Molecular shocks and the massive outflow in NGC 3079

doi:10.1093/mnras/276.4.1197

Cited by 5 publications

(2 citation statements)

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“…Note however that 𝑊 1𝜎 of H𝛼 reaches up to ∼1000 km s −1 , considerably larger than the [C II] widths. The [C II] 158 widths are similar to the values derived by Hawarden et al (1995) from H 2 ro-vibrational transitions and mapped by Israel et al (1998).…”

Section: Wind Kinematics and Multiwavelength Comparisonsupporting

confidence: 86%

Exploring the Dust Content of Galactic Halos with Herschel. IV. NGC 3079

Veilleux,

Melendez,

Stone

et al. 2021

Preprint

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We present the results from an analysis of deep Herschel far-infrared observations of the edge-on disk galaxy NGC 3079. The PSF-cleaned PACS images at 100 and 160 𝜇m display a 25 × 25 kpc 2 X-shape structure centered on the nucleus that is similar in extent and orientation to that seen in H𝛼, X-rays, and the far-ultraviolet. One of the dusty filaments making up this structure is detected in the SPIRE 250 𝜇m map out to ∼ 25 kpc from the nucleus. The match between the far-infrared filaments and those detected at other wavelengths suggests that the dusty material has been lifted out of the disk by the same large-scale galactic wind that has produced the other structures in this object. A closer look at the central 10 × 10 kpc 2 region provides additional support for this scenario. The dust temperatures traced by the 100to-160 𝜇m flux ratios in this region are enhanced within a biconical region centered on the active galactic nucleus, aligned along the minor axis of the galaxy, and coincident with the well-known double-lobed cm-wave radio structure and H𝛼-X-ray nuclear superbubbles. PACS imaging spectroscopy of the inner 6-kpc region reveals broad [C II] 158 𝜇m emission line profiles and OH 79 𝜇m absorption features along the minor axis of the galaxy with widths well in excess of those expected from beam smearing of the disk rotational motion. This provides compelling evidence that the cool material traced by the [C II] and OH features directly interacts with the nuclear ionized and relativistic outflows traced by the H𝛼, X-ray, and radio emission.

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Section: Wind Kinematics and Multiwavelength Comparisonsupporting

confidence: 86%

Exploring the Dust Content of Galactic Halos with Herschel. IV. NGC 3079

Veilleux,

Melendez,

Stone

et al. 2021

Preprint

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“…Cecil et al (2001) does indeed harbour star forming molecular gas (Lawrence et al 1985), pointing to the possibility of a starburst driven wind (Veilleux et al 1994;Sofue & Vogler 2001;Shafi et al 2015). However, this is disputed in Hawarden et al (1995) who favour an AGN 10 driven wind.…”

Section: The Superbubble In Ngc 3079mentioning

confidence: 99%

Relativistic jet feedback – III. Feedback on gas discs

Mukherjee

Bicknell

Wagner

et al. 2018

Monthly Notices of the Royal Astronomical Society

200

238

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We study the interactions of a relativistic jet with a dense turbulent gaseous disk of radius ∼ 2 kpc. We have performed a suite of simulations with different mean density, jet power and orientation. Our results show that: A) the relativistic jet couples strongly with the gas in the inner kpc, creating a cavity and launching outflows. B) The high pressure bubble inflated by the jet and its back-flow compresses the disk at the outer edges, driving inflows within the disk. C) Jets inclined towards the disk affect the disk more and launch sub-relativistic, wide-angle outflows along the minor axis. D) Shocks driven directly by the jet and the jet-driven energy bubble raise the velocity dispersion throughout the disk by several times its initial value. E) Compression by the jet-driven shocks can enhance the star formation rate in the disk, especially in a ring-like geometry close to the axis. However, enhanced turbulent dispersion in the disk also leads to quenching of star formation. Whether positive or negative feedback dominates depends on jet power, ISM density, jet orientation with respect to the disc, and the time-scale under consideration. Qualitatively, our simulations compare favourably with kinematic and morphological signatures of several observed galaxies such as NGC 1052, NGC 3079, 3C 326 and 3C 293.

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Exploring the dust content of galactic haloes with Herschel – IV. NGC 3079

Veilleux

Meléndez

Stone

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the results from an analysis of deep Herschel far-infrared observations of the edge-on disk galaxy NGC 3079. The PSF-cleaned PACS images at 100 and 160 μm display a 25 × 25 kpc2 X-shape structure centered on the nucleus that is similar in extent and orientation to that seen in Hα, X-rays, and the far-ultraviolet. One of the dusty filaments making up this structure is detected in the SPIRE 250 μm map out to ∼ 25 kpc from the nucleus. The match between the far-infrared filaments and those detected at other wavelengths suggests that the dusty material has been lifted out of the disk by the same large-scale galactic wind that has produced the other structures in this object. A closer look at the central 10 × 10 kpc2 region provides additional support for this scenario. The dust temperatures traced by the 100-to-160 μm flux ratios in this region are enhanced within a biconical region centered on the active galactic nucleus, aligned along the minor axis of the galaxy, and coincident with the well-known double-lobed cm-wave radio structure and Hα-X-ray nuclear superbubbles. PACS imaging spectroscopy of the inner 6-kpc region reveals broad [C II] 158 μm emission line profiles and OH 79 μm absorption features along the minor axis of the galaxy with widths well in excess of those expected from beam smearing of the disk rotational motion. This provides compelling evidence that the cool material traced by the [C II] and OH features directly interacts with the nuclear ionized and relativistic outflows traced by the Hα, X-ray, and radio emission.

show abstract

Molecular shocks and the massive outflow in NGC 3079

Cited by 5 publications

References 0 publications

Exploring the Dust Content of Galactic Halos with Herschel. IV. NGC 3079

Exploring the Dust Content of Galactic Halos with Herschel. IV. NGC 3079

Relativistic jet feedback – III. Feedback on gas discs

Exploring the dust content of galactic haloes with Herschel – IV. NGC 3079

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