Methane Emissions

Fevre, Chris Le

doi:10.26889/9781784670887

Cited by 20 publications

(28 citation statements)

References 9 publications

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“…For instance, galaxies inhabiting clusters with low σ, that are less massive, are expected to have undergone stronger galaxy-galaxy interactions than galaxies in clusters with high σ, since the low-velocities increase the cross section for mergers (e.g. Le Févre et al 2000). On the other hand, more-massive clusters have stronger potentials and ram-pressure stripping (which goes as ρσ 2 , with ρ the gas density) is extremely strong in them (e.g.…”

Section: Host Cluster Mass Dependencesmentioning

confidence: 99%

The evolution of ultra-diffuse galaxies in nearby galaxy clusters from the Kapteyn IAC WEAVE INT Clusters Survey

Piña

Aguerri

Peletier

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the population of ultra-diffuse galaxies (UDGs) in a set of eight nearby (z < 0.035) galaxy clusters, from the Kapteyn IAC WEAVE INT Clusters Survey (KIWICS). We report the discovery of 442 UDG candidates in our eight field of views, with 247 of these galaxies lying at projected distances < 1 R 200 from their host cluster. With the aim of testing theories about their formation, we study the scaling relations of UDGs comparing with different types of galaxies, finding that in the full parameter space they behave as dwarf galaxies and their colors do not seem to correlate with their effective radii. To investigate the influence of the environment on the evolution of UDGs we analyze their structural properties as functions of the projected clustercentric distance and the mass of their host cluster. We find no systematic trends for the stellar mass nor effective radius as function of the projected distance. However, the fraction of blue UDGs seems to be lower towards the center of clusters, and UDGs in the inner and outer regions of clusters have different Sérsic index and axis ratio distributions. Specifically, the axis ratio distributions of the outer and inner UDGs resemble the axis ratio distributions of, respectively, late-type dwarfs and dwarf ellipticals in the Fornax Cluster suggesting an environmentally-driven evolution and another link between UDGs and dwarf galaxies. In general our results suggest strong similarities between UDGs and smaller dwarf galaxies in their structural parameters and their transformation within clusters.

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Section: Host Cluster Mass Dependencesmentioning

confidence: 99%

The evolution of ultra-diffuse galaxies in nearby galaxy clusters from the Kapteyn IAC WEAVE INT Clusters Survey

Piña

Aguerri

Peletier

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Despite the necessity to characterize the properties of z > 3 massive, star-forming disks, only limited/small samples of such galaxies exist (e.g., Hodge et al 2012;De Breuck et al 2014;Jones et al 2017;Shao et al 2017). For instance, out of the 118 SFGs at 4 < z < 6 in the recent ALPINE [C II] survey, no more than 15% of them are rotating disks (Le Fèvre et al 2019). Among the hundreds of SMGs across the two square degree COSMOS field (e.g., Casey et al 2013;Brisbin et al 2017), only AzTEC1 (z = 4.341), AzTEC/C159 (z = 4.569), J1000+0234 (z = 4.542), and Vd−17871 (z = 4.622) exhibit convincing evidence for gas-dominated rotating disks Tadaki et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The Redshift and Star Formation Mode of AzTEC2: A Pair of Massive Galaxies at z = 4.63

Jiménez-Andrade

Zavala

Magnelli

et al. 2020

ApJ

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We combine observations from the Atacama Large Millimeter/submillimeter Array (ALMA) and the NOrthern Extended Millimeter Array (NOEMA) to assess the redshift and to study the star formation conditions in AzTEC2: one of the brightest sub-millimeter galaxies (SMGs) in the COSMOS field (S 1.1mm = 10.5 ± 1.4 mJy). Our high-resolution observations confirm that AzTEC2 splits into two components (namely AzTEC2-A and AzTEC2-B) for which we detect [C II] and 12 CO(5→4) line emission, implying a redshift of 4.626±0.001 (4.633±0.001) for AzTEC2-A (AzTEC2-B) and ruling out previous associations with a galaxy at z ∼ 1. We use the 12 CO(5→4) line emission and adopt typical SMG-like gas excitation conditions to estimate the molecular gas mass, which is M gas (α CO /2.5) = 2.1 ± 0.4 × 10 11 M for AzTEC2-A, and a factor four lower for AzTEC2-B. With the infrared-derived star formation rate of AzTEC2-A (1920 ± 100 M yr −1 ) and AzTEC2-B (710 ± 35 M yr −1 ), they both will consume their current gas reservoir within (30−200) Myr. We find evidence of a rotation-dominated [C II] disk in AzTEC2-A, with a de-projected rotational velocity of v rot (i = 39 • ) = 660 ± 130 km s −1 , velocity dispersion 100 km s −1 , and dynamical mass of M dyn (i = 39 • ) = 2.6 +1.2 −0.9 × 10 11 M . We propose that an elevated gas accretion rate from the cosmic web might be the main driver of the intense levels of star formation in AzTEC2-A, which might be further enhanced by gravitational torques induced by its minor companion (AzTEC2-B). These results strengthen the picture whereby the population of single-dish selected SMGs is rather heterogeneous, including a population of pairs of massive, highly-active galaxies in a pre-coalescence phase.

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“…Here we present new Very Large Telescope (VLT) VIsible MultiObject Spectrograph (VIMOS; Le Févre et al 2003) observations of two star-forming dwarf galaxies using the integral field unit (IFU) spectroscopy mode (hereafter VIMOS-IFU). UM 461 (upper panel in Figure 1) is a well studied H ii/BCD galaxy (e.g.…”

Section: Introductionmentioning

confidence: 99%

Detecting metal-poor gas accretion in the star-forming dwarf galaxies UM 461 and Mrk 600

Lagos

Scott

Nigoche-Netro³

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Using VIMOS-IFU observations, we study the interstellar medium (ISM) of two star-forming dwarf galaxies, UM 461 and Mrk 600. Our aim was to search for the existence of metallicity inhomogeneities that might arise from infall of nearly pristine gas feeding ongoing localized star-formation. The IFU data allowed us to study the impact of external gas accretion on the chemical evolution as well as the ionised gas kinematics and morphologies of these galaxies. Both systems show signs of morphological distortions, including cometary-like morphologies. We analysed the spatial variation of 12 + log(O/H) abundances within both galaxies using the direct method (T e ), the widely applied HII-CHI-mistry code, as well as by employing different standard calibrations. For UM 461 our results show that the ISM is fairly well mixed, at large scales, however we find an off-centre and low-metallicity region with 12 + log(O/H) < 7.6 in the SW part of the brightest H ii region, using the direct method. This result is consistent with the recent infall of a low mass metal-poor dwarf or H i cloud into the region now exhibiting the lowest metallicity, which also displays localized perturbed neutral and ionized gas kinematics. Mrk 600 in contrast, appears to be chemically homogeneous on both large and small scales. The intrinsic differences in the spatially resolved properties of the ISM in our analysed galaxies are consistent with these systems being at different evolutionary stages.

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Methane Emissions

Cited by 20 publications

References 9 publications

The evolution of ultra-diffuse galaxies in nearby galaxy clusters from the Kapteyn IAC WEAVE INT Clusters Survey

The evolution of ultra-diffuse galaxies in nearby galaxy clusters from the Kapteyn IAC WEAVE INT Clusters Survey

The Redshift and Star Formation Mode of AzTEC2: A Pair of Massive Galaxies at z = 4.63

Detecting metal-poor gas accretion in the star-forming dwarf galaxies UM 461 and Mrk 600

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