A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli, A.; Fossati, M.; Longobardi, A.; Khashayar, Kianfar,; Dametto, N. Z.; Amram, P.; Anderson, J. P.; Andreani, P.; Boissier, S.; Boquien, M.; Buat, V.; Consolandi, G.; Cortese, Luca; Côté, Patrick; Cuillandre, J. C.; Ferrarese, Laura; Galbany, L.; Gavazzi, G.; Gwyn, Stephen; Hensler, G.; Hutchings, J. B.; Peng, Eric W.; Postma, J.; Roediger, Joel; Roehlly, Y.; Serra, P.; Trinchieri, G.

doi:10.1051/0004-6361/202142482

Cited by 10 publications

(18 citation statements)

References 233 publications

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“…Figure 8 shows that the rotating gas is less extended along the disc upwind (+1.8 arcsec), where it reaches 50 arcsec (∼4 kpc) in both the north-east and south-west directions, than in the tail (70 arcsec to the north-east and 60 arcsec to the south-west). This result is expected in a ram pressure stripping scenario, where the gas is removed outside-in (e.g., Quilis et al 2000;Vollmer et al 2001;Boselli et al , 2022Roediger & Hensler 2005;Tonnesen & Bryan 2009).…”

Section: Pvds Along the Major Axismentioning

confidence: 64%

“…Figure 6 shows the velocity dispersion of the galaxy as measured from the PUMA and GHASP datasets. Following Boselli et al (2022) we checked that the velocity profiles have a single peak, (i.e. that the barycentric method applied to measure the velocity dispersions does not introduce any strong systematic bias in the results).…”

Section: Velocity Dispersionmentioning

confidence: 99%

“…The PUMA velocity dispersion is higher than the one measured in the GHASP data because of its reduced spectral resolution. It is indeed difficult to measure velocities far below the instrumental resolution (σ LSF = 19.5 and 13.1 km s −1 , respectively) as it has been recently discussed in Boselli et al (2022) in comparing VLT/MUSE data with FP data obtained with GHASP.…”

Section: Velocity Dispersionmentioning

confidence: 99%

“…The kinematics of the stripped gas is thus a crucial parameter for understanding the process of star formation within the tails. Observations and simulations of ram pressure stripped galaxies consistently indicate that a ram pressure stripping process is able to drastically perturb the velocity field of a spiral galaxy, displacing its kinematic centre with respect to the photometric one and affecting its rotation curve (RC; Vollmer et al 2001Vollmer et al , 2004Vollmer et al , 2006Vollmer et al , 2008Kronberger et al 2008;Merluzzi et al 2013;Fumagalli et al 2014;Consolandi et al 2017;Sheen et al 2017;Bellhouse et al 2017Bellhouse et al , 2019Boselli et al 2022). Despite the advent of extraordinary new instrumentation in the optical (Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope (VLT)) and radio (Atacama Large Millimeter/submillimeter Array -ALMA) domain, multi-frequency data at high angular and spectral resolution of nearby ram pressure stripped galaxies, where the proximity allows us to study the star formation process down to the scale of individual HII regions, are only sporadically available.…”

Section: Introductionmentioning

confidence: 97%

“…Indeed, gravitational perturbations act indifferently on the stellar and gaseous components, also producing tidal structures visible in deep broad-band imaging data. Several galaxies undergoing a ram pressure stripping event have been identified so far (Boselli et al 2016a(Boselli et al , 2018a(Boselli et al , 2022Fossati et al 2018;Longobardi et al 2020;Junais et al 2021). Among them, NGC 4330 is an edge-on galaxy with evident tails of atomic (Chung et al 2007(Chung et al , 2009 and ionised (Abramson et al 2011;Fossati et al 2018) gas, which indicates that the galaxy is entering the cluster from the south and impacting the intracluster medium (ICM) almost face on.…”

Section: Introductionmentioning

confidence: 99%

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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Sardaneta

