ALMA-IMF. VII. First release of the full spectral line cubes: Core kinematics traced by DCN J=(3-2)
arXiv:2306.14710 · doi:10.1051/0004-6361/202245429
Abstract
ALMA-IMF is an Atacama Large Millimeter/submillimeter Array (ALMA) Large Program designed to measure the core mass function (CMF) of 15 protoclusters chosen to span their early evolutionary stages. It further aims to understand their kinematics, chemistry, and the impact of gas inflow, accretion, and dynamics on the CMF. We present here the first release of the ALMA-IMF line data cubes (DR1), produced from the combination of two ALMA 12m-array configurations. The data include 12 spectral windows, with eight at 1.3mm and four at 3mm. The broad spectral coverage of ALMA-IMF (~6.7 GHz bandwidth coverage per field) hosts a wealth of simple atomic, molecular, ionised, and complex organic molecular lines. We describe the line cube calibration done by ALMA and the subsequent calibration and imaging we performed. We discuss our choice of calibration parameters and optimisation of the cleaning parameters, and we demonstrate the utility and necessity of additional processing compared to the ALMA archive pipeline. As a demonstration of the scientific potential of these data, we present a first analysis of the DCN (3-2) line. We find that DCN traces a diversity of morphologies and complex velocity structures, which tend to be more filamentary and widespread in evolved regions and are more compact in the young and intermediate-stage protoclusters. Furthermore, we used the DCN (3-2) emission as a tracer of the gas associated with 595 continuum cores across the 15 protoclusters, providing the first estimates of the core systemic velocities and linewidths within the sample. We find that DCN (3-2) is detected towards a higher percentage of cores in evolved regions than the young and intermediate-stage protoclusters and is likely a more complete tracer of the core population in more evolved protoclusters. The full ALMA 12m-array cubes for the ALMA-IMF Large Program are provided with this DR1 release.
75 pages (21 main body; 54 appendix), 37 figures. The ALMA-IMF DR1 line release is hosted at https://dataverse.harvard.edu/dataverse/alma-imf
References in corpus (30)
- The Critical Density and the Effective Excitation Density of Commonly Observed Molecular Dense Gas Tracers
- The Mass Distribution and Lifetime of Prestellar Cores in Perseus, Serpens, and Ophiuchus
- Fragmentation of Molecular Clumps and Formation of Protocluster
- ATLASGAL - Kinematic distances and the dense gas mass distribution of the inner Galaxy
- pyspeckit: A spectroscopic analysis and plotting package
- ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results
- Multiscale, multiwavelength extraction of sources and filaments using separation of the structural components: getsf
- Dense core properties in the Infrared Dark cloud G14.225-0.506 revealed by ALMA
- From diffuse gas to dense molecular cloud cores
- Thermal Feedback in the high-mass star and cluster forming region W51
- ALMA Observations of Massive Clouds in the Central Molecular Zone: Jeans Fragmentation and Cluster Formation
- Episodic accretion constrained by a rich cluster of outflows
- ALMA-IMF. V. Prestellar and protostellar core populations in the W43 cloud complex
- The dense gas mass fraction in the W51 cloud and its protoclusters
- The Origin of the Stellar Mass Distribution and Multiplicity
- PRODIGE -- Envelope to Disk with NOEMA II. Small-scale temperature structure and a streamer feeding the SVS13A protobinary using CH3CN and DCN
- Diversity of chemistry and excitation conditions in the high-mass star forming complex W33
- ALMA-IMF VI -- Investigating the origin of stellar masses: Core mass function evolution in the W43-MM2&MM3 mini-starburst
- Magnetic Fields in Massive Star-Forming Regions (MagMaR) I. Linear Polarized Imaging of the UCHII Region G5.89-0.39
- ALMA-IMF II -- investigating the origin of stellar masses: Continuum Images and Data Processing
- The Formation of Very Massive Stars
- Molecular analysis of a high-mass prestellar core candidate in W43-MM1
- Mother of Dragons: A Massive, quiescent core in the dragon cloud (IRDC G028.37+00.07)
- The ALMA Survey of 70 Dark High-mass Clumps in Early Stages (ASHES). VII: Chemistry of Embedded Dense Cores
- The ALMA Survey of 70 m Dark High-mass Clumps in Early Stages (ASHES). V. Deuterated Molecules in the 70 m dark IRDC G14.492-00.139
- ALMA-IMF IV -- A comparative study of the main hot cores in W43-MM1: detection, temperature and molecular composition
- Radio and infrared recombination studies of the southern massive star-forming region G333.6-0.2
- The L1157-B1 astrochemical laboratory: testing the origin of DCN
- ALMA ACA and Nobeyama observations of two Orion cores in deuterated molecular lines
- Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA
Cited by in corpus (12)
- ALMA-IMF XI: The sample of hot core candidates A rich population of young high-mass proto-stars unveiled by the emission of methyl formate
- ALMA-IMF X -- The core population in the evolved W33-Main (G012.80) protocluster
- ALMA-IMF XIII: NH kinematic analysis on the intermediate protocluster G353.41
- ALMA-IMF XVI: Mass-averaged temperature of cores and protostellar luminosities in the ALMA-IMF protoclusters
- ALMA-IMF XVII -- Census and lifetime of high-mass prestellar cores in 14 massive protoclusters
- ALMA-IMF XVIII: The assembly of a star cluster: Dense NH (1-0) kinematics in the massive G351.77 protocluster
- Emergence of high-mass stars in complex fiber networks (EMERGE) II. The need for data combination in ALMA observations
- ALMAGAL IV. Morphological comparison of molecular and thermal dust emission using the histogram of oriented gradients (HOG) method
- ngVLA Synthetic Observations of Ionized Gas in Massive Protostars
- The fragmentation properties of massive star-forming regions in 30Dor-10 at 2000 au resolution
- ALMAGAL VIII. Early phases of triggered star formation in source AG286.07161.8229
- The interdependence between density PDF, CMF and IMF and their relation with Mach number in simulations