On the origin of dwarf elliptical galaxies: the fundamental plane

Aguerri, J. A. L.; González-García, A. César

doi:10.1051/0004-6361:200810339

Cited by 84 publications

(117 citation statements)

References 103 publications

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“…15) could indicate that the cluster environment has an impact on the bar sizes. In fact, numerical simulations show that tidally induced bars are on average longer than bars in isolated disks (Aguerri & González-García 2009). To investigate this possibility, we measured the projected distances (R CC ) of the cluster galaxies from the corresponding cluster center, assuming that all galaxies are at the cluster redshift.…”

Section: The Properties Of the Barsmentioning

confidence: 99%

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Barazza¹,

Jablonka

Desai

et al. 2009

A&A

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We present a study of large-scale bars in field and cluster environments out to redshifts of ∼0.8 using a final sample of 945 moderately inclined disk galaxies drawn from the EDisCS project. We characterize bars and their host galaxies and look for relations between the presence of a bar and the properties of the underlying disk. We investigate whether the fraction and properties of bars in clusters are different from their counterparts in the field. The properties of bars and disks are determined by ellipse fits to the surface brightness distribution of the galaxies using HST/ACS images in the F814W filter. The bar identification is based on quantitative criteria after highly inclined (>60 • ) systems have been excluded. The total optical bar fraction in the redshift range z = 0.4−0.8 (median z = 0.60), averaged over the entire sample, is 25% (20% for strong bars). For the cluster and field subsamples, we measure bar fractions of 24% and 29%, respectively. We find that bars in clusters are on average longer than in the field and preferentially found close to the cluster center, where the bar fraction is somewhat higher (∼31%) than at larger distances (∼18%). These findings however rely on a relatively small subsample and might be affected by small number statistics. In agreement with local studies, we find that disk-dominated galaxies have a higher optical bar fraction (∼45%) than bulge-dominated galaxies (∼15%). This result is based on Hubble types and effective radii and does not change with redshift. The latter finding implies that bar formation or dissolution is strongly connected to the emergence of the morphological structure of a disk and is typically accompanied by a transition in the Hubble type. The question whether internal or external factors are more important for bar formation and evolution cannot be answered definitely. On the one hand, the bar fraction and properties of cluster and field samples of disk galaxies are quite similar, indicating that internal processes are crucial for bar formation. On the other hand, we find evidence that cluster centers are favorable locations for bars, which suggests that the internal processes responsible for bar growth are supported by the typical interactions taking place in such environments.

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Section: The Properties Of the Barsmentioning

confidence: 99%

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Barazza¹,

Jablonka

Desai

et al. 2009

A&A

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“…Moore et al 1996;Benson et al 2002Benson et al , 2003Aguerri & González-García 2009;Brooks et al 2013). However, the interplay of the different physical processes and their time-scales are not clear (e.g.…”

Section: Introductionmentioning

confidence: 99%

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

Agulli¹,

Aguerri²,

Sánchéz-Janssen³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a new deep spectroscopic catalogue for Abell 85, within 3.0 × 2.6 Mpc 2 and down to M r ∼ M * r +6. Using the Visible Multi-Object Spectrograph at the Very Large Telescope and the AutoFiber 2 at the William Herschel Telescope, we obtained almost 1430 new redshifts for galaxies with m r ≤ 21 mag and µ e,r ≤ 24 mag arcsec −2 . These redshifts, together with SDSS-DR6 and NED spectroscopic information, result in 460 confirmed cluster members. This data set allows the study of the luminosity function (LF) of the cluster galaxies covering three orders of magnitudes in luminosities. The total and radial LFs are best modelled by a double Schechter function. The normalized LFs show that their bright (M r ≤ −21.5) and faint (M r ≥ −18.0) ends are independent of clustercentric distance and similar to the field LFs unlike the intermediate luminosity range (−21.5 ≤ M r ≤ −18.0). Similar results are found for the LFs of the dominant types of galaxies: red, passive, virialized and early-infall members. On the contrary, the LFs of blue, star-forming, non-virialized and recent-infall galaxies are well described by a single Schechter function. These populations contribute to a small fraction of the galaxy density in the innermost cluster region. However, in the outskirts of the cluster, they have similar densities to red, passive, virialized and early-infall members at the LF faint end. These results confirm a clear dependence of the colour and star formation of Abell 85 members in the cluster centric distance.

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“…Tidal forces can strip dark matter, stars, and gas into low surface brightness streams that trail along the orbit of the galaxy through the cluster (Smith et al 2010). Low surface brightness disk galaxies are especially sensitive to harassment and may have their stellar disks truncated and heated (Aguerri & González-García 2009), converting them into dispersion supported objects that resemble early-type dwarfs (Moore et al 1998). However high surface brightness giant disks are much more robust to harassment (Moore et al 1999), losing only a small fraction of stars, and suffering some disk thickening (Gnedin 2003).…”

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confidence: 99%

The sensitivity of harassment to orbit: mass loss from early-type dwarfs in galaxy clusters

Smith

Sánchéz-Janssen

Beasley

et al. 2015

Mon. Not. R. Astron. Soc.

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125

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We conduct a comprehensive numerical study of the orbital dependence of harassment on early-type dwarfs consisting of 168 different orbits within a realistic, Virgo-like cluster, varying in eccentricity and pericentre distance. We find harassment is only effective at stripping stars or truncating their stellar disks for orbits that enter deep into the cluster core. Comparing to the orbital distribution in cosmological simulations, we find that the majority of the orbits (more than three quarters) result in no stellar mass loss. We also study the effects on the radial profiles of the globular cluster systems of early-type dwarfs. We find these are significantly altered only if harassment is very strong. This suggests that perhaps most early-type dwarfs in clusters such as Virgo have not suffered any tidal stripping of stars or globular clusters due to harassment, as these components are safely embedded deep within their dark matter halo. We demonstrate that this result is actually consistent with an earlier study of harassment of dwarf galaxies, despite the apparent contradiction. Those few dwarf models that do suffer stellar stripping are found out to the virial radius of the cluster at redshift=0, which mixes them in with less strongly harassed galaxies. However when placed on phase-space diagrams, strongly harassed galaxies are found offset to lower velocities compared to weakly harassed galaxies. This remains true in a cosmological simulation, even when halos have a wide range of masses and concentrations. Thus phase-space diagrams may be a useful tool for determining the relative likelihood that galaxies have been strongly or weakly harassed.

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On the origin of dwarf elliptical galaxies: the fundamental plane

Cited by 84 publications

References 103 publications

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

The sensitivity of harassment to orbit: mass loss from early-type dwarfs in galaxy clusters

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