THE SPLASH SURVEY: SPECTROSCOPY OF 15 M31 DWARF SPHEROIDAL SATELLITE GALAXIES

By Erik J. Tollerud, R. Beaton, M. Geha, James S. Bullock, P. Guhathakurta, J. Kalirai, S. Majewski, E. Kirby, K. Gilbert, B. Yniguez and 6 more. 2011

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We present a resolved star spectroscopic survey of 15 dwarf spheroidal (dSph) satellites of the Andromeda galaxy (M31). We filter foreground contamination from Milky Way (MW) stars, noting that MW substructure is evident in this contaminant sample. We also filter M31 halo field giant stars and identify the remainder as probable dSph members. We then use these members to determine the kinematical properties of the dSphs. For the first time, we confirm that And XVIII, XXI, and XXII show kinematics consistent with bound, dark-matter-dominated galaxies. From the velocity dispersions for the full sample of dSphs we determine masses, which we combine with the size and luminosity of the galaxies to produce mass–size–luminosity scaling relations. With these scalings we determine that the M31 dSphs are fully consistent with the MW dSphs, suggesting that the well-studied MW satellite population provides a fair sample for broader conclusions. We also estimate dark matter halo masses of the satellites and find that there is no sign that the luminosity of these galaxies depends on their dark halo mass, a result consistent with what is seen for MW dwarfs. Two of the M31 dSphs (And XV, XVI) have estimated maximum circular velocities smaller than 12 km s−1 (to 1σ), which likely places them within the lowest-mass dark matter halos known to host stars (along with Boötes I of the MW). Finally, we use the systemic velocities of the M31 satellites to estimate the mass of the M31 halo, obtaining a virial mass consistent with previous results.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1e1d6ec11845295cf286e0802310e43c3851d227

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Citations in the corpus

ELVIS: Exploring the Local Volume in Simulations (2013, unknown): “…Mv,2, where Mv,2 ≥ Mv,1), the distance between host centers ∆R, the pair approach velocity, and local environment: • Mass of each host: 1012 ≤Mv ≤ 3× 1012M (Tollerud et al. 2012; Boylan-Kolchin et al. 2013; Fardal et al. 2013; Piffl et al. 2013) • Total mass: 2× 1012 ≤Mv,1 +Mv,2 ≤ 5× 1012M (Li &…”
A KINEMATIC STUDY OF THE ANDROMEDA DWARF SPHEROIDAL SYSTEM (2013, methodology): “New studies of the kinematics of M31 dSphs (Collins et al. 2010, 2011; Kalirai et al. 2010; Tollerud et al. 2012; Chapman et al. 2012) have dramatically increased the number of systems with a measured velocity dispersion, and have shown that instead of being kinematically hotter, these systems are…”
One Law to Rule Them All: The Radial Acceleration Relation of Galaxies (2016, unknown): “…(2011), 46: Conn et al. (2012), 47: Geha et al. (2010), 48: McConnachie et al. (2005), 20 21 49: Geha et al. (2006), 50: McConnachie & Irwin (2006), 51: Tollerud et al. (2012), 52: Ho et al. (2012), 53: Chapman et al. (2007), 54: Collins et al. (2013), 55: Brasseur et al. (2011), 56: Kalirai et…”
The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, background): “The combined likelihood of having, within the Local Group, two independent MW-type DM haloes hosting a MW and Andromeda galaxy with their satellite systems is thus ,1.4 0.4¼ 0.056%.”
Too big to fail in the Local Group (2014, result): “However, the central masses of the M31 dSphs appear to be consistent with the MW dSphs (Tollerud et al. 2012), and are therefore inconsistent with the subhaloes expected to host them (Tollerud et al. 2014).”
THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, methodology): “The stars were selected for membership based on position in the CMD and radial velocity (see Tollerud et al. 2012).”
The Local Group on FIRE: dwarf galaxy populations across a suite of hydrodynamic simulations (2018, unknown): “We therefore begin by generally replicating the analyses of Boylan-Kolchin et al. (2012), Tollerud et al. (2012), and GarrisonKimmel et al. (2014b), who identified problematic (sub)haloes by comparing the circular velocity curves of simulated systems with constraints on observed dwarf galaxies.”
THE M31 VELOCITY VECTOR. II. RADIAL ORBIT TOWARD THE MILKY WAY AND IMPLIED LOCAL GROUP MASS (2012, methodology): “For all dSphs, including those from Paper I and not listed in Table 2, we used the newly measured LOS velocities from Tollerud et al. (2012), where available.”
The AIMSS Project I: bridging the star cluster, galaxy divide (2014, background): “Data on the MW and M31 dSph/dE systems come from Walker et al. (2009), McConnachie (2012), Tollerud et al. (2012, 2013), and references therein.”
WHY BARYONS MATTER: THE KINEMATICS OF DWARF SPHEROIDAL SATELLITES (2012, methodology): “The MW data is taken from tables 3 and 4 in McConnachie (2012), while the Andromeda data is compiled from Tollerud et al. (2012), Collins et al. (2013a), and Tollerud et al. (2013).”
The properties of warm dark matter haloes (2013, methodology): “Follow-up studies of stellar kinematics have been used to investigate their dynamics and mass content (Walker et al. 2009, 2010; Wolf et al. 2010; Tollerud et al. 2012).”
Bent by baryons: the low-mass galaxy-halo relation (2014, methodology): “For the MW satellites we use virial masses estimated by Peñarrubia et al. (2008), while for M31 satellites we convert vmax estimates by Tollerud et al. (2012) using the relation for satellites given by Klypin et al. (2011).”
Dwarf galaxies in CDM and SIDM with baryons: observational probes of the nature of dark matter (2014, background): “…data of Local Group dwarfs (MW+M31 dSphs+dIrrs) (taken from Côté, Carignan & Freeman 2000; McGaugh 2005; Peñarrubia, McConnachie & Navarro 2008; Woo, Courteau & Dekel 2008; Stark, McGaugh & Swaters 2009; Misgeld & Hilker 2011; Oh et al. 2011; Ferrero et al. 2012; Tollerud et al. 2012).”