Tidal Distortions in NGC1052-DF2 and NGC1052-DF4: Independent Evidence for a Lack of Dark Matter

Keim, Michael A.; Dokkum, Pieter van; Danieli, Shany; Lokhorst, Deborah; Li, Jiaxuan; Shen, Zili; Abraham, Roberto; Chen, Seery; Gilhuly, Colleen; Liu, Qing; Merritt, Allison; Miller, Tim B.; Pasha, I. I.; Polzin, Ava

doi:10.3847/1538-4357/ac7dab

Cited by 18 publications

(20 citation statements)

References 88 publications

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“…Thus the asymmetry of an ultra-diffuse dwarf galaxy's potential (see Fig. 3) will affect the morphology of its tidal features with implications for the interpretation of its dark matter content in Newtonian gravitation (cases in point being the dark-matter-lacking dwarf galaxies NGC1052-DF2/DF4, Famaey et al 2018;Kroupa et al 2018;Keim et al 2022;Montes et al 2021). Wu & Kroupa (2013) analyse the phase transition a massive star cluster experiences on a radial orbit when moving from the Newtonian into the outer Milgromian regime, and Thomas et al (2018) demonstrate that the asymmetry of a cluster's potential leads to asymmetrically long tidal tails II explaining the unequal lengths of the observed tidal tails of the globular cluster Palomar 5.…”

Section: Emergence From Molecular Cloud and Lifetimesmentioning

confidence: 99%

Asymmetrical tidal tails of open star clusters: stars crossing their cluster’s práh† challenge Newtonian gravitation

Kroupa

Jeřabková

Thies

et al. 2022

Monthly Notices of the Royal Astronomical Society

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After their birth a significant fraction of all stars pass through the tidal threshold (práh) of their cluster of origin into the classical tidal tails. The asymmetry between the number of stars in the leading and trailing tails tests gravitational theory. All five open clusters with tail data (Hyades, Praesepe, Coma Berenices, COIN-Gaia 13, NGC 752) have visibly more stars within $d_{\rm cl}\approx 50\,{\rm pc}$ of their centre in their leading than their trailing tail. Using the Jerabkova-compact-convergent-point (CCP) method, the extended tails have been mapped out for four nearby 600–2000 Myr old open clusters to $d_{\rm cl} > 50\,{\rm pc}$. These are on near-circular Galactocentric orbits, a formula for estimating the orbital eccentricity of an open cluster being derived. Applying the Phantom of Ramses code to this problem in Newtonian gravitation the tails are near-symmetrical. In Milgromian dynamics (MOND), the asymmetry reaches the observed values for 50 < dcl/pc < 200 being maximal near peri-galacticon, and can slightly invert near apo-galacticon, and the Küpper epicyclic overdensities are asymmetrically spaced. Clusters on circular orbits develop orbital eccentricity due to the asymmetrical spill-out, therewith spinning up opposite to their orbital angular momentum. This positive dynamical feedback suggests Milgromian open clusters to demise rapidly as their orbital eccentricity keeps increasing. Future work is necessary to better delineate the tidal tails around open clusters of different ages and to develop a Milgromian direct n-body code.

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Section: Emergence From Molecular Cloud and Lifetimesmentioning

confidence: 99%

Asymmetrical tidal tails of open star clusters: stars crossing their cluster’s práh† challenge Newtonian gravitation

Kroupa

Jeřabková

Thies

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Initially, the main question was whether the dynamical masses and distances were measured correctly (see, e.g., Martin et al 2018;Laporte et al 2019;Trujillo et al 2019), but as the anomalous properties of the galaxies were gradually confirmed (and corroborated with independent evidence; see Dutta Chowdhury et al 2019;Keim et al 2022), the focus shifted to the question of how they were formed. Proposals include assembly out of tidally removed gas (Fensch et al 2019), stripping of dark matter by close encounters with NGC 1052 (Ogiya 2018;Carleton et al 2019;Nusser 2020;Moreno et al 2022;Ogiya et al 2022) or NGC 1035 (Montes et al 2020), jet-or outflow-induced star formation, like Minkowski's object (van Breugel et al 1985;Natarajan et al 1998), and extreme feedback in low-mass halos (Trujillo-Gomez et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Monochromatic Globular Clusters as a Critical Test of Formation Models for the Dark Matter–deficient Galaxies NGC 1052-DF2 and NGC 1052-DF4

