The NIRSPEC Brown Dwarf Spectroscopic Survey (BDSS)

Paper I: McLean, I.S., McGovern, M.R., Burgasser, A.J., Kirkpatrick, J.D., Prato, L., & Kim, S.S. 2003, ApJ, 596, 561

Paper II: McLean, I.S., Prato, L., McGovern, M.R., Burgasser, A.J., Kirkpatrick, J.D., Rice, E.L., & Kim, S.S. 2007, ApJ, 658, 1217

Please cite one or both of the above references if you use or display these data in your publications or presentations.

Data Archive

Announcements

Poster presented at 209th AAS Meeting
JPEG

UCLA Press Release, 3 September 2003
PDF

Introduction to the BDSS
MS PowerPoint  HTML export

NIRSPEC

NIRSPEC positioned at the KECK II Nasymth platform

Introduction - BDSS

The Brown Dwarf Spectroscopic Survey (BDSS), established in 1998 by Dr. Ian McLean in collaboration with Dr. J. Davy Kirkpatrick at IPAC, is designed to study near-infrared moderate-to-high resolution spectra for a large sample of low-mass stars and sub-stellar mass objects in the M and newly defined L and T dwarf classes. The BDSS was initiated following the successful first light commissioning of the Keck-II Near-Infrared Spectrometer (NIRSPEC) in April 1999. The goals of the BDSS are:

  1. obtain a uniform set of moderate resolution (R~ 2,000) NIR spectra for a large sample of very low-mass stars and brown dwarfs to examine general spectral properties and facilitate comparisons with theoretical spectral energy distributions;
  2. obtain a set of high resolution spectra (R~20,000) for detailed comparison of individual spectral features with model atmospheres; and
  3. monitor selected sources for Doppler shifts induced by unresolved binary companions.

For a description of NIRSPEC see:

McLean, I.S., et al. 1998, Proc. SPIE, 3354, 566 (PDF)
McLean, I.S., et al. 2000, Proc. SPIE, 4008, 1048 (PDF)

Description of Low-Resolution Data Products

Filter Configurations All data products were obtained with NIRSPEC in its low resolution (R~2000) mode with the 42x0.38 arcsecond (2 pixel) slit in place. Six filters (NIRSPEC-1 through NIRSPEC-6) give overlapping wavelength coverage from 0.96 - 2.31 microns. The table on the right lists the seven instrumental configurations we have used and their effective wavelength range of importance to the survey. Note: The NIRSPEC-6 is a broad H+K filter centered at 1.925 microns with a bandwidth of 0.75 microns. Since the entire NIRSPEC-6 bandwidth cannot be simultaneously observed on the detector, two configurations, N6a and N6b, are used to obtain the long wavelength half of the H-band and the K-band, respectively. NIRSPEC-5 (essentially H-band) was used only for one observation of the T8 dwarf 2MASS 0415-09.

The table below lists the sample of low mass stars and brown dwarfs included in our survey. The observing strategy for these objects was to obtain a 300s exposure with the source at each of two positions separated by ~20" along the 0.38" slit. Most objects were observed in an ABBA pattern giving total integration time of 20 minutes per grating/filter configuration. For fainter objects (J~16) this procedure was repeated to maintain a signal-to-noise ratio of at least 20:1 per resolution element over the majority of the spectral region observed. Reduction of the spectra was accomplished using REDSPEC, software designed and developed primarily for NIRSPEC data reduction. Data from filters NIRSPEC-3 through NIRSPEC-6 were combined to create a 1.14-2.31 micron composite spectrum. In some cases the shorter wavelength end was extended out to 0.96 microns with the inclusion of data from the NIRSPEC-1 & 2 filters. Composite spectra were flux calibrated (in Flambda units) using 2MASS photometry, following the prescription of McLean et al. (2001). See paper for details concerning the observing strategy and data reduction process.

Data products can be downloaded individually from the table of objects given below or in groups found the next section. Individual data files contain six lines of introductory text followed by two columns of wavelength (microns) in the first and normalized flambda in the second. Composite spectra follow the same prescription except the second column is replaced by flux calibrated data (W m^-2 um^-1) using 2MASS photometry.

