443 research outputs found
The most metal-poor galaxies
Metallicity is a key parameter that controls many aspects in the formation
and evolution of stars and galaxies. In this review we focus on the metal
deficient galaxies, in particular the most metal-poor ones, because they play a
crucial role in the cosmic scenery. We first set the stage by discussing the
difficult problem of defining a global metallicity and how this quantity can be
measured for a given galaxy. The mechanisms that control the metallicity in a
galaxy are reviewed in detail and involve many aspects of modern astrophysics:
galaxy formation and evolution, massive star formation, stellar winds, chemical
yields, outflows and inflows etc. Because metallicity roughly scales as the
galactic mass, it is among the dwarfs that the most metal-poor galaxies are
found. The core of our paper reviews the considerable progress made in our
understanding of the properties and the physical processes that are at work in
these objects. The question on how they are related and may evolve from one
class of objects to another is discussed. While discussing metal-poor galaxies
in general, we present a more detailed discussion of a few very metal-poor blue
compact dwarf galaxies like IZw18. Although most of what is known relates to
our local universe, we show that it pertains to our quest for primeval galaxies
and is connected to the question of the origin of structure in the universe. We
discuss what QSO absorption lines and known distant galaxies tell us already?
We illustrate the importance of star-forming metal-poor galaxies for the
determination of the primordial helium abundance, their use as distance
indicator and discuss the possibility to detect nearly metal-free galaxies at
high redshift from Ly emission.Comment: 96 pages, 12 figures. To appear in the A&A Review. Version including
proof correction
High Carbon in I Zwicky 18: New Results from Hubble Space Telescope Spectroscopy
We present new measurements of the gas-phase C/O abundance ratio in both the
NW and SE components of the extremely metal-poor dwarf irregular galaxy I Zw
18, based on ultraviolet spectroscopy of the two H II regions using the Faint
Object Spectrograph on the Hubble Space Telescope. We determine values of log
C/O = -0.63 +/- 0.10 for the NW component and log C/O = -0.56 +/- 0.09 for the
SE component. In comparison, log C/O = -0.37 in the sun, while log C/O = -0.85
+/- 0.07 in the three most metal-poor irregular galaxies measured by Garnett et
al. (1995a). Our measurements show that C/O in I Zw 18 is significantly higher
than in other comparably metal-poor irregular galaxies, and above predictions
for the expected C/O from massive star nucleosynthesis. These results suggest
that carbon in I Zw 18 has been enhanced by an earlier population of lower-mass
carbon producing stars; this idea is supported by stellar photometry of I Zw 18
and its companion, which demonstrate that the current bursts of massive stars
were not the first. Despite its very low metallicity, it is likely that I Zw 18
is not a ``primeval'' galaxy.Comment: 14 pages including 4 figures; uses aaspp4.sty. Accepted for
publication in ApJ. Postscript version also available by e-mail request to
author at [email protected]
Extended Tidal Structure In Two Lyman Alpha-Emitting Starburst Galaxies
We present new VLA C-configuration HI imaging of the Lyman Alpha-emitting
starburst galaxies Tol 1924-416 and IRAS 08339+6517. The effective resolution
probes neutral gas structures larger than 4.7 kpc in Tol 1924-416, and larger
than 8.1 kpc in IRAS 08339+6517. Both systems are revealed to be tidally
interacting: Tol 1924-416 with ESO 338-IG04B (6.6 arcminutes = 72 kpc minimum
separation), and IRAS 08339+6517 with 2MASX J08380769+6508579 (2.4 arcminutes =
56 kpc minimum separation). The HI emission is extended in these systems, with
tidal tails and debris between the target galaxies and their companions. Since
Lyman Alpha emission has been detected from both of these primary systems,
these observations suggest that the geometry of the ISM is one of the factors
affecting the escape fraction of Lyman Alpha emission from starburst
environments. Furthermore, these observations argue for the importance of
interactions in triggering massive star formation events.Comment: ApJ, in press; 11 pages, 2 color figure
POX 186: the ultracompact Blue Compact Dwarf Galaxy reveals its nature
High resolution, ground based R and I band observations of the ultra compact
dwarf galaxy POX 186 are presented. The data, obtained with the ESO New
Technology Telescope (NTT), are analyzed using a new deconvolution algorithm
which allows one to resolve the innermost regions of this stellar-like object
into three Super-Star Clusters (SSC). Upper limits to both masses (M\sim 10^5
M_{\odot}) and the physical sizes (\le 60pc) of the SSCs are set. In addition,
and maybe most importantly, extended light emission underlying the compact
star-forming region is clearly detected in both bands. The R-I color rules out
nebular H\alpha contamination and is consistent with an old stellar population.
