The carnegie supernova program
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The Carnegie Supernova Program. Zwicky Symposium Saturday, January 17, 2004 Carnegie Observatories. Type Ia Supernovae for Cosmology. Advantages: small dispersion single objects (simpler than galaxies) can be observed over wide z range . Challenges: dust (grey dust)

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The carnegie supernova program

The Carnegie Supernova Program

Zwicky Symposium Saturday, January 17, 2004

Carnegie Observatories


Type ia supernovae for cosmology

Type Ia Supernovae for Cosmology

Advantages:

  • small dispersion

  • single objects (simpler than galaxies)

  • can be observed over wide z range

  • Challenges:

  • dust (grey dust)

  • chemical composition

  • evolution

  • photometric calibration

  • environmental differences


Carnegie supernova project

Carnegie Supernova Project

  • Infrared observations of Type Ia & II supernovae

  • High and low z (0 < z < 0.8)

    : improved constraints on w

  • I-band Hubble diagram

CSP coI’s:

Gaston Folatelli

Wendy Freedman

Mario Hamuy

Barry Madore

Nidia Morell

Eric Persson

Mark Phillips

Nick Suntzeff

Pamela Wyatt

Ray Carlberg (CFHT Legacy)

Alex Filippenko, Weidong Li (KAIT)

Nick Suntzeff (ESSENCE)


Carnegie supernova project1

Carnegie Supernova Project

Why an I-band Hubble diagram?

  • Advantages:

    - dust

    - chemical composition

    - low dispersion

    => reduce systematics


Barris et al 2003

Barris et al. (2003)

unbinned

binned (median)


Overview of carnegie supernova project

Overview of Carnegie Supernova Project

Low z:

Swope 1-meter (C40)

  • u’BVr’i’ CCDphotometry

  • YJHIR array

  • RAPID SWITCHING (< 15min)

  • C40 9 month campaigns over 5 years

  • densely sampled (every 2nd night) photometry

  • SNIa and SNII


Overview of carnegie supernova project1

Overview of Carnegie Supernova Project

Dupont 2.5-meter

  • u’BVr’i’CCDphotometry

  • YJHIR array

  • spectroscopy

  • densely sampled photometry

  • and spectroscopy 0 < z < 0.2

  • well-determined k-corrections

  • SNIa and SNII


Overview of carnegie supernova project2

Overview of Carnegie Supernova Project

High z:

Magellan 6.5-meter

  • RIYJ photometry

  • Magellan spectroscopy

  • ~200 nights over 5 years

  • ~200 SNIa

  • 0.2 < z < 0.8


Overview of carnegie supernova project3

Overview of Carnegie Supernova Project

Swope 1-meter (C40)

Dupont 2.5-meter

Magellan 6.5-meter

Low z:

High z:

  • u’BVr’I’YJHphotometry

  • Dupont spectroscopy

  • r’i’YJ photometry

  • Magellan spectroscopy

  • ~200 nights over 5 years

  • ~200 SNIa

  • 0.2 < z < 0.8

  • C40 9 month campaigns

  • over 5 years

  • densely sampled photometry

  • and spectroscopy 0 < z < 0.2

  • SNIa and SNII


Carnegie supernova project2

Carnegie Supernova Project

  • Goals:

  • minimize systematics

  • accurate reddenings,

  • K-corrections

  • H0 (H-band observations

  • for Cepheids + SNIa)

  • WL

  • peculiar flows

  • physics of SNI and II

Magellan


Carnegie supernova project3

Carnegie Supernova Project

Nearby supernovae:

  • ~30 observed to date

  • UBVRIJHK light curves

  • excellent sampling

Krisciunas et al. (2002)

SN2001el


Carnegie supernova project4

Carnegie Supernova Project

  • decline rate versus magnitude

  • BVIH

  • H-band promising as

  • distance indicator

Mark Phillips et al.


Carnegie supernova project5

Carnegie Supernova Project

H-band Hubble diagram

Log velocity (km/sec)

Distance Modulus (mag)

Krisciunas et al.


Ongoing supernova searches

Ongoing Supernova Searches

High z:

Low z:

  • CFHT Legacy Survey :

  • ugriz light curves

  • CFHT MegaCam

  • 2000 SN over 5 years

  • 0.1 < z < 1

  • LOTOSS (KAIT) :

  • UBVRIlight curves

  • Lick

  • 0 < z < ~0.15

  • ESSENCE :

  • VRIlight curves

  • CTIO 4m Mosaic Imager

  • 200 SN over 5 years

  • 0.15 < z < 0.75

  • SN Factory:

  • spectophotometry, UH

  • 3200 – 10000 Ao

  • NEAT, Palomar

  • ***E.g., redshifts posted on web within 2 days!!!!!


Cfht legacy survey success

CFHT Legacy Survey : Success!

CFHT Legacy candidates: September 03

  • finding ~ 15 SN1a

  • per month

  • generally finding

  • ~ 2 mag before

  • peak

  • collaboration with

  • Carlberg et al.

  • followup SN1a

  • 0.2 < z < 0.8

  • at RIYJ


Cfht legacy survey success1

CFHT Legacy Survey : Success!

CFHT Legacy candidates: September 03

REFERENCE

DIFFERENCE

  • Try to catch supernovae on

  • the rise for followup.

  • IAB ~ 22 – 25 mag


The carnegie supernova program

Followup Spectroscopy: ESSENCE & CFHTLS

  • VLT

  • Gemini

  • Magellan

e.g.:

SNIa

  • SN Ia spectrum

  • z = 0.54

  • t = 20 min

  • VLT FORSI


Panic magellan 6 5 meter ir imager

PANIC: Magellan 6.5-meter IR Imager

Antennae

  • 1024 x 1024 array

  • 1 – 2.5 micron imager

  • 2’ x 2’ FOV

  • 0.125 “/pixel

PANIC: Eric Persson


Panic magellan ir imager

PANIC: Magellan IR Imager

  • 35 nights of

  • Magellan time

  • November 03

  • through March 04

  • optical r’I’imaging

  • near-IR YJimaging

  • optical spectroscopy


Imacs inamori magellan areal camera and spectrograph

IMACS: Inamori Magellan Areal Camera and Spectrograph

  • 2 cameras

  • f/4 : 15’ FOV

  • f/2 : 30’ FOV

  • 8192 x 8192 CCD array

  • installed August, 2003

  • Followup spectroscopy

  • RI photometry

Alan Dressler, Bruce Bigelow


Magellan snia observations

Magellan SNIa Observations

z ID I-mag Discovery

0.20 e132.wcc1_7 21.3 Essence 0.30 d149.wcc4_11 19.5 Essence 0.30 e108.wdd8_4 21.8 Essence

0.55 c031022-02 23.0 Legacy 0.69 c031217_23 23.9 Legacy


First magellan panic images

First Magellan PANIC Images

November 3, 2003

J-band

Y-band

ESSENCE SNIa : z = 0.33 (d149) 36-minute dithered exposures


First magellan panic images1

First Magellan PANIC Images

November 3, 2003

J-band

Y-band

CFHT SNIa : z = 0.55 (1022) 36-minute dithered exposures

(total exposures 2 hours per filter)

Stay tuned…


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