Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations of<i>z</i>= 0 bulges, discs and spheroids

We combine the latest spectrally stacked data of 21-cm emission from the ALFALFA survey with an updated version of the Dark Sage semi-analytic model to investigate the relative contributions of secular and environmental astrophysical processes on shaping the H i fractions and quiescence of galaxies in the local Universe. We calibrate the model to match the observed mean H i fraction of all galaxies as a function of stellar mass. Without consideration of stellar feedback, disc instabilities, and active galactic nuclei, we show how the slope and normalisation of this relation would change significantly. We find Dark Sage can reproduce the relative impact that halo mass is observed to have on satellites' H i fractions and quiescent fraction. However, the model satellites are systematically gas-poor. We discuss how this could be affected by satellite-central cross-contamination from the group-finding algorithm applied to the observed galaxies, but that it is not the full story. From our results, we suggest the anti-correlation between satellites' H i fractions and host halo mass, seen at fixed stellar mass and fixed specific star formation rate, can be attributed almost entirely to ram-pressure stripping of cold gas. Meanwhile, stripping of hot gas from around the satellites drives the correlation of quiescent fraction with halo mass at fixed stellar mass. Further detail in the modelling of galaxy discs' centres is required to solidify this result, however. We contextualise our results with those from other semi-analytic models and hydrodynamic simulations.

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“…Lange et al 2016). Galaxies that never suffered an instability in their existence, however, meet the observed relation quite precisely.…”

Section: Caveats Discussion and Conclusionmentioning

confidence: 55%

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Stevens

Brown

2017

Monthly Notices of the Royal Astronomical Society

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“…Combining the visual morphological classifications of GAMA sources with z0.06 presented by Kelvin et al (2014) and the bulge-disk decompositions of this sample presented by Lange et al (2016) and cross-matching with our samples using GAMA's unique source identifier, we find an average r-band B/T value of B/T=0.3 (0.18) in the high (low) stellar mass range of the FIELDGALAXY sample and a comparable value of B/T=0.32 (0.19) for those galaxies in the FIELDGALAXY parent sample visually classified as S0/SaSd/Irr. As fading will only act to increase the B/T ratio, we restrict ourselves to considering the high stellar mass range as our fiducial galaxy.…”

Section: Appendix a Selection Of Disk/spiral Galaxiesmentioning

confidence: 68%

“…Distribution of r-band B/T values for GAMA sources in the FIELDGALAXY (red) and FIELDGALAXY parent sample (gray) with z0.06 as determined by Lange et al (2016). Those members of the FIELDGALAXY parent sample visually classified (Kelvin et al 2014) as Sab-Sd/Irr galaxies are shown in blue, while the superset additionally including S0/Sa galaxies is shown in green.…”

Section: Appendix B Deriving Attenuation Correctionsmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): Gas Fueling of Spiral Galaxies in the Local Universe. I. The Effect of the Group Environment on Star Formation in Spiral Galaxies

