Loading in 5 sec....

The Carnegie Supernova Project PowerPoint Presentation

The Carnegie Supernova Project

- 135 Views
- Uploaded on
- Presentation posted in: General

The Carnegie Supernova Project

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Wendy Freedman

CarnegieObservatories

Cosmology 2007

San Servolo, Italy

August 30, 2007

HST ACS data

Knop et al. 2003

Riess et al. 2004

Astier et al. 2006

Wood-Vasey et al. 2007

WLF et al. 2007

- Reduce systematics (reddening, calibration, K-corrections…)
- I-band restframe Hubble diagram
=> observations in the near-IR (>1m)

“Y” , J bands

(To date only UBV restframe…)

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

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/

High z:

Low z:

- CFHT Legacy Survey
- ESSENCE

- LOTOSS (KAIT)
- SN Factory

Intermediate z:

- SDSS-II

CSP followup and collaboration

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)

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

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

Low z

supernovae

Examples of CSP Low-z Light Curves

- SN 2006X
- NGC 4321
- (M100)
- Type Ia
- Spectra from
- du Pont and
- Magellan /
- LDSS2

SN2006X

Nidia Morell

Magellan High-z IR Observations: Two Examples

d149wcc4_11 (ESSENCE)

z ~ 0.3

c040117-14 (CFHT Legacy)

z ~ 0.6

Target

Template

Difference

SNLS

SDSS-II

ESSENCE

- 58 SN Ia
- as of 3/07
- 41 with
- templates
- 16 with
complete

reductions,

reddenings

Number

Redshift 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

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

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

*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

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**

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

*PRELIMINARY*

maximum

likelihood

CSP+BAO:

M = 0.3 ± 0.1

w = -0.9 ± 0.2

95% confidence

- Assumption:
- flat universe

W = P /

0.5 seeing

HST 1.5m

GMT AO

SNe studies are limited by confusion

GMT AO will address this

GMT Science

Working

Group

--P. McCarthy

- 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

- Australia
- Carnegie Observatories
- Harvard University
- Smithsonian Astrophysical Observatory
- Texas A&M University
- University of Arizona
- University of Michigan
- University of Texas, Austin
- + …OTHERS TBD

- 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