The evolution of dwarf galaxies: a comparison of UBVR photometry

Dunn, Jacqueline

doi:10.1111/j.1365-2966.2010.17117.x

Cited by 12 publications

(10 citation statements)

References 26 publications

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“…In the Fornax cluster an abundant population of faint LSB galaxies with µ r,0 ≥ 23 mag arcsec −2 were catalogued by Muñoz et al (2015) and Venhola et al (2017), of which a few have r 50 > 3 kpc (Venhola et al 2017). Several such objects in different environments were also reported by Dunn (2010).…”

Section: Introductionmentioning

confidence: 73%

A population of faint low surface brightness galaxies in the Perseus cluster core

Wittmann

Lisker

Tilahun

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the detection of 89 low surface brightness (LSB), and thus low stellar density galaxy candidates in the Perseus cluster core, of the kind named 'ultra-diffuse galaxies', with mean effective V-band surface brightnesses 24.8-27.1 mag arcsec −2 , total V-band magnitudes −11.8 to −15.5 mag, and half-light radii 0.7-4.1 kpc. The candidates have been identified in a deep mosaic covering 0.3 deg 2 , based on wide-field imaging data obtained with the William Herschel Telescope. We find that the LSB galaxy population is depleted in the cluster centre and only very few LSB candidates have half-light radii larger than 3 kpc. This appears consistent with an estimate of their tidal radius, which does not reach beyond the stellar extent even if we assume a high dark matter content (M/L = 100). In fact, three of our candidates seem to be associated with tidal streams, which points to their current disruption. Given that published data on faint LSB candidates in the Coma cluster -with its comparable central density to Perseus -show the same dearth of large objects in the core region, we conclude that these cannot survive the strong tides in the centres of massive clusters.

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Section: Introductionmentioning

confidence: 73%

A population of faint low surface brightness galaxies in the Perseus cluster core

Wittmann

Lisker

Tilahun

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…We also searched the NASA Extragalactic Database (NED) under the following three classifications: dwarfs (dwarf, nucleated, dwarf elliptical (dE), dwarf lenticular (S0), dwarf spiral (dS), dwarf irregular (dI) and blue compact dwarf (BCD)); E peculiar; and compact E. Dwarfs are ill defined in the literature (see e.g. Dunn 2010, for a review on the various definitions), and some known dwarfs, such as NGC 185 and 147, are labelled in NED as elliptical galaxies. Thus, we expanded our search parameters to ensure that we did not lose any potential dwarfs in the nearby Universe.…”

Section: Nearby Galaxy Samplementioning

confidence: 99%

Infrared signature of active massive black holes in nearby dwarf galaxies

Marleau

Clancy

Habas

et al. 2017

A&A

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Context. We investigate the possible presence of active galactic nuclei (AGN) in dwarf galaxies and other nearby galaxies to identify candidates for follow-up confirmation and dynamical mass measurements. Aims. We identify candidate active central massive black holes (CMBH) using their mid-infrared emission, verify their nature using existing catalogues and optical line emission diagnostics, and study the relationship between their mass and the mass of their host galaxy. Methods. We use the Wide-field Infrared Survey Explorer (WISE) All-Sky Release Source Catalog and examine the infrared colours of a sample of dwarf galaxies and other nearby galaxies in order to identify both unobscured and obscured candidate AGN by applying the infrared colour diagnostic. Stellar masses of galaxies are obtained using a combination of three independent methods. Black hole masses are estimated using the bolometric luminosity of the AGN candidates and computed for three cases of the bolometric-toEddington luminosity ratio. Results. We identify 303 candidate AGN, of which 276 were subsequently found to have been independently identified as AGN via other methods. The remaining 9% require follow-up observations for confirmation. The activity is detected in galaxies with stellar masses from ∼ 10 6 to 10 9 M ; assuming the candidates are AGN, the black hole masses are estimated to be ∼ 10 3 − 10 6 M , adopting L bol = 0.1L Edd . The black hole masses probed are several orders of magnitude smaller than previously reported for centrally located massive black holes. We examine the stellar mass versus black hole mass relationship in this low galaxy mass regime. We find that it is consistent with the existing relation extending linearly (in log-log space) into the lower mass regime. Conclusions. These findings suggest that CMBH are present in low-mass galaxies and in the Local Universe, and provide new impetus for follow-up dynamical studies of quiescent black holes in local dwarf galaxies.

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“…Here we compare the gross properties of the simulated dwarfs, both with and without merger trees, with observed kinematic and photometric scaling relations at z = 0. (2003), Hunter & Elmegreen (2006), Dunn (2010) and Kirby et al (2013) are presented in the Vband, so no transformation was needed. The V-band magnitudes of van Zee (2000) (2003) where we transform the V-band magnitude to the B-band magnitude using MV =MB-0.7.…”

Section: Scaling Relationsmentioning

confidence: 99%

Numerical simulations of dwarf galaxy merger trees

Cloet-Osselaer

Rijcke

Vandenbroucke

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We investigate the evolution of dwarf galaxies using N -body/SPH simulations that incorporate their formation histories through merger trees constructed using the extended Press-Schechter formalism. The simulations are computationally cheap and have high spatial resolution. We compare the properties of galaxies with equal final mass but with different merger histories with each other and with those of observed dwarf spheroidals and irregulars.We show that the merger history influences many observable dwarf galaxy properties. We identify two extreme cases that make this influence stand out most clearly: (i) merger trees with one massive progenitor that grows through relatively few mergers and (ii) merger trees with many small progenitors that merge only quite late. At a fixed halo mass, a type (i) tree tends to produce galaxies with larger stellar masses, larger half-light radii, lower central surface brightness, and since fewer potentially angular momentum cancelling mergers are required to build up the final galaxy, a higher specific angular momentum, compared with a type (ii) tree.We do not perform full-fledged cosmological simulations and therefore cannot hope to reproduce all observed properties of dwarf galaxies. However, we show that the simulated dwarfs are not unsimilar to real ones.

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The evolution of dwarf galaxies: a comparison of UBVR photometry

Cited by 12 publications

References 26 publications

A population of faint low surface brightness galaxies in the Perseus cluster core

A population of faint low surface brightness galaxies in the Perseus cluster core

Infrared signature of active massive black holes in nearby dwarf galaxies

Numerical simulations of dwarf galaxy merger trees

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