Description of High-Resolution Data Products

NIRSPEC-3 Echelle Configurations All high-resolution data products were obtained with NIRSPEC in its high-resolution (R~20,000) mode with the 12 arcsecond by 0.432 arcsecond (3 pixel) slit in place except in the case of 2MASS 1507-16, for which the 0.576 arcsecond slit (4 pixels) was used because of poor seeing. The NIRSPEC-3 filter, approximating standard J-band coverage, was used for all observations. The table on the left lists the effective wavelength coverage of each echelle order for the given instrument settings.

The table below lists the sample of low mass stars and brown dwarfs included in our high-resolution survey. The observing strategy for these objects was to obtain a 300-second or 600-second exposure (40 seconds by 3 coadds for Wolf 359 and 360 seconds for 2MASS 0746+20) with the source at each of two positions separated by seven arcseconds along the 12-arcsecond-long slit. Most objects were observed in an ABBA pattern giving total integration time of 20-40 minutes. For fainter objects (J~16) this procedure was repeated to maintain a signal-to-noise ratio of at least 20:1 per resolution element over the majority of the spectral region observed. Reduction of the spectra was accomplished using REDSPEC, software designed and developed primarily for NIRSPEC data reduction. See paper for details concerning the observing strategy and data reduction process.

Data products can be downloaded individually from the table of objects given below or in groups found the next section. Individual data files contain six lines of introductory text followed by two columns of wavelength (microns) in the first and flux (normalized within each order) in the second.

Download Data Products

Download entire BDSS low-resolution archive: Gzip Archive , WinZip
Groups - Filter Sets
Download entire N1 filter data set: Gzip Archive , WinZip
Download entire N2 filter data set: Gzip Archive , WinZip
Download entire N3 filter data set: Gzip Archive , WinZip
Download entire N4 filter data set: Gzip Archive , WinZip
Download entire N6a filter data set: Gzip Archive , WinZip
Download entire N6b filter data set: Gzip Archive , WinZip
Download entire flux calibrated composite data:
Download flux calibrated JHKs <1.140-2.315 um> data set: Gzip Archive , WinZip
Download flux calibrated zJHKs <0.960-2.315 um> data set: Gzip Archive , WinZip
Download all flux calibrated composite data: Gzip Archive , WinZip
Download entire BDSS high-resolution archive: Gzip Archive , WinZip
Groups - Echelle Orders
Download entire order 58 data set: Gzip Archive , WinZip
Download entire order 59 data set: Gzip Archive , WinZip
Download entire order 60 data set: Gzip Archive , WinZip
Download entire order 61 data set: Gzip Archive , WinZip
Download entire order 62 data set: Gzip Archive , WinZip
Download entire order 63 data set: Gzip Archive , WinZip
Download entire order 64 data set: Gzip Archive , WinZip
Download entire order 65 data set: Gzip Archive , WinZip

