The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

Béthermin, M.; Fudamoto, Yoshinobu; Ginolfi, M.; Loiacono, F.; Khusanova, Y.; Capak, P.; Cassata, P.; Faisst, Andreas L.; Fèvre, O. Le; Schaerer, D.; Silverman, John D.; Yan, Lin; Amorín, R.; Bardelli, S.; Boquien, M.; Cimatti, A.; Davidzon, I.; Dessauges‐Zavadsky, M.; Fujimoto, Seiji; Gruppioni, C.; Hathi, N. P.; Ibar, E.; Jones, G. C.; Koekemoer, Anton M.; Lagache, G.; Lemaux, Brian C.; Moreau, C.; Oesch, Pascal; Pozzi, F.; Riechers, Dominik A.; Talia, M.; Toft, Sune; Vallini, L.; Vergani, D.; Zamorani, G.; Zucca, E.

doi:10.1051/0004-6361/202037649

Cited by 183 publications

(185 citation statements)

References 135 publications

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“…As discussed in Béthermin et al (2020), the mean [C II] line flux rms is 0.14 Jy km s −1 for this sample. The spectral maps have yielded 75 [C II] emission lines with the peak flux to noise ratio SNR peak 3.5σ and 43 nondetections (<3.5σ).…”

Section: The [C Ii] Emission Line Measurementsmentioning

confidence: 73%

“…-and many of them have multiple components and are clearly interacting. Several ALPINE papers (Béthermin et al 2020;Le Fèvre et al 2020;Loiacono et al 2020) discuss this property. Jones et al (2020) has focused on one triple merger system, deimos_cosmos_818760, with three [C II] components.…”

Section: The [C Ii] Emission Line Measurementsmentioning

confidence: 99%

“…The goal of this paper is to address these questions, using a unique set of observations taken by the ALMA Large Program to INvestigate C II at Early times (ALPINE) survey (Béthermin et al 2020;Faisst et al 2020;Le Fèvre et al 2020). Our paper is organized as follows.…”

Section: Introductionmentioning

confidence: 99%

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The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

Yan

Sajina

Loiacono

et al. 2020

ApJ

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We present the [C II] 158 μm line luminosity functions (LFs) at z∼4-6 using the ALMA observations of 118 sources, which are selected to have UV luminosity M 1500Å <−20.2 and optical spectroscopic redshifts in COSMOS and ECDF-S. Of the 118 targets, 75 have significant [C II] detections and 43 are upper limits. This is by far the largest sample of [C II] detections, which allows us to set constraints on the volume density of [C II] emitters at z∼4-6. But because this is a UV-selected sample, we are missing [C II]-bright but UV-faint sources, making our constraints strict lower limits. Our derived LFs are statistically consistent with the z∼0 [C II] LF at 10 8.25-10 9.75 L e. We compare our results with the upper limits of the [C II] LF derived from serendipitous sources in the ALPINE maps. We also infer the [C II] LFs based on published far-IR and CO LFs at z∼4-6. Combining our robust lower limits with these additional estimates, we set further constraints on the true number density of [C II] emitters at z∼4-6. These additional LF estimates are largely above our LF at L [CII] >10 9 L e , suggesting that UV-faint but [C II]-bright sources likely make significant contributions to the [C II] emitter volume density. When we include all the LF estimates, we find that available model predictions underestimate the number densities of [C II] emitters at z∼4-6. Finally, we set a constraint on the molecular gas mass density at z∼4-6, with ρ mol ∼(2-7)×10 7 M e Mpc −3. This is broadly consistent with previous studies.

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Section: The [C Ii] Emission Line Measurementsmentioning

confidence: 73%

Section: The [C Ii] Emission Line Measurementsmentioning

confidence: 99%

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The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

Yan

Sajina

Loiacono

et al. 2020

ApJ

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“…Targeted studies such as the ALMA Large Programme to INvestigate [CII] at Early times (ALPINE) survey (e.g. [584,[640][641][642][643][644]) are a more promising way to detect [CII] emission at high-redshift. ALPINE targeted a sample of 118 spectroscopically confirmed star-forming galaxies at 4.4 < z < 5.9 with a typical beam size of 0.7 arcsec (≃6 kpc).…”

