<i>XMM-Newton</i>observation of the ULIRG NGC 6240

Boller, Th.; Keil, Ralf; Hasinger, G.; Costantini, E.; Fujimoto, R.; Anabuki, Naohisa; Lehmann, I.; Gallo, Luigi

doi:10.1051/0004-6361:20031217

Cited by 36 publications

(48 citation statements)

References 28 publications

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“…Both the temperature and the column density increase toward the central nuclei (Boller et al 2003;Netzer et al 2005;Wang et al 2014). The cold-temperature plasma, which is the outermost, extends up to ∼1.…”

Section: The Modelmentioning

confidence: 99%

“…The primary emission obscured by a column density of about N H ∼ 2 × 10 24 cm −2 emerges only at higher energies and was originally detected by the PDS instrument on board BeppoSAX (Vignati et al 1999). The nuclear intrinsic bolometric luminosity is in the quasar regime (L bol ∼ 10 45 erg s −1 , Vignati et al 1999;Ikebe et al 2000;Lira et al 2002;Boller et al 2003).…”

Section: Introductionmentioning

confidence: 99%

“…The two nuclei are surrounded by extended X-ray emission modeled as a multitemperature plasma; the temperature and column density increase toward the central regions and the metal abundances are higher than solar ( Z Z ∼ 2−2.5 − Netzer et al 2005; Z Z = 10 − Boller et al 2003;Wang et al 2014). …”

Section: Introductionmentioning

confidence: 99%

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Hard X-ray emission of the luminous infrared galaxy NGC 6240 as observed by NuSTAR

Puccetti

Comastri

Bauer

et al. 2016

A&A

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We present a broadband (∼0.3−70 keV) spectral and temporal analysis of NuSTAR observations of the luminous infrared galaxy NGC 6240 combined with archival Chandra, XMM-Newton, and BeppoSAX data. NGC 6240 is a galaxy in a relatively early merger state with two distinct nuclei separated by ∼1. 5. Previous Chandra observations resolved the two nuclei and showed that they are both active and obscured by Compton-thick material. Although they cannot be resolved by NuSTAR, we were able to clearly detect, for the first time, both the primary and the reflection continuum components thanks to the unprecedented quality of the NuSTAR data at energies >10 keV. The NuSTAR hard X-ray spectrum is dominated by the primary continuum piercing through an absorbing column density which is mildly optically thick to Compton scattering (τ 1.2, N H ∼ 1.5 × 10 24 cm −2 ). We detect moderately hard X-ray (>10 keV) flux variability up to 20% on short (15−20 ks) timescales. The amplitude of the variability is largest at ∼30 keV and is likely to originate from the primary continuum of the southern nucleus. Nevertheless, the mean hard X-ray flux on longer timescales (years) is relatively constant. Moreover, the two nuclei remain Compton-thick, although we find evidence of variability in the material along the line of sight with column densities N H ≤ 2 × 10 23 cm −2 over long (∼3−15 yr) timescales. The observed X-ray emission in the NuSTAR energy range is fully consistent with the sum of the best-fit models of the spatially resolved Chandra spectra of the two nuclei.

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Section: The Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Hard X-ray emission of the luminous infrared galaxy NGC 6240 as observed by NuSTAR

Puccetti

Comastri

Bauer

et al. 2016

A&A

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“…In a photoionized gas, emission from the resonant r iron line is weak, while the forbidden f and the intercombination i lines contribute almost equally to the total emission, considering a wide range of densities (Porquet & Dubau 2000;Bautista & Kallman 2000). On the other hand, in a collisionally ionized gas, the ratio of the lines points in favor of a dominant resonant line, with respect to the forbidden and intercombination lines, such as the case of NGC 6240 (Boller et al 2003;Wang et al 2014). In NGC 4945, the Fe xxv He-α complex is dominated by the forbidden f line (Fig.…”

