The peculiar optical-UV X-ray spectra of the X-ray weak quasar PG 0043+039

Kollatschny, W.; Schartel, N.; Zetzl, M.; Santos-Lleó, M.; Rodríguez-Pascual, P. M.; Ballo, L.; Talavera, A.

doi:10.1051/0004-6361/201526820

Cited by 6 publications

(4 citation statements)

References 71 publications

(130 reference statements)

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“…Besides Mkn 335 and 1H0707-495, we also successfully observed Mkn 1048, PG 0844+349, PG 0043+039, PG 2112+059, PG 1535+547, and HE 1136-2304 (Parker et al 2014;Gallo et al 2011;Kollatschny et al 2015Kollatschny et al , 2016Schartel et al 2007Schartel et al , 2010Ballo et al 2008;Parker et al 2016;Komossa et al 2017;Zetzl et al 2018) with XMM-Newton and NuSTAR. One of the most recent AGN discovered as part of this survey was RX J2317.8-4422 (α 2000 = 23h 17m 50s, δ 2000 = -44 • 22 ′ 27 ′′ , z=0.134).…”

Section: Introductionsupporting

confidence: 56%

Swift, NuStar and XMM-Newton observations of the NLS1 galaxy RX J2317.8–4422 in an extreme X-ray low flux state

Grupe

Komossa

Gallo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report the discovery of RX J2317.8-4422 in an extremely low X-ray flux state by the Neil Gehrels Swift observatory in 2014 April/May. In total, the low-energy X-ray emission dropped by a factor 100. We have carried out multi-wavelength followup observations of this Narrow-Line Seyfert 1 galaxy. Here we present observations with Swift, XMM-Newton, and NuSTAR in October and November 2014 and further monitoring observations by Swift from 2015 to 2018. Compared with the beginning of the Swift observations in 2005, in the November 2014 XMM-Newton and NuSTAR observation RX J2317-4422.8 dropped by a factor of about 80 in the 0.3-10 keV band. While the high-state Swift observations can be interpreted by a partial covering absorption model with a moderate absorption column density of N H = 5.4 × 10 22 cm −2 or blurred reflection, due to dominating background at energies above 2 keV the low-state XMM-Newton data can not distinguish between different multi-component models and were adequately fit with a single power-law model. We discuss various scenarios like a long-term change of the accretion rate or absorption as the cause for the strong variability seen in RX J2317.8-4422.

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Section: Introductionsupporting

confidence: 56%

Swift, NuStar and XMM-Newton observations of the NLS1 galaxy RX J2317.8–4422 in an extreme X-ray low flux state

Grupe

Komossa

Gallo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…An interesting candidate is the extremely X-ray weak BAL quasar PG 0043+039 whose UV spectrum peaks at ∼2500 Å and shows a set of broad humps that can be explained as cyclotron line emission from a strongly magnetised hot plasma close to the supermassive black hole (SMBH; Kollatschny et al 2015Kollatschny et al , 2016.…”

Section: Truncated Accretion Disksmentioning

confidence: 99%

Broad-band spectral energy distribution of 3000 Å break quasars from the Sloan Digital Sky Survey

Meusinger

Schalldach

Mirhosseini

et al. 2016

A&A

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Context. In past decades, huge surveys have confirmed the existence of populations of exotic and hitherto unknown quasar types. The discovery and investigation of these rare peculiar objects is important because they may represent links to special evolutionary stages and hold clues to the evolution of quasars and galaxies. Aims. The Sloan Digital Sky Survey (SDSS) discovered the unusual quasars J010540.75-003313.9 and J220445.27+003141.8 and a small number of similar objects. Their spectra are characterised by a break in the continuum around 3000 Å that neither shows the typical structure of broad absorption line (BAL) troughs nor is explained by typical intrinsic dust reddening. The main aim of the present paper was twofold. First, a new target-oriented search was performed in the spectra database of the SDSS to construct a sizable sample of such 3000 Å break quasars. Second, their broad-band spectral energy distribution (SED) was compared with SEDs of BAL quasars. Methods. We used the method of Kohonen self-organising maps for data mining in the SDSS spectra archive to search for more quasars with properties comparable to the prototypes J010540.75-003313.9 and J220445.27+003141.8. We constructed a sample of 3000 Å break quasars and comparison samples of quasars with similar properties, to some extent, but also showing indications for typical BAL features. Particular attention was payed to a possible contamination by rare stellar spectral types, in particular DQ white dwarfs. We construct ensemble-averaged broad-band SEDs based on archival data from SDSS, GALEX, 2MASS, UKIDSS, WISE, and other surveys. The SEDs were corrected for dust absorption at the systemic redshifts of the quasars by the comparison with the average SED of normal quasars. Results. We compiled a list of 23 quasars classified as 3000 Å break quasars with properties similar to 010540.75-003313.9 and J220445.27+003141.8. Their de-reddened arithmetic median composite SED is indistinguishable from that of the unusual BAL quasars. We conclude that 3000 Å break quasars are most likely extreme versions of BAL quasars. Assuming that the intrinsic SED of the continuum source is represented by the quasar composite SED, the 3000 Å break quasars tend to be intrinsically more luminous than ordinary quasars.

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“…They are believed to include intrinsically X-ray weak systems relative to their UV luminosity (e.g. Luo et al 2014;Kollatschny et al 2016), and are also likely to be outliers in the L X − L 6µm relation (e.g. Del Moro et al 2016).…”

Section: Discussionmentioning

confidence: 99%

Forward modeling the multiwavelength properties of Active Galactic Nuclei: application to X-ray and WISE mid-infrared samples

Georgakakis,

Ruiz,

LaMassa

2020

Preprint

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An empirical forward-modeling framework is developed to interpret the multiwavelength properties of Active Galactic Nuclei (AGN) and provide insights into the overlap and incompleteness of samples selected at different parts of the electromagnetic spectrum. The core of the model are observationally derived probabilites on the occupation of galaxies by X-ray selected AGN. These are used to seed mock galaxies drawn from stellar-mass functions with accretion events and then associate them with spectral energy distributions that describe both the stellar and AGN emission components. This approach is used to study the complementarity between X-ray and WISE mid-infrared AGN selection methods. We first show that the basic observational properties of the X-ray and WISE AGN (magnitude, redshift distributions) are adequately reproduced by the model. We then infer the level of contamination of the WISE selection and show that this is dominated by non-AGN at redshifts z < 0.5. These are star-forming galaxies that scatter into the WISE AGN selection wedge because of photometric uncertainties affecting their colours. Our baseline model shows a sharp drop in the number density of heavily obscured AGN above the Compton thick limit in the WISE bands. The model also overpredicts by a factor of 1.5 the fraction of X-ray associations in the WISE AGN selection box compared to observations. This suggests a population of X-ray faint sources that is not reproduced by the model. This discrepancy is discussed in the context of either heavily obscured or intrinsically X-ray weak AGN. Evidence is found in favour of the latter.

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The peculiar optical-UV X-ray spectra of the X-ray weak quasar PG 0043+039

Cited by 6 publications

References 71 publications

Swift, NuStar and XMM-Newton observations of the NLS1 galaxy RX J2317.8–4422 in an extreme X-ray low flux state

Swift, NuStar and XMM-Newton observations of the NLS1 galaxy RX J2317.8–4422 in an extreme X-ray low flux state

Broad-band spectral energy distribution of 3000 Å break quasars from the Sloan Digital Sky Survey

Forward modeling the multiwavelength properties of Active Galactic Nuclei: application to X-ray and WISE mid-infrared samples

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