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![Relationship between z and M B for the two types of starburst galaxies as compared to the irregular and normal spiral galaxies. The metallicity is given by [O/H] = log(O/H) gal-log(O/H) ⊙. The giant spirals and irregular galaxies follow a slightly steeper relation than the elliptical and the dSph, while the relationship is flatter for the starburst galaxies.](profile/Roger-Coziol/publication/1812714/figure/fig1/AS:669964784660543@1536743460935/Relationship-between-z-and-M-B-for-the-two-types-of-starburst-galaxies-as-compared-to-the.png)
Relationship between z and M B for the two types of starburst galaxies as compared to the irregular and normal spiral galaxies. The metallicity is given by [O/H] = log(O/H) gal-log(O/H) ⊙. The giant spirals and irregular galaxies follow a slightly steeper relation than the elliptical and the dSph, while the relationship is flatter for the starburst galaxies.
Source publication
In a diagram of metallicity (\~z) vs. luminosity (M$_B$), the different types of nearby (Z $< 0.05$) starburst galaxies seem to follow the same linear relationship as the normal spiral and irregular galaxies. However, for comparable luminosities the more massive starburst nucleus galaxies (SBNGs) show a slight metallic defficiency as compared to th...
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Citations
We present an analysis of the spectra of 62 galaxies in 15 compact groups. The galaxies are classified into four activity classes: galaxies without emission, starburst galaxies, luminous AGNs (Seyfert and LINERs), and low-luminosity AGNs (LLAGNs). The star formation in the Hickson compact group (HCG) starbursts is more intense than in normal spirals, but comparable to that observed in starburst-nucleus galaxies (SBNGs) in the field. In general, the HCG starbursts have mean solar gas metallicity and do not follow the metallicity-luminosity relation traced by the early-type SBNGs in the field, suggesting that most of them are late-type SBNGs. This morphology preference, coupled with the observation that the HCG starbursts are predominantly located in the halos of the groups, is consistent with the idea that compact groups are embedded in sparser structures. The stellar metallicities of the nonstarburst galaxies are comparable to those observed in normal galaxies with similar morphologies, but are relatively high for their luminosities. In these galaxies, the metal absorption line equivalent widths are slightly narrower than normal, while the Balmer absorption lines are relatively strong. All these observations suggest the presence of a population of intermediate-age stars. These galaxies could be poststarburst, but at a very advanced stage of evolution, the last bursts having happened more than 2 Gyr in the past. Our observations support a scenario in which the cores of the groups are slowly collapsing evolved systems embedded in more extended structures. In the cores of the groups, the interactions were more frequent and the galaxies evolved at a more rapid rate than in their halos.
The metallicities derived from spectroscopic observations of a sample of starburst nucleus galaxies (SBNGs) are compared with those of several other types of galaxies (normal giant, irregular, and H II galaxies) drawn from the literature. The SBNGs are deficient in metals with respect to normal galaxies of same morphological type, suggesting that SBNGs are galaxies still in the process of formation.
Breaking the SBNGs into early types (Sb and earlier) and late types reveals that the former seem to follow the same linear luminosity-metallicity relation as the irregular and elliptical galaxies, whereas the latter and the giant spirals show comparable (0.2 and 0.3 dex) excess abundances with respect to the linear relation. This difference between the two types of SBNGs is consistent with the predictions of the model of hierarchical formation of galaxies: the early-type SBNGs are building their bulges by successive mergers of small stellar and gaseous systems, while the late-type SBNGs are mostly accreting gas to form a disk.
