The kinematic connection between galaxies and dark matter haloes

By A. Dutton, C. Conroy, F. V. D. Bosch, Francisco Prada, S. More. 2010

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Using estimates of dark halo masses from satellite kinematics, weak gravitational lensing and halo abundance matching, combined with the Tully-Fisher (TF) and Faber-Jackson relations, we derive the mean relation between the optical, V opt, and virial, V 200, circular velocities of early- and late-type galaxies at redshift z � 0. For late-type galaxies, VoptV200 over the velocity range V opt = 90-260 km s −1 , and is consistent with V opt = V max,h (the maximum circular velocity of NFW dark matter haloes in the concordancecold dark matter (� CDM) cosmology). However, for early-type galaxies VoptV200, with the exception of early-type galaxies with Vopt � 350 km s −1 . This is inconsistent with early-type galaxies being, in general, globally isothermal. For low-mass (Vopt 250 km s −1 ) early-types V opt > V max,h, indicating that baryons have modified the potential well, while high-mass (Vopt 400 km s −1 ) early-types have V opt < V max,h. Folding in measurements of the black hole mass-velocity dispersion relation, our results imply that the supermassive black hole-halo mass relation has a logarithmic slope which varies from � 1. 4a t halo masses of� 10 12 h −1 Mto � 0.65 at halo masses of 10 13.5 h −1 M� . The values of V opt/V 200 we infer for the Milky Way (MW) and M31 are lower than the values currently favoured by direct observations and dynamical models. This offset is due to the fact that the MW and M31 have higher V opt and lower V 200 compared to typical late-type galaxies of the same stellar masses. We show that current high-resolution cosmological hydrodynamical simulations are unable to form galaxies which simultaneously reproduce both the V opt/V 200 ratio and the V opt-Mstar (Tully-Fisher/Faber-Jackson) relation.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fe38357ecac279c496b1724ecb851aae229b3f2c

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Citations in the corpus

GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, result): “Other authors have come to the same conclusions (e.g., Williams et al. 2010; Dutton et al. 2010, 2011).”
THE SPACE MOTION OF LEO I: THE MASS OF THE MILKY WAY'S DARK MATTER HALO (2012, methodology): “Dutton et al. (2010) and Reyes et al. (2011) parameterize this combination of data in terms of the typical ratio of a galaxy’s optical velocity Vopt (the circular velocity at 2.2 disk scale radii) to its virial velocity6 V200c.”
THE VELOCITY WIDTH FUNCTION OF GALAXIES FROM THE 40% ALFALFA SURVEY: SHEDDING LIGHT ON THE COLD DARK MATTER OVERABUNDANCE PROBLEM (2011, background): “However, the vrot/vhalo ratios obtained here are significantly larger than the average values inferred by Dutton et al. (2010) from a compilation of weak lensing and satellite kinematics datasets.”
FORMING REALISTIC LATE-TYPE SPIRALS IN A ΛCDM UNIVERSE: THE ERIS SIMULATION (2011, methodology): “2/V200 ratios from Smith et al. (2007) and Xue et al. (2008), were computed by Dutton et al. (2010) from these data sets after converting different virial mass definitions and for an assumed Milky Way’s V2.”
The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores (2013, methodology): “Using our results and the stellar mass TF relation from Dutton et al. (2010), we find that the flattest inner profiles are expected for galaxies withVrot ∼ 50 kms−1. α decreases for more massive galaxies, leading to cuspier profiles and eventually reaching the NFW prediction at the Milky Way mass.”
THE NEXT GENERATION VIRGO CLUSTER SURVEY (NGVS). I. INTRODUCTION TO THE SURVEY (2012, background): “The NGVS will allow an important first step toward defining a unified set of scaling relations to describe galaxies of different mass and morphology (e.g., Kassin et al. 2007; Dutton et al. 2010, 2011; McLaughlin et al. 2012).”
Two-dimensional kinematics of SLACS lenses – III. Mass structure and dynamics of early-type lens galaxies beyond z ≃ 0.1 (2011, unknown): “2009, Dutton et al. 2010).”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, methodology): “…(WL: Mandelbaum et al. 2006, 2008; Schulz et al. 2010; SK: Conroy et al. 2007; Klypin & Prada 2009; More et al. 2011) and took care to scale the stellar masses from these studies to a common Chabrier IMF and to adopt a common halo mass definition (M200,c; see Dutton et al. 2010 for more details).”
DARK AND LUMINOUS MATTER IN THINGS DWARF GALAXIES (2010, result): “Considering that more luminous galaxies are in general more massive (e.g., Guo et al. 2010; Dutton et al. 2010), this is largely consistent with the relationship between γdm and absolute B magnitude, as shown above.”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, background): “We therefore adopt the relations for 〈f⋆〉(M⋆) derived by Dutton et al. (2010).”
The local dark matter density (2014, background): “Such processes may even be important for galaxies as massive as the Milky Way (Dutton et al., 2010; Macciò et al., 2012).”
Constraints on star formation driven galaxy winds from the mass–metallicity relation at z= 0 (2010, result): “2005, 2009; Dutton et al. 2010b).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, methodology): “28star (Dutton et al. 2010b), where σe is the velocity dispersion within the half-light radius, and V2.”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, background): “The second line of evidence comes from direct halo mass measurements, obtained through weak lensing or kinematics studies (e.g. Dutton et al. 2010; Reyes et al. 2012).”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, methodology): “Therefore, a similar analysis as Dutton et al. (2010) but applied to the Pizagno et al. (2007) data in combination with our results would yield a higher Vopt/V200.”
Hierarchical formation of bulgeless galaxies – II. Redistribution of angular momentum via galactic fountains (2011, background): “…estimates of the relationship between stellar mass and halo mass (Mandelbaum et al. 2006; Koposov et al. 2008; Guo et al. 2010; Moster et al. 2010; Dutton et al. 2010; More et al. 2011; Avila-Reese et al. 2011) indicate that the current simulation has a factor ∼ 2 − 3 too many stars, implying…”
Galaxy Masses: A Review (2013, methodology): “By comparing with the rotation velocities within the optical disk, Vopt, one finds that on average for late-type galaxies Vopt/V200 ' 1.2 (Dutton et al. 2010; Reyes et al. 2011).”
The Sydney-AAO Multi-object Integral field spectrograph (2011, result): “Circular velocities can be compared to the results of galaxy lensing to constrain the dark matter halo profile and examine evidence of contraction of the halo in response to the baryons (Dutton et al. 2010; Reyes et al. 2011).”
Satellite kinematics – III. Halo masses of central galaxies in SDSS (2010, unknown): “Overall, the results obtained using all these very different methods are in remarkably good agreement with each other (see also Behroozi et al. 2010; Dutton et al. 2010), and with the results obtained here.”