1. Distinguishing Brownies from Fudge: The Low-Mass IMF the Companion Mass Ratio Distribution
Michael R. Meyer
Institute for Astronomy, ETH-Zurich
Morten Andersen, Julia Greissl, and Alan Aversa
Steward Observatory, The University of Arizona
Formation of Brown Dwarfs: ESA-CONSTELLATION Workshop
ESTEC, The Netherlands, 9-11 September, 2009

2. No local variations in stellar IMF (e.g. Meyer et al. 2000).
See also Lada & Lada (2003).

3. What about the sub-stellar IMF ? cf. Luhman et al. PPV (2007)
See also Muench et al. (2002).

4. Low Mass Stars and Sub-stellar Objects in NGC 1333
Wilking, Meyer, Greene, Mihail, & Carson (2004)

5. Near-IR Spectra of Low Mass Stars and Sub-stellar Objects
Greissl, Meyer, Wilking, Fanetti, Greene, Scheider, Young (2007)

6. H-R Diagrams for Sub-stellar Objects in NGC 1333*
Greissl, Meyer, Wilking, Fanetti, Greene, Schneider, Young (2007)

7. NICMOS Color-Magnitude Diagram for NGC 1333
Greissl, Meyer, Wilking, Fanetti, Greene, Scheider, Young (2007)

8. Ratio of Stars to Sub-stellar Objects for 7 Young Clusters
Andersen et al. (2008)

9. Ratio of Stars to Sub-stellar Objects for 7 Young Clusters
Andersen et al. (2008)

10. Replacing the K-S Statistic: Binomial Tail Product?
Andersen et al. (2008)

11. Replacing the K-S Statistic: Binomial Tail Product?
Andersen et al. (2008)

12. Replacing the K-S Statistic: Binomial Tail Product?
Andersen et al. (2008)

13. Probability of Various B-T-P for 7 Young Clusters:
Bottom Line - Flat or Rising IMF Ruled Out (P < 0.01 %).
Median BTP: 0.57 = 7.8 x 10-3
Andersen et al. (2008)

14. Probability of Various B-T-P for 7 Young Clusters:
Bottom Line - Flat or Rising IMF Ruled Out (P < 0.01 %).
Cf. Mean Mass of log-normal Msun? Covey et al. (2008)

15. The Companion Mass Ratio Distribution (Duquennoy & Mayor, 1991)
Frequency
Separation (AU)
Mc/Mp
Cf. Lada (2006); Burgasser et al. (2007); Metchev et al. (2009); Apai et al. (in prep)

16. The Companion Mass Ratio Distribution (Duquennoy & Mayor, 1991)
Frequency
Separation (AU)
Mc/Mp
Cf. Lada (2006); Burgasser et al. (2007); Metchev et al. (2009); Apai et al. (in prep)

17. The Companion Mass Ratio Distribution (Duquennoy & Mayor, 1991)
Frequency
Separation (AU)
Mc/Mp
Cf. Lada (2006); Burgasser et al. (2007); Metchev et al. (2009); Apai et al. (in prep)

18. The Companion Mass Ratio Distribution (cf. Chabrier 2005)
Frequency
Primary Mass
Mc/Mp
Cf. Lada (2006); Burgasser et al. (2007); Metchev et al. (2009); Apai et al. (in prep)

19. The Companion Mass Ratio Distribution (cf. Chabrier, 2005)
Frequency
Mc/Mp
Cf. Lada (2006); Burgasser et al. (2007); Metchev et al. (2009); Apai et al. (in prep)

20. The Companion Mass Ratio Distribution (cf. Chabrier, 2005)
Frequency
Mc/Mp
Cf. Lada (2006); Burgasser et al. (2007); Metchev et al. (2009); Apai et al. (in prep)

21. Executive Summary
The IMF turns over at low masses: there are fewer brown dwarfs compared to stars (Andersen et al. 2008).
Determining the companion mass ratio distribution (vs. primary star mass/separation) down to Jupiter masses could discern differences between brown dwarfs and planets (Apai et al. in preparation).

22. The Search for Variations: A Six-Parameter IMF
1. Mean Mass
5. Sub-stellar Break
log[N*]
3. High Mass Break
2. Variance
6. Sub-stellar Slope
4. High Mass Slope
log[M*/Mo]