Breaking the rules at <i>z</i> ≃ 0.45: The rebel case of RBS 1055

Marinucci, Andrea; Vietri, G.; Piconcelli, E.; Bianchi, S.; Guainazzi, M.; Lanzuisi, G.; Stern, Daniel; Vignali, C.

doi:10.1051/0004-6361/202244272

Cited by 5 publications

(4 citation statements)

References 120 publications

(133 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Similar large equi v alent widths have also been seen in a fe w po werful QSOs (e.g. Krumpe et al 2010 ;Marinucci et al 2022 ). KYNSED includes a disc reflection component with a selfconsistently calculated ionization profile.…”

Section: X-ray Reflectionsupporting

confidence: 69%

“…9 ). Our results add another QSO to the highly accreting sources with a low coronal temperature (e. (Marinucci et al 2022 ). The coronal temperature in J1144 is broadly consistent with these sources, being among the lowest.…”

Section: Cor Onal Pr Opertiesmentioning

confidence: 54%

“…Comparison of J1144 to other quasars from the literature, with L 2 −10 > 10 45 erg s −1 , in the kT − L 2-10 plane.also found low temperatures in two rapidly accreting AGN Mrk 382, IRAS 04416 + 1215. In Fig.10, we compare J1144 to other sources with L 2 −10 > 10 45 erg s −1 , namely: B2202-209(Kammoun et al 2017 ), 2MASS J1614346 + 470420 and B1422 + 231(Lanzuisi et al 2019 ), APM 08279 + 5255(Bertola et al 2022 ), and RBS 1055(Marinucci et al 2022 ). The coronal temperature in J1144 is broadly consistent with these sources, being among the lowest.…”

mentioning

confidence: 99%

See 2 more Smart Citations

The first X-ray look at SMSS J114447.77-430859.3: the most luminous quasar in the last 9 Gyr

Kammoun

Igo

Miller

et al. 2023

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

SMSS J114447.77-430859.3 (z = 0.83) has been identified in the SkyMapper Southern Survey as the most luminous quasar in the last $\sim 9\, \rm Gyr$. In this paper, we report on the eROSITA/Spectrum-Roentgen-Gamma (SRG) observations of the source from the eROSITA All Sky Survey, along with presenting results from recent monitoring performed using Swift, XMM-Newton, and NuSTAR. The source shows a clear variability by factors of ∼10 and ∼2.7 over timescales of a year and of a few days, respectively. When fit with an absorbed power law plus high-energy cutoff, the X-ray spectra reveal a Γ = 2.2 ± 0.2 and $E_{\rm cut}=23^{+26}_{-5}\, \rm keV$. Assuming Comptonisation, we estimate a coronal optical depth and electron temperature of τ = 2.5 − 5.3 (5.2 − 8) and $kT=8-18\, (7.5-14)\, \rm keV$, respectively, for a slab (spherical) geometry. The broadband SED is successfully modelled by assuming either a standard accretion disc illuminated by a central X-ray source, or a thin disc with a slim disc emissivity profile. The former model results in a black hole mass estimate of the order of 1010 M⊙, slightly higher than prior optical estimates; meanwhile, the latter model suggests a lower mass. Both models suggest sub-Eddington accretion when assuming a spinning black hole, and a compact (∼10 rg) X-ray corona. The measured intrinsic column density and the Eddington ratio strongly suggest the presence of an outflow driven by radiation pressure. This is also supported by variation of absorption by an order of magnitude over the period of $\sim 900\, \rm days$.

show abstract

Section: X-ray Reflectionsupporting

confidence: 69%

Section: Cor Onal Pr Opertiesmentioning

confidence: 54%

mentioning

confidence: 99%

See 1 more Smart Citation

The first X-ray look at SMSS J114447.77-430859.3: the most luminous quasar in the last 9 Gyr

Kammoun

Igo

Miller

et al. 2023

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…So far, a total of four non-blazar AGN have been observed (NGC 4151,, the Circinus galaxy, and IC 4329A). Only upper limits could be determined for MCG-05-23-16 (Marinucci et al, 2022b;Tagliacozzo et al, 2023) and IC 4329A (Ingram et al, 2023), which are not conclusive on the geometry of the X-ray source. The Circinus galaxy shows a polarization of 28 ± 7 per cent (at 68 per cent confidence level), with a polarization angle of 18°± 5°, roughly perpendicular to the radio jet (Ursini et al, 2023).…”

Section: Observational Constraintsmentioning

confidence: 95%

The high energy X-ray probe (HEX-P): probing the physics of the X-ray corona in active galactic nuclei

Kammoun,

Lohfink,

Masterson

et al. 2024

Front. Astron. Space Sci.

