Simulations of the OzDES AGN reverberation mapping project
Simulations of the OzDES AGN reverberation mapping project
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DOI：
10.1093/mnras/stv1718
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发表时间：
2015-04
影响因子：
4.8
通讯作者：
A. King;P. Martini;T. Davis;K. Denney;C. Kochanek;B. Peterson;A. Skielboe;M. Vestergaard;E. Huff
中科院分区：
文献类型：
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作者：
A. King;P. Martini;T. Davis;K. Denney;C. Kochanek;B. Peterson;A. Skielboe;M. Vestergaard;E. Huff
作为澳大利亚光谱暗能量巡天 (OzDES) 的一部分，我们正在五年内对暗能量巡天 (DES) 超新星场 30 deg(2) 区域的 500 个类星体进行大规模混响测绘研究。这些类星体的红移范围高达 4，表观 AB 星等在 16.8 星等 < r < 22.5 星等之间。该调查的目的是测量类星体连续体的波动和单个物体的广泛发射线通量之间的时间滞后，以便测量广泛的活动星系核（AGN）的黑洞质量并约束半径-光度（R-L）关系。在这里，我们研究了 OzDES 混响映射活动的预期效率及其可能的扩展。我们预计将恢复大约 35-45% 类星体的滞后。具有较短滞后和较大变异性的 AGN 更有可能产生滞后测量，并且滞后小于或类似于 6 个月或类似于 1 年的物体预计会得到最准确的恢复。预计基线 OzDES 混响映射活动将产生 H beta、MgII lambda 2798 和 C IV lambda 1549 的 R-L 关系参数的无偏差测量。通过增加光谱节奏、延长调查季节或提高发射线通量测量精度来扩展基线调查将显着改善所有广泛发射线的 R-L 参数约束。
As part of the Australian spectroscopic dark energy survey (OzDES) we are carrying out a large-scale reverberation mapping study of >= 500 quasars over five years in the 30 deg(2) area of the Dark Energy Survey (DES) supernova fields. These quasars have redshifts ranging up to 4 and have apparent AB magnitudes between 16.8 mag < r < 22.5 mag. The aim of the survey is to measure time lags between fluctuations in the quasar continuum and broad emission-line fluxes of individual objects in order to measure black hole masses for a broad range of active galactic nuclei (AGN) and constrain the radius-luminosity (R-L) relationship. Here we investigate the expected efficiency of the OzDES reverberation mapping campaign and its possible extensions. We expect to recover lags for similar to 35-45 per cent of the quasars. AGN with shorter lags and greater variability are more likely to yield a lag measurement, and objects with lags less than or similar to 6 months or similar to 1 yr are expected to be recovered the most accurately. The baseline OzDES reverberation mapping campaign is predicted to produce an unbiased measurement of the R-L relationship parameters for H beta, MgII lambda 2798, and C IV lambda 1549. Extending the baseline survey by either increasing the spectroscopic cadence, extending the survey season, or improving the emission-line flux measurement accuracy will significantly improve the R-L parameter constraints for all broad emission lines.