An H I aperture synthesis mosaic of the Small Magellanic Cloud

Stavely-Smith, L.; Saul, Rappaport; Hatzidimitriou, D.; Kesteven, M. J.; McConnell, D.

doi:10.1093/mnras/289.2.225

Cited by 151 publications

(48 citation statements)

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“…The SMC HI data set used in our analysis combines both single dish (Parkes, Stanimirovic et al 1999) and interferometer (ATCA, Staveley-Smith et al 1997) data. Both sets of observations were then combined (see Stanimirovic et al 1999), resulting in the final HI data cube with an angular resolution of 98″, velocity resolution of 1.65 km s −1 , and 1σ brightness temperature sensitivity of 1.3 K. The data has a continuous range of spatial scales between 30 and 4 kpc.…”

Section: The Smc In Hi: a Test Galaxy For Turbulence Studiesmentioning

confidence: 99%

“…The velocity range of the observations is 90-215 km s −1 . For more details about the ATCA and Parkes observations, data processing, and data combination (short spacing corrections) see Staveley-Smith et al (1997) and Stanimirovic et al (1999). HI self-absorption were corrected for following the scheme of Stanimirovic et al (1999).…”

Section: The Smc In Hi: a Test Galaxy For Turbulence Studiesmentioning

confidence: 99%

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The Turbulence Velocity Power Spectrum of Neutral Hydrogen in the Small Magellanic Cloud

Chepurnov

Burkhart

Lazarían

et al. 2015

ApJ

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We present the results of the Velocity Coordinate Spectrum (VCS) technique to calculate the velocity power spectrum of turbulence in the Small Magellanic Cloud (SMC) in 21 cm emission. We present an updated version of the VCS technique that takes into account regular motions, which is an important factor in our SMC VCS analysis. We have obtained a velocity spectral index of −3.85, a cold phase sonic Mach number of 5.6, and an injection scale of 2.3 kpc. The spectral index is steeper than the Kolmogorov index, which is expected for shock-dominated turbulence. The injection scale of 2.3 kpc suggests that HI supershells or tidal interactions with the Large Magellanic Cloud are the dominant drivers of turbulence in this dwarf galaxy. This implies that turbulence may be driven by multiple mechanisms in galaxies and that galaxy-galaxy interactions may play an important role in addition to supernova feedback.

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Section: The Smc In Hi: a Test Galaxy For Turbulence Studiesmentioning

confidence: 99%

Section: The Smc In Hi: a Test Galaxy For Turbulence Studiesmentioning

confidence: 99%

The Turbulence Velocity Power Spectrum of Neutral Hydrogen in the Small Magellanic Cloud

Chepurnov

Burkhart

Lazarían

et al. 2015

ApJ

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“…To this end, extensive mappings of the MCs have recently been conducted at a number of wavelengths. Surveys have been made in H i emission at 21 cm (H i Parkes All-Sky Survey [HIPASS]; Barnes et al 2001;Brüns et al 2005;Staveley-Smith et al 1997Stanimirović et al 1999;and Muller et al 2003), in molecular spectral CO lines (NANTEN; Fukui et al 1999;Mizuno et al 2001), as well as in the radio continuum (Haynes et al 1991: Dickel et al 2005, in the thermal infrared (Infrared Astronomical Satellite [IRAS]: Beichman et al 1988; Midcourse Space Experiment [MSX]: Mill et al 1994; Surveying the Agents of a Galaxy's Evolution [SAGE]: Meixner et al 2006; Spitzer Survey of the Small Magellanic Cloud [S 3 MC]: Bolatto et al 2007), in the near-infrared (Deep Near Infrared Survey of the Southern Sky [DENIS]: Epchtein et al 1997; Two Micron All-Sky Survey [2MASS]: Skrutskie et al 2006), in broadband optical colors ( Magellanic Clouds Photometric Survey [MCPS]: Zaritsky et al 2002Zaritsky et al , 2004 as well as in optical emission lines (Magellanic Cloud Emission Line Survey [MCELS]: Smith et al 1998), and at ultraviolet (Smith et al 1987) and X-ray wavelengths (ROSAT: Snowden & Petre 1994; Chandra and ACIS: Townsley et al 2006). While these surveys have deepened our understanding of the Clouds themselves-e.g., their star formation history, their stellar content, and their overall structure (van der Marel 2001)-the H i investigations are central to understanding the most obvious product of the MW-MC interactionthe Magellanic Stream.…”

