Coronal Proerties of the Seyfert 1 Galaxy 3C 120 with NuSTAR

Rani, Priyanka; Stalin, C. S.

doi:10.3847/1538-4357/aab356

Cited by 18 publications

(14 citation statements)

References 76 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Ronchini et al 2019), 3C 120 (e.g. Rani &Stalin 2018), and3C 390.3 (e.g. Sambruna et al 2009;Lohfink et al 2015) are consistent with being disk/corona-related.…”

Section: X-ray Spectral Propertiesmentioning

confidence: 56%

“…Also, importantly, those studies utilizing NuS-TAR data in the hard X-rays generally find a high-energy cutoff at ∼ 100 keV (e.g. Ballantyne et al 2014;Lohfink et al 2015;Rani & Stalin 2018), signifying a thermal Comptonization process of X-ray continuum production as for radioquiet Seyfert galaxies. Lohfink et al (2017) analyzed the Swift/NuSTAR X-ray spectra of an SSRQ (4C 74.26); no sign of jet emission but a high-energy cutoff of 183 +51 −35 keV was revealed.…”

Section: X-ray Spectral Propertiesmentioning

confidence: 99%

See 1 more Smart Citation

The $L_\mathrm{x}$-$L_\mathrm{uv}$-$L_\mathrm{radio}$ relation and corona-disk-jet connection in optically selected radio-loud quasars

Zhu,

Brandt,

Luo

et al. 2020

Preprint

View full text Add to dashboard Cite

Radio-loud quasars (RLQs) are more X-ray luminous than predicted by the X-rayoptical/UV relation (i.e. L x ∝ L γ uv ) for radio-quiet quasars (RQQs). The excess X-ray emission depends on the radio-loudness parameter (R) and radio spectral slope (α r ). We construct a uniform sample of 729 optically selected RLQs with high fractions of X-ray detections and α r measurements. We find that steep-spectrum radio quasars (SSRQs; α r ≤ −0.5) follow a quantitatively similar L x ∝ L γ uv relation as that for RQQs, suggesting a common coronal origin for the X-ray emission of both SSRQs and RQQs. However, the corresponding intercept of SSRQs is larger than that for RQQs and increases with R, suggesting a connection between the radio jets and the configuration of the accretion flow. Flat-spectrum radio quasars (FSRQs; α r > −0.5) are generally more X-ray luminous than SSRQs at given L uv and R, likely involving more physical processes. The emergent picture is different from that commonly assumed where the excess X-ray emission of RLQs is attributed to the jets. We thus perform model selection to compare critically these different interpretations, which prefers the coronal scenario with a corona-jet connection. A distinct jet component is likely important for only a small portion of FSRQs. The corona-jet, disk-corona, and disk-jet connections of RLQs are likely driven by independent physical processes. Furthermore, the coronajet connection implies that small-scale processes in the vicinity of SMBHs, probably associated with the magnetic flux/topology instead of black-hole spin, are controlling the radio-loudness of quasars.

show abstract

“…Ronchini et al 2019), 3C 120 (e.g. Rani &Stalin 2018), and3C 390.3 (e.g. Sambruna et al 2009;Lohfink et al 2015) are consistent with being disk/corona-related.…”

Section: X-ray Spectral Propertiesmentioning

confidence: 56%

Section: X-ray Spectral Propertiesmentioning

confidence: 99%

The $L_\mathrm{x}$-$L_\mathrm{uv}$-$L_\mathrm{radio}$ relation and corona-disk-jet connection in optically selected radio-loud quasars

Zhu,

Brandt,

Luo

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…Broadband X-ray spectral fits revealed the presence of a high energy cut-off at E cut = 83 +10 −8 keV [10]. Analysis of the same timing data presented by [35] hinted towards the presence of a QPO. Therefore, the goal of this study is to confirm the presence of QPO using well-established methods.…”

