Supermassive black holes are growing slowly by z∼5

被引:3
|
作者
Lai, Samuel [1 ,2 ]
Onken, Christopher A. [1 ,3 ,4 ]
Wolf, Christian [1 ,3 ,4 ]
Bian, Fuyan [5 ]
Fan, Xiaohui [6 ]
机构
[1] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia
[2] CSIRO, Space & Astron, POB 1130, Bentley, WA 6102, Australia
[3] Australian Natl Univ, Ctr Gravitat Astrophys, Res Sch Phys, Canberra, ACT 2611, Australia
[4] Australian Natl Univ, Ctr Gravitat Astrophys, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia
[5] European Southern Observ, Alonso Cordova 3107,Casilla 19001, Vitacura 19, Santiago, Chile
[6] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA
基金
澳大利亚研究理事会; 美国国家航空航天局; 美国国家科学基金会;
关键词
galaxies: active; galaxies: high-redshift; quasars: emission lines; quasars: supermassive black holes; ACTIVE GALACTIC NUCLEI; QUASAR LUMINOSITY FUNCTION; HIGH-REDSHIFT QUASARS; GALAXY STELLAR MASS; SIMILAR-TO; EDDINGTON-RATIO DISTRIBUTIONS; BROAD-LINE QUASARS; HIGH-Z EXPLORATION; LESS-THAN; DUTY CYCLES;
D O I
10.1093/mnras/stae1301
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We investigate the black hole mass function at z similar to 5 using XQz5, our recent sample of the most luminous quasars between the redshifts 4.5 < z < 5.3. We include 72 quasars with black hole masses estimated from velocity-broadened emission-line measurements and single-epoch virial prescriptions in the footprint of a highly complete parent survey. The sample mean Eddington ratio and standard deviation is log lambda approximate to -0.20 +/- 0.24. The completeness-corrected mass function is modelled as a double power law, and we constrain its evolution across redshift assuming accretion-dominated mass growth. We estimate the evolution of the mass function from z = 5-4, presenting joint constraints on accretion properties through a measured dimensionless e-folding parameter, k(ef) equivalent to <lambda > U(1 - & varepsilon;)/& varepsilon; = 1.79 +/- 0.06, where <lambda > is the mean Eddington ratio, U is the duty cycle, and & varepsilon; is the radiative efficiency. If these supermassive black holes were to form from seeds smaller than 10(8)M(circle dot), the growth rate must have been considerably faster at z >> 5 than observed from z = 5-4. A growth rate exceeding 3 x the observed rate would reduce the initial heavy seed mass to 10(5-6)M(circle dot), aligning with supermassive star and/or direct collapse seed masses. Stellar mass (10(2)M(circle dot)) black hole seeds would require greater than or similar to 4.5 x the observed growth rate at z >> 5 to reproduce the measured active black hole mass function. A possible pathway to produce the most extreme quasars is radiatively inefficient accretion flow, suggesting black holes with low angular momentum or photon trapping in supercritically accreting thick discs.
引用
收藏
页码:2245 / 2261
页数:17
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