High-Velocity Neon Line Emission From the Ulirg Iras F00183-7111: Revealing the Optically Obscured Base of a Nuclear Outflow

Spoon, H. W. W.; Armus, L.; Marshall, J. A.; Bernard─Salas, J.; Farrah, D.; Charmandaris, V.; Kent, Brian R.

doi:10.1088/0004-637x/693/2/1223

Cited by 37 publications

(52 citation statements)

References 62 publications

(136 reference statements)

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“…The inferred blueshift v 0.18 c lies in the range of high-velocity outflows found in growing number of Seyfert galaxies and quasars (e.g., Tombesi et al 2010). Given the presence of powerful outflow signatures observed in mid-IR (Spoon et al 2009), optical (Heckman et al 1990) and possibly radio (Ruffa et al in prep.) bands, detection of X-ray outflowing gas comes as no surprise.…”

Section: Direct Emission Scenariomentioning

confidence: 70%

“…7) but is becoming more radio-loud in recent years with elevated radio activity (Reynolds et al 2017). Curiously, the mid-IR AGN tracer [Ne v]λ14.32 µm is not detected in either objects (Armus et al 2007;Spoon et al 2004Spoon et al , 2009). Contrary to the common wisdom for AGN being variable X-ray sources, both IRAS F00183-7111 and Mrk 231 show stable intrinsic brightness over years.…”

Section: Similarities To Mrk 231 High Accretion Ratementioning

confidence: 99%

“…The radio to hard X-ray spectral energy distribution (SED) of IRAS F00183-7111 (in red). The radio data, submillimetre to infrared data, and the optical to UV data are taken from Norris et al (2012, references therein), Spoon et al (2009) and NED, respectively. For comparison, the SEDs of Arp 220 and Mrk 231, normalised to the far-infrared peak of IRAS F00183-7111, are overplotted in light grey and blue, respectively.…”

Section: Reflection Scenariomentioning

confidence: 99%

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The active nucleus of the ULIRG IRAS F00183–7111 viewed byNuSTAR

Iwasawa

Spoon

Comastri

et al. 2017

A&A

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We present an X-ray study of the ultra-luminous infrared galaxy IRAS F00183-7111 (z = 0.327), using data obtained from NuSTAR, Chandra X-ray Observatory, Suzaku and XMM-Newton. The Chandra imaging shows that a pointlike X-ray source is located at the nucleus of the galaxy at energies above 2 keV. However, the point source resolves into diffuse emission at lower energies, extending to the east, where the extranuclear [Oiii]λ5007 emission, presumably induced by a galactic-scale outflow, is present. The nuclear source is detected by NuSTAR up to the rest-frame 30 keV. The strong, high-ionization Fe K line, first seen by XMM-Newton, and subsequently by Suzaku and Chandra, is not detected in the NuSTAR data. The line flux appears to have been declining continuously between 2003 and 2016, while the continuum emission remained stable to within 30%. Further observations are needed to confirm this. The X-ray continuum below 10 keV is characterised by a hard spectrum caused by cold absorption of NH∼ 1 × 10 23 cm −2 , compatible to that of the silicate absorption at 9.7µm, and a broad absorption feature around 8 keV which we attribute to a high-ionization Fe K absorption edge. The latter is best described by a blueshifted, high-ionization (log ξ ∼ 3) absorber with a column density of NH∼ 1 × 10 24 cm −2 , similar to the X-ray high-velocity outflows observed in a number of active nuclei. No extra hard component, which would arise from a strongly absorbed (i.e. Compton-thick) source, is seen in the NuSTAR data. While a pure reflection scenario (with a totally hidden central source) is viable, direct emission from the central source of L 2−10keV 2 × 10 44 erg s −1 , behind layers of cold and hot absorbing gas may be an alternative explanation. In this case, the relative X-ray quietness (Lx/L bol,AGN ≤ 6 × 10 −3 ), the high-ionization Fe line, strong outflows inferred from various observations, and other similarities to the well-studied ULIRG/QSO Mrk 231 point that the central source in this ULIRG might be accreting close to the Eddington limit.

