Journal
ASTROPHYSICAL JOURNAL
Volume 883, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab3e6c
Keywords
galaxies: clusters: individual (A3627); galaxies: evolution; galaxies: individual (ESO 137-001); galaxies: ISM; ISM: molecules; submillimeter: galaxies
Categories
Funding
- Ministry of Education, Youth and Sports of the Czech Republic [LM2015067]
- Czech Science Foundation [19-18647S]
- NASA [GO6-17111X, 80NSSC18K0606]
- NSF [1714764]
- Australian Research Council - Australian Government [FT180100066]
- FCT (Portugal) [SFRH/BPD/103385/2014]
- POPH/FSE (EC)
- Fundacao para a Ciencia e a Tecnologia (FCT) [UID/FIS/04434/2013]
- FEDER through COMPETE2020 [POCI-01-0145-FEDER-007672]
- FCT/MCTES [PTDC/FIS-AST/29245/2017]
- UK Science and Technology Facilities Council [ST/M001008/1]
- Science and Technology Facilities Council [ST/P000541/1]
- European Research Council (ERC) under the European Union [757535]
- [RVO:67985815]
- [DL 57/2016/CP1364/CT0009]
- STFC [ST/R000840/1, ST/M001008/1, ST/P000541/1] Funding Source: UKRI
- Fundação para a Ciência e a Tecnologia [PTDC/FIS-AST/29245/2017, DL 57/2016/CP1364/CT0009] Funding Source: FCT
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We present the first high-resolution map of the cold molecular gas distribution as traced by CO(2-1) emission with ALMA in a long ram pressure stripped tail. The Norma cluster galaxy ESO 137-001 is undergoing a strong interaction with the surrounding intracluster medium and is one of the nearest jellyfish galaxies with a long multiphase and multicomponent tail. We have mapped the full extent of the tail at 1 '' (350 pc) angular resolution and found a rich distribution of mostly compact CO regions extending to nearly 60 kpc in length and 25 kpc in width. In total, about 10(9) M-circle dot of molecular gas was detected with ALMA. From comparison with previous APEX observations, we also infer the presence of a substantial extended molecular component in the tail. The ALMA CO features are found predominantly at the heads of numerous small-scale (similar to 1.5 kpc) fireballs (i.e., star-forming clouds with linear streams of young stars extending toward the galaxy) but also large-scale (similar to 8 kpc) superfireballs and double-sided fireballs that have additional diffuse ionized gas tails extending in the direction opposite the stellar tails. The new data help to shed light on the origin of the molecular tail; CO filaments oriented in the direction of the tail are likely young molecular features formed in situ, whereas large CO features tilted with respect to the tail may have originated from dense gas complexes that were gradually pushed away from the disk.
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