Constraining the z ∼ 1 Initial Mass Function with HST and JWST Lensed Stars in MACS J0416.1−2403
Authors:
- Sung Kei LiSLSung Kei Li
- Jose M. DiegoJDJose M. Diego
- Ashish K. MeenaAMAshish K. Meena
- Jeremy LimJLJeremy Lim
- Leo W. H. FungLFLeo W. H. Fung
- Arsen LevitskiyALArsen Levitskiy
- James NianiasJNJames Nianias
- Jose M. PalenciaJPJose M. Palencia
- Hayley WilliamsHWHayley Williams
- Jiashuo ZhangJZJiashuo Zhang
- Alfred AmruthAAAlfred Amruth
- Thomas J. BroadhurstTBThomas J. Broadhurst
Open Access
- 23 July 2025
- journal article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 988 (2) , 178
Abstract
Our understanding of galaxy properties and evolution is contingent on knowing the initial mass function (IMF), and yet to date the IMF is constrained only to local galaxies. Individual stars are now becoming routinely detected at cosmological distances, where luminous stars such as supergiants in background galaxies strongly lensed by galaxy clusters are temporarily further magnified by huge factors (up to 104) by intracluster stars, thus being detected as transients. The detection rate of these events depends on the abundance of luminous stars in the background galaxy and is thus sensitive to the IMF and the star formation history (SFH), especially for the blue supergiants detected as transients in the rest-frame ultraviolet/optical filters. As a proof of concept, we use simple SFH and IMF models constrained by spectral energy distributions (SEDs) to see how well we can predict the Hubble Space Telescope and James Webb Space Telescope transient detection rate in a lensed arc dubbed “Spock” (z = 1.0054). We find that demanding a simultaneous fit of the SED and the transient detection rate places constraints on the IMF, independent of the assumed simple SFH model. We conclude that our likelihood analysis indicates that the data definitively prefers the “Spock” galaxy to have a Salpeter IMF (α = 2.35) rather than a top-heavy IMF (α = 1)—which is thought to be the case in the early universe—with no clear excess of supergiants above the standard IMF.Keywords
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Funding Information
- Research Grants Council, University Grants Committee (GRF 17312122)
- Research Grants Council, University Grants Committee (C6017-20G)
- Ministerio de Ciencia, Innovación y Universidades (PID2022-128896NV-C51)
- UKRI ∣ Science and Technology Facilities Council (ST/X001075/1)
- MEC ∣ Agencia Estatal de Investigación (MDM-2017-0765-20-2)
- National Aeronautics and Space Administration (NAG5-12460)
- National Aeronautics and Space Administration (NNX14AN10G)
- NASA ∣ Goddard Space Flight Center (80NSSC18K0200)
This publication has 95 references indexed in Scilit:
- Identification of more than 40 gravitationally magnified stars in a galaxy at redshift 0.725Nature Astronomy, 2025
- Stress testing ΛCDM with high-redshift galaxy candidatesNature Astronomy, 2023
- Stellar initial mass function varies with metallicity and timeNature, 2023
- The faint light in groups and clusters of galaxiesNature Astronomy, 2022
- Array programming with NumPyNature, 2020
- SciPy 1.0: fundamental algorithms for scientific computing in PythonNature Methods, 2020
- The Dawes Review 8: Measuring the Stellar Initial Mass FunctionPublications of the Astronomical Society of Australia, 2018
- Extreme magnification of an individual star at redshift 1.5 by a galaxy-cluster lensNature Astronomy, 2018
- Two peculiar fast transients in a strongly lensed host galaxyNature Astronomy, 2018
- On the variation of the initial mass functionMonthly Notices of the Royal Astronomical Society, 2001