TY - JOUR
T1 - A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
AU - Shaban, Ahmed
AU - Bordoloi, Rongmon
AU - Chisholm, John
AU - Sharma, Soniya
AU - Sharon, Keren
AU - Rigby, Jane R.
AU - Gladders, Michael G.
AU - Bayliss, Matthew B.
AU - Barrientos, L. Felipe
AU - Lopez, Sebastian
AU - Tejos, Nicolas
AU - Ledoux, Cédric
AU - Florian, Michael K.
N1 - Funding Information:
This work is based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere under ESO program 098.A-0459(A). In addition, we used observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. A.S. and R.B. would like to thank Kavli Institute for Theoretical Physics (KITP), which is supported by the National Science Foundation (NSF) under grant No. NSF PHY-1748958, for hosting the Fundamentals of Gaseous Halos workshop. S.L. acknowledges support by FONDECYT grant 1191232.
Funding Information:
This work is based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere under ESO program 098.A-0459(A). In addition, we used observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. A.S. and R.B. would like to thank Kavli Institute for Theoretical Physics (KITP), which is supported by the National Science Foundation (NSF) under grant No. NSF PHY-1748958, for hosting the Fundamentals of Gaseous Halos workshop. S.L. acknowledges support by FONDECYT grant 1191232.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/9/1
Y1 - 2022/9/1
N2 - We image the spatial extent of a cool galactic outflow with fine-structure Fe ii* emission and resonant Mg ii emission in a gravitationally lensed star-forming galaxy at z = 1.70347. The Fe ii* and Mg ii (continuum-subtracted) emissions span out to radial distances of ∼14.33 and 26.5 kpc, respectively, with maximum spatial extents of ∼21 kpc for Fe ii* emission and ∼30 kpc for Mg ii emission. Mg ii emission is patchy and covers a total area of ∼184 kpc2, constraining the minimum area covered by the outflowing gas to be ∼13% of the total area. Mg ii emission is asymmetric and shows ∼21% more extended emission along the decl. direction. We constrain the covering fractions of the Fe ii* and Mg ii emission as a function of radial distance and characterize them with a power-law model. The Mg ii 2803 emission line shows two kinematically distinct emission components and may correspond to two distinct shells of outflowing gas with a velocity separation of Δv ∼ 400 km s−1. By using multiple images with different magnifications of the galaxy in the image plane, we trace the Fe ii* and Mg ii emissions around three individual star-forming regions. In all cases, both the Fe ii* and Mg ii emissions are more spatially extended compared to the star-forming regions traced by the [O ii] emission. These findings provide robust constraints on the spatial extent of the outflowing gas and, combined with outflow velocity and column density measurements, will give stringent constraints on mass-outflow rates of the galaxy.
AB - We image the spatial extent of a cool galactic outflow with fine-structure Fe ii* emission and resonant Mg ii emission in a gravitationally lensed star-forming galaxy at z = 1.70347. The Fe ii* and Mg ii (continuum-subtracted) emissions span out to radial distances of ∼14.33 and 26.5 kpc, respectively, with maximum spatial extents of ∼21 kpc for Fe ii* emission and ∼30 kpc for Mg ii emission. Mg ii emission is patchy and covers a total area of ∼184 kpc2, constraining the minimum area covered by the outflowing gas to be ∼13% of the total area. Mg ii emission is asymmetric and shows ∼21% more extended emission along the decl. direction. We constrain the covering fractions of the Fe ii* and Mg ii emission as a function of radial distance and characterize them with a power-law model. The Mg ii 2803 emission line shows two kinematically distinct emission components and may correspond to two distinct shells of outflowing gas with a velocity separation of Δv ∼ 400 km s−1. By using multiple images with different magnifications of the galaxy in the image plane, we trace the Fe ii* and Mg ii emissions around three individual star-forming regions. In all cases, both the Fe ii* and Mg ii emissions are more spatially extended compared to the star-forming regions traced by the [O ii] emission. These findings provide robust constraints on the spatial extent of the outflowing gas and, combined with outflow velocity and column density measurements, will give stringent constraints on mass-outflow rates of the galaxy.
UR - http://www.scopus.com/inward/record.url?scp=85137400099&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ac7c65
DO - 10.3847/1538-4357/ac7c65
M3 - Article
AN - SCOPUS:85137400099
VL - 936
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 77
ER -