Nearby, Young Moving Groups : Spatial and Kinematic Models

<p>Here we show the Spatial and Kinematic Models that were used to represent nearby, young moving groups in the spatial <em>XYZ </em>and dynamical<em> UVW </em>parameter spaces<em>.</em> The distribution of <em>bona fide</em> members in each parameter space are represented with gaussian ellipsoids that are free to rotate along any axes. Red dots are members, the blue dot is the Sun, the 3D orange ellipsoid and its three projections are the 1.5-sigma contour of the kinematic model, green lines and pale blue dots are projections of the positions of members (red dots).</p> <p>Please cite Gagné et al. 2014 when using this data product (see link).</p

J - Ks vs W1 Color-Magnitude Diagrams for Gagné et al. 2014 candidates

<p>These figures compare the position of each candidate member (red) of nearby, young moving groups in Gagné et al. (2014) to the color-magnitude sequences in Figure 3 (left) in the same reference, as well as new candidate members in Gagné et al. (in prep.) (black dots, purple dots for those whose youth is confirmed). See also Joe Filippazzo's BDNYC post on the photometric properties of young stars. The statistical distance predictions from BANYAN II were used when a parallax measurement was unavailable. An empty circle means that the magnitude has been corrected for binarity, and an upside-down triangle means that a parallax measurement was used.</p> <p>Please cite Gagné et al. 2014 and 2013 (see links) if you use these figures.</p

Expected UVW positions for moving group candidate members in Gagné et al. 2014

<p>These figures show the expected 3-dimensional UVW positions of candidate members to nearby, young moving groups (red points ; blue lines point to their projections on the 3 planes) in Gagné et al. (2014), compared to the UVW positions of bona fide members (green points ; their projections are also shown on the 3 planes, and only vertical lines pointing to their UV-plane projections are shown for clarity). The orange ellipsoid and its projections on the 3 planes represent the 1.5-sigma contour of the kinematic model of the moving group in question. The statistical distance and radial velocity predictions from BANYAN II were used to compute the UVW of candidate members when such measurements were unavailable. Only measurements of distance and radial velocity were used in the case of bona fide members.</p> <p>See also the other fileset (link below) for spatial XYZ versions of these figures.</p> <p>If you use any of these figures, please cite Gagné et al. (2014; see link below).</p

List of bona fide members of nearby, young moving groups

<p>This is a list of bona fide members to nearby, young associations, along with kinematic, 2MASS and WISE information.</p> <p>Please cite Gagné et al. 2014 (see link) when using these tables.</p> <p>Edit August 23, 2014 : I added a small IDL package to read the .csv tables into an IDL structure (read_csv_gagne2014_IDL_package.zip). Feel free to use it with this package. The syntax to use this routine would look like this :</p> <p>IDL> struc = read_csv_gagne2014('/Somepath/Argus__Argus.csv')</p> <p>And then you can view the structure content of the bonafide member #i with :</p> <p>IDL> help,struc[i]</p> <p>Or, for example, view all spectral types with :</p> <p>IDL> print,struc.spt</p

Electronic version of Gagné et al. 2014 Table 4

<p>This table is an electronic version of Table 4 in Gagné et al. (2014), listing the bayesian probabilities that known, young or red > M5 objects belong to each moving group considered.</p> <p>Please refer to this paper when using it (see link).</p

H - W2 vs W1 Color-Magnitude Diagrams for Gagné et al. 2014 candidates

<p>These figures compare the position of each candidate member (red) of nearby, young moving groups in Gagné et al. (2014) to the color-magnitude sequences in Figure 3 (right) in the same reference, as well as new candidate members in Gagné et al. (in prep.) (black dots, purple dots for those whose youth is confirmed). See also Joe Filippazzo's BDNYC post on the photometric properties of young stars. The statistical distance predictions from BANYAN II were used when a parallax measurement was unavailable. An empty circle means that the magnitude has been corrected for binarity, and an upside-down triangle means that a parallax measurement was used.</p> <p>Please cite Gagné et al. 2014 and 2013 (see links) if you use these figures.</p

SPIROU workshop talk 2011 : Searching for young low-mass stars in the solar neighborhood with SPIRou

<p>We present how SPIROU can be used to search for and characterize low-mass star members to nearby, young moving groups.</p

Electronic version of Gagné et al. 2014 Table 5

<p>This table is an electronic version of Table 5 in Gagné et al. (2014), describing the statistical predictions for radial velocity and distance of known, young or red > M5 objects depending on the moving group they belong to.</p> <p>Please refer to this paper when using it (see link).</p

Known, Young > M5 Dwarfs

<p>This file contains a list of all known low-mass stars and brown dwarfs with spectral types later than M5, assumed as belonging to the field prior to Gagné et al. 2014. The purpose of this list was to confirm or search for new candidate members in nearby, young moving groups (See Gagné et al. 2014, accepted for publication in the ApJ).</p

Moving Groups Parameters

<p>This idl savefile contains the parameters of all spatial and Kinematic models of nearby, young associations of Gagné et al. 2014. You can acess them with the following command in IDL :</p> <p>IDL> restore, 'mg_parameters_Gagne2014.sav', /verbose & help, params_all, /str</p> <p>Please cite Gagné et al. 2014 when you use this dataset.</p