Infrared Light Curves of Type Ia Supernovae with PAIRITEL · PDF fileInfrared Light Curves of Type Ia Supernovae with PAIRITEL Andrew Friedman ... Krisciunas et. al 2007, ApJ, 133,

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Infrared Light Curves ofInfrared Light Curves ofType Type Ia Ia Supernovae withSupernovae with

PAIRITELPAIRITEL Andrew Friedman (Harvard-CfA)

www.cfa.harvard.edu/oir/pairitel/ptel_sn.shtmlwww.www.pairitelpairitel.org.org, , afriedmanafriedman@@cfacfa..harvardharvard..eduedu

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Research Collaborators

CfA Supernova GroupRobert Kirshner, StephaneBlondin, Andrew Friedman,Maryam Modjaz, PeteChallis, W. MichaelWood-Vasey, MalcolmHicken (Harvard)

PAIRITEL ProjectJoshua Bloom, Dan Starr(UC Berkeley), CullenBlake, Emilio Falco, AndySzentgyorgi (Harvard),Mike Skrutskie (Virginia)

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Outline

1. Why Study SNe Ia in the near IR? Observations: Kirshner et. al 1973, Elias et. al 1981, Elias et.al 1985, Meikle 2000, Krisciunas et. al 2004, 2005, 2007 Theory: Hoflich et. al 1995, Wheeler et. al 1998, Pinto &Eastman 2000, Hoflich et. al 2002, Kasen 2006

2. PAIRITEL SN Project

3. Sample Light Curves

4. Future Work

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Advantages of Type Ia SNe in the NIR

• UBVRI SNe Ia are standardizable candles atthe ~0.18 mag level (MLCS2k2 method; Jha et.al 2005)

• JHK SNe Ia appear to be standard candles atthe 0.15-0.2 mag level or better (7-9% indistance), depending on the filter (Krisciunas et.al 2004, 2005)

• JHK LC’s show no decline rate relations inthe NIR (From 22 JHK SNe Ia) (Krisciunas et.al 2004, 2005)

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Standard Candles in the NIR?

Absolute mags of Type Ia SNe at max. light vs. the decline rateparameter ∆m15 (B) show a lack of decline rate relations, smallintrinsic scatter ~ 0.15-0.2 mag in JHK. (Hubble diagram right)

Krisciunas 2005 Krisciunas et. al 2004

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•JHK v.s. UBVRI observations have less systematicuncertainty due to dust extinction (AJHK < AV)(Cardelli, Clayton, & Mathis 1989)

•UBVRI + JHK → better determination of extinctionAv, distance (Krisciunas et. al 2007)

Advantages of Type Ia SNe in the NIR

0.1142174K0.1901587H0.2821250J1.000549VAλ/Avλ (nm)Band

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JHK Utility for Reddening

Krisciunas et. al 2007• Monte Carlo:Uncertainty indistance modulus(µ) vs. photometricaccuracy fordifferent filter sets.

• Not possible torecover µ moreaccurately than thephotometric limit(dashed line)

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Theoretical Models of NIR SNe Ia LC’s

•Theoretical models predict secondary maxima inIJHK ~30-35 days after explosion. (Also: Hoflich et. al1995, Wheeler et. al 1998, Hoflich et. al 2002)

Kasen 2006(sn2001el)Pinto & Eastman 2000(sn1992A)

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Theoretical Models of NIR SNe Ia

Intrinsicallybrighter SNeIa with more

56Ni have alater andrelatively

moreprominentsecondarymaxima in

IJHK.Kasen 2006

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1st peak in JHK → TypeIa SNe standard candlesat ≤ ~ 0.2 mag level,despite varying 56Ni mass.

Kasen 2006

Theoretical Models of NIR SNe Ia

Dots mark variation in 56Ni (0.4-0.9 Msun).

Best standard candle?1st H band peak,or J band minimumbetween peaks

mag of 1st peak

Lines are for 56Ni (0.4-0.9 Msun).

J band local min

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Outline

1. Why Study SNe Ia in the near IR?

2. PAIRITEL SN ProjectJosh Bloom, Cullen Blake, Dan StarrMaryam Modjaz, Michael Wood-Vasey

3. Sample Light Curves

4. Future Work

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Peters Automated InfraRed Imaging TELescope

• PAIRITEL 1.3m: the old 2MASS telescope at Mt.Hopkins, AZ• Roboticized by Josh Bloom, P.I. UC Berkeley,commissioned October 2004 (Bloom et. al 2006)• Autonomous, queue scheduled observing• Optimized for rapid Gamma-Ray Burst follow-up• ~20 science projects, including SNe follow-up

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PAIRITEL SN Project

Advantages• ~30% of time on a dedicated 1.3m robotic telescope• Simultaneous JHK observing• Homogeneous data set, well understood camera• Nightly observations → well sampled LC’s• Photometric calibration from 2MASS• Optical Data from Mt. Hopkins 1.2m, Spectra: 1.5m• Will more than double Krisciunas et al 2005, sample

Drawbacks• Follow up survey, wait for optical discovery, typing• Harder to catch 1st NIR LC peak. Typical T(Jmax)3-5 days prior to T(Bmax)

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www.cfa.harvard.edu/oir/pairitel/ptel_sn.shtml

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From Krisciunas et.al 2004, Table 1

N: # of epochsprior to t’=+10days (stretch time)

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Outline

1. Why Study SNe Ia in the near IR?

2. PAIRITEL SN Project

3. Sample Light CurvesPhotometry by Michael Wood-Vasey (plots by A.F.)ESSENCE/PAIRITEL photometry Pipeline: Michael Wood-Vasey, Maryam Modjaz, Armin Rest

4. Future Work

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Sample Light Curves: Excellent

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Sample Light Curves: Good

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Sample Light Curves: Fair

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Tominaga et al 2005

sn2006aj (grb060218)

Days after UT March 31 2005

Modjaz et. al in prep

•SN Ib/c ~20%of bolometricflux in NIR forhypernovae.

•Lends insightinto explosionmodels,GRB/SNconnection

sn2005bf

Sample UBVRIJHK Light Curves: Ib/c

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Outline

1. Why Study SNe Ia in the near IR?

2. PAIRITEL SN Project

3. Sample Light Curves

4. Future Work

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Future Work: Observations, Photometry

• Obtain Remaining Galaxy Template Images

• Re-Reduce Data at Berkeley - improvedmosaics, better sky subtraction

• Photometry of SNe Ia (NN2 method)

• Photometric Calibration (2MASS)

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Future Work: Science

•“The Absolute Brightness of Type Ia Supernovaein the Near Infrared from PAIRITEL”

•Perform Krisciunas et al analysis for our objects NIRHubble Diagrams

• Compare Krisciunas sample to ours (color terms,2MASS/Caltech CTIO/other filters)

• Test improvements in reddening measurements,distances w/ IR + Optical Data (Mt. Hopkins 1.2m)

•Impact on future space satellites (JDEM)

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• The Carnegie Supernova Project (CSP) Represents the mainsouthern hemisphere competition to the northern hemispherePAIRITEL Supernova Project / CfA Supernova Program

• Largely complementary set of nearby SNe in optical+NIR withsome number of overlap objects (Acad. Yr.: PTEL/CSP/overlap)For JHK: 04-05: 17/22/4, 05-06: 28/22/7, 06-07: 13/18/2

• They have kindly published SNe Light Curves w/o galaxytemplates here: http://csp1.lco.cl/~cspuser1/PUB/CSP.html

•Compare overlap SNe and global properties of low-z sample

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Conlusions• Type Ia SNe in NIR may be superior standard candles vs.optical (1st H peak, J minimum)

• Combined BVRIJHK data significantly reduces systematicerrors due to extinction, improves distance estimate errorsby a factor of ~3

•PAIRITEL SN project will further quantify this with ahomogenous, well sampled data set (~25-30 SNe Ia) morethan doubling published Krisciunas et. al 2005 sample. (Also complementary data from Carnegie SN Project)

• Future space satellites for cosmology, i.e. JDEM:DESTINY, SNAP (1.7µm), ADEPT, should seriouslyconsider NIR wavelength coverage out to ~2-6 µm to observeJHK rest frame (~1-2µm) for SNe at z~1-2.

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ReferencesBenford & Lauer 2006, Proc. Of SPIE, Vol. 6265 (DESTINY)Bloom et. al 2006, ASPC, 351, 751BCohen et. al 2003, ApJ, 126, 1090 (2MASS)Elias et al 1981, ApJ, 251, L13Elias et. al 1985, ApJ, 296, 379Freedman 2005, ASP Conf. Proc. Vol 339, p 50 (CSP)Hoflich et. al 1995, ApJ, 444, 831Hoflich et. al 2002, ApJ, 598, 791Kasen 2006, ApJ, 649, 939Kirshner et al 1973, ApJ, 180, L97Krisciunas et. al 2004, ApJL, 602, L81Krisciunas 2005, ASP Conf. Proc. Vol. 339, p75Krisciunas et. al 2007, ApJ, 133, 58Lauer 2005, New Astronomy Reviews, 49, 354 (DESTINY)Meikle 2000, MNRAS, 314, 782Modjaz et. al 2007 in prep.Pinto & Eastman 2000, ApJ, 530, 757Tominaga et. al 2005, ApJ, 633L, 97TWheeler et. al 1998, ApJ, 496, 908