BULGES OF NEARBY GALAXIES WITH<i>SPITZER</i>: SCALING RELATIONS IN PSEUDOBULGES AND CLASSICAL BULGES

Fisher, David B.; Drory, Niv

doi:10.1088/0004-637x/716/2/942

Cited by 194 publications

(275 citation statements)

References 79 publications

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“…do classical bulges and elliptical galaxies. Fisher & Drory (2010) present a similar result. They see almost no dependence of effective surface brightness on effective radius.…”

Section: The Fundamental Planesupporting

confidence: 71%

“…As the above evidence shows, most of our galaxies are likely to be pseudobulges. We therefore expect them to scale differently in the fundamental plane than in elliptical galaxies (Kormendy 1980;Carollo 1999;Kormendy & Kennicutt 2004;Fisher & Drory 2010). Specifically, we expect them to look more like disks.…”

Section: Bulge Morphologymentioning

confidence: 97%

“…Now, with detailed image decompositions in hand, we are in a position to address the morphology of the host galaxies. Galaxy structure (e.g., Sérsic index, the presence of bars or nuclear spirals) will help us determine whether each bulge is a classical or pseudobulge (Kormendy & Kennicutt 2004;Fisher & Drory 2010). We quantify the bar fraction, since bars have been suggested as a feeding mechanism for low-level AGN activity (e.g., Shlosman et al 1990).…”

Section: Galaxy Morphologymentioning

confidence: 99%

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The Host Galaxies of Low-Mass Black Holes

Jiang

Greene

et al. 2011

ApJ

103

150

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Using Hubble Space Telescope observations of 147 host galaxies of low-mass black holes (BHs), we systematically study the structures and scaling relations of these active galaxies. Our sample is selected to have central BHs with virial masses of ∼10 5 -10 6 M . The host galaxies have total I-band magnitudes of −23.2 < M I < −18.8 mag and bulge magnitudes of −22.9 < M I < −16.1 mag. Detailed bulge-disk-bar decompositions with GALFIT show that 93% of the galaxies have extended disks, 39% have bars, and 5% have no bulges at all at the limits of our observations. Based on the Sérsic index and bulge-to-total ratio, we conclude that the majority of the galaxies with disks are likely to contain pseudobulges and very few of these low-mass BHs live in classical bulges. The fundamental plane of our sample is offset from classical bulges and ellipticals in a way that is consistent with the scaling relations of pseudobulges. The sample has smaller velocity dispersion at fixed luminosity in the Faber-Jackson plane compared with classical bulges and elliptical galaxies. The galaxies without disks are structurally more similar to spheroidals than to classical bulges according to their positions in the fundamental plane, especially the Faber-Jackson projection. Overall, we suggest that BHs with mass 10 6 M live in galaxies that have evolved secularly over the majority of their history. A classical bulge is not a prerequisite to host a BH.

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“…do classical bulges and elliptical galaxies. Fisher & Drory (2010) present a similar result. They see almost no dependence of effective surface brightness on effective radius.…”

Section: The Fundamental Planesupporting

confidence: 71%

Section: Bulge Morphologymentioning

confidence: 97%

Section: Galaxy Morphologymentioning

confidence: 99%

See 1 more Smart Citation

The Host Galaxies of Low-Mass Black Holes

Jiang

Greene

et al. 2011

ApJ

103

150

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“…However, the effective radius is quite large, which can be explained by the extended X-structure in the central part of the galaxy. The moderate Sérsic index n ≈ 2.3 suggests that the bulge lies in the overlapping area between pseudo-bulges and classical bulges (Fisher & Drory 2010). However, low bulge flattening suggests that the central component may appear to be a classical bulge rather than a pseudo-bulge.…”

Section: Decomposition Of the Irac 36 µM Imagementioning

confidence: 98%

HERschelObservations of Edge-on Spirals (HEROES)

