A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli, A.; Fossati, M.; Longobardi, A.; Consolandi, G.; Amram, P.; Sun, Ming; Andreani, P.; Boquien, M.; Braine, J.; Combes, F.; Côté, Patrick; Cuillandre, Jean-Charles; Duc, P. A.; Emsellem, Éric; Ferrarese, Laura; Gavazzi, G.; Gwyn, Stephen; Hensler, G.; Peng, Eric W.; Plana, H.; Roediger, Joel; Sánchéz-Janssen, R.; Sarzi, Marc; Serra, P.; Trinchieri, G.

doi:10.1051/0004-6361/201834492

Cited by 26 publications

(37 citation statements)

References 120 publications

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“…The ionised gas emission was determined after subtracting the stellar continuum emission present in the NB filter. For this purpose, the contribution of the stellar continuum was derived as in Boselli et al (2019) from the r-band image combined with the g-band frame taken from the NGVS survey of the cluster (Ferrarese et al 2012) to quantify the colour correction necessary to take into account the dependence on the spectral shape of the emitting sources (Spector et al 2012). This continuum subtraction works very well since it does not leave any clear residual in the final image of the pure gas emission shown in Fig.…”

Section: Vestige Narrow-band Imagingmentioning

confidence: 99%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli

Lupi

Épinat

et al. 2021

A&A

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We study the IB(s)m galaxy IC 3476 observed in the context of the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE), a blind narrow-band Hα+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT. The deep narrow-band image reveals a very pertubed ionised gas distribution that is characterised by a prominent banana-shaped structure in the front of the galaxy formed of giant HII regions crossing the stellar disc. Star-forming structures, at ∼8 kpc from the edges of the stellar disc, are also detected in a deep far-ultraviolet ASTROSAT/UVIT image. This particular morphology indicates that the galaxy is undergoing an almost edge-on ram pressure stripping event. The same Hα+[NII] image also shows that the star formation activity is totally quenched in the leading edge of the disc, where the gas has been removed during the interaction with the surrounding medium. The spectral energy distribution fitting analysis of the multi-frequency data indicates that this quenching episode is very recent (∼50 Myr), and roughly corresponds to an increase of the star formation activity by a factor of ∼161% in the inner regions with respect to that expected for secular evolution. The analysis of these data, whose angular resolution enables the study of the induced effects of the perturbation down to the scale of individual HII regions (req ≃ 40 pc), also suggests that the increase of star formation activity is due to the compression of the gas along the stellar disc of the galaxy, which is able to increase its mean electron density and boost the star formation process producing bright HII regions with luminosities up to L(Hα) ≃ 1038 erg s−1. The combined analysis of the VESTIGE data with deep IFU spectroscopy gathered with MUSE and with high spectral resolution Fabry Perot data also indicates that the hydrodynamic interaction has deeply perturbed the velocity field of the ionised gas component while leaving that of the stellar disc unaffected. The comparison of the data with tuned high-resolution hydrodynamic simulations accounting for the different gas phases (atomic, molecular, ionised) consistently indicates that the perturbing event is very recent (50–150 Myr), once again confirming that ram pressure stripping is a violent phenomenon that is able to perturb the evolution of galaxies in rich environments on short timescales.

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Section: Vestige Narrow-band Imagingmentioning

confidence: 99%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli

Lupi

Épinat

et al. 2021

A&A

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“…Finally, Hα images with the only nebular line contribution are obtained via the subtraction of stellar continuum. The latter is obtained scaling the r -band image by a (g −r ) colour factor that accounts for the difference in the central wavelength of the narrow and broad band filters (see Boselli et al 2018Boselli et al , 2019Boselli et al , 2020Fossati et al 2018). The optical g -band information is taken from the Next Generation Virgo Cluster Survey (Ferrarese et al 2012), which we describe below.…”

