Do all QSOs have the same black hole mass
Do all QSOs have the same black hole mass
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所有 QSO 的黑洞质量都相同吗
DOI：
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
U. Sawangwit
中科院分区：
文献类型：
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作者：
T. Shanks;S. Croom;S. Fine;N. Ross;U. Sawangwit
来自SDSS、2QZ和2SLAQ的准恒星天体(QSO)在固定红移下覆盖一个数量级的光度，表现出相似的聚集幅度，最亮的样本显示的聚集长度仅比最弱的样本高11±9%。此外，z>；0.5处的类星系团演化可以用一个假设主机晕质量固定的模型来很好地拟合。如果晕和黑洞(BH)质量是相关的，那么这可能意味着类星体出现在相对较窄的晕质量范围内，而BH质量范围也相对较窄。哈勃太空望远镜和双子座对覆盖大光度范围的类星体的高分辨率成像也显示出类星体宿主星系的光度范围相对较窄。我们认为，早期类型星系向z≈1-2的缓慢演化也可能进一步支持类星体宿主BH质量的缓慢演化。结果将意味着，如果高z类星体以爱丁顿速率辐射，那么低z类型1Seyfert星系的辐射速率一定比爱丁顿低100倍的≈。我们根据四个经验模型讨论了结果，其中(I)类星体以LEdd的固定比例辐射，(Ii)类星体光度随时间“闪烁”，(Iii)类星体具有单一的BH质量，以及(Iv)类星体是长寿命的，并通过纯粹的光度演化(PLE)演化。我们的结论是，LEdd模型需要将MBH和Mhalo解耦，以绕过聚类结果。虽然单一的BH质量和闪变模型符合z>；0.5的聚集结果，但它们似乎被从z≈0时的混响映射中发现的MBH-L关系所拒绝。我们发现，Z<；0.5类星团数据的加入改善了长寿命类星体模型的拟合度，并表明PLE模型对类星体黑洞质量的预测与紫外线碰撞和混响的估计是合理的。
Quasi-stellar objects (QSOs) from SDSS, 2QZ and 2SLAQ covering an order of magnitude in luminosity at fixed redshift exhibit similar amplitudes of clustering, with the brightest sample showing a clustering length only 11 ± 9 per cent higher than the faintest sample. In addition, QSO clustering evolution at z > 0.5 is well fitted by a model that assumes a fixed host halo mass. If halo and black hole (BH) masses are related, then this may imply that QSOs occur in a relatively narrow range of halo masses with a correspondingly narrow range of BH mass. Hubble Space Telescope and Gemini high-resolution imaging of QSOs covering a large range in luminosity also show a relatively narrow range in QSO host galaxy luminosity. We argue that the slow evolution of early-type galaxies out to z≈ 1–2 may also provide further support for a slow evolution of QSO host BH masses. The result would mean that if high-z QSOs radiate at Eddington rates then low-z type 1 Seyfert galaxy must radiate at ≈100 times less than Eddington. We discuss the consequences in terms of four empirical models where (i) QSOs radiate at a fixed fraction of LEdd, (ii) QSO luminosity ‘flickers’ over time, (iii) QSOs have a single BH mass and (iv) QSOs are long lived and evolve via pure luminosity evolution (PLE). We conclude that the LEdd model requires MBH and Mhalo to be decoupled to circumvent the clustering results. While the single BH mass and flickering models fit the z > 0.5 clustering results, they appear to be rejected by the MBH–L relation found from reverberation mapping at z≈ 0. We find that the inclusion of z < 0.5 QSO clustering data improves the fit of a long-lived QSO model and suggest that the predictions of the PLE model for QSO BH masses agree reasonably with ultraviolet bump and reverberation estimates.
影响因子：
64.8
作者：
J. Kormendy;Ralf Bender;M. Cornell
通讯作者：
J. Kormendy;Ralf Bender;M. Cornell
影响因子：
64.8
作者：
J. Kormendy;R. Bender
通讯作者：
J. Kormendy;R. Bender