INTEGRAL/IBIS 17-yr hard X-ray all-sky survey

Krivonos, R.; Sazonov, S.; Кузнецова, Е. А.; Lutovinov, A.; Mereminskiy, I. A.; Tsygankov, Sergey S.

doi:10.1093/mnras/stab3751

“…In the hard X-rays (10 keV), obscuration is less important due to the lower photoelectric cross section of the obscuring material, which enables recovery of most of the X-ray flux up to ( ) N log cm 23.5 H 2 -(e.g., Ricci et al 2015). Therefore, hard X-ray surveys, such as those carried out by INTEGRAL (e.g., Paltani et al 2008;Beckmann et al 2009;Krivonos et al 2022), Swift/Burst Alert Telescope (BAT; e.g., Markwardt et al 2005;Tueller et al 2008;Cusumano et al 2010;Tueller et al 2010;Baumgartner et al 2013;Oh et al 2018), and NuSTAR (e.g., Alexander et al 2013;Civano et al 2015;Mullaney et al 2015;Harrison et al 2016;Del Moro et al 2017;Zappacosta et al 2018a;Masini et al 2018), are very well suited to detect and characterize obscured AGNs, particularly at low redshift. The all-sky Swift/BAT survey, in particular, has detected ∼1100 AGNs in the 14-195 keV band (Oh et al 2018).…”

Section: Introductionmentioning

confidence: 99%

BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes

Ricci

¹

,

Ananna

²

,

Temple

³

et al. 2022

ApJ

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We study the relation between obscuration and supermassive black hole (SMBH) accretion using a large sample of hard X-ray selected active galactic nuclei (AGNs). We find a strong decrease in the fraction of obscured sources above the Eddington limit for dusty gas ( log λ Edd ≳ − 2 ) confirming earlier results, and consistent with the radiation-regulated unification model. This also explains the difference in the Eddington ratio distribution functions (ERDFs) of type 1 and type 2 AGNs obtained by a recent study. The break in the ERDF of nearby AGNs is at log λ Edd * = − 1.34 ± 0.07 . This corresponds to the λ Edd where AGNs transition from having most of their sky covered by obscuring material to being mostly devoid of absorbing material. A similar trend is observed for the luminosity function, which implies that most of the SMBH growth in the local universe happens when the AGN is covered by a large reservoir of gas and dust. These results could be explained with a radiation-regulated growth model, in which AGNs move in the N H–λ Edd plane during their life cycle. The growth episode starts with the AGN mostly unobscured and accreting at low λ Edd. As the SMBH is further fueled, λ Edd, N H and the covering factor increase, leading the AGN to be preferentially observed as obscured. Once λ Edd reaches the Eddington limit for dusty gas, the covering factor and N H rapidly decrease, leading the AGN to be typically observed as unobscured. As the remaining fuel is depleted, the SMBH goes back into a quiescent phase.

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“…The catalog contains 120 previously undiscovered soft γ-ray emitters. We also checked our results by comparing them to the findings in Krivonos et al (2022).…”

Section: High-energy Surveys For Cross-matching Analysismentioning

confidence: 99%

“…This is also shown in recent results achieved thanks to the NuSTAR observations in the 3-20 keV band (Krivonos et al 2021a). This has also been possible thanks to improvements achieved in the preparation of hard X-ray source catalogs (see e.g., Markwardt et al 2005;Beckmann et al 2006;Krivonos et al 2007b;Sazonov et al 2007;Tueller et al 2008;Cusumano et al 2010;Bottacini et al 2012;Bird et al 2016;Mereminskiy et al 2016;Krivonos et al 2017;Oh et al 2018;Krivonos et al 2021bKrivonos et al , 2022 and the association of hard X-ray sources with their low-energy counterparts (e.g., Malizia et al 2010;Koss et al 2019;Bär et al 2019;Smith et al 2020) and their optical spectroscopy follow-ups (e.g., Masetti et al 2006aMasetti et al ,b, 2008Masetti et al , 2012Masetti et al , 2013Parisi et al 2014;Rojas et al 2017;Marchesini et al 2019).…”

