Bibcode
Filho, M. E.; Winkel, B.; Sánchez Almeida, J.; Aguerri, J. A. L.; Amorín, R.; Ascasibar, Y.; Elmegreen, B. G.; Elmegreen, D. M.; Gomes, J. M.; Humphrey, A.; Lagos, P.; Morales-Luis, A. B.; Muñoz-Tuñón, C.; Papaderos, P.; Vílchez, J. M.
Bibliographical reference
Astronomy and Astrophysics, Volume 558, id.A18, 30 pp.
Advertised on:
10
2013
Journal
Citations
50
Refereed citations
44
Description
Context. Extremely metal-poor (XMP) galaxies are chemically, and
possibly dynamically, primordial objects in the local Universe.
Aims: Our objective is to characterize the H i content of the XMP
galaxies as a class, using as a reference the list of 140 known local
XMPs compiled by Morales-Luis et al. (2011). Methods: We have
observed 29 XMPs, which had not been observed before at 21 cm, using the
Effelsberg radio telescope. This information was complemented with H i
data published in literature for a further 53 XMPs. In addition, optical
data from the literature provided morphologies, stellar masses,
star-formation rates and metallicities. Results: Effelsberg H i
integrated flux densities are between 1 and 15 Jy km s-1,
while line widths are between 20 and 120 km s-1. H i
integrated flux densities and line widths from literature are in the
range 0.1-200 Jy km s-1 and 15-150 km s-1,
respectively. Of the 10 new Effelsberg detections, two sources show an
asymmetric double-horn profile, while the remaining sources show either
asymmetric (seven sources) or symmetric (one source) single-peak 21 cm
line profiles. An asymmetry in the H i line profile is systematically
accompanied by an asymmetry in the optical morphology. Typically, the
g-band stellar mass-to-light ratios are ~0.1, whereas the H i gas
mass-to-light ratios may be up to two orders of magnitude larger.
Moreover, H i gas-to-stellar mass ratios fall typically between 10 and
20, denoting that XMPs are extremely gas-rich. We find an
anti-correlation between the H i gas mass-to-light ratio and the
luminosity, whereby fainter XMPs are more gas-rich than brighter XMPs,
suggesting that brighter sources have converted a larger fraction of
their H i gas into stars. The dynamical masses inferred from the H i
line widths imply that the stellar mass does not exceed 5% of the
dynamical mass, while the H i mass constitutes between 20 and 60% of the
dynamical mass. Furthermore, the dark matter mass fraction spans a wide
range, but can account, in some cases, for over 65% of the dynamical
mass. XMPs are found to be outliers of the mass - and luminosity -
metallicity relation, whereby they lack metals for their estimated
dynamical mass and luminosity, suggesting the presence of pristine gas.
However, they generally follow the luminosity - and baryonic mass
Tully-Fisher relation, indicating that the H i gas is partly virialized
and contains some rotational support. 60% of the XMP sources show a
small velocity offset (10-40 km s-1) between the H i gas and
the stellar/nebular component, implying that, in these sources, the H i
gas is not tightly coupled to the stars and ionized gas. The effective
yields provided by oxygen are often larger than the standard theoretical
yields, suggesting that the observed H i gas is relatively metal-free.
80% of the XMP sources present asymmetric optical morphology - 60 XMPs
show cometary structure, 11 show two bright star-forming knots and 18
show multiple star-forming regions. Star-formation rates are found to be
similar to those typically found in BCDs. However, specific
star-formation rates are high, with timescales to double their stellar
mass, at the current rate, of typically less than 1 Gyr.
Conclusions: XMP galaxies are among the most gas-rich objects in the
local Universe. The observed H i component suggests kinematical
disruption and hints at a primordial composition.
Full Fig. 1, Tables 3-5 are available in electronic form at http://www.aanda.orgReduced spectra are
only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/558/A18
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