A New Look at the Kinematics of Neutral Hydrogen in the Small Magellanic Cloud

By S. Stanimirović, L. Staveley-Smith, P. J. U. Berkeley, Atnf. 2003

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We have used the latest H I observations of the Small Magellanic Cloud (SMC), obtained with the Australia Telescope Compact Array and the Parkes telescope, to reexamine the kinematics of this dwarf irregular galaxy. A large velocity gradient is found in the H I velocity field, with a significant symmetry in isovelocity contours, suggestive of a differential rotation. A comparison of H I data with the predictions from tidal models for the SMC evolution suggests that the central region of the SMC corresponds to the central disklike or barlike component left from the rotationally supported SMC disk prior to its last two encounters with the Large Magellanic Cloud. In this scenario, the velocity gradient is expected as a leftover from the original, preencounter angular momentum. We have derived the H I rotation curve and the mass model for the SMC. This rotation curve rapidly rises to about 60 km s-1 up to the turnover radius of ~3 kpc. A stellar mass-to-light ratio of about unity is required to match the observed rotation curve, suggesting that a dark matter halo is not needed to explain the dynamics of the SMC. A set of derived kinematic parameters agrees well with the assumptions used in tidal theoretical models that led to a good reproduction of observational properties of the Magellanic System. The dynamical mass of the SMC, derived from the rotation curve, is 2.4 × 109 M☉.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/837011c5b4f054c9203a5d4d71f59d831c2e0230

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Citations in the corpus

THE ATOMIC-TO-MOLECULAR TRANSITION IN GALAXIES. II: H i AND H2 COLUMN DENSITIES (2008, methodology): “This survey differs from the SONG and THINGS data sets in that those surveys infer the presence of H2 via CO emission, whereas S3MC measures molecular hydrogen using measurements of dust from Spitzer combined with Hi measurements by Stanimirovic et al. (1999) and Stanimirović et al. (2004).”
The Parkes HI survey of the Magellanic System (2004, methodology): “…angular resolution were performed by Kim et al. (1998, 2003) Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20040321 for the LMC and by Stanimirovic et al. (1999, 2004) for the SMC, using the Australia Telescope Compact Array (ATCA).”
THIRD-EPOCH MAGELLANIC CLOUD PROPER MOTIONS. I. HUBBLE SPACE TELESCOPE/WFC3 DATA AND ORBIT IMPLICATIONS (2013, methodology): “To calculate a PM model prediction for each observed field, we keep the SMC center fixed at the H I kinematical center (α, δ) = (16.25◦,−72.42◦) (Stanimirović et al. 2004), the distance modulus fixed at m − M = 18.99 (Cioni et al. 2000), and the radial velocity fixed at vsys = 145.6 km s−1 (Harris…”
Too big to fail? The puzzling darkness of massive Milky Way subhaloes (2011, result): “Conservatively, we estimate that the Magellanic Clouds have Vinfall > 60 km s −1 and Vmax(z = 0) > 40 km s −1 (Stanimirović et al. 2004; Olsen & Massey 2007) and remove all subhaloes with these properties from our sample of subhaloes that are inconsistent with the dynamics of the bright MW dwarfs.”
A timing constraint on the (total) mass of the Large Magellanic Cloud (2015, methodology): “Application of the Tully-Fisher (1977) relation to the peak velocities of the SMC and LMC measured by Stanimirović et al. (2004) and van der Marel & Kallivayalil (2014), respectively, yields MSMC/MLMC ∼ (60kms−1/90kms−1)4 ∼ 0.2.”
Scaling relations and the fundamental line of the local group dwarf galaxies (2008, unknown): “…Larsen et al. (2000); (12) Lee et al. (1999); (13) Lee et al. (2002); (14) Mateo (1998); (15) Richer et al. (2001); (16) Schlegel et al. (1998); (17) Stanimirović et al. (2004); (18) Tiede et al. (2004); (19) van den Bergh (2000); (20) Zaritsky et al. (1989); through BdJ are generally slightly…”
THE STATE OF THE GAS AND THE RELATION BETWEEN GAS AND STAR FORMATION AT LOW METALLICITY: THE SMALL MAGELLANIC CLOUD (2011, methodology): “The underlying dynamics appear to be disk-like with an inclination i ≈ 40◦± 20◦, although disturbed by the interaction with the Milky Way and the LMC (Stanimirović et al. 2004).”
Cool outflows in galaxies and their implications (2020, background): “2004) and the escape velocity of the SMC (vesc ' 1.4 − 3 vcirc ' 85 − 180 km s−1, where vcirc = 60 km s−1; Stanimirović et al. 2004), McClure-Griffiths et al.”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, background): “The SMC has a total stellar mass of approximately 3 × 108 M (Stanimirović et al. 2004), corresponding to an abundance matching mass at accretion of 8.2 × 1010M .”
SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW (2011, background): “The far-infrared 70 & 160 µm observations trace the dust column density and, combined with the interferometric HI (Muller et al. 2003; Stanimirović et al. 2004) and CO (Mizuno et al. 2001, 2006) observations, measures the gas-to-dust variations across the whole SMC. Preliminary results from…”
The missing massive satellites of the Milky Way (2012, methodology): “Assuming that Vmax for the LMC and SMC can be identified with the rotation speed of their HI disks, or 60 and 50 km/s, respectively (Kim et al. 1998; Stanimirović et al. 2004), we find, using the data in Table 1, that only ∼ 62% of V200 = 150 km/s halos would be expected not to host an LMC-like…”
The Spitzer Survey of the Small Magellanic Cloud: S3MC Imaging and Photometry in the Mid- and Far-Infrared Wave Bands (2006, background): “INTRODUCTION The SmallMagellanic Cloud (SMC), one of the closest andmost prominent neighbors of the Milky Way, is a southern hemisphere dwarf galaxy of low mass (Mdyn 2:4 ; 109 M ; Stanimirović et al. 2004) and small size (R 3 kpc).”
Small Dwarf Galaxies within Larger Dwarfs: Why Some Are Luminous while Most Go Dark (2008, methodology): “This “LMC group” was dominated by the LMC and had a parent halo circular velocity of 75 km s−1 (Kim et al. 1998) with its brightest satellite, the SMC, having a rotation velocity of 60 km s−1 as estimated from its HI distribution (Stanimirovic et al. 2004).”