2014
DOI: 10.1088/0004-637x/787/2/147
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The Cos/Uves Absorption Survey of the Magellanic Stream. Iii. Ionization, Total Mass, and Inflow Rate Onto the Milky Way

Abstract: Dynamic interactions between the two Magellanic Clouds have flung large quantities of gas into the halo of the Milky Way. The result is a spectacular arrangement of gaseous structures including the Magellanic Stream, the Magellanic Bridge, and the Leading Arm (collectively referred to as the Magellanic System). In this third paper of a series studying the Magellanic gas in absorption, we analyze the gas ionization level using a sample of 69 Hubble Space Telescope/Cosmic Origins Spectrograph sightlines that pas… Show more

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Cited by 158 publications
(283 citation statements)
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References 150 publications
(182 reference statements)
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“…A.1), much of this negative-velocity gas is related to the MS, which has a very large cross section on the sky (see Sect. 5.1; Fox et al 2014). In addition, some of this ionized material at high negative velocities possibly is related to UV-absorbing LG gas in the general direction of the LG barycenter (see Sembach et al 2003).…”
Section: Interpretation Of Observed Trendsmentioning
confidence: 99%
“…A.1), much of this negative-velocity gas is related to the MS, which has a very large cross section on the sky (see Sect. 5.1; Fox et al 2014). In addition, some of this ionized material at high negative velocities possibly is related to UV-absorbing LG gas in the general direction of the LG barycenter (see Sembach et al 2003).…”
Section: Interpretation Of Observed Trendsmentioning
confidence: 99%
“…Ram pressure stripping by the CGM of the host galaxy is thought to be the dominant stripping mechanism, but other forces can be important, for instance when satellites come in as an interacting pair (Pearson et al, 2016;Marasco et al, 2016). The gas is largely heated when it is ram pressure stripped (Tepper-García et al, 2015;Gatto et al, 2013;Fox et al, 2014), and (again) it is not completely clear how it ultimately cools to feed the galaxy's star formation. It may sink to the disk as density enhancements in the halo and ultimately cool closer to the disk as it slows and encounters a denser surrounding medium (Heitsch & Putman, 2009;Joung et al, 2012b;Bland-Hawthorn et al, 2007).…”
Section: Expected Modes Of Accretionmentioning
confidence: 99%
“…Most of the gas thought to be in the halo of the Milky Way has unknown distances. The only halo gas known to be at large radii is that associated with the Magellanic System (Putman et al, 2003;Fox et al, 2014). It is difficult to say when the gas of Magellanic origin will accrete as it is likely to have a large tangential velocity component and will slow and be heated as it falls.…”
Section: Direct Observational Evidence For Accretionmentioning
confidence: 99%
“…This gas presumably came from the Magellanic clouds during their interaction with each other (Diaz and Bekki 2012) and is now experiencing a drag force from its motion in the hot MW halo gas (Mastropietro et al 2005). Taking into account the neutral and ionized gas, the Magellanic stream contains 2 × 10 9 M at a distance of 55 kpc (Fox et al 2014). If the gas in the Magellanic system survives to reach the MW disk over its inflow time of ∼0.5-1.5 Gyr, it will represent an average inflow rate of 4-7 M year −1 potentially raising the current MW SFR.…”
Section: Neutral Gas Observationsmentioning
confidence: 99%
“…Multiple signs of an evaporative interaction with the hot halo indicate that the stream may not survive its journey to the disk fully intact. It will break apart by hydrodynamic instabilities and evaporate, contributing the hot halo mass (Bland-Hawthorn et al 2007;Fox et al 2014).…”
Section: Neutral Gas Observationsmentioning
confidence: 99%