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Spectroscopy program of The SuperNovae Legacy Survey

Filiol Mélanie3rd year PhD

Supervisors : Mazure Alain & Basa Stéphane

Laboratoire d’Astrophysique de Marseille, France

On behalf of the SNLS Collaboration*

* Complete member listhttp://cfht.hawai.edu/SNLS

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Motivations

• Fundamental complement to the photometric observations done by the CFHT Legacy Survey

• Spectroscopic program– Identify supernova type– Measure the redshift

After 5 years of SNLS program, 700 SNe Ia discovered Measure cosmological parameters

with a precision w ~ 0.1

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Observations - Time Allocation• VLT:

– Large Program on the ESO FORS1.– 60 hr/semester, 4 semesters allocated.– Observation in Service Mode.– From October 2005, new large program on FORS1 and FORS2 - Mode MOS.

• GEMINI North and South: – Joint Canadian/UK/US proposal – 60 hr/semester on GMOS.– Observation in Service Mode.

• KECK: – 4 nights/yr on LRIS.– Observation in Service Visitor

Coordinator : S. Basa

Coordinator : I. Hook

Coordinator : M. Sullivan

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Bright (mag>~23.0) SNe sent to VLT : smaller overheads Faint SNe equitably sent to VLT and Gemini VLT replaced by Keck for D3 field

Coordination between the telescopes

D4

D2

D1

D3

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Observations with VLT Large Program

Target of Opportunity : A precise observation date does not have to be

provided in advance Observations are submitted as soon as a candidate

is discovered at CFHT Our observation have priority and are conducted in

Service Mode

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• When a trigger is available, observations are activated by web form : finding charts, very precise instructions have to be defined (slit width, grism, moon phase, weather conditions ….)

• If constraints are fulfill, observations are performed during the night

• Data are available about 12 hours after in Garching

• Preprocessing of the data is done with the FORS pipeline, customized for the SNLS use

The delay between the submission of an observation and its analysis is about 24 hours.

Procedure VLT

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Supernova Identification

SN Identification is based on the ² fitting of our spectrum with a model (local SN + local galaxy)

: fraction of supernova S : fraction of galaxy G

Linear combinations of a galaxy template and a supernova template spectrum (library representative SN and galaxy templates)

² = Σ

obsmin =

obs

max

{ }Sobs() – S(rest(1+z)) + G(rest(1+z))

obs()

²

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Results of June 2003 to July 2005Telescopes Candidates

VLT Gemini Keck Total/SN

Ia 95 82 36 213 (68%)

Ibc 4 2 1 7 (2%)

I 12 7 - 19(6%)

II 16 1 3 20(7%)

AGN 11 - - 11(3%)

Not Idenfied 17 21 7 45(14%)

Total / Telescope 155 113 47 315

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Redshift determinationSNLS-04D1dc and host galaxy Texpo = 1500sec

Host galaxy 04D1dc at z=0.211 Texpo = 1500sec

1. Host galaxy spectrum extracted

separately

2. Galaxy lines identified in supernova spectrum

SNLS-03D4at and host galaxy at z = 0.633 Texpo = 1500sec

OR

OR

3. No host and no galaxy lines in spectrum redshift estimated by the fitting template spectra

Basa S., Filiol M. & SNLS CollaborationSubmitted

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Redshift resolution

Resolution of ~ 1%

Redshift distribution of SN Ia

SN Ia & Ia ?

SN Ia?

Basa S., Filiol M. & SNLS CollaborationSubmitted

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Age resolution

SN Ia & Ia ?

SN Ia?

Age distribution of SN Ia

Age

from

the

spec

trum

fit (

day,

from

the

LC m

ax)

Age from the LC (day, from the LC max)

Basa S., Filiol M. & SNLS CollaborationSubmitted

SN Ia?SN Ia

Precision of ~ 3 days

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Host galaxies

Host galaxy identified by the test ² when we are not extracting thehost spectrum.3 Groups :

1. Elliptic, Bulge, S02. Early Spiral Sa, Sb3. Late Spiral Sc and Starburst

SNLS 1st year Study Mark Sullivan (2003)* RSAC+

Group I 25.5 % 28.5 % 28.9 %

Group II 32.7 % 25.7 % 35.6 %

Group III 41.8 % 45.7 % 35.5 %

* MNRA, 340, 1057 The Hubble diagram of type Ia supernovae as a function of host galaxy morphology+ Glazebrook (1995), Abraham (1996), Lauger (2005 – astroph0509500) etc. …

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Conclusion

• 213 SN Ia discovered in 2 years

• Additional sciences– The Hubble diagram as a function of host galaxy morphology– UV emission– Study evolution SN Ia

Hubble Diagram (SNLS 1st year)m = 0.263 13 ± 0.042 w = -1.023 ± 0.090

Cf. Talk D. Fouchez

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SNLS Collaboration members http://snls.in2p3.fr/people/snls-members.html

• France : – LAM : S.Basa, A. Mazure, Filiol Mélanie (PhD) …– CCPM : C. Tao, D. Fouchez, P. Ripoche (PhD) …– LPNHE, Paris : R. Pain, P. Astier, C. Balland, S. Baumont (PhD) …– Observatory Meudon : M. Mouchet, A. Darbon …– CEA : J. Rich, N. Palanque-Delabrouille …

• Canada :– University Toronto : R. Calberg, M. Sullivan, A. Howeel, K. Perett …– University Victoria : C. Pritchet, D. Balam …

• UK :– University Oxford : I. Hook, J. Bronder (PhD) …

SNLS Papers :• The SNLS : Spectroscopic Identification of SN with the ESO/VLT – 1st result-, S.

Basa, M. Filiol & al. (submitted)• The SNLS : Measurement of m, and w from the 1st year data set, P. Astier & al. (submitted A&A)• Gemini spectroscopy of SN from SNLS, A. Howell & al. (submitted)• Photometric selection oh high-redshift type Ia supernovae candidates. M. Sullivan & al. (submitted)

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Finding Charts

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Test ², Graphical User InterfaceGregory Sainton

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Supernovae Ia

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VLT StatisticsJune 2003 – November 2004

Candidate type Number Fraction

Ia 65 58 %

Ibc 3 3 %

I 8 6 %

II 15 13 %

AGN 11 10 %

Not Identified 11 10 %