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Section: Direct Emission Scenariomentioning

confidence: 70%

Section: Similarities To Mrk 231 High Accretion Ratementioning

confidence: 99%

Section: Reflection Scenariomentioning

confidence: 99%

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The active nucleus of the ULIRG IRAS F00183–7111 viewed byNuSTAR

Iwasawa

Spoon

Comastri

et al. 2017

A&A

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“…It contains a heavily obscured AGN with L X ∼ 10 44 erg s −1 , and shows a reflection-dominated X-ray spectrum with a strong Fe xxv line (Nandra & Iwasawa 2007). A remarkable characteristic of this ULIRG is the presence of fast outflows (up to ∼3000 km s −1 ) probed by optical [Oiii]λ5007 (Heckman et al 1990), and the mid-IR [Ne ii] lines (Spoon et al 2009). A small-scale radio jet imaged with VLBI supports the idea of an AGN driven outflow (Norris et al 2011).…”

Section: High-z Type II Objects: the Local Analogue And Eddington Ratiomentioning

confidence: 96%

Fe K emission from active galaxies in the COSMOS field

Iwasawa

Mainieri²,

Brusa

et al. 2012

A&A

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We present a rest-frame spectral stacking analysis of ∼1000 X-ray sources detected in the XMM-COSMOS field to investigate the iron-K line properties of active galaxies beyond redshift z ∼ 1. In Type I AGN that have a typical X-ray luminosity of L X ∼ 1.5 × 10 44 (erg s −1 ) and z ∼ 1.6 the cold Fe K at 6.4 keV is weak (EW ∼ 0.05 keV), which agrees with the known trend. In contrast, high-ionization lines of Fe xxv and Fe xxvi are pronounced. These high-ionization Fe K lines appear to have a connection with high accretion rates. While no broad Fe emission is detected in the total spectrum, it might be present, albeit at low significance (∼2σ), when the X-ray luminosity is restricted to the range below 3 × 10 44 erg s −1 , or when an intermediate range of Eddington ratio around λ ∼ 0.1 is selected. In Type II AGN, both cold and high-ionzation lines become weak with increasing X-ray luminosity. However, we detected strong high-ionization Fe K (EW ∼ 0.3 keV) in the spectrum of objects at z > 2, while we found no 6.4 keV line. We also found that the primary source of the high-ionization Fe K emission are those objects detected with Spitzer-MIPS at 24 μm. Given their median redshift of z 2.5, their bolometric luminosity is likely to reach 10 13 L and the MIPS-detected emission most likely originates from hot dust heated by embedded AGN, probably accreting at high Eddington ratio. These properties match those of rapidly growing black holes in ultra-luminous infrared galaxies at the interesting epoch (z ∼ 2-3) of galaxy formation.

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“…Some sources, notably IRAS 07598+6508 (z=0.148), Mrk 1014 (z=0.163), IRAS 13451+1232 (z=0.122) and IRAS 08572 +3915 (z=0.058), do not show CO lines. These sources are associated with AGN/BAL QSOs (Lipari 1994;Boller et al 2002;Spoon et al 2009). Note that the FTS spectrum of IRAS 08572+3915 has been reported in Efstathiou et al (2014) and was modeled with an edge-on AGN torus.…”

Section: Fitted Spectramentioning

confidence: 99%

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Pearson¹,

Rigopoulou²,

Hurley³

et al. 2016

ApJS

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We present the Herschel SPIRE Fourier Transform Spectroscopy (FTS) atlas for a complete flux-limited sample of local ultraluminous infrared galaxies (ULIRGs) as part of the HERschel Ultra Luminous InfraRed Galaxy Survey (HERUS). The data reduction is described in detail and was optimized for faint FTS sources ,with particular care being taken for the subtraction of the background, which dominates the continuum shape of the spectra. To improve the final spectra, special treatment in the data reduction has been given to any observation suffering from artifacts in the data caused by anomalous instrumental effects. Complete spectra are shown covering 200-671 μm, with photometry in the SPIRE bands at 250, 350, and 500 μm. The spectra include near complete CO ladders for over half of our sample, as well as fine structure lines from [C I] 370 μm, [C I] 609 μm, and [N II] 205 μm. We also detect H 2 O lines in several objects. We construct CO spectral line energy distributions (SLEDs) for the sample, and compare their slopes with the far-infrared (FIR) colors and luminosities. We show that the CO SLEDs of ULIRGs can be broadly grouped into three classes based on their excitation. We find that the mid-J (5<J<8) lines are better correlated with the total FIR luminosity, suggesting that the warm gas component is closely linked to recent star formation. The higher J transitions do not linearly correlate with the FIR luminosity, consistent with them originating in hotter, denser gas that is unconnected to the current star formation. We conclude that in most cases more than one temperature component is required to model the CO SLEDs.

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High-Velocity Neon Line Emission From the Ulirg Iras F00183-7111: Revealing the Optically Obscured Base of a Nuclear Outflow

Cited by 37 publications

References 62 publications

The active nucleus of the ULIRG IRAS F00183–7111 viewed byNuSTAR

The active nucleus of the ULIRG IRAS F00183–7111 viewed byNuSTAR

Fe K emission from active galaxies in the COSMOS field

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

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