On the need of an ultramassive black hole in OJ 287

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00575401" target="_blank" >RIV/67985815:_____/23:00575401 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68407700:21230/23:00368114

Výsledek na webu

<a href="https://hdl.handle.net/11104/0345903" target="_blank" >https://hdl.handle.net/11104/0345903</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stad2249" target="_blank" >10.1093/mnras/stad2249</a>

Jazyk výsledku

angličtina

Název v původním jazyce

On the need of an ultramassive black hole in OJ 287

Popis výsledku v původním jazyce

The highly variable blazar OJ 287 is commonly discussed as an example of a binary black hole system. The 130 yr long optical light curve is well explained by a model where the central body is a massive black hole of 18.35 $times$ 10(9) solar mass that supports a thin accretion disc. The secondary black hole of 0.15 x 10(9) solar mass impacts the disc twice during its 12 yr orbit, and causes observable flares. Recently, it has been argued that an accretion disc with a typical Active Galactic Nuclei (AGN) accretion rate and above mentioned central body mass should be at least six magnitudes brighter than OJ 287's host galaxy and would therefore be observationally excluded. Based on the observations of OJ 287's radio jet, detailed in Marscher and Jorstad (2011), and up-to-date accretion disc models of Azadi et al. (2022), we show that the V-band magnitude of the accretion disc is unlikely to exceed the host galaxy brightness by more than one magnitude, and could well be fainter than the host. This is because accretion power is necessary to launch the jet as well as to create electromagnetic radiation, distributed across many wavelengths, and not concentrated especially on the optical V-band. Further, we note that the claimed V-band concentration of accretion power leads to serious problems while interpreting observations of other AGN. Therefore, we infer that the mass of the primary black hole and its accretion rate do not need to be smaller than what is determined in the standard model for OJ 287.

Název v anglickém jazyce

On the need of an ultramassive black hole in OJ 287

Popis výsledku anglicky

The highly variable blazar OJ 287 is commonly discussed as an example of a binary black hole system. The 130 yr long optical light curve is well explained by a model where the central body is a massive black hole of 18.35 $times$ 10(9) solar mass that supports a thin accretion disc. The secondary black hole of 0.15 x 10(9) solar mass impacts the disc twice during its 12 yr orbit, and causes observable flares. Recently, it has been argued that an accretion disc with a typical Active Galactic Nuclei (AGN) accretion rate and above mentioned central body mass should be at least six magnitudes brighter than OJ 287's host galaxy and would therefore be observationally excluded. Based on the observations of OJ 287's radio jet, detailed in Marscher and Jorstad (2011), and up-to-date accretion disc models of Azadi et al. (2022), we show that the V-band magnitude of the accretion disc is unlikely to exceed the host galaxy brightness by more than one magnitude, and could well be fainter than the host. This is because accretion power is necessary to launch the jet as well as to create electromagnetic radiation, distributed across many wavelengths, and not concentrated especially on the optical V-band. Further, we note that the claimed V-band concentration of accretion power leads to serious problems while interpreting observations of other AGN. Therefore, we infer that the mass of the primary black hole and its accretion rate do not need to be smaller than what is determined in the standard model for OJ 287.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2023

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

525

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

5

Strana od-do

1153-1157

Kód UT WoS článku

001051114800030

EID výsledku v databázi Scopus

2-s2.0-85168816317