Section: Diffuse Highly-ionized Fe Emissionmentioning

confidence: 99%

Spatially resolved Fe K spectroscopy of NGC 4945

Marinucci

Bianchi

Fabbiano

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the imaging and spectroscopic analysis of the combined Chandra ACIS-S observations of the Compton-thick Seyfert 2 galaxy NGC 4945. We performed a spatially-resolved spectroscopy of the circumnuclear environment of the source, picturing the innermost 200 parsecs around the highly absorbed nucleus. The additional 200 ks ACIS-S data with respect to the previous campaign allowed us to map with even greater detail the central structure of this source and to discover an enhanced iron emission in the innermost nuclear region, with respect to the associated Compton reflection continuum. We revealed that the Equivalent Width of the iron Kα line is spatially variable (ranging from 0.5 to 3 keV), on scales of tens of parsecs, likely due to the ionization state and orientation effects of the reprocessing material, with respect to the central X-ray illuminating source. A clump of highly ionized Fe xxv He-α is also detected, 40 parsecs east to the nucleus. When observations taken years apart are considered, the central unresolved reflected emission is found to remain constant.

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“…Ptak et al (2003) pointed out to the complexity of the nuclear spectrum of this galaxy and constructed a more complex model that, in addition to the standard MEKAL and power law components, also included a Gaussian fit for the FeKα and a Compton reflection component with different column densities. To give an idea of the complexity of the source, let us point out that Boller et al (2003) best-modelled the FeKα line as resolved into 3 narrow lines: a neutral FeKα line at 6.4 keV, an ionised line at 6.7 keV, and a blend of higher ionised lines (FeXXVI and Fe Kβ line) at 7.0 keV. For consistency with the statistical analysis, we modelled the continuum spectrum with the combination of a thermal plus a power law component, without taking the complexity of the FeKα line into account.…”

Section: Ngc 6251 (Ugc 10501)mentioning

confidence: 99%

An X-ray view of 82 LINERs with Chandra and XMM-Newton data

González‐Martín¹,

Masegosa

Márquez

et al. 2009

A&A

179

226

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We present the results of a homogeneous X-ray analysis for 82 nearby low-ionisation, narrow emission-line regions (LINERs) selected from the catalogue of Carrillo et al. (1999, Rev. Mex. Astron. Astrofis., 35, 187). All sources have available Chandra (68 sources) and/or XMM-Newton (55 sources) observations. This is the largest sample of LINERs with X-ray spectral data (60 out of the 82 objects), and it significantly improves our previous analysis based on Chandra data for 51 LINERs (Gonzalez-Martin et al. 2006b, A&A, 460, 45). It both increases the sample size and adds XMM-Newton data. New models permit the inclusion of double absorbers in the spectral fits. Nuclear X-ray morphology is inferred from the compactness of detected nuclear sources in the hard band (4.5-8.0 keV). Sixty per cent of the sample shows a compact nuclear source and are classified as active galactic nucleus (AGN) candidates. The spectral analysis indicates that best fits involve a composite model: 1) absorbed primary continuum and 2) soft spectrum below 2 keV described by an absorbed scatterer and/or a thermal component. The resulting median spectral parameters and their standard deviations are Γ = 2.11 ± 0.52, kT = 0.54 ± 0.30 keV, log(NH1) = 21.32 ± 0.71 and log(NH2) = 21.93 ± 1.36. We complement our X-ray results with an analysis of HST optical images and literature data on emission lines, radio compactness, and stellar population. After adding all these multiwavelength data, we conclude that evidence supports the AGN nature of their nuclear engine for 80% of the sample (66 out of 82 objects).

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XMM-Newtonobservation of the ULIRG NGC 6240

Cited by 36 publications

References 28 publications

Hard X-ray emission of the luminous infrared galaxy NGC 6240 as observed by NuSTAR

Hard X-ray emission of the luminous infrared galaxy NGC 6240 as observed by NuSTAR

Spatially resolved Fe K spectroscopy of NGC 4945

An X-ray view of 82 LINERs with Chandra and XMM-Newton data

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