Multi-wavelength campaign on NGC 7469

Peretz, U.; Behar, E.; Kriss, G. A.; Kaastra, J. S.; Arav, Nahum; Bianchi, S.; Branduardi‐Raymont, G.; Cappi, M.; Costantini, E.; Marco, Barbara De; Gesu, Laura Di; Ebrero, J.; Kaspi, S.; Mehdipour, M.; Middei, R.; Paltani, S.; Petrucci, P.-O.; Ponti, G.; Ursini, F.

doi:10.1051/0004-6361/201731655

Cited by 15 publications

(31 citation statements)

References 30 publications

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“…We then included all the emission and absorption features (e.g due to the warm absorbers) derived from the analysis of the XMM-Newton RGS spectra of our campaign by Behar et al (2017). Since none of these components display significant variability during our campaign (Behar et al 2017;Peretz et al 2018), we keep all their parameters fixed in our following fits to the values found from the RGS data (see Behar et al 2017, for a detailed description of all the components). Some line-like features still remained in the pn spectra, and even if very weak, they result significant in terms of χ 2 , as a consequence of the high number of counts in the soft band.…”

Section: Spectral Analysis: 05-80 Kev Bandmentioning

confidence: 99%

“…NGC 7469 was studied also more recently: Petrucci et al (2004) investigated the UV/X-ray variability, Scott et al (2005) analysed its simultaneous X-ray, far-ultraviolet, and near-ultraviolet spectra using Chandra, FUSE and STIS, while Patrick et al (2011) studied this source taking advantage of Suzaku observations. Previous XMM-Newton data were analysed in Blustin et al (2003) and De Marco et al (2009), while some results from the 2015 observational campaign have been presented in Behar et al (2017); Peretz et al (2018).…”

Section: Introductionmentioning

confidence: 99%

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Multi-wavelength campaign on NCG 7469

Middei

Bianchi

Cappi

et al. 2018

A&A

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We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe Kα emission line in all the spectra and weaker contributions from Fe Kβ, neutral Ni Kα, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (Γ = 1.78 ± 0.02) together with a high energy cut-off Ecut = 170−40+60 keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45−12+15 keV and, assuming a spherical geometry, an optical depth τ = 2.6 ± 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3−0.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 ± 0.03 keV and a corresponding optical depth τ = 9.2 ± 0.2.

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Section: Spectral Analysis: 05-80 Kev Bandmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Multi-wavelength campaign on NCG 7469

Middei

Bianchi

Cappi

et al. 2018

A&A

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“…In addition to spectral lines from the AGN wind, Fe XVII emission lines from a collisionally ionised component were also found, which is likely associated with the starburst activity of NGC 7469. Furthermore, variability in the ionic column density of the warm absorber between the individual 2015 RGS spectra are investigated in Peretz et al (2018), where lines from individual ions are independently measured. No significant changes in the ionic column densities were found among the 2015 observations.…”

Section: Introductionmentioning

confidence: 99%

Multi-wavelength campaign on NGC 7469

Behar

Peretz

Kriss

et al. 2018

A&A

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We investigate the physical structure of the active galactic nucleus (AGN) wind in the Seyfert-1 galaxy NGC 7469 through high-resolution X-ray spectroscopy with Chandra HETGS and photoionisation modelling. Contemporaneous data from Chandra, HST, and Swift are used to model the optical-UV-X-ray continuum and determine the spectral energy distribution (SED) at two epochs, 13 yr apart. For our investigation we use new observations taken in December 2015–January 2016, and historical ones taken in December 2002. We study the impact of a change in the SED shape, seen between the two epochs, on the photoionisation of the wind. The HETGS spectroscopy shows that the AGN wind in NGC 7469 consists of four ionisation components, with their outflow velocities ranging from − 400 to − 1800 km s-1. From our modelling we find that the change in the ionising continuum shape between the two epochs results in some variation in the ionisation state of the wind components. However, for the main ions detected in X-rays, the sum of their column densities over all components remains in practice unchanged. For two of the four components, which are found to be thermally unstable in both epochs, we obtain 2 < r < 31 pc and 12 < r < 29 pc using the cooling and recombination timescales. For the other two thermally stable components, we obtain r < 31 pc and r < 80 pc from the recombination timescale. The results of our photoionisation modelling and thermal stability analysis suggest that the absorber components in NGC 7469 are consistent with being a thermally driven wind from the AGN torus. Finally, from analysis of the zeroth-order ACIS/HETG data, we discover that the X-ray emission in the range 0.2–1 keV is spatially extended over 1.5–12′′. This diffuse soft X-ray emission is explained by coronal emission from the nuclear starburst ring in NGC 7469. The star formation rate inferred from this diffuse soft X-ray emission is consistent with those found by far-infrared studies of NGC 7469.

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“…atomic and mildly ionized species (up to +3) we use the ISMAbs model (Gatuzz et al 2014). The ionized component, is modeled using our ion-by-ion fitting model -Ibifit (Peretz et al 2017). The model fits the column density of all the astrophysical abundant ions, taking into account the transitions, oscillator strengths and photoelectric edges, which were computed using the HULLAC code (Bar-Shalom et al 2001).…”

Section: Ion-by-ion Fittingmentioning

confidence: 99%

“…We assume a discrete step-function AM D of a few temperature bins, and solve simultaneously for all ions to obtain AM D(T). The general process for solving the equations is described in Peretz et al (2017). The AM D was calculated here using the ion detections from Table 1 and not upper limits, except for O +5 that we used from the UV detection (Sembach et al 2001).…”

Section: Column Densitiesmentioning

confidence: 99%

The ionic composition of the local absorber towards 3C 273

Gissis

Peretz

Behar

2020

Monthly Notices of the Royal Astronomical Society

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Hot ionized gas is observed in the local vicinity of our galaxy through spectral absorption features. The most common hypothesis is that this gas forms a halo surrounding our Milky-Way (MW), in collisional ionization equilibrium. In this paper we investigate the elemental abundance of this hot and ionized local gas. We use a 2.4 Ms stacked X-ray spectrum of the bright blazar 3C 273 and probe the local absorption features. Using ion-by-ion fitting of the X-ray absorption lines we derive the column density of each ionization species. Based on the column densities we reconstruct the Absorption measure distribution (AMD), namely the hydrogenic column density as a function of temperature. We report the elemental abundances of C, N, Ne, and Fe relative to solar O. Previous measurements of local X-ray emission lines in conjunction with the present column densities indicate a scale height of 1 − 80 kpc and hydrogen number density of 10 −4 − 10 −3 cm -3 for the hot ionized gas. Additionally, we detect He-like O lines from the quasar broad line region with velocities of 6400±1500 km s −1 .

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Multi-wavelength campaign on NGC 7469

Cited by 15 publications

References 30 publications

Multi-wavelength campaign on NCG 7469

Multi-wavelength campaign on NCG 7469

Multi-wavelength campaign on NGC 7469

The ionic composition of the local absorber towards 3C 273

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