Letter | Published:

Dense cloud cores revealed by CO in the low metallicity dwarf galaxy WLM

Nature volume 525, pages 218221 (10 September 2015) | Download Citation

Abstract

Understanding stellar birth requires observations of the clouds in which they form. These clouds are dense and self-gravitating, and in all existing observations they are molecular, with H2 the dominant species and carbon monoxide (CO) the best available tracer1,2. When the abundances of carbon and oxygen are low compared with that of hydrogen, and the opacity from dust is also low, as in primeval galaxies and local dwarf irregular galaxies3, CO forms slowly and is easily destroyed, so it is difficult for it to accumulate inside dense clouds4. Here we report interferometric observations of CO clouds in the local group dwarf irregular galaxy Wolf–Lundmark–Melotte (WLM)5, which has a metallicity that is 13 per cent of the solar value6,7 and 50 per cent lower than the previous CO detection threshold. The clouds are tiny compared to the surrounding atomic and H2 envelopes, but they have typical densities and column densities for CO clouds in the Milky Way. The normal CO density explains why star clusters forming in dwarf irregulars have similar densities to star clusters in giant spiral galaxies. The low cloud masses suggest that these clusters will also be low mass, unless some galaxy-scale compression occurs, such as an impact from a cosmic cloud or other galaxy. If the massive metal-poor globular clusters in the halo of the Milky Way formed in dwarf galaxies, as is commonly believed, then they were probably triggered by such an impact.

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Acknowledgements

We wish to thank P. Massey and the Local Group Survey team for the use of their Hα image of WLM. L. Hill made the colour composite inset in Fig. 1. M.R. would like to thank C. Herrera and J. Garcia for support with the CASA implementation to reduce the raw data and A. Rojas for support in the ALMA data reduction. M.R. is grateful to A. Leroy for providing the galaxy data to produce Fig. 3. M.R. thanks the ALMA Director for the invitation to spend her 2015 sabbatical leave at the Joint ALMA Observatory (JAO) in Santiago, where this article was finished. P.C. is grateful to L. Young and S. Madden for invaluable guidance on Herschel data reduction. M.R. wishes to acknowledge support from the Comisión Nacional de Investigación Científica y Tecnológica (CONICYT) through FONDECYT grant no. 1140839. M.R. is partially supported by CONICYT project BASAL PFB-06. The contributions from D.A.H. were funded by the Lowell Observatory Research Fund. P.C. acknowledges support from NASA (National Aeronautics and Space Administration) JPL RSA grant 1433776 to L. Young and grant 1456896 to D.A.H. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. NRAO is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc.

Author information

Affiliations

  1. Departamento de Astronomía, Universidad de Chile, Casilla 36-D, 8320000 Santiago, Chile

    • Monica Rubio
  2. IBM Research Division, T.J. Watson Research Center, 1101 Kitchawan Road, Yorktown Heights, New York 10598, USA

    • Bruce G. Elmegreen
  3. Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, Arizona 86001, USA

    • Deidre A. Hunter
  4. Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK

    • Elias Brinks
  5. Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, 7630355 Santiago, Chile

    • Juan R. Cortés
  6. National Radio Astronomy Observatory, Avenida Nueva Costanera 4091, Vitacura, 7630197 Santiago, Chile

    • Juan R. Cortés
  7. New Mexico Institute of Mining and Technology, Socorro, New Mexico 87801, USA

    • Phil Cigan

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Contributions

D.A.H., Principal Investigator of the ALMA proposal, identified likely CO sources from the re-processed data files using a direct search for significant emission in each frequency channel and for continuous emissions in adjacent channels. M.R. re-processed the ALMA results from the originally calibrated data delivered by ALMA to get better sensitivity and resolution, finalized the identification of emission sources, extracted spectra of the sources, produced Figs 1 and 2, and produced the measurements in Table 1. B.G.E. wrote the text of the manuscript and interpreted the main science results. E.B. oversaw the technical application of radio interferometry to molecular line mapping, and determined the noise limitations and deconvolution strategy for the angular size and velocity width measurements. J.R.C. made the size and linewidth measurements, produced the virial masses and CO luminosities, determined the main observational parameters and made Fig. 3. P.C. reduced the Herschel [C ii] data and made the [C ii] map used in Fig. 1. All authors contributed to the discussions leading to this manuscript.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to Bruce G. Elmegreen.

This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00208.S.

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DOI

https://doi.org/10.1038/nature14901

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