Simulations of the formation and evolution of isolated dwarf galaxies

Valcke, Sander; Rijcke, S. De; Dejonghe, Herwig

doi:10.1111/j.1365-2966.2008.13654.x

Cited by 78 publications

(132 citation statements)

References 80 publications

(112 reference statements)

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“…Large amounts of cold Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. interstellar matter are unexpected in dEs, as both internal (supernova explosions) and external effects (ram-pressure stripping, galaxy interactions, tidal effects) are thought to be able to expel the gas from the shallow potential on short timescales (Michielsen et al 2004;van Zee et al 2004;Roediger & Hensler 2005;Boselli et al 2008a,b;Valcke et al 2008). That the Hi detected dEs are found preferentially near the edge of the cluster supports the idea that understanding environmental effects is crucial to constraining the evolutionary history of dEs.…”

Section: Introductionsupporting

confidence: 53%

“…In particular, the population of dEs can be subdivided into nucleated and non-nucleated subclasses and several papers report evidence of disks, spiral structure, bars or star formation (e.g., Jerjen et al 2000;Barazza et al 2002;Geha et al 2003;Graham et al 2003a,b;De Rijcke et al 2003;Lisker et al 2006a,b). Kinematical studies demonstrate that dEs are not simple pressure-supported systems: some dEs seem to be rotationally supported (Simien et al 2002;Pedraz et al 2002;Geha et al 2003;De Rijcke et al 2003;van Zee et al 2004;Toloba et al 2009), whereas others show evidence of kinematically decoupled cores ; Thomas et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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TheHerschelVirgo Cluster Survey

Looze¹,

Baes²,

Zibetti³

et al. 2010

A&A

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We use the science demonstration phase data of the Herschel Virgo Cluster Survey to search for dust emission of early-type dwarf galaxies in the central regions of the Virgo cluster as an alternative way of identifying the interstellar medium. We present the first possible far-infrared detection of cluster early-type dwarf galaxies: VCC 781 and VCC 951 are detected at the 10σ level in the SPIRE 250 μm image. Both detected galaxies have dust masses of the order of 10 5 M and average dust temperatures ≈20 K. The detection rate (less than 1%) is quite high compared to the 1.7% detection rate for Hi emission, considering that dwarfs in the central regions are more Hi deficient. We conclude that the removal of interstellar dust from dwarf galaxies resulting from ram pressure stripping, harassment, or tidal effects must be as efficient as the removal of interstellar gas.

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Section: Introductionsupporting

confidence: 53%

Section: Introductionmentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Looze¹,

Baes²,

Zibetti³

et al. 2010

A&A

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“…Such intermittent star formation episodes occurring spontaneously in hydrodynamical simulations have been mentioned by Stinson et al (2007) and Valcke et al (2008). M#576 in Fig.2 offers the example of an intermediate mass self-regulated system (M i = 4.39 × 10 8 M ⊙ ).…”

Section: Self-regulationmentioning

confidence: 99%

The dynamical and chemical evolution of dwarf spheroidal galaxies

Revaz¹,

Jablonka

Sawala

et al. 2009

A&A

124

168

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We present a large sample of fully self-consistent hydrodynamical Nbody/Tree-SPH simulations of isolated dwarf spheroidal galaxies (dSphs). It has enabled us to identify the key physical parameters and mechanisms at the origin of the observed variety in the Local Group dSph properties. The initial total mass (gas + dark matter) of these galaxies is the main driver of their evolution. Star formation (SF) occurs in series of short bursts. In massive systems, the very short intervals between the SF peaks mimic a continuous star formation rate, while less massive systems exhibit well separated SF bursts, as identified observationally. The delay between the SF events is controlled by the gas cooling time dependence on galaxy mass. The observed global scaling relations, luminosity-mass and luminosity-metallicity, are reproduced with low scatter. We take advantage of the unprecedentedly large sample size and data homogeneity of the ESO Large Programme DART, and add to it a few independent studies, to constrain the star formation history of five Milky Way dSphs, Sextans, LeoII, Carina, Sculptor and Fornax. For the first time, [Mg/Fe] vs [Fe/H] diagrams derived from high-resolution spectroscopy of hundreds of individual stars are confronted with model predictions. We find that the diversity in dSph properties may well result from intrinsic evolution. We note, however, that the presence of gas in the final state of our simulations, of the order of what is observed in dwarf irregulars, calls for removal by external processes.

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“…Therefore, it is likely to be a critically important factor driving the evolution of low mass galaxies (e.g., Dekel & Silk, 1986;Mac Low & Ferrara, 1999;Ferrara & Tolstoy , 2000;Salvadori et al, 2008) like the Carina dSph, with M tot = 6.1 ± 2.3 × 10 6 M ⊙ within the half radius 241 ± 23kpc (Walker et al, 2009). If the bursts of star formation observed in Carina are part of an ongoing cycle of heating and cooling of an initial gas reservoir (e.g., Stinson et al, 2007;Valcke et al, 2008), there should be a clear evolutionary path in the observed abundances, showing the influence of SNe Ia enrichment at increasing [Fe/H] values. On the other hand, if the ISM is removed after each burst of star formation then new gas is required to power the subsequent star formation activity.…”

Section: Physical Interpretationmentioning

confidence: 99%

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

Lemasle

Hill

Tolstoy

et al. 2012

A&A

191

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Context. The ages of individual Red Giant Branch stars can range from 1 Gyr old to the age of the Universe, and it is believed that the abundances of most chemical elements in their photospheres remain unchanged with time (those that are not affected by the first dredge-up). This means that they trace the interstellar medium in the galaxy at the time the star formed, and hence the chemical enrichment history of the galaxy. Aims. Colour-Magnitude Diagram analysis has shown the Carina dwarf spheroidal to have had an unusually episodic star formation history and this is expected to be reflected in the abundances of different chemical elements. Methods. We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R≈20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.

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Simulations of the formation and evolution of isolated dwarf galaxies

Cited by 78 publications

References 80 publications

TheHerschelVirgo Cluster Survey

TheHerschelVirgo Cluster Survey

The dynamical and chemical evolution of dwarf spheroidal galaxies

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

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