An Evolving and Mass-dependent sigma sSFR-M(* )Relation for Galaxies

Antonios Katsianis, Xianzhong Zheng, Valentino Gonzalez, Guillermo Blanc, Claudia del P. Lagos, Luke J. M. Davies, Peter Camps, Ana Trcka, Maarten Baes, Joop Schaye, James W. Trayford, Tom Theuns, Marko Stalevski

Research output: Contribution to journalArticle

Abstract

The scatter (sigma(sSFR)) of the specific star formation rates of galaxies is a measure of the diversity in their star formation histories (SFHs) at a given mass. In this paper, we employ the Evolution and Assembly of GaLaxies and their Environments (EAGLE) simulations to study the dependence of the sigma(sSFR) of galaxies on stellar mass (M-*) through the sigma(sSFR)-M-* relation in z similar to 0-4. We find that the relation evolves with time, with the dispersion depending on both stellar mass and redshift. The models point to an evolving U-shaped form for the sigma(sSFR)-M-* relation, with the scatter being minimal at a characteristic mass M*( )of 10(9.5) M-circle dot and increasing both at lower and higher masses. This implies that the diversity of SFHs increases toward both the low- and high-mass ends. We find that feedback from active galactic nuclei is important for increasing the sigma(sSFR) for high-mass objects. On the other hand, we suggest that feedback from supernovae increases the sigma(sSFR) of galaxies at the low-mass end. We also find that excluding galaxies that have experienced recent mergers does not significantly affect the sigma(sSFR)-M-* relation. Furthermore, we employ the EAGLE simulations in combination with the radiative transfer code SKIRT to evaluate the effect of SFR/stellar mass diagnostics in the sigma(sSFR)-M-* relation, and find that the SFR/M(* )methodologies (e.g., SED fitting, UV+IR, UV+IRX-beta) widely used in the literature to obtain intrinsic properties of galaxies have a large effect on the derived shape and normalization of the sigma(sSFR)-M-* relation.

Original languageEnglish
Article number11
Number of pages17
JournalAstrophysical Journal
Volume879
Issue number1
DOIs
Publication statusPublished - 1 Jul 2019

Cite this

Katsianis, Antonios ; Zheng, Xianzhong ; Gonzalez, Valentino ; Blanc, Guillermo ; Lagos, Claudia del P. ; Davies, Luke J. M. ; Camps, Peter ; Trcka, Ana ; Baes, Maarten ; Schaye, Joop ; Trayford, James W. ; Theuns, Tom ; Stalevski, Marko. / An Evolving and Mass-dependent sigma sSFR-M(* )Relation for Galaxies. In: Astrophysical Journal. 2019 ; Vol. 879, No. 1.
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abstract = "The scatter (sigma(sSFR)) of the specific star formation rates of galaxies is a measure of the diversity in their star formation histories (SFHs) at a given mass. In this paper, we employ the Evolution and Assembly of GaLaxies and their Environments (EAGLE) simulations to study the dependence of the sigma(sSFR) of galaxies on stellar mass (M-*) through the sigma(sSFR)-M-* relation in z similar to 0-4. We find that the relation evolves with time, with the dispersion depending on both stellar mass and redshift. The models point to an evolving U-shaped form for the sigma(sSFR)-M-* relation, with the scatter being minimal at a characteristic mass M*( )of 10(9.5) M-circle dot and increasing both at lower and higher masses. This implies that the diversity of SFHs increases toward both the low- and high-mass ends. We find that feedback from active galactic nuclei is important for increasing the sigma(sSFR) for high-mass objects. On the other hand, we suggest that feedback from supernovae increases the sigma(sSFR) of galaxies at the low-mass end. We also find that excluding galaxies that have experienced recent mergers does not significantly affect the sigma(sSFR)-M-* relation. Furthermore, we employ the EAGLE simulations in combination with the radiative transfer code SKIRT to evaluate the effect of SFR/stellar mass diagnostics in the sigma(sSFR)-M-* relation, and find that the SFR/M(* )methodologies (e.g., SED fitting, UV+IR, UV+IRX-beta) widely used in the literature to obtain intrinsic properties of galaxies have a large effect on the derived shape and normalization of the sigma(sSFR)-M-* relation.",
keywords = "cosmology: theory, galaxies: star formation, surveys, STAR-FORMATION-RATE, DUST RADIATIVE-TRANSFER, ACTIVE GALACTIC NUCLEI, M-ASTERISK RELATION, DARK-MATTER HALOES, BLACK-HOLE GROWTH, MAJOR MERGER RATE, STELLAR MASS, EAGLE SIMULATIONS, FORMATION RATES",
author = "Antonios Katsianis and Xianzhong Zheng and Valentino Gonzalez and Guillermo Blanc and Lagos, {Claudia del P.} and Davies, {Luke J. M.} and Peter Camps and Ana Trcka and Maarten Baes and Joop Schaye and Trayford, {James W.} and Tom Theuns and Marko Stalevski",
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Katsianis, A, Zheng, X, Gonzalez, V, Blanc, G, Lagos, CDP, Davies, LJM, Camps, P, Trcka, A, Baes, M, Schaye, J, Trayford, JW, Theuns, T & Stalevski, M 2019, 'An Evolving and Mass-dependent sigma sSFR-M(* )Relation for Galaxies' Astrophysical Journal, vol. 879, no. 1, 11. https://doi.org/10.3847/1538-4357/ab1f8d

An Evolving and Mass-dependent sigma sSFR-M(* )Relation for Galaxies. / Katsianis, Antonios; Zheng, Xianzhong; Gonzalez, Valentino; Blanc, Guillermo; Lagos, Claudia del P.; Davies, Luke J. M.; Camps, Peter; Trcka, Ana; Baes, Maarten; Schaye, Joop; Trayford, James W.; Theuns, Tom; Stalevski, Marko.

