The Multiwavelength Survey by Yale-Chile (MUSYC): Survey Design and Deep Public UBVRIz' Images and Catalogs of the Extended Hubble Deep Field-South

By E. Gawiser, P. V. van Dokkum, D. Herrera, J. Maza, Francisco J. Castander, L. Infante, P. Lira, R. Quadri, R. Toner, E. Treister and 17 more. 2005

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We present UBVRIz' optical images taken with MOSAIC on the CTIO 4 m telescope of the 0.32 deg2 Extended Hubble Deep Field-South. This is one of four fields comprising the MUSYC survey, which is optimized for the study of galaxies at z = 3, active galactic nucleus (AGN) demographics, and Galactic structure. Our methods used for astrometric calibration, weighted image combination, and photometric calibration in AB magnitudes are described. We calculate corrected aperture photometry and its uncertainties and find through tests that these provide a significant improvement upon standard techniques. Our photometric catalog of 62,968 objects is complete to a total magnitude of RAB = 25, with R-band counts consistent with results from the literature. We select z ≃ 3 Lyman break galaxy (LBG) candidates from their UVR colors and find a sky surface density of 1.4 arcmin-2 and an angular correlation function w(θ) = (2.3 ± 1.0)θ-0.8, consistent with previous findings that high-redshift Lyman break galaxies reside in massive dark matter halos. Our images and catalogs are available online.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering

View Paper: https://www.semanticscholar.org/paper/40aeb9907c854aeb2c3508123bb93e7eede881c1

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Citations in the corpus

CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, background): “4 Coe et al. 2012 Previous authors have also noted that SExtractor tends to underestimate flux uncertainties (Feldmeier et al. 2002; Labbé et al. 2003; Gawiser et al. 2006) by as much as a factor of 2–3 (Becker et al. 2007).”
A Significant Population of Very Luminous Dust-Obscured Galaxies at Redshift z ~ 2 (2008, methodology): “The median rest-frame luminosity of DRGs is M 2200Å ≈ −18.3 AB mag for K < 21 (Vega) samples selected from the Hubble Deep Field South and MUSYC Deep fields (G. Rudnick, personal communication; Gawiser et al. 2006).”
The 0.4 < z < 1.3 star formation history of the Universe as viewed in the far-infrared (2009, methodology): “Finally, for the GOODS-S/ECDF-S region, we used the SIMPLE catalog (SpitzerIRAC / MUSYC Public Legacy in ECDF-S; Gawiser et al. 2006).”
IDENTIFYING LUMINOUS ACTIVE GALACTIC NUCLEI IN DEEP SURVEYS: REVISED IRAC SELECTION CRITERIA (2012, background): “Unfortunately, SExtractor tends to underestimate photometric uncertainties, as it does not account for the correlated sky noise present in mosaiced data (e.g., Gawiser et al. 2006; Barmby et al. 2008).”
3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES (2014, methodology): “We incorporate 14 Subaru medium bands from the Multiwavelength Survey by Yale-Chile (MUSYC, Cardamone et al. 2010; Gawiser et al. 2006).25 Four medium bands (three of which have FWHM > 1.”
GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, background): “1 to assess how many similarly bright field galaxies (Capak et al. 2004; Gawiser et al. 2006) are statistically expected within an area corresponding to the GRB’s localization accuracy.”
The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, background): “…faint sources, produce that uncertainties derived uniquely from pixel-to-pixel variations of adjacent sky pixels underestimate the real noise, since these effects correlate the signal of nearby pixels (see, e.g., Casertano et al. 2000; Labbé et al. 2003; Gawiser et al. 2006; Quadri et al. 2007).”
The LABOCA survey of the Extended Chandra Deep Field South: A photometric redshift survey of submillimetre galaxies (2010, methodology): “Therefore, we utilize the MUltiwavelength Survey by Yale-Chile (MUSYC; Gawiser et al. 2006) near-IR survey for U- to K-band imaging (Taylor et al. 2009b), and the Spitzer IRAC/MUSYC Public Legacy in ECDF-S (SIMPLE) imaging for Spitzer IRAC data (Damen et al. 2011).”
Lyα-EMITTING GALAXIES AT z = 2.1 IN ECDF-S: BUILDING BLOCKS OF TYPICAL PRESENT-DAY GALAXIES? (2009, methodology): “We followed the NDWFS (NOAO Deep Wide-Field Survey) cookbook 3 as modified by Gawiser et al. (2006a) plus a few additional steps described below.”
The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5 (2023, methodology): “Finally, we ﬁ t a curve to the noise in a given aperture as a function of pixels in that aperture, using the following equation ( Gawiser et al. 2006 ) : where σ N is the noise in an aperture containing N pixels and σ 1 is the pixel-to-pixel noise measured in each image as the sigma-clipped…”
CANDELS: CONSTRAINING THE AGN–MERGER CONNECTION WITH HOST MORPHOLOGIES AT z ∼ 2 (2011, methodology): “, the astrometry of each ObsID was registered to that of the GOODSMUSYC survey (Gawiser et al. 2006) by matching the positions of bright X-ray sources to H-band-selected sources, using the tool reproject_aspect.”
AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: THE REDSHIFT DISTRIBUTION AND EVOLUTION OF SUBMILLIMETER GALAXIES (2013, methodology): “…redshift distribution of ALESS SMGs The majority of our optical – near-infrared data comes from the MUltiwavelength Survey by Yale-Chile (MUSYC; Gawiser et al. 2006), which provides U–Kband imaging (Taylor et al. 2009) of the entire 0.5 × 0.5 degree ECDFS region (detection limits are given…”
THE MULTIWAVELENGTH SURVEY BY YALE–CHILE (MUSYC): DEEP MEDIUM-BAND OPTICAL IMAGING AND HIGH-QUALITY 32-BAND PHOTOMETRIC REDSHIFTS IN THE ECDF-S (2010, methodology): “The FWHM of the broad band filters is indicated by a red line.”
BLAST: RESOLVING THE COSMIC SUBMILLIMETER BACKGROUND (2009, methodology): “This deep catalog from SIMPLE (Spitzer IRAC / MUSYC Public Legacy in ECDFS, Gawiser et al. 2006) enabled the deblending of sources with separations as small as 0.5FWHM in the MIPS map, resulting in an extremely faint flux density limit S24 >∼ 15µJy.”
CEERS Key Paper. I. An Early Look into the First 500 Myr of Galaxy Formation with JWST (2022, methodology): “Finally, we fit a curve to the noise in a given aperture as a function of the pixels in that aperture, using the equation (Gawiser et al. 2006) s s a= b ( )N , 1N 1 where σN is the noise in an aperture containing N pixels, and σ1 is the pixel-to-pixel noise measured in each image as the…”