Taking measure of the Andromeda halo: A Kinematic analysis of the giant stream surrounding M31

By R. Ibata, S. Chapman, A. M. N. Ferguson, M. Irwin, G. Lewis, A. McConnachie. 2004

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We present a spectroscopic survey of the giant stellar stream found in the halo of the Andromeda galaxy. Taken with the DEIMOS multi-object spectrograph on the Keck2 telescope, these data display a narrow velocity dispersion of 11 ± 3k m s −1 , with a steady radial velocity gradient of 245 km s −1 over the 125-kpc radial extent of the stream studied so far. This implies that the Andromeda galaxy possesses a substantial dark matter halo. We fit the orbit of the stream in different galaxy potential models. In a simple model with a composite bulge, disc and halo, where the halo follows a universal profile that is compressed by the formation of the baryonic components, we find that the kinematics of the stream require a total mass inside 125 kpc of M 125 = 7.5 +2.5

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/eb5eb39f2f3eaa151e8c0935ebd6e82588a24772

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Citations in the corpus

THE LUMINOSITY PROFILE AND STRUCTURAL PARAMETERS OF THE ANDROMEDA GALAXY (2011, background): “However, the very faint extended structure around M31 (Ibata et al. 2004, 2007; Guhathakurta et al. 2005, hereafter Guha05; Irwin et al. 2005, hereafter Irwin05; Chapman et al. 2006; Gilbert et al. 2007, 2009b; McConnachie et al. 2009; Tanaka et al. 2010) revealed a complex portrait of galaxy…”
STECKMAP: STEllar Content and Kinematics from high resolution galactic spectra via Maximum A Posteriori (2005, background): “The highly detailed stellar content and kinematical information that can be obtained for the Milky Way or for nearby galaxies that can be resolved into stars, such as M31 (Ferguson et al. 2002; Ibata et al. 2004), could be extended to a larger sample of more distant galaxies.”
The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream (2018, methodology): “…method to gauge the mass distribution inside our own Milky Way (see e.g. Johnston et al. 1999; Koposov, Rix & Hogg 2010; Gibbons, Belokurov & Evans 2014; Küpper et al. 2015) and a handful of nearby galaxies (e.g. Ibata et al. 2004; Fardal et al. 2013; Amorisco, Martinez-Delgado & Schedler 2015).”
The Haunted Halos of Andromeda and Triangulum: A Panorama of Galaxy Formation in Action (2007, methodology): “In many ways Andromeda is the “sister” to the Milky Way, having very similar total masses (including the dark matter, Evans et al. 2000; Ibata et al. 2004), having shared a common origin, and probably sharing the same ultimate fate when they finally merge in the distant future.”
THE LARGE-SCALE STRUCTURE OF THE HALO OF THE ANDROMEDA GALAXY. I. GLOBAL STELLAR DENSITY, MORPHOLOGY AND METALLICITY PROPERTIES (2013, background): “It is interesting to note that by far the strongest signal of metal-rich stars (beyond the bound galaxies) is due to the so-called “Giant Stellar Stream” that protrudes down to the south of M31 (Ibata et al. 2001, 2004; Fardal et al. 2006, 2007, 2012; Gilbert et al. 2009).”
A wide-field H I mosaic of Messier 31 - II. The disk warp, rotation, and the dark matter halo (2009, unknown): “…208 +7 −6 504 Globular Clusters Galleti et al. (2006) 60 44+26−4 178 +48 −8 349 Globular Clusters c Côté et al. (2000) 100 79+5−5 185 +6 −6 12 Satellites d Ibata et al. (2004) 125 75+25−13 161 +25 −15 Stellar Stream Fardal et al. (2006) 125 74+12−12 160 +13 −14 Stellar Stream Courteau & van…”
The Detailed Star Formation History in the Spheroid, Outer Disk, and Tidal Stream of the Andromeda Galaxy (2006, background): “2001; Ibata et al. 2004; Ibata et al. 2005; McConnachie et al. 2003; Ferguson et al. 2002; Ferguson et al. 2005; Kalirai et al. 2006b; Guhathakurta et al. 2005).”
On the Accretion Origin of a Vast Extended Stellar Disk around the Andromeda Galaxy (2005, background): “However, the proximity of M31 has allowed us to follow up these detections with deep Keck/DEIMOS spectroscopic observations (initial results of the spectroscopic survey were presented in Ibata et al. 2004).”
Structural Parameters of Thin and Thick Disks in Edge-on Disk Galaxies (2005, background): “M31 also appears to also be actively disrupting dwarf galaxies with an observable stellar stream (Ibata et al. 2004) and a large extended disk (Ibata et al. 2005).”
The Local Group and Other Neighboring Galaxy Groups (2005, background): “Studying the kinematics of the giant stellar stream around the M 31, Ibata et al. (2004) measured the mass of Andromeda halo on the scale of 125 kpc.”
Tracing Galaxy Formation with Stellar Halos. I. Methods (2005, background): “…& Hernquist 1999; Johnston et al. 1999; Helmi & White 2001; Helmi et al. 2003; Law, Johnston & Majewski 2004), and even the potential of the galaxy in which it is orbiting (Johnston, Zhao, Spergel, & Hernquist 1999; Murali & Dubinski 1999; Ibata et al. 2001, 2004; Johnston, Law & Majewski 2005).”
THE M31 VELOCITY VECTOR. II. RADIAL ORBIT TOWARD THE MILKY WAY AND IMPLIED LOCAL GROUP MASS (2012, background): “This is relevant, since some previously reported mass estimates do fall on this low-mass end (e.g., Evans et al. 2000; Ibata et al. 2004).”
Stars beyond galaxies: the origin of extended luminous haloes around galaxies (2005, unknown): “…spectrographs in 10m-class telescopes have enabled the measurement of radial velocities of large samplesof giant stars throughout the Local Group (Ibata et al 2004), and dedicated c© 2005 RAS spectroscopic campaigns targeted on giant stars have dramatic lly increased the sample of tracers in the…”
The Metal-poor Halo of the Andromeda Spiral Galaxy (M31) (2006, background): “As demonstrated in Ibata et al. (2004), Guhathakurta et al. (2006b), and Kalirai et al. (2006), the stream consists of a kinematically cold population of stars blueshifted relative to M31 (in H13s stream stars have vrad < −380 km s −1, in a3 stream stars have vrad < −400 km s−1).”