TY - JOUR
T1 - A MUSE source-blind survey for emission from the circumgalactic medium
AU - Zhang, Huanian
AU - Zaritsky, Dennis
N1 - Publisher Copyright:
© 2024 The Authors.
PY - 2024/11/22
Y1 - 2024/11/22
N2 - The recent detection of optical emission lines from the circumgalactic medium (CGM) in combined, large samples of low-redshift, normal galaxy spectra hints at the potential to map the cool (∼104 kelvin) CGM in individual, representative galaxies. Using archival data from a forefront instrument (MUSE) on the VLT, we present a source-blind, wide-redshift- range (z ∼ 0 to 5) narrowband imaging survey for CGM emission. Our detected, resolved emission line sources are cataloged and include a 30-kiloparsec- wide Hα source likely tracing the CGM of a low-mass galaxy (stellar mass ∼ 108.78±0.42 solar mass) at z = 0.1723, a 60-kiloparsec- wide Ly α structure associated with a galaxy at z = 3.9076, and a 130-kiloparsec (∼rvir)-wide [O II] feature revealing an interaction between a galaxy pair at z = 1.2480. The Hα velocity field for the low-mass galaxy suggests that the CGM is more chaotic or turbulent than the galaxy disk, while that for the interacting galaxies shows large-scale (∼50 kiloparsec) coherent motions.
AB - The recent detection of optical emission lines from the circumgalactic medium (CGM) in combined, large samples of low-redshift, normal galaxy spectra hints at the potential to map the cool (∼104 kelvin) CGM in individual, representative galaxies. Using archival data from a forefront instrument (MUSE) on the VLT, we present a source-blind, wide-redshift- range (z ∼ 0 to 5) narrowband imaging survey for CGM emission. Our detected, resolved emission line sources are cataloged and include a 30-kiloparsec- wide Hα source likely tracing the CGM of a low-mass galaxy (stellar mass ∼ 108.78±0.42 solar mass) at z = 0.1723, a 60-kiloparsec- wide Ly α structure associated with a galaxy at z = 3.9076, and a 130-kiloparsec (∼rvir)-wide [O II] feature revealing an interaction between a galaxy pair at z = 1.2480. The Hα velocity field for the low-mass galaxy suggests that the CGM is more chaotic or turbulent than the galaxy disk, while that for the interacting galaxies shows large-scale (∼50 kiloparsec) coherent motions.
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U2 - 10.1126/sciadv.adp8629
DO - 10.1126/sciadv.adp8629
M3 - Article
C2 - 39565863
AN - SCOPUS:85210273004
SN - 2375-2548
VL - 10
JO - Science Advances
JF - Science Advances
IS - 47
M1 - eadp8629
ER -