Evolutionary Transition of Galaxies

Galaxies的进化过渡被定义为年轻Galaxies中恒星形成活动的一个突然衰退。我们已经建立了一个进化型的星系模型，并将其应用于集群中的椭圆星系。我们找到了一个颜色强度（CM）关系，即平均恒星金属的系统变体，即银河亮度的一个功能，这可能是银河系风模型中最好的解释。我们发现CM关系的演变在很大程度上取决于一个主要恒星形成的epoch。与those of elliptical galaxies in clusters at different redshifts strongly suggests that these galaxies should have formed at zy D2 > 2.5 - 4。We measured equibalent widths of several metallic lines in high redshift （z ~ 3 - 4） quasars and found very strong iron emManagement there。本建议是，这些类人猿宿主星系的最小内部因素已经由Ia型超级新星的模拟器充实。 ... More 所以，这些变化的银河系比SNIA生殖器大，一个典型的生命周期大约是1.5 Gyr。这意味着这些类星体的宿主星系，非常可能的椭圆形星系，形成在Z-D2 F-D2 > 5 - 9上。对集群椭圆形的CO亮度的简单计算，基于我们的CM关系分析，索引在活动恒星形成阶段的CO亮度必须足够高，才能被无线电望远镜检测到。这个合理地解释了为什么我们可以在z = 4.6的quasar中发现CO，如果主机银河是进化过渡前的一个椭圆形过渡。从这些结果来看，我们将椭圆形银河在进化过渡前的椭圆形过渡描述为Z ~ 4 - 5，有可能成为银河系的风，有一个希望，在未来附近进行微米级观测将变得更容易，我们也将能够获得更多如果在这些波浪长度区域的银河系特种，我们已经建立了一个进化型的银河系特种系，它对尘埃吸收和再排放的影响完全被纳入帐户。我们已经应用了一个模型来接近恒星爆炸的星系，并且在被观察到的光学近红外和远红外颜色中取得了成功。自从高redshift的primeval galaxies将非常类似于那些接近Starburst galaxies的人，我们相信我们有一种方法可以在没有任何不确定的情况下产生这些高redshift galaxies的年龄。这将最终引导我们来估计这些原始星系形成的epoch。Less（低）

An evolutionary transition of galaxies is defined as a sudden decline of star forming activity in young galaxies. We have built up an evolutionary model of galaxy spectra and have applied it to elliptical galaxies in clusters. We find that color-magnitude (CM) relation of elipticals is due to a systematic variation of mean stellar metallicity as a function of galaxy luminosity which could be best explained by a galactic wind model. We find that evolution of the CM relation strongly depends on an epoch of major star formation. A detailed comparison of our model CM relation with those of elliptical galaxies in clusters at different redshifts strongly suggests that these galaxies should have formed at zィイD2FィエD2 > 2.5 - 4.We measured equibalent widths of several metallic lines in high redshift (z 〜 3 - 4) quasars and found very strong iron emission there. This suggests that at least interstellar matter of host galaxies of these quasars was already enriched by ejecta of type Ia supernovae. … More Thus, galaxies at these redshifts are older than SNIa progenitors, a typical lifetime of which is around 1.5 Gyr. This means the host galaxies of these quasars, very likely elliptical galaxies, formed at zィイD2FィエD2 > 5 - 9.Simple calculation of CO luminosity of cluster ellipticals, based on our CM relation analysis, indicates that CO luminosity during actively star forming phase must be high enough to be detected by radio telescope. This reasonablly explains why we can detect CO in a quasar at z = 4.6, if the host galaxy is an elliptical before the onset of evolutionary transition.From these results, we conclude that the evolutionary transition in elliptical galaxies occurred at z 〜 4 - 5, possibly due to a galactic wind.With a hope that in near future submillimeter observations will become more easier and we will be able to get more spectra of galaxies in these wavelength region, we have newly built up an evolutionary model of galaxy spectra in which effects of dust absorption and re-emission are fully taken into account. We have applied the model to nearby star burst galaxies and are successful in desentagling age and dutiness from the observed optical-nearinfrared and farinfrared colours. Since primeval galaxies at high redshifts would be very similar to those nearby starburst galaxies, we believe that we have established a way to derive the age of these high redshift galaxies without any uncertainties. This would eventually lead us to estimate the epoch of formation of these primival galaxies. Less