490 research outputs found
Discovery of a massive variable star with Z=Zo/36 in the galaxy DDO 68
The Local Volume dwarf galaxy DDO 68, from the spectroscopy of its two
brightest HII regions (Knots 1 and 2) was designated as the second most
metal-poor star-forming galaxy [12+log(O/H)=7.14]. In the repeated spectral
observations in 2008 January with the 6-m telescope (BTA) of the HII region
Knot 3 [having 12+log(O/H)=7.10+-0.06], we find a strong evidence of a
transient event related to a massive star evolution. From the follow-up
observation with the higher spectral resolution in 2008 February, we confirm
this phenomenon, and give parameters of its emission-line spectrum comprising
of Balmer HI and HeI lines. The luminosities of the strongest transient lines
(Ha, Hb) are of a few 10^36 erg s^-1. We also detected an additional continuum
component in the new spectrum of Knot 3, which displays the spectral energy
distribution raising to ultraviolet. The estimate of the flux of this continuum
leads us to its absolute V-band magnitude of ~-7.1. Based on the spectral
properties of this transient component, we suggest that it is related to an
evolved massive star of luminous blue variable type with Z=Zo/36. We briefly
discuss observational constraints on parameters of this unique (in the aspect
of the record low metallicity of the progenitor massive star) event and propose
several lines of its study.Comment: 6 pages, 5 Postscript figures, to appear in MNRAS Letters in June
2008 issu
Search for and study of extremely metal-deficient galaxies
We summarize the progress in identifying and observational study of extremely
metal-deficient (XMD) gas-rich galaxies (BCGs, dIr and LSBDs). Due to volume
limitations only following issues are addressed: sample creation, some
statistical data, Colour-Magnitude Diagrams (CMD) and ages, the case of SBS
0335--052 system, and probable evolution paths of various XMD objects.Comment: 4 pages, 3 figures. To appear in the proceedings of Euroconference
"The evolution of galaxies. III. From simple approaches to self-consistent
models" Kiel, Germany, July 200
Environment status of blue compact galaxies and trigger of star formation
(abridged) The work studies active star formation (SF) and a possible trigger
of SF bursts due to gravitational interaction. Following the study by Taylor et
al. we extend the search for possible disturbing galaxies of various masses to
a much larger sample of 86 BCGs from the sky region of Second Byurakan survey.
The sample under study is separated by the criteria: EW([O III]5007 > 45 A and
V < 6,000 km/s and should be representative of all low-mass galaxies which
experience SF bursts. We argue that the moderate tidal disturbers should be
taken into account, and incorporate the respective range of distances in the
search for disturbing neighbours. The majority of the neighbours in the
vicinity of the studied BCGs are found through the study of their environment
among UZC galaxies, and the follow-up careful search of the fainter galaxies in
the NED database. For the remaining BCGs, the neighbouring galaxies are found
based on the results of the 6-m telescope spectroscopy. By studing the data on
the radial velocities of galaxies in the vicinity of BCGs we found: 1) 33 of
the studied BCGs (38.5 %) are associated with significantly brighter galaxies
(DB > 1.5 mag); 2) 23 BCGs (26.5%) have neighbours either of comparable or
significantly lower brightness; 3) 14 of the studied BCGs (16%) with no evident
associated galaxy are either certain, or probable, mergers. We conclude that in
\~80% (or more) BCGs from the studied sample, the SF bursts are triggered
either by tidal action of various strengths from other galaxies, or due to
mergers of low-mass galaxies. We briefly discuss the implications of our main
conclusion for evolutionary links of BCGs to other types of low-mass galaxies.
Among the ``isolated'' BCGs (without a bright neighbour) 43+-10% are probably
disturbed by dwarf galaxies and 26+-8% have a merger morphology.Comment: 22 pages, 7 figures, accepted to A&A on March 26, 200
On the metallicities of UM 133, UM 283 and UM 382
The study of group properties of the extremely metal-deficient gas-rich local
dwarfs is very promising for the understanding the galaxy formation process at
high redshifts. About 20 such objects have been picked up from the literature
in the recent review by Kunth & Ostlin(2000). However part of these galaxies
got low metallicity as a result of earlier observations, and can have rather
large uncertainties in their cited element abundances. Before to perform the
detailed studies of such galaxies as of some extreme group, it is useful to
revise their metallicities. We present the results of the SAO 6m telescope
spectrophotometry of two Blue Compact Galaxies (BCG) reported from earlier
studies as very metal-poor objects. Well measured [O III] line 4363 A allows to
deduce the temperature in HII regions and get reliable abundances of chemical
elements. For UM 133 we derive 12+log(O/H) = 7.63+/-0.02, coincident with the
published value. UM 382, according to our data, is significantly more
metal-rich: its 12+log(O/H) = 7.82+/-0.03 in comparison to the published value
7.45. The third galaxy, UM 283 seems have got its very low 12+log(O/H) = 7.59
due to a misprint. We used its published emission line intensities and derived
instead the value of 7.95. Thus the latter two galaxies should NOT be
considered as the extremely metal-poor BCGs.Comment: 5 pages, 2 figures, A&A in pres
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