We present MeerKAT H Iobservations of ESO 137-001, a quintessential jellyfish galaxy with long multi-phase tails formed due to the interaction with the intra-cluster medium of its host galaxy cluster, ACO 3627. Our observations reveal the presence of H Iin both the disc and outer regions of the galaxy for the first time, with a total H Imass of (3.5 ± 0.4)×108M⊙. ESO 137-001 is at an advanced stage of gas stripping; it is extremely H Ideficient and seems to have lost 90% of its initial H Imass; about 2/3 of the surviving H Iis found at larger radius than expected for a normal H Idisc and forms ∼40 kpc tail coincident with the tail detected at other wavelengths. Only ∼10% of the surviving H Iis still found within the stellar disc, consistent with the expectation of an outside-in truncation due to ram pressure. Similarly to other jellyfish galaxies, ESO137-001 has a high star formation rate for the low amount of H Idetected. We measure an H Idepletion time of 0.29 Gyr. However, when taking into account the total gas (H I+ H2) content, the depletion time is consistent with typical values measured in nearby spiral galaxies. This suggests that ESO 137-001 is at its current stage of ram pressure interaction characterised by an efficient H Istripping, rather than an enhanced conversion of H Ito H2, which was recently observed in some other jellyfish galaxies.
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MeerKAT HI commissioning observations of MHONGOOSE galaxy ESO 302-G014
Aims. We present the results of three commissioning H I observations obtained with the MeerKAT radio telescope. These observations make up part of the preparation for the forthcoming MHONGOOSE nearby galaxy survey, which is a MeerKAT large survey project that will study the accretion of gas in galaxies and the link between gas and star formation. Methods. We used the available H I data sets, along with ancillary data at other wavelengths, to study the morphology of the MHONGOOSE sample galaxy, ESO 302-G014, which is a nearby gas-rich dwarf galaxy. Results. We find that ESO 302-G014 has a lopsided, asymmetric outer disc with a low column density. In addition, we find a tail or filament of H I clouds extending away from the galaxy, as well as an isolated H I cloud some 20 kpc to the south of the galaxy. We suggest that these features indicate a minor interaction with a low-mass galaxy. Optical imaging shows a possible dwarf galaxy near the tail, but based on the current data, we cannot confirm any association with ESO 302-G014. Nonetheless, an interaction scenario with some kind of low-mass companion is still supported by the presence of a significant amount of molecular gas, which is almost equal to the stellar mass, and a number of prominent stellar clusters, which suggest recently triggered star formation. Conclusions. These data show that MeerKAT produces exquisite imaging data. The forthcoming full-depth survey observations of ESO 302-G014 and other sample galaxies will, therefore, offer insights into the fate of neutral gas as it moves from the intergalactic medium onto galaxies.
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- Award ID(s):
- 1903834
- PAR ID:
- 10280282
- Author(s) / Creator(s):
- ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »
- Date Published:
- Journal Name:
- Astronomy & Astrophysics
- Volume:
- 643
- ISSN:
- 0004-6361
- Page Range / eLocation ID:
- A147
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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