Stellar mass functions of galaxies, discs and spheroids at<i>z</i>∼ 0.1

Thanjavur, Karun; Simard, Luc; Bluck, Asa F. L.; Mendel, J. Trevor

doi:10.1093/mnras/stw495

Cited by 47 publications

(87 citation statements)

References 113 publications

(141 reference statements)

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“…The overall mass dependence and slope of the relations are similar. At higher masses (M > 10 10 M ), we find that TNG is in good agreement with the GAMA data, with more massive galaxies having a higher S/T (also consistent with findings by, e.g., Thanjavur et al 2016). The large error-bars at the high-mass end in the observations can be understood by the small volume probed by GAMA, which implies poorer sampling of relatively rare high-mass galaxies (Bernardi et al 2013).…”

Section: Comparison With Observationssupporting

confidence: 89%

Morphology and star formation in IllustrisTNG: the build-up of spheroids and discs

Tacchella

Diemer

Hernquist

et al. 2019

Monthly Notices of the Royal Astronomical Society

185

154

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Using the IllustrisTNG simulations, we investigate the connection between galaxy morphology and star formation in central galaxies with stellar masses in the range 10 9 − 10 11.5 M . We quantify galaxy morphology by a kinematical decomposition of the stellar component into a spheroidal and a disc component (spheroid-to-total ratio, S/T) and by the concentration of the stellar mass density profile (C 82 ). S/T is correlated with stellar mass and star-formation activity, while C 82 correlates only with stellar mass. Overall, we find good agreement with observational estimates for both S/T and C 82 . Low-and high-mass galaxies are dominated by random stellar motion, while only intermediate-mass galaxies (M ≈ 10 10 − 10 10.5 M ) are dominated by ordered rotation. Whereas higher mass galaxies are typical spheroids with high concentrations, lower-mass galaxies have low concentration, pointing to different formation channels. Although we find a correlation between S/T and star-formation activity, in the TNG model galaxies do not necessarily change their morphology when they transition through the green valley or when they cease their star formation, this depending on galaxy stellar mass and morphological estimator. Instead, the morphology (S/T and C 82 ) is generally set during the star-forming phase of galaxies. The apparent correlation between S/T and star formation arises because earlier forming galaxies had, on average, a higher S/T at a given stellar mass. Furthermore, we show that mergers drive in-situ bulge formation in intermediate-mass galaxies and are responsible for the recent spheroidal mass assembly in the massive galaxies with M > 10 11 M . In particular, these massive galaxies assemble about half of the spheroidal mass while star-forming and the other half through mergers while quiescent.

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Section: Comparison With Observationssupporting

confidence: 89%

Morphology and star formation in IllustrisTNG: the build-up of spheroids and discs

Tacchella

Diemer

Hernquist

et al. 2019

Monthly Notices of the Royal Astronomical Society

185

154

View full text Add to dashboard Cite

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“…With the possible exception of the highest galaxy masses, both expressions agree well with determinations by other groups (see Fig. 7 in [40] and Fig. 6 in [41]).…”

Section: B Galaxy Merger Ratesupporting

confidence: 87%

“…For the galaxy (stellar) mass function φ(M gal , z), we adopt the analytic expressions of [40] (Schechter fit) for z ≤ 0.2 and [14] (double Schechter fit) for z > 0.2. With the possible exception of the highest galaxy masses, both expressions agree well with determinations by other groups (see Fig.…”

Section: B Galaxy Merger Ratementioning

confidence: 99%

Evolution of massive black hole binaries in rotating stellar nuclei: Implications for gravitational wave detection

Rasskazov

Merritt

2017

Phys. Rev. D

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We compute the isotropic gravitational wave (GW) background produced by binary supermassive black holes (SBHs) in galactic nuclei. In our model, massive binaries evolve at early times via gravitational-slingshot interaction with nearby stars, and at later times by the emission of GWs. Our expressions for the rate of binary hardening in the "stellar" regime are taken from the recent work of Vasiliev et al., who show that in the non-axisymmetric galaxies expected to form via mergers, stars are supplied to the center at high enough rates to ensure binary coalescence on Gyr timescales. We also include, for the first time, the extra degrees of freedom associated with evolution of the binary's orbital plane; in rotating nuclei, interaction with stars causes the orientation and the eccentricity of a massive binary to change in tandem, leading in some cases to very high eccentricities (e > 0.9) before the binary enters the GW-dominated regime. We argue that previous studies have overestimated the mean ratio of SBH mass to galaxy bulge mass by factors of 2 -3. In the frequency regime currently accessible to pulsar timing arrays (PTAs), our assumptions imply a factor 2 -3 reduction in the characteristic strain compared with the values computed in most recent studies, removing the tension that currently exists between model predictions and the non-detection of GWs.

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“…Hence, if Earth had been randomly drawn from the cosmological population of TPs, the most likely outcome would have been for it not to be located in a Milky Way-type system, but in an elliptical. While many spheroid-dominated galaxies do contain a disk component, and vice versa, TPs in disks remain in minority even when the estimated stellar mass fractions in bona fide disks and spheroids (Moffett et al 2016b;Thanjavur et al 2016) are considered.…”

Section: Why Are We Not Living In An Elliptical Galaxy?mentioning

confidence: 99%

Terrestrial Planets Across Space and Time

Zackrisson

Calissendorff

Gonzalez

et al. 2016

ApJ

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The study of cosmology, galaxy formation and exoplanets has now advanced to a stage where a cosmic inventory of terrestrial planets may be attempted. By coupling semi-analytic models of galaxy formation to a recipe that relates the occurrence of planets to the mass and metallicity of their host stars, we trace the population of terrestrial planets around both solar-mass (FGK type) and lowermass (M dwarf) stars throughout all of cosmic history. We find that the mean age of terrestrial planets in the local Universe is 7 ± 1 Gyr for FGK hosts and 8 ± 1 Gyr for M dwarfs. We estimate that hot Jupiters have depleted the population of terrestrial planets around FGK stars by no more than ≈ 10%, and that only ≈ 10% of the terrestrial planets at the current epoch are orbiting stars in a metallicity range for which such planets have yet to be confirmed. The typical terrestrial planet in the local Universe is located in a spheroid-dominated galaxy with a total stellar mass comparable to that of the Milky Way. When looking at the inventory of planets throughout the whole observable Universe, we argue for a total of ≈ 1×1019 and ≈ 5×10 20 terrestrial planets around FGK and M stars, respectively. Due to light travel time effects, the terrestrial planets on our past light cone exhibit a mean age of just 1.7 ± 0.2 Gyr. These results are discussed in the context of cosmic habitability, the Copernican principle and searches for extraterrestrial intelligence at cosmological distances.

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Stellar mass functions of galaxies, discs and spheroids atz∼ 0.1

Cited by 47 publications

References 113 publications

Morphology and star formation in IllustrisTNG: the build-up of spheroids and discs

Morphology and star formation in IllustrisTNG: the build-up of spheroids and discs

Evolution of massive black hole binaries in rotating stellar nuclei: Implications for gravitational wave detection

Terrestrial Planets Across Space and Time

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