. The catalogue of extragalactic distances

Макаров, Д. И.; Prugniel, Philippe; Terekhova, Nataliya; Courtois, H. M.; Vauglin, I.

doi:10.1051/0004-6361/201423496

Cited by 823 publications

(742 citation statements)

References 73 publications

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“…Regarding the morphological type criterion, the classification is based on the information provided in the extragalactic database HyperLeda 2 (Makarov et al 2014). However, due to the higher quality of the analysed data over the previously available ones, a visual inspection of the images reconstructed from the MUSE datacubes was done to check the galaxies.…”

Section: Data and Galaxy Samplementioning

confidence: 99%

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The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Sánchez-Menguiano

Sanchez

Pérez

et al. 2018

A&A

146

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We characterised the oxygen abundance radial distribution of a sample of 102 spiral galaxies observed with VLT/MUSE using the O3N2 calibrator. The high spatial resolution of the data allowed us to detect 14345 H ii regions with the same image quality as with photometric data, avoiding any dilution effect. We developed a new methodology to automatically fit the abundance radial profiles, finding that 55 galaxies of the sample exhibit a single negative gradient. The remaining 47 galaxies also display, as well as this negative trend, either an inner drop in the abundances (21), an outer flattening (10), or both (16), which suggests that these features are a common property of disc galaxies. The presence and depth of the inner drop depends on the stellar mass of the galaxies with the most massive systems presenting the deepest abundance drops, while there is no such dependence in the case of the outer flattening. We find that the inner drop appears always around 0.5 r e , while the position of the outer flattening varies over a wide range of galactocentric distances. Regarding the main negative gradient, we find a characteristic slope in the sample of α O/H = − 0.10 ± 0.03 dex/r e . This slope is independent of the presence of bars and the density of the environment. However, when inner drops or outer flattenings are detected, slightly steeper gradients are observed. This suggests that radial motions might play an important role in shaping the abundance profiles. We define a new normalisation scale ('the abundance scale length', r O/H ) for the radial profiles based on the characteristic abundance gradient, with which all the galaxies show a similar position for the inner drop (∼ 0.5 r O/H ) and the outer flattening (∼ 1.5 r O/H ). Finally, we find no significant dependence of the dispersion around the negative gradient with any property of the galaxies, with values compatible with the uncertainties associated with the derivation of the abundances.

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Section: Data and Galaxy Samplementioning

confidence: 99%

“…This information was collected from the extragalactic database HyperLeda (Makarov et al 2014). The galaxies for which such information is not published (16) were not considered in this comparison, but were not excluded from the rest of the analysis.…”

Section: Effects Of Barsmentioning

confidence: 99%

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Sánchez-Menguiano

Sanchez

Pérez

et al. 2018

A&A

146

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“…The integrated Hα profile from data of Chemin et al (2006) has a width at 20% of the maximum Hα peak of 216 km s −1 . Combined with a small disk inclination (20 • , Makarov et al 2014), this implies a massive galaxy with most of rotation velocities greater than 245 km s −1 . This makes it an ideal target to study the structure and kinematics of the disk in detail and to test our new mass modeling strategy.…”

Section: A Brief Presentationmentioning

confidence: 99%

Asymmetric mass models of disk galaxies

Chemin

Huré

Soubiran

et al. 2016

A&A

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Mass models of galactic disks traditionally rely on axisymmetric density and rotation curves, paradoxically acting as if their most remarkable asymmetric features, such as lopsidedness or spiral arms, were not important. In this article, we relax the axisymmetry approximation and introduce a methodology that derives 3D gravitational potentials of disk-like objects and robustly estimates the impacts of asymmetries on circular velocities in the disk midplane. Mass distribution models can then be directly fitted to asymmetric line-of-sight velocity fields. Applied to the grand-design spiral M 99, the new strategy shows that circular velocities are highly nonuniform, particularly in the inner disk of the galaxy, as a natural response to the perturbed gravitational potential of luminous matter. A cuspy inner density profile of dark matter is found in M 99, in the usual case where luminous and dark matter share the same center. The impact of the velocity nonuniformity is to make the inner profile less steep, although the density remains cuspy. On another hand, a model where the halo is core dominated and shifted by 2.2−2.5 kpc from the luminous mass center is more appropriate to explain most of the kinematical lopsidedness evidenced in the velocity field of M 99. However, the gravitational potential of luminous baryons is not asymmetric enough to explain the kinematical lopsidedness of the innermost regions, irrespective of the density shape of dark matter. This discrepancy points out the necessity of an additional dynamical process in these regions: possibly a lopsided distribution of dark matter.