Section: Introductionmentioning

confidence: 99%

The Origin of the Magellanic Stream and Its Leading Arm

Nidever

Majewski

Burton

2008

ApJ

249

444

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We explore the Magellanic Stream (MS) using a Gaussian decomposition of the HI velocity profiles in the Leiden-Argentine-Bonn (LAB) all-sky HI survey. This decomposition exposes the MS to be composed of two filaments distinct both spatially (as first pointed out by Putman et al.) and in velocity. Using the velocity coherence of the filaments, one can be traced back to its origin in what we identify as the SouthEast HI Overdensity (SEHO) of the Large Magellanic Cloud (LMC), which includes 30 Doradus. Parts of the Leading Arm (LA) can also be traced back to the SEHO in velocity and position. Therefore, at least one-half of the trailing Stream and most of the LA originates in the LMC, contrary to previous assertions that both the MS and the LA originate in the Small Magellanic Cloud (SMC) and/or in the Magellanic Bridge. The two MS filaments show strong periodic, undulating spatial and velocity patterns that we speculate are an imprint of the LMC rotation curve. If true, then the drift rate of the Stream gas away from the Magellanic Clouds is ~49 km/s and the age of the MS is ~1.74 Gyr. The Staveley-Smith et al. high-resolution HI data of the LMC show gas outflows from supergiant shells in the SEHO that seem to be creating the LA and LMC filament of the MS. Blowout of LMC gas is an effect not previously accounted for but one that probably plays an important role in creating the MS and LA.Comment: 31 pages, 26 figures, Accepted for publication in Ap

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“…To this end, extensive mappings of the MCs have recently been conducted at a number of wavelengths. Surveys have been made in H I emission at 21-cm (HIPASS: Barnes et al 2001;Brüns et al 2005;Staveley-Smith et al 1997Stanimirović et al 1999;and Muller et al 2003), in molecular spectral CO lines (NANTEN: Fukui et al 1999;Mizuno et al 2001), as well as in the radio continuum (Haynes et al 1991;Dickel et al 2005), in the thermal infrared (IRAS: Beichman et al 1988;MSX: Mill et al 1994;SAGE: Meixner et al 2006; S 3 MC: Bolatto et al 2007), in the nearinfrared (DENIS: Epchtein et al 1997;2MASS: Skrutskie et al 2006), in broadband optical colors (MCPS: Zaritsky et al 2002Zaritsky et al , 2004 as well as in optical emission lines (MCELS: Smith et al 1998), and at ultraviolet (Smith, Cornett & Hill 1987) and X-ray wavelengths (ROSAT: Snowden & Petre 1994; Chandra and ACIS: Townsley et al 2006). While these surveys have deepened our understanding of the Clouds themselves -e.g., their star formation history, their stellar content, and their overall structure (van der Marel 2001) -the H I investigations are central to understanding the most obvious product of the MW-MC interaction -the Magellanic Stream.…”

Section: Introductionmentioning

confidence: 99%

The Origin of the Magellanic Stream and its Leading Arm

Nidever

Majewski

Burton

2008

Astrophysics and Space Science Proceedings

View full text Add to dashboard Cite

We explore the Magellanic Stream (MS) using a Gaussian decomposition of the H I velocity profiles in the Leiden-Argentine-Bonn (LAB) all-sky H I survey. This decomposition exposes the MS to be composed of two filaments distinct both spatially (as first pointed out by Putman et al.) and in velocity. Using the velocity coherence of the filaments, one can be traced back to its origin in what we identify as the SouthEast H I Overdensity (SEHO) of the Large Magellanic Cloud (LMC), which includes 30 Doradus. Parts of the Leading Arm (LA) can also be traced back to the SEHO in velocity and position. Therefore, at least one-half of the trailing Stream and most of the LA originates in the LMC, contrary to previous assertions that both the MS and the LA originate in the Small Magellanic Cloud (SMC) and/or in the Magellanic Bridge. The two MS filaments show strong periodic, undulating spatial and velocity patterns that we speculate are an imprint of the LMC rotation curve. If true, then the drift rate of the Stream gas away from the Magellanic Clouds is ∼49 km s −1 and the age of the MS is ∼1.74 Gyr. The Staveley-Smith et al. high-resolution H I data of the LMC show gas outflows from supergiant shells in the SEHO that seem to be creating the LA and LMC filament of the MS. Blowout of LMC gas is an effect not previously accounted for but one that probably plays an important role in creating the MS and LA.

show abstract

An H I aperture synthesis mosaic of the Small Magellanic Cloud

Cited by 151 publications

References 0 publications

The Turbulence Velocity Power Spectrum of Neutral Hydrogen in the Small Magellanic Cloud

The Turbulence Velocity Power Spectrum of Neutral Hydrogen in the Small Magellanic Cloud

The Origin of the Magellanic Stream and Its Leading Arm

The Origin of the Magellanic Stream and its Leading Arm

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