The SAMI Galaxy Survey: mass–kinematics scaling relations

Barat, Dilyar; D’Eugenio, Francesco; Colless, Matthew; Brough, Sarah; Catinella, Barbara; Cortese, Luca; Croom, S. M.; Medling, Anne M.; Oh, Sree; Sande, Jesse van de; Sweet, Sarah M.; Yi, Sukyoung K.; Bland-Hawthorn, Joss; Bryant, Julia J.; Goodwin, Michael; Groves, Brent; Lawrence, Jon; Owers, Matt S.; Richards, Samuel N.; Scott, Nicholas

doi:10.1093/mnras/stz1439

Cited by 34 publications

(29 citation statements)

References 51 publications

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“…The correlations between these characteristic measures of size, mass, and velocity are typically considered separately for ellipticals and spirals, although this is starting to change with the advent of integral field unit surveys, which have encouraged the use of more sophisticated kinematic measures (de Zeeuw et al 2002;Cappellari et al 2006;Weiner et al 2006;Kassin et al 2007;Cortese et al 2014;Barat et al 2019;Aquino-Ortíz et al 2020). Still, considering E and S galaxies separately seems justified (see e.g., Ouellette et al 2017), not only because their velocity metrics and morphologies differ, but also because they occupy rather distinct regions in mass-velocity-size space.…”

Section: Introductionmentioning

confidence: 99%

A unified scenario for the origin of spiral and elliptical galaxy structural scaling laws

Ferrero

Navarro

Abadi

et al. 2021

A&A

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Elliptical (E) and spiral (S) galaxies follow tight, but different, scaling laws that link their stellar masses, radii, and characteristic velocities. Mass and velocity, for example, scale tightly in spirals with little dependence on galaxy radius (the ‘Tully-Fisher relation’; TFR). On the other hand, ellipticals appear to trace a 2D surface in size-mass-velocity space (the ‘Fundamental Plane’; FP). Over the years, a number of studies have attempted to understand these empirical relations, usually in terms of variations of the virial theorem for E galaxies and in terms of the scaling relations of dark matter halos for spirals. We use Lambda cold dark matter (ΛCDM) cosmological hydrodynamical simulations to show that the scaling relations of both ellipticals and spirals arise as the result of (i) a tight galaxy mass–dark halo mass relation and (ii) the self-similar mass profile of cold dark matter halos. In this interpretation, E and S galaxies of a given stellar mass inhabit halos of similar masses, and their different scaling laws result from the varying amounts of dark matter enclosed within their luminous radii. This scenario suggests a new galaxy distance indicator applicable to galaxies of all morphologies and provides simple and intuitive explanations for long-standing puzzles, such as why the TFR is independent of surface brightness, or what causes the ‘tilt’ in the FP. Our results provide strong support for the predictions of ΛCDM in the strongly non-linear regime, as well as guidance for further improvements to cosmological simulations of galaxy formation.

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Section: Introductionmentioning

confidence: 99%

A unified scenario for the origin of spiral and elliptical galaxy structural scaling laws

Ferrero

Navarro

Abadi

et al. 2021

A&A

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“…1) We show that galaxies of all types lie on a plane relating mass, angular momentum and stellar-light distribution (Cortese et al 2016), 2) and that there is a relation between stellar population age and intrinsic ellipticity (van de Sande et al 2018). 3) By measuring the S 0.5 parameter, we demonstrate that we bring together the gas and stellar kinematic measurements of galaxies with all morphologies onto a single dynamical scaling relation (Barat et al 2019). 4) With high-order stellar kinematic measurements, we determine that galaxies with similar λ Re -ε e values can show different h 3 − V /σ signatures, which can be linked to their assembly history by comparing to zoom-in simulations (van de Sande et al 2017).…”

