J 2023

Broad-line region in active galactic nuclei: Dusty or dustless?

PANDEY, Ashwani, Bozena CZERNY, Swayamtrupta PANDA, Raj PRINCE, Vikram Kumar JAISWAL et. al.

Základní údaje

Originální název

Broad-line region in active galactic nuclei: Dusty or dustless?

Autoři

PANDEY, Ashwani, Bozena CZERNY, Swayamtrupta PANDA, Raj PRINCE, Vikram Kumar JAISWAL, Mary Loli MARTINEZ-ALDAMA, Michal ZAJAČEK (703 Slovensko, domácí) a Marzena SNIEGOWSKA

Vydání

Astronomy and Astrophysics, EDP Sciences, 2023, 0004-6361

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Odkazy

Impakt faktor

Impact factor: 6.500 v roce 2022

Kód RIV

RIV/00216224:14310/23:00134415

Organizační jednotka

Přírodovědecká fakulta

UT WoS

001125494400022

Klíčová slova anglicky

galaxies: active; galaxies: Seyfert; methods: numerical

Štítky

Příznaky

Mezinárodní význam, Recenzováno
Změněno: 21. 3. 2024 10:47, Mgr. Marie Novosadová Šípková, DiS.

Anotace

V originále

Context. Dust in active galactic nuclei is clearly present right outside the broad-line region (BLR) in the form of a dusty molecular torus. However, some models of the BLR predict that dust may also exist within the BLR. Aims. We study the reprocessing of radiation by the BLR with the aim of observing how the presence of dust affects the reprocessed continuum and the line properties. Methods.We calculated a range of models using the CLOUDY photoionisation code for dusty and dustless plasma. We paid particular attention to the well-studied object NGC 5548, and we compared the line equivalent width predictions with the data from observations for this object. Results. We obtained a rough agreement between the expected equivalent widths of the Hβ and Mg II lines and the observed values for NGC 5548 for the line distances implied by the time-delay measurement (for Hβ) and the radius-luminosity relation (for Mg II) when the medium is dusty. We found the incident radiation to be consistent with the radiation seen by the observer, so no shielding between the inner disc and the BLR is required. High ionisation lines such as He II, however, clearly form in the inner dustless region. When the additional absorber is present, the Hβ emitting region moves closer to the dustless part of the accretion disc surface.

Návaznosti

GX21-13491X, projekt VaV
Název: Zkoumání žhavého vesmíru a porozumění kosmické zpětné vazbě (Akronym: EHU)
Investor: Grantová agentura ČR, Exploring the Hot Universe and Understanding Comic Feedback