Evidence for the inside-out growth of the stellar mass distribution in galaxy clusters sincez~1

Abstract We constrain the mass distribution in nearby, star-forming galaxies with the Star Formation Reference Survey (SFRS), a galaxy sample constructed to be representative of all known combinations of star formation rate (SFR), dust temperature, and specific star formation rate (sSFR) that exist in the Local Universe. An innovative two-dimensional bulge/disk decomposition of the 2MASS/Ks-band images of the SFRS galaxies yields global luminosity and stellar mass functions, along with separate mass functions for their bulges and disks. These accurate mass functions cover the full range from dwarf galaxies to large spirals, and are representative of star-forming galaxies selected based on their infra-red luminosity, unbiased by AGN content and environment. We measure an integrated luminosity density j = 1.72 ± 0.93 × 109 L⊙ h−1 Mpc−3 and a total stellar mass density ρM = 4.61 ± 2.40 × 108 M⊙ h−1 Mpc−3. While the stellar mass of the average star-forming galaxy is equally distributed between its sub-components, disks globally dominate the mass density budget by a ratio 4:1 with respect to bulges. In particular, our functions suggest that recent star formation happened primarily in massive systems, where they have yielded a disk stellar mass density larger than that of bulges by more than 1 dex. Our results constitute a reference benchmark for models addressing the assembly of stellar mass on the bulges and disks of local (z = 0) star-forming galaxies.

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

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315003440 ◽

2014 ◽

Vol 10 (S311) ◽

pp. 82-85 ◽

Cited By ~ 6

Author(s):

Jonathan Sick ◽

Stephane Courteau ◽

Jean-Charles Cuillandre ◽

Julianne Dalcanton ◽

Roelof de Jong ◽

...

Keyword(s):

Stellar Population ◽

Spectral Energy Distribution ◽

Major Axis ◽

Stellar Mass ◽

Spectral Energy ◽

Population Synthesis ◽

Disk Formation ◽

Infrared Spectral ◽

Inside Out ◽

Additional Constraints

AbstractOur 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/Li*) 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/Li* 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 × 1010 M⊙ for the M31 bulge and disk.

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Relative distribution of dark matter and stellar mass in three massive galaxy clusters

Astronomy and Astrophysics ◽

10.1051/0004-6361/201425122 ◽

2015 ◽

Vol 575 ◽

pp. A108 ◽

Cited By ~ 8

Author(s):

S. Andreon

Keyword(s):

Dark Matter ◽

Galaxy Clusters ◽

Stellar Mass ◽

Relative Distribution ◽

Massive Galaxy

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The Variation of Gas Mass Distribution in Galaxy Clusters: Effects of Preheating and Shocks

The Astrophysical Journal ◽

10.1086/308982 ◽

2000 ◽

Vol 536 (2) ◽

pp. 523-530 ◽

Cited By ~ 16

Author(s):

Yutaka Fujita ◽

Fumio Takahara

Keyword(s):

Galaxy Clusters ◽

Mass Distribution

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Characterization of Omega-WINGS galaxy clusters

Astronomy and Astrophysics ◽

10.1051/0004-6361/201731605 ◽

2018 ◽

Vol 609 ◽

pp. A133 ◽

Cited By ~ 5

Author(s):

S. Cariddi ◽

M. D’Onofrio ◽

G. Fasano ◽

B. M. Poggianti ◽

A. Moretti ◽

...

Keyword(s):

Galaxy Clusters ◽

Cluster Formation ◽

Stellar Mass ◽

Nearby Galaxy ◽

Observable Universe ◽

Cluster Galaxy ◽

Growth Profiles ◽

First Time ◽

Integrated Luminosity ◽

Mass Profiles

Context. Galaxy clusters are the largest virialized structures in the observable Universe. Knowledge of their properties provides many useful astrophysical and cosmological information. Aims. Our aim is to derive the luminosity and stellar mass profiles of the nearby galaxy clusters of the Omega-WINGS survey and to study the main scaling relations valid for such systems. Methods. We merged data from the WINGS and Omega-WINGS databases, sorted the sources according to the distance from the brightest cluster galaxy (BCG), and calculated the integrated luminosity profiles in the B and V bands, taking into account extinction, photometric and spatial completeness, K correction, and background contribution. Then, by exploiting the spectroscopic sample we derived the stellar mass profiles of the clusters. Results. We obtained the luminosity profiles of 46 galaxy clusters, reaching r200 in 30 cases, and the stellar mass profiles of 42 of our objects. We successfully fitted all the integrated luminosity growth profiles with one or two embedded Sérsic components, deriving the main clusters parameters. Finally, we checked the main scaling relation among the clusters parameters in comparison with those obtained for a selected sample of early-type galaxies (ETGs) of the same clusters. Conclusions. We found that the nearby galaxy clusters are non-homologous structures such as ETGs and exhibit a color–magnitude (CM) red-sequence relation very similar to that observed for galaxies in clusters. These properties are not expected in the current cluster formation scenarios. In particular the existence of a CM relation for clusters, shown here for the first time, suggests that the baryonic structures grow and evolve in a similar way at all scales.

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