• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Star formation and AGN activity in galaxies classified using the 1.6 μm bump and PAH features at z = 0.4-2
【24h】

Star formation and AGN activity in galaxies classified using the 1.6 μm bump and PAH features at z = 0.4-2

机译：使用1.6μm凸点和PAH特征在z = 0.4-2处分类的星系中的恒星形成和AGN活性

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

We studied the star-formation and AGN activity of massive galaxies in the redshift range z = 0.4-2, which were detected in a deep survey field using the AKARI InfraRed (IR) astronomical satellite and Subaru telescope toward the North Ecliptic Pole (NEP). The AKARI/IRC Mid-InfraRed (MIR) multiband photometry was used to trace the starforming activities with Polycyclic Aromatic Hydrocarbon (PAH) emission, which is effective not only to distinguish between star-forming and AGN galaxies, but also to estimate the Star Formation Rate (SFR) with converting its flux to the total emitting IR (TIR) luminosity. In combination with the analyses of the stellar components, we studied the MIR SED features of star-forming and AGN-harboring galaxies, which we summarize below: (1) The rest-frame 7.7-μm and 5-μm luminosities are good tracers of star-forming and AGN activities from their PAH and dusty tori emissions, respectively. (2) For dusty star-forming galaxies without AGN, their SFR shows a correlation that is nearly proportional to their stellar mass, and their specific SFR (sSFR) per unit stellar mass increases with redshift. Extinctions estimated from their TIR luminosities are larger than those from their optical SED fittings, which may be caused by geometric variations of dust in them. (3) Even for dusty star-forming galaxies with AGN, SFRs can be derived from their TIR luminosities with subtraction of the obscured AGN contribution, which indicates that their SFRs were possibly quenched around z ? 0.8 compared with those without AGN. (4) The AGN activity from their rest-frame 5-μm luminosity suggests that their Super Massive Black Holes (SMBHs) could already have grown to ? 3 × 10 ~8M ⊙ in most massive galaxies with 10 ~11M ⊙ at z > 1.2, and the mass relation between SMBHs and their host galaxies has already become established by z ? 1-2.
机译：我们研究了在红移范围z = 0.4-2中的大型星系的恒星形成和AGN活动，这些星系是使用AKARI红外（IR）天文卫星和斯巴鲁望远镜朝北黄极（NEP）在深层调查场中检测到的。 AKARI / IRC中红外（MIR）多波段光度法用于跟踪多环芳烃（PAH）发射的恒星形成活动，这不仅有效区分了恒星形成星系和AGN星系，而且还估计了恒星形成速率（SFR），将其通量转换为总发射IR（TIR）光度。结合对恒星成分的分析，我们研究了恒星形成星系和AGN携带星系的MIR SED特征，总结如下：（1）7.7-μm和5μm的其余帧光度是对分别来自其PAH和粉尘托里排放的恒星形成活动和AGN活动。 （2）对于没有AGN的尘埃状恒星形成星系，它们的SFR显示出与其恒星质量几乎成正比的相关性，并且每单位恒星质量的比SFR（sSFR）随着红移而增加。从其TIR亮度估算的消光比从其光学SED配件估算的消光大，这可能是由于它们中灰尘的几何变化引起的。 （3）即使对于具有AGN的尘埃形成恒星星系，SFR仍可从其TIR光度中减去模糊的AGN贡献得出，这表明它们的SFR可能在z？附近淬灭。与没有AGN的患者相比为0.8。 （4）从其静止帧5μm的光度得出的AGN活性表明，他们的超大规模黑洞（SMBH）可能已经成长为？在大多数大型星系中，3×10〜8M most在z> 1.2时具有10〜11M⊙，并且SMBH和它们的宿主星系之间的质量关系已经由z确立。 1-2。

著录项

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号