A Long Look at NGC 3783 with the<i>XMM‐Newton</i>Reflection Grating Spectrometer

Behar, E.; Rasmussen, Andrew; Blustin, A. J.; Šako, M.; Kahn, S. M.; Kaastra, J. S.; Branduardi‐Raymont, G.; Steenbrugge, K. C.

doi:10.1086/378853

Cited by 137 publications

(186 citation statements)

References 35 publications

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“…The strongest line visible in a typical Seyfert 1 high-resolution X-ray spectrum is the O vii forbidden emission line, although other lines are also detected depending on the quality of the spectrum (among others Ne ix f and C v f). No significant blueshift is detected in the emission lines of NGC 5548 (Kaastra et al 2002), while NGC 3783 shows evidence of redshifted emission lines, which could be an indication of a P-Cygni like wind (Kaspi et al 2002;Behar et al 2003).…”

Section: Introductionmentioning

confidence: 85%

X-ray narrow line region variability as a geometry probe

Detmers¹,

Kaastra

McHardy

2009

A&A

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We study the long time scale variability of the gas responsible for the X-ray narrow emission lines in the Seyfert 1 galaxy NGC 5548, in order to constrain the location and geometry of the emitting gas. Using X-ray spectra taken with the Chandra−LETGS and HETGS instruments and with XMM−Newton RGS and combining them with long-term monitoring observations of the Rossi X-ray Timing Explorer (RXTE), we perform a correlation analysis in order to try to constrain the time scale on which the narrow line emitting gas responds to variations of the continuum flux. With the inclusion of the 2007 Chandra−LETGS observation we have an additional observation at an historically low flux level. We conclude that the NLR in NGC 5548 is in the form of an ionization cone, compact in size, and located between 1 and 15 pc from the central source, depending on the exact geometry of the NLR.

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Section: Introductionmentioning

confidence: 85%

X-ray narrow line region variability as a geometry probe

Detmers¹,

Kaastra

McHardy

2009

A&A

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“…Such SMW jets can inflate fat bubbles (Sternberg et al 2007), and through that transfer energy to the ICM (or ISM) and make the JFM efficient in galactic (e.g., Ciotti et al 2010;Choi et al 2015) and cluster (e.g., Gilkis & Soker 2012) scales. Wide-angle sub-relativistic outflows are revealed by X-ray observation as well (e.g., Behar et al 2003). Chartas et al (2016) for example, find the outflow from the AGN HS 0810+2554 to have a covering factor of > 0.6, and to carry about ten times more energy than that carried by radiation from the AGN.…”

Section: The Jetsmentioning

confidence: 98%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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“…Previous studies have found a WA in NGC 3783 (Kaspi et al 2002;Blustin et al 2002;Behar et al 2003;Scott et al 2014). We utilised all archival data from XMM- Newton (2000 and2001) and Chandra HETGS (2000, 2001, and 2013) to produce a set of time-averaged spectra.…”

Section: Modelling Of the Obscuring Wind In Ngc 3783mentioning

confidence: 99%

Chasing obscuration in type-I AGN: discovery of an eclipsing clumpy wind at the outer broad-line region of NGC 3783

Mehdipour

Kaastra

Kriss

et al. 2017

A&A

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In 2016 we carried out a Swift monitoring program to track the X-ray hardness variability of eight type-I AGN over a year. The purpose of this monitoring was to find intense obscuration events in AGN, and thereby study them by triggering joint XMM-Newton, NuSTAR, and HST observations. We successfully accomplished this for NGC 3783 in December 2016. We found heavy X-ray absorption produced by an obscuring outflow in this AGN. As a result of this obscuration, interesting absorption features appear in the UV and X-ray spectra, which are not present in the previous epochs. Namely, the obscuration produces broad and blue-shifted UV absorption lines of Lyα, C iv, and N v, together with a new high-ionisation component producing Fe xxv and Fe xxvi absorption lines. In soft X-rays, only narrow emission lines stand out above the diminished continuum as they are not absorbed by the obscurer. Our analysis shows that the obscurer partially covers the central source with a column density of few 10 23 cm −2 , outflowing with a velocity of few thousand km s −1 . The obscuration in NGC 3783 is variable and lasts for about a month. Unlike the commonly-seen warm-absorber winds at pc-scale distances from the black hole, the eclipsing wind in NGC 3783 is located at about 10 light days. Our results suggest the obscuration is produced by an inhomogeneous and clumpy medium, consistent with clouds in the base of a radiatively-driven disk wind at the outer broad-line region of the AGN.

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A Long Look at NGC 3783 with theXMM‐NewtonReflection Grating Spectrometer

Cited by 137 publications

References 35 publications

X-ray narrow line region variability as a geometry probe

X-ray narrow line region variability as a geometry probe

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Chasing obscuration in type-I AGN: discovery of an eclipsing clumpy wind at the outer broad-line region of NGC 3783

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