Keck Spectra Of z 2 Ultraviolet-Luminous Supernovae: Host Properties, Population III Stars, And The Initial Mass Function At High Redshift

Details Keck Spectra Of z 2 Ultraviolet-Luminous Supernovae: Host Properties, Population III Stars, And The Initial Mass Function At High Redshift Keck Spectra Of z 2 Ultraviolet-Luminous Supernovae: Host Properties, Population III Stars, And The Initial Mass Function At High Redshift

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21742301c&link_type=abstract

American Astronomical Society, AAS Meeting #217, #423.01; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

We present 10 spectroscopically confirmed supernovae (SNe) detected in Lyman break galaxies (LBGs) at z = 2.0-2.4. Nine of the 10 spectra exhibit long-lived, luminous rest-frame UV emission features observed in local type IIn SNe, with several spectra showing strong Ly-alpha emission. We investigate the properties of the host galaxies with respect to the 70,000 monitored r' < 26.5 z 2 LBGs in the survey and find that type IIn SNe are found preferentially in hosts that are fainter and bluer than the median of the full sample.
The remaining event does not display similar emission-line behavior and, in particular, does not show late-time hydrogen emission. The photometric behavior of this extremely luminous event, M(UV) -21, is reminiscent of ultra-luminous events recently discovered at lower redshift argued to be pair instability supernovae (PISNe). Because Population III stars are believed to result in PISNe, detections of such events at z 2, and higher, may provide the first observational examples of Population III stars. Finally, we present an approach that exploits these data to enable the first direct constraint on the form of the stellar initial mass function at high redshift.
The SNe are photometrically detected in the four square-degree fields of the Deep component of the Canada-France-Hawaii Telescope Legacy Survey. Follow-up deep spectroscopy of SN candidates was performed at the W. M. Keck Observatory.

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