Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM

Read, Justin I.; Iorio, Giuliano; Agertz, Oscar; Fraternali, Filippo

doi:10.1093/mnras/stw1876

Cited by 227 publications

(303 citation statements)

References 137 publications

(143 reference statements)

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“…A similar higher-than-expected stellar mass to halo mass ratio is observed for dwarf galaxies (e.g., Boylan-Kolchin et al 2012;Ferrero et al 2012;Miller et al 2014;Brook et al 2014;Read et al 2017). While the low-mass galaxy sub-samples used in this paper are not as low mass as the dwarf galaxies observed in the local group (the minimum stellar mass of VUDS galaxies used in our sample is M = 10 8.75 M while the masses of local dwarf galaxies are 10 6 − 10 9 M ), the low mass observationmodels discrepancy of SHMR we observe is consistent with these low-mass low redshift samples and it is possible that similar processes are behind it at high z for the higher mass galaxies.…”

Section: The Stellar To Halo Mass Relation For Low Mass Galaxiessupporting

confidence: 71%

The VIMOS Ultra Deep Survey

Durkalec

Fèvre

Pollo

et al. 2018

A&A

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We present the study of the dependence of galaxy clustering on luminosity and stellar mass in the redshift range 2 < z < 3.5 using 3236 galaxies with robust spectroscopic redshifts from the VIMOS Ultra Deep Survey (VUDS), covering a total area of 0.92 deg 2 . We measure the two-point real-space correlation function w p (r p ) for four volume-limited sub-samples selected by stellar mass and four volume-limited sub-samples selected by M UV absolute magnitude. We find that the scale dependent clustering amplitude r 0 significantly increases with increasing luminosity and stellar mass. For the least luminous galaxies (M UV < −19.0) we measure a correlation length r 0 = 2.87 ± 0.22 h −1 Mpc and slope γ = 1.59 ± 0.07, while for the most luminous (M UV < −20.2) r 0 = 5.35 ± 0.50 h −1 Mpc and γ = 1.92 ± 0.25. This corresponds to a strong relative bias between these two sub-samples of ∆b/b * = 0.43. Fitting a 5-parameter HOD model we find that the most luminous (M UV < −20.2) and massive (M > 10 10 h −1 M ) galaxies occupy the most massive dark matter haloes with M h = 10 12.30 h −1 M . Similar to the trends observed at lower redshift, the minimum halo mass M min depends on the luminosity and stellar mass of galaxies and grows from M min = 10 9.73 h −1 M to M min = 10 11.58 h −1 M from the faintest to the brightest among our galaxy sample, respectively. We find the difference between these halo masses to be much more pronounced than is observed for local galaxies of similar properties. Moreover, at z ∼ 3, we observe that the masses at which a halo hosts, on average, one satellite and one central galaxy is M 1 ≈ 4M min over all luminosity ranges, significantly lower than observed at z ∼ 0 indicating that the halo satellite occupation increases with redshift. The luminosity and stellar mass dependence is also reflected in the measurements of the large scale galaxy bias, which we model as b g,HOD (> L) = 1.92 + 25.36(L/L * ) 7.01 . We conclude our study with measurements of the stellar-to-halo mass ratio (SHMR). We observe a significant model-observation discrepancy for low-mass galaxies, suggesting a higher than expected star formation efficiency of these galaxies.

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Section: The Stellar To Halo Mass Relation For Low Mass Galaxiessupporting

confidence: 71%

The VIMOS Ultra Deep Survey

Durkalec

Fèvre

Pollo

et al. 2018

A&A

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“…The discussion in Garrison-Kimmel et al (2014) suggests that if Read et al (2016b) were to use the Baldry et al (2012) Constraints from this works: we show 68/95% credibility intervals (dark/light coloured bands) on the posterior predictive SMHM relation for two of our present models, both of which include the effect of the MW disk. In red, we show constraints on stellar mass for a given halo mass (to be interpreted vertically) assuming our fiducial SMHM model; in yellow, constraints on halo mass for a given stellar mass (to be interpreted horizontally) assuming our scatter model.…”

