GEMS: The Surface Brightness and Surface Mass Density Evolution of Disk Galaxies

By M. Barden, Hans-Walter Rix, R. Somerville, Eric F. Bell, B. Häußler, C. Peng, A. Borch, S. Beckwith, J. Caldwell, Catherine Heymans and 7 more. 2005

198 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Global and Planetary Change, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4ca813b96c0eb8fac22f1c2cf6c5ad82c5ca4c49

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Global and Planetary Change

In Instrumentation

Citations in the corpus

Environmental effects on satellite galaxies: the link between concentration, size and colour profile (2008, result): “Such a scenario is for example supported by the findings of Barden et al. (2005) and Trujillo et al. (2006) who studied the stellar mass-size evolution for late type galaxies.”
Towards a more realistic population of bright spiral galaxies in cosmological simulations (2013, background): “This suggests that around z = 1 galaxies start to lie on the local relation (see also Barden et al. 2005).”
Galaxy And Mass Assembly (GAMA): mass–size relations of z < 0.1 galaxies subdivided by Sérsic index, colour and morphology (2014, background): “…University Press on behalf of the Royal Astronomical Society at U niversity of N ottingham on July 12, 2016 http://m nras.oxfordjournals.org/ 2604 R. Lange et al. (Driver 1999; La Barbera et al. 2003; Trujillo et al. 2004, 2006, 2007; Barden et al. 2005; Trujillo, Carrasco & Ferré-Mateu 2012).”
Early type galaxies have been the predominant morphological class for massive galaxies since only z~1 (2011, methodology): “Many studies (e.g. Shen et al. 2003; Barden et al. 2005; McIntosh et al. 2005; Trujillo et al. 2006) have used n=2.5 as a quantitative way to segregate between early and late-type galaxies.”
The STAGES view of red spirals and dusty red galaxies: Mass-dependent quenching of star formation in cluster infall (2008, background): “The time-scale for ram-pressure stripping though is tRPS ∝ rgal √ ρISMv −1 rel ∝ √ ρISMM∗ assuming constant surface mass density of disc galaxies (Barden et al. 2005) and equal infall velocity.”
Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging (2008, background): “Barden et al. 2005, ApJ, 635, 959 Bernardi M., Sheth R. K., Nichol R. C. et al., 2006, ApJ, 640, 241 Bertin E. & Arnouts S., 1996, A&AS, 117, 393 Boylan-Kolchin M., Ma C-P., Quataert E., 2006, MNRAS, 369, 1081 Bruzual G., Charlot S., 2003, MNRAS, 344, 1000 Bundy K. et al., 2006, ApJ, 651, 120…”
The effect of gas fraction on the morphology and time-scales of disc galaxy mergers (2009, background): “These galaxies also have higher star-formation rates per unit mass (Noeske et al. 2007) and similar or smaller effective radii (Barden et al. 2005; Melbourne et al. 2007) suggestive of higher gas densities than local disc galaxies.”
Strong size evolution of the most massive galaxies since z~2 (2007, methodology): “Interestingly, this trend of smaller sizes at redder bands dre(λ)/dlogλ=-0.6(±0.2) is in qualitative agreement to what is found in nearby galaxies -0.18>dre(λ)/dlogλ>-0.25 (Barden et al. 2005; McIntosh et al. 2005).”
A DEEP HUBBLE SPACE TELESCOPE H-BAND IMAGING SURVEY OF MASSIVE GAS-RICH MERGERS. II. THE QUEST QSOs (2006, methodology): “To make a bimodal decision based on a free Sérsic index n, we refer to studies both published (Barden et al. 2005; McIntosh et al. 2005) and unpublished (GEMS private communication, B. Häussler et al. 2006, private communication).”
Compact high-redshift galaxies are the cores of the most massive present-day spheroids (2009, background): “…this apparent evolution must be particular to this class of galaxies: disc E-mail: phopkins@astro.berkeley.edu †Canada Research Chair in Astrophysics. galaxies are not similarly compact at high redshift (Ferguson et al. 2004; Ravindranath et al. 2004; Barden et al. 2005; Somerville et al. 2008).”
THE RISE AND FALL OF PASSIVE DISK GALAXIES: MORPHOLOGICAL EVOLUTION ALONG THE RED SEQUENCE REVEALED BY COSMOS (2009, methodology): “A value of n = 2.5 has often been used to divide disks from spheroidals (e.g, Barden et al. 2005).”
A DIVERSITY OF PROGENITORS AND HISTORIES FOR ISOLATED SPIRAL GALAXIES (2012, methodology): “This idea is supported by observations (Barden et al. 2005; Maier et al. 2009), and it has already been seen in other simulations (Brooks et al. 2011) and semi-analytic models (Somerville et al. 2008; Firmani & Avila-Reese 2009; Dutton et al. 2010).”
The Millennium Galaxy Catalogue: bulge–disc decomposition of 10 095 nearby galaxies (2006, methodology): “Using Hubble Space Telescope imaging, several statistically significant samples of high-redshift galaxies with measured structural parameters have been constructed (e.g. Simard et al. 2002; Ravindranath et al. 2004; Barden et al. 2005).”
DETAILED DECOMPOSITION OF GALAXY IMAGES. II. BEYOND AXISYMMETRIC MODELS (2009, background): “…(e.g., Tully & Fisher 1977; Hinz et al. 2003; Bedregal et al. 2006), the evolution of disky galaxies (Simard et al. 2002; Ravindranath et al. 2004; Barden et al. 2005), the cosmic evolution of galaxy morphology (e.g., Lilly et al. 1998; Marleau & Simard 1998; Hathi et al. 2009) in both…”
The Fundamental Scaling Relations of Elliptical Galaxies (2005, background): “We note that the redshift-dependence of disk scale lengths agrees well with the distribution of disk scale lengths seen out to redshift z 1 (e.g., Ravindranath et al. 2004; Barden et al. 2005).”
GEMS: Galaxy Fitting Catalogs and Testing Parametric Galaxy Fitting Codes: GALFIT and GIM2D (2007, methodology): “Using such methods, the evolution of the structure of disk galaxies (Lilly 1998; Simard & Pritchet 1998; Ravindranath et al. 2004; Barden et al. 2005; Trujillo & Pohlen 2005; Sargent et al. 2006) and spheroid-dominated galaxies (e.g., Schade et al. 1997, 1999; McIntosh et al. 2005; Trujillo et al.…”
How Stellar Feedback Simultaneously Regulates Star Formation and Drives Outflows (2015, unknown): “…fromHopkins et al. (2010), Re(M⋆|z = 0) ≈ 5.28 kpc ( M⋆ 1010 M⊙ )0.25 , Re(M⋆, z) = Re(M⋆|z = 0)(1 + z)−0.6, (B3) which is based on a compilation of observations (Trujillo et al. 2004; Ravindranath et al. 2004; Ferguson et al. 2004; Barden et al. 2005; Toft et al. 2007; Akiyama et al. 2008).”