Isolated and non-isolated dwarfs in terms of modified Newtonian dynamics

Gentile, Gianfranco; Angus, Garry W.; Famaey, Benoît; Oh, Se Heon; Blok, W. J. G. de

doi:10.1051/0004-6361/201218997

Cited by 13 publications

(21 citation statements)

References 27 publications

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“…where x = R/Ropt and In and Kn are the modified Bessel functions computed at 0.53 x. This scheme is fairly well supported in dds for which the HI surface density data are available (e.g., data from Oh et al 2015;Gentile et al 2010Gentile et al , 2012. In order to clarify the latter, we plot in Fig.…”

Section: Gas Discmentioning

confidence: 71%

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The universal rotation curve of dwarf disc galaxies

Karukes

Salucci

2016

Mon. Not. R. Astron. Soc.

135

197

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We use the concept of the spiral rotation curves universality to investigate the luminous and dark matter properties of the dwarf disc galaxies in the local volume (size ∼ 11 Mpc). Our sample includes 36 objects with rotation curves carefully selected from the literature. We find that, despite the large variations of our sample in luminosities (∼ 2 of dex), the rotation curves in specifically normalized units, look all alike and lead to the lower-mass version of the universal rotation curve of spiral galaxies found in Persic et al. We mass model the double normalized universal rotation curve V (R/R opt )/V opt of dwarf disc galaxies: the results show that these systems are totally dominated by dark matter whose density shows a core size between 2 and 3 stellar disc scale lengths. Similar to galaxies of different Hubble types and luminosities, the core radius r 0 and the central density ρ 0 of the dark matter halo of these objects are related by ρ 0 r 0 ∼ 100 M pc −2 . The structural properties of the dark and luminous matter emerge very well correlated. In addition, to describe these relations, we need to introduce a new parameter, measuring the compactness of light distribution of a (dwarf) disc galaxy. These structural properties also indicate that there is no evidence of abrupt decline at the faint end of the baryonic to halo mass relation. Finally, we find that the distributions of the stellar disc and its dark matter halo are closely related.

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Section: Gas Discmentioning

confidence: 71%

“…The observed circular velocities of HI taking fromGentile et al (2010Gentile et al ( , 2012;Oh et al (2015) (points) and the approximation for the distribution of HI component as described inTonini et al (2006) (dashed lines).…”

mentioning

confidence: 99%

The universal rotation curve of dwarf disc galaxies

Karukes

Salucci

2016

Mon. Not. R. Astron. Soc.

135

197

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“…Such a low inclination (and hence much larger rotation velocities) has been argued for by Gentile et al (2012, see also Sánchez-Salcedo, Hidalgo-Gámez & Martínez-García 2014 after re-analysing the data for DDO 50 presented by Oh et al (2011). The Gentile et al analysis focuses on the low ellipticity of the outer regions of the H I disc, and was motivated by an attempt to reconcile DDO 50 with the predictions of Modified Newtonian Dynamics.…”

Section: Inclination Effectsmentioning

confidence: 87%

Missing dark matter in dwarf galaxies?

Oman

Navarro

Sales

et al. 2016

Mon. Not. R. Astron. Soc.

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“…• from the baryonic TF relation, whereas Gentile et al (2012) constrained the outer value of i between 20…”

Section: Irregularsmentioning

confidence: 99%

Evolution of dwarf galaxies: a dynamical perspective

Lelli

Fraternali

Verheijen

2014

A&A

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For a rotating galaxy, the inner circular-velocity gradient d R V(0) provides a direct estimate of the central dynamical mass density, including gas, stars, and dark matter. We consider 60 low-mass galaxies with high-quality H I and/or stellar rotation curves (including starbursting dwarfs, irregulars, and spheroidals), and estimatewhere R d is the galaxy scale length. For gas-rich dwarfs, we find that V R d /R d correlates with the central surface brightness μ 0 , the mean atomic gas surface density Σ gas , and the star formation rate surface density Σ SFR . Starbursting galaxies, such as blue compact dwarfs (BCDs), generally have higher values of V R d /R d than dwarf irregulars, suggesting that the starburst is closely related to the inner shape of the potential well. There are, however, some "compact" irregulars with values of V R d /R d similar to BCDs. Unless a redistribution of mass takes place, BCDs must evolve into compact irregulars. Rotating spheroidals in the Virgo cluster follow the same correlation between V R d /R d and μ 0 as gasrich dwarfs. They have values of V R d /R d comparable to those of BCDs and compact irregulars, pointing to evolutionary links between these types of dwarfs. Finally, we find that, as for spiral galaxies and massive starbursts, the star-formation activity in dwarfs can be parametrized as Σ SFR = Σ gas /τ orb , where τ orb is the orbital time and 0.02.

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Isolated and non-isolated dwarfs in terms of modified Newtonian dynamics

Cited by 13 publications

References 27 publications

The universal rotation curve of dwarf disc galaxies

The universal rotation curve of dwarf disc galaxies

Missing dark matter in dwarf galaxies?

Evolution of dwarf galaxies: a dynamical perspective

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