Section: Implications For Reionisationmentioning

confidence: 58%

“…Read et al (2016b) also argue that a shallow SMHM relation may be made consistent with the Local Group galaxy abundance if environmental factors re-shape the field-derived SMHM relation, alleviating the tensions found by Garrison-Kimmel et al (2014).…”

Section: Implications For Reionisationmentioning

confidence: 79%

“…Three of these (Garrison-Kimmel et al 2014, cyan;Brook et al 2014, blue;Koposov et al 2009, red) predict SMHM relations consistent with our constraints on stellar mass at fixed halo mass for our fiducial SMHM relation (1σ/2σ constraints shown by dark/light red bands). Two other works are discrepant: Read et al (2016b) predict a significantly shallower relation (black), while GarrisonKimmel et al (2017) a somewhat steeper one (magenta). To understand why these differences arise, we briefly discuss the methodologies and data-sets used in these works.…”

Section: Implications For Reionisationmentioning

confidence: 93%

“…For their abundance matching study, Read et al (2016b) use the same observational data-set as Behroozi et al (2013a), finding a shallow inferred SMHM relation (black line). The discussion in Garrison-Kimmel et al (2014) suggests that if Read et al (2016b) were to use the Baldry et al (2012) Constraints from this works: we show 68/95% credibility intervals (dark/light coloured bands) on the posterior predictive SMHM relation for two of our present models, both of which include the effect of the MW disk.…”

Section: Implications For Reionisationmentioning

confidence: 99%

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The upper bound on the lowest mass halo

Jethwa¹,

Erkal²,

Belokurov³

2017

Monthly Notices of the Royal Astronomical Society

176

207

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We explore the connection between galaxies and dark matter halos in the Milky Way (MW) and quantify the implications on properties of the dark matter particle and the phenomenology of low-mass galaxy formation. This is done through a probabilistic comparison of the luminosity function of MW dwarf satellite galaxies to models based on two suites of zoom-in simulations. One suite is dark-matter-only while the other includes a disk component, therefore we can quantify the effect of the MW's baryonic disk on our results. We apply numerous Stellar-Mass-Halo-Mass (SMHM) relations allowing for multiple complexities: scatter, a characteristic break scale, and subhalos which host no galaxy. In contrast to previous works we push the model/data comparison to the faintest dwarfs by modeling observational incompleteness, allowing us to draw three new conclusions. Firstly, we constrain the SMHM relation for 10 2 < M * /M < 10 8 galaxies, allowing us to bound the peak halo mass of the faintest MW satellite to M vir > 2.4 × 10 8 M (1σ). Secondly, by translating to a Warm Dark Matter (WDM) cosmology, we bound the thermal relic mass m WDM > 2.9 keV at 95% confidence, on a par with recent constraints from the Lyman-α forest. Lastly, we find that the observed number of ultra-faint MW dwarfs is in tension with the theoretical prediction that reionisation prevents galaxy formation in almost all 10 8 M halos. This can be tested with the next generation of deep imaging surveys. To this end, we predict the likely number of detectable satellite galaxies in the Subaru/HSC survey and the LSST. Confronting these predictions with future observations will be amongst our strongest tests of WDM and the effect reionisation on low-mass systems.

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Hi in the Outskirts of Nearby Galaxies

Bosma

2017

Astrophysics and Space Science Library

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The HI in disk galaxies frequently extends beyond the optical image, and can trace the dark matter there. I briefly highlight the history of high spatial resolution HI imaging, the contribution it made to the dark matter problem, and the current tension between several dynamical methods to break the disk-halo degeneracy. I then turn to the flaring problem, which could in principle probe the shape of the dark halo. Instead, however, a lot of attention is now devoted to understanding the role of gas accretion via galactic fountains. The current Λ cold dark matter theory has problems on galactic scales, such as the core-cusp problem, which can be addressed with HI observations of dwarf galaxies. For a similar range in rotation velocities, galaxies of type Sd have thin disks, while those of type Im are much thicker. After a few comments on modified Newtonian dynamics and on irregular galaxies, I close with statistics on the HI extent of galaxies.

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Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM

Cited by 227 publications

References 137 publications

The VIMOS Ultra Deep Survey

The VIMOS Ultra Deep Survey

The upper bound on the lowest mass halo

Hi in the Outskirts of Nearby Galaxies

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