The kinematical properties of superbubbles and H ii regions of the Large Magellanic Cloud derived from the 3D Hα Survey

Ambrocio-Cruz, P.; Coarer, E. Le; Rosado, M.; Russeil, D.; Amram, P.; Laval, A.; Épinat, B.; Ramírez, M. D. Pérez; Odonne, M.; Goldès, G.

doi:10.1093/mnras/stw054

Cited by 19 publications

(18 citation statements)

References 49 publications

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“…Since all the points plotted in these panels are included within the MUSE field, where the Hα emission is sufficiently high to enable an accurate estimate of the velocity dispersion in the Farby-Perot cube, the Hα data are corrected for [NII] contamination and dust attenuation using their local estimate in the MUSE data. The velocity dispersion of the HII regions ranges between 15 σ 40 km s −1 , and is thus comparable to that observed in the giant HII regions of other nearby galaxies (e.g., Smith & Weedman 1970;Chu & Kennicutt 1994;Ambrocio-Cruz et al 2016;Bresolin et al 2020). The first three plots do not show any correlation, but suggest that the HII regions located on the front region formed after the dynamical interaction with the IGM, have, on average, a higher Hα luminosity and electron density per unit velocity dispersion than their counterparts on the stellar disc, with a similar distribution of their size.…”

Section: Kinematical Propertiessupporting

confidence: 79%

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: Kinematical Propertiessupporting

confidence: 79%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli

Lupi

Épinat

et al. 2021

A&A

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“…This region is also categorized as a superbubble by a Hα shell, and the OB association LH 47 is located in the center of the shell. Ambrocio-Cruz et al (2016) investigated kinematic features of Hα emission and compared it with the L-and D-components. These authors showed that compact Hii regions N44B and C have two Hα components with a velocity difference of ∼30 km s −1 , and interpreted that N44B and C belong to the L-and D-components, respectively.…”

Section: Lha 120-n 44mentioning

confidence: 99%

“…The mean intensity of the diffuse L-component is ∼40 % of that of the Hi Ridge. Several Hii regions (Ambrocio-Cruz et al 2016) are located in the south of the diffuse L-component. The Dcomponent is extended over the entire LMC and is characterized by the morphological properties with many cavities and voids (e.g., Kim et al 1998b;Dawson et al 2013).…”

Section: Distribution Of the L-and D-componentsmentioning

confidence: 99%

Formation of the Active Star-forming Region LHA 120-N 44 Triggered by Tidally Driven Colliding H i Flows

Tsuge

Sano

Tachihara

et al. 2019

ApJ

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N44 is the second active site of high mass star formation next to R136 in the Large Magellanic Cloud (LMC). We carried out a detailed analysis of Hi at 60 arcsec resolution by using the ATCA & Parkes data. We presented decomposition of the Hi emission into two velocity components (the L-and D-components) with the velocity separation of ∼60 km s −1 . In addition, we newly defined the I-component whose velocity is intermediate between the L-and D-components. The D-component was used to derive the rotation curve of the LMC disk, which is consistent with the stellar rotation curve (Alves & Nelson 2000). Toward the active cluster forming region of LHA 120-N 44, the three velocity components of Hi gas show signatures of dynamical interaction including bridges and complementary spatial distributions. We hypothesize that the L-and D-components have been colliding with each other since 5 Myrs ago and the interaction triggered formation of the O and early B stars ionizing N44. In the hypothesis the I-component is interpreted as decelerated gas in terms of momentum exchange in the collisional interaction of the Land D-components. In the N44 region the P lanck sub-mm dust optical depth is correlated with the Hi intensity, which is well approximated by a linear regression. We found that the N44 region shows a significantly steeper regression line than in the Bar region, indicating less dust abundance in the N44 region, which is ascribed to the tidal interaction between the LMC with the SMC 0.2 Gyrs ago.

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“…It is known that the gas velocity dispersion in the giant H II region correlates with the Hα luminosity or diameter, in the sense that the σ is higher in the H II region with a higher Hα luminosity or larger diameter (Terlevich & Melnick 1981;Fernández Arenas et al 2018). There is the minimum value of the gas velocity dispersion in H II regions of a given Hα luminosity or diameter for H II regions with a Hα luminosity higher than ∼10 38 erg/s (Relaño et al 2005;Zaragoza-Cardiel et al 2015;Ambrocio-Cruz et al 2016). The integral emission line profile of a giant H II region measued at low resolution is rather smooth and well fitted by a Gaussian, while the observations at high spatial and spectral resolution reveal that a giant H II region breaks up into many discrete components (Chu & Kennicutt 1994;Bresolin et al 2020).…”

Section: Minor Merger or Interaction As A Reason For The Spot Of Enha...mentioning

confidence: 92%

MaNGA galaxies with off-centered spots of enhanced gas velocity dispersion

Pilyugin,

Cedres,

Zinchenko

et al. 2021

Preprint

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Off-centered spots of the enhanced gas velocity dispersion, σ, are revealed in some galaxies from the Mapping Nearby Galaxies at Apache Point Observatory survey (MaNGA). Aiming to clarify the origin of the spots of enhanced σ, we examine the distributions of the surface brightness, the line-of-sight velocity, the oxygen abundance, the gas velocity dispersion, and the Baldwin-Phillips-Terlevich (BPT) spaxel classification in seven galaxies. We find that the enhanced σ spots in six galaxies can be attributed to a (minor) interaction with a satellite. Three galaxies in our sample have a very close satellite (the separation in the sky plane is comparable to the optical radius of the galaxy). The spots of enhanced σ in those galaxies are located at the edge of the galaxy close to the satellite. The spots of enhanced σ in three other galaxies are related to bright spots in the photometric B band within the galaxy, which can be due to the projection of a satellite in the line of sight of the galaxy. The oxygen abundances in the spots in these three galaxies are reduced. This suggests that the low-metallicity gas from the satellite is mixed with the interstellar medium of the disk, that is, the gas exchange between the galaxy and its satellite takes place. The spectra of the spaxels within a spot are usually H II-region-like, suggesting that the interaction (gas infall) in those galaxies does not result in appreciable shocks. In contrast, the spot of the enhanced σ in the galaxy M-8716-12703 is associated with an off-centered active galactic nucleus-like (AGN-like) radiation distribution. One can suggest that the spot of the enhanced σ in the M-8716-12703 galaxy is different in origin, or that the characteristics of gas infall in this case differs from that in other galaxies.

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The kinematical properties of superbubbles and H ii regions of the Large Magellanic Cloud derived from the 3D Hα Survey

Cited by 19 publications

References 49 publications

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Formation of the Active Star-forming Region LHA 120-N 44 Triggered by Tidally Driven Colliding H i Flows

MaNGA galaxies with off-centered spots of enhanced gas velocity dispersion

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