Semester: 2004A		Partner reference: Not Available		PI time requested: 10.0 hours
Gemini reference: Not Available		Partner ranking: Not Available		PI minimum time requested: 1.0 nights
Instruments(s): GMOS North		NTAC recommended time: 0.0 nights		PI future time requested: 120.0 hours
Observing mode: queue		NTAC minimum recommended: 0.0 nights		PI total from all partners: 60.0 hours (joint proposals)
Time awarded: Not Available		Proposal submitted to: United States
		...also submitted to...United Kingdom, Canada (joint proposals)

The goal for Gemini this semester is to obtain types and redshifts for ~60 SNeIa out to z~=0.9. This will provide a high quality SNeIa sample comparable in size to existing SNeIa samples, but with superior photometry, light-curve sampling, and colour information. Gemini observations represent a vital component of our overall spectroscopic followup strategy, which also involves the ESO VLT, Keck, and Magellan telescopes.

Science Justification

Our goal is to distinguish between these models (which arise from fundamental physics) using direct geometric distance measurements of supernovae. To do this requires a concerted program to find ~1000 SNeIa at 0.2<z<1 (more than 10x the current sample), and obtain multi-colour (g'r'i'z') light curves with excellent (2-3d) sampling. (The multicolour observations improve reddening determinations; the time sampling is essential for measuring maximum light and determining the light curve "scale factor", which correlates with maximum light brightness.)

THE CFHT LEGACY SURVEY

The CFHT Legacy Survey (CFHTLS) is tailor-made for this purpose (202 nights of telescope time over 5 years, more than 500 epochs on four 1 sq deg fields, typical photometric sampling every ~2 days rest-frame, g'r'i'z' filters plus some u*, and almost real-time SN triggers - see http://www.cfht.hawaii.edu/Science/CFHTLS for more information). This unsurpassed "rolling search" strategy is possible thanks both to queue scheduling of CFHT, and to an enormous commitment of telescope time; it leads to improved efficiency for spectroscopic followup because: (1) it allows us to monitor the rise of the object and trigger spectroscopy at maximum light; (2) the flux of the target is well known since it is measured one or two days before max; this allows us an improved estimate of exposure time; (3) the detection of objects uses a lightcurve rather than a single flux difference.

The CFHTLS SN team is now routinely delivering SN detections and photometry within 24 hr of data being taken. The reader is referred to http://legacy.astro.utoronto.ca/ for 'up-to-the-minute' information on SN discoveries, and to Fig. 1 for some representative light curves from engineering time in 2003A.

THIS PROPOSAL

This application is to enable the vital spectroscopic classification of the candidate SNeIa from the CFHTLS imaging survey. Spectroscopy also provides an accurate estimate of the redshift to the SNeIa. The confirmed sample of SNeIa will be used to obtain a precise measurement of the cosmological parameters (Omega_mass,Omega_Lambda) and a measurement of the equation of state of the dark energy w with a precision of better than +-0.10 (1000 SNe) when combined with weak lensing constraints - see Fig. 2. The goal for this semester is to confirm ~60 SNeIa (z<~0.9) at Gemini.

This proposal is part of a well-organized international collaboration aimed at a precise measurement of cosmological parameters using the CFHTLS. The collaboration involves astronomers in Canada and France, as the lead agencies of the the CFHTLS; it also comprises groups in the USA, UK, and Europe. Spectroscopic followup time has been committed at the VLT; time is being applied for at Keck (PI Perlmutter) and Magellan (PI Carlberg, with additional observations by Magellan staff). More details of the spectroscopic followup strategy appear below.

DISCUSSION

Supernova obserations can be subjected to many straightforward tests to check for systematic effects. The CFHTLS u*g'r'i'z' data can be used to measure SN colours and hence test for reddening by comparison with colours for nearby SNe. (We have other collaborative plans to use IR data to extend colour measurements to the highest redshift objects in our sample at z~0.9.). In addition we will have a large enough sample to be able to study subsets divided by host galaxy type (derived from the host galaxy spectra or high resolution imaging), or galactocentric radius - this allows us to check for effects associated with changes in the underlying host galaxy population (metallicity, extinction, age), similar to the study of Sullivan et al (2003 MNRAS 340, 1057). The SN spectra themselves can be stacked to obtain a high S/N mean spectrum for different host galaxy types or z ranges; these can be compared against local SN spectra to check for small evolutionary effects.

