Tidal disruption of the Magellanic Clouds by the Milky Way

Putman, M. E.; Gibson, Brad K.; Staveley‐Smith, L.; Banks, G. D.; Barnes, David G.; Bhatal, R.; Disney, M. J.; Ekers, R. D.; Freeman, K. C.; Haynes, R. F.; Henning, P. A.; Jerjen, Helmut; Kilborn, V. A.; Koribalski, B. S.; Knezek, Patricia; Malin, D. F.; Mould, Jeremy; Oosterloo, Tom; Price, R. M.; Ryder, S. D.; Sadler, E. M.; Stewart, I. M.; Stootman, F.; Vaile, R. A.; Webster, R. L.; Wright, A. E.

doi:10.1038/29466

Cited by 246 publications

(259 citation statements)

References 18 publications

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“…Spectacular systems such as the Antennae (Arp 1966 ;Toomre & Toomre 1972) and the Cartwheel galaxy (Struck-Marcell & Higdon 1993 ;Higdon 1996) are extreme examples of distortion caused by nearby companions. Locally, the Magellanic Stream o †ers a close-up view of a system dominated by the gravitational Ðeld of the Milky Way Galaxy (Putman et al 1998). Intense infrared emission appears to be triggered by strong interactions between spiral galaxies that are rich in molecular gas (Sanders & Mirabel 1996), and there is evidence that low surface brightness (LSB) galaxies accompanied by nearby dwarf galaxies will be rapidly transformed into starbursting blue compact galaxies because of tidal e †ects (Taylor 1997).…”

Section: Introductionmentioning

confidence: 99%

On the Neutral Gas Content and Environment of NGC 3109 and the Antlia Dwarf Galaxy

Barnes

Blok

2001

The Astronomical Journal

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As part of a continuing survey of nearby galaxies, we have mapped the neutral gas content of the low surface brightness Magellanic-type galaxy NGC 3109 and its environment, including the Antlia dwarf galaxy, at unprecedented velocity resolution and brightness sensitivity. The H I mass of NGC 3109 is measured to be 3.8^0.5 ] 108A substantial warp in the disk of NGC 3109 is detected in the H I M _ . emission image in the form of an extended low surface brightness feature. We report a positive detection in H I of the nearby Antlia dwarf galaxy and measure its total neutral gas mass to be 6.8^1.4 ] 105We show the warp in NGC 3109 to lie at exactly the same radial velocity as the gas in the Antlia M _ . dwarf galaxy and speculate that Antlia disturbed the disk of NGC 3109 during a mild encounter D1 Gyr in the past. H I data for a further eight galaxies detected in the background are presented.

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Section: Introductionmentioning

confidence: 99%

On the Neutral Gas Content and Environment of NGC 3109 and the Antlia Dwarf Galaxy

Barnes

Blok

2001

The Astronomical Journal

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“…The ongoing interaction with the Milky Way also allows us to study in detail the complex mechanisms that rule the interaction among galaxies (see e.g. Putman et al 1998;Muller et al 2004;Stanimirović et al 2004;Bekki & Chiba 2007;Venzmer, Kerp & Kalberla 2012;For, Staveley-Smith & McClure-Griffiths 2013). Additionally, the MCs are more metal poor than our Galaxy and host a large population of young populous clusters, thus they are useful to test the physical and numerical assumptions at the basis of stellar evolution codes (see e.g.…”

Section: Introductionmentioning

confidence: 99%

The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

Ripepi

Moretti

Marconi

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The VISTA survey of the Magellanic Clouds System (VMC) is collecting deep K s -band time-series photometry of the pulsating variable stars hosted in the system formed by the two Magellanic Clouds and the Bridge connecting them. In this paper we have analysed a sample of 130 Large Magellanic Cloud (LMC) Type II Cepheids (T2CEPs) found in tiles with complete or near complete VMC observations for which identification and optical magnitudes were obtained from the OGLE III survey. We present J and K s light curves for all 130 pulsators, including 41 BL Her, 62 W Vir (12 pW Vir) and 27 RV Tau variables. We complement our near-infrared photometry with the V magnitudes from the OGLE III survey, allowing us to build a variety of PeriodLuminosity (P L), Period-Luminosity-Colour (P LC) and Period-Wesenheit (P W ) relationships, including any combination of the V, J, K s filters and valid for BL Her and W Vir classes. These relationships were calibrated in terms of the LMC distance modulus, while an independent absolute calibration of the P L(K s ) and the P W (K s , V ) was derived on the basis of distances obtained from Hubble Space T elescope parallaxes and Baade-Wesselink technique. When applied to the LMC and to the Galactic Globular Clusters hosting T2CEPs, these relations seem to show that: 1) the two population II standard candles RR Lyrae and T2CEPs give results in excellent agreement with each other; 2) there is a discrepancy of ∼0.1 mag between population II standard candles and Classical Cepheids when the distances are gauged in a similar way for all the quoted pulsators. However, given the uncertainties, this discrepancy is within the formal 1σ uncertainties.

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“…As a consequence it is very likely that this spiral-like structure has been generated by external effects to M31, either by tidal effects after the passage of a galaxy satellite or even by gas accretion from the intergalactic medium or from a former gas rich companion (NGC 205?). It is also remarkable how this external structure has a similar mass as the Magellanic Stream in the halo of the Milky Way ( [12]). Numerical simulations are necessary to investigate the different possibilities and find the origin of the faint new perturbations.…”

Section: Resultsmentioning

confidence: 99%

Deep wide field HI imaging of M31

Chemin¹,

Carignan²,

Foster³

2010

Proceedings of Panoramic Radio Astronomy: Wide-Field 1-2 GHz Research on Galaxy Evolution — PoS(PRA2009)

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We report on preliminary results from a new deep 21-cm survey of the Andromeda galaxy, based on observations performed with the Synthesis Telescope and the 26-m antenna at DRAO. The HI distribution and kinematics of the disc are analyzed and basic dynamical properties are derived. New HI structures are discovered, like thin HI spur-like structures and an external arm in the disc outskirts. The HI spurs are related to perturbed stellar clumps outside the main disc of M31. The external arm lies on the far, receding side of the galaxy and has no obvious counterpart in the opposite side. These HI perturbations probably result from tidal interactions with companions. It is found a dynamical mass of (4.7 ± 0.5) × 10 11 M ⊙ enclosed within a radius R = 38 kpc and a total mass of ∼ 1 × 10 12 M ⊙ inside the virial radius.

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Tidal disruption of the Magellanic Clouds by the Milky Way

Cited by 246 publications

References 18 publications

On the Neutral Gas Content and Environment of NGC 3109 and the Antlia Dwarf Galaxy

On the Neutral Gas Content and Environment of NGC 3109 and the Antlia Dwarf Galaxy

The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

Deep wide field HI imaging of M31

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