----- Submission 1 (Fri May 13 02:00:11 GMT 2005) ----- warnings can be ignored. EN. Calibrating the Mass-Luminosity Relation at the End of the Main Sequence We propose to use HST-FGS1R to calibrate the mass-luminosity relation (MLR) for stars less massive than 0.2 Msun, with special emphasis on objects near the stellar/brown dwarf border. Our goals are to determine M_V values to 0.05 magnitude, masses to 5\ than double the number of objects with masses determined to be less than 0.20 Msun. This program uses the combination of HST-FGS3/FGS1R at optical wavelengths and ground-based infrared interferometry to examine nearby, subarcsecond binary systems. The high precision measurements with HST-FGS3/FGS1R (to 1 mas in the separations) for these faint targets (V = 10--15) simply cannot be equaled by any ground based technique. As a result of these measurements, we are deriving high quality luminosities and masses for the components in the observed systems, and characterizing their spectral energy distributions from 0.5 to 2.2 Mum. Several of the objects included have M < 0.1 Msun, placing them at the very end of the stellar main sequence. Three of the targets are brown dwarf candidates, including the current low mass record holder, GJ 1245C, with a mass of 0.062 +/- 0.004 Msun. The payoff of this proposal is high because all 10 of the systems selected have already been resolved with HST- FGS3/FGS1R during Cycles 5--10 and contain most of the reddest objects for which masses can be determined.
Cycle 5--13 Update: FGS-TRANS observations of the systems were (generally) made at the beginning and end of Cycle 5 and once each in Cycles 6/7/8/9/10/11/12/13, resulting in about six observations so far for each system (except Gl 54 and GJ 2005, which were added more recently). Additional Cycle 10 measurements have not yet been carried out for eight of the systems. The TRANS mode observations are used to map the binary orbits via determination of the separations and position angles, and to measure the magnitude difference of the components so that luminosities can be derived. In Cycles 8-13 FGS-POS measurements have been made to locate the position of the center of mass of each system with respect to background stars. This allows us to determine the fractional masses of the components so that individual masses can be derived. Because of the long orbital periods of these systems, radial velocity techniques are not typically useful in getting fractional masses because the velocity differences are small, in addition to the complicating factor that the systems are generally faint and the velocities are of poor precision. The timing of observations has been carefully planned to provide points on the orbits every 20--30^degrees, and a similar strategy will be used in Cycles 11/12/13. Experience from Gl 748 (17 observations) and Gl 791.2 (14 observations) indicates that a set of roughly 12 measurements spread around the orbit is sufficient to achieve orbital parameter errors smaller than 1\ error in the semimajor axis triples in Kepler's Third Law, which is why we need orbital elements with minimal error, and the consequent orbital coverage. Cycle 11--13 Plan: We propose to continue this effort to (1) increase the orbital coverage from six to nine years, thereby passing the critical half-orbit point on all of the systems, (2) determine the first masses for six systems, (3) revise masses for four systems, (4) refine the brightness ratios, and (5) employ the low-cost (in the sense of number of orbits) technique to measure the fractional masses in nine systems. In essence, via this program HST-FGS will be the instrument responsible for defining the MLR for the most populous stars in the Galaxy --- not a bad legacy for the sometimes forgotten HST instrument. Each of the 10 systems will be observed once each Cycle in FGS-TRANS mode through filter F583W to determine the separation, position angle, and brightness difference between the components. For the TRANS mode observations, 20--60 scans 0.8--3.0" in length are typically made across the binary. The F583Waperture has been selected because it is the best calibrated of the filters available in FGS. The transmission of the telescope through F583W is already calibrated to the Johnson V band (Henry et al 1999), and will allow the magnitude difference at visible wavelengths to be attained with high accuracy. During the same orbit, nine of the systems will be observed in FGS-POS mode to relate the binary to a background grid of stars in order to find the center of mass (Gl 473 is the lone exception because it lacks reference stars). POS mode observations will include multiple runs through the field. The POS mode observations allow to get fractional masses for each system. Over time, the vector connecting the two components rotates about the center of mass as they orbit one another. By overlapping the yearly vectors, we pinpoint the center of mass and derive the fractional masses, provided that the movement of the system due to its proper motion and parallax can be removed using accurate ground-based data. Errors in the location of vector overlap due to parallax uncertainties are minimized by observing the systems at nearly the same time every year. GJ 1215 and GJ 2005 are the most difficult targets due to faintness, but they are arguably the most important targets --- their secondaries have masses in the brown dwarf regime. 12 false 0.0 false false false false false SUPPORTED STAR M V-IV B-V = 1.54+/-0.05 TYPE=M2V BEWARE: second component at 4" with V = 12.4 BD+66D34 LHS114 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV B-V = 1.72+/-0.05 TYPE=M5V ROSS614 LHS1849 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV B-V = 1.60+/-0.05 TYPE=M4V Comments: WOLF414 LHS2565 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV B-V = 1.84+/-0.05 TYPE=M6V WOLF424 LHS333 J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV B-V = 1.60+/-0.1 TYPE=M3V coords from GO 6036 = GJ1081-NEW G096-045 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV B-V = 1.90+/-0.05 TYPE=M6V V1581CYG LHS3494 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV B-V = 1.54+/-0.05 TYPE=M2V LHS221 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.00457 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.00583 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.00607 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.00943 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.01009 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.01155 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.01260 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.01999 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.00473 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC04110.00473 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC3149.00606 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC3149.00132 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC3149.01167 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC3149.01073 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC3149.00600 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC02922.00143 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC02922.00581 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC02922.00134 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV V = 9.80+/-0.05 B-V = 1.57+/-0.05 TYPE=M3.0V LHS1208 HIP5496 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC8855.00240 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC9136.00023 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC8855.00236 J2000 00 00 0.0000 +00 00 0.00 J2000 CALIBRATION ASTROMETRIC GSC8855.00190 J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV GJ3421 GSC3767.01193 J2000 00 00 0.0000 +00 00 0.00 J2000 STAR M V-IV This is the same target as LHS224AB, but with a false magnitude specification that will facilitate acquisition for the POS mode exposures. 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