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  LLAMA: The MBH–σ relation of the most luminous local AGNs

Caglar, T., Burtscher, L., Brandl, B., Brinchmann, J., Davies, R. I., Hicks, E. K. S., et al. (2020). LLAMA: The MBH–σ relation of the most luminous local AGNs. Astronomy and Astrophysics, 634: A114. doi:10.1051/0004-6361/201936321.

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LLAMA The MBH–σ⋆ relation of the most luminous local AGNs.pdf (beliebiger Volltext), 23MB
 
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Caglar, Turgay, Autor
Burtscher, Leonard, Autor
Brandl, Bernhard, Autor
Brinchmann, Jarle, Autor
Davies, Richard I.1, Autor           
Hicks, Erin K. S., Autor
Koss, Michael, Autor
Lin, Ming-Yi, Autor
Maciejewski, Witold, Autor
Müller-Sánchez, Francisco, Autor
el Rogemar, A. Ri, Autor
el Rogério, Ri, Autor
Rosario, David J., Autor
Schartmann, Marc2, Autor           
Schnorr-Müller, Allan, Autor
Shimizu, T. Taro1, Autor           
Storchi-Bergmann, Thaisa, Autor
Veilleux, Sylvain, Autor
de Xivry, Gilles Orban, Autor
Bennert, Vardha N., Autor
Affiliations:
1Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159889              
2Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              

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 Zusammenfassung: Context. The MBH–σ relation is considered a result of coevolution between the host galaxies and their supermassive black holes. For elliptical bulge hosting inactive galaxies, this relation is well established, but there is still discussion concerning whether active galaxies follow the same relation.
Aims. In this paper, we estimate black hole masses for a sample of 19 local luminous active galactic nuclei (AGNs; LLAMA) to test their location on the MBH–σ relation. In addition, we test how robustly we can determine the stellar velocity dispersion in the presence of an AGN continuum and AGN emission lines, and as a function of signal-to-noise ratio.
Methods. Supermassive black hole masses (MBH) were derived from the broad-line-based relations for Hα, Hβ, and Paβ emission line profiles for Type 1 AGNs. We compared the bulge stellar velocity dispersion (σ) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We applied an extinction correction to the observed broad-line fluxes and we corrected the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps.
Results. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34 ≤ log MBH ≤ 7.75 M and the σ⋆CaT estimates range between 73 ≤ σ⋆CaT ≤ 227 km s−1. From the so-constructed MBH − σ relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample.
Conclusions. We find that our sample of local luminous AGNs is consistent with the MBH–σ relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion.

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 Datum: 2020-02-19
 Publikationsstatus: Online veröffentlicht
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 Identifikatoren: DOI: 10.1051/0004-6361/201936321
Anderer: LOCALID: 3222857
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Titel: Astronomy and Astrophysics
  Andere : Astron. Astrophys.
Genre der Quelle: Zeitschrift
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Ort, Verlag, Ausgabe: France : EDP Sciences S A
Seiten: - Band / Heft: 634 Artikelnummer: A114 Start- / Endseite: - Identifikator: ISSN: 1432-0746
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1