An estimate of H_0 from Keck spectroscopy of the gravitational lens system 0957+561

Emilio E. Falco, Irwin I. Shapiro, Leonidas A. Moustakas, Marc Davis

Published 1997-02-18Version 1

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 sigma_v of the central lens galaxy G1 is sigma_v = 279 +- 12 km/s. However, there appears to be a significant decrease in sigma_v as a function of distance from the center of G1 that is not typical of brightest cluster galaxies. Within 0.2" of the center of G1, we find the average sigma_v = 316+- 14 km/s, whereas for positions > 0.2" from the center of G1, we find the average sigma_v= 266+-12 km/s. A plausible explanation is that G1 contains a central massive dark object of mass M_MDO ~ 4x10^9 h_100^{-1} M_sun (h_100 = H_0/100km/s/Mpc), which contributes to the central velocity dispersion, and that the outer value of sigma_v is the appropriate measure of the depth of the potential well of G1. The determination of a luminosity-weighted estimate of sigma_v is essential for a determination of H_0 from 0957+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 0957+561, Delta tau_BA = 417+-3 d (Kundic et al. 1996), we obtain an estimate for the Hubble constant: H_0 = 62+-7 km/s/Mpc. If for some reason the trend of sigma_v 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/Mpc. These standard errors do not, however, 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 (1991), as updated by Grogin & Narayan (1996a, b). The reduced chi^2