Galaxy Groups in the Third Data Release of the Sloan Digital Sky Survey

By M. Merchán, A. Zandivarez. 2004

133 citations recorded by the source corpus.

We present a new sample of galaxy groups identified in the Sloan Digital Sky Survey Data Release 3. Following previous works, we use the well-tested friends-of-friends algorithm developed by Huchra and Geller, which takes into account the number density variation due to the apparent magnitude limit of the galaxy catalog. To improve the identification, we implement a procedure to avoid the artificial merging of small systems in high-density regions and then apply an iterative method to recompute the group centers position. As a result, we obtain a new catalog with 10,864 galaxy groups with at least four members. The final group sample has a mean redshift of 0.1 and a median velocity dispersion of 230 km s-1.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7f8e534370bea72103b3d2fb399f40d8157a9150

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Citations in the corpus

Galaxy Groups in the SDSS DR4. I. The Catalog and Basic Properties (2007, methodology): “…group finder of Yang et al. (2005a) to identify groups in the New York University Value-Added Galaxy Catalogue (NYUVAGC) of Blanton et al. (2005) which is also based on the SDSS DR2, and Merchán & Zandivarez (2005) used a FOF algorithm to identify groups in the SDSS DR3 (Abazajian et al. 2005).”
Percolation Galaxy Groups and Clusters in the SDSS Redshift Survey: Identification, Catalogs, and the Multiplicity Function (2006, methodology): “Merchán & Zandivarez (2005) used a friends-of-friends algorithm to identify groups in the SDSS Data Release 3 (DR3; Abazajian et al. 2005a).”
GALAXY CLUSTERS IDENTIFIED FROM THE SDSS DR6 AND THEIR PROPERTIES (2009, methodology): “…(2002), Eke et al. (2004), and Yang et al. (2005) for the two-degree field Galaxy Redshift Survey (2dfGRS), Gerke et al. (2005) for the DEEP2 Galaxy Redshift Survey, and Merchán & Zandivarez (2005), Berlind et al. (2006), Yang et al. (2007), Deng et al. (2007), and Tago et al. (2008) for the SDSS.”
Observational probes of cosmic acceleration (2012, background): “2 (Merchán and Zandivarez, 2002; Kochanek et al., 2003; Miller et al., 2005; Merchán and Zandivarez, 2005; Berlind et al., 2006; Yang et al., 2007; Li and Yee, 2008; Blackburne and Kochanek, 2011), though high redshift spectroscopic catalogs do exist (Gerke et al.”
Groups of Galaxies in the Two Micron All Sky Redshift Survey (2006, methodology): “For comparison, we also show the velocity dispersions of groups in Sloan Digital Sky Survey Data Release 3 (SDSSDR3, Merchán & Zandivarez 2005).”
On the efficiency and reliability of cluster mass estimates based on member galaxies (2006, background): “To further complicate the issue, twice the harmonic mean radius is also usually re- ferred to as the ’virial radius’ (e.g. Girardi et al. 1998; Merchán & Zandivarez 2005).”
Galaxy Alignments: Observations and Impact on Cosmology (2015, methodology): “The analysis was based on a catalogue of close to 5 × 105 ‘groups’ with a minimum estimated halo mass of 1012M /h, found using an adaptive halo-based group finder (Yang et al. 2005, 2007).”
Galaxy Masses: A Review (2013, methodology): “…Trujillo-Gomez et al. 2011; Papastergis et al. 2011, 2012), constraints on halo masses by statistical techniques such as those involving satellite kinematics (More et al. 2011a; Wojtak & Mamon 2013), group catalogs (Yang et al. 2009), and abundance matching (Behroozi et al. 2013), to name a few.”