Section: Introductionmentioning

confidence: 65%

A Possible Quasi-Periodic Oscillation in the X-ray Emission of 3C 120

et al. 2021

Self Cite

View full text Add to dashboard Cite

We present here the detection of a possible quasi-periodic oscillation (QPO) signal in the X-ray light curve of the active galactic nucleus 3C 120, a broad line radio galaxy at z = 0.033. The hint of a QPO at the 3σ level at 7.1 × 10−6 Hz (∼1.65 days) was detected based on the analysis of X-ray data acquired in the 3–79 keV band by the Nuclear Spectroscopic Telescope Array (NuSTAR). The data, when processed separately in the soft (3–10 keV), hard (10–79 keV) and the total (3–79 keV) bands using four different techniques, namely discrete correlation function, Lomb Scargle periodogram, structure–function, and power spectral density indicated the presence of a QPO. 3C 120 very well fits in the negative correlation in the frequency of the QPO versus the black hole mass (FQPO versus MBH) diagram known for stellar-mass and supermassive black hole sources. Considering the observed signs of QPO to represent the innermost stable orbit of the accretion disk, we found a black hole mass of 1.9×109 M⊙ for a Kerr black hole and 3.04×108 M⊙ for a Schwarzschild black hole. This deduced black hole mass from QPO measurement is a few times larger than the black hole mass obtained from reverberation mapping observations.

show abstract

“…Similarly, Comptonization parameters for the BLRG 3C 390.3 were constrained by Lohfink et al (2015) using broad-band X-ray data. Using radio/X-ray data, a link between the events in the jet emission and accretion disk has been studied in the BLRG 3C 111 (Chatterjee et al 2011) and the BLRG 3C 120 (Lohfink et al 2013;Rani, & Stalin 2018). Studying more BLRGs will provide valuable data points needed to study the difference between jetted and non-jetted central engines.…”

Section: Introductionmentioning

confidence: 99%

Broad-band X-ray observation of broad-line radio galaxy 3C 109

Chalise,

Lohfink,

Kara

et al. 2020

Preprint

View full text Add to dashboard Cite

We present a study of the central engine in the broad-line radio galaxy 3C 109. To investigate the immediate surrounding of this accreting, supermassive black hole, we perform a multi-epoch broadband spectral analysis of a joint NuSTAR/XMM observation (2017), an archival XMM observation (2005) and the 105-month averaged Swift-BAT data. We are able to clearly separate the spectrum into a primary continuum, neutral and ionized absorption, and a reflection component. The photon index of the primary continuum has changed since 2005 (Γ = 1.61 +0.02 −0.01 → 1.54 ± 0.02), while other components remain unchanged, indicative of minimal geometric changes to the central engine. We constrain the high-energy cutoff of 3C 109 (E cut = 49 +7 −5 keV ) for the first time. The reflector is found to be ionized (log ξ = 2.3 +0.1 −0.2 ) but no relativistic blurring is required by the data. SED analysis confirms the super-Eddington nature of 3C 109 initially (λ Edd > 2.09). However, we do not find any evidence for strong reflection (R = 0.18 +0.04 −0.03 ) or a steep power law index, as expected from a super-Eddington source. This puts the existing virial mass estimate of 2 ×10 8 M ⊙ into question. We explore additional ways of estimating the Eddington ratio, some of which we find to be inconsistent with our initial SED estimate. We obtain a new black hole mass estimate of 9.3 ×10 8 M ⊙ , which brings all Eddington ratio estimates into agreement and does not require 3C 109 to be super-Eddington.

show abstract

Coronal Proerties of the Seyfert 1 Galaxy 3C 120 with NuSTAR

Cited by 18 publications

References 76 publications

The $L_\mathrm{x}$-$L_\mathrm{uv}$-$L_\mathrm{radio}$ relation and corona-disk-jet connection in optically selected radio-loud quasars

The $L_\mathrm{x}$-$L_\mathrm{uv}$-$L_\mathrm{radio}$ relation and corona-disk-jet connection in optically selected radio-loud quasars

A Possible Quasi-Periodic Oscillation in the X-ray Emission of 3C 120

Broad-band X-ray observation of broad-line radio galaxy 3C 109

Contact Info

Product

Resources

About