The Effect of Bars on the Ionized ISM: Optical Emission Lines from Milky Way Analogs
Por:
Krishnarao D., Tremonti C., Fraser-Mckelvie A., Kraljic K., Boardman N.F., Masters K.L., Benjamin R.A., Haffner L.M., Jones A., Pace Z.J., Zasowski G., Bershady M., Bizyaev D., Brinkmann J., Brownstein J.R., Drory N., Pan K., Zhang K.
Publicada:
1 ene 2020
Resumen:
Gas interior to the bar of the Milky Way has recently been shown to be the closest example of a low-ionization (nuclear) emission region (LI(N)ER) in the universe. To better understand the nature of this gas, a sample of face-on galaxies with integral field spectroscopy is used to study the ionized gas conditions of 240 barred and 250 nonbarred galaxies, focusing on those that are most similar to the Milky Way. Strong optical line emission of [N ii] ?6584, Ha, [O iii] ?5007, and Hß are used to diagnose the dominant ionization mechanisms of gas across galaxies and the Galaxy via Baldwin-Phillips-Terlevich diagrams. Barred galaxies show a strong suppression of star formation and an increase in composite and LI(N)ER-like spectra in their inner regions when compared with similar nonbarred counterparts. This effect is lessened in galaxies of very low () or very high () total stellar mass. Bar masks from Galaxy Zoo:3D show the bar's nonaxisymmetric effect on the ionized gas and help predict the face-on distribution of ionized gas conditions near the bar of the Milky Way. © 2020. The American Astronomical Society. All rights reserved..
Filiaciones:
Krishnarao D.:
Department of Astronomy, University of Wisconsin-Madison, Madison, WI, United States
Tremonti C.:
Department of Astronomy, University of Wisconsin-Madison, Madison, WI, United States
Fraser-Mckelvie A.:
School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, United Kingdom
Kraljic K.:
Institute for Astronomy, University of Edinburgh, Edinburgh, United Kingdom
Boardman N.F.:
Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, United States
Masters K.L.:
Department of Physics and Astronomy, Haverford College, Haverford, PA, United States
Benjamin R.A.:
Department of Physics, University of Wisconsin-Whitewater, Whitewater, WI, United States
Haffner L.M.:
Physical Sciences Department, Embry-Riddle Aeronautical University, Daytona Beach, FL, United States
Jones A.:
Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL, United States
Pace Z.J.:
Department of Astronomy, University of Wisconsin-Madison, Madison, WI, United States
Zasowski G.:
Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, United States
Bershady M.:
Department of Astronomy, University of Wisconsin-Madison, Madison, WI, United States
South African Astronomical Observatory, Cape Town, South Africa
Bizyaev D.:
Apache Point Observatory, Sunspot, NM, United States
Sternberg Astronomical Institute, Moscow State University, Moscow, Russian Federation
Brinkmann J.:
Apache Point Observatory, Sunspot, NM, United States
Brownstein J.R.:
Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, United States
Drory N.:
McDonald Observatory, University of Texas at Austin, Austin, TX, United States
Pan K.:
Apache Point Observatory, Sunspot, NM, United States
Zhang K.:
Lawrence Berkeley National Laboratory, Berkeley, CA, United States
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