Near-infrared spectroscopy of Type Ia supernovae Eric Y. Hsiao - - PowerPoint PPT Presentation

Near-infrared spectroscopy

• f Type Ia supernovae

Eric

• Y. Hsiao

Las Campanas Observatory Aarhus University Florida State University

• n behalf of the Carnegie Supernova Project and collaborations
• M. M. Phillips, C. Contreras, N. Morrell, C. R. Burns, M. Stritzinger, C. Gall,
• S. E. Persson, N. B. Suntzeff, W. L. Freedman
• G. H. Marion, D. J. Sand, T. Diamond,
• R. P

. Kirshner, et al.

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Why NIR?

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0.8 1.0 1.2 1.4 1.6 1.8 2.0

m15(B)

20 19 18 17

Mmax

20 19 18 17

Mmax

20 19 18 17

Mmax

20 19 18 17

Mmax

IKC J H K B V

20 19 18 17

Mmax

20 19 18 17

Mmax

0.01 < z < 0.1 (Ho = 74) Cepheid, SBF, PNLF

Kasen (2006) Phillips (2005)

Theory Observation

NIR

• ptical

NIR

• ptical

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

0.8 1 1.2 1.4 1.6 20 19.5 19 18.5 18 17.5 17 16.5 16

m15(B) Peak Magnitude

0.8 1 1.2 1.4 1.6

m15(B)

MB B0µ MH H0µ

Why NIR?

3

Mandel et al. (2011)

• ptical

NIR

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Why NIR?

In the NIR, achieve higher precision through 2 routes: ■ By avoiding things we do not understand (shortcut) ■ By constraining the physics (more fun!)

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Credit: ESO

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

CSP NIR spectroscopy

Carnegie Supernova Project ■ CSP I (2004-2008) ■ CSP II (2011-2015) PI: Mark Phillips NIR observations of ~100 SNe Ia 1-m Swope optical light curves 2.5-m du Pont NIR light curves, optical spectra 6.5-m Magellan NIR spectra

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Credit: Yuri Beletsky

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015 6

# of Ia

• ptical spectra

104

# of Ia NIR spectra

102

41 from Marion et al. (2009) + 91T, 94D, 98bu, 99by, 99ee, 02bo, 02dj, 03du, 05cf, 05df, 11fe, 13ebh,14J

CSP NIR spectroscopy

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015 7

CSP NIR spectroscopy

Hsiao et al. in prep

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Probing SN Ia physics

■ Unburned material

Premax C I 1.0693 Marion et al. (2006)

■ Boundary between C/O burning

Premax Mg II 1.0927 Wheeler et al. (1998)

■ Radioactive nickel

Postmax H-band break Wheeler et al. (1998), Höflich et al. (2002)

■ Stable nickel

Transitional phase [Ni II] Friesen et al. (2014)

■ Companion signature

Postmax P-beta Maeda et al. (2014)

■ Central density and B-field

Nebular phase [Fe II] 1.6440 Penney & Höflich (2014), Diamond et al. (2015)

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Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Unburned material

Premax C I 1.0693

■ Carbon: pristine material from the progenitor ■ Incomplete burning: constraints for explosion models ■ Optical C II 6580

detected in 20-30% of SNe Ia

Thomas et al. (2011) Folatelli et al. (2012) Silverman et al. (2012)

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Thomas et al. (2011)

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Unburned material

Premax C I 1.0693

■ NIR provides a more complete census of carbon than the optical ■ Unburned material ubiquitous?

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Hsiao et al. (2013, 2015), Sand et al. in prep

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 log10(F) + constant 0.60 0.65

2010 0

• ptical C II

0.6580 SN 1999by

4.0

SYNAPPS C II

1.00 1.05

2010 0

NIR C I 1.0693

3.3 0.4

SYNAPPS C I

0.60 0.65

2010 0

iPTF13ebh

11.9 11.1 6.7 3.8 0.5

1.00 1.05

2010 0

12.8 10.7 6.8 3.7 1.0

0.60 0.65

2010 0

SN 2011fe

12.7 6.6 +0.4

1.00 1.05

2010 0

velocity (103 km/s) rest wavelength (µm)

12.6 6.7 +0.3

0.60 0.65

2010 0

SN 2014J

9.1 6.2 3.6 0.6

1.00 1.05

2010 0

9.9 6.3 2.9 0.4

0.60 0.65

2010 0

ASAS14lp

1.0

1.00 1.05

2010 0

9.9 3.9

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Boundary between C/O burning

