Phot ometric Diversity f rom the C ar negie Super no va P...
Transcript of Phot ometric Diversity f rom the C ar negie Super no va P...
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Photometric Diversity from the Carnegie Supernova
Project (CSP)
Mark M. PhillipsCarnegie Observatories
Las Campanas Observatory
Thursday, August 20, 2009
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1987PASP...99..592P
My first paper on a SN Ia (Phillips et al. 1987)
Thursday, August 20, 2009
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1987PASP...99..592P
My first paper on a SN Ia (Phillips et al. 1987)
1987PASP...99..592P
Thursday, August 20, 2009
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CSP Observational Goals1. Obtain precision ugriBVYJH light curves and
spectrophotometry of
• ≥ 100 SNe Ia (z ≤ 0.07)
• ≥ 100 SNe II (z ≤ 0.05)
• ≥ 20 SNe Ibc (z ≤ 0.05)
2.Obtain rest system i band light curves of ~100 SNe Ia at 0.1 < z < 0.7
Thursday, August 20, 2009
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1. Gain insight into the progenitors and explosion mechanisms of SNe
2.Refine methods for determining distances to SNe Ia and SNe II
3.Provide a new fundamental reference for observations of high-z SNe
4.Characterize dark energy by producing an i-band Hubble diagram of low and high-z SNe Ia where reddening corrections are small
CSP Science Goals
Thursday, August 20, 2009
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CSP Telescopes/InstrumentsOptical (ugriBV) 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) Optical (0.32-1.0 μm) Spectroscopy: Las Campanas du Pont 2.5-m telescope + WFCCD (or Modspec, or B&C) Magellan 6.5-m telescope + LDSS-3 (or IMACS) CTIO 1.5-m telescope + Cassegrain Spectrograph (service mode) ESO NTT+EMMI
Swope 1-m Du Pont 2.5-m Magellan 6.5-m
Thursday, August 20, 2009
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Other collaboratorsAlex Filippenko (UC Berkeley)
Weidong Li (UC Berkeley)Ray Carlberg (Univ. Toronto)
Josh Frieman (Chicago/Fermi Lab.)Jose Luis Prieto (Ohio St./OCIW)
CSP PeopleChile
Mark Phillips (OCIW/LCO) P.I. Low-zMario Hamuy (U. Chile) Original P.I. Low-z
Max Stritzinger (OCIW/LCO, postdoc)Gastón Folatelli (U. Chile, former 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)Abdo Campillay (research assistant)
Pasadena
Wendy Freedman (OCIW) P.I. High-zEric Persson (OCIW)
Chris Burns (OCIW, postdoc)Barry Madore (OCIW/Pasadena)
Don Neill (Caltech)Pamela Wyatt (OCIW/IPAC)
David Murphy (OCIW)
Texas A&M
Nick SuntzeffKevin Krisciunas
Lifan WangDarren Depoy
Calán/Tololo Alumni
Thursday, August 20, 2009
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Recent CSP Papers• “The Carnegie Supernova Project: First Near-Infrared Hubble Diagram to z ~ 0.7”, Freedman et al. 2009, ApJ, in press (arXiv:0907.4524)
• “The Carnegie Supernova Project: First Photometry Data Release of Low-Redshift Type Ia Supernovae”, Contreras et al. 2009, AJ, submitted • “The Carnegie Supernova Project: Analysis of the First Sample of Low-Redshift Type Ia Supernovae”, Folatelli et al. 2009, AJ, submitted
Thursday, August 20, 2009
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Recent CSP Papers
Carlos Contreras
Gastón Folatelli
Thursday, August 20, 2009
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CSP Low-Redshift PassbandsOptical Near-infrared
0.0
0.1
0.2
0.3
0.4
0.5
3000 4000 5000 6000 7000 8000Wavelength
0.0
0.1
0.2
0.3
0.4
Frac
tiona
l Thr
ough
put
u
g ri
B
V
Precise measurements of the CSP passbands are scheduled for January 2010
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Color Term Coefficients
-0.10.00.10.2
ctu
-0.2-0.10.00.1
ctg
-0.2-0.10.00.1
ctr
-0.10.00.1
cti
-0.10.00.10.2
ctB
2453500 2454000 2454500J.D.
-0.2-0.10.00.1
ctV
+0.045 (027)
-0.015 (014)
-0.014 (016)
+0.002 (016)
+0.066 (014)
-0.061 (011)
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Extinction Coefficients
0.20.40.60.8
k u
0.00.20.4
k g
-0.20.00.20.4
k r
-0.20.00.20.4
k i
0.00.20.40.6
k B
2453500 2454000 2454500J.D.
