The radio jet in M51

Crane, P.; Vanderhulst, Jm

doi:10.1086/116132

Cited by 43 publications

(67 citation statements)

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“…The Hubble classifications were taken either from the Third Reference Catalog of Bright Galaxies ( RC3; de Vaucouleurs et al 1991) or the NED and were coded according to the numerical scheme of the RC3. Of the sources that remained after filtering for the redshift and declination limits, we chose not to reobserve four well-studied galaxies: M51 ( Ford et al 1985;Crane & van der Hulst 1992), NGC 3079 (de Bruyn 1977; Duric et al 1983;Irwin & Saikia 2003), NGC 3516 ( Wrobel & Heeschen 1988;Baum et al 1993), and NGC 4151 ( Baum et al 1993;Pedlar et al 1993). These four sources were, however, included in the sample in the statistical analyses to follow (see x 4).…”

Section: Sample Selectionmentioning

confidence: 99%

A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

et al. 2006

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Seyfert galaxies commonly host compact jets spanning 10-100 pc scales, but larger structures are resolved out in long-baseline aperture synthesis surveys. Previous, targeted studies showed that kiloparsec-scale radio structures ( KSRs) may be a common feature of Seyfert and LINER galaxies, and the origin of KSRs may be starbursts or active galactic nuclei (AGNs). We report a new Very Large Array survey of a complete sample of Seyfert and LINER galaxies. Out of all of the surveyed radio-quiet sources, we find that 44% (19 out of 43) show extended radio structures at least 1 kpc in total extent that do not match the morphology of the disk or its associated star-forming regions. The detection rate is a lower limit owing to the combined effects of projection and resolution. The infrared colors of the KSR host galaxies are unremarkable compared to other Seyfert galaxies, and the large-scale outflows orient randomly with respect to the host galaxy axes. The KSR Seyfert galaxies instead stand out by deviating significantly from the far-infrared-radio correlation for star-forming galaxies, with tendency toward radio excess, and they are more likely to have a relatively luminous, compact radio source in the nucleus; these results argue that KSRs are powered by the AGNs rather than starbursts. The high detection rate indicates that Seyfert galaxies generate radio outflows over a significant fraction of their lifetime, which is much longer than the dynamical timescale of an AGNpowered jet but is comparable instead to the buoyancy timescale. The likely explanation is that the KSRs originate from jet plasma that has been decelerated by interaction with the nuclear interstellar medium ( ISM ). Based on a simple ram pressure argument, the kinetic power of the jet on kiloparsec scales is about 3 orders of magnitude weaker than the power of the jet on 10-100 pc scales. This result is consistent with the interaction model, in which case virtually all of the jet power must be lost to the ISM within the inner kiloparsec.

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Section: Sample Selectionmentioning

confidence: 99%

A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

et al. 2006

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“…The CO(1-0) emission peaks toward the centers of most spiral galaxies (Sakamoto et al 1999b), and the associated interstellar dust and its extinction often determine the emergent optical-UV spectrum of the AGN. In the optical, galactic nuclei are classified according to the width of Balmer lines, emission of high-ionization atoms, and the ratios of permitted to forbidden emission lines; in the radio continuum, the activity can manifest as central triple sources (Colbert et al 1996;Ho & Ulvestad 2001;Crane & van der Hulst 1992) or circumnuclear radio continuum structures (e.g., NGC 1326, García-Barreto et al 1991a;NGC 4314, García-Barreto et al 1991b).…”

Section: Introductionmentioning

confidence: 99%

CO in the Bipolar Radio Continuum Galaxy NGC 3367

et al. 2005

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CO(1-0) emission has been imaged at 2 00 resolution in the central 10 kpc of the barred spiral galaxy NGC 3367. This galaxy has bipolar synchrotron lobes out to a radius of 6 kpc, straddling the compact nucleus. The peak molecular emission is in a source of radius 2 00 (425 pc) centered on the galaxy nucleus. The molecular gas mass is $3 ; 10 8 M in this peak and $5:9 ; 10 8 M within a radius of 4B5 (950 pc). The very large gas masses in the central source imply extinctions sufficiently high to completely obscure optical emission lines (e.g., broad-line region) associated with the nuclear radio source. The observed Balmer lines probably originate in the narrow-line region a few hundred parsecs from the nucleus. The CO emission in the central region is elongated northeastsouthwest, very similar to the position angle of the large-scale synchrotron lobes. This elongation is likely due to the nonaxisymmetric gravitational potential of the stellar bar. We infer that the northeast radio continuum lobe is on the far side of the galaxy and the southwest lobe is on the near side. The central mass of molecular gas is of sufficient mass to power the active galactic nucleus accretion luminosity for over 10 8 yr at 3 M yr À1 .

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“…Because the PSF was stable during the night ( §2.1), we stacked standard star images for each filter to derive the PSF radial profile (top row of • ) are marked with green circles in both panels. A 6 cm VLA radio map of Crane & van der Hulst (1992) is overlaid with green contours in the right panel. b Number of standard star observations during the night.…”

Section: Psf Characterization and Radial Profile Analysis Of M51 Nucleusmentioning

confidence: 99%

Ground-based Mid-infrared Study of the Compton-thick AGN in M51 at 10–100 pc Scale*

Ohyama

Matsushita

et al. 2017

ApJ

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We performed near-diffraction-limited ( 0. 4 FWHM) N -band imaging of one of the nearest Active Galactic Nucleus (AGN) in M51 with 8.2m Subaru telescope to study the nuclear structure and spectral energy distribution (SED) at 8-13 µm. We found that the nucleus is composed of an unresolved core (at 13 pc resolution, or intrinsic size corrected for the instrumental effect of < 6 pc) and an extended halo (at a few tens pc scale), and each of their SEDs is almost flat. We examined the SED by comparing with the archival Spitzer IRS spectrum processed to mimic our chopping observation of the nucleus, and the published radiative-transfer model SEDs of the AGN clumpy dusty torus. The halo SED is likely due to circumnuclear star formation showing little Polycyclic Aromatic Hydrocarbon (PAH) emission due to the AGN. The core SED is likely dominated by the AGN because of the following two reasons. Firstly, the clumpy torus model SEDs can reproduce the red mid-infrared continuum with apparently moderate silicate 9.7 µm absorption. Secondly, the core 12 µm luminosity and the absorption-corrected X-ray luminosity at 2-10 keV in the literature follow the mid-infrared-X-ray luminosity correlation known for the nearby AGNs including the Compton-thick ones.

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The radio jet in M51

Cited by 43 publications

References 0 publications

A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

CO in the Bipolar Radio Continuum Galaxy NGC 3367

Ground-based Mid-infrared Study of the Compton-thick AGN in M51 at 10–100 pc Scale*

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