Small‐Scale Structure at High Redshift. I. Glimpses of the Interstellar Medium at Redshift ∼3.5

Abstract

We obtained Keck High Resolution Echelle Spectrometer (FWHM \ 4.4 km s~1) spectra of images A and C of the gravitationally lensed quasar Q1422]231 The images are separated by (z em \ 3.628). 1A .3 on the sky. In an absorption system at gas column density variations by an order of magni-z abs \ 3.538, tude and velocity shear on the order of 10 km s~1 are observed in the low-ionization (Si II and C II) lines. The transverse separation in the absorbing cloud is estimated to be as small as 26 pc, corre-h 50 ~1 sponding to an e †ective angular resolution of 4 mas as seen from the Earth. In contrast, the high-ionization (C IV) gas appears mostly featureless and thus must be considerably more extended. The abundances of the elements carbon, silicon, and oxygen appear to be close to the solar values. The observation provides the Ðrst spatially and kinematically resolved probe of the interstellar medium at high redshift on scales small enough to be inÑuenced by individual stars or star clusters. The mass associated with the low-ionization "" cloudlets ÏÏ is likely to be less than about 3000 and possibly less M _ than 1 The velocity shear that is seen across the lines of sight is too large to be caused by galactic M _. bulk motion, so the velocity Ðeld of the low-ionization gas must be strongly inÑuenced by small-scale local gasdynamics. While presently it cannot be excluded that the disturbances of the gas are due to high-velocity outÑows from the background quasar, the observed velocity and density structure of the z \ 3.538 absorption is consistent with our line of sight running through an expanding shell of gas, possibly a supernova bubble or a stellar wind.