Gas Accretion and Angular Momentum

Stewart, Kyle R.

doi:10.1007/978-3-319-52512-9_11

Cited by 15 publications

(6 citation statements)

References 132 publications

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“…This means that only the combination of a dwarf galaxy velocity and a large spin allows the model to reproduce the properties of NGVS 3543. Cosmological simulations indicate that the spin parameter distribution is expected to be lognormal, with a peak at 0.05, and σ = 0.5 (Mo et al 1998), but cold gas accretion could lead to larger angular momentum (Stewart 2017). The value of λ = 0.14 is beyond the peak of the distribution, but is not totally unexpected based on these considerations.…”

Section: Galaxy Evolution Models With Ram-pressure Stripping Applied To Ngvs 3543mentioning

confidence: 95%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Junais

Boissier

Boselli

et al. 2021

A&A

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Context. The evolution of galaxies depends on their interaction with the surrounding environment. Ultra-diffuse galaxies (UDGs) have been found in large numbers in clusters. We detected a few star-forming blobs in the VESTIGE survey, located at ∼5 kpc from a UDG, namely NGVS 3543, in association with an HI gas cloud AGC 226178, suggesting a recent interaction between this low-surface-brightness system and the surrounding cluster environment. Aims. We use a complete set of multi-frequency data including deep optical, UV, and narrow-band Hα imaging and HI data to understand the formation process that gave birth to this peculiar system. Methods. For this purpose, we measured (i) the multi-wavelength radial surface brightness profiles of NGVS 3543 and compared them to the predictions of spectro-photometric models of galaxy evolution in rich clusters; and (ii) the aperture photometry of the blue regions in the vicinity of NGVS 3543 in order to determine their age and stellar mass. Results. Comparisons of the observations with evolutionary models indicate that NGVS 3543 has undergone a ram-pressure stripping that peaked ∼100 Myr ago, transforming a blue gas-rich UDG into a red gas-poor UDG. Star formation has taken place in the ram pressure stripped gas, the mass of which is ∼108 M⊙, forming star complexes with a typical age of ∼20 Myr and a stellar mass of ∼104 M⊙. Conclusions. These results suggest that we are observing for the first time the ongoing transformation of a gas-rich UDG into a red and quiescent UDG under the effect of a ram-pressure stripping event. The same process could explain the lack of star-forming UDGs in rich environments observed in several nearby clusters.

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Section: Galaxy Evolution Models With Ram-pressure Stripping Applied To Ngvs 3543mentioning

confidence: 95%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Junais

Boissier

Boselli

et al. 2021

A&A

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“…This corresponds to an extrapolation by a factor of several in spatial scale; a key assumption in our analysis is therefore that the galaxies' gaseous halos at this radius co-rotates with their inner region where the spin is measured. In a hierarchical formation scenario, this is not necessarily the case, for outer halos may have built up from contributions with different angular momenta [49]. Nevertheless, recent measurements on simulations show a strong correlation in the angular momentum of hot gas across most of the virial radius [50].…”

Section: Stackingmentioning

confidence: 98%

Probing gaseous galactic halos through the rotational kinematic Sunyaev-Zeldovich effect

Matilla

Haiman

2020

Phys. Rev. D

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The rotational kinematic Sunyaev-Zeldovich (rkSZ) signal, imprinted on the cosmic microwave background (CMB) by the gaseous halos (spinning "atmospheres") of foreground galaxies, would be a novel probe of galaxy formation. Although the signal is too weak to detect in individual galaxies, we analyze the feasibility of its statistical detection via stacking CMB data on many galaxies for which the spin orientation can be estimated spectroscopically. We use an "optimistic" model, in which fully ionized atmospheres contain the cosmic baryon fraction and spin at the halo's circular velocity vcirc, and a more realistic model, based on hydrodynamical simulations, with multi-phase atmospheres spinning at a fraction of vcirc. We incorporate realistic noise estimates into our analysis. Using low-redshift galaxy properties from the MaNGA spectroscopic survey (with median halo mass of 6.6 × 10 11 M ), and CMB data quality from Planck, we find that a 3σ detection would require a few×10 4 galaxies, even in the optimistic model. This is too high for current surveys, but upcoming higher-angular resolution CMB experiments will significantly reduce the requirements: stacking CMB data on galaxy spins in a ∼ 10 deg 2 can rule out the optimistic models, and ≈350 deg 2 will suffice for a 3σ detection with ACT. As a proof-of-concept, we stacked Planck data on the position of ≈ 2, 000 MaNGA galaxies, aligned with the galaxies' projected spin, and scaled to their halos' angular size. We rule out average temperature dipoles larger than ≈ 1.9 µK around field spiral galaxies.

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“…As shown in Table 1, the ratio of misaligned galaxies to counterrotators in quiescent merging/interacting sample is about 4:1, greater than the ratio in the whole quiescent sample (2:1 as discussed above). We think this is because during merging galaxy pairs transfer their orbital angular momentum into spin of remnant halo, and also of stars and gas (Di Matteo et al 2009;Codis et al 2012;Stewart 2017;Lagos et al 2018). In semi-analytic model, the spin direction of merger remnant is set as the orbital axis direction of merging galaxies in the last resolved moment (Stevens et al 2016).…”

Section: Quiescent Galaxiesmentioning

confidence: 99%

The impact of merging on the origin of kinematically misaligned and counter-rotating galaxies in MaNGA

Shi

Bizyaev

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy mergers and interactions are expected to play a significant role leading to offsets between gas and stellar motions in galaxies. Herein we crossmatch galaxies in MaNGA MPL-8 with the Dark Energy Spectroscopic Instrument (DESI) Legacy Surveys and identify 311 merging galaxies that have reliable measurements of the ΔPA, the difference between the stellar and gas kinematic position angles to investigate the impacts of merging on gas-stellar rotation misalignments. We find that the merging fractions of misaligned galaxies (30○ ≤ ΔPA <150○) are higher than that of co-rotators (ΔPA < 30○) in both quiescent and star-forming galaxies. This result suggests that merging is one process to produce kinematic misalignments. The merging fraction of counter-rotators (ΔPA ≤ 150○) is lower than that of misaligned galaxies in both quiescent and star-forming galaxies, while in the latter it is likely even lower than that of co-rotators. The orbital angular momentum transfer to the spins of stars and gas during merging and the tidal feature disappearance can lead to small merging fractions in counter-rotators. Numerous new stars that inherit angular momentum from gas after merging can further lower the merging fraction of star-forming counter-rotators.

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Gas Accretion and Angular Momentum

Cited by 15 publications

References 132 publications

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Probing gaseous galactic halos through the rotational kinematic Sunyaev-Zeldovich effect

The impact of merging on the origin of kinematically misaligned and counter-rotating galaxies in MaNGA

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