Dokkum

Shen

Romanowsky

et al. 2022

ApJL

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It was recently proposed that the dark matter–deficient ultradiffuse galaxies DF2 and DF4 in the NGC 1052 group could be the products of a “bullet dwarf” collision between two gas-rich progenitor galaxies. In this model, DF2 and DF4 formed at the same time in the immediate aftermath of the collision, and a strong prediction is that their globular clusters should have nearly identical stellar populations. Here we test this prediction by measuring accurate V 606 − I 814 colors from deep HST/ACS imaging. We find that the clusters are extremely homogeneous. The mean color difference between the globular clusters in DF2 and DF4 is ΔDF2−DF4 = −0.003 ± 0.005 mag, and the observed scatter for the combined sample of 18 clusters with M 606 < −8.6 in both galaxies is σ obs = 0.015 ± 0.002 mag. After accounting for observational uncertainties and stochastic cluster-to-cluster variation in the number of red giants, the remaining scatter is σ intr = 0.008 − 0.006 + 0.005 mag. Both the color difference and the scatter are an order of magnitude smaller than in other dwarf galaxies, and we infer that the bullet scenario passes an important test that could have falsified it. No other formation models have predicted this extreme uniformity of the globular clusters in the two galaxies. We find that the galaxies themselves are slightly redder than the clusters, consistent with a previously measured metallicity difference. Numerical simulations have shown that such differences are expected in the bullet scenario, as the galaxies continued to self-enrich after the formation of the globular clusters.

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“…Data source: Gannon et al (2022). There is also evidence it may be undergoing a tidal interaction (Keim et al 2022, although see Montes et al 2021). We do however note there is some evidence for rotation in NGC 1052-DF2 which may help alleviate the paucity of dark matter implied by its low velocity dispersion (Lewis et al 2020;Montes et al 2021).…”

Section: A011 Pudg-r15mentioning

confidence: 89%

Keck Spectroscopy of the Coma Cluster Ultra-Diffuse Galaxy Y358: Dynamical Mass in a Wider Context

Gannon¹,

Forbes²,

Brodie³

et al. 2022

Preprint

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We examine ultra-diffuse galaxies (UDGs) and their relation to non-UDGs in mass-radius-luminosity space. We begin by publishing Keck/KCWI spectroscopy for the Coma cluster UDG Y358, for which we measure both a recessional velocity and velocity dispersion. Our recessional velocity confirms association with the Coma cluster and Y358's status as a UDG. From our velocity dispersion (19 ± 3 km s −1 ) we calculate a dynamical mass within the half-light radius which provides evidence for a core in Y358's dark matter halo. We compare this dynamical mass, along with those for globular cluster (GC)-rich/-poor UDGs in the literature, to mass profiles for isolated, gas-rich UDGs and UDGs in the NIHAO/FIRE simulations. We find GC-poor UDGs have dynamical masses similar to isolated, gas-rich UDGs, suggesting an evolutionary pathway may exist between the two. Conversely, GC-rich UDGs have dynamical masses too massive to be easily explained as the evolution of the isolated, gas-rich UDGs. The simulated UDGs match the dynamical masses of the GC-rich UDGs. However, once compared in stellar mass -halo mass space, the FIRE/NIHAO simulated UDGs do not match the halo masses of either the isolated, gas-rich UDGs or the GC-rich UDGs at the same stellar mass. Finally, we supplement our data for Y358 with other UDGs that have measured velocity dispersions in the literature. We compare this sample to a wide range of non-UDGs in mass-radius-luminosity space, finding UDGs have a similar locus to non-UDGs of similar luminosity with the primary difference being their larger half-light radii.

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Tidal Distortions in NGC1052-DF2 and NGC1052-DF4: Independent Evidence for a Lack of Dark Matter

Cited by 18 publications

References 88 publications

Asymmetrical tidal tails of open star clusters: stars crossing their cluster’s práh† challenge Newtonian gravitation

Asymmetrical tidal tails of open star clusters: stars crossing their cluster’s práh† challenge Newtonian gravitation

Monochromatic Globular Clusters as a Critical Test of Formation Models for the Dark Matter–deficient Galaxies NGC 1052-DF2 and NGC 1052-DF4

Keck Spectroscopy of the Coma Cluster Ultra-Diffuse Galaxy Y358: Dynamical Mass in a Wider Context

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