Local Group Dwarf Spheroidals: Correlated Deviations From the Baryonic Tully-Fisher Relation

McGaugh, Stacy S.; Wolf, Joe

doi:10.1088/0004-637x/722/1/248

Cited by 136 publications

(196 citation statements)

References 127 publications

(198 reference statements)

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“…Ultra-faint dwarf spheroidals are expected to be increasingly affected by this kind of non-equilibrium dynamics, as shown to be true even for Newtonian weak-field dynamics (Kroupa 1997, Sect. 6.1), and even more strongly so in MOND (McGaugh & Wolf 2010).…”

Section: A Consistency Checkmentioning

confidence: 83%

“…Both the MOND and MOG approaches have been applied to the satellite galaxy problem with appreciable success (Milgrom 1995;Brada & Milgrom 2000;Angus 2008;Moffat & Toth 2008;Hernandez et al 2010;McGaugh & Wolf 2010). It has already been conclusively demonstrated that spiral galaxy rotation curves are well recovered in MOND purely by the baryon distribution without any parameter adjustments (Sanders & McGaugh 2002;McGaugh 2004McGaugh , 2005aSanders & Noordermeer 2007), and MOG is reported to also do well on this account (Brownstein & Moffat 2006).…”

Section: Non-newtonian Weak-field Gravitymentioning

confidence: 99%

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Local-Group tests of dark-matter concordance cosmology

Kroupa

Famaey

Boer

et al. 2010

A&A

225

301

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Predictions of the concordance cosmological model (CCM) of the structures in the environment of large spiral galaxies are compared with observed properties of Local Group galaxies. Five new, most probably irreconcilable problems are uncovered: 1) A wide variety of published CCM models consistently predict some form of relation between dark-matter-mass and luminosity for the Milky Way (MW) satellite galaxies, but none is observed.2) The mass function of luminous sub-haloes predicted by the CCM contains too few satellites with dark matter (DM) mass ≈10 7 M within their innermost 300 pc than in the case of the MW satellites.3) The Local Group galaxies and data from extragalactic surveys indicate there is a correlation between bulge-mass and the number of luminous satellites that is not predicted by the CCM. 4) The 13 new ultra-faint MW satellites define a disc-of-satellites (DoS) that is virtually identical to the DoS previously found for the 11 classical MW satellites, implying that most of the 24 MW satellites are correlated in phase-space. 5) The occurrence of two MW-type DM halo masses hosting MW-like galaxies is unlikely in the CCM. However, the properties of the Local Group galaxies provide information leading to a solution of the above problems. The DoS and bulge-satellite correlation suggest that dissipational events forming bulges are related to the processes forming phase-space correlated satellite populations. These events are well known to occur since in galaxy encounters energy and angular momentum are expelled in the form of tidal tails, which can fragment to form populations of tidal-dwarf galaxies (TDGs) and associated star clusters. If Local Group satellite galaxies are to be interpreted as TDGs then the substructure predictions of the CCM are internally in conflict. All findings thus suggest that the CCM does not account for the Local Group observations and that therefore existing as well as new viable alternatives have to be further explored. These are discussed and natural solutions for the above problems emerge.

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Section: A Consistency Checkmentioning

confidence: 83%

Section: Non-newtonian Weak-field Gravitymentioning

confidence: 99%

Local-Group tests of dark-matter concordance cosmology

Kroupa

Famaey

Boer

et al. 2010

A&A

225

301

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“…Many of the uncertainties involved in measuring and interpreting velocity dispersions have been discussed by McGaugh & Wolf (2010). We emphasize here just two possible systematics that we fear will make it extremely difficult to distinguish between the various possibilities.…”

Section: Challenges To Interpretationmentioning

confidence: 96%

The new Milky Way satellites: alignment with the VPOS and predictions for proper motions and velocity dispersions

Pawlowski

McGaugh

Jerjen

2015

Mon. Not. R. Astron. Soc.

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The evidence that stellar systems surrounding the Milky Way (MW) are distributed in a Vast Polar Structure (VPOS) may be observationally biased by satellites detected in surveys of the northern sky. The recent discoveries of more than a dozen new systems in the southern hemisphere thus constitute a critical test of the VPOS phenomenon. We report that the new objects are located close to the original VPOS, with half of the sample having offsets less than 20 kpc. The positions of the new satellite galaxy candidates are so well aligned that the orientation of the revised best-fitting VPOS structure is preserved to within 9 degrees and the VPOS flattening is almost unchanged (31 kpc height). Interestingly, the shortest distance of the VPOS plane from the MW center is now only 2.5 kpc, indicating that the new discoveries balance out the VPOS at the Galactic center. The vast majority of the MW satellites are thus consistent with sharing a similar orbital plane as the Magellanic Clouds, confirming a hypothesis proposed by Kunkel & Demers and Lynden-Bell almost 40 years ago. We predict the absolute proper motions of the new objects assuming they orbit within the VPOS. Independent of the VPOS results we also predict the velocity dispersions of the new systems under three distinct assumptions: that they (i) are dark-matter-free star clusters obeying Newtonian dynamics, (ii) are dwarf satellites lying on empirical scaling relations of galaxies in dark matter halos, and (iii) obey MOND.

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“…For example, KK98-251 is a dwarf irregular satellite of NGC 6946, but both lie on the same BTFR with no indication of a shift in normalization. Current data for the ultrafaint dwarf satellites of the Milky Way do place them below the BTFR, but this shift occurs at much smaller scales (V f 20 km s −1 ; Walker et al 2009;Wolf et al 2010;McGaugh & Wolf 2010).…”

Section: Some Specific Modelsmentioning

confidence: 99%

The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

McGaugh

2012

Self Cite

436

459

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The baryonic Tully-Fisher relation (BTFR) is an empirical relation between baryonic mass and rotation velocity in disk galaxies. It provides tests of galaxy formation models in ΛCDM and of alternative theories like modified Newtonian dynamics (MOND). Observations of gas-rich galaxies provide a measure of the slope and normalization of the BTFR that is more accurate (if less precise) than that provided by star-dominated spirals, as their masses are insensitive to the details of stellar population modeling. Recent independent data for such galaxies are consistent with M b = AV 4 f with A = 47 ± 6 M km −4 s 4 . This is equivalent to MOND with a 0 = 1.3 ± 0.3 Å s −2 . The scatter in the data is consistent with being due entirely to observational uncertainties. It is unclear why the physics of galaxy formation in ΛCDM happens to pick out the relation predicted by MOND. We introduce a feedback efficacy parameter E to relate halo properties to those of the galaxies they host. E correlates with star formation rate and gas fraction in the sense that galaxies that have experienced the least star formation have been most impacted by feedback.

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Local Group Dwarf Spheroidals: Correlated Deviations From the Baryonic Tully-Fisher Relation

Cited by 136 publications

References 127 publications

Local-Group tests of dark-matter concordance cosmology

Local-Group tests of dark-matter concordance cosmology

The new Milky Way satellites: alignment with the VPOS and predictions for proper motions and velocity dispersions

The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

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