Probing the source structure in lensed AGNs
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2022-04
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Universidad de Valparaíso
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Instituto de Fisica y Astronomia
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Resumen
Accurate determination of supermassive black hole masses are crucial to correctly understand the connection between supermassive black holes and their host galaxies, specially with the correlation that exists between the supermassive black hole mass and some physical parameters of the host galaxy. This connection is relatively well determined in the local universe over 4 orders of magnitude. However, at high redshifts (z > 1), due to flux limitation it is challenging to determine the physical parameters of the faintest systems. Fortunately, gravitational lensed quasars are highly magnified, and thus offers the opportunity to study a fainter population that otherwise is not accessible.
In this work, I study the inner region of the lensed quasars. The mass of the black hole is determined using the single-epoch method for 15 lens systems using the Balmer lines (Hα and Hβ). In addition, I present supermassive black hole mass for MgII and CIV, and compare them with the previous masses and also with the literature. For the first time the black hole mass was obtained for WGD2038-4008 (Melo et al. 2021) and QJ0158-4325 (Melo et al. in prep I). The luminosity range obtained for all the sample was 44.1 ≤ log10(Lbol /Lsun) ≤ 47.6, which is in agreement with the correlation of Lbol vs MBH of lensed and non-lensed AGNs.
In addition, chromatic microlensing was detected in three systems, which offered an alterna- tive technique to measure the accretion disk size. Our estimations does not agree with the one obtained using the single epoch method.
Finally, I conclude that the new black hole masses reach a fainter and low-luminosity region in the black hole mass - luminosity plane.
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NUCLEOS GALACTICOS ACTIVOS, ANALISIS ESPECTRAL, HOYOS NEGROS (ASTRONOMIA)