WALLABY early science - III. An HI study of the spiral galaxy NGC 1566

A. Elagali; L. Staveley-Smith; J. Rhee; O. I. Wong; A. Bosma; T. Westmeier; B. S. Koribalski; G. Heald; B. Q. For; D. Kleiner; K. Lee-Waddell; J. P. Madrid; A. Popping; T. N. Reynolds; M. J. Meyer; J. R. Allison; C. D.P. Lagos; M. A. Voronkov; P. Serra; L. Shao; J. Wang; C. S. Anderson; J. D. Bunton; G. Bekiaris; W. M. Walsh; V. A. Kilborn; P. Kamphuis; S. H. Oh

doi:10.1093/mnras/stz1448

WALLABY early science - III. An HI study of the spiral galaxy NGC 1566

A. Elagali^*, L. Staveley-Smith, J. Rhee, O. I. Wong, A. Bosma, T. Westmeier, B. S. Koribalski, G. Heald, B. Q. For, D. Kleiner, K. Lee-Waddell, J. P. Madrid, A. Popping, T. N. Reynolds, M. J. Meyer, J. R. Allison, C. D.P. Lagos, M. A. Voronkov, P. Serra, L. ShaoJ. Wang, C. S. Anderson, J. D. Bunton, G. Bekiaris, W. M. Walsh, V. A. Kilborn, P. Kamphuis, S. H. Oh

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

44 Citations (Scopus)

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, Burkert, and pseudo-isothermal darkmatter halo profiles fit the observed rotation curve reasonably well and recover dark matter fractions of 0.62, 0.58, and 0.66, respectively. Down to the column density sensitivity of our observations (NHI = 3.7 × 1019 cm-2), we detect no HI clouds connected to, or in the nearby vicinity of, the HI disc of NGC 1566 nor nearby interacting systems. We conclude that, based on a simple analytic model, ram pressure interactions with the IGM can affect the HI disc of NGC 1566 and is possibly the reason for the asymmetries seen in the HI morphology of NGC 1566.

Original language	English
Pages (from-to)	2797-2817
Number of pages	21
Journal	Monthly Notices of the Royal Astronomical Society
Volume	487
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stz1448
Publication status	Published - 2019

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Elagali, A., Staveley-Smith, L., Rhee, J., Wong, O. I., Bosma, A., Westmeier, T., Koribalski, B. S., Heald, G., For, B. Q., Kleiner, D., Lee-Waddell, K., Madrid, J. P., Popping, A., Reynolds, T. N., Meyer, M. J., Allison, J. R., Lagos, C. D. P., Voronkov, M. A., Serra, P., ... Oh, S. H. (2019). WALLABY early science - III. An HI study of the spiral galaxy NGC 1566. Monthly Notices of the Royal Astronomical Society, 487(2), 2797-2817. https://doi.org/10.1093/mnras/stz1448

@article{80e3e10e88194a7891505fec9e7dceca,

title = "WALLABY early science - III. An HI study of the spiral galaxy NGC 1566",

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, Burkert, and pseudo-isothermal darkmatter halo profiles fit the observed rotation curve reasonably well and recover dark matter fractions of 0.62, 0.58, and 0.66, respectively. Down to the column density sensitivity of our observations (NHI = 3.7 × 1019 cm-2), we detect no HI clouds connected to, or in the nearby vicinity of, the HI disc of NGC 1566 nor nearby interacting systems. We conclude that, based on a simple analytic model, ram pressure interactions with the IGM can affect the HI disc of NGC 1566 and is possibly the reason for the asymmetries seen in the HI morphology of NGC 1566.",

keywords = "Galaxies: Individual: NGC 1566, Galaxies: Kinematics and dynamics, Galaxies: Starburst, Radio lines: Galaxies",

