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

AbstractWe have analyzed Chandra/High Energy Transmission Grating 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 photoionization models to fit the 1st-order spectra; the fit required three distinct emission-line components. To estimate the total mass of ionized gas (M) 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 an M ≍ 5.4 × 105Mʘ. 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 is approximately 1.8 Mʘ 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 emitting mass outflow rate does not drop off at r > 100pc, which suggests that it may have a greater impact on the host galaxy.

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

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa428 ◽

2020 ◽

Vol 493 (3) ◽

pp. 3893-3910

Author(s):

S B Kraemer ◽

T J Turner ◽

J D Couto ◽

D M Crenshaw ◽

H R Schmitt ◽

...

Keyword(s):

Emission Line ◽

Total Mass ◽

High Energy ◽

Zeroth Order ◽

Space Telescope ◽

X Ray ◽

First Order ◽

Ngc 4151 ◽

Outflow Rate ◽

Mass Outflow

ABSTRACT 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 first-order spectra, we measure an average line velocity ∼−230 km s−1, suggesting significant outflow of X-ray gas. We generated cloudy photoionization models to fit the first-order spectra; the fit required three distinct emission line components. To estimate the total mass of ionized 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 × 105 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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X-Ray Properties of Galactic Nuclei

Highlights of Astronomy ◽

10.1017/s1539299600004512 ◽

1980 ◽

Vol 5 ◽

pp. 623-630

Author(s):

Daniel W. Weedman

Keyword(s):

Emission Line ◽

Active Galactic Nuclei ◽

Galactic Nuclei ◽

Seyfert Galaxy ◽

Seyfert Galaxies ◽

Strong Emission ◽

X Ray ◽

Ngc 4151 ◽

Survey Results ◽

Emission Line Galaxies

Preparing this review was my just punishment for stating only two years ago - in another review (Weedman 1977) - that Seyfert galaxies are not strong X-ray sources. I said that because, as recently as three years ago, NGC 4151 was the only Seyfert galaxy known as an X-ray source. Now we have 36 Seyfert 1 galaxies, along with 12 other galaxies with strong emission-line nuclei, that are X-ray sources. And this is all without even having HEAO-2 data at our disposal yet. The study of active galactic nuclei with X-ray astronomy is progressing so rapidly that a reviewer feels almost hopeless. The best I can do is summarize what is known as of the summer of 1979 and give a simple overview of how X-ray and other properties relate.Some excellent reviews of the X-ray properties of Seyfert and other emission-line galaxies already exist. I especially recommend that by Andrew Wilson (1979). He provides very complete references as of a year ago, but X-ray astronomy is progressing so rapidly that he then had only somewhat more than half the active nuclei now in Tables 1 and 2. It was the group working with the Ariel V SSI that made the initial comprehensive X-ray studies of Seyfert galaxies (Ward et al. 1977, Elvis et al. 1978). The UHURU results for Seyfert galaxies followed soon after and are summarized by Tananbaum et al. (1978); the HEAO-A-2 survey results are now in press (Marshall et al. 1979) I have tried to incorporate these and other recent results in Tables 1 and 2.

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Exploring the Inner Narrow-Line Regions of Seyfert Galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s174392131000685x ◽

2009 ◽

Vol 5 (S267) ◽

pp. 401-401

Author(s):

S. B. Kraemer ◽

D. M. Crenshaw ◽

M. L. Trippe ◽

H. R. Schmitt ◽

M. Meléndez

Keyword(s):

Emission Line ◽

Seyfert Galaxies ◽

Uv Spectra ◽

Narrow Line ◽

Ngc 4151 ◽

Radial Extent ◽

Wide Range ◽

Heterogeneous Nature ◽

Mass Outflow ◽

Ngc 1068

In HST/STIS optical spectra of Seyfert galaxies, there is often a bright knot of [O iii] emission in the inner NLR. In the case of the Seyfert 1 galaxy NGC 4151, we have shown that the emission-line gas may be associated with the mass outflow detected in absorption in UV spectra, which suggests that we are probing regions close to the AGN. Here we present results for the luminous Seyfert 2 galaxy Mrk 573. The spectra reveal the presence of lines from a wide range of ionization states (see Figure 1), which is indicative of the heterogeneous nature of the emission-line gas. As in our studies of other Seyfert galaxies, including NGC 1068, NGC 4151, and Mrk 3, there is evidence for emission from low-ionization gas outside the nominal emission-line bicone. Finally, based on photoionization modeling, we find that the central emission-line knot in Mrk 573 is some tens of parsecs from the AGN, similar to other Seyfert 2 galaxies, which suggests that the material that is obscuring the central AGN in Seyfert 2s must have a similar radial extent.

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The Complex Structure of the CIV Emission Line in the Seyfert 1 Galaxy NGC 4151 at Minimum States

Symposium - International Astronomical Union ◽

10.1017/s0074180900140574 ◽

1989 ◽

Vol 134 ◽

pp. 120-121

Author(s):

M.-H. Ulrich

Keyword(s):

Emission Line ◽

Complex Structure ◽

Absorption Lines ◽

Short Article ◽

X Ray ◽

Ngc 4151

NGC 4151 passes rather frequently through states of deep minima characterized by a weak UV continuum and a nearly complete fading of the broad components of CIV and other permitted lines. The phenomenon described in this short article is best observed during these minima [7]. Other properties of the UV and X-ray continuum and of the emission and absorption lines of NGC 4151 have been presented and discussed elsewhere [1–6].

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HST observations of [O III] emission in nearby QSO2s: Physical properties of the outflows

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320004196 ◽

2020 ◽

Vol 15 (S359) ◽

pp. 269-271

Author(s):

Anna Trindade Falcao ◽

S. B. Kraemer ◽

T. C. Fischer ◽

D. M. Crenshaw ◽

M. Revalski ◽

...

Keyword(s):

Physical Properties ◽

Emission Line ◽

Radial Distance ◽

Space Telescope ◽

X Ray ◽

Medium Resolution ◽

Mass Outflow ◽

Imaging Spectrograph

AbstractWe used Space Telescope Imaging Spectrograph (STIS) long slit medium-resolution G430M and G750M spectra to analyze the extended [O III] λ5007 emission in a sample of twelve QSO2s from Reyes et al. (2008). The purpose of the study was to determine the properties of the mass outflows and their role in AGN feedback. We measured fluxes and velocities as functions of deprojected radial distances. Using photoionization models and ionizing luminosities derived from [O III], we were able to estimate the densities for the emission-line gas. From these results, we derived masses, mass outflow rates, kinetic energies and kinetic luminosity rates as a function of radial distance for each of the targets. Masses are several times 103 - 107 solar masses, which are comparable to values determined from a recent photoionization study of Mrk 34 (Revalski). Additionally, we are studying the possible role of X-ray winds in these QSO2s.

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White-Light Coronal Structures: Streamers and CMEs

International Astronomical Union Colloquium ◽

10.1017/s0252921100025045 ◽

1994 ◽

Vol 144 ◽

pp. 82

Author(s):

E. Hildner

Keyword(s):

Emission Line ◽

Electron Density ◽

White Light ◽

Coronal Mass Ejections ◽

X Rays ◽

Solar Cycles ◽

Temperature Function ◽

X Ray ◽

Eclipse Observations ◽

Coronal Structures

AbstractOver the last twenty years, orbiting coronagraphs have vastly increased the amount of observational material for the whitelight corona. Spanning almost two solar cycles, and augmented by ground-based K-coronameter, emission-line, and eclipse observations, these data allow us to assess,inter alia: the typical and atypical behavior of the corona; how the corona evolves on time scales from minutes to a decade; and (in some respects) the relation between photospheric, coronal, and interplanetary features. This talk will review recent results on these three topics. A remark or two will attempt to relate the whitelight corona between 1.5 and 6 R⊙to the corona seen at lower altitudes in soft X-rays (e.g., with Yohkoh). The whitelight emission depends only on integrated electron density independent of temperature, whereas the soft X-ray emission depends upon the integral of electron density squared times a temperature function. The properties of coronal mass ejections (CMEs) will be reviewed briefly and their relationships to other solar and interplanetary phenomena will be noted.

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The May 1985 Superoutburst of OY Carinae: II. Phase-Resolved IUE Spectroscopy and Exosat Observations

International Astronomical Union Colloquium ◽

10.1017/s025292110010510x ◽

1987 ◽

Vol 93 ◽

pp. 371-376 ◽

Cited By ~ 2

Author(s):

B.J.M. Hassall ◽

T. Naylor ◽

G.T. Bath ◽

P.A. Charles ◽

G. Sonneborn ◽

...

Keyword(s):

Emission Line ◽

Line Spectrum ◽

X Ray ◽

Dwarf Nova ◽

Uv Emission ◽

Emission Line Spectrum ◽

Coronal Region

AbstractWe present ultraviolet and X-ray observations of the eclipsing SU UMa dwarf nova OY Car early in the decline from a superoutburst. From the UV emission line spectrum and lack of X-ray eclipse, we deduce the presence of an extended coronal region.

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X-Ray Structure between the Innermost Disk and Optical Broad-line Region in NGC 4151

The Astrophysical Journal ◽

10.3847/1538-4357/aadbaa ◽

2018 ◽

Vol 865 (2) ◽

pp. 97 ◽

Cited By ~ 7

Author(s):

J. M. Miller ◽

E. Cackett ◽

A. Zoghbi ◽

D. Barret ◽

E. Behar ◽

...

Keyword(s):

Broad Line ◽

X Ray ◽

Ngc 4151 ◽

Broad Line Region ◽

Line Region

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Limits on mass outflow from optical tidal disruption events

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab240 ◽

2021 ◽

Vol 502 (3) ◽

pp. 3385-3393

Author(s):

Tatsuya Matsumoto ◽

Tsvi Piran

Keyword(s):

Energy Band ◽

New Method ◽

Hydrodynamic Modelling ◽

X Rays ◽

Will Emit ◽

Tidal Disruption ◽

X Ray ◽

Mass Outflow ◽

Current Sample ◽

Stellar Masses

ABSTRACT The discovery of optical/UV (ultraviolet) tidal disruption events (TDEs) was surprising. The expectation was that, upon returning to the pericentre, the stellar-debris stream will form a compact disc that will emit soft X-rays. Indeed, the first TDEs were discovered in this energy band. A common explanation for the optical/UV events is that surrounding optically thick matter reprocesses the disc’s X-ray emission and emits it from a large photosphere. If accretion follows the super-Eddington mass infall rate, it would inevitably result in an energetic outflow, providing naturally the reprocessing matter. We describe here a new method to estimate, using the observed luminosity and temperature, the mass and energy of outflows from optical transients. When applying this method to a sample of supernovae, our estimates are consistent with a more detailed hydrodynamic modelling. For the current sample of a few dozen optical TDEs, the observed luminosity and temperature imply outflows that are significantly more massive than typical stellar masses, posing a problem to this common reprocessing picture.

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