Bibcode
Leaman, Ryan; Fragkoudi, Francesca; Querejeta, Miguel; Leung, Gigi Y. C.; Gadotti, Dimitri A.; Husemann, Bernd; Falcón-Barroso, Jesus; Sánchez-Blázquez, Patricia; van de Ven, Glenn; Kim, Taehyun; Coelho, Paula; Lyubenova, Mariya; de Lorenzo-Cáceres, Adriana; Martig, Marie; Martinez-Valpuesta, Inma; Neumann, Justus; Pérez, Isabel; Seidel, Marja
Referencia bibliográfica
Monthly Notices of the Royal Astronomical Society, Volume 488, Issue 3, p.3904-3928
Advertised on:
9
2019
Número de citas
21
Número de citas referidas
19
Descripción
Stellar feedback plays a significant role in modulating star formation,
redistributing metals, and shaping the baryonic and dark structure of
galaxies - however, the efficiency of its energy deposition to the
interstellar medium is challenging to constrain observationally. Here we
leverage HST and ALMA imaging of a molecular gas and dust shell (M_{
H_2} ˜ 2× 105 M_{⊙ }) in an outflow from the
nuclear star-forming ring of the galaxy NGC 3351, to serve as a boundary
condition for a dynamical and energetic analysis of the outflowing
ionized gas seen in our MUSE TIMER survey. We use STARBURST99 models and
prescriptions for feedback from simulations to demonstrate that the
observed star formation energetics can reproduce the ionized and
molecular gas dynamics - provided a dominant component of the momentum
injection comes from direct photon pressure from young stars, on top of
supernovae, photoionization heating, and stellar winds. The mechanical
energy budget from these sources is comparable to low luminosity active
galactic neuclei, suggesting that stellar feedback can be a relevant
driver of bulk gas motions in galaxy centres - although here
≲10-3 of the ionized gas mass is escaping the galaxy. We
test several scenarios for the survival/formation of the cold gas in the
outflow, including in situ condensation and cooling. Interestingly, the
geometry of the molecular gas shell, observed magnetic field strengths
and emission line diagnostics are consistent with a scenario where
magnetic field lines aided survival of the dusty ISM as it was initially
launched (with mass-loading factor ≲1) from the ring by stellar
feedback. This system's unique feedback-driven morphology can hopefully
serve as a useful litmus test for feedback prescriptions in
magnetohydrodynamical galaxy simulations.
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Bienvenida a la página web del g rupo de investigación Traces of Galaxy Formation. Somos un grupo de investigación amplio, diverso y muy activo cuyo objetivo principal es entender la formación de galaxias en el Universo de una manera lo más completa posible. Con el estudio detellado de las poblaciones estelares como bandera, estamos constantemente
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