The peculiar small-scale X-ray morphology of NGC 5846 observed with $\vec{Chandra}$

Trinchieri, G.; Goudfrooij, Paul

doi:10.1051/0004-6361:20020311

Cited by 45 publications

(51 citation statements)

References 46 publications

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“…They detected, however, a large amount of individual, compact sources in the luminosity range from 3 to 20× 10 38 erg s −1 . Filho et al (2004) reanalysed the data already presented in Trinchieri & Goudfrooij (2002) and reported a weak, hard (2-10 keV) nuclear source with Γ = 2.29, which is compatible within the errors with the value we obtain from the spectral fitting. Satyapal et al (2005) analysed the Chandra data of this galaxy that they classed within Non-AGN LINERs, fitting its spectrum with a single thermal model with kT = 0.65 keV, exactly the same as in GM+06 for our single RS model.…”

Section: Ngc 5846 (Ugc 9706)supporting

confidence: 87%

“…F.12 the two galaxies closest to it are the two small ones to the W (NGC 5845, at cz = 1458 km s −1 ) and NGC 5839, at 1225 km s −1 ); the barred spiral to the E is NGC 5850, at 2556 km s −1 , and hence it does not conform a close interacting pair. Based on Chandra data, Trinchieri & Goudfrooij (2002) revealed a complex X-ray morphology with no clear nuclear identification (see also Fig. C.70).…”

Section: Ngc 5846 (Ugc 9706)mentioning

confidence: 99%

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

González‐Martín¹,

Masegosa

Márquez

et al. 2009

A&A

178

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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Section: Ngc 5846 (Ugc 9706)supporting

confidence: 87%

Section: Ngc 5846 (Ugc 9706)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

178

226

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“…The inner region of the galaxy contains dust and a radio core (Moellenhoff et al 1992). Ho et al (1997) classified this galaxy as an ambiguous case like transient 2.0 objects but the revision made by González-Martín et al (2009b) Filho et al (2004), Satyapal et al (2005), and Trinchieri & Goudfrooij (2002). Three different models were fitted (PL, APEC, and MEPL), and an order-of-magnitude difference in luminosity was found between Filho et al (2004) (log L(2−10 keV) = 38.4) and the other two works (39.4 and 39.6 + − 0.4, respectively), maybe entirely due to the different models used.…”

Section: Appendix A: Notes and Comparisons With Previous Results For mentioning

confidence: 99%

X-ray spectral variability of seven LINER nuclei withXMM-NewtonandChandradata

Hernández-García

González‐Martín

Márquez

et al. 2013

A&A

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Context. One of the most distinctive features in active galactic nuclei (AGN) is the variability of their emission. Variability has been discovered at X-ray, UV, and radio frequencies on timescales from hours to years. Among the AGN family and according to theoretical studies, low-ionization nuclear emission line region (LINER) nuclei would be objects variable on long timescales. Aims. Our purpose is to investigate spectral X-ray variability in LINERs and to understand the nature of these types of objects, as well as their accretion mechanism. Methods. Chandra and XMM-Newton public archives were used to compile X-ray spectra of seven LINER nuclei at different epochs with timescales of years. To search for variability we fit all spectra from the same object with a set of models to identify the parameters responsible for the variability pattern. We also analyzed the light curves to search for short timescale (from hours to days) variability. Whenever possible, UV variability was also studied. Results. We found spectral variability in four objects (NGC 1052, NGC 3226, NGC 4278, and NGC 4552), with variations mostly related to hard energies (2-10 keV). These variations are generated by several possible changes that act either alone or in combination: changes in the soft excess or in the absorber. Added to this can be intrinsic variations of the source, which may also be responsible by themselves for the spectral variability. These variations occurred within years, the shortest timescale being found for NGC 4278 (two months). Another two galaxies (NGC 4261 and NGC 5846) apparently do not vary. No short timescale variations during individual observations were found. Our analysis confirms the previously reported anticorrelation between the X-ray spectral index, Γ, and the Eddington ratio, L bol /L Edd , and also the correlation between the X-ray to UV flux ratio, α ox , and the Eddington ratio, L bol /L Edd . These results support an advection dominated accretion flow as the accretion mechanism in LINERs.

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“…In the central region of NGC 5846, a prominent dust shell has been found (Goudfrooij & Trinchieri 1998). In contrast to the X-ray faint galaxy NGC 4365, NGC 5846 shows a complex X-ray morphology, coupled with an equally peculiar energy distribution of the X-ray photons (Trinchieri & Goudfrooij 2002).…”

Section: Galaxies In (Sub-)groups: Ngc 4365 and Ngc 5846mentioning

confidence: 97%

The age structure of globular cluster systems in early-type galaxies and its dependence on host galaxy properties

Hempel

Kissler-Patig²,

Puzia³

et al. 2006

A&A

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Aims. We present the results of an optical -near-infrared photometric survey of globular cluster systems in early-type galaxies. Our project aims to study correlations between the age structure of the globular cluster systems and environmental as well as structural parameters of their host galaxies. Methods. To derive the age structure in globular cluster systems we use combined optical and near-infrared photometry. This combination facilitates the detection of young globular cluster sub-populations if their age differs significantly from the old (∼13 Gyr) population, i.e. if their age is < ∼ 7 Gyr. We investigate globular cluster systems in galaxies located in the central regions of galaxy clusters (NGC 1399, M 87, NGC 4478), galaxies which are members of (sub-) groups (NGC 4365, NGC 5846) and isolated galaxies (NGC 3115 and NGC 7192). Further, we look for correlations between globular cluster system properties and structural parameters of the galaxies (velocity dispersion σ, color ((V − K), (B − V)), and luminosity M V ). For a quantitative analysis we define the "Methuselah" parameter, Mth -based on the fraction of young and old metal-rich globular clusters weighted by age, characterizing the age structure of a globular cluster system. Results. We find that, within our galaxy sample, group galaxies appear to host an intermediate-age globular cluster population, whereas the globular cluster systems in cluster galaxies and in rather isolated galaxies are dominated by an old globular cluster population. A weak correlation of Mth with the H β index of the integrated light of the host galaxies is the only trend found with respect to internal galaxy parameters.

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The peculiar small-scale X-ray morphology of NGC 5846 observed with $\vec{Chandra}$

Cited by 45 publications

References 46 publications

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

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

X-ray spectral variability of seven LINER nuclei withXMM-NewtonandChandradata

The age structure of globular cluster systems in early-type galaxies and its dependence on host galaxy properties

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