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Planck early results. XV. Spectral energy distributions and radio continuum spectra of northern extragalactic radio sources |
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Planck early results. XVI. The Planck view of nearby galaxies |
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Planck early results. XVII. Origin of the submillimetre excess dust emission in the Magellanic Clouds |
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Planck early results. XXI. Properties of the interstellar medium in the Galactic plane |
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Planck early results. XXII. The submillimetre properties of a sample of Galactic cold clumps |
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Planck early results. XXVI. Detection with Planck and confirmation by XMM-Newton of PLCK G266.6-27.3, an exceptionally X-ray luminous and massive galaxy cluster at z ~ 1 |
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A spectrograph for exoplanet observations calibrated at the centimetre-per-second level |
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Spitzer Mid-IR Spectroscopy of Powerful 2 Jy and 3CRR Radio Galaxies. I. Evidence against a Strong Starburst-AGN Connection in Radio-loud AGN |
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HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm |
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Herschel and SCUBA-2 imaging and spectroscopy of a bright, lensed submillimetre galaxy at z = 2.3 |
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The Herschel Space Observatory view of dust in M81 |
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Radial distribution of gas and dust in spiral galaxies . The case of M 99 (NGC 4254) and M 100 (NGC 4321) |
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HerMES: SPIRE Science Demonstration Phase maps†‡ |
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On the origin of M81 group extended dust emission |
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HerMES: deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations |
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Measures of star formation rates from infrared (Herschel) and UV (GALEX) emissions of galaxies in the HerMES fields |
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Discovery of a Multiply Lensed Submillimeter Galaxy in Early HerMES Herschel/SPIRE Data |
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Redshift Determination and CO Line Excitation Modeling for the Multiply Lensed Galaxy HLSW-01 |
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Dynamical Structure of the Molecular Interstellar Medium in an Extremely Bright, Multiply Lensed z ~= 3 Submillimeter Galaxy Discovered with Herschel |
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Herschel/HerMES: the X-ray-infrared correlation for star-forming galaxies at z˜1 |
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The suppression of star formation by powerful active galactic nuclei |
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HerMES: deep number counts at 250 μm, 350 μm and 500 μm in the COSMOS and GOODS-N fields and the build-up of the cosmic infrared background |
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The promise of Bayesian analysis for prominence seismology |
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The GREGOR Fabry-Pérot Interferometer |
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The Acoustic Cutoff Frequency of the Sun and the Solar Magnetic Activity Cycle |
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