author = "A. Elagali and L. Staveley-Smith and J. Rhee and Wong, {O. I.} and A. Bosma and T. Westmeier and Koribalski, {B. S.} and G. Heald and For, {B. Q.} and D. Kleiner and K. Lee-Waddell and Madrid, {J. P.} and A. Popping and Reynolds, {T. N.} and Meyer, {M. J.} and Allison, {J. R.} and Lagos, {C. D.P.} and Voronkov, {M. A.} and P. Serra and L. Shao and J. Wang and Anderson, {C. S.} and Bunton, {J. D.} and G. Bekiaris and Walsh, {W. M.} and Kilborn, {V. A.} and P. Kamphuis and Oh, {S. H.}",

note = "Publisher Copyright: {\textcopyright} 2019 The Author(s).",

year = "2019",

doi = "10.1093/mnras/stz1448",

language = "English",

volume = "487",

pages = "2797--2817",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press ",

number = "2",

}

Elagali, A, Staveley-Smith, L, Rhee, J, Wong, OI, Bosma, A, Westmeier, T, Koribalski, BS, Heald, G, For, BQ, Kleiner, D, Lee-Waddell, K, Madrid, JP, Popping, A, Reynolds, TN, Meyer, MJ, Allison, JR, Lagos, CDP, Voronkov, MA, Serra, P, Shao, L, Wang, J, Anderson, CS, Bunton, JD, Bekiaris, G, Walsh, WM, Kilborn, VA, Kamphuis, P & Oh, SH 2019, 'WALLABY early science - III. An HI study of the spiral galaxy NGC 1566', Monthly Notices of the Royal Astronomical Society, vol. 487, no. 2, pp. 2797-2817. https://doi.org/10.1093/mnras/stz1448

TY - JOUR

T1 - WALLABY early science - III. An HI study of the spiral galaxy NGC 1566

AU - Elagali, A.

AU - Staveley-Smith, L.

AU - Rhee, J.

AU - Wong, O. I.

AU - Bosma, A.

AU - Westmeier, T.

AU - Koribalski, B. S.

AU - Heald, G.

AU - For, B. Q.

AU - Kleiner, D.

AU - Lee-Waddell, K.

AU - Madrid, J. P.

AU - Popping, A.

AU - Reynolds, T. N.

AU - Meyer, M. J.

AU - Allison, J. R.

AU - Lagos, C. D.P.

AU - Voronkov, M. A.

AU - Serra, P.

AU - Shao, L.

AU - Wang, J.

AU - Anderson, C. S.

AU - Bunton, J. D.

AU - Bekiaris, G.

AU - Walsh, W. M.

AU - Kilborn, V. A.

AU - Kamphuis, P.

AU - Oh, S. H.

PY - 2019

Y1 - 2019

N2 - 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, Burkert, and pseudo-isothermal darkmatter halo profiles fit the observed rotation curve reasonably well and recover dark matter fractions of 0.62, 0.58, and 0.66, respectively. Down to the column density sensitivity of our observations (NHI = 3.7 × 1019 cm-2), we detect no HI clouds connected to, or in the nearby vicinity of, the HI disc of NGC 1566 nor nearby interacting systems. We conclude that, based on a simple analytic model, ram pressure interactions with the IGM can affect the HI disc of NGC 1566 and is possibly the reason for the asymmetries seen in the HI morphology of NGC 1566.

AB - 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, Burkert, and pseudo-isothermal darkmatter halo profiles fit the observed rotation curve reasonably well and recover dark matter fractions of 0.62, 0.58, and 0.66, respectively. Down to the column density sensitivity of our observations (NHI = 3.7 × 1019 cm-2), we detect no HI clouds connected to, or in the nearby vicinity of, the HI disc of NGC 1566 nor nearby interacting systems. We conclude that, based on a simple analytic model, ram pressure interactions with the IGM can affect the HI disc of NGC 1566 and is possibly the reason for the asymmetries seen in the HI morphology of NGC 1566.

KW - Galaxies: Individual: NGC 1566

KW - Galaxies: Kinematics and dynamics

KW - Galaxies: Starburst

KW - Radio lines: Galaxies

UR - http://www.scopus.com/inward/record.url?scp=85075241370&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz1448

DO - 10.1093/mnras/stz1448

M3 - Article

SN - 0035-8711

VL - 487

SP - 2797

EP - 2817

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

WALLABY early science - III. An HI study of the spiral galaxy NGC 1566

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