A proper motion study of the Lupus clouds using VO tools (a collaboration with the SVO) Francisco Jiménez Esteban (CAB & SVO) Belén López Martí (CAB) & Enrique Solano (CAB & SVO) Gaia: II Reunión Científica de la REG, Santillana del Mar, September 2011

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept The Lupus clouds One of the nearest low-mass star forming regions d= pc age<5 Myr Star-count map by Cambrésy et al. (1999)

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept The Lupus clouds Within or near the Gould Belt x x

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept The Lupus clouds The stellar & substellar population: Most recent results A large increase of the stellar and substellar population (but few spectra so far) Comerón (2008): –Review of previous results. –Lists 74 known members of Lup 1, 2, 3 & 4 Merín et al. (2008): –Spitzer c2d census of 159 PMS stars & candidates in Lup 1, 3 & 4 –Mostly objects with disks and/or envelopes Comerón et al. (2009): –~130 new cool, ~without envelope or disk, very low-mass members in Lup 1, 3 & 4.

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members Sample: Compilation from Comerón (2008), Merín et al. (2008) & Comerón et al. (2009) 331 objects Method: –Multiple Cone Search using TOPCAT –Matching radius: 2 –Astrometric catalogues: USNO-B1, SSS, PPMX and UCAC3 –Purge resulting catalog using UCAC3 information: Errors != 0 Useful observations >3 Final sample: 178 objects Goal: To check membership of proposed Lupus candidate members

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members Two kinematic groups!

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members Lupus 1: The two groups have different spatial distributions and proper motion directions.

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members Lupus 3: The two groups have different spatial distributions and proper motion directions.

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members Lupus 4: The two groups have different proper motion directions.

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members Group B is formed mostly by diskless stars, while Group A contains sources with and without disks. Group B, as a whole, represent a later evolutionary stage than Group A.

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members The Group B sources tend to be brighter and redder than the Group A sources. Their infrared colours are consistent with reddened background giants (but also with reddened late K and early M-type stars).

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Proper motions of Lupus members Comparison with Gould Belt populations ROSAT Gould Belt stars (Wichmann et al. 1997)Upper Scorpius members (Bouy & Martín 2009)

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Properties of Lupus kinematic members Group A sources with and without disks

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Properties of Lupus kinematic members Effective temperature No trend (better precision required)

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Properties of Lupus kinematic members Physical parameters No trend (better precision required)

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept Conclusions We have found two distinct kinematic groups in our compiled catalog of Lupus candidate members. The properties of the Group B sources (lower proper motions, location outside the cloud cores, virtual lack of sources with disks, optical and near-infrared colours) suggest that they are a background population or mixture of populations unrelated to the Lupus clouds. Group A sources have properties consistent with them being a genuine population of the Lupus clouds. Their proper motions are also consistent with those of other Gould Belt populations. We find no correlations between the proper motions and the properties of the Group A sources. More accurate measurements are required (Gaia).

Gaia: II Reunión Científica de la REG, Santillana del Mar, Sept More details in López Martí et al., 2011, A&A, 529, A108 More details in López Martí et al., 2011, A&A, 529, A108