The Subaru/XMM-Newton Deep Survey (SXDS). II. Optical Imaging and Photometric Catalogs

By H. Furusawa, G. Kosugi, M. Akiyama, T. Takata, K. Sekiguchi, I. Tanaka, I. Iwata, M. Kajisawa, N. Yasuda, M. Doi and 26 more. 2008

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We present multi-wave band optical imaging data obtained from observations of the Subaru/XMM-Newton Deep Survey (SXDS). The survey field, centered at R .A . = 02h18m00s, decl . = − 05°00′00′′, has been the focus of a wide range of multiwavelength observing programs spanning from X-ray to radio wavelengths. A large part of the optical imaging observations are carried out with Suprime-Cam on Subaru Telescope at Mauna Kea in the course of Subaru Telescope “Observatory Projects.” This paper describes our optical observations, data reduction and analysis procedures employed, and the characteristics of the data products. A total area of 1.22 deg2 is covered in five contiguous subfields, each of which corresponds to a single Suprime-Cam field of view (~34′ × 27′), in five broadband filters, B, V, Rc, i′, and z′, to the depths of B = 28.4, V = 27.8, Rc = 27.7, i′ = 27.7, and z′ = 26.6, respectively (AB, 3 σ, ϕ = 2′′). The data are reduced and compiled into five multi-wave band photometric catalogs, separately for each Suprime-Cam pointing. The i′-band catalogs contain about 900,000 objects, making the SXDS catalogs one of the largest multi-wave band catalogs in corresponding depth and area coverage. The SXDS catalogs can be used for an extensive range of astronomical applications such as the number density of the Galactic halo stars to the large-scale structures at the distant universe. The number counts of galaxies are derived and compared with those of existing deep extragalactic surveys. The optical data, the source catalogs, and configuration files used to create the catalogs are publicly available via the SXDS Web page (http://www.naoj.org/Science/SubaruProject/SXDS/index.html).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8cd4e99fa4ac1d501a40707cde01382109b48ea6

