Context : This paper is part of our ongoing study of star formation in the ( far- ) outer Galaxy .

Aims : Our goal in this paper is to study stars and molecular gas in the direction of IRAS06145+1455 ( WB89-789 ) .
The kinematic distance of the associated molecular cloud is 11.9 kpc .
With a galactocentric distance of \sim 20.2 kpc , this object is at the edge of the ( molecular ) disk of the Galaxy .

Methods : We use near-IR ( J , H , K ) , molecular line- , and dust continuum observations .

Results : The near-IR data show the presence of an ( embedded ) cluster of about 60 stars , with a radius \sim 1.3 pc and an average stellar surface density \sim 12 pc ^ { -2 } .
We find at least 14 stars with NIR-excess , 3 of which are possibly Class I objects .
The cluster is embedded in a \sim 1000 M _ { \odot } molecular/dust core , from which a molecular outflow originates .
The temperature of most of the outflowing gas is \lower 2.58 pt \hbox { $ \sim$ } \kern - 7.75 pt \raise 2.795 pt \hbox { $ < $ } 40 K , and the total mass of the swept-up material is \lower 2.58 pt \hbox { $ \sim$ } \kern - 7.75 pt \raise 2.795 pt \hbox { $ < $ } 10 M _ { \odot } .
Near the center of the flow , indications of much higher temperatures are found , probably due to shocks .
A spectrum taken of one of the probable cluster members shows a tentative likeness to that of a K3 III-star ( with an age of at least 20 Myr ) .
If correct , this would confirm the kinematic distance .

Conclusions : This cluster is the furthest one from the Galactic center yet detected .
The combination of old and recent activity implies that star formation has been going on for at least 20 Myr , which is difficult to understand considering the location of this object , where external triggers are either absent or weak , compared to the inner Galaxy .
This suggests that once star formation is occurring , later generations of stars may form through the effect of the first generation of stars on the ( remnants of ) the original molecular cloud .