Revealing the velocity structure of the filamentary nebula in NGC 1275 in its entirety

Gendron-Marsolais, Marie-Lou; Hlavacek-Larrondo, J.; Martin, Thomas; Drissen, Laurent; McDonald, Michael; Fabian, A. C.; Edge, A. C.; Hamer, Stephen; McNamara, B. R.; Morrison, G.

doi:10.1093/mnrasl/sly084

Cited by 59 publications

(72 citation statements)

References 33 publications

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“…These filaments are not resolved in our observations and likely consist of many smaller strands (eg. Perseus cluster, Fabian et al 2008;Gendron-Marsolais et al 2018). We also identify clear and possible kpc-scale circumnuclear molecular gas disks in several systems where the emisson peak of a kpc-scale molecular structure is centred on the nucleus and the velocity structure is consistent with rotation about the galaxy's systemic velocity.…”

Section: Resultssupporting

confidence: 55%

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Driving massive molecular gas flows in central cluster galaxies with AGN feedback

Russell

McNamara

Fabian

et al. 2019

Monthly Notices of the Royal Astronomical Society

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119

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We present an analysis of new and archival ALMA observations of molecular gas in twelve central cluster galaxies. We examine emerging trends in molecular filament morphology and gas velocities to understand their origins. Molecular gas masses in these systems span 10 9 − 10 11 M , far more than most gas-rich galaxies. ALMA images reveal a distribution of morphologies from filamentary to disk-dominated structures. Circumnuclear disks on kiloparsec scales appear rare. In most systems, half to nearly all of the molecular gas lies in filamentary structures with masses of a few ×10 8−10 M that extend radially several to several tens of kpc. In nearly all cases the molecular gas velocities lie far below stellar velocity dispersions, indicating youth, transience or both. Filament bulk velocities lie far below the galaxy's escape and free-fall speeds indicating they are bound and being decelerated. Most extended molecular filaments surround or lie beneath radio bubbles inflated by the central AGN. Smooth velocity gradients found along the filaments are consistent with gas flowing along streamlines surrounding these bubbles. Evidence suggests most of the molecular clouds formed from low entropy X-ray gas that became thermally unstable and cooled when lifted by the buoyant bubbles. Uplifted gas will stall and fall back to the galaxy in a circulating flow. The distribution in morphologies from filament to disk-dominated sources therefore implies slowly evolving molecular structures driven by the episodic activity of the AGN.

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Section: Resultssupporting

confidence: 55%

“…We note that the smaller strands that make up these filaments may have more complex dynamics within this larger scale smooth gradient (eg. Hatch et al 2006;Gendron-Marsolais et al 2018).…”

Section: Velocity Structurementioning

confidence: 99%

Driving massive molecular gas flows in central cluster galaxies with AGN feedback

Russell

McNamara

Fabian

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

119

111

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“…5. Complex structures in the velocity field of the ionised gas filaments have been observed in other radio galaxies such as NGC 1275 in Perseus (Gendron-Marsolais et al 2018), where star formation is also present (Canning et al 2014).…”

Section: The Origin Of the Filamentmentioning

confidence: 90%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli

Fossati

Longobardi

et al. 2019

A&A

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We observed the giant elliptical galaxy M 87 during the Virgo Environmental Survey Tracing Galaxy Evolution (VESTIGE), a blind narrow-band Hα+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the Canada French Hawaii Telescope (CFHT). The deep narrow-band image confirmed the presence of a filament of ionised gas extending up to ≃3 kpc in the north-western direction and ≃8 kpc to the southeast, with a couple of plumes of ionised gas, the weakest of which, at ≃18 kpc from the nucleus, was previously unknown. The analysis of deep optical images taken from the NGVS survey confirms that this gas filament is associated with dust seen in absorption which is now detected up to ≃2.4 kpc from the nucleus. We also analysed the physical and kinematical properties of the ionised gas filament using deep IFU MUSE data covering the central 4.8 × 4.8 kpc2 of the galaxy. The spectroscopic data confirm a perturbed kinematics of the ionised gas, with differences in velocity of ≃700–800 km s−1 on scales of ≲1 kpc. The analysis of 2D diagnostic diagrams and the observed relationship between the shock-sensitive [OI]/Hα line ratio and the velocity dispersion of the gas suggest that the gas is shock-ionised.

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“…Moreover, Figure 10 reveals an excellent agreement between the Hitomi velocity dispersion for the Perseus Cluster and the line width of the ensemble warm Hα+[NII] phase obtained from SITELLE data . In a subsequent work, Gendron-Marsolais et al (2018) studied several smaller-scale patches of the NGC 1275 nebula detected with SITELLE, finding that, while the velocity dispersions of the filamentary nebula surrounding NGC 1275 are indeed as low and uniform as the Hitomi measurements of the ICM, there is no correlation between the bulk velocities of the different phases.…”

Section: Recent Progress Using Micro-calorimeter X-ray Spectroscopymentioning

confidence: 99%

Constraining Gas Motions in the Intra-Cluster Medium

et al. 2019

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The detailed velocity structure of the diffuse X-ray emitting intracluster medium (ICM) remains one of the last missing key ingredients in understanding the microphysical properties of these hot baryons and constraining our models of the growth and evolution of structure on the largest scales in the Universe. Direct measurements of the gas velocities from the widths and shifts of X-ray emission lines were recently provided for the central region of the Perseus Cluster of galaxies by Hitomi, and upcoming high-resolution Xray microcalorimeters onboard XRISM and Athena are expected to extend these studies to many more systems. In the mean time, several other direct and indirect methods have been proposed for estimating the velocity structure in the ICM, ranging from resonant scattering to X-ray surface brightness fluctuation analysis, the kinematic Sunyaev-Zeldovich effect, or using optical line emitting nebulae in the brightest cluster galaxies as tracers of the motions of the ambient plasma. Here, we review and compare the existing estimates of the velocities of the hot baryons, as well as the various overlapping physical processes that drive motions in the ICM, and discuss the implications of these measurements for constraining the viscosity and identifying the source of turbulence in clusters of galaxies.

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Revealing the velocity structure of the filamentary nebula in NGC 1275 in its entirety

Cited by 59 publications

References 33 publications

Driving massive molecular gas flows in central cluster galaxies with AGN feedback

Driving massive molecular gas flows in central cluster galaxies with AGN feedback

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Constraining Gas Motions in the Intra-Cluster Medium

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