The Carnegie Supernova Project (CSP): Latest Results SN2006X

Outline of Talk What is the CSP? General statistics Low-z SNe Ia First BVugriYJHK data set High-z SNe Ia i band Hubble Diagram to z ~ 0.7 Type Ib/Ic SNe SN 2007Y Making the Data Available SN2008aw

People Other collaborators Alex Filippenko (UC Berkeley) Weidong Li (UC Berkeley) Ray Carlberg (Univ. Toronto) Josh Frieman (Chicago/Fermi Lab.) Darren Depoy (Ohio St.) Jose Luis Prieto (Ohio St.) OCIW Wendy Freedman P.I. High-z Eric Persson Barry Madore Chris Burns (postdoc) Pamela Wyatt (OCIW/IPAC) David Murphy Texas A&M Nick Suntzeff Kevin Krisciunas Lifan Wang Chile Mark Phillips (OCIW/LCO) P.I. Low-z Mario Hamuy (U. Chile) Original P.I. Low-z Max Stritzinger (OCIW/LCO, postdoc) Gastón Folatelli (U. Chile, postdoc) Miguel Roth (OCIW/LCO) Nidia Morrell (OCIW/LCO) Alejandro Clocchiatti (PUC) Wojtek Krzeminski (OCIW/LCO retired) Carlos Contreras (former research assistant) Sergio Gonzalez (research assistant) Luis Boldt (research assistant) Francisco Salgado (research assistant)

Chilean Students Involved with the CSP Felipe Olivares (U. Chile) Alejandra Molina (U. Chile) Luis Boldt (PUC) Felipe Murgas (U. Chile) María José Maureira (U. Chile) Fernando Becerra (U. Chile) and Carlos Contreras (PUC)

Obtain high-quality, gap-free BVugriYJHK light curves and optical spectrophotometry of: ≥100 nearby (z<0.07) Type Ia supernovae ≥100 nearby (z<0.05) Type II supernovae ≥20 nearby (z<0.05) Type Ibc supernovae Refine methods for obtaining distances to Type Ia and Type II supernovae Provide a new fundamental reference for observations of high-z supernovae Gain insight into the progenitors and explosion mechanisms of supernovae Low-z CSP Goals

Telescopes/Instruments Optical (u’BVg’r’i’) Photometry: Las Campanas Swope 1-m telescope + CCD Infrared (YJsHKs) Photometry: Las Campanas Swope 1-m telescope + RetroCam (YJH) Las Campanas du Pont 2.5-m telescope + WIRC (YJHK) Las Campanas Baade 6.5-m telescope + PANIC (YJHK) High-z Optical ( μ m) Spectroscopy: Las Campanas du Pont 2.5-m telescope + WFCCD (or Modspec, or B&C) Magellan Clay 6.5-m telescope + LDSS-3 (or IMACS) CTIO 1.5-m telescope + Cassegrain Spectrograph (service mode) ESO NTT+EMMI Swope 1-mDu Pont 2.5-mMagellan 6.5-m } Low-z workhorse

Observing Campaigns One 9-month campaign per year from September-May ~230 nights per campaign at Swope 1-m ~80 nights per campaign at duPont 2.5-m A few nights of Magellan time A total of five campaigns will be carried out The final campaign will end in this coming May!

Filters BV + ugri + YJHK s

Sources for Supernovae LOSS + many others And, beginning in 2008, CHASE!

Statistics After 4 Campaigns Through 4 campaigns, observations have been obtained of 286 SNe. Of these, a full set of follow-up observations has been obtained for 194 (67%)

Statistics (cont.) In general, no SN is followed for less than 1 month Median coverage for SNe Ia is ~70 days Coverage of SNe II is intentionally longer in order to follow them until end of plateau phase

Statistics (cont.) Through the first 4 campaigns, a total of 1,190 spectra of 211 SNe have been obtained Classifications reported to IAUC for 101 SNe Most spectra obtained at Las Campanas Observatory Additional spectra obtained with ESO NTT, and in collaboration with Darren Depoy & Jose Luis Prieto For the SNe selected for follow-up during the first three campaigns, average sampling frequency was ~1 spectrum per 9-10 days This has been improved during the last two campaigns through a collaboration with the Millennium Center for Supernova Studies (Mario Hamuy, PI)

SNe Ia Observed in Campaigns 1 & 2

Low-z SNe Ia: Redshift Range by Type ~75% of SNe Ia lie in Hubble flow (z > 0.015) Median redshift of SNe II is less than that of SNe Ia since SNe II are intrinsically less luminous; nevertheless, more than half of SNe II lie in Hubble Flow SNe Ib/Ic are much less common, and also relatively nearby due to their low luminosities

Low-z SNe Ia: Optical Light Curves  m 15 (B)

Low-z SNe Ia: Optical Light Curves

Low-z SNe Ia: Range of Decline Rates

Low-z SNe Ia: Near-Infrared Photometry Near-IR (NIR) photometry is a key component of the Low-z CSP Goal is to obtain NIR observations of most SNe at a cadence of one set of YJH observations per 3-5 days This goal was not achieved for the first CSP campaign (due to delays in completing the Retrocam imager for the Swope 1 m telescope) The 2nd, 3rd, and 4th campaigns have achieved this goal, resulting in some of the best NIR light curves of SNe Ia, SNe Ib/c, and SNe II ever obtained NIR light curves will be obtained for > 80% of SNe

Low-z SNe Ia: Light Curve Templates

CSP i’ light curvesi’ templates

Low-z SNe Ia: Light Curve Shapes The secondary maximum is observed from the r to the K bands, and is strongest in the Y band (1.03 µm) The time between the primary and secondary maxima is typically ~30 days; the secondary maxima occurs earlier for faster-declining events

Commercial Break For many more results on the CSP sample of Low-z SNe, don’t miss Gaston Folatelli’s talk this afternoon!

