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首页> 外文期刊>The Astrophysical journal >AGE, EVOLUTION, AND DISPERSION OF THE LOOSE GROUPS OF BLUE STARS IN THE NORTHEAST RADIO LOBE OF CENTAURUS A
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AGE, EVOLUTION, AND DISPERSION OF THE LOOSE GROUPS OF BLUE STARS IN THE NORTHEAST RADIO LOBE OF CENTAURUS A

机译：CENTURUS东北射电瓣内蓝星松散群的年龄，演化和散布。

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The association of shocked gas and loose groups of young stars in the northeast radio lobe of Cen-taurus A (NGC 5128) provides direct evidence for shock-induced star formation. In this paper, we present UBV photometry of the blue stars based on observations made with the 2.5 m du Pont Telescope at Las Campanas Observatory. In a field covering 8.8′ x 8.8′, three groups are identified. Color-magnitude and color-color diagrams are plotted for each group. Two-color photometry of the many foreground field stars belonging to our own Galaxy indicates a foreground reddening E_(B-V) = 0.14 mag ±0.02 mag. The new photometry is compared with that carried out in a small section of the field with the Hubble Space Telescope. The HST frames, in conjunction with the ground-based material allow compact star clusters to be identified, some of which are exciting small H Ⅱ regions. Positions, finding charts, and photometry are given for 50 stars with V < 23.0 mag and (B— V) < 0.4 mag. The brightest blue star, at V = 19.94 mag, has an estimated absolute visual magnitude M_V = —8.2 mag, which is comparable to that of the brightest A-type supergiants in the Large Magellanic Cloud. Most of the blue stars lie just inside the 1.4 GHz contours of the large-scale jetlike feature recently detected by Morganti et al. It is suggested that rather than being a component of the jet that powers the radio lobes, this feature, which resembles a spiral arm of a normal galaxy, results from compression of ambient gas by the jet. Bolometric magnitudes and effective temperatures are derived for the bright blue stars and plotted. Iso-chrones based on the Geneva evolutionary tracks are fitted and indicate a significant age spread for the stars extending up to 15 million years. The older stars are distributed more widely than the younger stars indicating that star formation extends over time and that the blue stars eventually disperse into the extended stellar envelope of the galaxy.
机译：Cen-taurus A（NGC 5128）东北无线电波瓣中的冲击气体和年轻恒星散落群之间的联系为冲击引起的恒星形成提供了直接证据。在本文中，我们基于在Las Campanas天文台用2.5 m du Pont望远镜进行的观测，介绍了蓝星的UBV光度法。在一个覆盖8.8'x 8.8'的字段中，确定了三个组。为每个组绘制了色度图和色图。属于我们自己的银河系的许多前景场恒星的双色测光表明前景发红E_（B-V）= 0.14 mag±0.02 mag。将新的测光法与使用哈勃太空望远镜在小范围内进行的测光法进行了比较。 HST框架与地面材料相结合，可以识别出紧凑的星团，其中一些是令人兴奋的HⅡ小区域。给出了V <23.0 mag和（BV）<0.4 mag的50颗恒星的位置，寻找图表和测光法。在V = 19.94 mag时，最亮的蓝星具有估计的绝对视觉大小M_V = -8.2 mag，可与麦哲伦星云中最亮的A型超巨星相比。 Morganti等人最近发现，大多数蓝星都位于大规模射流状特征的1.4 GHz轮廓内。有人提出，该特征不是射束为无线电波提供动力的组成部分，而是正常星系的旋臂，它是由射流压缩环境气体引起的。得出明亮的蓝色恒星的吸光度值和有效温度，并将其绘制出来。拟合了基于日内瓦演化轨道的等时线，表明恒星的年龄分布显着延长到1500万年。年长的恒星比年幼的恒星分布更广泛，这表明恒星的形成随着时间的流逝而扩展，而蓝色的恒星最终散布到银河系延伸的恒星包络中。

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