AI 中文总结
研究202个红移在\(0.02<z\lesssim0.8\)的类星体，利用多波段光谱能量分布分解，通过CIGALE和AGNfitter建模及多冷尘埃模板量化不确定性，得出类星体宿主星系远红外恒星形成率相关结论及指标关系。
AI 中文摘要
可靠的恒星形成率对于研究黑洞增长与类星体宿主星系之间的联系至关重要。我们利用多波段光谱能量分布分解研究了202个红移在\(0.02<z\lesssim0.8\)的SDSS和PG类星体的远红外恒星形成率及宿主星系属性。测光涵盖从光学到远红外波段，并补充了JCMT/SCUBA - 2在450和850微米的观测。用CIGALE和AGNfitter对光谱能量分布建模，采用多个冷尘埃模板量化系统不确定性。五个远红外恒星形成率估计值之间模型依赖的中值散射为\(0.14\) dex，AGNfitter给出的远红外恒星形成率比CIGALE平均估计值低\(0.09\) dex。对于有SCUBA - 2覆盖的58个类星体，包含SCUBA - 2数据平均仅使采用的远红外恒星形成率改变约\(0.01\) dex，但会影响个别源。在远红外受限样本中，许多类星体宿主位于恒星形成主序列之上或之上，但SDSS子样本的红移依赖远红外选择限制了对整个类星体宿主群体的结论。主序列偏移与直接爱丁顿比无明显相关性，而与基于红外的\(L_{\rm tor}/L_{\rm Edd}\)代理正相关。尘埃模型中的最小辐射场强度\(U_{\rm min}\)随热光度和尘埃温度增加。WISE W2（4.6微米）和W3（12微米）与赫歇尔波段结合也可为\(f_{\rm AGN}\)提供有用经验指标。
英文摘要
Reliable star formation rates (SFRs) are essential for studying the connection between black hole growth and quasar host galaxies. We study the far-infrared (FIR) SFRs and the host galaxy properties of 202 SDSS and PG quasars at $0.02<z\lesssim0.8$, spanning $\log({\rm SFR}_{\rm FIR}/M_\odot\,{\rm yr}^{-1})\simeq-0.45$--$2.76$, using multiwavelength spectral energy distribution (SED) decomposition. The photometry covers wavelengths from the optical to the FIR and is supplemented by JCMT/SCUBA-2 observations at 450 and 850 $μ$m. We model the SEDs with CIGALE and AGNfitter and adopt multiple cold dust templates to quantify systematic uncertainties. The median model-dependent scatter among the five FIR SFR estimates is $0.14$ dex, and AGNfitter gives FIR SFRs lower than the mean CIGALE estimate by a median of $0.09$ dex. For the 58 quasars with SCUBA-2 coverage, including SCUBA-2 data changes the adopted FIR SFR by only $\sim$0.01 dex on average but can affect individual sources with limited Herschel coverage or radio-loud emission. Within our FIR-constrained sample, many quasar hosts lie on or above the star-forming main sequence, but the redshift-dependent FIR selection of the SDSS subsample limits conclusions about the full quasar-host population. We find no clear correlation between the main-sequence (MS) offset and the direct Eddington ratio, while the offset is positively related to the infrared-based $L_{\rm tor}/L_{\rm Edd}$ proxy. The minimum radiation field intensity in the dust model, $U_{\rm min}$, increases with bolometric luminosity and dust temperature. WISE W2 (4.6 $μ$m) and W3 (12 $μ$m) combined with Herschel bands can also provide useful empirical indicators of $f_{\rm AGN}$.
Comments42 pages, 24 figures
Journal refUniverse 12 (7), 213 (2026)
