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CSI: LMC Type Ia Supernova Remnants
You-Hua Chu University of Illinois
Academia Sinica Institute of Astronomy
and Astrophysics (ASIAA)
R.A. Gruendl, K.C. Pan, P.M. Ricker, R. Foley,
A. Holmes, K. Litke, R. Tippens, D. Weisz
1. Surviving companions in Type Ia SNRs 2. Identification of Type Ia SNRs 3. HST search for surviving companions in Type Ia SNRs in the LMC
1. Surviving companions in Type Ia SNRs 2. Identification of Type Ia SNRs 3. HST search for surviving companions in Type Ia SNRs in the LMC
Two Origins of Supernovae (SNe)
Core-collapse SNe – massive stars Type Ia SNe - white dwarfs (WDs)
Type Ia SN – two possibilities
(1)Single degenerate WD with a normal star companion (2) Double degenerate merger of 2 WDs
Supernova Progenitors
Luminous massive stars can be detected in pre-explosion images.
SN2003gd (Smartt et al. 2004)
After Before
Progenitors of SNe Ia are too faint to be identified.
Was it single degenerate (SD) or double degenerate (DD)?
Embarrassing -- SNe Ia are cosmological distance indicators…
Single Degenerate Scenario of Ia SN
The surviving companion may be identified by its - Faster rotation - Chemical pollution - “Runaway” velocity - Anomalous color and luminosity
Evolution of a Surviving Companion
Pan, Ricker, Taam 2010, 2012
He Star MS star
The surviving companion may be identified by its - Faster rotation - Chemical pollution - “Runaway” velocity - Anomalous color and luminosity
If a surviving companion is found, the SD origin is affirmed.
Searching for Surviving Companions
SN 1006 - Gonzalez-Hernandez et al. 2012 - Kerzendorf et al. 2012 - no surviving companion is found
Tycho’s SN 1572 - Ruiz-Lapuente et al. 2004 (Tycho-G) - Gonzalez-Hernandez et al. 2009 ([Ni/Fe] high) - Kerzendorf et al. 2012 (Ni/Fe normal, no cand.)
Kepler’s SN 1604 - Kerzendorf et al. 2013 (no red giant or >10L
)
Photo credit: Roger Smith
The Large Magellanic Cloud distance 50 kpc; DM = 18.5
Kerzendorf uses Gemini GMOS to Take spectra of the brightest stars in Ia SNRs.
It is possible to use HST images and color-magnitude diagrams to diagnose surviving companions.
Searching for Surviving Companions
SNR 0509-67.5 SNR 0519-69.0
Shaefer & Pagnotta 2012 Edwards et al. 2012 (only V and Hα)
1. Surviving companions in Type Ia SNRs 2. Identification of Type Ia SNRs 3. HST search for surviving companions in Type Ia SNRs in the LMC
Identification of Type Ia SNRs
Balmer-dominated SN ejecta running into a neutral medium; collisionless shock (Chevalier et al. 1980)
SNR 0509-67.5 Hα + X-ray
Size 7 pc
Identification of Type Ia SNRs
Balmer-dominated X-ray Kα emission of Si,S,Ar,Ca,Fe
Hα X-ray
DEM L71 Size 20 pc
Identification of Type Ia SNRs
Balmer-dominated X-ray Kα emission of Si,S,Ar,Ca,Fe
Type Ia SNR
C-C SNR
LMC ISM
Hughes et al. 1995
Identification of Type Ia SNRs
Balmer-dominated X-ray Kα emission of Si,S,Ar,Ca,Fe Spectra of SN light echoes
Light echoes of: SN1987A
Identification of Type Ia SNRs
Balmer-dominated X-ray Kα emission of Si,S,Ar,Ca,Fe Spectra of SN light echoes
Rest et al. 2005, 2008
Light echoes of: SN1987A (27 yr)
N103B (860 yr)
SNR 0519-67.5 (610 yr)
SNR 0509-69.0 (410 yr)
Identification of Type Ia SNRs
Balmer-dominated X-ray Kα emission of Si,S,Ar,Ca,Fe Spectra of SN light echoes Old stellar/interstellar environment
