Spitzer Matching Survey of the UltraVISTA Ultra-deep Stripes (SMUVS): Full-mission IRAC Mosaics and Catalogs

Abstract

This paper describes new deep 3.6 and 4.5 µm imaging of three UltraVISTA near-infrared survey stripes within the COSMOS field. The observations were carried out with Spitzer's Infrared Array Camera (IRAC) for the Spitzer Matching Survey of the Ultra-VISTA Deep Stripes (SMUVS). In this work we present our data reduction techniques, and document the resulting mosaics, coverage maps, and catalogs in both IRAC passbands for the three easternmost UltraVISTA survey stripes, covering a combined area of about 0.66 deg 2 , of which 0.45 deg 2 have at least 20 hr integration time. SMUVS reaches point-source sensitivities of about 25.0 AB mag (0.13 µJy) at both 3.6 and 4.5 µm with a significance of 4σ, accounting for both survey sensitivity and source confusion. To this limit the SMUVS catalogs contain a total of ∼350,000 sources, each of which is detected significantly in at least one IRAC band. Because of its uniform and high sensitivity, relatively large area coverage, and the wide array of ancillary data available in COSMOS, the SMUVS survey will be useful for a large number of cosmological investigations. We make all images and catalogues described herein publicly available via the Spitzer Science Center.

The Brightest z ≳ 8 Galaxies over the COSMOS UltraVISTA Field

“…(Taniguchi et al 2007), and Subaru HyperSuprimeCam g, r, i, z and y (Aihara et al 2017a,b). For this work, we used full-depth Spitzer /IRAC 3.6µm and 4.5µm mosaics we built combining observations from all available programs: S-COSMOS (Sanders et al 2007), the Spitzer Extended Deep Survey (Ashby et al 2013), the Spitzer-Cosmic Assembly Near-Infrared Deep Extragalactic Survey (S-CANDELS, Ashby et al 2015), the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH, PI: Capak), the Spitzer Matching survey of the UltraVISTA ultra-deep Stripes (SMUVS, Caputi et al 2017;Ashby et al 2018). Compared to the original S-COSMOS IRAC data, SPLASH provides a large improvement in depth over nearly the whole UltraVISTA area, covering the central 1.2 square degree COSMOS field to 25.5 mag (AB) at 3.6 and 4.5µm.…”

“…This search takes advantage of the deepest-available ground-based optical+near-infrared observations, in particular the DR3 release of UltraVISTA which provides ∼ 1.4 mag deeper data in Y, J, H, K s compared to DR1 (McCracken et al 2012). Our study also takes advantage of deep Spitzer/IRAC (Fazio et al 2004) observations from the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH, PI: Capak) and the Spitzer Matching survey of the UltraVISTA ultradeep Stripes (SMUVS, PI: Caputi -Caputi et al 2017;Ashby et al 2018) programs. The increased depth and the inclusion of Spitzer/IRAC data, probing the restframe optical, now makes it possible to access the galaxy population at z 8 through reliable sample selections.…”

Automated Mining of the ALMA Archive in the COSMOS Field (A3COSMOS). I. Robust ALMA Continuum Photometry Catalogs and Stellar Mass and Star Formation Properties for ∼700 Galaxies at z = 0.5–6

“…comm. ) and are also present in the IRAC catalogs from the Spitzer Matching Survey of the UltraVISTA Ultra-deep Stripes (SMUVS; Ashby et al 2018), their stellar masses and photometric redshifts have large uncertainties due to the lack of shorter-wavelength information. We therefore omit these sources from our galaxy catalog (see the "no optical/near-IR prior-redshift galaxies" entry in Fig.…”

The BUFFALO HST Survey

“…Their measurements of the high-redshift luminosity function enable BUFFALO to choose a depth in five optical and nearinfrared passbands with the Advanced Camera for Surveys (ACS) and the Wide Field Camera 3 (WFC3) that is optimized to select the most luminous galaxies at z>6 and study their physical properties, such as stellar masses, by fully exploiting the preexisting, deep Spitzer/IRAC data around the Frontier Fields. BUFFALO is thus the logical extension of the HFF (Lotz et al 2017), as well as previous HST+Spitzer extragalactic legacy surveys such as GOODS (Giavalisco et al 2004), HUDF (Beckwith et al 2006;Ellis et al 2013;Illingworth et al 2013;Labbé et al 2015), CANDELS (Grogin et al 2011;Koekemoer et al 2011), S-CANDELS (Ashby et al 2015), COSMOS (Scoville et al 2007), SMUVS (Ashby et al 2018), Brightest of Reionizing Galaxies (BoRG)/HIPPIES (Trenti et al 2011;Yan et al 2011), Cluster Lensing And Supernovae with Hubble (CLASH; Postman et al 2012), SURFS UP (Bradač et al 2014), or RELICS (Coe et al 2019).…”