Mosenkov

Allaert

Baes

et al. 2016

A&A

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We investigate the dust energy balance for the edge-on galaxy IC 2531, one of the seven galaxies in the HEROES sample. We perform a state-of-the-art radiative transfer modelling based, for the first time, on a set of optical and near-infrared galaxy images. We show that by taking into account near-infrared imaging in the modelling significantly improves the constraints on the retrieved parameters of the dust content. We confirm the result from previous studies that including a young stellar population in the modelling is important to explain the observed stellar energy distribution. However, the discrepancy between the observed and modelled thermal emission at far-infrared wavelengths, the so-called dust energy balance problem, is still present: the model underestimates the observed fluxes by a factor of about two. We compare two different dust models, and find that dust parameters, and thus the spectral energy distribution in the infrared domain, are sensitive to the adopted dust model. In general, the THEMIS model reproduces the observed emission in the infrared wavelength domain better than the popular BARE-GR-S model. Our study of IC 2531 is a pilot case for detailed and uniform radiative transfer modelling of the entire HEROES sample, which will shed more light on the strength and origins of the dust energy balance problem.

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“…They are expected to have very different structural properties, because the bulges formed via secular evolutionary processes are expected to have more disk-like properties, while the so-called "classical" bulges are expected to have properties that are more related to elliptical galaxies (e.g. Athanassoula 2005;Fisher & Drory 2008;Gadotti 2009;Fisher & Drory 2010, for a detail discussion on the properties on both types of bulges, see the review by Based on observations obtained at Siding Spring Observatory (RSAA, ANU, Australia) and the INT telescope at the ING, La Palma, Spain.…”

Section: Introductionmentioning

confidence: 99%

Study of stellar populations in the bulges of barred galaxies

Pérez

Sánchez‐Blázquez

2011

A&A

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Aims. We wish to determine the influence of bars on the building of galaxy bulges through analysis of ages and metallicities derived from stellar absorption line-strength indices. Methods. Long-slit spectroscopy was obtained for a sample of 20 early-type barred galaxies. Line-strength indices were measured and used to derive age and metallicity gradients in the bulge region by comparing them with stellar population models. The same analysis was carried out with similar data for unbarred galaxies taken from the literature. Results. The bulges of barred galaxies seem to be more metal rich, at a given velocity dispersion (σ), than the bulges of unbarred galaxies, as measured by a few metallicity sensitive indices. There are indications that the ratio of relative abundance of alpha elements with respect to iron, [E/Fe], derived for the bulges of barred galaxies tend to lie above the values of the unbarred galaxies at a given σ. The metallicity gradients for the majority of the bulges are negative so less metal-rich towards the end of the bulge. The gradient values show a large scatter for galaxies with σ below 150 km s −1 . The age distribution is related to the presence of a bulge substructure, such as a nuclear ring or an inner disk. The metallicity of both the bulge and the bar are very well correlated, indicating a close link between the enrichment histories of both components. Conclusions. Bulges of barred early type galaxies might have experienced a different chemical enrichment than do the bulges of unbarred galaxies of the same morphological type, the same central velocity dispersion, and low inclination angles. The hinted stellar populations differences separating the bulges of barred and unbarred galaxies and the strong link between the metallicity of the bulge and the presence of a bar points to scenarios where they both form simultaneously in processes that lead to rapid and massive episodes of star formation, possibly linked to the bar formation. To confirm and generalise the results found here, it would be useful to extend the data set to a larger number of unbarred galaxies and a wider range of morphological types

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BULGES OF NEARBY GALAXIES WITHSPITZER: SCALING RELATIONS IN PSEUDOBULGES AND CLASSICAL BULGES

Cited by 194 publications

References 79 publications

The Host Galaxies of Low-Mass Black Holes

The Host Galaxies of Low-Mass Black Holes

HERschelObservations of Edge-on Spirals (HEROES)

Study of stellar populations in the bulges of barred galaxies

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