Updated Models for the Creation of a Low-z QSO Absorber by a Dwarf
  Galaxy Wind
  We present new GALEX images and optical spectroscopy of J1229+02, a dwarf
post-starburst galaxy located 81 kpc from the 1585 km/s absorber in the 3C 273
sight line. The absence of H\alpha\ emission and the faint GALEX UV fluxes
confirm that the galaxy's recent star formation rate is $<10^{-3}
M_{\odot}$/yr. Absorption-line strengths and the UV-optical SED give similar
estimates of the acceptable model parameters for its youngest stellar
population where $f_m$ < 60% of its total stars (by mass) formed in a burst
$t_sb$ = 0.7-3.4 Gyr ago with a stellar metallicity of -1.7 < [Fe/H] < +0.2; we
also estimate the stellar mass of J1229+02 to be 7.3 < log($M_*/M_{\odot}$) <
7.8. Our previous study of J1229+02 found that a supernova-driven wind was
capable of expelling all of the gas from the galaxy (none is observed today)
and could by itself plausibly create the nearby absorber. But, using new data,
we find a significantly higher galaxy/absorber velocity difference, a younger
starburst age, and a smaller starburst mass than previously reported. Simple
energy-conserving wind models for J1229+02 using fiducial values of $f_m$ ~
0.1, $t_sb$ ~ 2 Gyr, and log(M$_*/M_{\odot}$) ~ 7.5 allow us to conclude that
the galaxy alone cannot produce the observed QSO absorber; i.e., any putative
ejecta must interact with ambient gas from outside J1229+02. Because J1229+02
is located in the southern extension of the Virgo cluster ample potential
sources of this ambient gas exist. Based on the two nearest examples of strong
metal-line absorbers discovered serendipitously (the current one and the 1700
km/s metal-line absorber in the nearby Q1230+0115 sight line), we conclude that
absorbers with $10^{14} < N_{HI} < 10^{16}$ cm$^{-2}$ at impact parameters
>1$R_{vir}$ are likely intergalactic systems and cannot be identified
unambiguously as the circumgalactic material of any one individual galaxy.
