Spatial distribution and galactic model parameters of cataclysmic variables

TL;DR

This study analyzes the spatial distribution, galactic parameters, and luminosity function of 459 cataclysmic variables in the solar neighborhood, revealing their vertical distribution, scaleheight, and local space density, with implications for theoretical models.

Contribution

It provides the first comprehensive analysis of CVs' spatial distribution and galactic parameters using a calibrated sample and compares different density functions for better modeling.

Findings

Exponential fits best for z-distributions of all CVs and subtypes.

Scaleheight of CVs is approximately 158 pc.

Local space density of CVs is about 3×10^{-5} pc^{-3}.

Abstract

The spatial distribution, galactic model parameters and luminosity function of cataclysmic variables (CVs) in the solar neighbourhood have been determined from a carefully established sample of 459 CVs. The sample contains all of the CVs with distances computed from the Period-Luminosity-Colours (PLCs) relation of CVs which has been recently derived and calibrated with {\em 2MASS} photometric data. It has been found that an exponential function fits best to the observational z-distributions of all of the CVs in the sample, non-magnetic CVs and dwarf novae, while the sech^{2} function is more appropriate for nova-like stars and polars. The vertical scaleheight of CVs is 158$\pm$14 pc for the {\em 2MASS} J-band limiting apparent magnitude of 15.8. On the other hand, the vertical scaleheights are 128$\pm$20 and 160$\pm$5 pc for dwarf novae and nova-like stars, respectively. The local space density of CVs is found to be $\sim3\times10^{-5}$ pc^{-3} which is in agreement with the lower limit of the theoretical predictions. The luminosity function of CVs shows an increasing trend toward higher space densities at low luminosities, implying that the number of short-period systems should be high. The discrepancies between the theoretical and observational population studies of CVs will almost disappear if for the z-dependence of the space density the sech^{2} density function is used.