Context. We present the results of the reverberation monitoring of the MgII broad line and FeII pseudocontinuum for the luminous quasar CTS C30.10 (z = 0.90052) with the Southern African Large Telescope in 2012-2021. Aims. We aimed at disentangling the MgII and UV FeII variability and the first measurement of UV FeII time delay for a distant quasar. Methods. We used several methods for the time-delay measurements and determined the FeII and MgII time delays. We also performed a wavelength-resolved time delay study for a combination of MgII and FeII in the 2700 - 2900 Å rest-frame wavelength range. Results. We obtain a time delay for MgII of 275 . 5 + 12 . 4 − 19 . 5 days in the rest frame, and we have two possible solutions of 270 . 0 + 13 . 8 − 25 . 3 days and 180 . 3 + 26 . 6 − 30 . 0 in the rest frame for FeII. Combining this result with the old measurement of FeII UV time delay for NGC 5548, we discuss for first time the radius-luminosity relation for UV FeII with the slope consistent with 0 . 5 within the uncertainties. Conclusions. Because the FeII time delay has a shorter time-delay component but the lines are narrower than MgII, we propose that the line-delay measurement is biased toward the part of the broad line region (BLR) facing the observer. The bulk of the Fe II emission may arise from the more distant BLR region, however, the region that is shielded from the observer. disks – quasars: emission lines – quasars: individual: CTS C30.10 – Techniques: spectroscopic, photometric

https://www.aanda.org/articles/aa/pdf/forth/aa43194-22.pdf

Wavelength-resolved reverberation mapping of quasar CTS C30.10: Dissecting MgII and FeII emission regions

We present a study of the [O iii] λ5007 line profile in a subsample of eight active galactic nuclei (AGNs) and six non-AGNs in the optically selected green valley at z < 0.5 using long-slit spectroscopic observations obtained with the 11 m Southern African Large Telescope. Gaussian decomposition of the line profile was performed to study its different components. We observe that the AGN profiles are more complex than the non-AGN ones. In particular, in most AGNs (5/8) we detect a blue wing of the line. We derive the FWHM velocities of the wing and systemic component, and find that the AGNs show higher FWHM velocities than the non-AGNs in their core component. We also find that the AGNs show blue wings with a median velocity width of approximately 600 km s−1, and a velocity offset from the core component in the range −90 to −350 km s−1, in contrast to the non-AGN galaxies, where we do not detect blue wings in any of their [O iii] λ5007 line profiles. Using the spatial information in our spectra, we show that at least three of the outflow candidate galaxies have centrally driven gas outflows extending across the whole galaxy. Moreover, these are also the galaxies which are located on the main sequence of star formation, raising the possibility that the AGNs in our sample are influencing the star formation of their host galaxies (such as positive feedback). This is in agreement with our previous work where we studied the star formation, morphology, and stellar population properties of a sample of green valley AGNs and non-AGN galaxies.

The [O iii] Profiles of Far-infrared Active and Inactive Optically Selected Green Valley Galaxies

Context. HE 0435 − 5304 from Hamburg European Southern Observatory survey is a quasar that appears in the literature with two conﬂicting redshift values: ∼ 1 . 2 and ∼ 0 . 4. It was used in the studies of the intergalactic medium through ﬁtting of the narrow absorption lines in its ultraviolet (UV) spectrum. This source is also known historically as a luminous infrared galaxy. Aims. We present optical spectra of HE 0435 − 5304, aiming to precisely measure its redshift and to study its physical properties. In particular, properties of its active nucleus, which is studied in the context of the source being identiﬁed here as an ultra-luminous infrared galaxy (ULIRG), allow us to place this quasar in the context of the general population. Methods. We analyzed optical spectra of the quasar HE 0435 − 5304. Fitting the spectra, we focused on modeling H β and [O III] lines. Based on these, we derived the virial black hole mass, bolometric luminosity, and Eddington ratio of the active galactic nucleus (AGN). Additionally, we performed broad band photometry ﬁtting which allows us to quantify host galaxy parameters. Based on available mixed IR / optical / UV data spanning over a decade, we discuss the possible evolution of physical properties of the source and the inﬂuence of the observing conditions on our results. Results. The improved redshift value of HE 0435 − 5304 is estimated to 0 . 42788 ± 0 . 00027 based on the [O II] line – the narrowest line in the spectra – which is mostly consistent with the narrowest components of the other emission lines. The source was found to be a relatively massive and luminous AGN whose host galaxy is actively forming stars. Although its stellar population seems to be heavily obscured, we did not ﬁnd evidence for signiﬁcant obscuration of the nucleus. We conclude that the AGN HE 0435 − 5304 is a rather prominent iron emitter from the extreme type-A population very close to the narrow-line Seyfert 1 group. The fact that the width of the H β line appears to be systematically growing in its broadest component with time may suggest that this AGN is changing its broad line region. However, because of the inﬂuence of atmospheric e ﬀ ects contaminating spectral proﬁles, this ﬁnding is uncertain.

K. Małek

Papers

AGN in the ULIRG HE 0435-5304