MHONGOOSE: A MeerKAT nearby galaxy H I survey

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dc.contributor.authorde Blok, W. J. G.en
dc.contributor.authorHealy, J.en
dc.contributor.authorMaccagni, F. M.en
dc.contributor.authorPisano, D. J.en
dc.contributor.authorBosma, A.en
dc.contributor.authorEnglish, J.en
dc.contributor.authorJarrett, T.en
dc.contributor.authorMarasco, A.en
dc.contributor.authorMeurer, G. R.en
dc.contributor.authorVeronese, S.en
dc.contributor.authorBigiel, F.en
dc.contributor.authorChemin, L.en
dc.contributor.authorFraternali, F.en
dc.contributor.authorHolwerda, B. W.en
dc.contributor.authorKamphuis, P.en
dc.contributor.authorKloeckner, H. R.en
dc.contributor.authorKleiner, D.en
dc.contributor.authorLeroy, A. K.en
dc.contributor.authorMogotsi, M.en
dc.contributor.authorOman, K. A.en
dc.contributor.authorSchinnerer, E.en
dc.contributor.authorVerdes-Montenegro, L.en
dc.contributor.authorWestmeier, T.en
dc.contributor.authorWong, O. I.en
dc.contributor.authorZabel, N.en
dc.contributor.authorAmram, P.en
dc.contributor.authorCarignan, C.en
dc.contributor.authorCombes, F.en
dc.contributor.authorBrinks, E.en
dc.contributor.authorDettmar, R. J.en
dc.contributor.authorGibson, B. K.en
dc.contributor.authorJozsa, G. I. G.en
dc.contributor.authorKoribalski, B. S.en
dc.contributor.authorMcgaugh, S. S.en
dc.contributor.authorOosterloo, T. A.en
dc.contributor.authorSpekkens, K.en
dc.contributor.authorSchroeder, A. C.en
dc.contributor.authorAdams, E. A. K.en
dc.contributor.authorAthanassoula, E.en
dc.contributor.authorBershady, M. A.en
dc.contributor.authorBeswick, R. J.en
dc.contributor.authorBlyth, S.en
dc.contributor.authorElson, E. C.en
dc.contributor.authorFrank, B. S.en
dc.contributor.authorHeald, G.en
dc.contributor.authorHenning, P. A.en
dc.contributor.authorKurapati, S.en
dc.contributor.authorLoubser, S. I.en
dc.contributor.authorLucero, D.en
dc.contributor.authorMeyer, M.en
dc.contributor.authorNamumba, B.en
dc.contributor.authorOh, S. -H.en
dc.contributor.authorSardone, A.en
dc.contributor.authorSheth, K.en
dc.contributor.authorSmith, M. W. L.en
dc.contributor.authorSorgho, A.en
dc.contributor.authorWalter, F.en
dc.contributor.authorWilliams, T.en
dc.contributor.authorWoudt, P. A.en
dc.contributor.authorZijlstra, A.en
dc.date.accessioned2025-10-29T14:19:14Zen
dc.date.available2025-10-29T14:19:14Zen
dc.date.issued2024-08-21en
dc.description.abstractThe MHONGOOSE (MeerKAT H I Observations of Nearby Galactic Objects: Observing Southern Emitters) survey maps the distribution and kinematics of the neutral atomic hydrogen (H I) gas in and around 30 nearby star-forming spiral and dwarf galaxies to extremely low H I column densities. The H I column density sensitivity (3 sigma over 16 km s(-1)) ranges from similar to 5 x 10(17) cm(-2) at 90 '' resolution to similar to 4 x 10(19) cm(-2) at the highest resolution of 7 ''. The H I mass sensitivity (3 sigma over 50 km s(-1)) is similar to 5.5 x 10(5) M-circle dot at a distance of 10 Mpc (the median distance of the sample galaxies). The velocity resolution of the data is 1.4 km s(-1). One of the main science goals of the survey is the detection of cold accreting gas in the outskirts of the sample galaxies. The sample was selected to cover a range in H I masses from 10(7) M-circle dot to almost 10(11) M-circle dot in order to optimally sample possible accretion scenarios and environments. The distance to the sample galaxies ranges from 3 to 23 Mpc. In this paper, we present the sample selection, survey design, and observation and reduction procedures. We compared the integrated H I fluxes based on the MeerKAT data with those derived from single-dish measurement and find good agreement, indicating that our MeerKAT observations are recovering all flux. We present H I moment maps of the entire sample based on the first ten percent of the survey data, and find that a comparison of the zeroth- and second-moment values shows a clear separation in the physical properties of the H I between areas with star formation and areas without related to the formation of a cold neutral medium. Finally, we give an overview of the H I-detected companion and satellite galaxies in the 30 fields, five of which have not previously been cataloged. We find a clear relation between the number of companion galaxies and the mass of the main target galaxy.en
dc.description.sponsorshipEuropean Research Council (ERC) under the European Union [882793]; Royal Society Dorothy Hodgkin Fellowship; STFC [ST/T000244/1]; European Research Council (ERC) through Advanced Investigator grant [GA 786910]; South African Research Chairs Initiative of the Department of Science and Technology; National Research Foundation [77825]; CNES; Chilean Agencia Nacional de Investigacion y Desarrollo (ANID) through Fondo Nacional de Desarrollo Cientifico y Tecnologico (FONDECYT) Regular Project [1210992]; German Federal Ministry of Education and Research (BMBF) Verbundforschung grant [05A20PC4]; Natural Sciences and Engineering Research Council of Canada (NSERC); MCIN/AEI [CEX2021-001131-S, PID2021-123930OB-C21]; ERDF A way of making Europe; European Union; National Aeronautics and Space Administration; NOIRLab; Lawrence Berkeley National Laboratory (LBNL); U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago, Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; National Astronomical Observatories of China; Chinese Academy of Sciences [XDB09000000]; Ministry of Finance; External Cooperation Program of Chinese Academy of Sciences [114A11KYSB20160057]; Chinese National Natural Science Foundation [12120101003, 11433005]; Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy [DE-AC02-05CH1123]; National Energy Research Scientific Computing Center; DOE Office of Science User Facility; U.S. National Science Foundation, Division of Astronomical Sciences [AST-0950945]; Academy of Finland (AKA) [77825] Funding Source: Academy of Finland (AKA); Science and Technology Facilities Council [ST/T000244/1] Funding Source: researchfishen
dc.format.mimetypeapplication/pdfen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202348297en
dc.identifier.eissn1432-0746en
dc.identifier.issn0004-6361en
dc.identifier.urihttps://hdl.handle.net/10919/138801en
dc.identifier.volume688en
dc.language.isoenen
dc.publisherEDP Sciencesen
dc.rightsCreative Commons Attribution 4.0 Internationalen
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/en
dc.subjectgalaxies: dwarfen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: ISMen
dc.subjectgalaxies: spiralen
dc.subjectradio lines: galaxiesen
dc.titleMHONGOOSE: A MeerKAT nearby galaxy H I surveyen
dc.title.serialAstronomy & Astrophysicsen
dc.typeArticle - Refereeden
dc.type.dcmitypeTexten

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