  We present the X-ray spectral and timing analysis of the transient black hole
X-ray binary 4U 1630-47, observed with the AstroSat, Chandra and MAXI space
missions during its soft X-ray outburst in 2016. The outburst, from the rising
phase until the peak, is neither detected in hard X-rays (15-50 keV) by the
Swift/BAT nor in radio. Such non-detection along with the source behavior in
the hardness-intensity and color-color diagrams obtained using MAXI data
confirm that both Chandra and AstroSat observations were performed during the
high soft spectral state. The High Energy Grating (HEG) spectrum from the
Chandra high-energy transmission grating spectrometer (HETGS) shows two strong,
moderately blueshifted absorption lines at 6.705$_{-0.002}^{+0.002}$ keV and
6.974$_{-0.003}^{+0.004}$ keV, which are produced by Fe XXV and Fe XXVI in a
low-velocity ionized disk wind. The corresponding outflow velocity is
determined to be 366$\pm$56 km/s. Separate spectral fits of Chandra/HEG,
AstroSat/SXT+LAXPC and Chandra/HEG + AstroSat/SXT+LAXPC data show that the
broadband continuum can be well described with a relativistic disk-blackbody
model, with the disk flux fraction of $\sim 0.97$. Based on the best-fit
continuum spectral modeling of Chandra, AstroSat and Chandra+AstroSat joint
spectra and using the Markov Chain Monte Carlo simulations, we constrain the
spectral hardening factor at 1.56$^{+0.14}_{-0.06}$ and the dimensionless black
hole spin parameter at 0.92 $\pm$ 0.04 within the 99.7% confidence interval.
Our conclusion of a rapidly-spinning black hole in 4U 1630-47 using the
continuum spectrum method is in agreement with a previous finding applying the
reflection spectral fitting method.