This casts doubt on the hypothesis that Blue Compact Dwarf Galaxies (BCDG) are
young galaxies.Comment: 4 figures postscript, 2 tables, to appear in A&A main journa
HST observations of the blue compact dwarf SBS 0335-052: a probable young galaxy
We present HST WFPC2 V and I images and GHRS UV spectrophotometry of the
spectral regions around Ly and OI 1302 of the extremely metal-deficient
(Z~Zsun/41) blue compact dwarf (BCD) galaxy SBS 0335-052. All the star
formation in the BCD occurs in six super-star clusters (SSC) with ages =< 3-4
Myr. Dust is clearly present and mixed spatially with the SSCs. There is a
supershell of radius ~380 pc, delineating a large supernova cavity. The
instantaneous star formation rate is ~0.4 Msun yr^-1. Strong narrow Ly
emission is not observed. Rather there is low intensity broad (FWZI = 20 A)
Ly emission superposed on even broader Ly absorption by the HI
envelope. This broad low-intensity emission is probably caused by resonant
scattering of Ly photons. The BCD appears to be a young galaxy,
undergoing its very first burst of star formation. This conclusion is based on
the following evidence: 1) the underlying extended low-surface-brightness
component is very irregular and filamentary, suggesting that a significant part
of the emission comes from ionized gas; 2) it has very blue colors (-0.34 =<
(V-I) =< 0.16), consistent with gaseous emission colors; 3) the OI 1302
line is not detected in absorption in the GHRS spectrum, setting an upper limit
for N(O)/N(H) in the HI envelope of the BCD of more than 3000 times smaller
than the value in Orion.Comment: 20 pages and 6 Postscript figures. Submitted to Astrophysical Journa
Rest-Frame Ultraviolet Spectra of z~3 Lyman Break Galaxies
We present the results of a systematic study of the rest-frame UV
spectroscopic properties of Lyman Break Galaxies (LBGs). The database of almost
1000 LBG spectra proves useful for constructing high S/N composite spectra. The
composite spectrum of the entire sample reveals a wealth of features
attributable to hot stars, HII regions, dust, and outflowing neutral and
ionized gas. By grouping the database according to galaxy parameters such as
Lyman-alpha equivalent width, UV spectral slope, and interstellar kinematics,
we isolate some of the major trends in LBG spectra which are least compromised
by selection effects. We find that LBGs with stronger Lyman-alpha emission have
bluer UV continua, weaker low-ionization interstellar absorption lines, smaller
kinematic offsets between Lyman-alpha and the interstellar absorption lines,
and lower star-formation rates. There is a decoupling between the dependence of
low- and high-ionization outflow features on other spectral properties. Most of
the above trends can be explained in terms of the properties of the large-scale
outflows seen in LBGs. According to this scenario, the appearance of LBG
spectra is determined by a combination of the covering fraction of outflowing
neutral gas which contains dust, and the range of velocities over which this
gas is absorbing. Higher sensitivity and spectral resolution observations are
still required for a full understanding of the covering fraction and velocity
dispersion of the outflowing neutral gas in LBGs, and its relationship to the
escape fraction of Lyman continuum radiation in galaxies at z~3.Comment: 28 pages including 17 figures. Accepted for publication in Ap
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