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Quasars as tracers of cosmic flows

Published online by Cambridge University Press:  12 October 2016

J. Modzelewska
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland email: jmodzel@camk.edu.pl, bcz@camk.edu.pl
B. Czerny
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland email: jmodzel@camk.edu.pl, bcz@camk.edu.pl
M. Bilicki
Affiliation:
Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Rondebosch, South Africa
K. Hryniewicz
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland email: jmodzel@camk.edu.pl, bcz@camk.edu.pl ISDC Data Centre for Astrophysics, Observatoire de Geneve, Universite de Geneve, Chemin d'Ecogia 16, 1290 Versoix, Switzerland
M. Krupa
Affiliation:
Astronomical Observatory of the Jagiellonian University, Orla 171, 30-244 Cracow, Poland
F. Petrogalli
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland email: jmodzel@camk.edu.pl, bcz@camk.edu.pl
W. Pych
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland email: jmodzel@camk.edu.pl, bcz@camk.edu.pl
A. Kurcz
Affiliation:
Astronomical Observatory of the Jagiellonian University, Orla 171, 30-244 Cracow, Poland
A. Udalski
Affiliation:
Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland
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Abstract

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Quasars, as the most luminous persistent sources in the Universe, have broad applications for cosmological studies. In particular, they can be employed to directly measure the expansion history of the Universe, similarly to SNe Ia. The advantage of quasars is that they are numerous, cover a broad range of redshifts, up to z = 7, and do not show significant evolution of metallicity with redshift. The idea is based on the relation between the time delay of an emission line and the continuum, and the absolute monochromatic luminosity of a quasar. For intermediate redshift quasars, the suitable line is Mg II. Between December 2012 and March 2014, we performed five spectroscopic observations of the QSO CTS C30.10 (z = 0.900) using the South African Large Telesope (SALT), supplemented with photometric monitoring, with the aim of determining the variability of the line shape, changes in the total line intensity and in the continuum. We show that the method is very promising.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

References

Borodoi, R., Lilly, S. J., Kacprzak, G. G., & Churchill, C. W. 2014, ApJ, 784, 108 CrossRefGoogle Scholar
Bruhweiler, F. & Verner, E. 2008, ApJ, 675, 83 CrossRefGoogle Scholar
Czerny, B., & Hryniewicz, K. 2011,A&A, 525, L8 Google Scholar
Czerny, B., Hryniewicz, K., Maity, I., et al. 2013, A&A, 556, A97 Google Scholar
Kelly, B. C., Vestergaard, M., et al. 2010,ApJ, 719, 1315 CrossRefGoogle Scholar
Modzelewska, J., Czerny, B., Hryniewicz, K. et al. 2014,A&A, in press, (arXiv1408.1520)Google Scholar
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