Galaxy masses

Courteau, Stéphane; Cappellari, Michele; Jong, Roelof S. de; Dutton, Aaron A.; Emsellem, Éric; Hoekstra, Henk; Koopmans, L. V. E.; Mamon, G. A.; Maraston, Claudia; Treu, Tommaso; Widrow, Lawrence M.

doi:10.1103/revmodphys.86.47

Cited by 288 publications

(278 citation statements)

References 651 publications

(68 reference statements)

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“…In the same way that the radii of discs are computed by assuming that the infall of gas conserves angular momentum, the radii of bulges are computed by assuming that mergers conserve the total mechanical energy of the merging galaxies. Accounting for systematic departures of observed galaxies from the Hernquist model (Cappellari et al 2006;Courteau et al 2014), this assumption is in reasonably good agreement with observations of the FJR (Cappellari et al 2013), although it tends to underestimate the velocity dispersions of lowermass ellipticals. This tendency can be explained as an effect of dissipation, which plays an important role in major mergers at Mstars < 10 11 M⊙ but not in major mergers at larger masses Bernardi et al 2011;Cattaneo et al 2011).…”

Section: Resultssupporting

confidence: 75%

“…It has the advantage that its total mass, gravitational potential and velocity dispersion can be computed analytically, but there is no physical reason why galaxies should follow it. In fact, systematic departures from C = 3.31 are observed (Cappellari et al 2013;Courteau et al 2014). We therefore treat C as a parameter of the model to be constrained by observations.…”

Section: Mergersmentioning

confidence: 99%

See 1 more Smart Citation

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

Cattaneo

Blaizot

Devriendt

et al. 2017

Monthly Notices of the Royal Astronomical Society

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GalICS 2.0 is a new semianalytic code to model the formation and evolution of galaxies in a cosmological context. N-body simulations based on a Planck cosmology are used to construct halo merger trees, track subhaloes, compute spins and measure concentrations. The accretion of gas onto galaxies and the morphological evolution of galaxies are modelled with prescriptions derived from hydrodynamic simulations. Star formation and stellar feedback are described with phenomenological models (as in other semianalytic codes). GalICS 2.0 computes rotation speeds from the gravitational potential of the dark matter, the disc and the central bulge. As the rotation speed depends not only on the virial velocity but also on the ratio of baryons to dark matter within a galaxy, our calculation predicts a different Tully-Fisher relation from models in which v rot ∝ v vir . This is why GalICS 2.0 is able to reproduce the galaxy stellar mass function and the Tully-Fisher relation simultaneously. Our results are also in agreement with halo masses from weak lensing and satellite kinematics, gas fractions, the relation between star formation rate (SFR) and stellar mass, the evolution of the cosmic SFR density, bulge-to-disc ratios, disc sizes and the Faber-Jackson relation.

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Section: Resultssupporting

confidence: 75%

Section: Mergersmentioning

confidence: 99%

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

Cattaneo

Blaizot

Devriendt

et al. 2017

Monthly Notices of the Royal Astronomical Society

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show abstract

“…By comparison, we have also plotted mass-to-light ratios predicted by three colour-M/L * relations (Zibetti et al 2009;Taylor et al 2011;Into & Portinari 2013). These fits systematically vary by 0.3 dex, far larger than the 0.1 dex of internal systematic uncertainty typically claimed by g − i -M/L * fits Courteau et al (2014). Compared to our full SED fits, modelling of the gi SED is less biased than these other M/L * fits, which are based on other stellar population synthesis models.…”

Section: Sed Stellar Mass Modellingmentioning

confidence: 93%

The Stellar Mass of M31 as inferred by the Andromeda Optical & Infrared Disk Survey

Sick

Courteau

Cuillandre³

et al. 2014

Proc. IAU

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Abstract. Our proximity and external vantage point make M31 an ideal testbed for understanding the structure of spiral galaxies. The Andromeda Optical and Infrared Disk Survey (ANDROIDS) has mapped M31's bulge and disk out to R=40 kpc in ugriJKs bands with CFHT using a careful sky calibration. We use Bayesian modelling of the optical-infrared spectral energy distribution (SED) to estimate profiles of M31's stellar populations and mass along the major axis. This analysis provides evidence for inside-out disk formation and a declining metallicity gradient. M31's i-band mass-to-light ratio (M/L * i ) decreases from 0.5 dex in the bulge to ∼ 0.2 dex at 40 kpc. The best-constrained stellar population models use the full ugriJKs SED but are also consistent with optical-only fits. Therefore, while NIR data can be successfully modelled with modern stellar population synthesis, NIR data do not provide additional constraints in this application. Fits to the gi-SED alone yield M/L * i that are systematically lower than the full SED fit by 0.1 dex. This is still smaller than the 0.3 dex scatter amongst different relations for M/Li via g − i colour found in the literature. We advocate a stellar mass of M * (30 kpc) = 10.3 +2.3 −1.7 × 10 10 M for the M31 bulge and disk.

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“…Fardal et al 2013;Cautun et al 2014a,b;González, Kravtsov & Gnedin 2014;Piffl et al 2014;Veljanoski et al 2014, for a compilation of other measurements and discussions of systematic effects see Courteau et al 2014;Wang et al 2015). This results in 2849 MS-II haloes and in 63 COCO haloes in the required mass range.…”

Section: Data a N D S A M P L E S E L E C T I O Nmentioning

confidence: 94%

Planes of satellite galaxies: when exceptions are the rule

Cautun¹,

Bose²,

Frenk³

et al. 2015

Mon. Not. R. Astron. Soc.

100

114

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The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model (ΛCDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of the MW and M31 planes in ΛCDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high resolution cosmological simulations. We find that planar structures are very common, and that ∼10% of ΛCDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and ΛCDM predictions. In fact, ∼10% of ΛCDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.

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Galaxy masses

Cited by 288 publications

References 651 publications

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

The Stellar Mass of M31 as inferred by the Andromeda Optical & Infrared Disk Survey

Planes of satellite galaxies: when exceptions are the rule

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