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J/A+A/612/L6       j-M law from dwarf to massive spirals         (Posti+, 2018)

The angular momentum-mass relation: a fundamental law from dwarf irregulars to massive spirals. Posti L., Fraternali F., di Teodoro E. M., Pezzulli G. <Astron. Astrophys. 612, L6 (2018)> =2018A&A...612L...6P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby; Stars, masses Keywords: galaxies: kinematics and dynamics - galaxies: spiral - galaxies: structure - galaxies: formation Abstract: In a {LAMBDA} CDM Universe, the specific stellar angular momentum (j*) and stellar mass (M*) of a galaxy are correlated as a consequence of the scaling existing for dark matter haloes (jh∝2/3). The shape of this law is crucial to test galaxy formation models, which are currently discrepant especially at the lowest masses, allowing to constrain fundamental parameters, such as, for example, the retained fraction of angular momentum. In this study, we accurately determine the empirical j*-M* relation (Fall relation) for 92 nearby spiral galaxies (from S0 to Irr) selected from the Spitzer Photometry and Accurate Rotation Curves (SPARC) sample in the unprecedented mass range 7≲logM*/M≲11.5. We significantly improve all previous estimates of the Fall relation by determining j* profiles homogeneously for all galaxies, using extended HI rotation curves, and selecting only galaxies for which a robust j* could be measured (converged j*(<R) radial profile). We find the relation to be well described by a single, unbroken power-law j*αM*α over the entire mass range, with α=0.55±0.02 and orthogonal intrinsic scatter of 0.17±0.01dex. We finally discuss some implications of this fundamental scaling law for galaxy formation models and, in particular, the fact that it excludes models in which discs of all masses retain the same fraction of the halo angular momentum. Description: The table contains the estimates of the stellar masses and specific angular momenta of 92 spiral galaxies in the SPARC sample (Lelli et al., 2016, Cat. J/AJ/152/157). Estimates are given both for the whole galaxy and only for its disc component, together with standard uncertainties. Two flags on the quality of the measurements, assessing whether the observed specific angular momentum profiles have reached convergence (defined in Eq. 2 in the paper), are also provided. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table.dat 81 92 List of galaxy masses and specific angular momenta
See also: J/AJ/152/157 : Mass models for 175 disk galaxies with SPARC (Lelli+, 2016) Byte-by-byte Description of file: table.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Galaxy Galaxy name (1) 14- 15 I2 --- T Hubble type (1) 17 I1 --- fD [1/5] Distance method (2) 19- 26 E8.2 Msun Mstar Galaxy's stellar mass (3) 28- 35 E8.2 Msun Mdisc Disc's stellar mass (3) 37- 44 E8.2 Msun e_Mstar Uncertainty on the stellar masses (3) 46- 53 E8.2 jstar Galaxy's specific angular momentum 55- 62 E8.2 jdisc Disc's specific angular momentum 64- 71 E8.2 e_jstar Uncertainty on the specific angular momenta 73- 76 F4.2 --- jdiff Relative difference between last 2 points of jstar profile (4) 78- 81 F4.2 --- jgrad Gradient of jstar profile at last grid point (4)
Note (1): same convention as in Lelli, McGaugh & Schombert, 2016, Cat. J/AJ/152/157 Note (2): SPARC galaxies classification depending on the distance estimate is defined as follows: 1 = Hubble-Flow assuming H0=73km/s/Mpc and correcting for Virgo-centric infall 2 = Magnitude of the tip of the red giant branch 3 = Cepheids magnitude-period relation 4 = Ursa Major cluster of galaxies 5 = Supernovae light curve Note (3): the following 3.6mu mass-to-light ratios have been used M/Lbulge=0.5, M/Ldisc=0.7. Note (4): these two quantities define the quality of the measured specific angular momentum profile and they are defined in Equation (2). Galaxies with "converged" jstar(<R) profiles are those with jdifflast=jgradlast=0
Acknowledgements: Lorenzo Posti, posti(at)
(End) Patricia Vannier [CDS] 16-Apr-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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