Dwarf Galaxies Also Have Stellar Halos

Minniti, D.; Zijlstra, A. A.

doi:10.1086/310189

Cited by 78 publications

(70 citation statements)

References 31 publications

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“…The comparison of the two results may indicate the presence of a gradient in the stellar population in the halo, as suggested by Marleau et al (2000). However, the small field of view of HST puts serious limitations to the conclusions in the cases where the strong gradients in galaxy populations exist (see, for example, the case of Local Group dwarf galaxies like Leo I (Gallart et al 1999;Held et al 2000) or WLM (Minniti & Zijlstra 1996, 1997). …”

Section: Introductionmentioning

confidence: 92%

Stellar populations in NGC 5128 with the VLT: Evidence for recent star formation

Rejkuba

Minniti²,

Silva

et al. 2001

A&A

107

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Abstract. We resolve stars of the nearest giant elliptical galaxy NGC 5128 using VLT with FORS1 and ISAAC. We construct deep U , V and Ks color-magnitude and color-color diagrams in two different halo fields (in the halo and in the north-eastern diffuse shell). In the outer, shell field, at ∼14 kpc from the center of the galaxy, there is a significant recent star formation with stars as young as 10 Myr, approximately aligned with the prominent radio and X-ray jet from the nucleus of the host AGN. Ionized gas filaments are evident in ultraviolet images near the area where neutral Hi and CO molecular gas was previously observed. The underlying stellar population of the halo of the giant elliptical is predominantly old with a very broad metallicity distribution. The presence of an extended giant branch reaching M bol = −5 mag suggests the existence of a significant intermediate-age AGB population in the halo of this galaxy.

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Section: Introductionmentioning

confidence: 92%

Stellar populations in NGC 5128 with the VLT: Evidence for recent star formation

Rejkuba

Minniti²,

Silva

et al. 2001

A&A

107

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“…In the Fornax dSph, N-body simulations suggest that no significant amount of stars have been lost (Peñarrubia et al 2009). This is less well constrained in WLM and IKN, although WLM is one of the most isolated galaxies in the Local Group, possibly near the zero-velocity surface, and may not have interacted significantly with other galaxies during its lifetime (Sandage & Carlson 1985;Minniti & Zijlstra 1996). D'Antona et al (2013) have argued that it may be possible to accommodate the high M GC /M field ratio observed in Fornax, even if the polluters of the second generation stars in GCs are massive AGB stars.…”

Section: Overall Metallicities and Implications For The Formation Of mentioning

confidence: 99%

Chemical composition and constraints on mass loss for globular clusters in dwarf galaxies: WLM and IKN

Larsen

Brodie

Forbes

et al. 2014

A&A

111

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Aims. We determine the metallicities of globular clusters (GCs) in the WLM and IKN dwarf galaxies, using VLT/UVES and Keck/ESI spectroscopy. These measurements are combined with literature data for field stars to constrain GC formation scenarios. For the WLM GC, we also measure detailed abundance ratios for a number of light, α, Fe-peak, and n-capture elements, which are compared with literature data for the Fornax dSph and the Milky Way. Methods. The abundances are derived by computing synthetic integrated-light model spectra and adjusting the input composition until the best fits to the observed spectra are obtained. Conclusions. The GCs in the WLM and IKN dwarf galaxies resemble those in the Fornax dSph by being significantly more metalpoor than a typical halo GC in the Milky Way and other large galaxies. They are also substantially more metal-poor than the bulk of the field stars in their parent galaxies. It appears that only a small fraction of the Milky Way GC system could have been accreted from galaxies similar to these dwarfs. The relatively high Na abundance in the WLM GC suggests that the [Na/O] anti-correlation is present in this cluster, while the high ratios of metal-poor GCs to field stars in the dwarfs are in tension with GC formation scenarios that require GCs to have lost a very large fraction of their initial mass.

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“…Irregular galaxies, which are the close relatives of spiral galaxies, have the simplest composition. The discovery of a stellar halo in two irregular galaxies, WLM and NGC 3109, was announced in the papers by Minniti and his colleagues [9], [10]. Later, based on the study of the stellar population of 25 irregular galaxies, Tikhonov [11][12][13] showed that every irregular galaxy has a thick disk the dimensions of which are 2-3 times as large as the visible body of the galaxy.…”

Section: Introductionmentioning

confidence: 99%

Stellar Disks and Halos of Edge-on Spiral Galaxies: NGC 891, NGC 4144, and NGC 4244

Тихонов

Galazutdinova

2005

Astrophysics

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The results of the stellar photometry of the images ACS/WFC and WFPC2 of the HST are used to study stellar population and spatial distribution of stars in three edge-on galaxies: NGC 891, NGC 4144 and NGC 4244. The measuring of the number density of the old stars revealed two stellar substructures in these galaxies: thick disk and halo. The borders of these substructures consisting mainly of red giants, are determined by the change of number density gradient of the old stars. The revealed halos have flattened shapes and extend up to 25 kpc from the galaxy planes. The obtained results of number density distributions of different type stars perpendicular to the galaxy planes allow us to verify our stellar model of spiral galaxies. Using the determination of the tip of red giant branch (TRGB method) we have derived the following distances: D = 9.82 Mpc (NGC 891), D = 7.24 Mpc (NGC 4144) D = 4.29 Mpc (NGC 4244).

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Dwarf Galaxies Also Have Stellar Halos

Cited by 78 publications

References 31 publications

Stellar populations in NGC 5128 with the VLT: Evidence for recent star formation

Stellar populations in NGC 5128 with the VLT: Evidence for recent star formation

Chemical composition and constraints on mass loss for globular clusters in dwarf galaxies: WLM and IKN

Stellar Disks and Halos of Edge-on Spiral Galaxies: NGC 891, NGC 4144, and NGC 4244

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