AI 中文总结
该研究针对单历元黑洞质量估计器的局限，利用27个SDSS-RM类星体的近红外光谱，校准了基于宽帕邢线Pα和Pβ的黑洞质量估计关系，可作为紫外或光学宽线受限时的互补工具。
AI 中文摘要
基于静止帧紫外或光学宽发射线的单历元（SE）黑洞质量估计器可能受尘埃消光或波长覆盖范围的限制。我们直接利用反响映射（RM）质量校准基于宽帕邢线Pα和Pβ的估计器。我们获取了27个SDSS-RM类星体的LBT/LUCI近红外光谱，并将其与具有RM质量的活动星系核（AGN）的存档帕邢线测量结果结合。经过连续谱扣除后，我们使用多分量和单高斯轮廓模型测量了线光度和半高全宽（FWHM）。我们拟合了公式log(M_BH/M_⊙)=a+b log(L/10^41 erg s^-1)+c log(FWHM/10^3 km s^-1)，包含本征弥散。基准关系使用经测光校正的线光度和组合宽轮廓的FWHM。对于Pα，我们得到(a,b,c)=(6.86^(+0.24)_(-0.25),0.47^(+0.11)_(-0.10),1.24^(+0.49)_(-0.48))，本征弥散为0.28^(+0.08)_(-0.06) dex；对于Pβ，得到(7.00±0.24,0.48^(+0.10)_(-0.09),0.91^(+0.46)_(-0.47))，弥散为0.32^(+0.08)_(-0.06) dex。使用单高斯宽度、5100埃连续谱光度或固定维里斜率的关系，其弥散在不确定度范围内一致。当紫外或光学宽发射线被消光或不可用时，这些关系提供互补的质量估计器，应在校准样本的参数范围内应用，且仍受与RM维里因子相关的系统不确定度影响。
英文摘要
Single-epoch (SE) black hole mass estimators based on rest-frame ultraviolet or optical broad lines can be limited by dust attenuation or wavelength coverage. We calibrate estimators based on broad Paschen P$α$ and P$β$ directly against reverberation mapping (RM) masses. We obtained LBT/LUCI near-infrared spectra of 27 SDSS-RM quasars and combined them with archival Paschen measurements for AGNs with RM masses. After continuum subtraction, we measured line luminosities and full widths at half maximum (FWHMs) using multi-component and single-Gaussian profile models. We fitted $\log(M_{\rm BH}/M_\odot)=a+b\log(L/10^{41}\,{\rm erg\,s^{-1}})+c\log({\rm FWHM}/10^3\,{\rm km\,s^{-1}})$, including intrinsic scatter. The fiducial relations use photometrically corrected line luminosities and FWHMs of the combined broad profiles. For P$α$, we obtain $(a,b,c)=(6.86^{+0.24}_{-0.25},0.47^{+0.11}_{-0.10},1.24^{+0.49}_{-0.48})$ with an intrinsic scatter of $0.28^{+0.08}_{-0.06}$ dex. For P$β$, we obtain $(7.00\pm0.24,0.48^{+0.10}_{-0.09},0.91^{+0.46}_{-0.47})$ with a scatter of $0.32^{+0.08}_{-0.06}$ dex. Relations using single-Gaussian widths, 5100 Å continuum luminosities, or fixed virial slopes have scatters consistent within the uncertainties. These relations provide complementary mass estimators when ultraviolet or optical broad lines are attenuated or unavailable. They should be applied within the parameter ranges of the calibration sample and remain subject to the systematic uncertainty associated with the RM virial factor.
CommentsSubmitted to Astronomy & Astrophysics (A&A); 12 pages, 9 figures
