<i>SPITZER</i>MID-INFRARED SPECTROSCOPY OF COMPACT SYMMETRIC OBJECTS: WHAT POWERS RADIO-LOUD ACTIVE GALACTIC NUCLEI?

Willett, Kyle; Stocke, John T.; Darling, Jeremy; Perlman, Eric S.

doi:10.1088/0004-637x/713/2/1393

Cited by 53 publications

(107 citation statements)

References 132 publications

(221 reference statements)

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“…The narrowband 24 μm luminosities (see Section 3.2 and Table 1), measured on the LH spectra, span three orders of magnitude, from 5.4 × 10 9 L (3C 305) to ULIRG-like luminosities of 1.1 × 10 12 L (4C 12.50). For 4C 12.50 and OQ 208, our measurements are in agreement with those of Willett et al (2010) on low-resolution IRS data.…”

Section: Thermal Dust Continuum and Aromatic Features (Pahs)supporting

confidence: 87%

“…The locations of PAH features and emission lines are marked for each object. The low-resolution spectra for 3C 293, OQ 208, and PKS 1549-79 were already presented by Ogle et al (2010) and Willett et al (2010). arises from a distribution of densities and shock velocities. With the present data we cannot exclude the presence of very high density gas (n H > 10 5 cm −3 ).…”

Section: Molecular Hydrogenmentioning

confidence: 78%

“…Although PAH emission is expected to be diminished because of PAH destruction by hard UV or X-ray radiation close to the AGN (Voit 1992) or because of gas suppression close to the nuclei, it is unlikely that their abundances are reduced significantly at galactic scales by AGN effects (Ogle et al 2010). Silicate absorption at 9.7 and 18 μm is present in the lowresolution spectra of OQ 208 and 4C 12.50 (Willett et al 2010), as well as PKS 1549-79. OQ 208 is the only galaxy showing silicate emission (Willett et al 2010).…”

Section: Thermal Dust Continuum and Aromatic Features (Pahs)mentioning

confidence: 95%

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Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

Guillard

Ogle

Emonts

et al. 2012

ApJ

115

157

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Observations of ionized and neutral gas outflows in radio galaxies (RGs) suggest that active galactic nucleus (AGN) radio jet feedback has a galaxy-scale impact on the host interstellar medium, but it is still unclear how the molecular gas is affected. Thus, it is crucial to determine the physical conditions of the molecular gas in powerful RGs to understand how radio sources may regulate the star formation in their host galaxies. We present deep Spitzer Infrared Spectrograph (IRS) high-resolution spectroscopy of eight nearby RGs that show fast H i outflows. Strikingly, all of these H i-outflow RGs have bright H 2 mid-IR lines that cannot be accounted for by UV or X-ray heating. This strongly suggests that the radio jet, which drives the H i outflow, is also responsible for the shock excitation of the warm H 2 gas. In addition, the warm H 2 gas does not share the kinematics of the ionized/neutral gas. 4C 12.50, 3C 459, and PKS 1549-79. This shows that, contrary to the H i gas, the H 2 gas is inefficiently coupled to the AGN jet-driven outflow of ionized gas. While the dissipation of a small fraction (<10%) of the jet kinetic power can explain the turbulent heating of the molecular gas, our data show that the bulk of the warm molecular gas is not expelled from these galaxies.

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Section: Thermal Dust Continuum and Aromatic Features (Pahs)supporting

confidence: 87%

Section: Molecular Hydrogenmentioning

confidence: 78%

Section: Thermal Dust Continuum and Aromatic Features (Pahs)mentioning

confidence: 95%

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Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

Guillard

Ogle

Emonts

et al. 2012

ApJ

115

157

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“…Moreover, the maximum distance from the AGN where the in-falling gas could be located is 75 pc. This is less than twice the radius within which the SMBH dominates the kinematics of the galaxy (r ∼ 45 pc, assuming that the velocity dispersion of the stars is ∼ 200 km s −1 and M SMBH ∼ 4 × 10 8 M , Willett et al 2010). This is also in good agreement with the predictions of chaotic cold accretion models (e.g.…”

Section: Accretion Of Molecular Gas In Radio Agnmentioning

confidence: 95%

ALMA observations of AGN fuelling

Maccagni

Morganti

Oosterloo

et al. 2018

A&A

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We present ALMA observations of the 12 CO (2-1) line of the newly born (t radio ∼ 10 2 years) active galactic nucleus (AGN), PKS B1718-649. These observations reveal that the carbon monoxide in the innermost 15 kpc of the galaxy is distributed in a complex warped disk. In the outer parts of this disk, the CO gas follows the rotation of the dust lane and of the stellar body of the galaxy hosting the radio source. In the innermost kiloparsec, the gas abruptly changes orientation and forms a circumnuclear disk (r 700 pc) with its major axis perpendicular to that of the outer disk. Against the compact radio emission of PKS B1718-649 (r ∼ 2 pc), we detect an absorption line at red-shifted velocities with respect to the systemic velocity (∆v = +365 ± 22 km s −1 ). This absorbing CO gas could trace molecular clouds falling onto the central super-massive black hole. A comparison with the near-infra red H 2 1-0 S(1) observations shows that the clouds must be close to the black hole (r 75 pc). The physical conditions of these clouds are different from the gas at larger radii, and are in good agreement with the predictions for the conditions of the gas when cold chaotic accretion triggers an active galactic nucleus. These observations on the centre of PKS B1718-649 provide one of the best indications that a population of cold clouds is falling towards a radio AGN, likely fuelling its activity.

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“…The aim, from the numerical perspective, should be to produce results that can be compared with the state-of-art observations that try to relate the propagation of jets at these scales with the feedback (positive or negative) on the host galaxy (e.g., O'Dea 1998, Labiano 2008, Ogle et al 2010, Willett et al 2010.…”

Section: Discussionmentioning

confidence: 99%

Radio source evolution

Perucho¹

2016

Astron Nachr

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Baldwin (1982) wrote that \emph{the distribution of sources in the radio luminosity, $P$, overall physical size, $D$, diagram} could be considered as \emph{the radio astronomer's $H-R$ diagram}. However, unlike the case of stars, not only the intrinsic properties of the jets, but also those of the host galaxy and the intergalactic medium are relevant to explain the evolutionary tracks of radio radio sources. In this contribution I review the current status of our understanding of the evolution of radio sources from a theoretical and numerical perspective, using the $P-D$ diagram as a framework. An excess of compact (linear size $\leq 10$~kpc) sources could be explained by low-power jets being decelerated within the host galaxy, as shown by recent numerical simulations. Finally, I discuss the possible tracks that radio sources may follow within this diagram, and the physical processes that can explain the different tracks.Comment: Submitted for publication in Astronomische Nachrichten. Review contribution to the proceedings of the 5th Workshop on CSS and GPS radio sources, held in Rimini (Italy) in May 2015. Applied some minor corrections as suggested by the referee and updated the bibliograph

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SPITZERMID-INFRARED SPECTROSCOPY OF COMPACT SYMMETRIC OBJECTS: WHAT POWERS RADIO-LOUD ACTIVE GALACTIC NUCLEI?

Cited by 53 publications

References 132 publications

Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

ALMA observations of AGN fuelling

Radio source evolution

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