Section: Introductionmentioning

confidence: 99%

A multifrequency characterization of the extragalactic hard X-ray sky

Kosiba

¹

,

Massaro

²

,

Peña-Herazo

³

et al. 2023

A&A

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Context. Nowadays, we know that the origin of the cosmic X-ray background (CXB) is the integrated emission of nearby active galactic nuclei. Therefore, in order to obtain a precise estimate of the contribution of different source classes to the CXB, it is crucial to achieve full characterization of the hard-X ray sky. Aims. We present a multifrequency analysis of all sources listed in the third release of the Palermo Swift-BAT hard X-ray catalog (3PBC) with the goal of (i) identifying and classifying the largest number of sources adopting multifrequency criteria, with particular emphasis on extragalactic populations and (ii) extracting sources belonging to the class of Seyfert galaxies to present here the release of the second version of the Turin-SyCAT. Methods. We outline a classification scheme based on radio, infrared (IR), and optical criteria that allows us to distinguish between unidentified and unclassified hard X-ray sources, as well as to classify those sources belonging to the Galactic and the extragalactic populations. Results. Our revised version of the 3PBC lists 1176 classified, 820 extragalactic, and 356 Galactic sources, as well as 199 unclassified and 218 unidentified sources. According to our analysis, the hard X-ray sky is mainly populated by Seyfert galaxies and blazars. For the blazar population, we report trends between the hard X-ray and the gamma-ray emissions based on the fact that a large fraction of them also have a counterpart detected by the Fermi satellite. These trends are all in agreement with the expectations of inverse Compton models which are widely adopted to explain the blazar broadband emission. For the Seyfert galaxies, we present the second version of the Turin-SyCAT, including a total of 633 Seyfert galaxies, with 282 new sources corresponding to an increase of ∼80 % with respect to the previous release. Comparing the hard X-ray and the infrared emissions of Seyfert galaxies, we confirm that there is no clear difference between the flux distribution of the infrared-to-hard X-ray flux ratio of Seyfert galaxies Type 1 and Type 2. However, there is a significant trend between the mid-IR flux and hard X-ray flux, confirming previous statistical results in the literature. Conclusions. We provide two catalog tables. The first is the revised version of the 3PBC catalog based on our multifrequency analyses. The second catalog table is a release of the second version of the Turin-SyCAT catalog. Finally, we highlight that extensive soft X-ray data are already available in the form of the SWIFT archive which can be used to search for potential counterparts of unidentified hard X-ray sources. All these datasets will be reduced and analyzed in a forthcoming analysis to determine the precise position of lowenergy counterparts in the 0.5 -10 keV energy range for 3PBC sources that can be targets of future optical spectroscopic campaigns; this is necessary to obtain their precise classification.

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“…The source position was covered over four epochs in the XMM Slew Surveys, including two epochs of X-ray detection in 2010 and 2015, respectively. The source was also covered by the ROSAT (Voges et al 1999) and INTEGRAL (Krivonos et al 2022) sky surveys, but not detected. We summarize the archival X-ray coverage in Table 5.…”

Section: X-ray Coverage From Surveysmentioning

confidence: 99%

SRGA J181414.6-225604: A New Galactic Symbiotic X-Ray Binary Outburst Triggered by an Intense Mass-loss Episode of a Heavily Obscured Mira Variable

De

¹

,

Mereminskiy

²

,

Soria

³

et al. 2022

ApJ

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We present the discovery and multiwavelength characterization of SRGA J181414.6-225604, a Galactic hard X-ray transient discovered during the ongoing SRG/ART-XC sky survey. Using data from the Palomar Gattini-IR survey, we identify a spatially and temporally coincident variable infrared (IR) source, IRAS 18111-2257, and classify it as a very-late-type (M7–M8), long-period (1502 ± 24 days), and luminous (M K ≈ −9.9 ± 0.2) O-rich Mira donor star located at a distance of ≈14.6+2.9 −2.3 kpc. Combining multicolor photometric data over the last ≈25 yr, we show that the IR counterpart underwent a recent (starting ≈800 days before the X-ray flare) enhanced mass-loss (reaching ≈2.1 × 10−5 M ⊙ yr−1) episode, resulting in an expanding dust shell obscuring the underlying star. Multi-epoch follow-up observations from Swift, NICER, and NuSTAR reveal a ≈200 day long X-ray outburst reaching a peak luminosity of L X ≈ 2.5 × 1036 erg s−1, characterized by a heavily absorbed (N H ≈ 6 × 1022 cm−2) X-ray spectrum consistent with an optically thick Comptonized plasma. The X-ray spectral and timing behavior suggest the presence of clumpy wind accretion, together with a dense ionized nebula overabundant in silicate material surrounding the compact object. Together, we show that SRGA J181414.6-225604 is a new symbiotic X-ray binary in outburst, triggered by an intense dust-formation episode of a highly evolved donor. Our results offer the first direct confirmation for the speculated connection between enhanced late-stage donor mass loss and the active lifetimes of symbiotic X-ray binaries.

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INTEGRAL/IBIS 17-yr hard X-ray all-sky survey

Cited by 30 publications

References 247 publications

BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes

BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes

A multifrequency characterization of the extragalactic hard X-ray sky

SRGA J181414.6-225604: A New Galactic Symbiotic X-Ray Binary Outburst Triggered by an Intense Mass-loss Episode of a Heavily Obscured Mira Variable

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