Low-Resolution Data Products

 D  -- Link to individual ascii data file (flux vs. wavelength).
 P  -- Link to individual postscript plot of data.
Type Object Name   RA (2000)    Dec (2000)  J H Ks Coverage    N1       N2       N3       N4       N6a       N6b    Composite
M6 Wolf 359 (Gl 406) 10 56 28.9 07 00 53 7.09 6.48 6.08 N1,2,3,4,6a,6b D P D P D P D P D P D P D P
M6 Gl 283B 07 40 20.6 -17 24 48 12.65 12.61 12.58 N3 D P DP
M7 LHS 2351 11 06 19.0 04 28 33 12.33 11.72 11.33 N3 D P DP
M7 VB 8 (LHS 429) 16 55 35.3 -08 23 40 9.78 9.20 8.82 N3 D P DP
M8 LP 412-31 03 20 59.7 18 54 23 11.76 11.07 10.64 N3 D P DP
M8 VB 10 (LHS 474) 19 16 57.6 05 09 02 9.91 9.23 8.77 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
M9 LHS 2065 08 53 36.2 -03 29 32 11.21 10.47 9.94 N3,4,6a,6b D P D P D P D P DP
M9 2MASS 1239+20 12 39 19.3 20 29 52 14.45 13.68 13.20 N3 D P DP
L0 2MASS 0345+25 03 45 43.2 25 40 23  13.99   13.17   12.67  N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L0 HD 89744B 10 22 14.9 41 14 27 14.89 14.04 13.62   N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L0.5 2MASS 0746+20AB     07 46 42.6 20 00 32 11.74 11.00 10.49 N3 D P DP
L1 2MASS 1300+19 13 00 42.6 19 12 35 12.71 12.07 11.61 N3 D P DP
L1 2MASS 0208+25 02 08 18.3 25 42 53 14.02 13.11 12.58 N3 D P DP
L1 2MASS 1439+19 14 39 28.4 19 29 15 12.76 12.05 11.58 N3 D P DP
L1 2MASS 1658+70 16 58 03.8 70 27 02 13.29 12.49 11.93 N3,4,6a,6b D P D P D P D P DP
L1 2MASS 2130-08 21 30 44.6 -08 45 20 14.14 13.33 12.82 N3 D P DP
L1 2MASS 1035+25 10 35 24.6 25 07 45 14.70 13.88 13.28 N3,4,6a,6b D P D P D P D P DP
L2 Kelu-1 13 05 40.2 -25 41 06 13.42 12.39 11.73 N3,4,6a,6b D P D P D P D P DP
L2 2MASS 0015+35 00 15 44.8 35 16 03 13.82 12.81 12.24 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L2 2MASS 1726+15 17 26 00.1 15 38 19 15.65 14.46 13.64 N3 D P DP
L3 2MASS 1506+13 15 06 54.4 13 21 06 13.41 12.41 11.75 N3 D P DP
L3 2MASS 1615+35 16 15 44.2 35 59 01 14.55 13.55 12.89 N3 D P DP
L3.5 2MASS 0036+18 00 36 16.2 18 21 10 12.44 11.58 11.03 N3 D P DP
L4 GD 165B 14 24 39.1 09 17 10 15.55 14.55 14.06 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L4 2MASS 2158-15 21 58 04.6 -15 50 10 15.04 13.87 13.19 N3 D P DP
L5 2MASS 1507-16 15 07 47.7 -16 27 39 12.82 11.90 11.30 N3,4,6a,6b D P D P D P D P DP
L5 DENIS 1228-15AB 12 28 15.2 -15 47 34 14.38 13.36 12.81 N3 D P DP
L6 2MASS 0103+19 01 03 32.0 19 35 36 16.26 14.88 14.15 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L6 2MASS 0850+10AB 08 50 35.9 10 57 16 16.46 15.23 14.46 N3 D P DP
L6.5 2MASS 2244+20 22 44 31.7 20 43 43 16.41 14.97 13.93 N3,4,6a,6b D P D P D P D P DP
L7 DENIS 0205-11AB 02 05 29.4 -11 59 30 14.58 13.59 12.98 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L7 2MASS 1728+39AB 17 28 11.5 39 48 59 15.96 14.78 13.90 N3 D P DP
L8 Gl 337C 09 12 14.7 14 59 40 15.55 14.66 14.03 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L8 2MASS 1632+19 16 32 29.1 19 04 41 15.86 14.59 13.98 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
L8 Gl 584C 15 23 22.6 30 14 56 16.32 15.00 14.24 N3,4,6a,6b D P D P D P D P DP
L8 2MASS 0310+16 03 10 59.9 16 48 16 16.43 14.95 14.40 N3 D P DP
L8 2MASS 0328+23 03 28 42.7 23 02 05 16.67 15.62 14.84 N3 D P DP
T0 SDSS 0423-04 04 23 48.6 -04 14 04 14.45 13.44 12.94 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
T1 SDSS 0837-00 08 37 17.2 -00 00 18 16.77 >15.8 >15.3 N3,4,6a,6b D P D P D P D P DP
T1 SDSS 0151+12 01 51 41.7 12 44 30 16.52 15.58 15.09 N3 D P DP
T2 SDSS 1254-01 12 54 53.9 -01 22 47 14.88 14.04 13.83 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
T3 SDSS 1021-03 10 21 09.7 -03 04 20 16.26 15.33 15.10 N3 D P DP
T3.5 SDSS 1750+17 17 50 33.0 17 59 04 16.58 15.97 >16.0 N3 D P DP
T4.5 SDSS 0926+58 09 26 15.4 58 47 21 15.72 15.33 15.44 N3 D P DP
T5 2MASS 2254+31 22 54 18.8 31 23 49 15.28 15.04 14.83 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
T5 2MASS 0559-14 05 59 19.1 -14 04 48 13.83 13.68 13.61 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
T6 2MASS 2356-15 23 56 54.7 -15 53 11 15.80 15.64 15.83 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
T6 SDSS 1624+00 16 24 14.4 00 29 15 15.49 15.52 >15.4 N3 D P DP
T6.5 2MASS 1237+65 12 37 39.2 65 26 15 16.03 15.72 >15.9 N3 D P DP
T7 2MASS 1553+15 15 53 02.2 15 32 36 15.81 15.92 15.51 N3 D P DP
T7 2MASS 0727+17 07 27 18.2 17 10 01 15.55 15.82 15.56 N3 D P DP
T8 Gl 570D 14 57 15.0 -21 21 48 15.33 15.28 15.27 N1,2,3,4,6a,6b D P D P D P D P D P D P DP
T8 2MASS 0415-09 04 15 19.5 -09 35 06 15.71 15.57 15.45 N3,5,6b D P D P D P DP
All coordinates and JHKs photometry are from the 2MASS All-Sky Data Release. Magnitude uncertainties can be obtained from Table 2 of McLean et al. (2003).
Spectral types for M dwarfs based on the classification scheme of Kirkpatrick, Henry, & McCarthy (1991) and Kirkpatrick, Henry, & Simons (1995).
Spectral types for L dwarfs based on the Kirkpatrick optical classification scheme.
Spectral types for T dwarfs based on the Burgasser near-infrared classification scheme.

