Predicted MOND velocity dispersions for a catalog of ultra-diffuse galaxies in group environments

Müller, Oliver; Famaey, Benoît; Zhao, Hongsheng

doi:10.1051/0004-6361/201834914

Cited by 28 publications

(30 citation statements)

References 76 publications

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“…The median size of the seven clusters is r 4.1 pc h á ñ = . Looking ahead, we can determine the stellar velocity dispersion of NGC1052-DF4(see Danieli et al 2019;Emsellem et al 2019), constrain its dark matter mass (e.g., Laporte et al 2019;Wasserman et al 2018), and assess the implications for alternative gravity (Famaey et al 2018;van Dokkum et al 2018b): taken together, NGC1052-DF2 and NGC1052-DF4 seem in tension with recent predictions from Modified Newtonian Dynamics (Müller et al 2019). Following the adage "one is an exception but two is a population" this new object provides impetus for characterizing the properties of diffuse, dark-matter-deficient galaxies as a class.…”

Section: Discussionmentioning

confidence: 98%

A Second Galaxy Missing Dark Matter in the NGC 1052 Group

Dokkum

Danieli

Abraham

et al. 2019

ApJL

217

204

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The ultra-diffuse galaxy NGC1052-DF2 has a very low velocity dispersion, indicating that it has little or no dark matter. Here we report the discovery of a second galaxy in this class, residing in the same group. NGC1052-DF4 closely resembles NGC1052-DF2 in terms of its size, surface brightness, and morphology; has a similar distance of D 19.9 2.8 Mpc sbf =  ; and also has a population of luminous globular clusters extending out to 7 kpc  from the center of the galaxy. Accurate radial velocities of the diffuse galaxy light and seven of the globular clusters were obtained with the Low Resolution Imaging Spectrograph on the Keck I telescope. The velocity of the diffuse light is identical to the median velocity of the clusters, v v 1445 km s halo 1 s~-). We conclude that NGC1052-DF2 is not an isolated case but that a class of such objects exists. The origin of these large, faint galaxies with an excess of luminous globular clusters and an apparent lack of dark matter is, at present, not understood.

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Section: Discussionmentioning

confidence: 98%

A Second Galaxy Missing Dark Matter in the NGC 1052 Group

Dokkum

Danieli

Abraham

et al. 2019

ApJL

217

204

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“…When a i ≈ a e < a 0 , the object is quasi-Newtonian i.e. Newton's law of Gravity applies with an effective gravitational constant G e f f ≥ G (Famaey & McGaugh 2012;McGaugh & Milgrom 2013;Famaey et al 2018;Müller et al 2019a). According to the Famaey & McGaugh (2012) formulation, the MOND acceleration a at the half-light radius is…”

Section: Comparison With Famaey and Mcgaugh (2012)mentioning

confidence: 99%

“…There are three other bright nearby galaxies in the group close to DF4 in terms of their sky positions. These galaxies are NGC 1052, NGC 1042, and NGC 1035 with baryonic masses of M NGC1052 = 10 11 M (Bellstedt et al 2018), M NGC1042 = 2.4 × 10 10 M , and M NGC1035 = 1.9 × 10 10 M (Müller et al 2019a), respectively, assuming they are all at a distance of D = 20 Mpc. To estimate the total baryonic mass of NGC 1042 and NGC 1035 with K-band absolute magnitudes of M K,1042 = −8.85 and M K,1035 = −9.13, respectively (Skrutskie et al 2006;Brough et al 2006), we follow the approach in Müller et al (2019a).…”

Section: The External Field Effect Of Three Possible Hostsmentioning

confidence: 99%

A new formulation of the external field effect in MOND and numerical simulations of ultra-diffuse dwarf galaxies – application to NGC 1052-DF2 and NGC 1052-DF4