-0.20.00.20.4
k V
0.502 (086)
0.193 (026)
0.103 (027)
0.060 (028)
0.249 (037)
0.136 (027)
2 out of every 3 nights were photometricThursday, August 20, 2009
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CSP Low-Redshift SampleIa II Ib/Ic/IIb Total
Actual 129 93 31 253Expected 100 100 25 225
LOSS40%
Puckett13%
SDSS11%
CHASE11%
ROTSE7%
Other18%
Thursday, August 20, 2009
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Examples of Light Curves I16
18
20
16
18
20
16
18
20
16
18
20
16
18
20mag
nitu
de 16
18
20
16
18
20
16
18
20
640 660 680 700 720JD 2453000+
16
18
20640 660 680 700 720
JD 2453000+
16
18
20
u B
g V
r i
Y J
H K
SN 2005el16
18
20
16
18
20
16
18
20
16
18
20
16
18
20mag
nitu
de 16
18
20
16
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16
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20
700 720 740 760 780JD 2453000+
16
18
20
700 720 740 760 780JD 2453000+
16
18
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u B
g V
r i
Y J
H K
SN 2005ki
z = 0.015 z = 0.019Thursday, August 20, 2009
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Examples of Light Curves II18
20
22
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22
18
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18
20
22
18
20
22mag
nitu
de 18
20
22
18
20
22
18
20
22
340 360 380 400 420JD 2453000+
18
20
22340 360 380 400 420 440
JD 2453000+
18
20
22
u B
g V
r i
Y J
H K
SN 2004gs
16
18
20
16
18
20
16
18
20
16
18
20
16
18
20mag
nitu
de 16
18
20
16
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16
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20
420 440 460 480 500JD 2453000+
16
18
20420 440 460 480 500
JD 2453000+
16
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20
u B
g V
r i
Y J
H K
SN 2005al
z = 0.027 z = 0.012Thursday, August 20, 2009
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Examples of Light Curves III18
20
22
18
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22
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18
20
22
18
20
22mag
nitu
de 18
20
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18
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22
700 720 740 760 780JD 2453000+
18
20
22700 720 740 760 780
JD 2453000+
18
20
22
u B
g V
r i
Y J
H K
SN 2005lu
20
22
24
18
20
22
18
20
22
18
20
22
18
20
22mag
nitu
de
18
20
22
18
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22
18
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22
960 980 1000 1020 1040JD 2453000+
18
20
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960 980 1000 1020 1040JD 2453000+
18
20
22
u B
g V
r i
Y J
H K
SN 2006eq
z = 0.050 z = 0.032Thursday, August 20, 2009
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The Secondary Maximum
The timing and strength of the secondary maximum is predicted to be primarily a function of the 56Ni mass -- and, therefore, Δm15(B)
Kasen (2006)
tB
t2m1
m2
m0
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The Secondary Maximum
Kasen (2006) CSP data
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The Secondary Maximum
Krisciunas et al. (2001)
An alternative method to measure the strength of the secondary maximum is the 〈i〉20-40 parameter
Thursday, August 20, 2009
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The Secondary Maximum
Krisciunas et al. (2001)
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The Secondary Maximum
What produces this?• Mixing?• Metallicity?• Geometry?
Is this a possible third parameter for reducing the dispersion in the Hubble diagram???
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SN Ia Color Excesses
Lira Relation for Suspected Low-Reddening SNe Ia
Implied Intrinsic Color vs. Decline Rate Relations
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SN Ia Color Excesses
0.5 1.0 1.5Δm15(B)
-0.4
-0.2
0.0
0.2
0.4
E(B-
V) ta
il - E(
B-V
) max
-0.2 -0.1 0 0.1 0.2 0.3E(B-V)max
-0.4
-0.2
0.0
0.2
0.4
E(B-
V) ta
il - E(
B-V
) max
This paperPhillips et al. (1999)
-0.1 0 0.1 0.2 0.3 0.4Bmax - Vmax
-19.5 -19.0 -18.5MB(corr)
How can this be?
• Is there is a component of one or the other of these color excesses which is not due to dust?
• Are we seeing evidence for time-variable extinction??
Thursday, August 20, 2009
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The Reddening Law
05A06X
Color excess ratios are a function of RV
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The Reddening Law
The Wang/Goobar dust scattering model looks promising to explain the low RV values of highly reddened SNe Ia
Thursday, August 20, 2009
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The Reddening Law
SNe Ia with low reddenings are consistent with Rv ~ 3Thursday, August 20, 2009
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The Reddening Law
But when Rv is treated as a free parameter to minimize B = MB + b ∗ [Δm15(B) - 1.1] + RB ∗ E(B-V) + μ ,
a value of RV ~ 1.5 is obtained, even for low-reddening eventsThursday, August 20, 2009
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Near-IR Light Curves
Kasen (2006)
CSP data
Thursday, August 20, 2009
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Near-IR Light Curves
• Over the decline rate range 0.7 < Δm15(B) < 1.7, the dispersion in absolute magnitudes in J and Y is < 0.20 mag, with no correction for Δm15(B)• There is some evidence for a slight dependence on Δm15(B) in J
Thursday, August 20, 2009
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SNe Ia as Precision Standard Candles
Combining Hubble diagrams in different bands does not yield a significant improvement in the observed dispersion
Filter σ (mag)u 0.13g 0.14r 0.13i 0.14B 0.14V 0.14Y 0.15J 0.12
H 0.16
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SNe Ia as Precision Standard Candles
This is because the residuals in each color are highly correlated, presumably due to peculiar velocities
The implication is that we are actually measuring distances to a precision of 3-4%
Thursday, August 20, 2009
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!"# $"! $"% $"& $"' $"# %"!
