arXiv 2102.091902021-02-18astro-ph.GA

邻近类星体主星系的多样形态、恒星星族和黑洞标度关系

The Diverse Morphology, Stellar Population, and Black Hole Scaling Relations of the Host Galaxies of Nearby Quasars

Yulin Zhao, Luis C. Ho, Jinyi Shangguan, Minjin Kim, Dongyao Zhao, Hua Gao

备注：: 24 pages, 12 figure, 3 tables, accepted for publication in ApJ
DOI：: 10.3847/1538-4357/abe8d4

摘要：

我们利用哈勃空间望远镜3号宽视场相机对35个低红移（$z < 0.5$）Palomar-Green类星体进行了静止标架$B$和$I$成像。我们进行多分量的二维图像分解分离的主机星系从其明亮的活动核，其形态特征，并测量其光度特性。特别注意致力于量化的星系核球的结构参数，确定其$B-I$颜色，并估计其恒星质量。大约有一半的样本，包括较低的亮度（$L_{5100} \lesssim 10^{45}\,\mathrm{erg\,s^{-1}}$），但最高的爱丁顿比类星体，居住在盘星系，往往是酒吧和拥有伪隆起。巨大的恒星质量、大的有效半径和微弱的表面亮度表明，最明亮的类星体的宿主星系大多是椭圆星系。主要的合并只占我们样本的一小部分（$\lesssim 20\%$）。我们的类星体样本大致服从黑洞质量和宿主星系（球、核、总）恒星质量之间的标度关系。黑洞质量大于$\sim 10^8\,M_\odot$的星系的行为类似于经典的凸起和早型星系，而那些质量较小的黑洞，特别是窄线塞弗特1，是与晚型星系中的伪凸起一致。宿主星系的凸起，无论它们是经典的还是伪的，都遵循不活跃的经典凸起和椭圆星系的有效半径和平均有效表面亮度之间的相对紧密的反比关系。我们认为，伪隆起经历最近或正在进行的核恒星形成。

英文摘要：

We present rest-frame $B$ and $I$ imaging of 35 low-redshift ($z < 0.5$) Palomar-Green quasars using the Hubble Space Telescope Wide Field Camera 3. We perform multi-component two-dimensional image decomposition to separate the host galaxy from its bright active nucleus, characterize its morphology, and measure its photometric properties. Special care is devoted to quantifying the structural parameters of the galaxy bulge, determine its $B-I$ color, and estimate its stellar mass. Roughly half of the sample, comprising the less luminous ($L_{5100} \lesssim 10^{45}\,\mathrm{erg\,s^{-1}}$) but most high Eddington ratio quasars, reside in disk galaxies that are often barred and possess pseudo bulges. The large stellar masses, large effective radii, and faint surface brightnesses suggest that the host galaxies of the most luminous quasars are mostly ellipticals. Major mergers constitute only a minority ($\lesssim 20\%$) of our sample. Our quasar sample roughly obeys the scaling relations between black hole mass and host galaxy (bulge, core, total) stellar mass. Hosts with black holes more massive than $\sim 10^8\,M_\odot$ behave similarly to classical bulges and early-type galaxies, while those with less massive black holes, particular the narrow-line Seyfert 1s, are consistent with pseudo bulges in late-type galaxies. The host galaxy bulges, irrespective of whether they are classical or pseudo, follow the relatively tight inverse relation between effective radius and mean effective surface brightness of inactive classical bulges and ellipticals. We argue that pseudo bulges experience recent or ongoing nuclear star formation.

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