BLACK HOLE AND GALAXY COEVOLUTION FROM CONTINUITY EQUATION AND ABUNDANCE MATCHING
BLACK HOLE AND GALAXY COEVOLUTION FROM CONTINUITY EQUATION AND ABUNDANCE MATCHING
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DOI：
10.1088/0004-637x/810/1/74
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发表时间：
2015-09-01
影响因子：
4.9
通讯作者：
Danese, L.
中科院分区：
文献类型：
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作者：
Aversa, R.;Lapi, A.;Danese, L.
我们用基于连续性方程和丰度匹配技术的统计方法研究了星系和托管超大质量黑洞(BHS)在整个宇宙历史上的共同演化。具体地说，我们给出了不含源项的连续性方程的解析解。从活动星系核(AGN)光度函数重建超大质量BH质量函数。这种方法包括在独立数据集上测试物理激励的活动星系核的光曲线，该曲线描述了爱丁顿比和辐射效率从薄盘到薄盘的演变。条件。我们很好地复制了BH质量函数、活动星系核占空比与质量和红移的函数的局部估计，以及爱丁顿比函数和具有给定恒星质量的星系以给定的爱丁顿比拥有活动星系核的比例。我们采用了同样的方法来重建与星系中恒星形成相关的紫外光和远红外光度函数在不同红移下的观测恒星质量函数。这些结果表明，恒星和黑洞在星系中的积累是通过原位过程进行的，干合并至少在恒星质量方面起到了微不足道的作用。小于或类似3 x 10(11)M圆点和BH质量小于或类似于10(9)M圆点，其中统计数据更安全且受系统误差的影响较小。此外，我们开发了一种改进的丰度匹配技术，将星系的恒星和BH含量与引力主导的暗物质(DM)分量联系起来。由此产生的关系构成了星系演化模型的试验台，突出了恒星和活动星系核反馈在恒星形成过程中的互补作用。此外，它们还可以在数值模拟中实施，以填充DM晕或测量次网格物理。此外，它们可能被用来研究星系/活动星系核星团作为红移、质量和/或光度的函数。事实上，BHS和星系的星系团性质与目前的观测结果完全一致，从而进一步验证了我们从连续性方程得到的结果。最后，我们的分析强调了(I)在细盘中观察到的活动星系核的比例。(2)已经在z大于或类似于6。一定是在小于或类似于10(8)年的时间尺度上形成了大量尘埃。在恒星形成强烈的星系中，使这些源完全在(亚)毫米波段的ALMA调查范围内。
We investigate the coevolution of galaxies and hosted supermassive black holes (BHs) throughout the history of the universe by a statistical approach based on the continuity equation and the abundance matching technique. Specifically, we present analytical solutions of the continuity equation without source terms. to reconstruct the supermassive BH mass function from the active galactic nucleus (AGN) luminosity functions. Such an approach includes physically motivated AGN light curves tested on independent data sets, which describe the evolution of the Eddington ratio and radiative efficiency from slim-to thin-disk. conditions. We nicely reproduce the local estimates of the BH mass function, the AGN duty cycle as a function of mass and redshift, along with the Eddington ratio function and the fraction of galaxies with given stellar mass hosting an AGN with given Eddington ratio. We exploit the same approach to reconstruct the observed stellar mass function at different redshift from the ultraviolet and far-IR luminosity functions associated with star formation in galaxies. These results imply that the build-up of stars and BHs in galaxies occurs via in situ processes, with dry mergers playing a marginal role at least for stellar masses. less than or similar to 3 x 10(11) M-circle dot and BH masses less than or similar to 10(9) M-circle dot, where the statistical data are more secure and less biased by systematic errors. In addition, we develop an improved abundance matching technique to link the stellar and BH content of galaxies to the gravitationally dominant dark matter (DM) component. The resulting relationships constitute a testbed for galaxy evolution models, highlighting the complementary role of stellar and AGN feedback in the star formation process. In addition, they may be operationally implemented in numerical simulations to populate DM halos or to gauge subgrid physics. Moreover, they may be exploited to investigate the galaxy/AGN clustering as a function of redshift, mass, and/or luminosity. In fact, the clustering properties of BHs and galaxies are found to be in full agreement with current observations, thus further validating our results from the continuity equation. Finally, our analysis highlights that (i) the fraction of AGNs observed in the slim-disk. regime, where most of the BH mass is accreted, increases with redshift; and (ii) already at z greater than or similar to 6. a substantial amount of dust must have formed over timescales less than or similar to 10(8) yr. in strongly star-forming galaxies, making these sources well within the reach of ALMA surveys in (sub) millimeter bands.