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We report new HST COS and STIS spectroscopy of a star-forming region (~100solar masses/year) in the center of the X-ray cluster RXJ1532.9+3021 (z=0.362),to follow-up the CLASH team discovery of luminous UV filaments and knots in thecentral massive galaxy. We detect broad (~500 km/s) Lyman alpha emission lineswith extraordinarily high equivalent width (EQW~200 Angstroms) and somewhatless broadened H-alpha (~220 km/s). Emission lines of N V and O VI are notdetected, which constrains the rate at which gas cools through temperatures of10^6 K to be less than about 10 solar masses/year. The COS spectra also show aflat rest-frame UV continuum with weak stellar photospheric features,consistent with the presence of recently-formed hot stars forming at a rate of~10 solar masses/year, uncorrected for dust extinction. The slope andabsorption lines in these UV spectra are similar to those of Lyman BreakGalaxies at z approximately 3, albeit those with the highest Lyman-alphaequivalent widths and star-formation rates. This high-EQW Lyman-alpha source isa high-metallicity galaxy rapidly forming stars in structures that look nothinglike disks. This mode of star formation could significantly contribute to thespheroidal population of galaxies. The constraint on the luminosity of any O VIline emission is stringent enough to rule out steady and simultaneous gascooling and star formation, unlike similar systems in the Phoenix Cluster andAbell 1795. The fact that the current star formation rate differs from thelocal mass cooling rate is consistent with recent simulations of episodic AGNfeedback and star formation in a cluster atmosphere.

Observations of Lyman-alpha and O VI: Signatures of Cooling and Star Formation in a Massive Central Cluster Galaxy