From: Astier et al Measuring Dark Energy with SNe Ia: Current State of the Art From: Wood-Vasey et al SN Legacy SurveyESSENCE

From: Kowalski et al Current State of the Art (cont.) Limits on w and Ω M Limits on Ω  and Ω M Ω  = ± (stat) ± (sys) w = ± (stat) ± (sys)

CSP High-z SNe Ia At the redshift range (0.3 < z < 1.0) observed by SNLS and ESSENCE, the light curves correspond to the UBV bands in the rest system To minimize errors due to reddening, the Carnegie Supernova Project (CSP) has been working to produce the first rest system i band Hubble diagram over the redshift range (0.01 < z < 0.7) This is a completely new and independent data set! z = 0.35z = 0.63

CSP High-z SNe Ia: Sources of Supernovae

SN3241 Discovered by SDSS z = 0.25 D149wcc4-11 Discovered by ESSENCE z = D2bt Discovered by SNLS z = CSP High-z SNe Ia: Host Galaxy Subtractions

z = 0.25 Y filter z = 0.30 Y filter z = J filter CSP High-z SNe Ia: Light Curves

The First Rest System i Band Hubble Diagram to z ~ 0.7

Current State of the Art (cont.) Limits on w and Ω M Limits on Ω  and Ω M Premliminary results: Ω  = 0.76 ± 0.08 (stat) ± 0.08 (sys) w = ± 0.08 (stat) ± 0.08 (sys)

SN 2007Y: A Type Ic SN The CSP observes ALL nearby SNe caught at or before maximum Max Stritzinger has been working on CSP data obtained of SN 2007Y, a type Ib/c SN This SN was also observed with Swift in the UV and X-Rays These data are among the best ever obtained for a SN of this type

SN 2007Y: Light Curves CSP + Swift observations Late-time photometry obtained with ESO VLT

SN 2007Y: Bolometric Light Curve

SN 2007Y: Optical Spectra Comparison with SN 2005bf CSP Spectra of SN 2007Y

SN 2007Y: Nebular Phase Spectroscopy IIb Ib Spectrum obtained with Magellan 6.5 m Clay Telescope

SN 2007Y: Conclusions Ejected mass of 56 Ni ~ 0.6 solar masses (bolometric light curve + nebular phase spectra) Ejected oxygen mass ~ 0.2 solar masses (nebular phase spectra) Total ejected mass below 4500 km s -1 was 0.42 solar masses (nebular phase spectra) ZAMS mass of progenitor ~13 solar masses (nebular phase spectra) Explosion energy ~ erg (light curves + optical spectra) SN 2007Y among the least energetic SN Ib studied to date

Making the Data Available In early-February, we expect to submit three papers: A first data paper presenting optical and NIR photometry for 35 Low-z SNe Ia An accompanying analysis paper of these data, and A third paper presenting rest system i band light curves of 35 High-z SNe Ia Next week, a paper on the type Ib SN 2007Y will also be submitted Data will be made available immediately thereafter to those who are interested via a special web site We will also work with IPAC to make the data permanently accessible via NED

Refereed Publications Including CSP Data 1)Hamuy, M., et al. 2006, PASP,118, 839, “The Carnegie Supernova Project: The Low- Redshift Survey” � 2)Folatelli, G., et al. 2006, ApJ, 641, 1039, “SN 2005bf: A Possible Transition Event between Type Ib/c Supernovae and Gamma-Ray Bursts” 3)Phillips, M. M., et al. 2007, PASP, 119, 360, “The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations?” 4)Hsiao, E. Y., et al. 2007, ApJ, 663, 1187, “K-corrections and Spectral Templates of Type Ia Supernovae � ” 5) �� Taubenberger, S., et al. 2008, MNRAS, 385, 75, “The Underluminous Type Ia Supernova 2005bl and the Class of Objects Similar to SN 1991bg � ” Published: To be submitted soon: 1)Contreras, C., et al. 2009, “The Carnegie Supernova Project: First Photometry Data Release of Type Ia Supernovae” � 2)Folatelli, G., et al. 2009, “The Carnegie Supernova Project: Analysis of the First Sample of Low-Redshift Type Ia Supernovae” 3)Freedman, W. L., et al. 2009, “The Carnegie Supernova Project: First Near-Infrared Hubble Diagram to z ~ 0.7” 4)Stritzinger, M., et al. 2009, “The He-Rich Core-Collapse Supernova 2007Y: Observations from X-Ray to Radio Wavelengths”