In: Astrophysical Journal, Vol. 879, No. 1, 11, 01.07.2019.

Research output: Contribution to journalArticle

TY - JOUR

T1 - An Evolving and Mass-dependent sigma sSFR-M(* )Relation for Galaxies

AU - Katsianis, Antonios

AU - Zheng, Xianzhong

AU - Gonzalez, Valentino

AU - Blanc, Guillermo

AU - Lagos, Claudia del P.

AU - Davies, Luke J. M.

AU - Camps, Peter

AU - Trcka, Ana

AU - Baes, Maarten

AU - Schaye, Joop

AU - Trayford, James W.

AU - Theuns, Tom

AU - Stalevski, Marko

PY - 2019/7/1

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N2 - The scatter (sigma(sSFR)) of the specific star formation rates of galaxies is a measure of the diversity in their star formation histories (SFHs) at a given mass. In this paper, we employ the Evolution and Assembly of GaLaxies and their Environments (EAGLE) simulations to study the dependence of the sigma(sSFR) of galaxies on stellar mass (M-*) through the sigma(sSFR)-M-* relation in z similar to 0-4. We find that the relation evolves with time, with the dispersion depending on both stellar mass and redshift. The models point to an evolving U-shaped form for the sigma(sSFR)-M-* relation, with the scatter being minimal at a characteristic mass M*( )of 10(9.5) M-circle dot and increasing both at lower and higher masses. This implies that the diversity of SFHs increases toward both the low- and high-mass ends. We find that feedback from active galactic nuclei is important for increasing the sigma(sSFR) for high-mass objects. On the other hand, we suggest that feedback from supernovae increases the sigma(sSFR) of galaxies at the low-mass end. We also find that excluding galaxies that have experienced recent mergers does not significantly affect the sigma(sSFR)-M-* relation. Furthermore, we employ the EAGLE simulations in combination with the radiative transfer code SKIRT to evaluate the effect of SFR/stellar mass diagnostics in the sigma(sSFR)-M-* relation, and find that the SFR/M(* )methodologies (e.g., SED fitting, UV+IR, UV+IRX-beta) widely used in the literature to obtain intrinsic properties of galaxies have a large effect on the derived shape and normalization of the sigma(sSFR)-M-* relation.

AB - The scatter (sigma(sSFR)) of the specific star formation rates of galaxies is a measure of the diversity in their star formation histories (SFHs) at a given mass. In this paper, we employ the Evolution and Assembly of GaLaxies and their Environments (EAGLE) simulations to study the dependence of the sigma(sSFR) of galaxies on stellar mass (M-*) through the sigma(sSFR)-M-* relation in z similar to 0-4. We find that the relation evolves with time, with the dispersion depending on both stellar mass and redshift. The models point to an evolving U-shaped form for the sigma(sSFR)-M-* relation, with the scatter being minimal at a characteristic mass M*( )of 10(9.5) M-circle dot and increasing both at lower and higher masses. This implies that the diversity of SFHs increases toward both the low- and high-mass ends. We find that feedback from active galactic nuclei is important for increasing the sigma(sSFR) for high-mass objects. On the other hand, we suggest that feedback from supernovae increases the sigma(sSFR) of galaxies at the low-mass end. We also find that excluding galaxies that have experienced recent mergers does not significantly affect the sigma(sSFR)-M-* relation. Furthermore, we employ the EAGLE simulations in combination with the radiative transfer code SKIRT to evaluate the effect of SFR/stellar mass diagnostics in the sigma(sSFR)-M-* relation, and find that the SFR/M(* )methodologies (e.g., SED fitting, UV+IR, UV+IRX-beta) widely used in the literature to obtain intrinsic properties of galaxies have a large effect on the derived shape and normalization of the sigma(sSFR)-M-* relation.

KW - cosmology: theory

KW - galaxies: star formation

KW - surveys

KW - STAR-FORMATION-RATE

KW - DUST RADIATIVE-TRANSFER

KW - ACTIVE GALACTIC NUCLEI

KW - M-ASTERISK RELATION

KW - DARK-MATTER HALOES

KW - BLACK-HOLE GROWTH

KW - MAJOR MERGER RATE

KW - STELLAR MASS

KW - EAGLE SIMULATIONS

KW - FORMATION RATES

U2 - 10.3847/1538-4357/ab1f8d

DO - 10.3847/1538-4357/ab1f8d

M3 - Article

VL - 879

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 11

ER -