Hα Star Formation Rates for z>1 Galaxy Clusters in the IRAC Shallow Cluster Survey Using WFC3 IR Grism Spectroscopy

Details Hα Star Formation Rates for z>1 Galaxy Clusters in the IRAC Shallow Cluster Survey Using WFC3 IR Grism Spectroscopy Hα Star Formation Rates for z>1 Galaxy Clusters in the IRAC Shallow Cluster Survey Using WFC3 IR Grism Spectroscopy

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21840304z&link_type=abstract

American Astronomical Society, AAS Meeting #218, #403.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

We present new HST WFC3 grism data for 17 z>1 galaxy clusters in the IRAC Shallow Cluster Survey (ISCS). Using the G141 grism (λ = 1.10 - 1.65 μm, 46.5 A/pixel), we identified ˜5-15 new cluster members in each cluster candidate with a visual inspection of emission line galaxies in the reduced 1-d and 2-d spectral extractions. Given the redshift range of the cluster candidates and the wavelength coverage of the G141 grism, the emission line most identified was the blended Hα+NII. Correlations found in the literature between the EW of Hα+NII and the line ratio of NII to Hα were used to deblend the two fluxes. Hα emission was used as an indicator of star formation. Our program is sensitive to an unobscured star formation rate of 4 M&sun; / Year for z=1.5 and a nominal 1:4 ratio of NII to Hα. Concurrent MIPS 24μm data allows for the comparison of different SFR tracers. Whenever possible, we also use the ratio of Hβ/Hα to estimate dust obscuration and correct the SFRs. This dataset allows the study of a wide-range of star formation rates in dense cluster cores during the peak epoch of galaxy formation.

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