Letter by Cappellari et al Regarding Article, “Statin Therapy and Outcome After Ischemic Stroke: Systematic Review and Meta-analysis of Observational Studies and Randomized Trials”

Cappellari, Manuel; Moretto, Giuseppe; Bovi, Paolo

doi:10.1161/strokeaha.113.001207

Cited by 345 publications

(845 citation statements)

References 4 publications

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“…Metallicities at large radii for both stars and globular clusters have been obtained from the CaT index. For the innermost radii, we adopt stellar metallicities from SAURON (Bacon et al 2001) and ATLAS 3D (Cappellari et al 2011) surveys for the galaxies in common. Combining SAURON, ATLAS 3D and SLUGGS values, we have been able to spectroscopically measure the metallicity of the stellar component out to almost 4 Re, and of the red and blue globular clusters out to almost 15 Re.…”

Section: Discussionmentioning

confidence: 99%

The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

Pastorello

Forbes

Usher

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The outer halo regions of early-type galaxies carry key information about their past accretion history. However, spectroscopically probing the stellar component at such galactocentric radii is still challenging. Using Keck/DEIMOS, we have been able to measure the metallicities of the stellar and globular cluster components in 12 early-type galaxies out to more than 10 R e . We find similar metallicity gradients for the metalpoor and metal-rich globular cluster subpopulations, suggesting a common formation process for the two subpopulations. This is in conflict with most current theoretical predictions, where the metal-poor globular clusters are thought to be purely accreted and metal-rich globular clusters mostly formed in-situ. Moreover, we find that the globular cluster metallicity gradients show a trend with galaxy mass, being steeper in lower-mass galaxies than in higher-mass galaxies. This is similar to what we find for the outermost galaxy stars and suggests a more active accretion history, with a larger role played by major mergers, in the most massive galaxies. This conclusion is qualitatively consistent with expectations from two-phase galaxy assembly models. Finally, we find that the small difference in metallicity between galaxy stars and metal-rich globular clusters at 1 R e may correlate with galaxy mass. The origin of this difference is not currently clear.

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Section: Discussionmentioning

confidence: 99%

The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

Pastorello

Forbes

Usher

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…This is surprising since the current theory is that slow rotators are more likely to be the central galaxy of a group or cluster, whereas fast rotators are more likely to be satellite galaxies (Cappellari et al 2011;D'Eugenio et al 2013;Houghton et al 2013;Scott et al 2014). However, the MaNGA sample was chosen to be agnostic to galaxy environment, giving rise to a representative distribution of galaxy environments.…”

Section: Environmental Densitiesmentioning

confidence: 92%

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

Smethurst

Masters

Lintott

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Do the theorised different formation mechanisms of fast and slow rotators produce an observable difference in their star formation histories? To study this we identify quenching slow rotators in the MaNGA sample by selecting those which lie below the star forming sequence and identify a sample of quenching fast rotators which were matched in stellar mass. This results in a total sample of 194 kinematically classified galaxies, which is agnostic to visual morphology. We use u − r and N U V − u colours from SDSS and GALEX and an existing inference package, starpy, to conduct a first look at the onset time and exponentially declining rate of quenching of these galaxies. An Anderson-Darling test on the distribution of the inferred quenching rates across the two kinematic populations reveals they are statistically distinguishable (3.2σ). We find that fast rotators quench at a much wider range of rates than slow rotators, consistent with a wide variety of physical processes such as secular evolution, minor mergers, gas accretion and environmentally driven mechanisms. Quenching is more likely to occur at rapid rates (τ ∼ < 1 Gyr) for slow rotators, in agreement with theories suggesting slow rotators are formed in dynamically fast processes, such as major mergers. Interestingly, we also find that a subset of the fast rotators quench at these same rapid rates as the bulk of the slow rotator sample. We therefore discuss how the total gas mass of a merger, rather than the merger mass ratio, may decide a galaxy's ultimate kinematic fate.

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“…Finally, we conclude in Section 6. Throughout this paper we assume a distance of 11.4±1.1 Mpc for NGC4697 (Cappellari et al 2011), as derived from surface brightness fluctuation measurements in Tonry et al (2001). At this distance one arcsecond corresponds to a physical scale of 55 pc.…”

Section: Introductionmentioning

confidence: 99%

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

Davis

Bureau

Onishi

et al. 2017

Monthly Notices of the Royal Astronomical Society

106

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As part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project, we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotating early-type galaxy NGC4697. This estimate is based on Atacama Large Millimeter/submillimeter Array (ALMA) cycle-3 observations of the 12 CO(2-1) emission line with a linear resolution of 29 pc (0. 53). We find that NGC4697 hosts a small relaxed central molecular gas disc with a mass of 1.6×10 7 M , co-spatial with the obscuring dust disc visible in optical Hubble Space Telescope (HST) imaging. We also resolve thermal 1 mm continuum emission from the dust in this disc. NGC4697 is found to have a very low molecular gas velocity dispersion, σ gas =1.65 +0.68 −0.65 km s −1 . This seems to be partially because the giant molecular cloud mass function is not fully sampled, but other mechanisms such as chemical differentiation in a hard radiation field or morphological quenching also seem to be required. We detect a Keplerian increase of the rotation of the molecular gas in the very centre of NGC4697, and use forward modelling of the ALMA data cube in a Bayesian framework with the KIN-EMATIC MOLECULAR SIMULATION (KINMS) code to estimate a SMBH mass of (1.3 +0.18 −0.17 ) ×10 8 M and an i-band mass-to-light ratio of 2.14 +0.04 −0.05 M /L (at the 99% confidence level). Our estimate of the SMBH mass is entirely consistent with previous measurements from stellar kinematics. This increases confidence in the growing number of SMBH mass estimates being obtained in the ALMA era.

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Letter by Cappellari et al Regarding Article, “Statin Therapy and Outcome After Ischemic Stroke: Systematic Review and Meta-analysis of Observational Studies and Randomized Trials”

Cited by 345 publications

References 4 publications

The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

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