Amram

Boselli

et al. 2022

A&A

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Using the VESTIGE survey, a deep narrow-band Hα imaging survey of the Virgo cluster carried out at the CFHT with MegaCam, we discovered a long and diffuse tail of ionised gas in the edge-on late-type galaxy NGC 4330. This peculiar feature indicates an ongoing ram pressure stripping event able to remove the gas in the outer region of the disc. Tuned hydrodynamic simulations suggest that the ram pressure stripping event is occurring almost face-on, making NGC 4330 the ideal candidate for studying the effects of the perturbation in the direction perpendicular to the disc plane. We present here two new independent sets of Fabry-Perot observations (R ≃ 10 000) with the purpose of understanding the effects of the ram pressure stripping process on the kinematics of the ionised gas. Despite their limited sensitivity to the diffuse gas emission, the data allowed us to measure the velocity and the velocity dispersion fields over the galaxy disc and in several features at the edges or outside the stellar disc formed after the ram pressure stripping event. We constructed the position-velocity diagrams and the rotation curves of the galaxy using three different techniques. The data show, consistent with the hydrodynamic simulations, that the galaxy has an inner solid-body rotation up to ∼2.4 kpc, with non-circular streaming motions outside this radius and in the several external features formed during the interaction of the galaxy with the surrounding intracluster medium. The data also indicate a decrease in the rotational velocity of the gas with increasing distance from the galaxy disc along the tails, suggesting a gradual but not linear loss of angular momentum in the stripped gas. Consistent with a ram pressure stripping scenario, the i-band image shows a boxy shape at the south-west edge of the disc, where the stellar orbits might have been perturbed by the modification of the gravitational potential well of the galaxy due to the displacement of the gas in the z direction.

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Section: Pvds Along the Major Axismentioning

confidence: 64%

Section: Velocity Dispersionmentioning

confidence: 99%

Section: Velocity Dispersionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

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Amram

Boselli

et al. 2022

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Ram pressure stripping in high-density environments

Boselli

Fossati

Sun

2022

Astron Astrophys Rev

155

117

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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli

Fossati

Roediger

et al. 2023

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Using a compilation of Hα fluxes for 384 star-forming galaxies detected during the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE), we study several important scaling relations linking the star formation rate, specific star formation rate, stellar mass, stellar mass surface density, and atomic gas depletion timescale for a complete sample of galaxies in a rich environment. The extraordinary sensitivity of the narrow-band imaging data allows us to sample the whole dynamic range of the Hα luminosity function, from massive galaxies (M star 10 11 M ) to dwarf systems (M star 10 6 M ), where the ionised gas emission is due to the emission of single O-early B stars. This extends previous works to a dynamic range in stellar mass and star formation rate (10 −4 S FR 10 M yr −1 ) that has never been explored so far. The main-sequence relation derived for all star-forming galaxies within one virial radius of the Virgo cluster has a slope comparable to that observed in other nearby samples of isolated objects, but its dispersion is about three times larger (∼ 1 dex). The dispersion is tightly connected to the available amount of HI gas, with gas-poor systems located far below objects of similar stellar mass, but with a normal HI content. When measured on unperturbed galaxies with a normal HI gas content (HI − de f ≤ 0.4), the relation has a slope a=0.92±0.06, an intercept b = -1.57±0.06 (at a pivot point of log M star = 8.451 M ), and a scatter σ 0.40, and it has a constant slope in the stellar mass range 10 6 M star 3 × 10 11 M . The specific star formation rate of HI-poor galaxies is significantly lower than that of HI-rich systems of similar stellar mass, while their atomic gas consumption timescale τ HI is fairly similar, in particular, for objects of stellar mass 10 7 M star 10 9 M . We compare these observational results to the prediction of models expressly tuned to reproduce the effects induced by the interaction of galaxies with their surrounding environment. The observed scatter in the main-sequence relation can be reproduced only after a violent and active stripping process such as ram-pressure stripping that removes gas from the disc (outer parts first) and quenches star formation on short (< 1 Gyr) timescales. This rules out milder processes such as starvation. This interpretation is also consistent with the position of galaxies of different star formation activity and gas content within the phase-space diagram. We also show that the star-forming regions that formed in the stripped material outside perturbed galaxies are located well above the main-sequence relation drawn by unperturbed systems. These extraplanar HII regions, which might be at the origin of ultra-compact dwarf galaxies (UCDs) and other compact sources typical in rich environments, are living a starburst phase lasting only 50 Myr. They later become quiescent systems.

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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Cited by 10 publications

References 233 publications

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Ram pressure stripping in high-density environments

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

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