W. M. KECK OBSERVATORY
Observing Proposal Coversheet for Semester 2005B
Allocating Institution:   UC
No. of nights requested:   2
No. of nights estimated to complete program in addition to those requested here:   None
Is this the first application for this program?   No
Institutional use: Proposal # _______
LRIS
CIT Proposals Only

CIT Priority:    ToO Interrupts?  Yes

UC Proposals Only

UC PI position:  faculty  

INVESTIGATOR INFORMATION

Principal Investigator:
Prof. Saul Perlmutter   (saul@lbl.gov)
Physics Department, University of California-Berkeley, LBL 50-232, Berkeley, CA 94720
(w) 510-486-5203 / (FAX) 510-486-6738 / (h) 510-841-7285

Co-Investigators:
Prof. Gerson Goldhaber: G_Goldhaber@lbl.gov
Mamoru Doi: doi@ioa.s.u-tokyo.ac.jp
Vitaliy Fadeyev: VAFadeyev@lbl.gov
Naoki Yasuda: yasuda@icrr.u-tokyo.ac.jp
Rollin Thomas: RCThomas@lbl.gov
Tony Spadafora: ALSpadafora@lbl.gov
Greg Aldering: aldering@panisse.lbl.gov
Kyle Dawson: KDawson@lbl.gov
David Schlegel: DJSchlegel@lbl.gov
Tomoki Morokuma: tmorokuma@ioa.s.u-tokyo.ac.jp
Lifan Wang: LWang@lbl.gov
Chris Lidman: clidman@eso.org
OBSERVING TEAM AND LOCATION

Observers projected to be present in Hawaii:  Greg Aldering, Kyle Dawson, Saul Perlmutter, David Schlegel
Observer location:  Waimea-HQ

PROGRAM

Title:  Exploring the Decelerating Epoch: Putting a New Sample of z>1 SNe Ia on the Hubble Diagram

Summary of Program (less than 100 words, for general distribution):
By determining the host-galaxy redshifts for nine well-studied supernovae, we propose to complete a comprehensive multi-telescope campaign that has yielded the largest-to-date sample of SNe Ia in the "decelerating" redshift range. This sample would more than double the number of such SNe Ia on the Hubble diagram in this sparsely populated redshift range. This larger sample will make it possible to begin to look for a Hubble-plot ridgeline and for outliers, providing tests for non-Ia contamination, and for a residual extinction tail and gravitational lensing asymmetric distribution. Exploring such redshifts will be key for measurements of dark energy's w and ultimately w'.

Observing Time Preference & Instrument Selection
Moon D G-DL B G-DE D
From Date 01 Aug 11 Aug 15 Aug 25 Aug 29 Aug
To Date 10 Aug 14 Aug 24 Aug 28 Aug 08 Sep
InstrumentNo. nights ~ LST
@midnite		 20:40 21:10 21:35 22:05 22:25
LRIS2Request 1 X X X X X
Request 2          
Request 3          
Request 4          

Moon G-DL B G-DE D G-DL B G-DE D G-DL B
From Date 09 Sep 13 Sep 23 Sep 28 Sep 08 Oct 12 Oct 23 Oct 27 Oct 06 Nov 10 Nov
To Date 12 Sep 22 Sep 27 Sep 07 Oct 11 Oct 22 Oct 26 Oct 05 Nov 09 Nov 20 Nov
~ LST
@midnite		 23:00 23:30 00:00 00:30 00:55 01:25 01:55 02:25 02:50 03:20
Request 1 X X X A X X X P X X
Request 2                    
Request 3                    
Request 4                    

Moon G-DE D G-DL B G-DE D G-DL B G-DE D
From Date 21 Nov 26 Nov 05 Dec 09 Dec 21 Dec 26 Dec 03 Jan 08 Jan 19 Jan 24 Jan
To Date 25 Nov 04 Dec 08 Dec 20 Dec 25 Dec 02 Jan 07 Jan 18 Jan 23 Jan 31 Jan
~ LST
@midnite		 03:50 04:20 04:45 05:15 05:50 06:15 06:40 07:15 07:45 08:10
Request 1 X A X X X X X X X X
Request 2                    
Request 3                    
Request 4                    

Additional information on Observing Time Preferences and Instrument Needs

Specific dates needed:   None
Dates to avoid:   None
Details or special requests:   Please contact the P.I. before scheduling to coordinate with other telescopes' observing programs.
RA range of objects:   RA range: 02:17:00 to 02:21:00, DEC range: -05:10:00 to -04:30:00

Special instrument needs:  None

Late multislit mask request:  

to your input form
WMKO Coversheet Processor by Gregory D. Wirth (WMKO)
Please direct comments on this form to bschaefer@keck.hawaii.edu
Last revision of this form: v1.14, 03-Mar-2005