An IDL implementation for Astrometry.net

<p>This IDL program is an implementation to run the Astrometry.net pipeline as part of your other IDL routines. It also adds the possibility to specify a time limit to each file for which an astrometric solution is searched for, which is very handy for the reduction of large data sets.</p> <p>See the file astrometrynet_manual.pdf for detailed informations on how to install the Astrometry.net package (which is not provided where) on your system. A french version of the manual is also available.</p> <p>See the header of astrometrynet.pro for detailed informations on how to use this IDL routine.</p

***Outdated, v1*** An IDL routine to estimate the mass of low-mass stars and brown dwarfs

<p>***This fileset is outdated. Please refer to the last link below for an up-to-date-version***</p> <p>This IDL routine uses the 2MASS and WISE J, H, Ks, W1 and W2 apparent magnitudes and the distance of a given object, along with an estimated age range, to determine its most probable mass range using AMES-COND isochrones (Baraffe et al. (2003) in combination with CIFIST2011 BT-SETTL atmosphere models (Allard et al. 2013, Rajpurohit et al. 2013) in a likelihood analysis. Errors on the distance and photometry, when input, are propagated to the estimated mass range. This routine was used to estimate the masses of candidate members in Table 3 of Gagné et al. (2014).</p> <p>**IMPORTANT NOTE : To be able using this routine, you will have to download the IDL save file named "baraffe_interpol_input.sav" and modify the first line of the "baraffe_interpol.pro" routine to your local path that leads to the file.**</p> <p>See the main file "banyan_mass.pro" for more information on how to use this routine.</p> <p>Please cite Gagné et al. 2014, Baraffe et al. 2003, Allard et al. 2013 and Rajpurohit et al. 2013 (see links) if you use this procedure.</p

Moving Group Candidates Estimated Mass Function

<p>These plots show histograms of the mass estimates of <em>bona fide</em> members and candidates members of all young moving groups including TW Hydrae, Beta Pictoris, Tucana-Horologium, Carina, Columba, Argus and AB Doradus. Green bars are <em>bona fide</em> members, yellow bars represent a log-normal IMF consistent with the current number of <em>bona fide</em> members, red bars are candidate members from Gagné et al. (in prep.), purple bars are candidates members for which youth was confirmed (Gagné et al. in prep. and Gagné et al. 2013, submitted to ApJ). Fuschia bars are candidate members from Malo et al. (2013) and Malo et al. (2014, submitted to ApJ).</p> <p>Masses were estimated by comparing absolute magnitudes computer from Bayesian statistical distance predictions with AMES-COND isochrones (Baraffe et al. 2003) in combination with CIFIST2011 BT-SETTL atmosphere models (Allard et al. 2013, Rajpurohit et al. 2013) in a likelihood analysis (See Gagné et al. 2013, submitted to ApJ for more information).</p> <p>All files are available in PDF and EPS formats.</p> <p>Please cite the article below (see link) if you use these figures.</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

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

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

Posterior probability density functions for NYA memberships of known, young brown dwarfs

<p>These figures show the 2-dimensional posterior probability density functions associated with each hypothesis, as a function of radial velocity and distance for all candidate members presented in Gagné et al. (2014). When measurements are available, they are indicated in red. The probabilities in these figures' legends do *not* take radial velocity and/or distance measurements into account, even when they are available and shown on the plots. Please refer to Gagné et al. (2014) to obtain Bayesian probabilities that take these measurements into account. These figures are similar to Figure 10 in Gagné et al. (2014).</p> <p><br>Please cite Gagné et al. (2014) whenever using these.</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