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Gaia DR2 proper motions of dwarf galaxies within 420 kpc: Orbits, Milky Way mass, tidal influences, planar alignments, and group infall
Open accessAbstract
A proper understanding of the Milky Way (MW) dwarf galaxies in a cosmological context requires knowledge of their 3D velocities and orbits. However, proper motion (PM) measurements have generally been of limited accuracy and are available only for more massive dwarfs. We therefore present a new study of the kinematics of the MW dwarf galaxies. We use the Gaia DR2 for those dwarfs that have been spectroscopically observed in the literature. We derive systemic PMs for 39 galaxies and galaxy candidates out to 420 kpc, and generally find good consistency for the subset with measurements available from other studies. We derive the implied Galactocentric velocities, and calculate orbits in canonical MW halo potentials of low (0.8 × 10 12 M ⊙ ) and high mass (1.6 × 10 12 M ⊙ ). Comparison of the distributions of orbital apocenters and 3D velocities to the halo virial radius and escape velocity, respectively, suggests that the satellite kinematics are best explained in the high-mass halo. Tuc III, Crater II, and additional candidates have orbital pericenters small enough to imply significant tidal influences. Relevant to the missing satellite problem, the fact that fewer galaxies are observed to be near apocenter than near pericenter implies that there must be a population of distant dwarf galaxies yet to be discovered. Of the 39 dwarfs: 12 have orbital poles that do not align with the MW plane of satellites (given reasonable assumptions about its intrinsic thickness); 10 have insufficient PM accuracy to establish whether they align; and 17 satellites align, of which 11 are co-orbiting and (somewhat surprisingly, in view of prior knowledge) 6 are counter-orbiting. Group infall might have contributed to this, but no definitive association is found for the members of the Crater-Leo group.
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Citations
Cites
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Galactic Anomalies and Particle Dark Matter
Fairbairn, M. (2022) · Symmetry · doi:10.3390/sym14040812 · Cited by 9
Determining satellite infall times using machine learning
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Cold, Old, and Metal-poor: New Stellar Substructures in the Milky Way’s Dwarf Spheroidals
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“…et al. (2018) set a lower limit on the mass of the MW DM halo of 9.1+6.2 −2.6 × 10 11 M⊙, based on the assumption that Leo I is indeed bound to the MW. Recentely, Fritz et al. (2018) found that Leo I is “back-splashing” if one considers the (preferred) heavy MW DM halo model (MMW = 1.6 × 10 12 M⊙).”
BackgroundInfluentialSearching for Dwarf Galaxies in Gaia DR2 Phase-space Data Using Wavelet Transforms
Darragh-Ford, E., Nadler, E. O., McLaughlin, S., & Wechsler, R. H. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac0053 · Cited by 8
A New Absolute Proper Motion Determination of Leo I Using HST/WFPC2 Images and Gaia EDR3
Casetti‐Dinescu, D. I., Hansen, C. K., Girard, T. M., Kozhurina-Platais, V., Platais, I., & Horch, E. P. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac30dc · Cited by 8
The escape of globular clusters from the satellite dwarf galaxies of the Milky Way
Rostami-Shirazi, A., Haghi, H., Khalaj, P., Asl, A. F., & Zonoozi, A. H. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1070 · Cited by 8
Chemical and stellar properties of early-type dwarf galaxies around the Milky Way
Belokurov, V. A., & Evans, N. W. (2022) · Nature Astronomy · doi:10.1038/s41550-022-01740-w · Cited by 11
Santos-Santos, I., Gámez-Marín, M., Domínguez-Tenreiro, R., Tissera, P. B., Bignone, L., Pedrosa, S., Artal, H., Gómez-Flechoso, M. Á., Rufo-Pastor, V., Martínez-Serrano, F. J., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/aca1c8 · Cited by 8
“Here, as in Paper I, the term “co-orbitation” will mean kinematical coherence no matter the sense of rotation within an aperture αco−orbit= 36°.87 (see Fritz et al. 2018).”