Grootes

Tuffs

Popescu

et al. 2017

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We quantify the effect of the galaxy group environment (for group masses of 10 12.5 -1014.0 M e ) on the current star formation rate (SFR) of a pure, morphologically selected sample of disk-dominated (i.e., late-type spiral) galaxies with redshift 0.13. The sample embraces a full representation of quiescent and star-forming disks with stellar mass M * 10 9.5 M e . We focus on the effects on SFR of interactions between grouped galaxies and the putative intrahalo medium (IHM) of their host group dark matter halos, isolating these effects from those induced through galaxy-galaxy interactions, and utilizing a radiation transfer analysis to remove the inclination dependence of derived SFRs. The dependence of SFR on M * is controlled for by measuring offsets Δlog(ψ * ) of grouped galaxies about a single power-law relation in specific SFR,, exhibited by non-grouped "field" galaxies in the sample. While a small minority of the group satellites are strongly quenched, the group centrals and a large majority of satellites exhibit levels of ψ * statistically indistinguishable from their field counterparts, for all M * , albeit with a higher scatter of 0.44 dex about the field reference relation (versus 0.27 dex for the field). Modeling the distributions in Δlog(ψ * ), we find that (i) after infall into groups, disk-dominated galaxies continue to be characterized by a similar rapid cycling of gas into and out of their interstellar medium shown prior to infall, with inflows and outflows of ∼1.5-5 x SFR and ∼1-4 x SFR, respectively; and (ii) the independence of the continuity of these gas flow cycles on M * appears inconsistent with the required fueling being sourced from gas in the circumgalactic medium on scales of ∼100 kpc. Instead, our data favor ongoing fueling of satellites from the IHM of the host group halo on ∼Mpc scales, i.e., from gas not initially associated with the galaxies upon infall. Consequently, the color-density relation of the galaxy population as a whole would appear to be primarily due to a change in the mix of disk-and spheroid-dominated morphologies in the denser group environment compared to the field, rather than to a reduced propensity of the IHM in higher-mass structures to cool and accrete onto galaxies. We also suggest that the required substantial accretion of IHM gas by satellite disk-dominated galaxies will lead to a progressive reduction in the specific angular momentum of these systems, thereby representing an efficient secular mechanism to transform morphology from star-forming disk-dominated types to more passive spheroid-dominated types.

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“…The right panel shows the half-mass radius of stars, considering both the bulge and disk components, for disk-dominated, star forming galaxies only (sSF R > 0.3/t H , M bulge /M⋆ < 0.5). The diamonds with error bars and triangles in the middle panel are observed stellar disk sizes based on SDSS and GAMA (Dutton et al 2011;Lange et al 2016, half-light radius for disk only). The triangles are observed sizes based on GAMA data (Lange et al 2015, half-light radius for disk and bulge).…”

Section: Appendix B: Resolution Testsmentioning

confidence: 99%

H2-based star formation laws in hierarchical models of galaxy formation

Xie

Lucia

Hirschmann

et al. 2017

Monthly Notices of the Royal Astronomical Society

101

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We update our recently published model for GAlaxy Evolution and Assembly (GAEA), to include a self-consistent treatment of the partition of cold gas in atomic and molecular hydrogen. Our model provides significant improvements with respect to previous ones used for similar studies. In particular, GAEA (i) includes a sophisticated chemical enrichment scheme accounting for non-instantaneous recycling of gas, metals, and energy; (ii) reproduces the measured evolution of the galaxy stellar mass function; (iii) reasonably reproduces the observed correlation between galaxy stellar mass and gas metallicity at different redshifts. These are important prerequisites for models considering a metallicity dependent efficiency of molecular gas formation. We also update our model for disk sizes and show that model predictions are in nice agreement with observational estimates for the gas, stellar and star forming disks at different cosmic epochs. We analyse the influence of different star formation laws including empirical relations based on the hydrostatic pressure of the disk, analytic models, and prescriptions derived from detailed hydrodynamical simulations. We find that modifying the star formation law does not affect significantly the global properties of model galaxies, neither their distributions. The only quantity showing significant deviations in different models is the cosmic molecular-to-atomic hydrogen ratio, particularly at high redshift. Unfortunately, however, this quantity also depends strongly on the modelling adopted for additional physical processes. Useful constraints on the physical processes regulating star formation can be obtained focusing on low mass galaxies and/or at higher redshift. In this case, self-regulation has not yet washed out differences imprinted at early time.

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Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

Abstract: We perform automated bulge + disc decomposition on a sample of ∼7500 galaxies from the Galaxy And Mass Assembly (GAMA) survey in the redshift range of 0.002 Show more

Cited by 120 publications

References 112 publications

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Galaxy And Mass Assembly (GAMA): Gas Fueling of Spiral Galaxies in the Local Universe. I. The Effect of the Group Environment on Star Formation in Spiral Galaxies

H2-based star formation laws in hierarchical models of galaxy formation

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