Do reverberation mapping analyses provide an accurate picture of the broad-line region?. Issue 2 (21st June 2019)

• Record Type: Journal Article
• Authors: Mangham, S W; Knigge, C; Williams, P; Horne, Keith; Pancoast, A; Matthews, J H; Long, K S; Sim, S A; Higginbottom, N
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 488:Issue 2(2019)
• Page Start: 2780
• Page End: 2799
• Publication Date: 2019-06-21
• Subjects: radiative transfer -- quasars: general -- accretion discs; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz1713
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: Reverberation mapping (RM) is a powerful approach for determining the nature of the broad-line region (BLR) in active galactic nuclei. However, inferring physical BLR properties from an observed spectroscopic time series is a difficult inverse problem. Here, we present a blind test of two widely used RM methods: MEMEcho (developed by Horne) and CARAMEL (developed by Pancoast and collaborators). The test data are simulated spectroscopic time series that track the Hα emission line response to an empirical continuum light curve. The underlying BLR model is a rotating, biconical accretion disc wind, and the synthetic spectra are generated via self-consistent ionization and radiative transfer simulations. We generate two mock data sets, representing Seyfert galaxies and QSOs. The Seyfert model produces a largely negative response, which neither method can recover. However, both fail 'gracefully', neither generating spurious results. For the QSO model both CARAMEL and expert interpretation of MEMEcho ś output both capture the broadly annular, rotation-dominated nature of the line-forming region, though MEMEcho analysis overestimates its size by 50 per cent, but CARAMEL is unable to distinguish between additional inflow and outflow components. Despite fitting individual spectra well, the CARAMEL velocity-delay maps and RMS line profiles are strongly inconsistent with the input data. Finally, since the Hα line-forming region is rotation dominated, neither method recovers the disc wind nature of the underlying BLR model. Thus considerable care is required when interpreting the results of RM analyses in terms of physical models.