An estimate of H-0 from Keck spectroscopy of the gravitational lens system 0957+561

We present long-slit LRIS/Keck spectroscopic observations of the gravitational lens system 0957 + 561. Averaged over all of our data, the rest-frame velocity dispersion a, of the central lens galaxy G1 is sigma(upsilon) = 279 +/- 12 km s(-1). However, there appears to be a significant decrease in sigma(upsilon) as a function of distance from the center of G1 that is not typical of the brightest cluster galaxies. Within 0.''2 of the center of G1, we find the average sigma(upsilon) = 316 +/- 14 km s(-1), whereas for positions greater than 0.''2 from the center of G1, we find the average sigma(upsilon) = 266 +/- 12 km s(-1). A plausible explanation is that G1 contains a central massive dark object of mass M-MDO approximate to x 10(9) h(100)(-1) M. (h(100) = H-0/100 km s(-1) Mpc(-1)), which contributes to the central velocity dispersion, and that the outer value of sigma(upsilon) is the appropriate measure of the depth of the potential well of G1. The determination of a luminosity-weighted estimate of sigma(upsilon) is essential for a determination of H-0 from Q0957 + 561; our accurate measurements remove one of the chief uncertainties in the assumed form of the mass distribution of the lens. Thus, with the recent apparent reduction in the uncertainty in the measurement of the time delay for the images A and B of Q0957 + 561, Delta tau(BA) = 417 +/- 3 days (Kundic et al.), we obtain an estimate for the Hubble constant: H-0 = 62 +/- 7 km s(-1) Mpc(-1). If for some reason the trend of sigma(upsilon) with slit position is spurious and we should use the dispersion averaged along the slit, then the estimate of H-0 increases to 67 +/- 8 km s(-1) Mpc(-1). These standard errors, however, do not include any contribution from any errors in the assumed form of the mass distribution of the lens. In particular, we used the mass model described by Falco, Gorenstein, & Shapiro, as updated by Grogin & Narayan. The reduced chi(2) of model fits to the available position and magnification data for this system is relatively high (similar to 4), indicating that the estimate of H-0 may have a significant contribution from model errors. Further observations, discussed herein, should allow such errors to be estimated reliably.