The Structure of Halo Gas around M33

Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00506406" target="_blank" >RIV/67985815:_____/16:00506406 - isvavai.cz</a>
Result on the web
<a href="http://dx.doi.org/10.1017/S1743921316011455" target="_blank" >http://dx.doi.org/10.1017/S1743921316011455</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1017/S1743921316011455" target="_blank" >10.1017/S1743921316011455</a>

Result language
angličtina
Original language name
The Structure of Halo Gas around M33
Original language description
Understanding the distribution of gas in and around galaxies is vital for our interpretation of galaxy formation and evolution. As part of the Arecibo Galaxy Environment Survey (AGES) we have observed the neutral hydrogen (HI) gas in and around the nearby Local Group galaxy M33 to a greater depth than previous observations. As part of this project we investigated the absence of optically detected dwarf galaxies in its neighbourhood, which is contrary to predictions of galaxy formation models. We observed 22 discrete clouds, 11 of which were previously undetected and none of which have optically detected counterparts. We find one particularly interesting hydrogen cloud, which has many similar characteristics to hydrogen distributed in the disk of a galaxy. This cloud, if it is at the distance of M33, has a HI mass of around 10(7) M-circle dot and a diameter of 18 kpc, making it larger in size than M33 itself.
Czech name
—
Czech description
—

Project
—
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year
2016
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Similar results(10)