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 , 2014

SN2014A in M82

M82 General: Systemic velocity 209 km/sec At SNe: 133 km/sec (1 kpc from center) Starburst, dwarf (10 10 solar masses) Strong interaction with M 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

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 moving away from us. backside, away or frontside infall.? halo HVCs? M82 systemicMilky Way M82 at SN

SN2014J HD  Ori B7 Ia B8 Ia HD B0.5 V HD O9 V HD (not corrected for tellurics) DIB  5780 DIB  5797 * * SN2014A, two Galactic stars of same reddening, and Galactic standards (observer rest frame)

* * Na I Tellurics left in Expanded region showing numerous DIBs replicated in SN2014J

6284  6376, 6379 (example of Lorentzian)

K I C2C2

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

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

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

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 arXiv

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

Quadratic Recombination equil. Linear

Square-root

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

Models of DIB profiles based on a)Components derived from K I b)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

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, C 2 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 6376/ Others are being explored.

FIN

Na I

C2C2 C2C2 C2C2 C2 DIBs in Galactic stars and SN2014J

Ca ICH+ DIB 4428 CH Ca I, CH+ and CH + region of  4430 DIB