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SN1014J in M82

SN1014J in M82 A Pseudo-GOTOQ and what we can learn with really big telescopes and DIBs about QSOALS. Donald G. York, Dan Welty, Jiaqi Jiang University of Chicago Julie Dahlstrom Carthage College Adam Ritchey University of Washington. Galaxies in Absorption

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SN1014J in M82

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  1. SN1014J in M82 A Pseudo-GOTOQ and what we can learn with really big telescopes and DIBs about QSOALS Donald G. York, Dan Welty, Jiaqi Jiang University of Chicago Julie Dahlstrom Carthage College Adam Ritchey University of Washington Galaxies in Absorption Paris, IAP, Sept. 22-24, 2014

  2. SN2014A in M82

  3. M82 General: Systemic velocity 209 km/sec At SNe: 133 km/sec (1 kpc from center) Starburst, dwarf (1010solar masses) Strong interaction with M81 0.3-1 Gyr. ago Central SFR, <10 Myr Outer 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 properties High gamma ray flux (cosmic rays), high Li abundance

  4. Disk is at 133km/sec HV gas (halo) is moving away from us. backside, away or frontside infall.? Log [N(Na I)/N(Ca II)] Log [N(Ca I)/N( K I)] halo HVCs? Log [N(Ca I)/N(Ca II)] Milky Way M82 systemic M82 at SN Log [N(CH+)/N(CH)]

  5. SN2014A, two Galactic stars of same reddening, and Galactic standards (observer rest frame) DIB l 5780 DIB l 5797 SN2014J B7 Ia HD183143 B8 Ia bOri B0.5 V HD204837 O9 V HD214680 * * HD214680 (not corrected for tellurics) 5760 5900 5780 5920

  6. 5797 Na I 5780 * * Tellurics left in Expanded region showing numerous DIBs replicated in SN2014J 5700 5800 5900

  7. (example of Lorentzian) l 6284 ll6376, 6379

  8. K I C2

  9. Black =500pc distant from Earth Blue and green= NGC6530 stars, 1500 pc distant Red=Her 36, 1500 pc distant

  10. Isolating the anomalous DIB Profiles to within 0.5 pc of Her 36 Distance from Her 36 1000 pc 10 pc 0.5 pc Herschel 36 IR pumping of J = 1 level of CH+ (not known anyplace else In ISM)

  11. Profiles of atomic and diatomic Features, showing dense clouds to the left and weak (non-molecular) clouds to the right. SN2014J

  12. 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, York arXiv1407.5723

  13. Welty, Dahlstrom, Ritchey and York, ApJ, 792, 106 (2014)

  14. Quadratic Recombination equil. Linear

  15. Square-root

  16. Velocity of Na I components (green) and positions of mean wavelength center of SN2014A DIBs

  17. Models of DIB profiles based on Components derived from K I Assuming a weighting of 1:1 for 5780 to K I (red) Assuming a 1/1 weighting in the right components and 7/1 in the left (dense) components (green). d) Original data in black

  18. 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.

  19. FIN

  20. Na I Na I

  21. C2 C2 C2 C2 DIBs in Galactic stars and SN2014J 4950 4850 4750

  22. Ca I CH+ CH DIB l 4428 Ca I, CH+ and CH + region of l4430 DIB

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