H I and optical observations of dwarf galaxies

Davies, R. D.; Kinman, T. D.

doi:10.1093/mnras/258.2.334

Cited by 111 publications

(114 citation statements)

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“…This dwarf lies (in projection) approximately between the elliptical Cen A and the spiral M 83. The proximity to these two giant galaxies may explain why the M HI /L B value for the dwarf is several times lower than typical values for dIs at comparable luminosities (e.g., Staveley-Smith et al 1992). …”

Section: A1334−277 (Eso444−g084)mentioning

confidence: 75%

Nebular abundances of nearby southern dwarf galaxies

Lee

Grebel

Hodge

2003

A&A

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Abstract.The results of optical spectroscopy of H II regions in a sample of southern dwarf irregulars consisting of five dwarf galaxies in the Centaurus A group, four dwarfs in the Sculptor group, and eight additional dwarf galaxies are presented. Oxygen abundances are derived using the direct method where [O III]λ4363 is detected; otherwise, abundances are derived with the bright-line method using the McGaugh and the Pilyugin calibrations. ESO358−G060 has the lowest oxygen abundance (12+log(O/H) = 7.32) in the sample, which is comparable to the value for the second most metal-poor galaxy known (SBS 0335−052). In all, new oxygen abundances are reported for nine dwarf galaxies; updated values are presented for the remaining galaxies. Derived oxygen abundances are in the range from 3% to 26% of the solar value. Oxygen abundances for dwarfs in the southern sample are consistent with the metallicity-luminosity relationship defined by a control sample of dwarf irregulars with [O III]λ4363 abundances and well-measured distances. However, NGC 5264 appears to have an (upper branch) oxygen abundance approximately two to three times higher than other dwarfs at similar luminosities. Nitrogen-to-oxygen and neon-to-oxygen abundance ratios are also reported; in particular, IC 1613 and IC 5152 show elevated nitrogen-to-oxygen ratios for their oxygen abundances.

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Section: A1334−277 (Eso444−g084)mentioning

confidence: 75%

Nebular abundances of nearby southern dwarf galaxies

Lee

Grebel

Hodge

2003

A&A

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“…, discussed, e.g., by Staveley-Smith et al (1992) for LSB dIs and BCGs, and recently by Smoker et al (2000) for emission-line galaxies from the University of Michigan survey. The former authors derived β = −0.3 ± 0.1, while the latter give for their H i-detected University of Michigan survey ELGs β = −0.2 ± 0.1.…”

Section: Distributions Of M(h I)/l B For Various Bcg Samplesmentioning

confidence: 81%

Studies of galaxies in voids

Pustilnik¹,

Martin²,

Huchtmeier³

et al. 2002

A&A

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Abstract. We present here results of studies of the properties of galaxies located in very low density environments. We observed 26 blue compact galaxies (BCGs) from the Second Byurakan (SBS) and Case surveys located in voids with the radial velocities V hel . 11 000 km s −1 , two BCGs in the void behind the Virgo cluster and 11 BCGs in denser environments. H i fluxes and profile widths, as well as estimates of total H i masses, are presented for the 27 detected galaxies (of which 6 are in three galaxy pairs and are not resolved by the radiotelescope beam). Preliminary comparisons of void BCGs with similar objects from intermediate density regions -in the general field and the Local Supercluster (sub-samples of BCGs in the SBS zone) and in the dense environment of the Virgo Cluster (a BCD sample) -are performed using the hydrogen-to-blue-luminosity ratio M (H i)/LB. We find that for the same blue luminosity, for MB > −18. m 0, BCGs in lower density environment have on average more H i. The slope β of the M (H i)/LB _ L β for BCGs shows a trend of steepening with decreasing bright galaxy density, being very close to zero for the densest environment considered here and reaching β = −0.4 for voids.

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“…Thus, if LSBGs are progenitors of BCGs, they first must reduce the angular momentum of the gas during the transition phase, in order to increase the H I surface density and thereby the SFR. In a similar discussion, Staveley-Smith et al [150] concluded that LSBGs and BCGs as classes probably were unrelated. An important issue concerns the H 2 content.…”

Section: Gas Contentmentioning

confidence: 91%

Star Forming Dwarf Galaxies

Bergvall¹

2011

Astrophysics and Space Science Proceedings

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Star forming dwarf galaxies (SFDGs) have a high gas content and low metallicities, reminiscent of the basic entities in hierarchical galaxy formation scenarios. In the young universe they probably also played a major role in the cosmic reionization. Their abundant presence in the local volume and their youthful character make them ideal objects for detailed studies of the initial stellar mass function (IMF), fundamental star formation processes and its feedback to the interstellar medium. Occasionally we witness SFDGs involved in extreme starbursts, giving rise to strongly elevated production of super star clusters and global superwinds, mechanisms yet to be explored in more detail. SFDGs is the initial state of all dwarf galaxies and the relation to the environment provides us with a key to how different types of dwarf galaxies are emerging. In this review we will put the emphasis on the exotic starburst phase, as it seems less important for present day galaxy evolution but perhaps fundamental in the initial phase of galaxy formation.

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H I and optical observations of dwarf galaxies

Cited by 111 publications

References 0 publications

Nebular abundances of nearby southern dwarf galaxies

Nebular abundances of nearby southern dwarf galaxies

Studies of galaxies in voids

Star Forming Dwarf Galaxies

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