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

SN2014A in M82

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

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

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)

5700 5800 5900

57805797

* *

Na I

Tellurics left in

Expanded region showing numerous DIBs replicated in SN2014J

l 6284

ll 6376, 6379

(example of Lorentzian)

K I

C2

Black =500pc distant from EarthBlue and green= NGC6530 stars, 1500 pc distantRed=Her 36, 1500 pc distant

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

Profiles of atomic and diatomicFeatures, 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, YorkarXiv1407.5723

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

QuadraticRecombination equil.

Linear

Square-root

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

center of SN2014A DIBs

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

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.

FIN

Na I Na I

4750 4850 4950

C2C2C2C2 DIBs in Galactic stars and SN2014J

Ca I CH+DIB l 4428

CH

Ca I, CH+ and CH + region of l 4430 DIB