Maximum Disk Mass Models for Spiral Galaxies

Palunas, Povilas; Williams, T. B.

doi:10.1086/316878

Cited by 161 publications

(239 citation statements)

References 61 publications

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“…For maximum disk, a crit < a 0 , which simply says that the mass discrepancy appears at a somewhat lower acceleration, as should be true by construction. A similar result can be seen in other data (e.g., Palunas & Williams 2000), although the availability of the gas component is necessary for the smooth appearance in Figure 5. The correlation appears to break down at low accelerations if the gas component is neglected, since it is often the dominant baryonic component at large radii and low accelerations.…”

Section: Constraints On Halo Parameters From the Acceleration Scalesupporting

confidence: 89%

“…One manifestation of this is in the efficacy of maximum disk (e.g., van Albada & Sancisi 1986) in describing the inner parts of rotation curves. If one scales up the stellar contribution to the rotation curves of high surface brightness (HSB) spirals to the maximum allowed by the data, one often finds a good match in the details (the ''bumps and wiggles'') between the shape of the rotation curve and that predicted by the observed stellar mass (e.g., Kalnajs 1983;Sellwood 1999;Palunas & Williams 2000). This only works out to some radius where dark matter must be invoked but does suggest that the preponderance of the mass at small radii is stellar.…”

Section: Introductionmentioning

confidence: 99%

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The Mass Discrepancy–Acceleration Relation: Disk Mass and the Dark Matter Distribution

McGaugh

2004

ApJ

217

309

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The mass discrepancy in disk galaxies is shown to be well correlated with acceleration, increasing systematically with decreasing acceleration below a critical scale a 0 % 3700 km 2 s À2 kpc À1 ¼ 1:2 ; 10 À10 m s À2 . For each galaxy, there is an optimal choice of stellar mass-to-light ratio that minimizes the scatter in this mass discrepancy-acceleration relation. The same mass-to-light ratios also minimize the scatter in the baryonic TullyFisher relation and are in excellent agreement with the expectations of stellar population synthesis. Once the disk mass is determined in this fashion, the dark matter distribution is specified. The circular velocity attributable to the dark matter can be expressed as a simple equation that depends only on the observed distribution of baryonic mass. It is a challenge to understand how this very fine-tuned coupling between mass and light comes about.

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Section: Constraints On Halo Parameters From the Acceleration Scalesupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

The Mass Discrepancy–Acceleration Relation: Disk Mass and the Dark Matter Distribution

McGaugh

2004

ApJ

217

309

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“…Palunas & Williams (2000) give maximum disc M/L I-band ratios for a sample of 74 spiral galaxies. The luminosities of their galaxies have been corrected for absorption as if observed face-on.…”

Section: The Mass-to-light Ratiomentioning

confidence: 99%

Dark and luminous matter in the NGC 3992 group of galaxies

Bottema¹,

Verheijen²

2002

A&A

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Abstract. Detailed neutral hydrogen observations have been obtained of the large barred spiral galaxy NGC 3992 and its three small companion galaxies, UGC 6923, UGC 6940, and UGC 6969. For the main galaxy, the H i distribution is regular with a low level radial extension outside the stellar disc. However, at exactly the region of the bar, there is a pronounced central H i hole in the gas distribution. Likely gas has been transported inwards by the bar and because of the emptyness of the hole no large accretion events can have happened in recent galactic times. The gas kinematics is very regular and it is demonstrated that the influence of the bar potential on the velocity field is negligible. A precise and extended rotation curve has been derived showing some distinct features which can be explained by the non-exponential radial light distribution of NGC 3992. The decomposition of the rotation curve gives a slight preference for a sub maximal disc, though a range of disc contributions, up to a maximum disc situation fits nearly equally well. For such a maximum disc contribution, which might be expected in order to generate and maintain the bar, the required mass-to-light ratio is large but not exceptional.

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“…Additionally, the HI rotation curves are almost always calculated from the observe surface densities assuming that the disc is effectively infinite, systematically minimizing the rotation curve velocity at the edge of the discs (Casertano 1983). -"... scaling of HI to represent the dark component only works in combination with maximal discs" (Palunas & Williams 2000). This effect is not surprising, since the models using HI alone could simply be correcting for the missing H 2 gas component most strongly associated with the stars.…”

Section: Introductionmentioning

confidence: 99%

The Bosma effect revisited

Hessman

Ziebart

2011

A&A

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Context. The observed proportionality between the centripetal contribution of the dynamically insignificant HI gas in the discs of spiral galaxies and the dominant contribution of dark matter (DM) -the "Bosma effect" -has been repeatedly mentioned in the literature but largely ignored. Since this phenomenology, if statistically significant, tells us something about the relationship between the visible baryonic and invisible DM, it is important to re-examine the reality of this effect using formal tests and more modern data. Aims. We have re-examined the evidence for the Bosma effect, either by scaling the contribution of the HI gas alone or by using both the observed stellar disc and HI gas as proxies. Methods. We have calculated Bosma effect models for 17 galaxies in The HI Nearby Galaxy Survey data set. The results are compared with two models for exotic cold DM: internally consistent cosmological Navarro-Frenk-White (NFW) models with constrained compactness parameters, and "universal rotation curve" (URC) models using fully unconstrained Burkert density profiles. Results. Fits to spiral galaxy rotation curves computed using just HI scaling are inadequate, despite the clear proportionality seen in the outer discs. The poor performance is obviously related to the prominent decrease in the HI surface density in regions of high stellar surface density, where HI has been converted into molecules and stars. The Bosma models that partially correct for this physical effect using the stellar discs as additional proxies are statistically nearly as good as the URC models and clearly better than the NFW ones. Conclusions. We confirm the correlation between the centripetal effects of DM and that of the interstellar medium of spiral galaxies. The efficacy of "maximal disc" models is explained as the natural consequence of "classic" Bosma models which include the stellar disc as a proxy in regions of reduced atomic gas. The perception that the Bosma effect could be due to the near-equality of the HI surface density and the projected mass density of a cold DM halo is incorrect, both theoretically and empirically. The standard explanation -that the effect reflects a statistical correlation between the visible and exotic DM -seems highly unlikely, given that the geometric forms and hence centripetal signatures of spherical halo and disc components are so different. A literal interpretation of the Bosma effect as being due to the presence of significant amounts of disc DM requires a median visible baryon to disc DM ratio of about 40%.

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Maximum Disk Mass Models for Spiral Galaxies

Cited by 161 publications

References 61 publications

The Mass Discrepancy–Acceleration Relation: Disk Mass and the Dark Matter Distribution

The Mass Discrepancy–Acceleration Relation: Disk Mass and the Dark Matter Distribution

Dark and luminous matter in the NGC 3992 group of galaxies

The Bosma effect revisited

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