The Data Pages

• Mass Models and Rotation Curves
• 175 disk galaxies of all morphological types T ≥ 0
• Homogeneous [3.6] micron surface photometry
• HI rotation curves supplemented in some cases with Hα data
• See the SPARC data page

• [3.6] micron surface photometry
• [Images & charts] | [XML] | [Query script] (type "./xml_archangel.py -h" for list of options)
• Stellar Populations and the Star Formation Histories of LSB Galaxies: IV Spitzer Surface Photometry of LSB Galaxies
  Schombert, J.M., & McGaugh, S.S. 2014, PASA, 31, e011

• Optical surface photometry, colors, & Hα data
• [Surface brightness profiles] | [Color maps]
• Stellar Populations and the Star Formation Histories of LSB Galaxies: I. Optical and H-alpha Imaging
  Schombert, J.M., Maciel, T., & McGaugh, S.S. 2011, Advances in Astronomy, 2011, 143698 (18pp)
• Breif presentation

• The main sequence of low mass star forming galaxies is linear (SFR ∝ M_* with slope 1.04 ± 0.06)
• Masses and star formation rates from Table 1 of
• The Star-forming Main Sequence of Dwarf Low Surface Brightness Galaxies
  McGaugh, S.S.,Schombert, J.M., & Lelli, F. 2017, ApJ, 851, 22 (9pp)

• Data for Local Group Dwarf Satellites.
• Table 1 data
• Table 2 data from
• Local Group Dwarf Spheroidals: Correlated Deviations from the Baryonic Tully-Fisher Relation
  McGaugh, S.S., & Wolf, J. 2010, ApJ, 722, 248

• The baryon fractions of objects ranging from the smallest dwarf galaxies to the largest clusters of galaxies.
• The figures: Fig. 1 | Fig. 2 | logarithmic version of Fig. 2
• The data: Table 2 from
• The Baryon Content of Cosmic Structures
  McGaugh, S.S., Schombert, J.M., de Blok, W.J.G., & Zagursky, M.J. 2010, ApJ, 708, L14

• The rotation curves derives from two dimensional velocity fields observed with densepak.
• The data: densepak rotation curves.
• Mass Models of Low Surface Brightness Galaxies with High Resolution Optical Velocity Fields
  Kuzio de Naray, R., McGaugh, S.S., & de Blok, W.J.G. 2008, ApJ, 676, 920
• High Resolution Optical Velocity Fields of 11 Low Surface Brightness Galaxies
  Kuzio de Naray, R., McGaugh, S.S., de Blok, W.J.G., & Bosma, A. 2006, ApJS, 165, 461

• The rotation curves of LSB galaxies with long slit Halpha observations. A subset also have 21 cm data and mass models (the rotation due to the luminsous mass components, stars & gas).
• The data: Halpha position-velocity data.
• High-resolution rotation curves of low surface brightness galaxies: Data
  McGaugh, S.S., Rubin, V.C., & de Blok, W.J.G. 2001, AJ, 122, 2381
• The data: Smoothed hybrid Halpha-HI rotation curves.
• High-resolution rotation curves of low surface brightness galaxies: Mass Models
  de Blok, W.J.G., McGaugh, S.S., & Rubin, V.C. 2001, AJ, 122, 2396

• Older rotation curves:
  HI Observations of Low Surface Brightness Galaxies: Probing Low Density Galaxies
  de Blok, W.J.G., McGaugh, S.S., & van der Hulst, J.M. 1996, MNRAS, 283, 18.
  Associated mass models: R-band stellar mass models and HI gas mass models.

• Disk galaxies obey a relation between between disk mass (stars + gas) and rotation velocity (V_flat) over at least 5 decades in stellar mass.

