Galactic Bulges from [ITAL]Hubble Space Telescope[/ITAL] Near-Infrared Camera Multi-Object Spectrometer Observations: The Lack of [CLC][ITAL]r[/ITAL][/CLC][TSUP]1/4[/TSUP] Bulges

Balcells, M.; Graham, Alister W.; Domínguez-Palmero, Lilian; Peletier, Reynier F.

doi:10.1086/367783

Cited by 178 publications

(217 citation statements)

References 39 publications

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“…The exact shape of bulge profiles remains under debate (e.g., Balcells et al 2003, and references therein). Locally, there is evidence that the bulges of late-type spiral galaxies may be better fit by an n = 1 profile, whereas bright ellipticals and the bulges of early-type spiral galaxies follow an n = 4 profile (de Jong 1996;Courteau et al 1996;Andredakis 1998).…”

Section: Fitting Modelmentioning

confidence: 99%

Evolution of the early-type galaxy fraction in clusters since z = 0.8

Simard

Clowe

Desai

et al. 2009

A&A

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We study the morphological content of a large sample of high-redshift clusters to determine its dependence on cluster mass and redshift. Quantitative morphologies are based on PSF-convolved, 2D bulge+disk decompositions of cluster and field galaxies on deep Very Large Telescope FORS2 images of eighteen, optically-selected galaxy clusters at 0.45 < z < 0.80 observed as part of the ESO Distant Cluster Survey ("EDisCS"). Morphological content is characterized by the early-type galaxy fraction f et , and early-type galaxies are objectively selected based on their bulge fraction and image smoothness. This quantitative selection is equivalent to selecting galaxies visually classified as E or S0. Changes in early-type fractions as a function of cluster velocity dispersion, redshift and star-formation activity are studied. A set of 158 clusters extracted from the Sloan Digital Sky Survey is analyzed exactly as the distant EDisCS sample to provide a robust local comparison. We also compare our results to a set of clusters from the Millennium Simulation. Our main results are: (1) the early-type fractions of the SDSS and EDisCS clusters exhibit no clear trend as a function of cluster velocity dispersion. (2) Mid-z EDisCS clusters around σ = 500 km s −1 have f et 0.5 whereas high-z EDisCS clusters have f et 0.4. This represents a ∼25% increase over a time interval of 2 Gyr. (3) There is a marked difference in the morphological content of EDisCS and SDSS clusters. None of the EDisCS clusters have early-type galaxy fractions greater than 0.6 whereas half of the SDSS clusters lie above this value. This difference is seen in clusters of all velocity dispersions. (4) There is a strong and clear correlation between morphology and star formation activity in SDSS and EDisCS clusters in the sense that decreasing fractions of [OII] emitters are tracked by increasing early-type fractions. This correlation holds independent of cluster velocity dispersion and redshift even though the fraction of [OII] emitters decreases from z ∼ 0.8 to z ∼ 0.06 in all environments. Our results pose an interesting challenge to structural transformation and star formation quenching processes that strongly depend on the global cluster environment (e.g., a dense ICM) and suggest that cluster membership may be of lesser importance than other variables in determining galaxy properties.

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Section: Fitting Modelmentioning

confidence: 99%

Evolution of the early-type galaxy fraction in clusters since z = 0.8

Simard

Clowe

Desai

et al. 2009

A&A

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“…Balcells et al (2003) report that early-type disk galaxies tend to have n < 3 and often from 1 to 2. Laurikainen et al (2007) find barred and unbarred early-type disk galaxies to have mean B/T between 0.25 and 0.35, while later Hubble types have B/T < 0.2; they also find mean bulge Sérsic indices to be ∼ 2.5 or less across the Hubble sequence.…”

Section: Introductionmentioning

confidence: 99%

BULGEnANDB/TIN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS

Weinzirl

Jogee

Khochfar

et al. 2009

ApJ

316

382

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We use the bulge Sérsic index n and bulge-to-total ratio (B/T ) to explore the fundamental question of how bulges form. We perform 2D bulge-disk-bar decomposition on H-band images of 143 bright, high mass (M ⋆ ≥ 1.0 × 10 10 M ⊙ ) low-to-moderately inclined (i < 70 • ) spirals. Our results are: (1) Our H-band bar fraction (∼ 58%) is consistent with that from ellipse fits. (5) We compare the results with predictions from a set of ΛCDM models. In the models, a high mass spiral can have a bulge with a present-day low B/T ≤ 0.2 only if it did not undergo a major merger since z ≤ 2. The predicted fraction (∼ 1.6%) of high mass spirals, which have undergone a major merger since z ≤ 4 and host a bulge with a present-day low B/T ≤ 0.2, is a factor of over thirty smaller than the observed fraction (∼ 66%) of high mass spirals with B/T ≤ 0.2. Thus, contrary to common perception, bulges built via major mergers since z ≤ 4 seriously fail to account for the bulges present in ∼ 66% of high mass spirals. Most of these present-day low B/T ≤ 0.2 bulges are likely to have been built by a combination of minor mergers and/or secular processes since z ≤ 4.

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“…Krajnović et al (2008) found NDs in early-type galaxies are associated with fast rotators. Near-infrared Hubble Space Telescope (HST) imaging has also provided indirect evidence for NDs as discy isophotes in the nuclei of early-type galaxies (Ravindranath et al 2001) or photometrically distinct exponential components in bulges (Balcells et al 2003). Erwin et al (2014) also found evidence for NDs which they call "discy pseudobulges".…”

Section: Introductionmentioning

confidence: 99%

The formation of stellar nuclear discs in bar-induced gas inflows

Cole

Debattista

Erwin

et al. 2014

Monthly Notices of the Royal Astronomical Society

123

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The role of gas in the mass assembly at the nuclei of galaxies is still subject to some uncertainty. Stellar nuclear discs bridge the gap between the large-scale galaxy and the central massive objects that reside there. Using a high resolution simulation of a galaxy forming out of gas cooling and settling into a disc, we study the formation and properties of nuclear discs. Gas, driven to the centre by a bar, settles into a rotating star-forming nuclear disc (ND). This ND is thinner, younger, kinematically cooler, and more metal-rich than the surrounding bar. The ND is elliptical and orthogonal to the bar. The complex kinematics in the region of the ND are a result of the superposition of older stars streaming along the bar and younger stars circulating within the ND. The signature of the ND is therefore subtle in the kinematics. Instead the ND stands out clearly in metallicity and age maps. We compare the model to the density and kinematics of real galaxies with NDs finding qualitative similarities. Our results suggest that gas dissipation is very important for forming nuclear structures.

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Galactic Bulges from [ITAL]Hubble Space Telescope[/ITAL] Near-Infrared Camera Multi-Object Spectrometer Observations: The Lack of [CLC][ITAL]r[/ITAL][/CLC][TSUP]1/4[/TSUP] Bulges

Cited by 178 publications

References 39 publications

Evolution of the early-type galaxy fraction in clusters since z = 0.8

Evolution of the early-type galaxy fraction in clusters since z = 0.8

BULGEnANDB/TIN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS

The formation of stellar nuclear discs in bar-induced gas inflows

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