This project is the first step in measuring w: it will assume constant w, and test the possibility that the dark energy is just the cosmological constant, i.e. the zero-point energy of the vacuum -- perhaps the simplest, best known dark energy model. Although the primary goal is to study SNeIa, some objects will turn out to be core collapse SNe. These are of interest in their own right (for measuring star formation rate as a function of z, and for studying the recently-discovered [Hamuy etal, astro-ph/0309122] relation between max brightness and envelope expansion velocity).

Attachments:

Technical Justification

We propose to use the GMOS spectrographs on Gemini N/S to obtain types and redshifts of supernovae with roughly 0.6<z<0.9. (Given the overheads with Gemini, it is most efficient to use GMOS on these fainter objects.) Based on our previous work (Hook, Perlmutter etal) these SNe will have I=23-24; GMOS exposures of up to 3600s will be needed, although in some cases 1800s will be sufficient. The goal in this proposal is to identify ~60 SNeIa in 2004A. Assuming overheads of 1800s per object and an equal split of 1800s and 3600s per target, a total of 60hr is requested from all partners. With experience, it may be possible to reduce overheads below 1800s.

All observations will use a 0.75" slit, the R400_G5305 grating, and OG515 order sorting filter. Our experience shows that the dispersion of the R400 grating (~2A/pix) gives excellent sky subtraction, and we can rebin the data ~10x afterwards for redshifts and SN typing. Nod-and-shuffle will be used for the faintest targets. Given the short time between SN discovery and spectroscopic observation, it is unfortunately not yet possible to design masks for multislit observations, but we are now discussing with Gemini a means of designing masks directly from astrometry (without GMOS pre-imaging). When this is implemented it should be possible to fabricate a multislit mask for a particular SN and its environs, and have it on the telescope within ~48 hr.

Guide stars: The coordinates quoted here are the coordinates for the main search fields. The exact coordinates of targets and associated guide stars will be entered into the Phase II file when known - based on previous experience we do not expect any difficulty in finding guide stars.

Gemini types and redshifts will be made public within a month of the observations being received from the Gemini Project Office.

SCHEDULING AND LOGISTICS

SNeIa will be discovered, and reach maximum light, throughout the semester. Thus observing time should be spread through the entire semester. We will obtain SN ID's in almost real time at CFHT (~24 hr turnaround), and will constantly update our Phase 2 proposal. See http://legacy.astro.utoronto.ca/ for the latest SN discoveries.

Jim Rich will be in charge of managing the distribution of SN ID's to the various telescopes involved in spectroscopy. In preparation for a given night, he will check the results of previous nights of spectroscopy, make a prioritized candidate list, and dispatch objects on this list to various telescopes. Gemini observations coordinator will be Isobel Hook (our contact for Phase 2 purposes).

INTERNATIONAL COLLABORATION

Spectroscopy on 8m class telescopes is essential for this project to succeed; the total amount of 8m time needed is well beyond the reach of any one group or nation. Our strategy for spectroscopic followup has progressed rapidly over the past few months, and at present is as follows:

o Gemini (this proposal) - We are applying for 6 nights per semester (2 UK, 3 Canada, 1 US). We have a preference for GMOS-N because of the lower fringing of the GMOS-N detectors, and because much of our observing this semester is in the Groth strip (accessible only from Hawaii). Hence this proposal is for GMOS-N only. However we would be able to use time on either telescope for fields D1 and D3 if that is easier to scehdule.

o ESO VLT - FORS1 time has been allocated over the next 2 years (60 hrs in 2003A, 60hrs in 2003B, ??? in 2004A). The PI is R. Pain; this group consists of UK, French and other European collaborators.

o Keck - Perlmutter et al. will apply for 4 nights of Keck time in Semester A. (The need for extra semester A time is discussed below.)

o Magellan - We will apply for 2-3 nights of Canadian time on Magellan. Carnegie scientists have also agreed to an informal arrangement in which they take spectra of z<~0.6 SNe in exchange for use of these SNe ID's for their own program of IR followup.

The following should be noted:

(1) Canadian and French astronomers are the principals behind the Legacy Survey. However, the role of followup spectroscopy is pivotal to the SN survey; hence Canada has agreed to the principle that it will be an equal partner with France in the Collaboration Board (which manages the collaboration) *only* if Canada contributes equal resources to the collaboration. The amount of UK Gemini + VLT time requested roughly satisfies this agreement.

(2) The ratio of 1 US to 2 UK to 3 Canadian Gemini nights recognizes the fact that our US collaborators are contributing 4 nights of Keck time, and UK is also contributing ESO time.

