The better half - asymmetric star formation due to ram pressure in the EAGLE simulations

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The better half - asymmetric star formation due to ram pressure in the EAGLE simulations. / Troncoso-Iribarren, P.; Padilla, N.; Santander, C.; Lagos, C. D. P.; Garcia-Lambas, D.; Rodriguez, S.; Contreras, S.

In: Monthly Notices of the Royal Astronomical Society, Vol. 497, No. 4, 10.2020, p. 4145-4161.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Troncoso-Iribarren, P, Padilla, N, Santander, C, Lagos, CDP, Garcia-Lambas, D, Rodriguez, S & Contreras, S 2020, 'The better half - asymmetric star formation due to ram pressure in the EAGLE simulations', Monthly Notices of the Royal Astronomical Society, vol. 497, no. 4, pp. 4145-4161. https://doi.org/10.1093/mnras/staa274

APA

Troncoso-Iribarren, P., Padilla, N., Santander, C., Lagos, C. D. P., Garcia-Lambas, D., Rodriguez, S., & Contreras, S. (2020). The better half - asymmetric star formation due to ram pressure in the EAGLE simulations. Monthly Notices of the Royal Astronomical Society, 497(4), 4145-4161. https://doi.org/10.1093/mnras/staa274

Vancouver

Troncoso-Iribarren P, Padilla N, Santander C, Lagos CDP, Garcia-Lambas D, Rodriguez S et al. The better half - asymmetric star formation due to ram pressure in the EAGLE simulations. Monthly Notices of the Royal Astronomical Society. 2020 Oct;497(4):4145-4161. https://doi.org/10.1093/mnras/staa274

Author

Troncoso-Iribarren, P. ; Padilla, N. ; Santander, C. ; Lagos, C. D. P. ; Garcia-Lambas, D. ; Rodriguez, S. ; Contreras, S. / The better half - asymmetric star formation due to ram pressure in the EAGLE simulations. In: Monthly Notices of the Royal Astronomical Society. 2020 ; Vol. 497, No. 4. pp. 4145-4161.

Bibtex

@article{09d13e2933fa493d9c349dc28ff3b6d9,
title = "The better half - asymmetric star formation due to ram pressure in the EAGLE simulations",
abstract = "We use the EAGLE simulations to study the effects of the intracluster medium on the spatially resolved star formation activity in galaxies. We study three cases of galaxy asymmetry dividing each galaxy into two halves using the plane (i) perpendicular to the velocity direction, differentiating the galaxy part approaching the cluster centre, hereafter dubbed the 'leading half', and the opposite 'trailing half'; (ii) perpendicular to the radial position of the satellite to the centre of the cluster; and (iii) that maximizes the star formation rate (SFR) difference between the two halves. For (i), we find an enhancement of the SFR, star formation efficiency, and interstellar medium pressure in the leading half with respect to the trailing one and normal star-forming galaxies in the EAGLE simulation, and a clear overabundance of gas particles in their trailing. These results suggest that ram pressure is boosting the star formation by gas compression in the leading half, and transporting the gas to the trailing half. This effect is more pronounced in satellites of intermediate stellar masses 10(9.5)-10(10.5)M(circle dot), with gas masses above 10(9)M(circle dot), and located within one virial radius or in the most massive clusters. In (iii), we find an alignment between the velocity and the vector perpendicular to the plane that maximizes the SFR difference between the two halves. It suggests that finding this plane in real galaxies can provide an insight into the velocity direction.",
keywords = "galaxies: evolution, galaxies: clusters: intracluster medium, software: simulations, GALAXY FORMATION, GALACTIC OUTFLOWS, PHASE-SPACE, EVOLUTION, MASS, JELLYFISH, CLUSTER, RATES, SCHMIDT, RELEASE",
author = "P. Troncoso-Iribarren and N. Padilla and C. Santander and Lagos, {C. D. P.} and D. Garcia-Lambas and S. Rodriguez and S. Contreras",
year = "2020",
month = oct,
doi = "10.1093/mnras/staa274",
language = "English",
volume = "497",
pages = "4145--4161",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

RIS

TY - JOUR

T1 - The better half - asymmetric star formation due to ram pressure in the EAGLE simulations

AU - Troncoso-Iribarren, P.

AU - Padilla, N.

AU - Santander, C.

AU - Lagos, C. D. P.

AU - Garcia-Lambas, D.

AU - Rodriguez, S.

AU - Contreras, S.

PY - 2020/10

Y1 - 2020/10

N2 - We use the EAGLE simulations to study the effects of the intracluster medium on the spatially resolved star formation activity in galaxies. We study three cases of galaxy asymmetry dividing each galaxy into two halves using the plane (i) perpendicular to the velocity direction, differentiating the galaxy part approaching the cluster centre, hereafter dubbed the 'leading half', and the opposite 'trailing half'; (ii) perpendicular to the radial position of the satellite to the centre of the cluster; and (iii) that maximizes the star formation rate (SFR) difference between the two halves. For (i), we find an enhancement of the SFR, star formation efficiency, and interstellar medium pressure in the leading half with respect to the trailing one and normal star-forming galaxies in the EAGLE simulation, and a clear overabundance of gas particles in their trailing. These results suggest that ram pressure is boosting the star formation by gas compression in the leading half, and transporting the gas to the trailing half. This effect is more pronounced in satellites of intermediate stellar masses 10(9.5)-10(10.5)M(circle dot), with gas masses above 10(9)M(circle dot), and located within one virial radius or in the most massive clusters. In (iii), we find an alignment between the velocity and the vector perpendicular to the plane that maximizes the SFR difference between the two halves. It suggests that finding this plane in real galaxies can provide an insight into the velocity direction.

AB - We use the EAGLE simulations to study the effects of the intracluster medium on the spatially resolved star formation activity in galaxies. We study three cases of galaxy asymmetry dividing each galaxy into two halves using the plane (i) perpendicular to the velocity direction, differentiating the galaxy part approaching the cluster centre, hereafter dubbed the 'leading half', and the opposite 'trailing half'; (ii) perpendicular to the radial position of the satellite to the centre of the cluster; and (iii) that maximizes the star formation rate (SFR) difference between the two halves. For (i), we find an enhancement of the SFR, star formation efficiency, and interstellar medium pressure in the leading half with respect to the trailing one and normal star-forming galaxies in the EAGLE simulation, and a clear overabundance of gas particles in their trailing. These results suggest that ram pressure is boosting the star formation by gas compression in the leading half, and transporting the gas to the trailing half. This effect is more pronounced in satellites of intermediate stellar masses 10(9.5)-10(10.5)M(circle dot), with gas masses above 10(9)M(circle dot), and located within one virial radius or in the most massive clusters. In (iii), we find an alignment between the velocity and the vector perpendicular to the plane that maximizes the SFR difference between the two halves. It suggests that finding this plane in real galaxies can provide an insight into the velocity direction.

KW - galaxies: evolution

KW - galaxies: clusters: intracluster medium, software: simulations

KW - GALAXY FORMATION

KW - GALACTIC OUTFLOWS

KW - PHASE-SPACE

KW - EVOLUTION

KW - MASS

KW - JELLYFISH

KW - CLUSTER

KW - RATES

KW - SCHMIDT

KW - RELEASE

U2 - 10.1093/mnras/staa274

DO - 10.1093/mnras/staa274

M3 - Journal article

VL - 497

SP - 4145

EP - 4161

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 4

ER -

ID: 258027470