!m15
(B)
!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
./0
1
2
/
3
4!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
0.01 < z < 0.1 (Ho = 74)
Cepheid, SBF, PNLF
0.8 1.0 1.2 1.4 1.6 1.8 2.0
Δm15(B)
The Transition from “Normal” SNe Ia to 1991bg-like Events
Phillips (2005)
91bg-like
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The Transition from “Normal” SNe Ia to 1991bg-like Events
0.0
0.5
1.0
1.5
2.0
Mag
nitu
de
SN 2007onSN 2004gsSN 2005keSN 2006gt
-10 -5 0 5 10 15 20Days Since Lu to H Max
0.0
0.5
1.0
1.5
2.0
B
V
SN Δm15(B)
2004gs 1.57
2005ke 1.74
2007on 1.85
2006gt 1.90
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The Transition from “Normal” SNe Ia to 1991bg-like Events
SN Δm15(B)
2004gs 1.57
2005ke 1.74
2007on 1.85
2006gt 1.90
0
1
2
3
SN 2007onSN 2004gsSN 2005keSN 2006gt
0
1
2
3Mag
nitu
de
-10 0 10 20 30 40 50 60Days Since Bmax
0
1
2
3
0
1
2
3
SN 2007onSN 2004gsSN 2005keSN 2006gt
0
1
2
3Mag
nitu
de
-10 0 10 20 30 40 50 60Days Since Bmax
0
1
2
3
Thursday, August 20, 2009
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The Transition from “Normal” SNe Ia to 1991bg-like Events
SN Δm15(B)
2004gs 1.57
2005ke 1.74
2007on 1.85
2006gt 1.90
0
1
2
3
SN 2007onSN 2004gsSN 2005keSN 2006gt
-10 0 10 20 30 40 50 60Days Since Bmax
0
1
2
3
SN 2005ke appears to be the oddball
Thursday, August 20, 2009
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The Transition from “Normal” SNe Ia to 1991bg-like Events
SN Δm15(B)
2004gs 1.57
2005ke 1.74
2007on 1.85
2006gt 1.904000 5000 6000 7000 8000 9000
Rest Wavelength
10
11
12
13
14
15
16
17
AB
mag
2004gs (-3.4)
2007on (+0.1)
2006gt (-0.2)
2005ke (+0.7)
}
Ti II
Thursday, August 20, 2009
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The Transition from “Normal” SNe Ia to 1991bg-like Events
SN Δm15(B)
2004gs 1.57
2005ke 1.74
2007on 1.85
2006gt 1.90
Again, SN 2005ke appears to be the oddball
0 20 40 60 80Days Since Lu to H Max
41.0
41.5
42.0
42.5
43.0
log
L u to
H
SN 2007onSN 2005keSN 2006gtSN 2004gs
Thursday, August 20, 2009
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Near-IR Light Curves
Thursday, August 20, 2009
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The Transition from “Normal” SNe Ia to 1991bg-like Events
!"# $"! $"% $"& $"' $"# %"!
!m15
(B)
!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
./0
1
2
/
3
4!%!
!$(
!$#
!$)
*+,-
!%!
!$(
!$#
!$)
*+,-
0.01 < z < 0.1 (Ho = 74)
Cepheid, SBF, PNLF
0.8 1.0 1.2 1.4 1.6 1.8 2.0
Δm15(B)Phillips (2005)
The transition region appears to be populated by two different subtypes of SNe Ia:
• The low-luminosity extension of “normal” events, and
• 1991bg-like events
Thursday, August 20, 2009
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Conclusions• The strength and timing of the secondary maximum of the iYJH light curves is a function of Δm15(B), but with some significant intrinsic variation
• Color excesses derived from the Lira relation and the Bmax - Vmax color show systematic differences
• Ratios of color excesses provide evidence of “normal” (RV ~ 3) dust reddening, while minimizing the Hubble diagram dispersion gives RV ~ 1.5 • Correlated residuals in ugriBVYJH Hubble diagrams strongly suggest that SNe Ia yield distances that are good to 3-4%
• The transition region in the luminosity vs. decline rate relation at 1.6 ≤ Δm15(B) ≤ 1.9 appears to be populated by two different subtypes of SNe Ia
Thursday, August 20, 2009
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Aspen Workshop on SNe Ia
Weeks of 2010 August 8 & 15
Thursday, August 20, 2009