(3) Gemini time plays a key role in our observations. The time is essential for observations of the Groth strip (1419+52 - not observable from Chile) in semester A; it is essential for SN coverage in May-July, when the weather is bad in Chile. Finally, Gemini is queue-scheduled, a fact that makes the time enormously useful for observations of transient objects, compared to block-scheduled telescopes such as Keck.

(4) The DEEP survey team (S. Faber PI) has agreed in principle to coordinating our observations with DEEP survey observations; this potentially optimizes or increases our Keck allocation. Since March 2003 R. Ellis and collaborators have been providing SN spectra and types in CFHTLS fields; in exchange we provide Ellis etal with ID's and photometry to complement their high resolution followup.

(5) Allowing for overheads, and for time lost to weather and misidentifications (e.g. AGN's, SNeII), the total time to be allocated will allow the followup of roughly 200 SNeIa per year.

Space does not allow for a complete list of the collaboration members. The Co-I's on this proposal represent the core group; see www.astro.uvic.ca/~pritchet/SN/03Bco-i.html for a complete list.

FUTURE TIME

Though the CFHTLS is a 5 year program, the first two years of the spectroscopy (~240 hr total) are critical: observations over this period will enable a first estimate of w with reasonable errors. We will also submit proposals with time requests like this one in 04B, and 05A. A detailed analysis of the photometric properties of SNe may provide an alternative to spectroscopic typing in the future.

Observation Details

Resources

• Gemini North
  • GMOS North
    • Focal Plane Unit
      • Nod and Shuffle 0.75 arcsec
      • Longslit 0.75 arcsec
    • Disperser
      • R400_G5305
    • Filter
      • OG515_G0306
• Gemini South

Observing Conditions

Name	Image Quality	Sky Background	Water Vapor	Cloud Cover
SN spec	70%	50%	Any	50%

Scheduling Information:

Synchronous dates:

Optimal dates:

Impossible dates:

Additional Information

Keywords: Cosmological distance scale, Dark matter, Survey

Publications:

• Sullivan, M. et al. (2003), "Hubble Diagram of Type Ia Supernovae and Galaxy Morphology", MNRAS, 340, 1057
• Kasen, D. et al. (includes Howell) (2003), "... Flux and Polarization Spectra of the Type Ia Supernova SN 2001el ...", ApJ, in press (astro-ph/0301312)
• Garnavich et al (includes R. Carlberg) (2003), "Afterglow of GRB 011121 and Its Progenitor SN2001ke", ApJ, 582, 924
• Perlmutter, S., and Schmidt, B. (2003), "Measuring Cosmology with Supernovae". In Supernovae & Gamma Ray Bursts, astro-ph/0303428
• Perlmutter, S. et al. (2003), "Multi-Color Light Curves of Type Ia Supernovae ...", ApJ, in press. astro-ph/0302341
• Stadel, Babul, et al (2003), "Amplification Bias of Supernovae from Gravitational Lensing", in prep.
• Patton, Pritchet, Carlberg, et al. (2002), "CNOC2 Close Pairs and Merger Rates", ApJ, 565, 208
• Hoekstra et al, (2002), "Constraints on Omega and sigma8 from weak lensing in RCS fields", ApJ, 577, 604
• Hoekstra et al, (2002), "Weak Lensing Study of Galaxy Biasing", ApJ, 577, 595
• Simard et al. (2002), "DEEP Groth Strip Survey. II. HST Structural Parameters of Galaxies in Groth Strip", ApJS, 142, 1
• van den Bergh et al (2002), "Visibility of Bars and Spiral Structure at High z", AJ, 123, 2913-2924
• van den Bergh et al (2002), "Classifications of the Host Galaxies of Supernovae", PASP, 114, xxx, 2002
• Howell, D.A. (2002), "Progenitors of Subluminous Type Ia SNe", ApJL, 554, L193
• Stetson and Gibson (2001), "The distance to Supernova 1998aq in NGC3982", MNRAS, 328, L1-L4
• McCarthy, Carlberg, et al (2001), "Las Campanas IR Survey: Early Type Galaxies ...", ApJ, 560, L131
• Gibson, B., and Stetson, P.B. (2001), "Supernova 1991T and Ho", ApJ, 547, L103
• Hoekstra, Franx, Kuijken, Carlberg, et al (2001), "Weak Lensing Study of Low Mass Groups", ApJ, 548, L5
• Gibson, Stetson, et al (2000), "... Cepheid Distances to Type IA Supernovae and the Value of Ho,'' ApJ, 529, 723
• Iwamoto et al (includes D.Balam) (2000), "Peculiar Type Ic Supernova 1997EF: Another Hypernova", ApJ 534, 660
• Stetson, P.B. (2000), "Homogeneous Photometry ... I. Photometric Standard Stars". PASP, 112, 925
• Balam et al (1990-2002), numerous IAU Circulars on SNe
• Clocchiatti et al (includes Stetson) (2000), "The Luminous Type IC Supernova 1992AR at z=0.145",ApJ, 529, 661-674
• Pain R. et al (2001) : "The Distant Type Ia SN rate" 2002, ApJ, 577, 120
• G. Goldhaber, et al, (2001), Timescale Stretch Parameterization of Type Ia Supernova B-Band Light Curves, Astrophysical Journal, 558, 359
• R.Knop, et al, (2003), New Constraints on Ometa_M, Omega_Lambda, and w from an Independent Set of Eleven High-Redshfit Supernovae Observed with HST, Astrophysical Journal, in press
• Aldering G, Knop R., Nugent P. (2000) "The rise times of High- and Low- redshift Type Ia Supernovae are consistent", AJ, 119, 2110
• R. Knop, et al, (2000), Latest Cosmological Results from Type Ia Supernovae, Bulletin of the American Astronomical Society, 197, 950
• A. Goobar et al, (2000), The acceleration of the Universe: measurement of cosmological parameters from Type Ia supernovae, Physica Scripta, T85, 47.
• Perlmutter S. et al (1999) "Measurements of Omega and Lambda from 42 High-z Supernovae", ApJ, 517, 565
• Perlmutter S. et al, (1998) "Discovery of a supernova explosion at half the age of the Universe and its cosmological implications", Nature 391, 51.
• Perlmutter S. et al (1997) "Measurement of the cosmological parameters Omega and Lambda from the first 7 supernovae at z>0.35", ApJ, 483, 565
• R. Pain, I. Hook, S. Perlmutter, et al., (1996) , The Type Ia supernova rate at z~0.4, Astrophysical Journal, 473, 356
• Supernova 2001ay in IC 4423, Circular 7612, P.Nugent, G.Aldering, I.Hook, S.Perlmutter, L.Wang
• Supernovae 1999bi, 1999bj, 1999bk, 1999bl, 1999bm, 1999bn, 1999bo, 1999bp, 1999bq, Circular 7136, Supernova Cosmology Project.

