ALMA reveals optically thin, highly excited CO gas in the jet-driven winds of the galaxy IC 5063

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00540088" target="_blank" >RIV/67985815:_____/16:00540088 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/201629689" target="_blank" >https://doi.org/10.1051/0004-6361/201629689</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201629689" target="_blank" >10.1051/0004-6361/201629689</a>

Jazyk výsledku

angličtina

Název v původním jazyce

ALMA reveals optically thin, highly excited CO gas in the jet-driven winds of the galaxy IC 5063

Popis výsledku v původním jazyce

Using CO (4-3) and (2-1) Atacama Large Millimeter Array (ALMA) data, we prove that the molecular gas in the jet-driven winds of the galaxy IC 5063 is more highly excited than the rest of the molecular gas in the disk of the same galaxy. On average, the CO(4-3)/CO(2-1) flux ratio is 1 for the disk and 5 for the jet accelerated or impacted gas. Spatially-resolved maps reveal that in regions associated with winds, the CO(4-3)/CO(2-1) flux ratio significantly exceeds the upper limit of 4 for optically thick gas. It frequently takes values between 5 and 11, and it occasionally further approaches the upper limit of 16 for optically thin gas. Excitation temperatures of 30 100K are common for the molecules in these regions. If all of the outflowing molecular gas is optically thin, at 30-50 K, then its mass is 2 x 10(6) M-circle dot. This lower mass limit is an order of magnitude below the mass derived from the CO(2-1) flux in the case of optically thick gas. Molecular winds can thus be less massive, but more easily detectable at high z than they were previously thought to be.

Název v anglickém jazyce

ALMA reveals optically thin, highly excited CO gas in the jet-driven winds of the galaxy IC 5063

Popis výsledku anglicky

Using CO (4-3) and (2-1) Atacama Large Millimeter Array (ALMA) data, we prove that the molecular gas in the jet-driven winds of the galaxy IC 5063 is more highly excited than the rest of the molecular gas in the disk of the same galaxy. On average, the CO(4-3)/CO(2-1) flux ratio is 1 for the disk and 5 for the jet accelerated or impacted gas. Spatially-resolved maps reveal that in regions associated with winds, the CO(4-3)/CO(2-1) flux ratio significantly exceeds the upper limit of 4 for optically thick gas. It frequently takes values between 5 and 11, and it occasionally further approaches the upper limit of 16 for optically thin gas. Excitation temperatures of 30 100K are common for the molecules in these regions. If all of the outflowing molecular gas is optically thin, at 30-50 K, then its mass is 2 x 10(6) M-circle dot. This lower mass limit is an order of magnitude below the mass derived from the CO(2-1) flux in the case of optically thick gas. Molecular winds can thus be less massive, but more easily detectable at high z than they were previously thought to be.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

—

Rok uplatnění

2016

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy & Astrophysics

ISSN

1432-0746

e-ISSN

—

Svazek periodika

595

Číslo periodika v rámci svazku

November

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

4

Strana od-do

L7

Kód UT WoS článku

000388573500142

EID výsledku v databázi Scopus

2-s2.0-84994651587