Mass Outflow in the Seyfert 1 Galaxy NGC 5548

Crenshaw, D. Michael; Kraemer, S. B.; Schmitt, H. R.; Kaastra, J. S.; Arav, Nahum; Gabel, J. R.; Korista, K. T.

doi:10.1088/0004-637x/698/1/281

Cited by 50 publications

(57 citation statements)

References 47 publications

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“…Note, that the gas emission also does not display any jump for high density case. The strong ILR emission found by (Mason, Puchnarewicz & Jones 1996;Crenshaw & Kraemer 2007;Crenshaw et al 2009), can be produced if the clouds are two orders of magnitude denser than those considered by NL93. Our results corroborate with the speculation made by Landt et al (2014), where they discuss the possible role of high density gas for the production of smooth BLR.…”

Section: Role Of the Gas Densitymentioning

confidence: 77%

The Intermediate-Line Region in Active Galactic Nuclei

Adhikari

Różáńska

Czerny

et al. 2016

ApJ

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We show that the recently observed suppression of the gap between the broad line region (BLR) and the narrow line region (NLR) in some AGN can be fully explained by an increase of the gas density in the emitting region. Our model predicts the formation of the intermediate line region (ILR) that is observed in some Seyfert galaxies by the detection of emission lines with intermediate velocity full width half maximum (FWHM) ∼ 700 -1200 km s −1 . These lines are believed to be originating from an ILR located somewhere between the BLR and NLR. As it was previously proved, the apparent gap is assumed to be caused by the presence of dust beyond the sublimation radius. Our computations with the use of cloudy photoionization code, show that the differences in the shape of spectral energy distribution (SED) from the central region of AGN, do not diminish the apparent gap in the line emission in those objects. A strong discontinuity in the line emission vs radius exists for all lines at the dust sublimation radius. However, increasing the gas density to ∼ 10 11.5 cm −3 at the sublimation radius provides the continuous line emission vs radius and fully explains the recently observed lack of apparent gap in some AGN. We show that such a high density is consistent with the density of upper layers of an accretion disk atmosphere. Therefore, the upper layers of the disk atmosphere can give rise to the formation of observed emission line clouds.

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Section: Role Of the Gas Densitymentioning

confidence: 77%

The Intermediate-Line Region in Active Galactic Nuclei

Adhikari

Różáńska

Czerny

et al. 2016

ApJ

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“…Fathi et al 2006;Storchi-Bergmann et al 2007;Davies et al 2009;Müller Sánchez et al 2009;Schnorr Müller et al 2011) and feedbackvia the interaction of the AGN radiation and mass outflow with the circumnuclear gas, affecting its kinematics and excitation (e.g. Wilson et al 1993;Schmitt & Kinney 1996;Veilleux, Goodrich & Wilson 1997;Ferruit, Wilson & Mulchaey 2000;Veilleux, Cecil & Bland-Hawthorn 2005;Holt et al 2006;Crenshaw & Kraemer E-mail: juniorfisicoo@gmail.com 2007; Crenshaw et al 2009Crenshaw et al , 2010aFischer et al 2010Fischer et al , 2011Müller-Sánchez et al 2011). …”

Section: Introductionmentioning

confidence: 99%

Feeding versus feedback in AGN from near-infrared IFU observations: the case of Mrk 766

Schönell¹,

Riffel²,

Storchi‐Bergmann³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We have mapped the emission-line flux distributions and ratios as well as the gaseous kinematics of the inner 450 pc radius of the type 1 Seyfert galaxy Mrk 766 using integral field near-infrared J-and K l -band spectra obtained with the Gemini Near Infrared Integral Field Spectrograph at a spatial resolution of 60 pc and velocity resolution of 40 km s −1 . Emission-line flux distributions in ionized and molecular gas extend up to ≈ 300 pc from the nucleus. Coronal [S IX] λ1.2523 µm line emission is resolved, being extended up to 150 pc from the nucleus. At the highest flux levels, the [Fe II] λ1.257 µm line emission is most extended to the south-east, where a radio jet has been observed. The emission-line ratios [Fe II] λ1.2570 µm/Paβ and H 2 λ2.1218 µm/Brγ show a mixture of Starburst and Seyfert excitation; the Seyfert excitation dominates at the nucleus, to the north-west and in an arc-shaped region between 0.2 and 0.6 arcsec to the south-east at the location of the radio jet. A contribution from shocks at this location is supported by enhanced [Fe II]/[P II] line ratios and increased [Fe II] velocity dispersion. The gas velocity field is dominated by rotation that is more compact for H 2 than for Paβ, indicating that the molecular gas has a colder kinematics and is located in the galaxy plane. There is about 10 3 M of hot H 2 , implying ≈10 9 M of cold molecular gas. At the location of the radio jet, we observe an increase in the [Fe II] velocity dispersion (150 km s −1 ), as well as both blueshift and redshifts in the channel maps, supporting the presence of an outflow there. The ionized gas mass outflow rate is estimated to be ≈10 M yr −1 , and the power of the outflow ≈0.08 L bol .

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“…However, as suggested by L2011, most of the mass loss is from the highionization/high-velocity component and components L3a and L4. Greater mass loss in more highly ionized gas than in the UV absorbers has been claimed for other AGN (e.g., NGC 5548; Crenshaw et al 2009). This is suggestive of a scenario in which the UV absorbers are knots or condensations in a more highly ionized wind, with the bulk of the mass contained in the latter.…”

Section: Radial Distances and Density Constraintsmentioning

confidence: 78%

“…Allowing the doublet ratios (e.g., N v λ1238.8/λ1242.8) to vary between 1 and 2 (see Crenshaw et al 2009) made little difference to the overall fits, so we fixed them to a value of 1. We adopted the minimum narrow-line fluxes needed to fit the observed profiles.…”

Section: Observational Resultsmentioning

confidence: 99%

“…Their non-zero fluxes in the COS spectra must be due to uncovered emission. To model the uncovered emission, we use our derived values for the instrumentally scattered light and the excess emission from the host galaxy, plus contributions from the NLR fluxes derived above, as we have done in the past (Kraemer et al 2002;Crenshaw et al 2009). Thus, a reasonable model for the uncovered emission is a combination of the excess continuum flux at a level of 1.2 ×10 −15 erg s −1 cm −2 Å −1 (half due to instrumental light, half to extra UV flux in the COS aperture) plus the NLR emission.…”

Section: Observational Resultsmentioning

confidence: 99%

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Observations of Outflowing Ultraviolet Absorbers in NGC 4051 With the Cosmic Origins Spectrograph

Kraemer¹,

Crenshaw²,

Dunn³

et al. 2012

ApJ

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We present new Hubble Space Telescope (HST)/Cosmic Origins Spectrograph (COS) observations of the narrowline Seyfert 1 galaxy NGC 4051. These data were obtained as part of a coordinated observing program including X-ray observations with the Chandra/High Energy Transmission Grating (HETG) spectrometer and Suzaku. We detected nine kinematic components of UV absorption, which were previously identified using the HST/Space Telescope Imaging Spectrograph (STIS). None of the absorption components showed evidence for changes in column density or profile within the ∼10 yr between the STIS and COS observations, which we interpret as evidence of (1) saturation, for the stronger components, or (2) very low densities, i.e., n H < 1 cm −3 , for the weaker components. After applying a + 200 km s −1 offset to the HETG spectrum, we found that the radial velocities of the UV absorbers lay within the O vii profile. Based on photoionization models, we suggest that, while UV components 2, 5, and 7 produce significant O vii absorption, the bulk of the X-ray absorption detected in the HETG analysis occurs in more highly ionized gas. Moreover, the mass-loss rate is dominated by high-ionization gas which lacks a significant UV footprint.

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Mass Outflow in the Seyfert 1 Galaxy NGC 5548

Cited by 50 publications

References 47 publications

The Intermediate-Line Region in Active Galactic Nuclei

The Intermediate-Line Region in Active Galactic Nuclei

Feeding versus feedback in AGN from near-infrared IFU observations: the case of Mrk 766

Observations of Outflowing Ultraviolet Absorbers in NGC 4051 With the Cosmic Origins Spectrograph

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