The high-redshift SFR M relation is sensitive to the employed star formation rate and stellar mass indicators: towards addressing the tension between observations and simulations
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The high-redshift SFR M relation is sensitive to the employed star formation rate and stellar mass indicators : towards addressing the tension between observations and simulations. / Katsianis, A.; Gonzalez, Eusebio Rial; Barrientos, D.; Yang, X.; Lagos, C. D. P.; Schaye, J.; Camps, P.; Trcka, A.; Baes, M.; Stalevski, M.; Blanc, G. A.; Theuns, T.
In: Monthly Notices of the Royal Astronomical Society, Vol. 492, No. 4, 01.03.2020, p. 5592-5606.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - The high-redshift SFR M relation is sensitive to the employed star formation rate and stellar mass indicators
T2 - towards addressing the tension between observations and simulations
AU - Katsianis, A.
AU - Gonzalez, Eusebio Rial
AU - Barrientos, D.
AU - Yang, X.
AU - Lagos, C. D. P.
AU - Schaye, J.
AU - Camps, P.
AU - Trcka, A.
AU - Baes, M.
AU - Stalevski, M.
AU - Blanc, G. A.
AU - Theuns, T.
PY - 2020/3/1
Y1 - 2020/3/1
N2 - There is a severe tension between the observed star formation rate (SFR)-stellar mass (M,) relations reported by different authors at z = En addition, the observations have not been successfully reproduced by state-of-the-art cosmological simulations that tend to predict a factor of 2-4 smaller SFRs at a fixed M. We examine the evolution of the SFR-M, relation of z = 1-4 galaxies using the SKIRT simulated spectral energy distributions of galaxies sampled from the Evolution and Assembly of GaLaxies and their Environments simulations. We derive SFRs and stellar masses by mimicking different observational techniques. We find that the tension between observed and simulated SFR-M* relations is largely alleviated if similar methods are used to infer the galaxy properties. We find that relations relying on infrared wavelengths (e.g. 24 jtm, MIPS- 24, 70, and 160 um or SPIRE- 250, 350, and 500 um) have SFRs that exceed the intrinsic relation by 0.5 dex. Relations that rely on the spectral energy distribution fitting technique underpredict the SFRs at a fixed stellar mass by-0.5 dex at z 4 but overpredict the measurements by 0.3 dex at z 1. Relations relying on dust corrected rest-frame ultraviolet luminosities, are flatter since they overpredict/underpredict SFRs for low/high star-forming objects and yield deviations from the intrinsic relation from 0.10 to-0.13 dex at z 4. We suggest that the severe tension between different observational studies can be broadly explained by the fact that different groups employ different techniques to infer their SFRs.
AB - There is a severe tension between the observed star formation rate (SFR)-stellar mass (M,) relations reported by different authors at z = En addition, the observations have not been successfully reproduced by state-of-the-art cosmological simulations that tend to predict a factor of 2-4 smaller SFRs at a fixed M. We examine the evolution of the SFR-M, relation of z = 1-4 galaxies using the SKIRT simulated spectral energy distributions of galaxies sampled from the Evolution and Assembly of GaLaxies and their Environments simulations. We derive SFRs and stellar masses by mimicking different observational techniques. We find that the tension between observed and simulated SFR-M* relations is largely alleviated if similar methods are used to infer the galaxy properties. We find that relations relying on infrared wavelengths (e.g. 24 jtm, MIPS- 24, 70, and 160 um or SPIRE- 250, 350, and 500 um) have SFRs that exceed the intrinsic relation by 0.5 dex. Relations that rely on the spectral energy distribution fitting technique underpredict the SFRs at a fixed stellar mass by-0.5 dex at z 4 but overpredict the measurements by 0.3 dex at z 1. Relations relying on dust corrected rest-frame ultraviolet luminosities, are flatter since they overpredict/underpredict SFRs for low/high star-forming objects and yield deviations from the intrinsic relation from 0.10 to-0.13 dex at z 4. We suggest that the severe tension between different observational studies can be broadly explained by the fact that different groups employ different techniques to infer their SFRs.
KW - galaxies: evolution
KW - galaxies: star formation
KW - SPECTRAL ENERGY-DISTRIBUTION
KW - M-ASTERISK RELATION
KW - TO 2 GALAXIES
KW - FORMING GALAXIES
KW - EAGLE SIMULATIONS
KW - MAIN-SEQUENCE
KW - POPULATION PROPERTIES
KW - RADIATIVE-TRANSFER
KW - FORMATION HISTORY
KW - CLUSTER GALAXIES
U2 - 10.1093/mnras/staa157
DO - 10.1093/mnras/staa157
M3 - Journal article
VL - 492
SP - 5592
EP - 5606
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 4
ER -
ID: 258028741