Premax Mg II 1.0927

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Wheeler et al. (1998), Höflich et al. (2002)

■ Strong, isolated line ■ Flat Mg velocity evolution: bottom of C burning layer ■ Boundary between C/O burning ■ Sensitive to transition density

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Boundary between C/O burning

Premax Mg II 1.0927

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0.8 1.0 1.2 1.4 1.6 1.8 2.0

• ptical lightcurve decline rate m15(B)

9 10 11 12 13 14 15 Mg II 1.0927 velocity (103 km/s)

94D 98bu 99by 99ee 02bo 02cr 02dj 03W 03du 05am 05cf 11fe 11iv

SNe with time series SNe without time series

15 10 5 5 10 phase relative to Bband maximum (d) 8 9 10 11 12 13 14 15 Mg II 1.0927 velocity (103 km/s) 11fe 05cf 05am 03du 02dj 99ee 99by 94D

Hsiao et al. (2013)

■ No correlation with light-curve decline rate ■ Transition density not the main driver of SN brightness?

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015 13

1 2 3 4 5 log10(F) + constant

20110826

texpl = 2.58 d tBmax = 14.6 d

20110828

texpl = 4.56 d tBmax = 12.6 d

20110831

texpl = 7.55 d tBmax = 9.7 d

20110903

texpl = 10.55 d tBmax = 6.7 d

20110907

texpl = 14.42 d tBmax = 2.8 d

20110910

texpl = 17.52 d tBmax = 0.3 d

20110913

texpl = 20.55 d tBmax = 3.3 d

20110918

texpl = 25.45 d tBmax = 8.2 d

20110922

texpl = 29.53 d tBmax = 12.3 d

20110927

texpl = 34.52 d tBmax = 17.3 d

0.9 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0 2.1 2.3 2.5

• bserved wavelength (µm)

0.9 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0 2.1 2.3 2.5

NIR spectra

• f SN 2011fe

Radioactive nickel

H-band break

Kirshner et al. (1973) Hsiao et al. (2013)

■ H-band break: most prominent SN Ia NIR feature

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Radioactive nickel

H-band break

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0.8 1.0 1.2 1.4 1.6 1.8 2.0 m15(B) 2.0 2.5 3.0 3.5 4.0 Hband break ratio R12

98bu 99ee 04da 11fe iPTF13ebh 99by 04S 05cf 11iv 02ha 05am

without time series with time series

0.6 0.8 1.0 1.2 sBV

98bu 99ee 11fe iPTF13ebh 99by 04S 05cf 11iv 05am

Hsiao et al. (2013, 2015)

5 10 15 20 25 restframe phase relative to Bband maximum (days) 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5 Hband break ratio R 98bu 99by 99ee 04da 05am 05cf 11fe 11iv 14J iPTF13ebh

1.5 1.6 1.7µm

f0 f1 R=f1/f0

■ The strong correlation is consistent with Chandrasekhar-mass delayed detonation ■ Dynamical merger would yield the opposite trend and weaker correlation

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Stable nickel

Transitional phase [Ni II]

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Friesen et al. (2014) Without forbidden lines With forbidden lines

■ 1.98 micron feature: possible [Ni II] ■ Nickel at late phase most likely stable nickel

SN2014J at 67d

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Stable nickel

Transitional phase [Ni II]

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Could come from: ■ High density progenitor

Friesen et al. (2014)

■ Metallicity of progenitor

Timmes et al. (2003)

■ Neutronization in simmering phase

Piro & Bildsten (2008)

0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 normalized F

65 d 69 d 72 d 77 d 99 d 113 d

1.9 2.0 2.1 2.2 2.3 2.4 2.5 rest wavelength (µm) 1.9 2.0 2.1 2.2 2.3 2.4 2.5

SN2012fr

Archival data CSP data

Friesen et al. (2014)

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Companion signature

Postmax P-beta

■ H stripped off non- degenerate companion, embedded at low velocity ■ Optical depth higher for

• ptical than NIR

■ P-beta stronger and appear above photosphere earlier than H-alpha

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Maeda et al. (2014)

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

Central density and B-field

Nebular phase [Fe II] 1.6440

■ Extract central density and B-field through [Fe II] line width ■ Central density constraints accretion rate and progenitor system

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Diamond et al. (2015)

Eric

• Y. Hsiao

Carnegie SN Ia Progenitor Workshop, August 2015

■ How can NIR spectroscopy help? ■ Don’t stop at the optical!

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