Showing 1–20 of 274 results
/ Date/ Name
Aug 30, 2018The [C II] emission as a molecular gas mass tracer in galaxies at low and high redshiftMar 3, 2010Submillimeter Number Counts at 250, 350 and 500 microns in BLAST dataDec 5, 2022CONCERTO: Simulating the CO, [CII], and [CI] line emission of galaxies in a 117 $\rm deg^2$ field and the impact of field-to-field varianceMay 11, 2023NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number CountsJun 4, 2022The ALMA REBELS Survey: Average [CII] $158\,\rm{μm}$ sizes of Star-Forming Galaxies from $z\sim 7$ to $z\sim 4$Aug 24, 2012HerMES: Cosmic Infrared Background Anisotropies and the Clustering of Dusty Star-Forming GalaxiesOct 3, 2018Concurrent starbursts in molecular gas disks within a pair of colliding galaxies at z = 1.52Apr 22, 2020The ALPINE-ALMA [CII] survey: Dust attenuation properties and obscured star formation at z~4.4-5.8Apr 22, 2020The ALPINE-ALMA [CII] survey: Molecular gas budget in the Early Universe as traced by [CII]May 4, 2020ALMACAL VII: First Interferometric Number Counts at 650 $μ$mMay 6, 2020GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxiesMay 6, 2020GOODS-ALMA: The slow downfall of star-formation in $z$ = 2-3 massive galaxiesFeb 3, 2020The ALPINE-ALMA [CII] survey. Little to no evolution in the [CII]-SFR relation over the last 13 GyrMay 31, 2021The ALPINE-ALMA [CII] survey: Dust mass budget in the early UniverseApr 15, 2013A Dust-Obscured Massive Maximum-Starburst Galaxy at a Redshift of 6.34Mar 20, 2013Planck 2013 results. I. Overview of products and scientific resultsMar 18, 2013The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observationsMar 27, 2013HerMES: A Deficit in the Surface Brightness of the Cosmic Infrared Background Due to Galaxy Cluster Gravitational LensingMar 1, 2012HerMES: A Statistical Measurement of the Redshift Distribution of Herschel-SPIRE Sources Using the Cross-correlation TechniqueMay 22, 2015HerMES: Current Cosmic Infrared Background Estimates Can be Explained by Known Galaxies and their Faint Companions at z < 4