The Model Pages

MODEL SECTION

• Predicted 21cm brightness temperature T₂₁ at high redshift [both `cosmic dawn' (z ≈ 20) and the `dark ages' (z ≈ 100)] for cosmologies with and without dark matter
  • ΛCDM with Planck parameters
  • No CDM model based on McGaugh (2004) (see below)
  • Predictions for the sky-averaged depth of the 21cm absorption signal at high redshift in cosmologies with and without non-baryonic cold dark matter
    McGaugh, S.S., 2018, Phys. Rev. Lett., 121, 081305

• Disk Galaxy Color--Mass-to-Light-Ratio Relations
  • Stellar Population mass-to-light ratio on-line tool
  • The Mass-to-light Ratios and the Star Formation Histories of Disk Galaxies
    Schombert, J.M., McGaugh, S.S., & Lelli, F. 2019, MNRAS, 483, 1496
  • Optical & Near Infrared photometry & colors
  • Table 1 data
  • Table 3 data
  • The bottom line:

    Color--Mass-to-Light Ratio Relations for Disk Galaxies McGaugh, S.S., & Schombert, J.M. 2014, AJ, 148, 77

• Dwarf Spheroidal satellites of Andromeda

  

  • Table of predicted and observed velocity dispersions
  • Andromeda Dwarfs in Light of Modified Newtonian Dynamics
    McGaugh, S.S., & Milgrom, M. 2013, ApJ, 766, 22
  • Andromeda Dwarfs in Light of MOND. II. Testing Prior Predictions
    McGaugh, S.S., & Milgrom, M. 2013, ApJ, 775, 139
  • Perseus I and the NGC 3109 association in the context of the Local Group dwarf galaxy structures
    Pawlowski, M.S., & McGaugh, S.S. 2014, MNRAS, 440, 908

• Milky Way Mass Models

  

  • 2019: Gaia data analyzed with the density profile of 2018 model.
  • Symmetric model: Table 2
  • Gaia data with adjusted Jeans term: Table 3
  • All elements of Fig. 3 (at right: full rotation curve model with the data of others scaled to the same R₀)
  • The Imprint of Spiral Arms on the Galactic Rotation Curve
    McGaugh, S.S. 2019, ApJ, 885, 87

  • 2018: Milky Way Mass Model updated to R₀ = 8.122 kpc.
  • Table of velcoties for all mass components (ascii) MRT (machine readable table)
  • Table including surface densities
  • Milky Way rotation curve for (R₀, Θ₀) = (8.122 kpc, 233.34 km/s): First Quadrant | Fourth Quadrant
    from the HI terminal velocities of McClure-Griffiths & Dickey (2007, 2016). See (and cite!) these papers if you use these data.
  • A Precise Milky Way Rotation Curve Model for an Accurate Galactocentric Distance
    McGaugh, S.S. 2018, RNAAS, 2, 156

    

  • 2016: Milky Way Mass Models based on the mass discrepancy-acceleration relation.
  • Table 1 data: global properties
  • Table 2 data: detailed mass models
  • Digital version of the Clemens (1985) CO terminal velocity data
  • See also the commentary for χ² and addenda.
  • The Surface Density Profile of the Galactic Disk from the Terminal Velocity Curve
    McGaugh, S.S. 2016, ApJ, 816, 42

  • 2008: Models of the radial run of stellar and gas surface density and rotation velocity in the Milky Way.
  • Models are given by disk scale length:
  • 2.0 | 2.1 | 2.2 | 2.3 | 2.4 | 2.5 | 2.7 | 3.0 | 3.5 | 4.0
    NOTE: the density and velocity of the bulge component in these models is given for a fiducial 10¹⁰ solar mass bulge. This needs to be scaled by the mass given in Table 1 of McGaugh (2008) that corresponds to each scale length. For example, for the 2.2 kpc model, Dbulge_2.2 = 0.40*Dbulge and Vbulge_2.2 = sqrt(0.40)*Vbulge.
  • Model fit to terminal velocity curve: bumps & wiggles | the inferred rotation curve
  • Radii in kpc, velocities in km/s, surface densities in solar masses per square parsec.
  • Milky Way Mass Models and MOND
    McGaugh, S.S. 2008, ApJ, 683, 137

• Cosmological Parameters from Rotation Curves

  

  • The concentrations of galaxy halos are related to the cosmology in which they form.*
  • c = 1.88 + 23.9 s₈ G_0.6
    where s₈ is the normalization of the power spectrum and G_0.6 is a modified shape parameter (see eqn 3 of the paper).
  • Data set the limit s₈ G_0.6 < 0.23.
    
  • A Limit on the Cosmological Mass Density and Power Spectrum from the Rotation Curves of Low Surface Brightness Galaxies
    McGaugh, S.S., Barker, M.K., & de Blok, W.J.G. 2003, ApJ, 584, 566
  • *This is related to the halo mass-concentration relation, e.g., Dutton & Maccio (2014)

• Cosmic Microwave Background
  • Purely baryonic model for the ripples in the microwave background which successfully predicted the amplitude of the second peak.
  • Confrontation of Modified Newtonian Dynamics Predictions with WMAP First Year Data
    McGaugh, S.S. 2004, ApJ, 611, 26
  • The model results, 2004.
  • BOOMERanG Data Suggest a Purely Baryonic Universe
    McGaugh, S.S. 2000, ApJ, 541, L33
  • The model results, 2000.
  • Distinguishing Between CDM and MOND: Predictions for the Microwave Background
    McGaugh, S.S. 1999, ApJ, 523, L99

  
  

• HII Region Abundances

  

  • Models and methods for extracting oxygen abundance data from HII region spectra by use of the R₂₃ method of Pagel.
  • Still the most accurate calibration around (van Zee & Haynes 2005; Lopez-Sanchez et al. 2012).

  • Oxygen Abundances and Chemical Evolution in Low Surface Brightness Galaxie
    Kuzio de Naray, R., McGaugh, S.S., & de Blok, W.J.G. 2004, MNRAS, 355, 887
  • Provides a convenient method by which O₃₂-R₂₃ data can be fed into simple analytic formulas which return log(O/H) and log(U).
  • HII Region Abundances: Model Oxygen Line Ratios
    McGaugh, S.S. 1991, ApJ, 380, 140
    
  • The model results.
  • The model HII region grid can be used to generate useful diagrams like the O₃₂-R₂₃ grid (figure) from which abundances and ionization parameters can be determined, e.g.,
  • Oxygen Abundances in Low Surface Brightness Disk Galaxies
    McGaugh, S.S. 1994 ApJ, 426, 135

• Tabulated values of the Bessel functions which appear in the equation for the rotation curve of an exponential disk (Freeman 1970). These sometimes come in handy.

This material is based in part upon work supported by the National Science Foundation under Grant AST0908370.

Stacy wearing theory hat.