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SN1014J in M82A Pseudo-GOTOQ and what we
can learn with really big telescopes and DIBs about
QSOALS
Donald G. York, Dan Welty, Jiaqi JiangUniversity of Chicago
Julie DahlstromCarthage College
Adam RitcheyUniversity of Washington
Galaxies in AbsorptionParis, IAP, Sept. 22-24, 2014
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SN2014A in M82
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M82
General:Systemic velocity 209 km/secAt SNe: 133 km/sec (1 kpc from center)Starburst, dwarf (1010
solar masses)Strong interaction with M81 0.3-1 Gyr. agoCentral SFR, <10 MyrOuter parts >100 Myr
Interstellar: H alpha filaments (reflection, but origin of dust??)Probably UV bump (not SMC/Calzetti)Where are filaments, where is SN (behind disk)?Mixed IS cloud propertiesHigh gamma ray flux (cosmic rays), high Li abundance
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Log [N(Na I)/N(Ca II)]
Log [N(Ca I)/N( K I)]
Log [N(Ca I)/N(Ca II)]
Log [N(CH+)/N(CH)]
Disk is at 133km/sec
HV gas (halo)is movingaway from us.
backside,away or frontsideinfall.?
halo HVCs?
M82 systemicMilky WayM82 at SN
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SN2014J
HD183143
b Ori
B7 Ia
B8 Ia
HD204837 B0.5 V
HD214680 O9 V
HD214680 (not corrected for tellurics)
DIB l 5780 DIB l 5797
* *
5760 5780 5900 5920
SN2014A, two Galactic stars of same reddening, and Galactic standards(observer rest frame)
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5700 5800 5900
57805797
* *
Na I
Tellurics left in
Expanded region showing numerous DIBs replicated in SN2014J
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l 6284
ll 6376, 6379
(example of Lorentzian)
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K I
C2
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Black =500pc distant from EarthBlue and green= NGC6530 stars, 1500 pc distantRed=Her 36, 1500 pc distant
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Distance from Her 36
1000 pc10 pc
0.5 pcHerschel 36
IR pumping of J = 1 level of CH+(not known anyplace else In ISM)
Isolating the anomalous DIBProfiles to within 0.5 pc of Her 36
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Profiles of atomic and diatomicFeatures, showing dense clouds to the left and weak(non-molecular) clouds to the right.SN2014J
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Selected lines compared between Jan. 27 spectra and Jan. 30 spectra for SN2014J. No shift in components in strength or position was found over 6 weeks.
Ritchey, Welty, Dahlstrom, YorkarXiv1407.5723
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Welty, Dahlstrom, Ritchey and York, ApJ, 792, 106 (2014)
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QuadraticRecombination equil.
Linear
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Square-root
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Velocity of Na I components (green) and positions of mean wavelength
center of SN2014A DIBs
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Models of DIB profiles based ona) Components derived
from K Ib) Assuming a weighting
of 1:1 for 5780 to K I (red)
c) Assuming a 1/1 weighting in the right components and 7/1 in the left (dense) components (green).
d) Original data in black
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Conclusions
• H I and 5780 correlation holds over several galaxies.
• K I and 4963 correlation likewise holds
• There are no dramatic differences in dust DIB relationships if radiation field is taken out using K I.
• DIBs of all sorts exist in M82: broad, narrow, C2 and normal.
• There are a few features that might make M82 peculiar and might indicate similar conditions in
GOTOs: CH+/CN and DIB ratios like DIB l6376/l6379.
• Others are being explored.
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FIN
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Na I Na I
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4750 4850 4950
C2C2C2C2 DIBs in Galactic stars and SN2014J
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Ca I CH+DIB l 4428
CH
Ca I, CH+ and CH + region of l 4430 DIB
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