White Dwarf Cosmochronometry. I. Monte Carlo Simulations of Proper-Motion- and Magnitude-limited Samples Using Schmidt's 1/V max Estimator

Details White Dwarf Cosmochronometry. I. Monte Carlo Simulations of Proper-Motion- and Magnitude-limited Samples Using Schmidt's 1/V max Estimator White Dwarf Cosmochronometry. I. Monte Carlo Simulations of Proper-Motion- and Magnitude-limited Samples Using Schmidt's 1/V max Estimator

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...497..870w&link_type=abstract

Astrophysical Journal v.497, p.870

Statistics

35

Methods: Statistical, Stars: Luminosity Function, Mass Function, Stars: Statistics, Stars: White Dwarfs

Scientific paper

Observationally, white dwarf stars are a remarkably homogeneous class with a minimum observed Teff ~ 4000 K. Theoretically, the physics that determines their cooling timescales is relatively more straightforward than that which determines main-sequence evolutionary timescales. As a result, the white dwarf luminosity function has for the last decade been used as a probe of the age and star formation rate of the Galactic disk, providing an estimated local disk age of ~10 Gyr with estimated total uncertainties of roughly 20%. A long-standing criticism of the technique is that the reality of the reported downturn in the luminosity function (LF) hinges on just a handful of stars and on statistical arguments that fainter (older) objects would have been observed were they present. Indeed, the likely statistical variations of these small-number samples represent one of the primary uncertainties in the derived Galactic age, and the behavior of Schmidt's 1/Vmax estimator in this limit is not well understood. In this work, we explore these uncertainties numerically by means of a Monte Carlo population synthesis code that simulates the kinematics and relative numbers of cooling white dwarfs. The "observationally selected" subsamples are drawn using typical proper motion and V-magnitude limits. The corresponding 1/Vmax LFs are then computed and compared to the input-integrated LFs. The results from our (noise-free) data suggest that (1) Schmidt's 1/Vmax technique is a reliable and well-behaved estimator of the true space density with typical uncertainties of ~50% for 50 point samples and 25% for 200 point samples; (2) the age uncertainties quoted in previously published observational studies of the LF are consistent with uncertainties in the Monte Carlo results--specifically, there is a ~15% and <~10% observational uncertainty in the ages inferred from 50 point and 200 point samples, respectively; and (3) the large statistical variations in the bright end of these LFs--even in the large-N limit--preclude using the white dwarf LF to obtain an estimate of the recent star formation rate as a function of time.

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