H i IN LOCAL GROUP DWARF GALAXIES AND STRIPPING BY THE GALACTIC HALO

By J. Grcevich, M. Putman. 2009

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We examine the H i content and environment of all of the Local Group dwarf galaxies (Mtot < 1010 M☉), including the numerous newly discovered satellites of the Milky Way and M31. All of the new dwarfs, with the exception of Leo T, have no detected H i. The majority of dwarf galaxies within ∼270 kpc of the Milky Way or Andromeda are undetected in H i (<104 M☉ for Milky Way dwarfs), while those further than ∼270 kpc are predominantly detected with masses ∼105 to 108 M☉. Analytical ram-pressure arguments combined with velocities obtained via proper motion studies allow for an estimate of the halo density of the Milky Way at several distances. This halo density is constrained to be greater than 2× 10−4–3 × 10−4 cm−3 out to distances of at least 70 kpc. This is broadly consistent with theoretical models of the diffuse gas in a Milky Way-like halo and is consistent with this component hosting a large fraction of a galaxy's baryons. Accounting for completeness in the dwarf galaxy count, gasless dwarf galaxies could have provided at most 2.1 × 108 M☉ of H i gas to the Milky Way, which suggests that most of our Galaxy's star formation fuel does not come from accreted small satellites in the current era.

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Citations in the corpus

Galactic Searches for Dark Matter (2012, background): “Indeed, the very strict upper limits on star formation processes and the gas content of these systems predicts a negligible gamma-ray flux from these sources (Grcevich and Putman, 2009).”
EIGHT NEW MILKY WAY COMPANIONS DISCOVERED IN FIRST-YEAR DARK ENERGY SURVEY DATA (2015, background): “…and M31 are almost exclusively early-type galaxies with no gas or recent star formation, while dwarfs beyond that limit often have irregular morphologies, contain gas, and/or are still forming stars (e.g., Einasto et al. 1974; Blitz & Robishaw 2000; Grcevich & Putman 2009; Spekkens et al. 2014).”
THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, background): “For example, they have very different gas fractions (Grcevich & Putman 2009), and even their metallicity distributions are shaped differently.”
Quenching and ram pressure stripping of simulated Milky Way satellite galaxies (2017, background): “Few satellites within 270 kpc of either the MW or M31 contain detectable H I gas and most systems beyond this distance do contain H I (Grcevich & Putman 2009), sometimes in significant amounts (RyanWeber et al. 2008).”
Too big to fail in the Local Group (2014, background): “Measurements for the field dwarfs are from Kirby et al. (2014) where available; the constraints on Leo T and Tucana are from Simon & Geha (2007) and Fraternali et al. (2009), respectively.”
THE SPACE MOTION OF LEO I: THE MASS OF THE MILKY WAY'S DARK MATTER HALO (2012, background): “…star formation persisted in Leo I until the past 0.5–1 Gyr (Smecker-Hane et al. 2009) and (2) the lack of H i detected in Leo I (MH i < 1.5 × 103 M ; Grcevich & Putman 2009), this implies that gas in MW dwarf satellites can be either expelled or removed on timescales shorter than one crossing…”
Constraints on the distribution and energetics of fast radio bursts using cosmological hydrodynamic simulations (2014, methodology): “…density distributions representative of the Galactic halo, overplotted with observational data and constrain s covering the entire virial radius, as presented by Miller & Bregman (2013), Grcevich & Putman (2009), Blitz & Robishaw (2000), Bregman & Lloyd-Davies (2007) and Gupta et al. (2012).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “…the remarkable observation of gas depletion in all dwarfs within a radius of about 270 kpc, with the exception of the high-mass LMC and SMC dwarfs (Grcevich & Putman 2009), which is well understood in terms of ram-pressure stripping by a hot medium (Nichols & Bland-Hawthorn 2011, Gatto et al.…”
THE SPLASH SURVEY: SPECTROSCOPY OF 15 M31 DWARF SPHEROIDAL SATELLITE GALAXIES (2011, background): “12 Hubble Fellow luminosities (103 < L/L < 10 8), lack of significant gas (Grcevich & Putman 2009), and low numbers compared to ΛCDM expectations (Klypin et al. 1999; Moore et al. 1999) are all puzzles that remain to be solved.”
ELVIS: Exploring the Local Volume in Simulations (2013, background): “…2013 RAS, MNRAS 000, 1–22 This presupposes that a process such as ram pressure stripping removes the gas from satellites upon infall and is motivated by observations demonstrating that the vast majority of Local Group satellites have negligible neutral gas content (Grcevich & Putman 2009).”
THE OBSERVED PROPERTIES OF DWARF GALAXIES IN AND AROUND THE LOCAL GROUP (2012, unknown): “…on n ach ie Table 4 (Continued) a References: (1) Martin et al. 2005; (2) Ibata et al. 1994; (3) Ibata et al. 1997; (4) Peñarrubia et al. 2011; (5) Grcevich & Putman 2009; (6) Simon et al. 2011; (7) Simon & Geha 2007; (8) Koch et al. 2009; (9) Belokurov et al. 2009; (10) Martin et al. 2007; (11)…”
Farthest Neighbor: The Distant Milky Way Satellite Eridanus II (2016, background): “250 kpc) and the more distant gas-rich star-forming dwarfs (Einasto et al. 1974; Blitz & Robishaw 2000; Grcevich & Putman 2009; Spekkens et al. 2014).”
The role of dwarf galaxy interactions in shaping the Magellanic System and implications for Magellanic Irregulars (2012, background): “This fact is difficult to reconcile with the expected gas loss and quenching of star formation the LMC should have incurred if it were indeed a long-term companion of the MW (Grcevich & Putman 2009).”
THE STRUCTURE OF THE MILKY WAY'S HOT GAS HALO (2013, methodology): “We choose a medium consistent with Blitz & Robishaw (2000) as opposed to Grcevich & Putman (2009) because an additional ambient medium as large as 2.5 × 10−4 cm−3 violates the observational constraint of the emission measure out of the Galactic plane, which will be discussed in greater detail in…”
Gaseous Galaxy Halos (2012, methodology): “The current chemical evolution models of our Galaxy are largely semi-analytic (although see Few et al., 2012; Kobayashi & Nakasato, 2011).”
A STELLAR MASS THRESHOLD FOR QUENCHING OF FIELD GALAXIES (2012, background): “…of galaxies below this stellar mass. Studies of dwarf galaxies within 10Mpc with stellar masses below 107 M⊙ are consistent with our results: low mass quenched galaxies exist only within a few virial radius of the Milky Way, M31 or the nearby M81 group (Grcevich & Putman 2009; Weisz et al. 2011).”