Simulations of galactic disks including a dark baryonic component

Revaz, Yves; Pfenniger, D.; Combes, F.; Bournaud, F.

doi:10.1051/0004-6361/200809883

Cited by 31 publications

(33 citation statements)

References 98 publications

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“…Observations of X-ray absorption lines have yielded large variations in the mass and distribution of the WHIM in the Milky Way: from ∼4×10 8 M ⊙ within 20 kpc (Bregman & Lloyd-Davies 2007) to ∼10 10 M ⊙ within 100 kpc (Gupta et al 2012). Studies of the baryonic Tully-Fisher relation suggest that there could be missing gas in the galaxy disk that scales with the HI gas component (Pfenniger & Revaz 2005;Begum et al 2008;Revaz et al 2009). These studies find that a multiplicative factor of 3-11 applied to the HI mass produces a tighter Tully-Fisher relation across dwarf to giant galaxy scales.…”

Section: Discussionmentioning

confidence: 99%

The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

Eckert

Kannappan

Lagos

et al. 2017

ApJ

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We examine the z = 0 group-integrated stellar and cold baryonic (stars + cold atomic gas) mass functions (group SMF and CBMF) and the baryonic collapse efficiency (group cold baryonic to dark matter halo mass ratio) using the RESOLVE and ECO survey galaxy group catalogs and a galform semi-analytic model (SAM) mock catalog. The group SMF and CBMF fall off more steeply at high masses and rise with a shallower low-mass slope than the theoretical halo mass function (HMF). The transition occurs at group-integrated cold baryonic mass M cold bary ∼ 10 11 M ⊙ . The SAM, however, has significantly fewer groups at the transition mass ∼1011 M ⊙ and a steeper low-mass slope than the data, suggesting that feedback is too weak in low-mass halos and conversely too strong near the transition mass. Using literature prescriptions to include hot halo gas and potential unobservable galaxy gas produces a group BMF with slope similar to the HMF even below the transition mass. Its normalization is lower by a factor of ∼2, in agreement with estimates of warm-hot gas making up the remaining difference. We compute baryonic collapse efficiency with the halo mass calculated two ways, via halo abundance matching (HAM) and via dynamics (extended all the way to three-galaxy groups using stacking). Using HAM, we find that baryonic collapse efficiencies reach a flat maximum for groups across the halo mass range of M halo ∼ 10 11.4−12 M ⊙ , which we label "nascent groups." Using dynamics, however, we find greater scatter in baryonic collapse efficiencies, likely indicating variation in group hot-to-cold baryon ratios. Similarly, we see higher scatter in baryonic collapse efficiencies in the SAM when using its true groups and their group halo masses as opposed to friends-of-friends groups and HAM masses.

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Section: Discussionmentioning

confidence: 99%

The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

Eckert

Kannappan

Lagos

et al. 2017

ApJ

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“…A candidate for disc DM that would naturally explain the Bosma effect is a nearly invisible ISM component consisting of very dense and cold H 2 cloudlets Gerhard & Silk 1996) whose dynamical effects within the galaxies could be very different from those usually assumed for the visible matter (Revaz et al 2009). Indeed, there are many reasons based on the formation and dissociation of H 2 to believe that the visible HI structures in galaxies belie only a fraction of the true gaseous content, fully independently of any questions concerning their centripetal signatures (Allen 2004).…”

Section: Discussionmentioning

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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“…Let us add that a factor c larger than 7 appears less likely from a dynamical point of view (Revaz et al 2008). With such a large factor, the total mass in gas (HI and dark) is about the same order as that in the stellar disc, at a redshift z = 0.…”

Section: Discussionmentioning

confidence: 99%

MOND and the dark baryons

Tiret¹,

Combes²

2009

A&A

Self Cite

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We consider for the first time the implications for the modified gravity MOND model of galaxies, of the presence of dark baryons, in the form of cold molecular gas in galaxy discs. We show that MOND models of rotation curves are still valid and universal, but the critical acceleration a 0 separating the Newtonian and MONDian regimes has a lower value. We quantify this modification as a function of the scale factor c between the total gas of the galaxy and the measured atomic gas. The main analysis concerns 43 resolved rotation curves and allows us to find the best pair (a 0 = 0.96 × 10 −10 m s −2 , c = 3), which is also compatible with the one obtained from a second method minimizing the scatter in the baryonic Tully-Fisher relation.

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Simulations of galactic disks including a dark baryonic component

Cited by 31 publications

References 98 publications

The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

The Bosma effect revisited

MOND and the dark baryons

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