BackgroundAbundance Analysis of Stars at Large Radius in the Sextans Dwarf Spheroidal Galaxy*
Roederer, I. U., Pace, A. B., Placco, V. M., Caldwell, N., Koposov, S. E., Mateo, M. L., Olszewski, E. W., & Walker, M. G. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ace3c1 · Cited by 11
Uzeirbegovic, E., Martin, G., Kaviraj, S., Jackson, R. A., Kraljic, K., Dubois, Y., Pichon, C., Devriendt, J., Peirani, S., Silk, J. I., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2632 · Cited by 7
Space astrometry with Gaia: Advances in understanding our Galaxy
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Gámez-Marín, M., Santos-Santos, I., Domínguez-Tenreiro, R., Pedrosa, S., Tissera, P. B., Gómez-Flechoso, M. Á., & Artal, H. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad27da · Cited by 7
Understanding the ‘feeble giant’ Crater II with tidally stretched wave dark matter
Pozo, A., Broadhurst, T. J., Emami, R., & Smoot, G. F. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1862 · Cited by 7
Gaia: The Galaxy in six (and more) dimensions
Pancino, E. (2019) · Advances in Space Research · doi:10.1016/j.asr.2019.11.007 · Cited by 7
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“In any case, Battaglia et al. (2022) and Sohn et al. (2013), along with estimates from Fritz et al. (2018) and Gaia Collaboration et al. (2018), agree on the timing of the (only) pericentric passage, ≃ 1 Gyr ago.”
Discovery of a Hypervelocity L Subdwarf at the Star/Brown Dwarf Mass Limit
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“We examined the intersection of J1249+3621’s orbit with 50 Milky Way satellites from Fritz et al. (2018) using the same procedure as our GCs, integrating back to 10 Gyr.”
MethodA Correlated Search for Local Dwarf Galaxies in GALFA-H i and Pan-STARRS
DeFelippis, D., Putman, M. E., & Tollerud, E. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab1e57 · Cited by 6
“…may still be ∼ 100 undiscovered satellites that are “missing” simply due to the incompleteness of large sky surveys, a conclusion also supported by Fritz et al. (2018)’s finding that there should be a population of undiscovered UFDs at the apocenter, thus illustrating the importance of…”
BackgroundDynamics of dwarf galaxies in f(R) gravity
Martino, I. D., Diaferio, A., & Ostorero, L. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad010 · Cited by 6
Identifying the possible ex-situ origin of the globular clusters of the Milky Way: a kinematic study
Rostami-Shirazi, A., Khalaj, P., & Haghi, H. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3046 · Cited by 6
Proper motions of the satellites of M31
Hodkinson, B. H., & Scholtz, J. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1893 · Cited by 6
La Silla-QUEST RR Lyrae star survey II: the Crater II tidal streams
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Effects of primordial fluctuations on relic neutrino simulations
Zimmer, F., Abellán, G. F., & Ando, S. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/10/098 · Cited by 5
“These potentials are formed by DM halos selected from the TangoSIDM project [33, 34] and have masses consistent with the estimated Milky-Way mass using the Gaia data [35–38], whose values are within the range of M 200 = (0 .”
Seo, C., Yoon, S.-J., Paudel, S., An, S.-H., & Moon, J.-S. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8634 · Cited by 5
Three new late-type hypervelocity star candidates from Gaia DR2 with refined selection criteria
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“…Galactic Potential Model I of Irrgang et al. (2013), since this model is the most realistic according to recent studies of the motions of globular clusters and satellite galaxies using Gaia DR2 astrometry (Gaia Collaboration et al. 2018b; Watkins et al. 2018; Sohn et al. 2018; Fritz et al. 2018).”
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“Gaia ’s present precision (DR3) is not sufficient for measuring bulk PMs of low-mass systems beyond ∼ 400 kpc (Fritz et al. 2018a), and its magnitude limit at G ∼ 20 .”
Self-citationTemporal Evolution of the Radial Distribution of Milky Way Satellite Galaxies
Patel, E., Chatur, L., & Mao, Y.-Y. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad87ee · Cited by 4
“Finally, we remind readers that the census of MW satellites is not yet complete and specifically that a majority of MW satellites are currently closer to pericenter than apocenter (see Fritz et al. 2018).”
