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The Carnegie Supernova Project. Wendy Freedman Carnegie Observatories Cosmology 2007 San Servolo, Italy August 30, 2007. State of the Art (2007): Type Ia Supernovae. HST ACS data. Knop et al. 2003. Riess et al. 2004. Astier et al. 2006. Wood-Vasey et al. 2007. WLF et al. 2007.

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The carnegie supernova project

The Carnegie Supernova Project

Wendy Freedman

CarnegieObservatories

Cosmology 2007

San Servolo, Italy

August 30, 2007


State of the art 2007 type ia supernovae

State of the Art (2007): Type Ia Supernovae

HST ACS data

Knop et al. 2003

Riess et al. 2004

Astier et al. 2006

Wood-Vasey et al. 2007

WLF et al. 2007


Carnegie supernova project primary goals

Carnegie Supernova Project: Primary Goals

  • Reduce systematics (reddening, calibration, K-corrections…)

  • I-band restframe Hubble diagram

    => observations in the near-IR (>1m)

    “Y” , J bands

    (To date only UBV restframe…)


Carnegie supernova project

Carnegie Supernova Project

Swope 1-meter

Dupont 2.5-meter

Magellan 6.5-meter

Low z:

High z:

  • u’BVg’r’i’YJHKphotometry

  • 2.5-meter spectroscopy

  • YJ photometry

  • Magellan 6.5-meter

  • ~100 SNe Ia at completion

  • observations near max

  • 0.2 < z < 0.8

  • C40 9 month campaigns

  • over 5 years (1350 nights)

  • densely sampled photometry

  • and spectroscopy 0 < z < 0.1

  • 100 SNe Ia, 100 SNe II


Carnegie supernova project csp

Carnegie Supernova Project (CSP)

Chris Burns

Carlos Contreras

Gaston Folatelli

Wendy Freedman (PI, High z)

Mario Hamuy

Barry Madore

Nidia Morell

Eric Persson

Mark Phillips (PI, Low z)

Miguel Roth

Nick Suntzeff

Pamela Wyatt

Collaborators:

Ray Carlberg, Chris Pritchet, Mark

Sullivan, Kathy Perrett, Andy

Howell (CFHT SN Legacy)

Alex Filippenko, Weidong Li (LOSS)

Nick Suntzeff (ESSENCE)

Josh Friemann, Masao Sato (SDSS-II)

Dan Kelson, Eric Hsiao

http://www.ociw.edu/csp/


Csp collaborations

CSP Collaborations

High z:

Low z:

  • CFHT Legacy Survey

  • ESSENCE

  • LOTOSS (KAIT)

  • SN Factory

Intermediate z:

  • SDSS-II

CSP followup and collaboration


Carnegie supernova project systematics

Carnegie Supernova Project: Systematics

Minimize effects due to:

  • Galactic reddening

  • Host reddening

  • Supernova Dust

  • Reddening

  • K-corrections

  • Environment

  • Calibration**

Overview: WLF 2005, astro-ph/0411176

Nugent et al (2002)


1 galactic extinction law

1. Galactic Extinction Law

AU / E(B-V)= 4.9

U

AB / E(B-V)= 4.1

B

V

AI / E(B-V) = 1.7

I

R V = AV / E(B-V)

Cardelli, Clayton and Mathis 1989


2 improved k corrections

2. Improved K-corrections

Eric Hsiao

Univ. Victoria

astro-ph 0703529

Thesis:

Improvement to

Standard (Nugent)

K-corrections

New spectra, at

many epochs and

including i-band

coverage (including

CSP low-z data).