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Citations in the corpus

PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, methodology): “In detail, the XMM-LSS field in PRIMUS consists of two separate (but spatially adjacent) subfields: the Subaru/XMM-Newton DEEP Survey field (XMM-SXDS16; Furusawa et al. 2008), and the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) field (hereafter, XMM-CFHTLS17).”
The Hyper Suprime-Cam SSP Survey: Overview and Survey Design (2017, background): “…2002), with its ∼ 0.25deg2 field of view and superb delivered image quality (routinely 0.6′′ FWHM), has been a world leader in wide-field studies of the distant narrow-band filters lie in relatively dark regions of the sky spectrum. and faint Universe (e.g., Iye et al. 2006; Furusawa et al. 2008).”
The VISTA deep extragalactic observations (VIDEO) survey (2012, methodology): “…as COSMOS (Scoville et al. 2007) and the UKIDSS Ultra Deep Survey (UKIDSS-UDS), coupled with the Subaru-XMM Deep Survey (e.g. Foucaud et al. 2007; Furusawa et al. 2008), cover ∼1 deg2 fields, relying on photometric redshifts to trace the evolutionary history of galaxies (e.g. Ilbert et al.…”
SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9 (2016, unknown): “…Quasar Survey (CFHQS; Willott et al. 2005, 2007, 2009, 2010a,b) explored fainter magnitudes than the SDSS and found a few tens of new quasars, including one very faint object (CFHQS J0216−0455; zAB = 24.4 mag at z = 6.01) discovered in the Subaru XMM-Newton Deep Survey (Furusawa et al. 2008) area.”
Delay Time Distribution Measurement of Type Ia Supernovae by the Subaru/XMM-Newton Deep Survey and Implications for the Progenitor (2008, methodology): “The Subaru/XMM-Newton Deep Survey (SXDS: Furusawa et al. 2008), which is the deepest survey among those wider than 1 deg2 with a broad coverage of various wavelengths, provides a unique data set for this purpose.”
The galaxy luminosity function at z ≃ 6 and evidence for rapid evolution in the bright end from z ≃ 7 to 5 (2014, methodology): “The UKIDSS UDS field includes deep optical imaging taken as part of the Subaru XMM-Newton Deep Survey (SXDS) in the B, V , R, i and z′ filters (Furusawa et al. 2008).”
CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, unknown): “These data reach a 3σ limit (2-arcsec diameter aperture) magnitude of B = 28.4, V = 27.8, R = 27.7, i = 27.7 and z = 26.6 (Furusawa et al. 2008).”
Star formation at z=1.47 from HiZELS: an Hα+[O ii] double-blind study* (2011, methodology): “The NB921 zero-points were determined using z′ data, so that the z′–NB921 colour distributions of SXDS would be consistent with that of Subaru Deep Field data (Kashikawa et al. 2004).”
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): “…include: deep optical imaging in the B-, V-, R-, i′- and z′-band filters from the Subaru XMM–Newton Deep Survey (SXDS; Sekiguchi et al. 2005; Furusawa et al. 2008); U-band imaging obtained with MegaCam on Canada–France–Hawaii Telescope; J-, H- and K-band United Kingdom Infrared Telescope…”
STELLAR POPULATIONS OF Lyα EMITTERS AT z ∼ 6–7: CONSTRAINTS ON THE ESCAPE FRACTION OF IONIZING PHOTONS FROM GALAXY BUILDING BLOCKS (2010, methodology): “Deep BV Ri′z′ images of the SXDF were taken with Suprime-Cam (Miyazaki et al. 2002) on the Subaru Telescope by the Subaru/XMM-Newton Deep Survey project (SXDS; Furusawa et al. 2008).”
Identification of the brightest Lyα emitters at z = 6.6 : Implications for the evolution of the luminosity function in the reionization era (2015, methodology): “For UDS, deep z-band data (26.6, 3σ) is available from the Subaru Extreme Deep Field (SXDF) project (Furusawa et al. 2008), as well as data in the optical bands B, V , R and i, with 3σ limits: 28.3, 28.4, 27.8 and 27.2 respectively (see Table 2.).”
A new multifield determination of the galaxy luminosity function at z = 7-9 incorporating the 2012 Hubble Ultra-Deep Field imaging (2012, methodology): “Moreover, in order to clean the sample of low-redshift interlopers, we have utilised a stack of the BV Ri′ Subaru imaging of the UDS described in Furusawa et al. (2008), which reaches a depth of ≥ 29 (2σ; 1.8′′diameter apertures).”
THE COSMIC BPT DIAGRAM: CONFRONTING THEORY WITH OBSERVATIONS (2013, methodology): “At z ∼ 1.5, we use 87 galaxies observed by Yabe et al. (2012) and Yabe et al. (2013, MNRAS, submitted) from the Subaru-XMM Deep Survey (SXDS) (Furusawa et al. 2008) and the UKIDSS Ultra Deep Survey (UDS) (Lawrence et al. 2007).”
REVERSAL OF FORTUNE: CONFIRMATION OF AN INCREASING STAR FORMATION–DENSITY RELATION IN A CLUSTER AT z = 1.62 (2010, methodology): “3-0510 has a wealth of multi-wavelength imaging data that includesBRi′z′ imaging from the Subaru-XMM Deep Survey (Furusawa et al. 2008) andJK imaging from the UKIRT IR Deep Sky Survey (UKIDSS, Lawrence et al. 2007); for these data, we utilized theK–selected catalog from Williams et al. (2009).”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, methodology): “Optical imaging is available from the Subaru–XMM Deep Survey (SXDS, Furusawa et al. 2008), obtained with the Subaru Prime Focus Camera (Suprime– Cam) in the broad bandpassesB, R, i′, andz′.”
The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching? (2013, methodology): “Optical imaging over the field was provided by the Subaru Suprime-Cam as part of the Subaru/XMM-Newton Deep Survey (SXDS; Furusawa et al. 2008).”
Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV Luminosity Functions at $z \sim 4-7$ Derived with the Half-Million Dropouts on the 100 deg$^2$ Sky (2017, unknown): “…obtained in the SXDS (Ouchi et al. 2008; Ouchi et al. 2010) and COSMOS fields (Murayama et al. 2007; Shioya et al. 2009), and high- z dropout galaxy candidates selected from the deep broadband images in these two fields (Furusawa et al. 2008; Capak et al. 2007) were also observed as mask fillers.”
The luminosity function, halo masses and stellar masses of luminous Lyman-break galaxies at redshifts 5 < z < 6 (2008, background): “The reduced optical imaging of the SXDS is now publicly available3 and full details of the observations, data reduction and calibration procedures are provided in Furusawa et al. (2008).”
UV LUMINOSITY FUNCTIONS AT REDSHIFTS z ∼ 4 TO z ∼ 10: 10,000 GALAXIES FROM HST LEGACY FIELDS (2014, background): “These observations reach a 3σ limiting magnitude (2′′-diameter aperture) of B = 28.4, V = 27.8, R = 27.7, i = 27.7 and z = 26.6 (Furusawa et al. 2008).”