THE SOFT X-RAY AND NARROW-LINE EMISSION OF Mrk 573 ON KILOPARSEC SCALES

González‐Martín, O.; Acosta–Pulido, J. A.; Pérez-García, A. M.; Almeida, C. Ramos

doi:10.1088/0004-637x/723/2/1748

Cited by 23 publications

(32 citation statements)

References 64 publications

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“…It has been claimed that high-resolution X-ray spectra are dominated by emission lines from the NLR in type 2 Seyferts (Guainazzi & Bianchi 2007). Moreover, the soft X-ray emission in a few AGN is extended on scales ranging from a few hundred parsecs to a few thousand parsecs, in close agreement with the morphology of the NLR seen at optical wavelengths for both LINERs and type 2 Seyferts (González-Martín et al 2010;Bianchi et al 2006;Masegosa et al 2011). In this case, we would expect ν SB to increase when the luminosity increases for the objects in our sample.…”

Section: Optical Versus X-ray Classessupporting

confidence: 67%

Synapses of active galactic nuclei:

González‐Martín

Díaz-González²,

Acosta–Pulido

et al. 2014

A&A

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Context. Many classes of active galactic nuclei (AGN) have been defined entirely through optical wavelengths, while the X-ray spectra have been very useful to investigate their inner regions. However, optical and X-ray results show many discrepancies that have not been fully understood yet. Aims. The main purpose of the present paper is to study the synapses (i.e., connections) between X-ray and optical AGN classifications.Methods. For the first time, the newly implemented  task allowed us to analyse broad band X-ray spectra of a sample of emission-line nuclei without any prior spectral fitting. Our sample comprises 162 spectra observed with XMM-Newton/pn of 90 local emission line nuclei in the Palomar sample. It includes, from the optical point of view, starbursts (SB), transition objects (T2), low-ionisation nuclear emission line regions (L1.8 and L2), and Seyfert nuclei (S1, S1.8, and S2). We used artificial neural networks (ANNs) to study the connection between X-ray spectra and optical classes. Results. Among the training classes, the ANNs are 90% efficient at classifying the S1, S1.8, and SB classes. The S1 and S1.8 classes show a negligible SB-like component contribution with a wide range of contributions from S1-and S1.8-like components. We suggest that this broad range of values is related to the high degree of obscuration in the X-ray regime. When including all the objects in our sample, the S1, S1.8, S2, L1.8, L2/T2/SB-AGN (SB with indications of AGN activity in the literature), and SB classes have similar average X-ray spectra, but these average spectra can be distinguished from class to class. The S2 (L1.8) class is linked to the S1.8 (S1) class with a larger SB-like component than the S1.8 (S1) class. The L2, T2, and SB-AGN classes constitute a class in the X-rays similar to the S2 class, albeit with larger portions of SB-like component. We argue that this SB-like component might come from the contribution of the host galaxy emission to the X-rays, which is high when the AGN is weak. Up to 80% of the emission line nuclei and, on average, all the optical classes included in our sample show a significant fraction of S1-like or S1.8-like components. Thus, an AGN-like component seems to be present in the vast majority of the emission line nuclei in our sample. Conclusions. The ANN trained in this paper is not only useful for studying the synergies between the optical and X-ray classifications, but might also be used to infer optical properties from X-ray spectra in surveys like eRosita.

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Section: Optical Versus X-ray Classessupporting

confidence: 67%

Synapses of active galactic nuclei:

González‐Martín

Díaz-González²,

Acosta–Pulido

et al. 2014

A&A

Self Cite

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“…Interestingly, the range is well within the optical BLR of 3C445 with R = 1.2 × 10 16 cm (Osterbrock et al 1976), suggesting we might be viewing the inner part of the BLR. Indeed, the best-fit Hydrogen density is consistent with the typical value of the BLR in AGN (10 8 − 10 12 cm −3 ; Gonzalez-Martin et al 2010. Besides, as discussed in Section 3, the FWHM ratio of Si XIV and H β is consistent with 1 at the two-parameter 99% confidence level, which also supports that the soft X-ray emitting gas locates in the BLR.…”

Section: Resultssupporting

confidence: 82%

Analysis of the 3C 445 soft X-ray spectrum as observed by Chandra high-energy gratings

Dong

Shao

Cheng

et al. 2018

Res. Astron. Astrophys.

