Spectroscopy of Dwarf Galaxies in the Virgo Cluster. I. Data, Chemical Abundances, and Ionization Structure

Vı́lchez, J. M.; Iglésias-Páramo, J.

doi:10.1086/345999

Cited by 49 publications

(40 citation statements)

References 74 publications

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“…Izotov et al 1997b;Vílchez & Iglesias-Páramo 1998;Kehrig et al 2008), we did not find any significant chemical abundance variation among the different knots in the galaxy, which points to a common chemical evolution scenario in all of them. Also, the nitrogen-to-oxygen abundance ratio values found are consistent with those obtained for BCDs and H ii galaxies (Vílchez & Iglesias-Páramo 2003;Pérez-Montero & Díaz 2005).…”

Section: Discussionsupporting

confidence: 88%

Mapping the starburst in blue compact dwarf galaxies

Cairós

Caon

Zurita

et al. 2009

A&A

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Aims. By means of optical integral field spectroscopy observations, we aim to differentiate and characterize the starburst component in the blue compact dwarf (BCD) galaxy Mrk 1418. In particular we propose to study the stellar and ionized gas morphology, to investigate the ionization mechanism(s) acting in the interstellar medium, and to derive the physical parameters and abundances of the ionized gas. Methods. Integral field spectroscopy observations of Mrk 1418 were carried out with the Potsdam multi-aperture spectrophotometer (PMAS) at the 3.5 m telescope at Calar Alto Observatory. The central 16 × 16 (1.14 × 1.14 kpc 2 at the distance of Mrk 1418) were mapped with a spatial sampling of 1 ; we took data in the 3590−6996 Å spectral range, with a linear dispersion of 3.2 Å per pixel.The seeing was about 1. 5. From these data we built maps of the most prominent emission lines, namely Results. Mrk 1418 shows a distorted morphology both in the continuum and in the ionized gas maps; the current star-formation episode is taking place in five knots, distributed around the nucleus of the galaxy. The interstellar medium surrounding these knots is photo-ionized by stars, with no clear evidence for other excitation mechanisms. The galaxy displays an inhomogeneous dust distribution, with the high Hα/Hβ ratio in the central areas indicating a large amount of dust. The oxygen abundances derived for the individual star-forming knots are very similar, suggesting that the ionized interstellar medium is chemically homogeneous in O/H over spatial scales of hundreds of parsecs. This abundance (Z ≈ 0.4 Z from the empirical calibrations) places Mrk 1418 among the high metallicity BCD group. Conclusions. These findings show the advantages of IFS when investigating the properties of such complex objects as BCDs, with an asymmetric star-forming component. Only a bidimensional mapping of their central regions allows approaching such questions as the star formation processes in BCDs, the star-forming history of the individual starburst knots, or the abundance gradients.

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Section: Discussionsupporting

confidence: 88%

Mapping the starburst in blue compact dwarf galaxies

Cairós

Caon

Zurita

et al. 2009

A&A

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“…Since the [Oii] λ3727 nebular line is outside the observed wavelength range of the SDSS spectra, we estimated the oxygen abundances following the method of Pilyugin & Thuan (2007). Our estimates agree, within the errors, with the measurements available in the literature for VCC 562 2 and VCC 1179 (Vílchez & Iglesias-Páramo 2003). The basic parameters of the three galaxies are given in Table 1.…”

Section: Sample Selectionsupporting

confidence: 56%

TheHerschelVirgo Cluster Survey

Grossi¹,

Hunt

Madden

et al. 2010

A&A

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We present the dust properties of a small sample of Virgo cluster dwarf galaxies drawn from the science demonstration phase data set of the Herschel Virgo Cluster Survey. These galaxies have low metallicities (7.8 < 12 + log(O/H) < 8.3) and star-formation rates < ∼ 10 −1 M yr −1 . We measure the spectral energy distribution (SED) from 100 to 500 μm and derive dust temperatures and dust masses. The SEDs are fitted by a cool component of temperature T ∼ < 20 K, implying dust masses around 10 5 M and dust-to-gas ratios D within the range 10 −3 −10 −2 . The completion of the full survey will yield a larger set of galaxies, which will provide more stringent constraints on the dust content of star-forming dwarf galaxies.

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“…The bright galaxies are consistent with the SDSS sample, but the faint end is elevated in metallicity above SDSS at a constant metallicity with luminosity (12 + log(O/H) = 8.46 ± 0.04). We note that Figure 21 of We plot dwarf galaxies belonging to various local clusters as triangles in Figure 6: Virgo (Vaduvescu et al 2007;Vílchez & Iglesias-Páramo 2003), Hercules , Fornax (Vaduvescu et al 2011), and Hydra (Vaduvescu et al 2011;Duc et al 2001). In general, these objects tend toward lower metallicity with faint luminosity.…”

Section: Additional Dwarf Galaxy Control Samplesmentioning

confidence: 99%

Choirs H I Galaxy Groups: The Metallicity of Dwarf Galaxies

Sweet

Drinkwater

Meurer

et al. 2014

ApJ

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We present a recalibration of the luminosity-metallicity relation for gas-rich, star-forming dwarfs to magnitudes as faint as M R ∼ −13. We use the Dopita et al. metallicity calibrations to calibrate the relation for all the data in this analysis. In metallicity-luminosity space, we find two subpopulations within a sample of high-confidence Sloan Digital Sky Survey (SDSS) DR8 star-forming galaxies: 52% are metal-rich giants and 48% are metal-medium galaxies. Metal-rich dwarfs classified as tidal dwarf galaxy (TDG) candidates in the literature are typically of metallicity 12 + log(O/H) = 8.70 ± 0.05, while SDSS dwarfs fainter than M R = −16 have a mean metallicity of 12 + log(O/H) = 8.28 ± 0.10, regardless of their luminosity, indicating that there is an approximate floor to the metallicity of low-luminosity galaxies. Our hydrodynamical simulations predict that TDGs should have metallicities elevated above the normal luminosity-metallicity relation. Metallicity can therefore be a useful diagnostic for identifying TDG candidate populations in the absence of tidal tails. At magnitudes brighter than M R ∼ −16, our sample of 53 star-forming galaxies in 9 H i gas-rich groups is consistent with the normal relation defined by the SDSS sample. At fainter magnitudes, there is an increase in dispersion of the metallicity of our sample, suggestive of a wide range of H i content and environment. In our sample, we identify three (16% of dwarfs) strong TDG candidates (12 + log(O/H) > 8.6) and four (21%) very metal-poor dwarfs (12 + log(O/H) < 8.0), which are likely gas-rich dwarfs with recently ignited star formation.

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Spectroscopy of Dwarf Galaxies in the Virgo Cluster. I. Data, Chemical Abundances, and Ionization Structure

Cited by 49 publications

References 74 publications

Mapping the starburst in blue compact dwarf galaxies

Mapping the starburst in blue compact dwarf galaxies

TheHerschelVirgo Cluster Survey

Choirs H I Galaxy Groups: The Metallicity of Dwarf Galaxies

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