Spectroscopy of very low mass stars and brown dwarfs in the Lambda Orionis star forming region - I. Enlarging the census down to the planetary mass domain in Collinder 69

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Table 5

Fitted slopes for the IMF of Collinder 69 taking into account the different methods to estimate the mass of the confirmed members (see text for further details).

Estimated α for
the mass range:	25–0.65 M_⊙		0.65–0.01 M_⊙

C69 IMF (I)	1.73		0.18
C69 IMF (II)	1.81		0.38
C69 IMF (III)	1.88		0.31
C69 IMF (IV)	1.79		0.16
C69 IMF (V)	1.85		0.38
C69 IMF (VI)	1.85		0.33

SOri¹		0.8
APer²³		0.6
M 35⁴		(0.81)–(–0.88)
Pleiades⁵		0.6

Notes. We also include the slopes estimated for low mass stars (the mass ranges are not always the same ones but roughly M_∗ < 0.8 M_⊙) in other studies of different open clusters. Slope estimated with data from:

⁽¹⁾

Béjar et al. (2001);

⁽²⁾

Barrado y Navascués et al. (2001a);

⁽³⁾

Barrado y Navascués et al. (2002);

⁽⁴⁾

Barrado y Navascués et al. (2001b);

⁽⁵⁾

Bouvier et al. (1998).

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