For additional information regarding objects in this archive see Davy Kirkpatrick's L & T Dwarf Archive.

High-Resolution Data Products

 D  -- Link to individual ascii data file (flux vs. wavelength).
 P  -- Link to postscript plot of all echelle orders.
Type Object Name   RA (2000)    Dec (2000)  J    Itime (s)    BVC (km/s)    58       59       60       61       62       63       64       65       PS Plot   
M6 Wolf 359 (Gl 406) 10 56 28.9 07 00 53 7.09 480 -22.56 D D D D D D D D P
M9 2MASS 0140+27 01 40 02.6 27 01 50 12.49 2400 -18.48 D D D D D D D D P
L0 2MASS 0345+25 03 45 43.2 25 40 23  13.99  2400 -6.48 D D D D D D D D P
L0.5 2MASS 0746+20AB     07 46 42.6 20 00 32 11.74 1440 7.40 D D D D D D P
L2 G196-3B 10 04 20.7 50 23 00 14.83 2400 -23.57 D D D D D D D D P
L2 Kelu-1 13 05 40.2 -25 41 06 13.42 5400 -11.99 D D D D D D D D P
L3.5 2MASS 0036+18 00 36 16.2 18 21 10 12.44 2400 -24.59 D D D D D D D D P
L4 GD 165B 14 24 39.1 09 17 10 15.55 5400 -9.39 D D D D D D D D P
L5 2MASS 1507-16 15 07 47.7 -16 27 39 12.82 2400 7.30 D D D D D D D D P
L7 DENIS 0205-11AB 02 05 29.4 -11 59 30 14.58 1200 4.62 D D D D D D D D P
T0 SDSS 0423-04 04 23 48.6 -04 14 04 14.45 2400 19.27 D D D D D D D D P
T2 SDSS 1254-01 12 54 53.9 -01 22 47 14.88 4200 -18.41 D D D D D D D D P
T4.5 2MASS 0559-14 05 59 19.1 -14 04 48 13.83 1200 22.54 D D D D D D D D P
T6p 2MASS 0937+29 09 37 34.7 29 31 42 14.65 3600 -28.64 D D D D D D D D P
All coordinates and J-band photometry are from the 2MASS All-Sky Data Release. Magnitude uncertainties can be obtained from Table 1 of McLean et al. (2007).

Itime is the total integration time in seconds, and BVC is the applied barycentric velocity correction in kilometers per second.

Note: 2MASS 0746 is missing orders 60 and 64 because of a lack of arc lamp lines for wavelength calibration. Other orders are calibrated with OH night sky lines.

The NIRSPEC Brown Dwarf Spectroscopic Survey (BDSS)

Paper I: McLean, I.S., McGovern, M.R., Burgasser, A.J., Kirkpatrick, J.D., Prato, L., & Kim, S.S. 2003, ApJ, 596, 561

Paper II: McLean, I.S., Prato, L., McGovern, M.R., Burgasser, A.J., Kirkpatrick, J.D., Rice, E. L., & Kim, S.S. 2007, ApJ, 658, 1217

Please cite one or both of the above references if you use or display these data in your publications or presentations.


Created by Mark McGovern
Maintained by Emily Rice, Greg Mace, and Antonia Hubbard
Last Updated: 27 July 2009
E-mail: erice {AT} astro {o} ucla {o} edu