The remarkable X-ray variability of IRAS 13224-3809 - I. The variability process

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F19%3A00517309" target="_blank" >RIV/67985815:_____/19:00517309 - isvavai.cz</a>

Výsledek na webu

<a href="http://hdl.handle.net/11104/0302633" target="_blank" >http://hdl.handle.net/11104/0302633</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/sty2527" target="_blank" >10.1093/mnras/sty2527</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The remarkable X-ray variability of IRAS 13224-3809 - I. The variability process

Popis výsledku v původním jazyce

We present a detailed X-ray timing analysis of the highly variable narrow-line Seyfert 1 ( NLS1) galaxy IRAS 13224-3809. The source was recently monitored for 1.5Ms with XMM-Newton, which, combined with 500 ks archival data, makes this the best-studied NLS1 galaxy in X-rays to date. We apply standard time- and Fourier-domain techniques in order to understand the underlying variability process. The source flux is not distributed lognormally, as expected for all types of accreting sources. The first non-linear rms-flux relation for any accreting source in any waveband is found, with rms. flux2/3. The light curves exhibit significant strong non-stationarity, in addition to that caused by the rms-flux relation, and are fractionally more variable at lower source flux. The power spectrum is estimated down to similar to 10(-7) Hz and consists of multiple peaked components: a low-frequency break at similar to 10(-5) Hz, with slope alpha < 1 down to low frequencies, and an additional component breaking at similar to 10(-3) Hz. Using the high-frequency break, we estimate the black hole mass MBH = [0.5-2] x 10(6)M(circle dot) and mass accretion rate in Eddington units,. m Edd greater than or similar to 1. The broad-band power spectral density (PSD) and accretion rate make IRAS 13224-3809 a likely analogue of very high/intermediate-state black hole X-ray binaries. The non-stationarity is manifest in the PSD with the normalization of the peaked components increasing with decreasing source flux, as well as the low-frequency peak moving to higher frequencies. We also detect a narrow coherent feature in the soft-band PSD at 7 x 10(-4) Hz, modelled with a Lorentzian the feature has Q similar to 8 and an rms similar to 3 per cent. We discuss the implication of these results for accretion of matter on to black holes.

Název v anglickém jazyce

The remarkable X-ray variability of IRAS 13224-3809 - I. The variability process

Popis výsledku anglicky

We present a detailed X-ray timing analysis of the highly variable narrow-line Seyfert 1 ( NLS1) galaxy IRAS 13224-3809. The source was recently monitored for 1.5Ms with XMM-Newton, which, combined with 500 ks archival data, makes this the best-studied NLS1 galaxy in X-rays to date. We apply standard time- and Fourier-domain techniques in order to understand the underlying variability process. The source flux is not distributed lognormally, as expected for all types of accreting sources. The first non-linear rms-flux relation for any accreting source in any waveband is found, with rms. flux2/3. The light curves exhibit significant strong non-stationarity, in addition to that caused by the rms-flux relation, and are fractionally more variable at lower source flux. The power spectrum is estimated down to similar to 10(-7) Hz and consists of multiple peaked components: a low-frequency break at similar to 10(-5) Hz, with slope alpha < 1 down to low frequencies, and an additional component breaking at similar to 10(-3) Hz. Using the high-frequency break, we estimate the black hole mass MBH = [0.5-2] x 10(6)M(circle dot) and mass accretion rate in Eddington units,. m Edd greater than or similar to 1. The broad-band power spectral density (PSD) and accretion rate make IRAS 13224-3809 a likely analogue of very high/intermediate-state black hole X-ray binaries. The non-stationarity is manifest in the PSD with the normalization of the peaked components increasing with decreasing source flux, as well as the low-frequency peak moving to higher frequencies. We also detect a narrow coherent feature in the soft-band PSD at 7 x 10(-4) Hz, modelled with a Lorentzian the feature has Q similar to 8 and an rms similar to 3 per cent. We discuss the implication of these results for accretion of matter on to black holes.

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

2019

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

1365-2966

e-ISSN

—

Svazek periodika

482

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

19

Strana od-do

2088-2106

Kód UT WoS článku

000454578700048

EID výsledku v databázi Scopus

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