• 2016 estimate of the intrinsic scatter:
• The intrinsic scatter of the BTFR is small: ≤ 0.11 dex in mass, consistent with zero.
• The data from
  The Small Scatter of the Baryonic Tully-Fisher Relation
  Lelli, F., McGaugh, S.S. & Schombert, J.M. 2016, ApJ, 816, L14

• 2015 calibration:
• The typical mass-to-light ratio is M_*/L = 0.45 at [3.6] and 0.57 in K_s (Msun/Lsun).
• The data (Table 1) and
• The data (Table 3) from
  Weighing Galaxy Disks with the Baryonic Tully-Fisher Relation
  McGaugh, S.S. & Schombert, J.M. 2015, ApJ, 802, 18

• 2011 calibration: M_d = 47 V⁴. Equivalent acceleration scale: a₀ = 1.3 x 10^-10 m s^-2.
  
• The data from The Baryonic Tully-Fisher Relation of Gas Rich Galaxies as a Test of ΛCDM and MOND
  McGaugh, S.S. 2012, AJ, 143, 40
  as used in
  A Novel Test of the Modified Newtonian Dynamics with Gas Rich Galaxies
  McGaugh, S.S. 2011, Phys. Rev. Lett., 106, 121303

• 2009 calibration:
• log(M_b) = x*log(Vf)+A with x = 3.94 ± 0.07 (random) ± 0.08 (systematic) and A = 1.79 ± 0.26 (random) ± 0.25 (systematic).
• Fit with slope fixed to 4: M_d = 45 V⁴.
  
• This calibration uses data for gas dominated galaxies with well measured rotation curves.
• The data from A First Attempt to Calibrate the Baryonic Tully-Fisher Relation with Gas Dominated Galaxies
  Stark, D.V., McGaugh, S.S., & Swaters, R.A. 2009, AJ, 138, 392

• 2005 calibration: M_d = 50 V⁴.
  This calibration uses only data where V_flat has been measured.
• The data from The Baryonic Tully-Fisher Relation of Galaxies with Extended Rotation Curves and the Stellar Mass of Rotating Galaxies
  McGaugh, S.S. 2005, ApJ, 632, 859.

• Original paper:
  The Baryonic Tully-Fisher Relation
  McGaugh, S.S., Schombert, J.M., Bothun, G.D., & de Blok, W.J.G. 2000, ApJ, 533, L99
• The data used in the original paper.

• Disk galaxies obey a relation between between the amplitude of the mass discrepancy (defined as the square of the ratio of the actual velocity to that expected for the baryons) and the acceleration. See also the radial acceleration relation on the SPARC data page.

• The data from Figure 9 and
  
• The data from Figure 10 of
  Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions
  Famaey, B., & McGaugh, S.S. 2012, Living Reviews in Relativity.
  The three panels of Fig. 10 are demarcated by the string "Panel".

• The data from Figure 5 of
  The Mass Discrepancy-Acceleration Relation: Disk Mass and the Dark Matter Distribution
  McGaugh, S.S. 2004, ApJ, 609, 652.
  There is a separate data file for each of the 8 panels of the figure, correpsonding to the different assumptions about stellar mass.

• MOND fits from
  Modified Newtonian Dynamics as an Alternative to Dark Matter
  Sanders, R.H., & McGaugh, S.S. 2002, ARA&A, 40, 263
• See also predictions on the Model Page.

• Mass models used in McGaugh et al. 2007, ApJ, 659, 149.
• The data.
• Tabulated for each galaxy are the radius (in kpc), the observed velocity (in km/s), the velocity due to the gas mass, the velocity of the stellar mass for the MDacc M/L, and the scaling factors to obtain the maximum disk M/L (Qmax) and population synthesis M/L (Qpop).

• FITS format CCD data with images of numerous LSB galaxies in UBVI and Halpha. The data have been flattened, etc.
• The data.
• The Morphology of Low Surface Brightness Disk Galaxies
  McGaugh, S.S., Schombert, J.M., & Bothun, G.D. 1995, AJ, 109, 2019
• Structural Characteristics and Stellar Composition of Low Surface Brightness Disk Galaxies
  McGaugh, S.S., & Bothun, G.D. 1994, AJ, 107, 530

The MODEL SECTION has moved to http://astroweb.case.edu/ssm/models/.

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

Much of these data brought to you by Team Diplomacy.