Section: The Vestige Surveymentioning

confidence: 99%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Longobardi

Boselli

Fossati

et al. 2020

A&A

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Aims. We measure far-infrared (FIR) emission from tails of stripped dust following the ionised and atomic gas components in galaxies undergoing ram pressure stripping. We study the dust-togas relative distribution and mass ratio in the stripped interstellar medium and relate them to those of the intra-cluster medium (ICM), thus linking the cluster-ICM-galaxy evolution at small-scales. The galaxy sample consists of three Scd Virgo galaxies with stellar masses in the range of 10 9 M * 10 10 M and within 1 Mpc from the cluster centre, namely NGC 4330, NGC 4522, and NGC 4654. Methods. Through the analysis of Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE) Hα, Herschel SPIRE FIR, and VLA Imaging of Virgo in Atomic gas HI data, we trace the spatial distribution of the tails and infer the dust and gas masses from the measured FIR 250 µm and HI flux densities. Dust-togas mass ratios in the tails are analysed as a function of the galaxy mass, metallicity, and dust temperature. Results. Along the stripped component, the dust distribution closely follows the HI and Hα emitting gas, which extend beyond the optical disc (defined by the B-band 25th magnitude isophote). In these regions, the dust-togas mass ratios are 2.0 ± 0.6 × 10 −3 , 0.7 ± 0.1 × 10 −3 , and 0.4 ± 0.03 × 10 −3 for NGC 4330, NGC 4522, and NGC 4654, respectively. Thus, dust is widespread in the stripped material with a lower dust-togas mass ratio (up to a factor of 15) than the one measured in the main body of nearby galaxies. We also find a negative trend in the dust-togas mass ratio as a function of the metallicity that can be explained in terms of a dust component more centrally concentrated in more metal-rich systems. Together with the finding that the stripped dust is cold, T d 25 K, our results can be interpreted as a consequence of an outside-in stripping of the galaxy interstellar medium. Conclusions. Gas and dust in galaxies are perturbed in a similar fashion by the cluster environment, although their relative contribution differs from the one measured in the main body of the galaxies. When this value is considered, ram pressure stripping is consistent with being one of the key mechanisms in building up the Virgo intra-cluster component, injecting dust grains into the ICM, thus contributing to its metal enrichment.

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“…The original Perseus data cube was binned up by a factor of 2 to increase the signal-to-noise ratio. The ionized filaments in Virgo and Abell 2597 was observed using the Multi Unit Spectroscopic Explorer (MUSE) with a spatial sampling of 0.2 and a spectral resolution of R = 3000 (Sarzi et al 2018;Boselli et al 2019;Tremblay et al 2018). For Perseus and Virgo, the velocity in each pixel of the velocity map is obtained as the peak of a Gaussian profile fit to the Hα + NII complex, and for Abell 2597, only Hα is used in the fit.…”

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confidence: 99%

“…Left: Velocity maps of the Hα filaments overlaid on the X-ray residual images (shown in grey) in the centers of Perseus (Gendron-Marsolais et al 2018), Abell 2597 and Virgo(Sarzi et al 2018;Boselli et al 2019).…”

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Direct Detection of Black Hole-driven Turbulence in the Centers of Galaxy Clusters

Gendron-Marsolais

Zhuravleva

et al. 2020

ApJL

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Supermassive black holes (SMBHs) are thought to provide energy that prevents catastrophic cooling in the centers of massive galaxies and galaxy clusters. However, it remains unclear how this "feedback" process operates. We use high-resolution optical data to study the kinematics of multi-phase filamentary structures by measuring the velocity structure function (VSF) of the filaments over a wide range of scales in the centers of three nearby galaxy clusters: Perseus, Abell 2597 and Virgo. We find that the motions of the filaments are turbulent in all three clusters studied. There is a clear correlation between features of the VSFs and the sizes of bubbles inflated by SMBH driven jets. Our study demonstrates that SMBHs are the main driver of turbulent gas motions in the centers of galaxy clusters and suggests that this turbulence is an important channel for coupling feedback to the environment. Our measured amplitude of turbulence is in good agreement with Hitomi Doppler line broadening measurement and X-ray surface brightness fluctuation analysis, suggesting that the motion of the cold filaments is wellcoupled to that of the hot gas. The smallest scales we probe are comparable to the mean free path in the intracluster medium (ICM). Our direct detection of turbulence on these scales provides the clearest evidence to date that isotropic viscosity is suppressed in the weakly-collisional, magnetized intracluster plasma.

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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Cited by 26 publications

References 120 publications

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Direct Detection of Black Hole-driven Turbulence in the Centers of Galaxy Clusters

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