H$α$-Derived Star-Formation Rates for the z=0.84 Galaxy Cluster CLJ0023+0423B

Details H$α$-Derived Star-Formation Rates for the z=0.84 Galaxy Cluster CLJ0023+0423B H$α$-Derived Star-Formation Rates for the z=0.84 Galaxy Cluster CLJ0023+0423B

2003-11-21

arxiv.org/abs/astro-ph/0311501v1

Astrophys.J. 604 (2004) 141-152

Astronomy and Astrophysics

Astrophysics

13 pages, 4 jpg figures, to be published in ApJ. Version with all figures inlined is available at http://www.astro.umass.edu/~

Scientific paper

10.1086/381729

We present H$\alpha$-derived star-formation rates (SFRs) for the galaxy cluster CL J0023+0423B at $z = 0.845$. Our $3\sigma$ flux limits corresponds to a star-formation rate of 0.24 \smy, and our minimum reliable H$\alpha$ + [N II] equivalent width is $> 10$ \AA, demonstrating that near-infrared narrow-band imaging can sample the star-forming galaxy population in distant clusters. Comparison with spectroscopy shows that the number of false detections is low ($9 \pm 6$%) and that our H$\alpha$ equivalent widths are correlated with spectroscopically determined [O II] equivalent widths. A magnitude-limited spectroscopic survey conducted over the same area missed 70% of the star-forming galaxies and 65% of the integrated star formation. Using Hubble Space Telescope Wide Field Planetary Camera 2 Archive images, we fit Sersic profiles to all galaxies with significant narrow-band equivalent widths and find that equivalent width decreases as the steepness of galaxy profile increases. We find no significant population of early type galaxies with ongoing star formation. The integrated SFR per cluster mass of CL J0023+0423B is a factor of ten higher than that of the three $z \sim 0.2$ clusters in the literature with available H$\alpha$ observations. A larger sample of $z \sim 0.8$ clusters spanning a range of cluster masses is needed to determine whether this variation is due to a difference in cluster mass or redshift.

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