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 & 8 others J. Wang, C. S. Anderson, J. D. Bunton, G. Bekiaris, W. M. Walsh, V. A. Kilborn, P. Kamphuis, S. -H. Oh

Research output: Contribution to journalArticle

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 km s(-1) emanating from this galaxy, which translates to an HI mass of 1.94 x 10(10) M-circle dot 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 (M-HI/M-*) of NGC 1566 is 0.29, which is high in comparison with galaxies that have the same stellar mass (10(10.8) M-circle dot). 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 x 10(19) 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 languageEnglish
Pages (from-to)2797-2817
Number of pages21
JournalMonthly Notices of the Royal Astronomical Society
Volume487
Issue number2
DOIs
Publication statusPublished - Aug 2019

Cite this

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. ; Shao, L. ; Wang, J. ; Anderson, C. S. ; Bunton, J. D. ; Bekiaris, G. ; Walsh, W. M. ; Kilborn, V. A. ; Kamphuis, P. ; Oh, S. -H. / WALLABY early science - III. An HI study of the spiral galaxy NGC 1566. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 487, No. 2. pp. 2797-2817.
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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 km s(-1) emanating from this galaxy, which translates to an HI mass of 1.94 x 10(10) M-circle dot 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 (M-HI/M-*) of NGC 1566 is 0.29, which is high in comparison with galaxies that have the same stellar mass (10(10.8) M-circle dot). 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 x 10(19) 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, MORPHOLOGY-DENSITY RELATION, DARK-MATTER HALO, RESOLUTION ROTATION CURVES, INFRARED ARRAY CAMERA, I-DEFICIENT GALAXIES, STAR-FORMATION, ENVIRONMENTAL DEPENDENCE, NEUTRAL HYDROGEN, REDSHIFT SURVEY, VIRGO CLUSTER",
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.}",
year = "2019",
month = "8",
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 UNIV PRESS UNITED KINGDOM",
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Elagali, A, Staveley-Smith, L, Rhee, J, Wong, OI, Bosma, A, Westmeier, T, Koribalski, BS, Heald, G, For, B-Q, 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, S-H 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

WALLABY early science - III. An HI study of the spiral galaxy NGC 1566. / 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.; Shao, L.; Wang, J.; Anderson, C. S.; Bunton, J. D.; Bekiaris, G.; Walsh, W. M.; Kilborn, V. A.; Kamphuis, P.; Oh, S. -H.

In: Monthly Notices of the Royal Astronomical Society, Vol. 487, No. 2, 08.2019, p. 2797-2817.

Research output: Contribution to journalArticle

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 - 2019/8

Y1 - 2019/8

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 km s(-1) emanating from this galaxy, which translates to an HI mass of 1.94 x 10(10) M-circle dot 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 (M-HI/M-*) of NGC 1566 is 0.29, which is high in comparison with galaxies that have the same stellar mass (10(10.8) M-circle dot). 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 x 10(19) 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 km s(-1) emanating from this galaxy, which translates to an HI mass of 1.94 x 10(10) M-circle dot 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 (M-HI/M-*) of NGC 1566 is 0.29, which is high in comparison with galaxies that have the same stellar mass (10(10.8) M-circle dot). 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 x 10(19) 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

KW - MORPHOLOGY-DENSITY RELATION

KW - DARK-MATTER HALO

KW - RESOLUTION ROTATION CURVES

KW - INFRARED ARRAY CAMERA

KW - I-DEFICIENT GALAXIES

KW - STAR-FORMATION

KW - ENVIRONMENTAL DEPENDENCE

KW - NEUTRAL HYDROGEN

KW - REDSHIFT SURVEY

KW - VIRGO CLUSTER

U2 - 10.1093/mnras/stz1448

DO - 10.1093/mnras/stz1448

M3 - Article

VL - 487

SP - 2797

EP - 2817

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -