near-ir diagnostics for sne
DESCRIPTION
Near-IR Diagnostics for SNe. Mark M. Phillips. Carnegie Observatories. Collaborators: K. Krisciunas ( CTIO /Carnegie ), N. Suntzeff ( CTIO ) M. Hamuy ( Carnegie ), E. Persson ( Carnegie ), W. Freedman ( Carnegie ), M. Roth ( Carnegie ) L. Germany ( ESO ). Outline of Talk: - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/1.jpg)
![Page 2: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/2.jpg)
Collaborators:
K. Krisciunas (CTIO/Carnegie), N. Suntzeff (CTIO)
M. Hamuy (Carnegie), E. Persson (Carnegie), W. Freedman (Carnegie), M. Roth (Carnegie)
L. Germany (ESO)
![Page 3: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/3.jpg)
Outline of Talk:
SNe Ia Morphology of NIR light curves Light curve templates Colors & Reddening Absolute magnitudes & Hubble diagram
SNe II A few words about Reddening Determinations
![Page 4: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/4.jpg)
Sources:
UBVRI: Suntzeff et al. (1999)
JHK: Mayya et al. (1998)Jha et al. (1999)
Hernandez et al. (2000)
UBVRIJHK Light Curves of a Typical SN Ia
Secondary maximum
Primary maximum
![Page 5: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/5.jpg)
SN m15(B)
• Secondary maximum occurs later for slower declining SNe
• Generally speaking, secondary maximum is stronger for slower declining SNe
![Page 6: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/6.jpg)
![Page 7: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/7.jpg)
![Page 8: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/8.jpg)
![Page 9: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/9.jpg)
Y band at 1.035 µm
Secondary maximum appears to have been significantly stronger than primary maximum!
![Page 10: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/10.jpg)
Krisciunas et al. (2001)
Strength of Secondary Maximum vs. Decline Rate in the I Band
![Page 11: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/11.jpg)
Krisciunas et al. (2001)
![Page 12: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/12.jpg)
Morphology of JHK lightcurves of SNe Ia:
Primary maxima occur a few days before T(Bmax)
As a general rule, the secondary maximum occurs later and is stronger in slower declining events
Secondary maximum can be brighter than primary maximum (e.g., in Y & H bands)
H & K light curves are relatively flat around T(Bmax)
![Page 13: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/13.jpg)
JHK Light Curves of 6
well-observed
SNe I
![Page 14: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/14.jpg)
JHK Light Curves of
the same 6 SNe I, but
corrected to a stretch
equivalent to m15(B) =
1.1Let’s zoom in on this time window, and do this more precisely
(e.g., include K corrections)
![Page 15: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/15.jpg)
Krisciunas et al. (2004)
Construction of JHK Stretch Templates
= 1980N (1.29)
= 1986G (1.79)
= 1998bu (1.05)
= 1999aw (0.81)
= 1999ee (0.94)
= 2000ca (1.01)
= 2001el (1.15)
SN m15(B)
![Page 16: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/16.jpg)
Fitting JHK Light Curves with the Stretch Templates
m15(B) = 0.99 m15(B) = 1.73
![Page 17: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/17.jpg)
Fitting JHK Light Curves with the Stretch Templates
m15(B) = 1.28 m15(B) = 1.63
![Page 18: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/18.jpg)
JHK light curve Templates for SNe Ia:
Stretch technique works well for JHK light curves in the window -12 to +10 days with respect to T(Bmax)
Allows reasonable estimates to be made of the maximum light magnitudes in JHK without the need to actually obtain photometry at maximum light
The same technique can most likely be extended to the I band as well (useful for observations of high-z SNe Ia)
![Page 19: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/19.jpg)
The B-V Color Evolution of Unreddened SNe Ia
From: Phillips et al. 1999
![Page 20: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/20.jpg)
From: Phillips et al. 1999
The B-V Color Evolution of Unreddened SNe Ia
![Page 21: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/21.jpg)
Colors at Maximum Light for Unreddened SNe Ia
Scatter corresponds to ± 0.05 mag in E(B-V)
This is as well as we can currently determine the reddening of an individual SN Ia
![Page 22: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/22.jpg)
Krisciunas et al. (2000)
"Worst Case NIR"Av = (1.126±0.072) x
E(V-K)
"Best Case Optical"Av = (3.1±0.1) x E(B-
V)
"Realistic Case Optical"
Av = (2.6±0.3) x E(B-V)
![Page 23: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/23.jpg)
Krisciunas et al. (2000)
SNe Ia with0.9 < m15(B) < 1.3
Shifted to Av = 0.0 locus
Optical-NIR Colors of Unreddened SNe
Ia
![Page 24: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/24.jpg)
SNe Ia with0.8 < m15(B) < 1.0
Shifted to Av = 0.0 locus
SNe Ia with0.9 < m15(B) < 1.3
Optical-NIR Colors of Unreddened SNe Ia
Krisciunas et al. (2004)
![Page 25: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/25.jpg)
Optical-NIR Colors vs. Δm15(B) Unreddened
SNe Ia
Scatter corresponds to ± 0.18 mag in Av
Equivalent to ± 0.06 mag in E(B-V)
This is as expected since reddening corrections were derived from BVI data
Krisciunas et al. (2004)
![Page 26: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/26.jpg)
Reddening:
SNe Ia with intermediate decline rates (0.9 < m15(B) < 1.3) have similar V-IR color evolution
As expected, the V-IR color evolution of slower declining (0.8 < m15(B) < 1.0) events is somewhat bluer
Use of optical-IR color evolution to determine reddening should ultimately prove more precise than optical-only colors
![Page 27: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/27.jpg)
Note that the
luminosity vs. decline
rate relaton in H may be
flat Phillips et al. (2003)
Absolute Magnitudes of SNe Ia
![Page 28: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/28.jpg)
Are SNe Ia “Perfect” Standard Candles in the NIR?
• We can try to answer this question by constructing Hubble diagrams in JHK
• Available data: 7 SNe Ia observed at LCO and CTIO + 9 SNe Ia with previously published photometry
• Use stretch template fits to find maximum light magnitudes
• Correct for reddening based on E(B-V) values determined from BVI photometry
• K corrections calculated from NIR spectra of SN 1999ee (Hamuy et al. 2002)
![Page 29: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/29.jpg)
Cepheid & SBF distances used to
derive “equivalent” v(cmb) assuming
Ho = 72
Krisciunas, Phillips, & Suntzeff (2004)
JHK Hubble Diagrams of SNe Ia
Are the deviations from the Hubble lines a function of
m15(B)?
= 0.14 mag
= 0.18 mag
= 0.12 mag
![Page 30: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/30.jpg)
NIR Absolute Magnitudes of SNe Ia
Within the precision of the observations, there are no obvious decline rate relations in the NIR
Mean values:
M(J) = -18.57 ± 0.14M(H) = -18.24 ± 0.18M(K) = -18.42 ± 0.12
Krisciunas, Phillips, & Suntzeff (2004)
![Page 31: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/31.jpg)
Absolute Magnitudes &Hubble Diagrams:
While SNe Ia are standardizable candles in the optical bands, they apparently are standard candles in the NIR at the ± 0.20 mag level or better (± 9% in distance)
The one disadvantage of the NIR is that SNe Ia are 1 mag less luminous in JHK than they are in the V band
![Page 32: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/32.jpg)
What about SNe II in the NIR?
• Plateau SNe (SNe II-P) are potentially useful distance indicators
• EPM (the models need more work)
• The Luminosity vs. Velocity Relation (looks encouraging)
• Major source of error is determining the dust reddening
• Since electron scattering is dominant opacity during plateau phase, SNe II-P should have similar similar hydrogen recombination tempertures during last part of plateau phase
• As in the case of SNe Ia, Optical-NIR colors offer significant promise for improving reddening estimates of SNe II-P
![Page 33: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/33.jpg)
SNe II-P are relatively bright in the NIR, with maximum occurring typically 2 months after explosion
NIR Light Curves of a Plateau SN II
Hamuy et al. (2001)
![Page 34: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/34.jpg)
Color curves and reddening
time since explosion (days)
B-V V-I
colo
r
Av=0.50 Av=0.85
Comparison of B-V and V-I Color Evolution:
SN 1999gi vs. SN 1999ee
Hamuy (2002)
![Page 35: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/35.jpg)
Color curves and reddening
time since explosion (days)
B-V V-I
colo
r
Av=-0.75 Av=0.10
Comparison of B-V and V-I Color Evolution:
SN 1999cr vs. SN 1999ee
Hamuy (2002)
![Page 36: Near-IR Diagnostics for SNe](https://reader035.vdocuments.site/reader035/viewer/2022062301/56815b07550346895dc8b5b5/html5/thumbnails/36.jpg)
Reddening Estimates
Comparison of B-V and V-I Reddening Determinations (Relative to SN 1999em)
• In many cases, values based on B-V are negative – differing metallicities may be responsible for this
• Values based on V-I appear to be better behaved
• V-NIR colors may give best estimates of all
Hamuy (2002)