A Comprehensive Model for the Monoceros Tidal Stream

By J. Peñarrubia, D. Martínez-Delgado, Hans-Walter Rix, M. Á. Gomez-Flechoso, J. Munn, Heidi Jo Newberg, Eric F. Bell, Brian Yanny, D. Zucker, E. Grebel. 2004

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We have compiled an extensive data set on potential parts of the Monoceros tidal stream and performed an exhaustive survey of dwarf galaxy semianalytic orbits in order to constrain its orbital properties. The best-fit orbits are subsequently realized as self-consistent N-body simulations in order to reproduce the spatial and velocity distribution of satellite debris. We find that all kinematic and geometric constraints can be fit by a single stream allowing for multiple wraps. The orbital eccentricity and inclination of the progenitor are strongly constrained to be e = 0.10 ± 0.05 and i = 25° ± 5°. Ten new estimates of proper motions from the Sloan Digital Sky Survey clearly exclude all retrograde orbits. Particles lost by the satellite populate two nearly concentric rings, naturally explaining the detection of stream stars at both 6-8 kpc (Ibata et al.; Newberg et al.) and 12-18 kpc (the Tri/And stream; Rocha-Pinto et al.) from the Sun. We have attempted to predict the present location of the Monoceros stream progenitor using different information: (1) the kinematical and spatial distribution of detections, and (2) the different mean metallicity in the inner and the outer rings. Because of the lack of observational data in the whole range of Galactic latitudes, the geometrical/kinematical constraints lead to a wide range of possible locations. By associating older parts of the model stream with lower metallicity parts of the observed data, we argue in favor of a current location of l ~ 245°, b ~ -18°, with a distance to the Sun rs ≃ 15 kpc. The mass of the progenitor has been poorly constrained because of the slow orbital decay. Similar fits have been obtained for masses (3-9) × 108 M☉. We have analyzed the possible common origin of the Canis Major dwarf and the Monoceros stream. The Canis Major dwarf moves on a prograde, nearly circular orbit (e ≃ 0.16) in the Milky Way disk (i ≃ 4 deg). This orbital inclination is too low to account for the large vertical dispersion of stream stars. However, the bimodal distribution of radial velocities in the central region found by Martin et al. probably indicates that their selection criteria for identifying dwarf stars lead to a contamination of background stars. In that case, the kinematical data outlined above might result in an underestimate of the orbital inclination. Finally, the distance estimation to Canis Major dwarf is around a factor of 2 smaller than that obtained from our model. Unfortunately, the possible identification of the Monoceros stream progenitor in Canis Major remains unclear.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The QUEST RR Lyrae Survey. II. The Halo Overdensities in the First Catalog (2006, background): “…of the Monoceros stream lies in the constellation Canis Major, but there is considerable controversy over this association and even the existence of the Canis Major galaxy (e.g., Martin et al. 2004; Momany et al. 2004; Martı́nezDelgado et al. 2005; Carraro et al. 2005; Peñarrubia et al. 2005).”
The Accretion Origin of the Milky Way’s Stellar Halo (2007, background): “1 kpc scale height of the thick disk cannot be a thick disk; this is the wellknown Low-Latitude stream (e.g., Newberg et al. 2002; Peñarrubia et al. 2005; Momany et al. 2006).”
The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution (2005, background): “The inhomogeneity of the stream apparent in the top three panels of Figure 13 as well as R¼ const projections of these maps and a theoretical study by Peñarrubia et al. (2005) support this conclusions as well.”
The Wobbly Galaxy : kinematics north and south with RAVE red-clump giants (2013, background): “The origin of all such structures is not yet fully understood: possible agents for the Monoceros ring are tidal debris (see e.g. Penarrubia et al. 2005), the excitation of the disc caused by accretion events (e.g. Kazantzidis et al. 2008) or the Galactic warp (Momany et al. 2006), while Humphreys…”
THE SAGITTARIUS DWARF GALAXY: A MODEL FOR EVOLUTION IN A TRIAXIAL MILKY WAY HALO (2010, background): “In particular, can realistic orbits be found to match such systems as the Monoceros tidal stream (e.g., Peñarrubia et al. 2005), the Magellanic Clouds17 (e.g., Besla et al. 2007; Rŭžička et al. 2007), the “orphan stream” (Belokurov et al. 2007), the GD-1 stream (Koposov et al. 2009), the…”
Dark matter in the Milky Way II. The HI gas distribution as a tracer of the gravitational potential (2007, background): “However, a possible scenario could be a ring-like mass concentration caused by a merger event; see Hayashi et al. (2003) and Peñarrubia et al. (2005, 2006).”
The influence of Sagittarius and the Large Magellanic Cloud on the stellar disc of the Milky Way Galaxy (2017, background): “…the tidal interaction of multiple mergers (Kazantzidis et al. 2008), a single-event encounter with a dwarf galaxy (Younger et al. 2008), a low-velocity fly-by (Gómez et al. 2016), and the tidal disruption of satellites in the plane of the disc (Peñarrubia et al. 2005; Sheffield et al. 2014).”
A Comparison of Elemental Abundance Ratios in Globular Clusters, Field Stars, and Dwarf Spheroidal Galaxies (2005, methodology): “However, the membership of certain GCs in the CMa dwarf has been called into question by Peñarrubia et al. (2005).”
The Milky Way Tomography with SDSS. II. Stellar Metallicity (2008, methodology): “This result is qualitatively in agreement with Penarrubia et al. (2005), who ruled out retrograde motions using models and proper motion measurements.”
LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) — The survey's science plan (2012, background): “The anticenter direction has proven to be particular rich insubstructure, including the Monoceros Ring (Newberg et al. 2002, Yanny et al. 2003, Penarrubia et al. 2005), the Anticenter Stream (Grillmair 2006b, Grillmair, Carlin, & Majewski 2008, Carlin et al. 2010), theEBS stream (Grillmair 2006b,…”
RINGS AND RADIAL WAVES IN THE DISK OF THE MILKY WAY (2015, background): “Although it has been suggested that the Monoceros Ring and TriAnd might be different parts of the same tidal stream (Peñarrubia et al. 2005), Chou et al. (2011) find different metallicities for the two substructures.”
Accreted versus in situ Milky Way globular clusters (2010, background): “Martin et al. (2004) identified several GCs that lie close to the favoured prograde orbit of the CMa dwarf in phase space (but see also Penarrubia et al. 2005 for alternative view).”
The formation and assembly history of the Milky Way revealed by its globular cluster population (2018, background): “This combination of age, mass, and metallicity thus provides an additional data point in the formation and assembly history of the Milky Way, even if our sample does not contain any GCs with such young ages.”
The Milky Way’s stellar disk (2013, background): “…simplistic) explanations have been advanced to explain it: either purely as deposited stellar debris from a satellite that had merged on a low-latitude, low-eccentricity prograde orbit (e.g., Peñarrubia et al. 2005), or simply as a combination of a disk warp and flare (e.g., Momany et al. 2006).”
Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph (2012, background): “…outer disk regions including the so-called Monoceros stream are expected to contain abundant tidal debris from a merging dwarf galaxy (e.g. Peñarrubia et al. 2005) which can be probed by observing G5V stars as faint asV = 21.5 − 22 mag with 19 Subaru/PFS; aV = 20 mag limit, practical for…”
The stellar halo of the Galaxy (2008, methodology): “Possible interpretations are that it is debris from an accreted satellite (e.g. Helmi et al. 2003b; Martin et al. 2004; Peñarrubia et al. 2005; Mart́ınez-Delgado et al. 2005), an overdensity associated to the Galactic warp (Momany et al. 2004, 6 This was posted as a preprint on astro-ph in March…”
ASSESSING THE MILKY WAY SATELLITES ASSOCIATED WITH THE SAGITTARIUS DWARF SPHEROIDAL GALAXY (2010, background): “…P. Frinchaboy 2010 [priv. communication]) is too 11 Alternatively it may instead be associated with some other tidal feature such as Monoceros/GASS; see Frinchaboy et al. 2006, Peñarrubia et al. 2005. uncertain to offer a significant constraint on the relation between Be 29 and the Sgr stream.”
A-type stars in the Canada–France Imaging Survey – II. Tracing the height of the disc at large distances with Blue Stragglers (2018, background): “Right-hand panel: z − R projection of disc BSs, identified by their PM (in grey) and by their circular velocity (coloured points). disruption of a dwarf galaxy (e.g. Peñarrubia et al. 2005).”