CSP {

Ca triplet


Csp low z targets

CSP Low z Targets

Low z

supernovae


The carnegie supernova project

Examples of CSP Low-z Light Curves


Carnegie supernova project1

Carnegie Supernova Project

  • SN 2006X

  • NGC 4321

  • (M100)

  • Type Ia

  • Spectra from

  • du Pont and

  • Magellan /

  • LDSS2

SN2006X

Nidia Morell


The carnegie supernova project

Magellan High-z IR Observations: Two Examples

d149wcc4_11 (ESSENCE)

z ~ 0.3

c040117-14 (CFHT Legacy)

z ~ 0.6

Target

Template

Difference


Carnegie supernova project high z

Carnegie Supernova Project: High z

SNLS

SDSS-II

ESSENCE

  • 58 SN Ia

  • as of 3/07

  • 41 with

  • templates

  • 16 with

    complete

    reductions,

    reddenings

Number

Redshift z


Carnegie supernova project high z1

Carnegie Supernova Project: High z

i’-band

light curves: low z

  • High z:

  • Observe pre-

  • maximum

  • Follow 3-7

  • epochs

  • Less than 10

    days after

    maximum

  • Gaps less than

  • 5 days

1st peak

2ndpeak

Redshift


Carnegie supernova project high z2

Carnegie Supernova Project: High z

J

z = 0.59

z = 0.62

Y

z = 0.32

gri : SDSS-II

Y: Magellan

.

i

r

Y

z = 0.52

z = 0.43

i

.

z = 0.62

ri: SNLS

YJ: Magellan

r

g

C. Burns


The carnegie supernova project

Carnegie Supernova Project: High z

  • Use optical data to

  • determine decline

  • rates (m15(B) ).

  • Use both optical and

  • near-IR data to

  • solve for reddening.

  • Use YJ light curves

  • to solve for the

  • distance modulus.

YJ

.

Template light curves from Prieto et al. (2006) nearby sample


Carnegie supernova project high z3

Carnegie Supernova Project: High z

*PRELIMINARY*

16 Type Ia

supernovae

First I-band

Hubble diagram

at z > 0.07

Riess et al. gold

Astier et al.

Magellan

  • small scatter at I

  • better than current

  • low-z sample

Redshift


Carnegie supernova project fisher matrix constraints on w o and

Carnegie Supernova Project: Fisher-Matrix Constraints on wo and

Current CSP

(50 SN Ia)

100 SN Ia

150 SN Ia

Stage I SNLS

(71 SN Ia)

Astier et al

(2006)

Chris Burns

WMAP plus H0 Key Project priors

95% confidence contours

CSP Allows for k-correction and color errors**


Carnegie supernova project fisher matrix constraints on w o and1

Carnegie Supernova Project: Fisher-Matrix Constraints on wo and

Current CSP

(50 SN Ia)

100 SN Ia

150 SN Ia

Stage II SNLS

(700 SN Ia)

Chris Burns

WMAP plus H0 Key Project priors

95% confidence contours


Carnegie supernova project high z4

Carnegie Supernova Project: High z

*PRELIMINARY*

maximum

likelihood

CSP+BAO:

M = 0.3 ± 0.1 

w =  -0.9 ±  0.2

95% confidence

  • Assumption:

  • flat universe

W = P / 


Sne ia the gmt

SNe Ia & The GMT

0.5 seeing

HST 1.5m

GMT AO

SNe studies are limited by confusion

GMT AO will address this

GMT Science

Working

Group

--P. McCarthy


The giant magellan telescope gmt

The Giant Magellan Telescope (GMT)

  • Alt-az structure

  • Seven 8.4-m primary mirrors

    • Cast borosilicate honeycomb

    • 25.3-m enclosed diameter

    • 24.5-m diffraction equivalent

    • 21.5-m equivalent aperture

  • 3.2-m adaptive Gregorian secondary mirror


Gmt institutions

GMT Institutions

  • Australia

  • Carnegie Observatories

  • Harvard University

  • Smithsonian Astrophysical Observatory

  • Texas A&M University

  • University of Arizona

  • University of Michigan

  • University of Texas, Austin

  • + …OTHERS TBD


Summary

Summary

  • First restframe I-band Hubble diagram for 0.2 < z < 0.7

  • Dispersion lower than for UBV

  • Lower sensitivity to reddening

  • Improved K-corrections

  • Preliminary Results: w = -0.9§ 0.2 (95% confidence)

  • Final sample 4-5 times greater

    • Low redshift : tests of systematics

    • High redshift: I-band Hubble diagram

    • “Local” calibration for JDEM


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