SALT long-slit spectroscopy of quasar HE 0435-4312: fast displacement of the Mg II emission line

Šredzińska, Justyna; Hryniewicz, Krzysztof; Krupa, Magdalena; Kurcz, Agnieszka; Marziani, Paola; Adhikari, T. P.; Basak, Rupal; You, Bei; Wang, Jian-Min; Hu, Chen; Pych, W.; Bilicki, Maciej

doi:10.1051/0004-6361/201628257

Cited by 9 publications

(3 citation statements)

References 135 publications

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“…Thus the turbulence in the range 10-20 km s −1 is generally favored for more efficient Fe II production, at such values are actually favored in detailed fitting of specific objects (e.g. Bruhweiler & Verner 2008;Hryniewicz et al 2014;Marziani et al 2013;Średzińska et al 2017).…”

Section: Turbulencementioning

confidence: 99%

Modeling of the Quasar Main Sequence in the Optical Plane

Panda

Czerny

Adhikari

et al. 2018

ApJ

114

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The concept of the quasar main sequence is very attractive since it stresses correlations between various parameters and implies the underlying simplicity. In the optical plane defined by the width of the Hβ line and the ratio of the equivalent width of the Fe II to Hβ observed objects form a characteristic pattern. In this paper, we use a physically motivated model to explain the distribution of quasars in the optical plane. Continuum is modelled as an accretion disk with a hard X-ray power law uniquely tight to the disk at the basis of observational scaling, and the Broad Line Region distance is determined also from observational scaling. We perform the computations of the FeII and Hβ line production with the code CLOUDY. We have only six free parameters for an individual source: maximum temperature of the accretion disk, Eddington ratio, cloud density, cloud column density, microturbulence, and iron abundance, and only the last four remain as global parameters in our modelling of the whole sequence. Our theoretically computed points cover well the optical plane part populated with the observed quasars, particularly if we allow for super-Solar abundance of heavy elements. Explanation of the exceptionally strong Fe II emitter requires a stronger contribution from the dark sides of the clouds. Analyzing the way how our model covers the optical plane we conclude that there is no single simple driver behind the sequence, as neither the Eddington ratio nor broad band spectrum shape plays the dominant role. Also, the role of the viewing angle in providing the dispersion of the quasar main sequence is apparently not as strong as expected.

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Section: Turbulencementioning

confidence: 99%

Modeling of the Quasar Main Sequence in the Optical Plane

Panda

Czerny

Adhikari

et al. 2018

ApJ

114

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“…This project requires using the MgII line, and our studies are pioneer in this respect, as such monitoring has never been done before. Data obtained so far with the South African Large Telescope (SALT) show that we achieve the required accuracy (below 2%) of the MgII measurement to determine its variability (Modzelewska et al, 2014;Sredzinska et al, 2016), and simulations indicate that the program can give the accuracy of 0.06-0.32 mag in the distance modulus for each of the concerned quasars (Czerny et al, 2013).…”

Section: Methodsmentioning

confidence: 84%

Tracing dark energy with quasars

Šredzińska¹,

Czerny²,

Bilicki³

et al. 2016

Preprint

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The file ptapap.cls is 1289 days old. Get a new one: http://users.camk.edu.pl/chris/pta/ptapap.tar.gzThe nature of dark energy, driving the accelerated expansion of the Universe, is one of the most important issues in modern astrophysics. In order to understand this phenomenon, we need precise astrophysical probes of the universal expansion spanning wide redshift ranges. Quasars have recently emerged as such a probe, thanks to their high intrinsic luminosities and, most importantly, our ability to measure their luminosity distances independently of redshifts. Here we report our ongoing work on observational reverberation mapping using the time delay of the Mg II line, performed with the South African Large Telescope (SALT).

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“…Peterson et al 2004) the continuum is measured at 5100 Å, in the case of MgII monitoring (e.g. Zhu et al 2017;Średzińska et al 2017, see also Koz lowski 2015) the continuum is measured at 3000 Å, which affects only the proportionally coefficient, but not the slope.…”

Section: Comparison Of the Fwhm And Ew Line Trends With The Blr Modelmentioning

confidence: 99%

Quasar main sequence in the UV plane

Śniegowska,

Kozłowski,

Czerny

et al. 2018

Preprint

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Active galaxies form a clear pattern in the optical plane showing the correlation between the Full Width Half Maximum (FWHM) of the Hβ line and the ratio of the Equivalent Width (EW) of the optical FeII emission and the EW(Hβ). This pattern is frequently refereed to as the quasar main sequence. In this paper we study the UV plane showing FWHM of the MgII line against the ratio of EW of UV FeII emission to EW(MgII). We show that the UV plane trends are different, with the underlying strong correlation between FWHM(MgII) and EW(MgII). This correlation is entirely driven by the choice of the continuum used to measure EW(MgII). If we correct for the strong curvature in the UV continuum related to the character of emission expected from accretion disk, the behavior of the FWHM vs. EW for MgII becomes similar to the behaviour of Hβ. Such a similarity is expected since both lines belong to the Low Ionization group of emission lines and come from a similar region. Such a similarity and weak coupling between FWHM and EW of the corresponding line is then also consistent with the Broad Line Region model based on the presence of dust in the accretion disk atmosphere.

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SALT long-slit spectroscopy of quasar HE 0435-4312: fast displacement of the Mg II emission line

Cited by 9 publications

References 135 publications

Modeling of the Quasar Main Sequence in the Optical Plane

Modeling of the Quasar Main Sequence in the Optical Plane

Tracing dark energy with quasars

Quasar main sequence in the UV plane

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