View full text Add to dashboard Cite

The hard X-ray emission in active galactic nuclei (AGN) and black hole X-ray binaries is thought to be produced by a hot cloud of electrons referred to as the corona. This emission, commonly described by a power law with a high-energy cutoff, is suggestive of Comptonization by thermal electrons. While several hypotheses have been proposed to explain the origin, geometry, and composition of the corona, we still lack a clear understanding of this fundamental component. NuSTAR has been playing a key role improving our knowledge of X-ray coronæ thanks to its unprecedented sensitivity above 10 keV. However, these constraints are limited to bright, nearby sources. The High Energy X-ray Probe (HEX-P) is a probe-class mission concept combining high spatial resolution X-ray imaging and broad spectral coverage (0.2–80 keV) with a sensitivity superior to current facilities. In this paper, we highlight the major role that HEX-P will play in further advancing our insights of X-ray coronæ notably in AGN. We demonstrate how HEX-P will measure key properties and track the temporal evolution of coronæ in unobscured AGN. This will allow us to determine their electron distribution and test the dominant emission mechanisms. Furthermore, we show how HEX-P will accurately estimate the coronal properties of obscured AGN in the local Universe, helping address fundamental questions about AGN unification. In addition, HEX-P will characterize coronæ in a large sample of luminous quasars at cosmological redshifts for the first time and track the evolution of coronæ in transient systems in real time. We also demonstrate how HEX-P will enable estimating the coronal geometry using spectral-timing techniques. HEX-P will thus be essential to understand the evolution and growth of black holes over a broad range of mass, distance, and luminosity, and will help uncover the black holes’ role in shaping the Universe.

show abstract

The XMM-Newton and NuSTAR view of IRASF11119+3257

Lanzuisi,

Matzeu,

Baldini

et al. 2024

A&A

View full text Add to dashboard Cite

IRASF11119+3257 is an ultra-luminous infrared galaxy with a post-merger morphology, hosting a type-1 quasar at z=0.189. It shows a prominent ultra-fast outflow (UFO) absorption feature ($ in its 2013 spectrum. This is the first system in which the energy released by the UFO was compared to that of the known galaxy-scale molecular outflow to investigate the mechanism driving active galactic nuclei (AGN) feedback. In 2021, we obtained the first long look of the target, coordinated with a simultaneous observation, with the goal of constraining the broad band continuum and the nuclear wind physical properties and energetics with an unprecedented accuracy. The new high-quality data allowed us to clearly detect at a confidence level $P>99.8<!PCT!>$ multiple absorption features associated with the known UFO at the 9.1 and 11.0 keV rest frames. Furthermore, an emission plus absorption feature at $1.1-1.3$ keV reveals the presence of a blueshifted P-Cygni profile in the soft band. We associate the two hard band features with blends of FeXXV and FeXXVI and line pairs and infer a large column ($ $ cmsq ) of highly ionized ($log gas outflowing at $ The 1.3 keV absorption line can be associated with a blend of Fe and Ne transitions, produced by a lower column ($ $ cmsq ) and ionization ($log gas component outflowing at the same speed. Using a radiative-transfer disk wind model to fit the highly ionized UFO, we derive a mass outflow rate comparable with the mass accretion rate and the Eddington limit ($ macc and $ medd ), and kinetic energy ($ and $ and momentum flux ($ among the highest reported in the literature. We measured an extremely low high-energy cutoff ($ keV). This and several other cases in the literature suggest that a steep X-ray continuum may be related to the formation of powerful winds. We also analyzed the ionized OIII component of the large-scale outflow through optical spectroscopy and derived a large outflow velocity ($ km/s) and energetics comparable with the large-scale molecular outflows. Finally, we observe a trend of decreasing outflow velocity from forbidden optical emission lines of decreasing ionization levels, interpreted as the outflow decelerating at large distances from the ionizing source. The lack of a significant momentum boost between the nuclear UFO and the different phases of the large-scale outflow, observed in IRASF11119 and in a growing number of similar sources, can be explained by (i) a momentum-driven expansion, (ii) an inefficient coupling of the UFO with the host interstellar medium, or (iii) by repeated energy-driven expansion episodes with a low duty cycle, that average out on long timescales to produce the observed large-scale outflow.

show abstract

Breaking the rules at z ≃ 0.45: The rebel case of RBS 1055

Cited by 5 publications

References 120 publications

The first X-ray look at SMSS J114447.77-430859.3: the most luminous quasar in the last 9 Gyr

The first X-ray look at SMSS J114447.77-430859.3: the most luminous quasar in the last 9 Gyr

The high energy X-ray probe (HEX-P): probing the physics of the X-ray corona in active galactic nuclei

The XMM-Newton and NuSTAR view of IRASF11119+3257

Contact Info

Product

Resources

About