<i>NuSTAR</i>REVEALS AN INTRINSICALLY X-RAY WEAK BROAD ABSORPTION LINE QUASAR IN THE ULTRALUMINOUS INFRARED GALAXY MARKARIAN 231

Teng, Stacy H.; Brandt, W. N.; Harrison, Fiona A.; Luo, B.; Alexander, D. M.; Bauer, F. E.; Boggs, Steven E.; Christensen, Finn Erland; Comastri, A.; Craig, William W.; Fabian, A. C.; Farrah, D.; Fiore, F.; Gandhi, P.; Grefenstette, Brian W.; Hailey, Charles J.; Hickox, Ryan C.; Madsen, K. K.; Ptak, A.; Rigby, Jane; Risaliti, G.; Saez, C.; Stern, Daniel; Veilleux, Sylvain; Walton, D. J.; Wik, Daniel R.; Zhang, W. W.

doi:10.1088/0004-637x/785/1/19

Cited by 92 publications

(116 citation statements)

References 98 publications

(194 reference statements)

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“…An alternative explanation for this discrepancy is that the AGN is intrinsically weak at X-ray wavelengths, as recently found by NuSTAR for the AGN in Mrk 231 (Teng et al 2014, see also Teng et al 2015).…”

Section: Agn Contribution To the Ir Luminositymentioning

confidence: 84%

NuSTAR UNVEILS A HEAVILY OBSCURED LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE LUMINOUS INFRARED GALAXY NGC 6286

Ricci

Bauer

Treister

et al. 2016

ApJ

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We report the detection of a heavily obscured active galactic nucleus (AGN) in the luminous infrared galaxy (LIRG) NGC 6286 identified in a 17.5 ks Nuclear Spectroscopic Telescope Array observation. The source is in an early merging stage and was targeted as part of our ongoing NuSTAR campaign observing local luminous and ultraluminous infrared galaxies in different merger stages. NGC 6286 is clearly detected above 10 keV and by including the quasi-simultaneous Swift/XRT and archival XMM-Newton and Chandra data, we find that the source is heavily obscured (N H ;(0.95−1.32) × 10 24 cm −2 ) with a column density consistent with being Compton-thick (CT, N log cm 24The AGN in NGC 6286 has a low absorption-corrected luminosity (L 2−10 keV ∼ 3 −20 × 10 41 erg s −1 ) and contributes 1% to the energetics of the system. Because of its low luminosity, previous observations carried out in the soft X-ray band (<10 keV) and in the infrared did not notice the presence of a buried AGN. NGC 6286 has multiwavelength characteristics typical of objects with the same infrared luminosity and in the same merger stage, which might imply that there is a significant population of obscured low-luminosity AGNs in LIRGs that can only be detected by sensitive hard X-ray observations.

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Section: Agn Contribution To the Ir Luminositymentioning

confidence: 84%

NuSTAR UNVEILS A HEAVILY OBSCURED LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE LUMINOUS INFRARED GALAXY NGC 6286

Ricci

Bauer

Treister

et al. 2016

ApJ

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“…Di Pompeo et al (2013) found a statistical excess in mid-IR luminosities of radio-loud BAL QSOs. Moreover, studies based on NuSTAR observations showed that the hard X-ray emission (8-24 keV) of BALs tend to be intrinsically weaker than that of non-BALs (Luo et al 2014;Teng et al 2014), even though in a previous Chandra survey conducted by Gallagher et al (2006), it was inferred that that BALs and non-BALs have the same X-ray fluxes in the energy range of 0.8-8 keV once intrinsic absorption is taken into account. The same conclusion was reached by Weymann et al (1991) noticing the similarity of the optical emission lines of BALs and other QSOs.…”

Section: Discussionmentioning

confidence: 99%

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Violino¹,

Coppin²,

Stevens³

et al. 2016

Mon. Not. R. Astron. Soc.

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It is thought that a class of broad absorption line (BAL) QSOs, characterised by Fe absorption features in their UV spectra (called 'FeLoBALs'), could mark a transition stage between the end of an obscured starburst event and a youthful QSO beginning to shed its dust cocoon, where Fe has been injected into the interstellar medium by the starburst. To test this hypothesis we have undertaken deep SCUBA-2 850 µm observations of a sample of 17 FeLoBAL QSOs with 0.89 z 2.78 and -23.31 M B -28.50 to directly detect an excess in the thermal emission of the dust which would probe enhanced star-formation activity. We find that FeLoBALs are not luminous sources in the submillimetre, none of them are individually detected at 850 µm, nor as a population through stacking (F s = 1.14 ± 0.58 mJy). Statistical and survival analyses reveal that FeLoBALs have sub-mm properties consistent with BAL and non-BAL QSOs with matched redshifts and magnitudes. An SED fitting analysis shows that the FIR emission is dominated by AGN activity, and a starburst component is required only in 6/17 sources of our sample; moreover the integrated total luminosity of 16/17 sources is L 10 12 L , high enough to classify FeLoBALs as infrared luminous.In conclusion, we do not find any evidence in support of FeLoBAL QSOs being a transition population between a ULIRG and an unobscured QSO; in particular, FeLoBALs are not characterized by a cold starburst which would support this hypothesis.

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“…BALQs do tend to show weaker X-ray emission (Brandt, Laor & Wills 2000), but generally by a factor of only 10-30. Recent high energy X-ray observations suggest the X-ray weakness is intrinsic and not due to absorption (Teng et al 2014). Furthermore, the recent study of Hamann et al (2013a) of mini-BALs with extreme velocity outflows, finds only weak X-ray absorption, which is not sufficient to prevent overionization.…”

Section: Introductionmentioning

confidence: 99%

Radiation pressure confinement – IV. Application to broad absorption line outflows

Baskin

Laor

Stern

2014

Monthly Notices of the Royal Astronomical Society

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A fraction of quasars present broad absorption lines, produced by outflowing gas with typical velocities of 3000-10,000 km s −1 . If the outflowing gas fills a significant fraction of the volume where it resides, then it will be highly ionized by the quasar due to its low density, and will not produce the observed UV absorption. The suggestion that the outflow is shielded from the ionizing radiation was excluded by recent observations. The remaining solution is a dense outflow with a filling factor f < 10 −3 . What produces such a small f ? Here we point out that radiation pressure confinement (RPC) inevitably leads to gas compression and the formation of dense thin gas sheets/filaments, with a large gradient in density and ionization along the line of sight. The total column of ionized dustless gas is a few times 10 22 cm −2 , consistent with the observed X-ray absorption and detectable P v absorption. The predicted maximal columns of various ions show a small dependence on the system parameters, and can be used to test the validity of RPC as a solution for the overionization problem. The ionization structure of the outflow implies that if the outflow is radiatively driven, then broad absorption line quasars should have L/L Edd 0.1.

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NuSTARREVEALS AN INTRINSICALLY X-RAY WEAK BROAD ABSORPTION LINE QUASAR IN THE ULTRALUMINOUS INFRARED GALAXY MARKARIAN 231

Cited by 92 publications

References 98 publications

NuSTAR UNVEILS A HEAVILY OBSCURED LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE LUMINOUS INFRARED GALAXY NGC 6286

NuSTAR UNVEILS A HEAVILY OBSCURED LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE LUMINOUS INFRARED GALAXY NGC 6286

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Radiation pressure confinement – IV. Application to broad absorption line outflows

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