Section: Continuum and [Cii] Line Searches At High Redshiftmentioning

confidence: 99%

High-redshift star formation in the Atacama large millimetre/submillimetre array era

2020

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The Atacama Large Millimetre/submillimetre Array (ALMA) is currently in the process of transforming our view of star-forming galaxies in the distant ( z ≳ 1 ) universe. Before ALMA, most of what we knew about dust-obscured star formation in distant galaxies was limited to the brightest submillimetre sources—the so-called submillimetre galaxies (SMGs)—and even the information on those sources was sparse, with resolved (i.e. sub-galactic) observations of the obscured star formation and gas reservoirs typically restricted to the most extreme and/or strongly lensed sources. Starting with the beginning of early science operations in 2011, the last 9 years of ALMA observations have ushered in a new era for studies of high-redshift star formation. With its long baselines, ALMA has allowed observations of distant dust-obscured star formation with angular resolutions comparable to—or even far surpassing—the best current optical telescopes. With its bandwidth and frequency coverage, it has provided an unprecedented look at the associated molecular and atomic gas in these distant galaxies through targeted follow-up and serendipitous detections/blind line scans. Finally, with its leap in sensitivity compared to previous (sub-)millimetre arrays, it has enabled the detection of these powerful dust/gas tracers much further down the luminosity function through both statistical studies of colour/mass-selected galaxy populations and dedicated deep fields. We review the main advances ALMA has helped bring about in our understanding of the dust and gas properties of high-redshift ( z ≳ 1 ) star-forming galaxies during these first 9 years of its science operations, and we highlight the interesting questions that may be answered by ALMA in the years to come.

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“…Pointing on known objects, with, for example, ALMA, NOEMA, and APEX/FLASH, [CII] is now detected in a large number of galaxies at high z (>150 at z > 4.5, with a large contribution from the ALMA ALPINE survey, e.g. Bethermin et al 2020). These types of observations are a tremendous step forward but we also need to look at the overall population, that is, observe large volume and unbiased surveys.…”

Section: [Cii] Intensity Mapping With Concertomentioning

confidence: 99%

A wide field-of-view low-resolution spectrometer at APEX: Instrument design and scientific forecast

Ade

Aravena

Barria³

et al. 2020

A&A

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Context. Characterising the large-scale structure in the Universe from present times to the high redshift epoch of reionisation is essential to constraining the cosmology, the history of star formation, and reionisation, to measuring the gas content of the Universe, and to obtaining a better understanding of the physical processes that drive galaxy formation and evolution. Using the integrated emission from unresolved galaxies or gas clouds, line intensity mapping (LIM) provides a new observational window to measure the larger properties of structures. This very promising technique motivates the community to plan for LIM experiments. Aims. We describe the development of a large field-of-view instrument, named CONCERTO (for CarbON CII line in post-rEionisation and ReionisaTiOn epoch), operating in the range 130–310 GHz from the APEX 12-m telescope (5100 m above sea level). CONCERTO is a low-resolution spectrometer based on the lumped element kinetic inductance detectors (LEKID) technology. Spectra are obtained using a fast Fourier transform spectrometer (FTS), coupled to a dilution cryostat with a base temperature of 0.1 K. Two two kilo-pixel arrays of LEKID are mounted inside the cryostat that also contains the cold optics and the front-end electronics. Methods. We present, in detail, the technological choices leading to the instrumental concept, together with the design and fabrication of the instrument and preliminary laboratory tests on the detectors. We also give our best estimates for CONCERTO sensitivity and give predictions for two of the main scientific goals of CONCERTO, that is, a [CII]-intensity mapping survey and observations of galaxy clusters. Results. We provide a detailed description of the instrument design. Based on realistic comparisons with existing instruments developed by our group (NIKA, NIKA2, and KISS), and on the laboratory characterisation of our detectors, we provide an estimate for CONCERTO sensitivity on the sky. Finally, we describe, in detail, two of the main scientific goals offered by CONCERTO at APEX.

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The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

Cited by 183 publications

References 135 publications

The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

High-redshift star formation in the Atacama large millimetre/submillimetre array era

A wide field-of-view low-resolution spectrometer at APEX: Instrument design and scientific forecast

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