Kinematics and physical properties of the nearby galaxy NGC 4656 and its TDG candidate

Muñoz-Elgueta, Nahir; Torres-Flores, S.; Amram, P.; Hernández-Jiménez, J. A.; Urrutia-Viscarra, F.; Oliveira, C. Mendes de; Gómez-López, J. A.

doi:10.1093/mnras/sty1934

Cited by 9 publications

(4 citation statements)

References 106 publications

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“…A clustered component, whose centroid is closer to the RGB centroid, and a very elongated tail, extending from the clustered component to the northeast (the "hook"). Moreover, in the last 0-20 Myr the clustered component has become more active with respect to the tail, suggesting that the SF is progressing toward the south-west, in apparent contrast with the result of Muñoz-Elgueta et al (2018). However, their finding is that the very recent SFR is more intense in the north-east region, compared to the central and southwest one.…”

Section: Sf Spatial Patternsmentioning

confidence: 88%

Star Formation Histories of the LEGUS Dwarf Galaxies. III. The Nonbursty Nature of 23 Star-forming Dwarf Galaxies*

Cignoni

Sacchi

Tosi

et al. 2019

ApJ

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We derive the recent star formation histories of 23 active dwarf galaxies using HST observations from the Legacy Extragalactic UV Survey (LEGUS). We apply a color-magnitude diagram fitting technique using two independent sets of stellar models, PARSEC-COLIBRI and MIST. Despite the non-negligible recent activity, none of the 23 star forming dwarfs show enhancements in the last 100 Myr larger than three times the 100-Myr-average. The unweighted mean of the individual SFHs in the last 100 Myr is also consistent with a rather constant activity, irrespective of the atomic gas fraction. We confirm previous results that for dwarf galaxies the CMD-based average star formation rates (SFRs) are generally higher than the FUV-based SFR. For half of the sample, the 60-Myr-average CMD-based SFR is more than two times the FUV SFR. In contrast, we find remarkable agreement between the 10-Myr-average CMD-based SFR and the Hα-based SFR. Finally, using core helium burning stars of intermediate mass we study the pattern of star formation spatial progression over the past 60 Myr, and speculate on the possible triggers and connections of the star formation activity with the environment in which these galaxies live. Approximately half of our galaxies show spatial progression of star formation in the last 60 Myr, and/or very recent diffuse and off-center activity compared to RGB stars.

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Section: Sf Spatial Patternsmentioning

confidence: 88%

Star Formation Histories of the LEGUS Dwarf Galaxies. III. The Nonbursty Nature of 23 Star-forming Dwarf Galaxies*

Cignoni

Sacchi

Tosi

et al. 2019

ApJ

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“…9). This might indicate that fresh star-forming gas is constantly fueled towards the center of galaxies, either due to VDI, minor/major mergers and/or tidal interactions (e.g., Larson 2003;Rupke et al 2010;Sillero et al 2017;Ellison et al 2018;Muñoz-Elgueta et al 2018). Regardless of the dominant mechanism driving the formation of stars in galaxies (on and above the MS), violent and secular galaxy's evolutionary channels lead to the formation of a bulge (e.g., Kormendy & Kennicutt 2004;Fisher 2006;Hopkins et al 2009;Brooks & Christensen 2016;Tonini et al 2016).…”

Section: Centrally-concentrated Star Formation; Evidence Of Bulge Gro...mentioning

confidence: 99%

Radio continuum size evolution of star-forming galaxies over 0.35 < z < 2.25

Jiménez-Andrade

Magnelli

Karim

et al. 2019

A&A

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To better constrain the physical mechanisms driving star formation, we present the first systematic study of the radio continuum size evolution of star-forming galaxies (SFGs) over the redshift range 0.35 < z < 2.25. We use the VLA COSMOS 3GHz map (noise rms = 2.3 µJy beam −1 , θ beam = 0.75 arcsec) to construct a mass-complete sample of 3184 radio-selected SFGs that reside on and above the main-sequence (MS) of SFGs. We constrain the overall extent of star formation activity in galaxies by applying a 2D-Gaussian model to their radio continuum emission. Extensive Monte Carlo simulations are used to validate the robustness of our measurements and characterize the selection function. We find no clear dependence between the radio size and stellar mass, M , of SFGs with 10.5 log(M /M ) 11.5. Our analysis suggests that MS galaxies are preferentially extended, while SFGs above the MS are always compact. The median effective radius of SFGs on (above) the MS of R eff = 1.5 ± 0.2 (1.0 ± 0.2) kpc remains nearly constant with cosmic time; a parametrization of the form R eff ∝ (1 + z) α yields a shallow slope of only α = −0.26 ± 0.08 (0.12 ± 0.14) for SFGs on (above) the MS. The size of the stellar component of galaxies is larger than the extent of the radio continuum emission by a factor ∼2 (1.3) at z = 0.5 (2), indicating star formation is enhanced at small radii. The galactic-averaged star formation rate surface density (Σ SFR ) scales with the distance to the MS, except for a fraction of MS galaxies ( 10%) that harbor starburst-like Σ SFR . These "hidden" starbursts might have experienced a compaction phase due to disk instability and/or merger-driven burst of star formation, which may or may not significantly offset a galaxy from the MS. We thus propose to jointly use Σ SFR and distance to the MS to better identify the galaxy population undergoing a starbursting phase.

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“…The package provides the velocity moment maps of the H α 3D data cube and it has been used by different authors during the last years (e.g. Boselli et al 2018;Muñoz-Elgueta et al 2018;Gómez-López et al 2019). The main advantage of the techniques implemented in this package is the use of adaptive spatial binning, based on a 2D Voronoi tessellation method, applied to the spatial dimensions of the 3D data cubes.…”

Section: H α Fabry-perot Observationsmentioning

confidence: 99%

A tidally induced global corrugation pattern in an external disc galaxy similar to the Milky Way

Gómez,

Torres-Flores,

Mora-Urrejola

et al. 2020

Preprint

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We study the two dimensional (2D) line-of-sight velocity (V los ) field of the low-inclination, late-type galaxy VV304a. The resulting 2D kinematic map reveals a global, coherent and extended perturbation that is likely associated with a recent interaction with the massive companion VV304b. We use multi-band imaging and a suite of test particle simulations to quantify the plausible strength of in-plane flows due to non-axisymmetric perturbations and show that the observed velocity flows are much too large to be driven either by spiral structure nor by a bar. We use fully cosmological hydrodynamical simulations to characterize the contribution from inand off-plane velocity flows to the V los field of recently interacting galaxy pairs like the VV304 system. We show that, for recently perturbed low-inclination galactic discs, the structure of the residual velocity field, after subtraction of an axisymmetric rotation model, can be dominated by vertical flows. Our results indicate that the V los perturbations in VV304a are consistent with a corrugation pattern. Its V los map suggests the presence of a structure similar to the Monoceros ring seen in the Milky Way. Our study highlights the possibility of addressing important questions regarding the nature and origin of vertical perturbations by measuring the lineof-sight velocities in low-inclination nearby galaxies.

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Kinematics and physical properties of the nearby galaxy NGC 4656 and its TDG candidate

Cited by 9 publications

References 106 publications

Star Formation Histories of the LEGUS Dwarf Galaxies. III. The Nonbursty Nature of 23 Star-forming Dwarf Galaxies*

Star Formation Histories of the LEGUS Dwarf Galaxies. III. The Nonbursty Nature of 23 Star-forming Dwarf Galaxies*

Radio continuum size evolution of star-forming galaxies over 0.35 < z < 2.25

A tidally induced global corrugation pattern in an external disc galaxy similar to the Milky Way

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