GEMS: Galaxy Evolution from Morphologies and SEDs

By Hans-Walter Rix, M. Barden, S. Beckwith, Eric F. Bell, A. Borch, J. Caldwell, B. Haeussler, K. Jahnke, S. Jogee, D. H. Mcintosh and 6 more. 2004

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GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800 arcmin2) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the Hubble Space Telescope. Centered on the Chandra Deep Field-South, it covers an area of ~28′ × 28′, or about 120 Hubble Deep Field areas, to a depth of mAB(F606W) = 28.3(5 σ) and mAB(F850LP) = 27.1(5 σ) for compact sources. In its central ~1/4, GEMS incorporates ACS imaging from the GOODS project. Focusing on the redshift range 0.2 ≲ z ≲ 1.1, GEMS provides morphologies and structural parameters for nearly 10,000 galaxies where redshift estimates, luminosities, and SEDs exist from COMBO-17. At the same time, GEMS contains detectable host galaxy images for several hundred faint active galactic nuclei. This paper provides an overview of the science goals, the experiment design, the data reduction, and the science analysis plan for GEMS.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b3bfb36ff1364995d7ee9313ed997b9105631a2f

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Citations in the corpus

Characterizing Bars at z ~ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift (2006, methodology): “Furthermore, with the advent of high-redshift HST surveys, such as the Tadpole field (Tran et al. 2003), the Galaxy Evolution from Morphology and SEDs (GEMS; Rix et al. 2004), the Great Observatories Origins Deep 1 We assume in this paper a flat cosmology with M ¼ 1 ¼ 0:3 and H0 ¼ 70 km s 1 Mpc 1.”
The Frontier Fields: Survey Design and Initial Results (2016, result): “However, this star is bright enough to act as an adaptive optics guide star, therefore provides a unique opportunity to obtain AO imaging (e.g. Schrimer et al. 2015, Gemini- GEMS) and spectroscopy of the critical curves surrounding a strong-lensing cluster.”
THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5 (2011, methodology): “Jogee et al. (2009) visually classified galaxies with stellar masses > 2.5× 1010M⊙ at 0.24 < z < 0.80 in V -band HSTACS images from the GEMS survey.”
A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, background): “…role in the new understanding of the Universe and its constituents brought about by the remarkable flow of data over the past few years, thanks to large surveys such as the 2dFGRS (Folkes et al. 1999), SDSS (York et al. 2000), GEMS (Rix et al. 2004), or COSMOS (Scoville et al. 2007), to name a few.”
THE 2012 HUBBLE ULTRA DEEP FIELD (UDF12): OBSERVATIONAL OVERVIEW (2012, background): “G. Illingworth, described in Oesch et al. 2010b,a and Bouwens et al. 2011b) and most recently in 2012 (UDF12, PI: R. Ellis, described in Ellis et al. 2012 together with the present paper).10 These surveys, in conjunction with wider, shallower HST surveys with the Advanced Camera for Surveys (ACS) in”
KiDS-450: cosmological parameter constraints from tomographic weak gravitational lensing (2016, methodology): “The r-band magnitude distribution of the galaxies is chosen such that it matches the number counts measured in KiDS-DR1/2, and we use deep HST observations from GEMS (Rix et al. 2004) and UVUDF (Rafelski et al. 2015) to extend the distribution to the 28th magnitude in order to account for the effect”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, background): “As mentioned above, ∼ 85% of such color-selected galaxies appear also morphologically early-type on the ACS images of the GEMS (Galaxy Evolution from Morphology and SED) survey (Rix et al. 2004, Bell et al. 2004a).”
HYDROGEN-POOR SUPERLUMINOUS SUPERNOVAE AND LONG-DURATION GAMMA-RAY BURSTS HAVE SIMILAR HOST GALAXIES (2013, methodology): “The host of PS1-10bzj (Lunnan et al. 2013) has serendipitous HST imaging from the GEMS survey (Rix et al. 2004), and is also shown in Figure 2.”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY—THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS, AND MOSAICS (2011, background): “The CANDELS Deep portion covers ∼ 125 square arcminutes to ∼ 10-orbit depth within the GOODS-North and GOODS-South Fields (Giavalisco et al. 2004) including the E-CDFS (Rix et al. 2004) as well as the WFC3 ERS2 field (Windhorst et al. 2011).”
The First Release COSMOS Optical and Near-IR Data and Catalog (2007, background): “…0 Monet et al., 2003, AJ, 125, 984 Pickles, A. J. 1998, PASP, 110, 863 Probst et al., 2003, Proc. of the SPIE, Volume 4841, pp. 411-419 (2003)., 411–419 Rix et al., 2004, ApJS, 152, 163 Robin et al., 2007, astro-ph/0612349 Sanders et al., 2007, astro-ph/0701318 Schinnerer et al., 2004, AJ, 128,…”
The Morphologies of Massive Galaxies at 1<z<3 in the CANDELS-UDS Field: Compact Bulges, and the Rise and Fall of Massive Disks (2012, methodology): “This issue is well documented in Häussler et al. (2007), where they used GEMS data (Rix et al. 2004) to test how well GALFIT can recover the input parameters of simulated n = 1 (disc) and n = 4 (bulge) galaxies.”
DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, background): “…redshift evolution of sizes, but fortunately the observational constraints (e.g. Trujillo et al.2006; Barden et al. 2005; Ravindranath et al. 2004; Rix et al. 2004; Ferguson et al. 2004; Akiyama et al. 2008) and state-of-theart models (Somerville et al. 2008b) suggest that any evolution is…”
A new measurement of the evolving near-infrared galaxy luminosity function out to z≃ 4: a continuing challenge to theoretical models of galaxy formation (2008, background): “Several deep multi-wavelengths surveys are now ongoing or have just been completed (Cimatti et al. 2002; Giavalisco et al. 2004; Rix et al. 2004; Lawrence et al. 2007; Scoville et al. 2007) with the aim of tracing the assembly history of galaxies.”
Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate (2005, methodology): “We use F850LP imaging from the GEMS survey (Rix et al. 2004) to provide 0B07 resolution rest-frame V-band data for 1492 galaxies with 0:65 z < 0:75.”
The Mass Assembly Histories of Galaxies of Various Morphologies in the GOODS Fields (2005, background): “Large galaxy surveys like DEEP2 (Davis et al. 2002) and COMBO-17 (Rix et al. 2004) are promising in this regard because they contain tens of thousands of galaxies spread over a wide area, although we note that stellar mass studies benefit greatly from spectroscopic redshifts.”
Galaxies in the Hubble Ultra Deep Field. I. Detection, Multiband Photometry, Photometric Redshifts, and Morphology (2006, methodology): “Large-area HST/ACS multiband surveys such as GEMS (Rix et al. 2004), GOODS (Gi- avalisco et al. 2004), and COSMOS (Scoville et al., in prep.) have contributed significantly to our understanding of galaxy evolution.”
WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, background): “Finally, increasing the number statistics atz< 1 (already underway with, e.g., the GEMS, AEGIS or COSMOS datasets; Rix et al. 2004, Davis et al. 2007, Scoville et al. 2007) and atz> 1 with the full five-field coverage of CANDELS (Grogin et al. 2011; Koekemoer et al. 2011) is likely to prove useful.”
NICMOS Imaging of DRGs in the HDF-S: A Relation between Star Formation and Size at z ~ 2.5 (2006, background): “By combining rest-frame optical sizes and multiwavelength spectral energy distributions we can begin to discern the evolutionary pathways of galaxies at various redshifts (e.g., Rix et al. 2004; Trujillo et al. 2004, 2006a; Longhetti et al. 2007).”