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“…There is a disagreement about the stage of the galaxy in the literature. ESO 533-4 has a small CMC, which makes it appear late type (Sc; de Vaucouleurs et al 1991), but its smooth appearance at 3.6 μm has recently caused it to be classified as Buta et al (2015); (5) NED; (6) from NED average of redshift-independent distances; (7) HyperLeda (Makarov et al 2014); (8) Comerón et al (2012); (9) atomic gas disc mass (M g ) and CMC mass (M CMC ) from Comerón et al (2014); (10) thin disc mass (M t ) and thick disc mass (M T ) from this paper.…”

Section: Eso 533-4mentioning

confidence: 99%

Galactic archaeology of a thick disc: Excavating ESO 533-4 with VIMOS

Comerón

Salo

Janz

et al. 2015

A&A

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The disc of galaxies is made of the superposition of a thin and a thick disc. Star formation is hosted in the thin discs and contributes to their growth. Thick discs are formed of old stars. The formation mechanisms of thick discs are under discussion. Thick discs might have formed either at high redshift on a short timescale or might have been built slowly over a Hubble-Lemaître time. They may have an internal or an external origin. Here we adopt a galactic archaeology approach to study the thick disc of ESO 533-4, i.e. we study the kinematics and the stellar populations of this galaxy in detail. ESO 533-4 is a Southern, nearby, and almost bulgeless galaxy. We present the first ever Integral Field Unit spectroscopy of an edge-on galaxy with enough depth and quality to study the thick disc. We exposed ESO 533-4 with the blue grism of the VIMOS instrument of the VLT for 6.5 h. The field of view covered an axial extent from ∼0.1 r 25 to ∼0.7 r 25 , where r 25 is the 25 mag arcsec −2 isophotal radius. This corresponds to the range from ∼1 kpc to ∼7 kpc. We used pPXF and the MILES library to obtain velocity and stellar population maps. We compared our kinematic data with simple GADGET-2 models. The apparent rotational lag of the thick disc of ESO 533-4 is compatible with that expected from the combinations of two effects: differential asymmetric drift and the projection effects arising from studying a disc a few degrees (2-3 • ) away from edge-on. Thus, ESO 533-4 contains little or no counter-rotating material. This is compatible with three formation scenarios: the secular dynamical heating of an initially thin disc, the formation of the thick disc at high redshift in an early turbulent disc phase, and the creation of a thick disc in a major merger event. If this last mechanism occurred in all galaxies, it would cause retrograde thick discs in half of them. These retrograde discs have not been observed in the five massive disc galaxies (circular velocity v c 120 km s −1 ) for which the kinematics of the thick disc is known. The stellar populations map indicates that the populations of the thin and the thick discs of ESO 533-4 are possibly separated in the Age − log (Z/Z ) plane. This would imply that thin and thick discs are formed of two distinct stellar populations. The stellar population results are not fully conclusive because of the high dust extinction in ESO 533-4 and because recovering stellar populations is a difficult inverse problem. Having said that, the stellar population results do not favour a secular evolution origin for the thick disc. Hence, we suggest that the thick disc of ESO 533-4 formed in a relatively short event.

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HyperLEDA. III. The catalogue of extragalactic distances

Cited by 823 publications

References 73 publications

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Asymmetric mass models of disk galaxies

Galactic archaeology of a thick disc: Excavating ESO 533-4 with VIMOS

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