Section: Resultsmentioning

confidence: 68%

“…The S 0.5 parameter, derived from the velocity and velocity dispersion such that S K = KV 2 rot + σ 2 , is a useful quantity that can unify the stellar and gas kinematic measurements of galaxies with all morphological types onto a single dynamical scaling relation (Weiner et al 2006;Kassin et al 2007;Cortese et al 2014). The log(M /M ) − log S 0.5 relation is explored in detail in Barat et al (2019) who use the SAMI Galaxy Survey to probe this relation down to low-stellar masses (log(M /M ) < 9; see Fig. 2).…”

Section: The Build-up Of Mass and Angular Momentum In Galaxies Acrossmentioning

confidence: 99%

“…However, the sample limits occur at different stellar masses for the gas and stellar measurements, which implies that the apparent non-linearity in the relation is not physical. Barat et al (2019) also empirically test the impact of changing the value of K in the S K parameter. By measuring the scatter in log(M /M ) − log S K as a function of K for both gas and stars, they find that the optimal value of K is between 0.2 and 0.7 for samples containing only early-type galaxies or mixtures of early and late-type galaxies.…”

Section: The Build-up Of Mass and Angular Momentum In Galaxies Acrossmentioning

confidence: 99%

“…log(M /M ) − log S0.5 scaling relations for stars (panel a) and gas (panel b) (from(Barat et al 2019),Fig. 4).…”

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confidence: 99%

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Key dynamical results from the SAMI Galaxy Survey

et al. 2019

Self Cite

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We present an overview of recent key results from the SAMI Galaxy Survey on the build-up of mass and angular momentum in galaxies across morphology and environment. The SAMI Galaxy survey is a multi-object integral field spectroscopic survey and provides a wealth of spatially-resolved, two-dimensional stellar and gas measurements for galaxies of all morphological types, with high-precision due the stable spectral resolution of the AAOmega spectrograph. The sample size of ~3000 galaxies allows for dividing the sample in bins of stellar mass, environment, and star-formation or morphology, whilst maintaining a statistical significant number of galaxies in each bin. By combining imaging, spatially resolved dynamics, and stellar population measurements, our result demonstrate the power of utilising integral field spectroscopy on a large sample of galaxies to further our understanding of physical processes involved in the build-up of stellar mass and angular momentum in galaxies.

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WALLABY – an SKA Pathfinder H i survey

Koribalski

Staveley‐Smith

Westmeier

et al. 2020

Astrophys Space Sci

201

125

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The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (H I) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 × 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radioquiet zone in Western Australia. WALLABY aims to survey three-quarters of the sky (−90 • < δ < +30 • ) to a redshift of z 0.26, and generate spectral line image cubes at ∼30 arcsec resolution and ∼1.6 mJy beam −1 per 4 km s −1 channel sensitivity. ASKAP's instantaneous field of view at 1.4 GHz, delivered by the PAF's 36 beams, is about 30 sq deg. At an integrated signal-to-noise ratio of five, WALLABY is expected to detect around half a million galaxies with a mean redshift of z ∼ 0.05 (∼200 Mpc). The scientific goals of WALLABY include: (a) a census of gas-rich galaxies in the vicinity of the Local Group; (b) a study of the H I properties of galaxies, groups and clusters, in particular the influence of the environment on galaxy evolution; and (c) the refinement of cosmological parameters using the spatial and redshift distribution of low-bias gas-rich galaxies. For context we provide an overview of recent and planned large-scale H I surveys. Combined with existing and new multi-wavelength sky surveys, WALLABY will enable an exciting new generation of panchromatic studies of the Local Universe. -First results from the WALLABY pilot survey are revealed, with initial data products publicly available in the CSIRO ASKAP Science Data Archive (CASDA).

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The SAMI Galaxy Survey: mass–kinematics scaling relations

Cited by 34 publications

References 51 publications

A unified scenario for the origin of spiral and elliptical galaxy structural scaling laws

A unified scenario for the origin of spiral and elliptical galaxy structural scaling laws

Key dynamical results from the SAMI Galaxy Survey

WALLABY – an SKA Pathfinder H i survey

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