HII & number of blue stars within 100 pc; eliminating C-C SNRs to get Type Ia SNRs (Chu & Kennicutt 1988)
Star formation history; coarse spatial grids (Badenes et al. 2009; Harris & Zaritsky 2009)
4’ = 60 pc
B 0509−67.5
DEM L71
B 0519−69.0 N103B
B 0548−70.4 DEM L316A
Type Ia SNRs in the LMC
B 0509−67.5
DEM L71
B 0519−69.0 N103B
B 0548−70.4 DEM L316A
Type Ia SNRs in the LMC
B 0509−67.5
DEM L71
B 0519−69.0 N103B
B 0548−70.4 DEM L316A
Type Ia SNRs in the LMC
Mg Si S
Ar Ca
S
Si
Si
S
Fe L-shell
B 0534−69.9 DEM L249
DEM L238 B 0454−67.2
Type Ia SNRs in the LMC
4’ = 60 pc
Type Ia SNRs in the LMC B 0534−69.9
B 0454−67.2 DEM L238
DEM L249
(XMM-Newton)
DEM L238 DEM L249
XMM-Central XMM-Shell Chandra-Central Borkowski et al. 2006
Fe L-shell emission
O/Fe ~ 13 for the LMC ISM < 1 for Type Ia SNe > 10 for C-C SNe
Large Type Ia SNRs show O/Fe ~ 1-5. Higher than Ia, but too low for C-C.
Ionization timescale (nt) high CSM density not expected around WDs
“Prompt” Type Ia – 107-108 yr after SF
We Learned from X-ray Spectra
1. Surviving companions in Type Ia SNRs 2. Identification of Type Ia SNRs 3. HST search for surviving companions in Type Ia SNRs in the LMC
HST Program for LMC Type Ia SNRs
Undergraduate “Scientific Writing” project.
Porposal was awarded 16 orbits to image 9 Type Ia SNRs in the LMC: - Search for surviving companions - Determine star formation history
Images in F475W, F555W, F814W, F656N and near-IR F110W, F160W for SNR 0509
The Case of SNR 0509-67.5
Schaefer & Pagnotta 2012
No surviving companion with V < 26.9.
A “smudge” is seen at the center of the SNR. It could be a galaxy; however, a SNR-related origin is not ruled out.
SNR 0509-67.5
We noticed a point-like source in F814W…
F814W (814nm) F110W (1.1μm) Spitzer (3.6μm) It is even more prominent in near-IR.
The SED is made with HST & Spitzer data. The 3.6” aperture is needed for Spitzer, but includes optically bright stars.
- The nucleus is redder than the disk. - Balmer jump? If yes, galaxy at z ≈ 0.8.
Balmer Jump?
Pagnotta, Walker, & Schaefer 2014
Gemini GMOS spectrum Detected one line from the smudge at 6766 Å. Concluded z = 0.031
Gemini GMOS detected line at 676nm.
If Hα line, z = 0.03. Too red.
If [O II] line, z = 0.8. Colors are right.
Photobomb galaxy !
4’ = 60 pc
B 0509−67.5
DEM L71
B 0519−69.0
B 0548−70.4
Four Balmer-Dominated SNRs
No clear candidates for surviving companions at the center of SNR. Abigail Holmes et al. in prep
Three Large Type Ia SNRs
Error circles are large Hard to pin down candidate survivors. Katrina Litke et al. in prep
4’ = 60 pc
The Case of SNR DEM L316
A – SN Ia B - CC SN
Williams & Chu 2005
A B
He stars MS stars
He stars MS stars
The Case of SNR DEM L316
F555-F814 F475-F555
F55
5
F55
5
The spread in the red clump indicates Differential extinction.
F555-F814 F475-F555
F55
5
The Case of SNR DEM L316
Need to examine multiple CMDs. More complicated than expected…
SNR N103B - Young and Prompt?
Rest et al. -- light echo, Type Ia, 860 yr
SNR N103B - Young and Prompt?
HST and Chandra images of N103B
1
2
3 4
5
6 7 8
9
10
11
12
13
SNR N103B - Young and Prompt?
Right positions in the CMD, wrong in the image. No obvious candidate for surviving companion.
Questions: What kind of progenitor?
Are these knots CSM or SN ejecta?
The crime has not been solved. Investigation is still ongoing…