Haghi

Kroupa

Banik

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The ultra-diffuse dwarf galaxy NGC 1052-DF2 (DF2) has ten (eleven) measured globular clusters (GCs) with a line-of-sight velocity dispersion of σ = 7.8 +5.2 −2.2 km/s (σ = 10.6 +3.9 −2.3 km/s). Our conventional statistical analysis of the original ten GCs gives σ = 8.0 +4.3 −3.0 km/s. The overall distribution of velocities agrees well with a Gaussian of this width. Due to the non-linear Poisson equation in MOND, a dwarf galaxy has weaker self-gravity when in close proximity to a massive host. This external field effect is investigated using a new analytic formulation and fully self-consistent live N-body models in MOND. Our formulation agrees well with that of Famaey and McGaugh (2012). These new simulations confirm our analytic results and suggest that DF2 may be in a deep-freeze state unique to MOND. The correctly calculated MOND velocity dispersion agrees with our inferred dispersion and that of van Dokkum et al. (2018b) if DF2 is within 150 kpc of NGC 1052 and both are 20 Mpc away. The GCs of DF2 are however significantly brighter and larger than normal GCs, a problem which disappears if DF2 is significantly closer to us. A distance of 10-13 Mpc makes DF2 a normal dwarf galaxy even more consistent with MOND and the 13 Mpc distance reported by Trujillo et. al. (2019). We discuss the similar dwarf DF4, finding good agreement with MOND. We also discuss possible massive galaxies near DF2 and DF4 along with their distances and peculiar velocities, noting that NGC 1052 may lie at a distance near 10 Mpc.

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“…Two of the most discussed UDGs (e.g., Hayashi & Inoue 2018;Kroupa et al 2018;Martin et al 2018;Ruiz-Lara et al 2019;Müller et al 2019a;Nusser 2020;Haslbauer et al 2019) are the now famous NGC 1052-DF2 (van Dokkum et al 2018) and NGC 1052-DF4 (van Dokkum et al 2019). These galaxies appear to have a deficiency of dark matter.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters

Müller

Marleau

Duc

et al. 2020

A&A

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The MATLAS deep imaging survey has uncovered a plethora of dwarf galaxies in the low density environment it has mapped. A fraction of them are unusually extended and have low surface brightness. Among these so-called ultra-diffuse galaxies, a few seem to host an excess of globular clusters (GCs). With the integral field unit spectrograph MUSE we have observed one of these galaxies – MATLAS J15052031+0148447 (MATLAS-2019) – located toward the nearby group NGC 5846 and measured its systemic velocity, age, and metallicity, and that of its GC candidates. For the stellar body of MATLAS-2019 we derive a metallicity of −1.33−0.01+0.19 dex and an age of 11.2−0.8+1.8 Gyr. For some of the individual GCs and the stacked GC population, we derive consistent ages and metallicities. From the 11 confirmed GCs and using a Markov Chain Monte Carlo approach we derived a dynamical mass-to-light ratio of 4.2−3.4+8.6 M⊙/L⊙. This is at the lower end of the luminosity-mass scaling relation defined by the Local Group dwarf galaxies. Furthermore, we could not confirm or reject the possibility of a rotational component in the GC system. If present, this would further modify the inferred mass. Follow-up observations of the GC population and of the stellar body of the galaxy are needed to assess whether this galaxy lacks dark matter, as was suggested for the pair of dwarf galaxies in the field of NGC 1052, or if this is a misinterpretation arising from systematic uncertainties of the method commonly used for these systems and the large uncertainties of the individual GC velocities.

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Predicted MOND velocity dispersions for a catalog of ultra-diffuse galaxies in group environments

Cited by 28 publications

References 76 publications

A Second Galaxy Missing Dark Matter in the NGC 1052 Group

A Second Galaxy Missing Dark Matter in the NGC 1052 Group

A new formulation of the external field effect in MOND and numerical simulations of ultra-diffuse dwarf galaxies – application to NGC 1052-DF2 and NGC 1052-DF4

Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters

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