2009
DOI: 10.1111/j.1365-2966.2009.14820.x
|View full text |Cite
|
Sign up to set email alerts
|

Formation and evolution of dwarf elliptical galaxies - II. Spatially resolved star formation histories

Abstract: We present optical VLT spectroscopy of 16 dwarf elliptical galaxies (or dEs) comparable in mass to NGC 205, and belonging to the Fornax cluster and to nearby groups of galaxies. Using full-spectrum fitting, we derive radial profiles of the SSP-equivalent ages and metallicities. We make a detailed analysis with ulyss and steckmap of the star-formation history in the core of the galaxies and in an aperture of one effective radius. We resolved the history into 1 to 4 epochs. The statistical significance of these … Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
4
1

Citation Types

26
179
0
1

Year Published

2009
2009
2020
2020

Publication Types

Select...
8
1

Relationship

0
9

Authors

Journals

citations
Cited by 129 publications
(206 citation statements)
references
References 87 publications
26
179
0
1
Order By: Relevance
“…They present a great variety of underlying structures, like discs, spiral Fulbright Fellow. arms, irregular features, some of them are also nucleated (Lisker et al 2006a,b). Their luminosity profiles are similar to exponential (Caon et al 1993;Ferrarese et al 2006;Lisker et al 2007) and they are not composed of a simple, old and metal rich stellar population, but they rather span luminosity-weighted ages from 1 Gyr to as old as the oldest objects in the universe (Michielsen et al 2008;Koleva et al 2009). Although in appearance dEs look like Es, their physical properties seem to be different from those of massive early-types.…”
Section: Introductionmentioning
confidence: 86%
“…They present a great variety of underlying structures, like discs, spiral Fulbright Fellow. arms, irregular features, some of them are also nucleated (Lisker et al 2006a,b). Their luminosity profiles are similar to exponential (Caon et al 1993;Ferrarese et al 2006;Lisker et al 2007) and they are not composed of a simple, old and metal rich stellar population, but they rather span luminosity-weighted ages from 1 Gyr to as old as the oldest objects in the universe (Michielsen et al 2008;Koleva et al 2009). Although in appearance dEs look like Es, their physical properties seem to be different from those of massive early-types.…”
Section: Introductionmentioning
confidence: 86%
“…For early-type dwarf galaxies in the Local Group, complex star formation histories have been derived, and it was shown that no two dwarfs are alike, not even within the same morphological subtype (Grebel 1997). Although there are examples of Local Group dwarf spheroidals with predominantly old and metal-poor populations (e.g., Ursa Minor, Draco), the case of a single, ancient starburst is quite unlikely for most of them; on the contrary, large metallicity spreads have been detected, and the early star formation appears to have been low and continuous (e.g., Ikuta & Arimoto 2002;Grebel et al 2003;Koch et al 2006;Coleman & de Jong 2008;Koleva et al 2009). Different models arrive at different durations to explain the observed metallicity spread (e.g., Ikuta & Arimoto 2002;Lanfranchi & Matteucci 2004;Marcolini et al 2008).…”
Section: Age Assumptionmentioning
confidence: 99%
“…Dwarf galaxies in groups have been looked at in detail in the past decade (e.g., Trentham & Tully 2002;Karachentsev et al 2004;Karachentsev 2005;Grebel 2007;Sharina et al 2008;Weisz et al 2008;Bouchard et al 2009;Dalcanton et al 2009;Koleva et al 2009). The main purpose of most of these studies was to catalog and characterize new objects in nearby groups and to look for possible environmental effects on galaxy evolution (see Grebel et al 2000, for details information is, of course, coming from our own Local Group, for which very deep observations permit us both to have a broad and detailed view of the physical properties of dwarf galaxies and to investigate how they form and evolve in this type of environment (Grebel 1997;Mateo 1998;van den Bergh 1999;Tolstoy et al 2009).…”
Section: Introductionmentioning
confidence: 99%
“…Koleva et al (2008) compared different models, and found that the Pégase-HR (Le Borgne et al 2004) and Vazdekis/Miles models were in precise agreement, while the BC03 model exhibited biases, which might be due to the poor metallicity coverage of STELIB library causing unreliable results at non-solar metallicities. In Koleva et al (2009a), they used full-spectrum fitting to derive the radial profiles of the SSP-equivalent ages and metallicities for a sample of 16 dwarf elliptical galaxies with their VLT spectra, and discussed the sensitivity of their results to the population model and IMF. Cid Fernandes & Gonzalez Delgado (2009) and Gonzalez Delgado & Cid Fernandes (2009) studied the ages, metallicities, and dust extinction of 27 star clusters in the Magellanic Clouds (from Leonardi & Rose 2003) by means of stellar population synthesis.…”
Section: Introductionmentioning
confidence: 99%