The faint end of the galaxy luminosity function

Trentham, Neil; Tully, R. Brent

doi:10.1046/j.1365-8711.2002.05651.x

Cited by 178 publications

(212 citation statements)

References 85 publications

(119 reference statements)

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“…With our SBF distance of 11.1 ± 0.9 Mpc we can now confirm this impression. The derived SBF distance is also in good agreement with the mean distance of 11 Mpc for the group (Trentham & Tully 2002). We note that there was not much of colour range found in the five fields we analysed to unambiguously apply the distance calibration.…”

Section: Ugc 5944 ([Fs90] 047)supporting

confidence: 76%

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New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

Rekola

Jerjen

Flynn

2005

A&A

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Abstract. We present Surface Brightness Fluctuation distances of nine early-type dwarf galaxies and the S0 galaxy NGC 4150 in the Local Volume based on deep B-and R-band CCD images obtained with the 2.56 m Nordic Optical Telescope. Typically, six stellar fields at various galactocentric distances have been chosen for each galaxy as appropriately free of foreground stars and other contaminants, and Fourier analysed to determine the distances, which are found to lie in the range of 3 to 16 Mpc. The SBF method is thus demonstrated to efficiently measure distances from the ground with mid-aperture telescopes for galaxies for which only the tip of the red giant branch method in combination with the Hubble Space Telescope has been available until now. We obtained the following distance moduli: 28.11 ± 0.15 mag (or 4.2 ± 0.3 Mpc) for UGC 1703, 27.61 ± 0.17 mag (or 3.3 ± 0.3 Mpc) for KDG 61, 29.00 ± 0.27 mag (or 6.3 ± 0.8 Mpc) for UGCA 200, 27.74 ± 0.18 mag (or 3.5 ± 0.3 Mpc) for UGC 5442, 30.22 ± 0.17 mag (or 11.1 ± 0.9 Mpc) for UGC 5944, 30.79 ± 0.11 mag (or 14.4 ± 0.7 Mpc) for NGC 4150, 31.02 ± 0.25 mag (or 16.0 ± 1.9 Mpc) for BTS 128, 29.27 ± 0.16 mag (or 7.1 ± 0.6 Mpc) for UGC 7639, 30.19 ± 0.23 mag (or 10.9 ± 1.2 Mpc) for UGC 8799 with an alternative distance of 30.61 ± 0.26 mag (or 13.2 ± 1.7 Mpc), and 29.60 ± 0.20 mag (or 8.3 ± 0.8 Mpc) for UGC 8882.

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Section: Ugc 5944 ([Fs90] 047)supporting

confidence: 76%

“…This dwarf elliptical is located right in the densest region of the Coma I group (Binggeli et al 1990;Trentham & Tully 2002) about 10 degrees away from the northern boundary of the Virgo cluster. The heliocentric velocity of BTS 128 of v = 1139 ± 86 km s −1 (Wegner et al 2001) is in good agreement with the Coma I cluster.…”

Section: Bts 128mentioning

confidence: 99%

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

Rekola

Jerjen

Flynn

2005

A&A

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“…The faint end slope of a composite LF, averaged over 60 nearby galaxy clusters, reveals a similar value of α = −1.28 (De Propris et al 2003). Previous studies have suggested that indeed the faint end slope of the LF is independent of environment: Trentham & Tully (2002) show such an almost invariable faint end slope in their study of five different environments with varying galaxy density and morphological content. They find a composite faint end slope of α = −1.19 for their entire sample.…”

Section: Luminosity Functionsupporting

confidence: 53%

“…Another useful parameter for describing the LF shape is the dwarf-to-giant ratio (Phillipps et al 1998;Sánchez-Janssen et al 2008). We compared our data with the study of Trentham & Tully (2002), adopting their definition of the d/g ratio as d/g = N(−17 < M R < −11)/N(M R < −17). By taking the completeness correction into account, we obtain d/g = 4.1 ± 0.6.…”

Section: Luminosity Functionmentioning

confidence: 99%

A normal abundance of faint satellites in the fossil group NGC 6482

Lieder¹,

Mieske²,

Sánchéz-Janssen³

et al. 2013

A&A

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A fossil group is considered the end product in a galaxy group's evolution. It is a massive central galaxy that dominates the luminosity budget of the group, and is the outcome of efficient merging between intermediate-luminosity members. Little is known, however, about the faint satellite systems of fossil groups. Here we present a Subaru/Suprime-Cam wide-field, deep imaging study in the B− and R−bands of the nearest fossil group NGC 6482 (M tot ∼ 4 × 10 12 M ), covering the virial radius out to 310 kpc. We performed detailed completeness estimations and selected group member candidates by a combination of automated object detection and visual inspection. A fiducial sample of 48 member candidates down to M R ∼ −10.5 mag is detected, making this study the deepest of a fossil group to now. We investigate the photometric scaling relations, the color-magnitude relation, and the luminosity function of our galaxy sample. We find evidence of recent and ongoing merger events among bright group galaxies. The color-magnitude relation is comparable to that of nearby galaxy clusters, and it exhibits significant scatter at the faintest luminosities. The completeness-corrected luminosity function is dominated by early-type dwarfs and is characterized by a faint end slope α = −1.32 ± 0.05. We conclude that the NGC 6482 fossil group shows photometric properties consistent with those of regular galaxy clusters and groups, including a normal abundance of faint satellites.

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“…It was found that the fraction of massive early-type galaxies (E/S0) and dwarf elliptical galaxies is higher in a dynamically more evolved system with high velocity dispersion (Trentham & Tully 2002;Tovmassian et al 2004;Tovmassian & Plionis 2009). Especially in the case of the NGC 3992 subgroup, which is the most dynamically evolved Ursa Major cluster subgroup, considering its high frequency of early-type galaxies, morphological transformation to early-type galaxies by interactions and merging between galaxies may have occurred more frequently in the early stages of its dynamical evolution than in the other subgroups.…”

Section: Environmental Effects In a Lower Density Clustermentioning

confidence: 99%

The properties of early-type galaxies in the Ursa Major cluster

Pak¹,

Rey²,

Lisker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Using SDSS-DR7 and NASA/IPAC Extragalactic Database spectroscopic data, we identify 166 galaxies as members of the Ursa Major cluster with M r < −13.5 mag. We morphological classify all galaxies by means of carefully inspecting g−, r−, i−band colour and monochromatic images. We show that the Ursa Major cluster is dominated by late-type galaxies, but also contains a significant number of earlytype galaxies, particularly in the dwarf regime. We present further evidence for the existence of several subgroups in the cluster, consistent with previous findings. The early-type fraction is found to correlate with the mass of the subgroup. We also investigate environmental effects by comparing the properties of the Ursa Major early-type dwarf galaxies to those of the Virgo cluster. In contrast to the Virgo, the red sequence of the Ursa Major cluster is only sparsely populated in the optical and ultraviolet colour-magnitude relations. It also shows a statistically significant gap between −18 < M r < −17 mag, i.e. the Ursa Major cluster lacks early-type dwarf galaxies at the bright end of their luminosity function. We discover that the majority of early-type dwarf galaxies in the Ursa Major cluster have blue cores with hints of recent or ongoing star formation. We suggest that gravitational tidal interactions can trigger central blue star forming regions in early-type dwarfs. After that, star formation would only fade completely when the galaxies experience ram pressure stripping or harassment, both of which are nearly absent in the Ursa Major cluster.

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The faint end of the galaxy luminosity function

Cited by 178 publications

References 85 publications

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

A normal abundance of faint satellites in the fossil group NGC 6482

The properties of early-type galaxies in the Ursa Major cluster

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