TY - JOUR
T1 - Separating line emission from star formation, shocks, and AGN ionization in NGC 1068
AU - D'Agostino, Joshua J.
AU - Kewley, Lisa J.
AU - Groves, Brent A.
AU - Medling, Anne M.
AU - Di Teodoro, Enrico
AU - Dopita, Michael A.
AU - Thomas, Adam D.
AU - Sutherland, Ralph S.
AU - Garcia-Burillo, Santiago
N1 - Publisher Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2019/8/11
Y1 - 2019/8/11
N2 - In the optical spectra of galaxies, the separation of line emission from gas ionized by star formation and an active galactic nucleus (AGN), or by star formation and shocks, are very well-understood problems. However, separating line emission between AGN and shocks has proven difficult. With the aid of a new three-dimensional diagnostic diagram, we show the simultaneous separation of line emission from star formation, shocks, and AGN in NGC 1068, and quantify the ratio of star formation, shocks, and AGN in each spaxel. The AGN, shock, and star formation luminosity distributions across the galaxy accurately align with X-ray, radio, and CO(3-2) observations, respectively. Comparisons with previous separation methods show that the shocked emission heavily mixes with the AGN emission. We also show that if the H α flux is to be used as a star formation rate indicator, separating line emission from as many sources as possible should be attempted to ensure accurate results.
AB - In the optical spectra of galaxies, the separation of line emission from gas ionized by star formation and an active galactic nucleus (AGN), or by star formation and shocks, are very well-understood problems. However, separating line emission between AGN and shocks has proven difficult. With the aid of a new three-dimensional diagnostic diagram, we show the simultaneous separation of line emission from star formation, shocks, and AGN in NGC 1068, and quantify the ratio of star formation, shocks, and AGN in each spaxel. The AGN, shock, and star formation luminosity distributions across the galaxy accurately align with X-ray, radio, and CO(3-2) observations, respectively. Comparisons with previous separation methods show that the shocked emission heavily mixes with the AGN emission. We also show that if the H α flux is to be used as a star formation rate indicator, separating line emission from as many sources as possible should be attempted to ensure accurate results.
KW - ISM: jets and outflows
KW - galaxies: ISM
KW - galaxies: Seyfert
KW - galaxies: active
KW - galaxies: evolution
KW - galaxies: star formation
UR - http://www.scopus.com/inward/record.url?scp=85072282132&partnerID=8YFLogxK
U2 - 10.1093/mnras/stz1611
DO - 10.1093/mnras/stz1611
M3 - Article
SN - 0035-8711
VL - 487
SP - 4153
EP - 4168
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -