The Supernova Type Ia Rate Evolution with SNLS

Creators: Neill, James D.; Sullivan, M.; Balam, D.; Pritchet, C. J.; Howell, D. A.; Perrett, K.; Astier, P.; Aubourg, É.; Basa, S.; Carlberg, R. G.; Conley, A.; Fabbro, S.; Fouchez, D.; Guy, J.; Hook, I.; Pain, R.; Palanque-Delabrouille, N.; Regnault, N.; Rich, J.; Taillet, R.; Aldering, G.; Antilogus, P.; Arsenijevic, V.; Balland, C.; Baumont, S.; Bronder, J.; Ellis, R. S.; Filiol, M.; Gonçalves, A. C.; Hardin, D.; Kowalski, M.; Lidman, C.; Lusset, V.; Mouchet, M.; Mourão, A.; Perlmutter, S.; Ripoche, P.; Schlegel, D.; Tao, C.

Style

An error occurred while generating the citation.

Abstract

We present a progress report on a project to derive the evolution of the volumetric supernova Type Ia rate from the Supernova Legacy Survey. Our preliminary estimate of the rate evolution divides the sample from Neill et al. into two redshift bins: 0.2 < z < 0.4, and 0.4 < z < 0.6. We extend this by adding a bin from the sample analyzed in Sullivan et al. in the range 0.6 < z < 0.75 from the same time period. We compare the derived trend with previously published rates and a supernova Type Ia production model having two components: one component associated closely with star formation and an additional component associated with host galaxy mass. Our observed trend is consistent with this model, which predicts a rising SN Ia rate out to at least z = 2.

Additional Information

© 2007 American Institute of Physics. Issue Date: 21 August 2007. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are grateful for our opportunity to conduct observations on this mountain. We acknowledge invaluable assistance from the CFHT Queued Service Observations team, led by P. Martin (CFHT). Our research would not be possible without the assistance of the support staff at CFHT, especially l-C. Cuillandre. The real-time pipelines for supernovae detection run on computers integrated in the CFHT computing system, and are very efficiently installed, maintained and monitored by K. Withington (CFHT). We also heavily rely on the real-time Elixir pipeline which is operated and monitored by l-C. Cuillandre, E. Magnier and K. Withington. We are grateful to L. Simard (CADC) for setting up the image delivery system and his kind and efficient responses to our suggestions for improvements. The Canadian collaboration members acknowledge support from NSERC and CIAR; French collaboration members from CNRS/IN2P3, CNRS/INSU, PNC and CEA. This work was supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the US Department of Energy. The France-Berkeley Fund provided additional collaboration support. We are indebted to A. Hopkins and 1 Beacom for providing us with a draft of their work on SFH prior to its publication. The views expressed in this article are those of the author and do not reflect the official policy or position of the United States Air Force, Department of Defense, or the U.S. Government.

Attached Files

Published - NEIaipcp07.pdf

Files

NEIaipcp07.pdf

Files (384.0 kB)

Name	Size	Download all
NEIaipcp07.pdf md5:b17fb56659a7d29d17a9634cdf021021	384.0 kB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes