The Galactic disk mass-budget : I. stellar mass-function and density

By G. Chabrier. 2001

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In this paper, we use the general theory worked out within the past few years for the structure and the evolution of low-mass stars to derive the stellar mass-function in the Galactic disk down to the vicinity of the hydrogen-burning limit, from the observed nearby luminosity functions. The accuracy of the mass-magnitude relationships derived from the afore-mentioned theory is examined by comparison with recent, accurate observational relationships in the M-dwarf domain. The mass function is shown to flatten out below $\sim 1 \msol$ but to keep rising down to the bottom of the main sequence. Combining the present determination below 1 $\msol$ and Scalo's (1986) mass function for larger masses, we show that the mass function is well described over the entire stellar mass range, from $\sim 100 \msol$ to $\sim 0.1 \msol$, by three functional forms, namely a two-segment power-law, a log-normal form or an exponential form, all normalized to the Hipparcos sample at 0.8 $\msol$. Integration of this mass function yields a reasonably accurate census of the entire stellar population in the Galactic disk, and its volume and surface mass-density.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

View Paper: https://www.semanticscholar.org/paper/765da328ca717298b5b1b52b36e96804095cdf00

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Citations in the corpus

The stellar and sub-stellar IMF of simple and composite populations (2011, neutral): “…(1998) ξL(lm) = Am −1.35exp [ − mo m ] Γ(lm) = −1.35 + mo m La thin short-dashed line A = − ; mo = 0.3M⊙ Larson (1998) ξL(lm) = A [ 1 + m mo ]−1.35 Γ(lm) = −1.35 ( 1 + mo m )−1 Lb thin long-dashed line A = − ; mo = 1M⊙ Chabrier (2001, 2002) ξ(m) = Am−δ exp [ − ( mo m )β ] Γ(lm) = 1− δ + β (…”
Imaging Extrasolar Giant Planets (2016, positive): “The most widely used hot-start models for imaged planets are the Cond and Dusty grids from Baraffe et al. (2003) and Chabrier (2001), Burrows et al. (1997), and Saumon & Marley (2008).”
The SILCC (SImulating the LifeCycle of molecular Clouds) project – I. Chemical evolution of the supernova-driven ISM (2014, methodology): “We typically use Minj = 800 M for single SNe, which roughly corresponds to a star formation efficiency of ∼8 per cent for a Chabrier initial stellar mass function (IMF; Chabrier 2001).”
Stellar Populations in the Nuclei of Late-Type Spiral Galaxies (2006, methodology): “BC03 adopted the Chabrier IMF because it is physically motivated and provides a better fit to counts of low-mass stars and brown dwarfs in the Galactic disc (Chabrier 2001, 2002, 2003a).”
Chemodynamics of the Milky Way - I. The first year of APOGEE data (2013, background): “As priors on x we assume a Chabrier-type initial mass function p(M) (Chabrier 2001), and assume different density and metallicity distributions as well as star-formation histories (SFH) for the Galactic components Bulge, Thin Disc, Thick Disc and Halo, following Burnett et al. (2011).”
Stellar population synthesis at the resolution of 2003 (2003, methodology): “Here we adopt the Chabrier (2003b) IMF because it is physically motivated and provides a better fit to counts of low-mass stars and brown dwarfs in the Galactic disc (Chabrier 2001, 2002, 2003a).”
The Evolution of L and T Dwarfs in Color-Magnitude Diagrams (2008, background): “While the observational evidence is consistent with a roughly flat SFR over the age of the Galaxy (Allen et al. 2005), we consider an exponentially decreasing SFRwith a characteristic timescale of ¼ 5 Gyr (Miller & Scalo 1979).”
CONFIRMATION OF FAINT DWARF GALAXIES IN THE M81 GROUP (2013, methodology): “From the web interface form, we chose bolometric corrections from Loidl et al. (2001), New Dwarf Galaxies in M81 9 circumstellar dust calculations as in Groenewegen (2006), and a Chabrier lognormal IMF (Chabrier 2001).”
The age–metallicity structure of the Milky Way disc using APOGEE (2017, methodology): “These values are found using PARSEC isochrones (Bressan et al. 2012), weighted with a Log-normal Chabrier (2001) IMF, as described in the calculation of the effective volume in Section 3.1.”
EIGHT ULTRA-FAINT GALAXY CANDIDATES DISCOVERED IN YEAR TWO OF THE DARK ENERGY SURVEY (2015, methodology): “We then created a grid of possible simple stellar populations modeled with the isochrones of Bressan et al. (2012) and populated according to a Chabrier (2001) initial mass function to use as signal templates.”
The effects of fly‐bys on planetary systems (2010, methodology): “We use the lognormal IMF of Chabrier (2001, 2002) to extend the stellar population in our reference cluster down to one Jupiter-mass objects.”
On the mass-to-light ratio of the local Galactic disc and the optical luminosity of the Galaxy (2006, result): “Our (SC) values are instead in very good agreement with the predictions for the Kroupa (1998) and Chabrier (2001) IMFs, which were derived from solar neighbourhood studies – a successful consistency check.”
Is molecular gas necessary for star formation (2011, background): “The mean stellar mass that we obtain from these simulations is slightly higher than the characteristic mass in the observationallydetermined IMF, which is typically found to be somewhat c© 0000 RAS, MNRAS 000, 000–000 less than a solar mass (Chabrier 2001; Kroupa 2002).”
New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies (2014, background): “In particular, the IMF is assumed to be represented by a log-normal function (Chabrier 2001) for all the components.”
Atmospheric circulations of terrestrial planets orbiting low-mass stars (2011, background): “The initial mass function is lognormal from Chabrier (2001).”
The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs (2020, methodology): “…laws (dN/dM ∝ M−α) with α values ranging from −1.0 to 1.5, the log-normal distribution (dN/dM ∝ e−(ln(M)−µ)2/2σ2 ) with values of the mean (µ) and standard deviation (σ) taken from Chabrier (2001), Chabrier (2003a), and Chabrier (2003b), and a bi-partite power law favored by Kroupa et al. (2013).”
Fitting the integrated spectral energy distributions of galaxies (2010, methodology): “Three empirical forms are most commonly used: a simple power-law model (Salpeter 1955; Massey 1998), a broken power-law (Kroupa 2001), or a lognormal form (Chabrier 2001).”
Brown dwarfs in the Pleiades cluster: Clues to the substellar mass function , (2002, methodology): “While the Pleiades mass function derived above includes unresolved cluster binaries, the Galactic disk mass function has been derived for the single star population (i.e. all binaries are resolved, cf. Chabrier 2001).”
THE PALOMAR/KECK ADAPTIVE OPTICS SURVEY OF YOUNG SOLAR ANALOGS: EVIDENCE FOR A UNIVERSAL COMPANION MASS FUNCTION (2008, background): “0.6; Chabrier 2001; Kroupa 2002; Allen et al. 2005) and in young stellar associations (−1 . α .”
Testing LMC Microlensing Scenarios: The Discrimination Power of the SuperMACHO Microlensing Survey (2005, background): “This break in power-law is well known and documented for the solar neighborhood (Kroupa et al. 1993; Reid & Hawley 2000; Chabrier 2001), and it is also seen in the LMC (Holtzman et al. 1997; Hunter et al. 1997; Olsen 1999; Alcock et al. 2001b).”