Journal article
WALLABY early science - III. An HI study of the spiral galaxy NGC 1566
A Elagali, L Staveley-Smith, J Rhee, OI Wong, A Bosma, T Westmeier, BS Koribalski, G Heald, BQ For, D Kleiner, K Lee-Waddell, JP Madrid, A Popping, TN Reynolds, MJ Meyer, JR Allison, CDP Lagos, MA Voronkov, P Serra, L Shao Show all
Monthly Notices of the Royal Astronomical Society | Published : 2019
Abstract
This paper reports on the atomic hydrogen gas (HI) observations of the spiral galaxy NGC 1566 using the newly commissioned Australian Square Kilometre Array Pathfinder radio telescope. We measure an integrated HI flux density of 180.2 Jy kms-1 emanating from this galaxy, which translates to an HI mass of 1.94 × 1010M⊙ at an assumed distance of 21.3Mpc. Our observations show that NGC 1566 has an asymmetric and mildly warped HI disc. The HI-to-stellar mass fraction (MHI/M∗) of NGC 1566 is 0.29, which is high in comparison with galaxies that have the same stellar mass (1010.8M⊙). We also derive the rotation curve of this galaxy to a radius of 50 kpc and fit different mass models to it. The NFW,..
View full abstractRelated Projects (1)
Grants
Awarded by Horizon 2020 Framework Programme
Funding Acknowledgements
We thank the anonymous referee for their positive and constructive comments that greatly improved the presentation of the results in this manuscript. AE is thankful for Davide Punzo and Kelley Hess for their help in making the 3D visualization of NGC 1566, and for Kyle Oman for providing the theoretical predictions for the relative velocity PDF of NGC 1566 from his N-body simulations and libraries. AB acknowledges financial support from the CNES (Centre National d'Etudes Spatiales, France). JW thanks support from the National Science Foundation of China (grant 11721303). This research was supported by the Australian Research Council Centre of Excellence for All-sky Astrophysics in 3 Dimensions (< 0:funding-source > < 0:funding-source > ASTRO 3D </0:funding-s ource > </0:funding-source >) through project number CE170100013. The ATCA is part of the Australia Telescope National Facility (ATNF) and is operated by CSIRO. The ATNF receives funds from the Australian Government. This work was supported by resources provided by the Pawsey Supercomputing Centre with funding from the Australian Government and the Government of Western Australia, including computational resources provided by the Australian Government under the National Computational Merit Allocation Scheme (project JA3). PS has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant number 679629; name FORNAX). This paper used archival HI data of NGC 1566 available in the Australia Telescope Online Archive (http://atoa.atnf.csiro.au). ASKAP is part of the ATNF and is operated by CSIRO. The Operation of ASKAP is funded by the Australian Government with support from the National Collaborative Research Infrastructure Strategy. ASKAP uses the resources of the Pawsey Supercomputing Centre. Establishment of ASKAP, the Murchison Radio-astronomy Observatory and the Pawsey Supercomputing Centre are initiatives of the Australian Government, with support from the Government of Western Australia and the Science and Industry Endowment Fund. We acknowledge the Wajarri Yamatji people, the custodians of the observatory land. This work used images of NGC 1566 available in the NED and the DSS website. NED is managed by the JPL (Caltech) under contract with NASA, whereas DSS is managed by the Space Telescope Science Institute (U.S. grant number NAG W-2166). We also used IR and UV images of NGC 1566 from the Spitzer Space Telescope and the NASA Galaxy Evolution Explorer websites, both space missions were managed by JPL under contract with NASA.