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We present a detailed analysis of the soft X-ray emission of 3C445 using an archival Chandra HETG spectrum. Highly-ionized H-and He-like Mg, Si and S lines, as well as a resolved low-ionized Si Kα line, are detected in the high resolution spectrum. The He-like triplets of Mg and Si are resolved into individual lines, and the calculated R ratios indicate a high density for the emitter. The low values of the G ratios indicate the lines originate from collisionally ionized plasmas. However, the detection of a resolved narrow Ne X RRC feature in the spectrum seems to prefer to a photoionized environment. The spectrum is subsequently modelled with a photoionization model, and the results are compared with that of a collisional model. Through a detailed analysis on the spectrum, we exclude a collisional origin for these emission lines. A one-component photoionization model provides a great fit to the emission features. The best-fit parameters are logξ = 3.3 +0.4 −0.3 erg cm s −1 , n H = 5 +15 −4.5 × 10 10 cm −3 and N H = 2.5 +3.8 −1.7 × 10 20 cm −2 . According to the calculated high density for the emitter, the measured velocity widths of the emission lines and the inferred the radial distance (6 × 10 14 -8 × 10 15 cm), we suggest the emission lines originating from matter locate in the broad line region (BLR). 3C445 is an ideal target for investigating the nature of the central engines of the radio-loud objects. High resolution observations have revealed a multitude of soft X-ray emission features from H-and He-like ions in this object. The XMM-Newton RGS spectra provided the first detection of the O VII and O VIII emission lines (Grandi et al. 2007). These lines are considered most likely from a warm photoionized gas. However, the relative low resolution and short exposure time restrict an accurate measurement of the line parameters. The subsequent Chandra LETG spectrum of 3C445 detected and resolved emission lines from H-and He-like O, Ne, Mg, and Si ions (Reeves et al. 2010). The spectrum gives the first detailed measurement of the soft X-ray emission of this object. Based on the emission features from O VII and O VIII, Reeves et al. (2010) inferred that the emission comes from photoionized gas which probably locates in the broad line region (BLR).The most recent Chandra HETG spectrum provides some distinct emission features in the soft Xray band from previous observations, e.g. resolved Mg XI and Si XIII triplets. These new characteristics may provide more accurate constraints on the physical states of the line emitting gas. As far as we know, no research on the soft X-ray emission has been published in the literature based on these data. Consequently, in this paper, we make a detailed research on the soft X-ray emission of 3C445 based on the spectrum observed by Chandra HETG. Our goal is to analyze the soft X-ray emission features in the spectrum and to make a detailed comparison with that obtained with the Chandra LETG spectrum (Reeves et al. 2010), in order to better understand the physical properties of the so...

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“…Bogdán et al (2017) analysed Chandra/HETG spectra of the Seyfert 2 galaxy Mrk 3 and derived some constraints on the emission-line gas. Although there have been efforts to model the X-ray NLR using Chandra imaging (e.g., Bianchi et al 2010;Gonzalez-Martin et al 2010;Maksym et al 2019), there have not been any other attempts to generate detailed physical models using HETG spectra.…”

Section: General Backgroundmentioning

confidence: 99%

Mass outflow of the X-ray emission line gas in NGC 4151

Kraemer

Turner

Couto

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We have analysed Chandra/High Energy Transmission Gratings spectra of the X-ray emission line gas in the Seyfert galaxy NGC 4151. The zeroth order spectral images show extended H-and He-like O and Ne, up to a distance r ∼ 200 pc from the nucleus. Using the 1st order spectra, we measure an average line velocity ∼ −230 km s −1 , suggesting significant outflow of X-ray gas. We generated Cloudy photoionisation models to fit the 1st order spectra; the fit required three distinct emission-line components. To estimate the total mass of ionised gas and the mass outflow rates, we applied the model parameters to fit the zeroth order emission-line profiles of Ne IX and Ne X. We determined the total mass of ≈ 5.4× 10 5 M . Assuming the same kinematic profile as that for the [O III] gas, derived from our analysis of Hubble Space Telescope/Space Telescope Imaging Spectrograph spectra, the peak X-ray mass outflow rate was ≈ 1.8 M yr −1 , at r ∼ 150 pc. The total mass and mass outflow rates are similar to those determined using [O III], implying that the X-ray gas is a major outflow component. However, unlike the optical outflows, the X-ray outflow rate does not drop off at r > 100 pc, which suggests that it may have a greater impact on the host galaxy.

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THE SOFT X-RAY AND NARROW-LINE EMISSION OF Mrk 573 ON KILOPARSEC SCALES

Cited by 23 publications

References 64 publications

Synapses of active galactic nuclei:

Synapses of active galactic nuclei:

Analysis of the 3C 445 soft X-ray spectrum as observed by Chandra high-energy gratings

Mass outflow of the X-ray emission line gas in NGC 4151

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