Allocations:

Reference	Time	% Useful	Comment
ESO VLT 2003A	80.0 hours		French + other European collaborators time on FORS1 (VLT) for CFHTLS SN followup; 160 hr allocated in 2003B, plus more time guaranteed in 2004A and B. The PI is R. Pain.
Gemini 02A/B	10.0 nights	95	"Gemini Deep Deep Survey" (Abraham, McCarthy, Carlberg et al) [includes ~5 nights science verification]
Magellan	12.0 nights	90	"Spectroscopy of Las Campanas Survey IR Galaxies" (McCarthy, Carlberg et al)
Gemini 02A	14.0 hours	75	"Star formation around High z QSO's" (Pritchet, Hartwick, Carlberg et al). Paper in preparation.
GN2002B-Q-36	23.0 hours	0	Simard PI - HDF N disk kinematics. No data taken due to heavy schedule of telescope shutdowns and instrument commissioning.
CFHT-02A-C14	10.0 nights	70	Stetson PI - Search for Planetary Transits in NGC6791. Data reduction in progress.
GN2001A-Q-10	12.0 hours	50	This was a joint proposal with GN2001A-Q-16 (submitted to the U.S. TAC) to observe distant supernovae with NIRI. Both were ranked highly and the full amount of requested time (35hrs) was awarded by the respective TACs. Because of cancellation of the queue this program was not carried out in queue mode. However it was used as a test program for NIRI SV (broadband imaging mode with the f/6 camera). About 12 hours of useful data were obtained, approximately half of our original request (when overheads are taken into account). We intend to obtain a final reference image for this SN with NIRI in semester 02B.
GN2002A-Q-30	12.0 hours		Hook PI. This was a joint proposal with GN2002A-Q18 (submitted to U.S. TAC) for GMOS observations of distant supernovae. Some data was acquired and a paper is in preparation.
GN2002A-Q-31	12.0 hours		Hook PI. This was a joint proposal with GN2002A-Q37 (submitted to U.S. TAC) for NIRI observations of distant supernovae. Some data obtained. Paper in preparation
GN2002A-Q-75	6.5 hours		Hook PI. This was a joint proposal with GN2002A-Q9 (submitted to Candian TAC) for GMOS spectroscopy of z>5 QSO candidates. Program completed and paper in preparation.

Proposal Contents