Can tides explain the low dark matter density in Fornax?
Genina, A., Read, J. I., Fattahi, A., & Frenk, C. S. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3526 · Cited by 4
The Milky Way satellite galaxy Leo T: A perturbed cored dwarf
Blaña, M., Burkert, A. M., Fellhauer, M., Calderón, D., Behrendt, M., & Schartmann, M. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451649 · Cited by 4
Scrutinizing the isotropic gamma-ray background in search of dark matter
Cholis, I., & Krommydas, I. (2024) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.110.103032 · Cited by 4
Warm dark matter model with a few keV mass is bad for the too-big-to-fail problem
Kang, X. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3118 · Cited by 4
“Using Gaia data the infall times and orbits for most satellites have been recently updated (Fritz et al. 2018; Fillingham et al. 2019).”
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Destruction of the central black hole gas reservoir through head-on galaxy collisions
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Tarchi, A., Castangia, P., Surcis, G., Brunthaler, A., Henkel, C., Pawlowski, M. S., Menten, K. M., Melis, A., Casu, S., Murgia, M., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3445 · Cited by 4
“For the VPOS of the MW, this can be tested using optical proper motion measurements, revealing that indeed most of the classical MW satellites co-orbit in the (VPOS) plane (Metz et al. 2008, Pawlowski & Kroupa 2013, Helmi et al. 2018, Fritz et al. 2018).”
MethodSelf-citationSantos-Santos, I., Domínguez-Tenreiro, R., & Pawlowski, M. S. (2019) · arXiv (Cornell University) · doi:10.48550/arxiv.1908.02298 · Cited by 4
“In this way, the so-called “VPOS-3” (Vast Polar Structure) and “GPoA” (Great Plane of Andromeda) planes were defined, consisting of 24 and 19 satellites respectively.”
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Arroyo-Polonio, J. M., Battaglia, G., & Thomas, G. F. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202558720 · Cited by 3
Self-citationMachine Learning the Dark Matter Halo Mass of Milky Way-Like Systems
Hayati, E., Behroozi, P., & Patel, E. (2024) · The Open Journal of Astrophysics · doi:10.33232/001c.116178 · Cited by 3
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Self-citationThe effect of measurement uncertainties on the inferred stability of planes of satellite galaxies
Kumar, P., Pawlowski, M. S., Kanehisa, K. J., Li, P., Júlio, M. P., & Taibi, S. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453087 · Cited by 3
Self-citationA detailed chemical study of the extreme velocity stars in the galaxy
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“In a recent publication Fritz et al. (2018) used the Gaia DR2 data to determine a possible proper motion of the dwarf.”
MethodInfluentialModelling the Canes Venatici I dwarf spheroidal galaxy
Carrillo, D. R. M., Fellhauer, M., Jara, A. G. A., Aravena, C. A., & Zapata, F. U. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201935602/pdf · Cited by 2
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“Amongst its many contributions, Gaia has provided important new insight into LG galaxies, including measurement of their proper motions, from which orbital trajectories and infall times for satellites into the MW have been determined (Helmi et al. 2018; Fritz et al. 2018; Simon 2018).”
A Physical Interpretation of Milky Way Galaxy Dynamics from Precision AstrometricsPreprint
Fortune, J. M. L. (2020) · arXiv (Cornell University) · doi:10.48550/arxiv.2008.10445 · Cited by 1
Mining the SPARC Galaxy Database: Finding "Hidden Variables" in the Baryonic Tully-Fisher RelationPreprint
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Most dwarf spheroidal galaxies surrounding the Milky Way cannot be dark-matter dominated satellitesPreprint
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Patel, E., Kallivayalil, N., Garavito-Camargo, N., Besla, G., Weisz, D. R., van der Marel, R. P., Boylan-Kolchin, M., Pawlowski, M. S., & Gómez, F. A. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acebee
Self-citationHow things go mostly right or badly wrong
McGaugh, S. (2023) · doi:10.59350/5y3k4-yb096
Variable stars in Local Group galaxies
Monelli, M., Piersimoni, A. M., Martínez-Vázquez, C. E., Cassisi, S., Stetson, P. B., Marconi, M., Pérez-García, P. J., Bono, G., Dall’Ora, M., Fiorentino, G., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453567
Dwarf galaxies in non-local gravity
Martino, I. D., Monica, R. D., & Roshan, M. (2025) · Physics of the Dark Universe · doi:10.1016/j.dark.2025.102044
“Additionally, luminosity values in the V-band, stellar mass-to-light ratio, and half-light radius for each galaxy are sourced from [27, 28, 29, 31, 32, 33, 34, 35, 36, 37, 38, 39, 40, 41, 30] and summarized in Table 1.”
Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Fu, H., Huang, Y., & Zhang, H. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ae0c09
“The position of these dwarf galaxies are taken from Fritz et al. (2018).”
InfluentialProbing the dark sector using the Fornax satellite
Zamlung, E., & Nusser, A. (2025) · Physical review. D/Physical review. D. · doi:10.1103/tqzj-28gz
The lives and deaths of faint satellite galaxies around M31
Merrow, A., Oman, K. A., & Fattahi, A. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag558
Chiu, C. K., Geha, M., Cerny, W., Kallivayalil, N., Richstein, H., Garling, C. T., & Willman, B. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae4a2a
“To quantitatively verify that W1 is at apocenter, we calculate the ratio f peri of Fritz et al. (2018): which is a proxy for the orbital phase in the radial direction. f peri = 0 and 1 indicate an object at pericenter and apocenter, respectively.”
Self-citationThe DECam MAGIC Survey: Uncovering the Tidal Tails of the Crater II Dwarf Galaxy
Atzberger, K. R., Pace, A. B., Kallivayalil, N., Chiti, A., Erkal, D., Cerny, W., Limberg, G., Placco, V. M., Prabhu, D. S., Stringfellow, G. S., et al. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae7f1f
“They selected targets from a combined parallax, proper motion ( mean CraII motion from T. K. Fritz et al. 2018 ) , and broadband photometric selection with the AAOmega spectrograph on the 3.9 m Anglo-Australian Telescope.”
InfluentialSelf-citationS5: Tidal Disruption in Crater 2 and Formation of Diffuse Dwarf Galaxies in the Local Group
Limberg, G., Ji, A., Li, T. S., Erkal, D., Koposov, S. E., Pace, A., Li, A. P., Awad, P., Senkevich, A., Bland-Hawthorn, J., et al. (2025) · Astrophysical Journal · doi:10.3847/1538-4357/aea28e · Cited by 1
“Targets were selected to also have proper motions consistent with the mean value for Cra2 (Fritz et al. 2018).”
Metadata
- Authors
- Fritz, T. K., Battaglia, G., Pawlowski, M. S., Kallivayalil, N., van der Marel, R., Sohn, S. T., Brook, C., & Besla, G.
- Affiliations
- Universidad de La Laguna (ES)
- University of California, Irvine (US)
- University of Virginia (US)
- Space Telescope Science Institute (US)
- University of Arizona (US)
- Venue
- Astronomy & Astrophysics
- Publisher
- EDP Sciences
- Published
- 2018-11
- Volume
- 619
- Pages
- A103
- ISSN
- 0004-6361 (ISSN-L)
- 1432-0746
- OpenAlex
- W4289328036
- Cited by
- 269
- References
- 135
- Citations by year
- 2026: 7 · 2025: 16 · 2024: 23 · 2023: 30 · 2022: 35 · 2021: 45 · 2020: 51 · 2019: 50 · 2018: 12
- FWCI
- 21.20
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (1455260, CAREER)
- National Aeronautics and Space Administration (HST‐HF2‐51379.001‐A, NAS 526555)
- Space Telescope Science Institute (NAS5- 26555, 26555)
- European Space Agency
- Ministerio de Economía y Competitividad (AYA2014-56795-P, RYC-2012-11537)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- Milky Way dwarf galaxies, proper motions, satellite kinematics, Gaia DR2, escape velocity, missing satellites problem, tidal interactions
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