J1207-3900. Material.

J1207-3900 : Additional Material

2MASS_JHK_J1207-3900_marker2

2MASS Color Mosaic for 2MASS J1207-3900

This page contains additional material for the Gagné et al. (2014b) paper 2014ApJ…785L..14G : The Coolest Isolated Brown Dwarf Candidate Member of TWA. All data is hosted on Figshare so that they get their own DOI if you wish to refer to a particular table or figure set. We ask that you always at least refer to 2014ApJ…785L..14G when using this material.

1) Additional figures.

1.1) Proper motion for J1207-3900 and J1247-3816 compared to TWA members.

This figure shows map of the position and proper motion of bona fide members to TW Hydrae (green arrows; Malo et al. 2013), compared to those of J1247-3816 and J1207-3900 (red arrows). Each star’s proper motion vector is prolongated into a great circle on the celestial sphere, to show that they converge in two points (the apex and anti-apex, blue circles are 1-sigma and 3-sigma apex calculated from the XYZUVW models; See Gagné et al. 2014a), which are often close to the Solar’s apex and anti-apex (black cross and plus signs). Thanks to Adric Riedel for help in the construction of these figures. DOI & Figshare link

1.2) XYZ and UVW statistical predictions for J1207-3900 and J1247-3816 compared to TWA members.

These figures show the expected 3-dimensional XYZ and UVW positions of J1207-3900 and J1247-3812 (see Gagné et al. 2014b; red points; blue lines point to their projections on the 3 planes), compared to the XYZ positions of bona fide members from Malo et al. 2013 (green points; their projections are also shown on the 3 planes, and only vertical lines pointing to their XY-or 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 spatial model of the moving group in question. The statistical distance predictions from BANYAN II (see Gagné et al. 2014a) for RVs and distances were used to compute the XYZ or UVW of the two TWA candidates. Measurements of distance and RVs were used in the case of bona fide members. DOI & Figshare link

1.3) J1207-3900 and J1247-3816 compared to the BASS sample in 2MASS/WISE CMDs.

These figures show the positions of J1207 and J1247 (red star symbols) in 2MASS/WISE color-magnitude diagrams, compared to the field sequence (black line), its scatter (gray region) and all candidate members to young moving groups from the BASS sample (black dots or purple dots when youth is confirmed; see Gagné et al. 2013). DOI & Figshare link 

1.4) 2D Probability density functions vs RV and distance for J1207-3900 and J1247-3816.

These figures show the 2-dimensional posterior probability density functions associated with each hypothesis, as a function of radial velocity and distance for J1207-3900 and J1247-3816 (see Gagné et al. 2014b). Please refer to Gagné et al. (2014a) for more details on these types of figures, which are output from BANYAN II. DOI & Figshare link

1.5) Comparison of the absolute J magnitude of J1207-3900 with young and field brown dwarfs.

This figure shows the expected position of J1207-3900 (Gagné et al. 2014b) in a spectral type-absolute magnitude diagram (from Liu et al. 2013), using the statistical distance prediction from BANYAN II (Gagné et al. 2014a). It can be seen that J1207-3900 is expected to be neither over- or under- luminous as compared to old, field L dwarfs. This is consistent with other young L1 dwarfs, which are inflated, but more dusty ; the two effects cancel out on their total luminosity. However, due to enhanced dust it has redder than normal NIR colors (see Gagné e tal. 2014b). DOI & Figshare link 

1.6) Comparison of NIR spectra of J1207-3900 and J1247-3816 with young and field brown dwarfs.

These figures compare J1207-3900 and J1247-3816 to various old and young spectroscopic templates. DOI & Figshare link

1.7) Comparison of NIR spectra of J1207-3900 and J1247-3816 with TWA candidates and members.

This figure shows the complete near-infrared spectra of J1207-3900 and J1247-3816 (see Gagné et al. 2014b), compared to other TW Hydrae candidates and members. DOI & Figshare link

1.8) J1207-3900 and J1247-3816 and BASS candidates in a CMD diagram.

This figure is an analog of Figure 4 in Gagné et al. (2014b; see first link below), but adding also all TWA candidates in the BASS survey (see Gagné et al. 2013; second link below). DOI & Figshare link

1.9) Signs of low-gravity in the optical spectrum of J1207-3900.

This figure shows the spectral indices of J1207-3900 (purple stars) as compared to the sequences defined in Cruz et al. 2009. It can be seen that the optical spectrum of J1207-3900 is consistent with it being a young, low-gravity object. DOI & Figshare link 

1.10) 2MASS Color Mosaic for J1207-3900 and J1247-3816.

For your own fun (or can be used as Finder Charts). DOI & Figshare link

2) Additional data.

2.1) All spectra in Gagné et al. 2014b.

Download them at the Montreal Spectral Library !

2.2) All spectral indices for J1207-3900 and J1247-3816.

These IDL save files each contain a structure, grouping all spectral indices from several bibliographical references. There is one IDL savefile per spectrum. You can find all spectra in the Montreal Spectral Library. The data can be restored into IDL with the following example command : IDL> restore, ‘J1247-3816_SpeX_LowRes15_spectral_indices.sav’, /verbose It is also possible to restore IDL save files in Python. DOI & Figshare link 

3) IDL Routines.

3.1) The IDL procedure that was used to build Figure 1.

This IDL function shows how Figure 1 was built in Gagné et al. (2014b). IDL 8 or over is required for this routine to work. We do not provide subroutines « read_spectrum_sep.pro » and « read_template_sep.pro » as those only serve for reading the spectra that are displayed. They restore into memory the lam, sp and esp variables, which are each a 3-pointer array containing the data for the J, H and K bands respectively. This routine is given with the sole purpose of learning how to use the IDL 8 graphic functions to create plots similar as that of Figure 1 in Gagné et al. 2014. This is why we do not give the subroutines. DOI & Figshare link

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