The Stellar Age Dependence of X-ray Emission from Normal Star-Forming Galaxies in the GOODS Fields

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dc.contributor.authorGilbertson, Woodrow
dc.contributor.authorLehmer, Bret
dc.contributor.authorDoore, Keith
dc.contributor.authorEufrasio, Rafael
dc.contributor.authorBasu-Zych, Antara
dc.contributor.authorBrandt, William
dc.contributor.authorFragos, Tassos
dc.contributor.authorGarofali, Kristen
dc.contributor.authorKovlakas, Konstantinos
dc.contributor.authorLuo, Bin
dc.contributor.authorTozzi, Paolo
dc.contributor.authorVito, Fabio
dc.contributor.authorWilliams, Benjamin F.
dc.contributor.authorXue, Yongquan
dc.date.accessioned2022-01-19T17:16:31Z
dc.date.available2022-01-19T17:16:31Z
dc.date.issued2021-12-20
dc.description.abstractThe Chandra Deep Field-South and North surveys (CDFs) provide unique windows into the cosmic history of X-ray emission from normal (non-active) galaxies. Scaling relations of normal galaxy X-ray luminosity (Lₓ The Chandra Deep Field-South and North surveys (CDFs) provide unique windows into the cosmic history of X-ray emission from normal (non-active) galaxies. Scaling relations of normal galaxy X-ray luminosity (Lₓ) with star formation rate (SFR) and stellar mass (M⋆) have been used to show that the formation rates of lowmass and high-mass X-ray binaries (LMXBs and HMXBs, respectively) evolve with redshift across z ≈ 0–2 following LHMXB/SFR ∝ (1 + z) and Lₗₘₓ/M⋆ ∝ (1 + z) ²−³. However, these measurements alone do not directly reveal the physical mechanisms behind the redshift evolution of X-ray binaries (XRBs). We derive star-formation histories for a sample of 344 normal galaxies in the CDFs, using spectral energy distribution (SED) fitting of FUV-to-FIR photometric data, and construct a self-consistent, age-dependent model of the Xray emission from the galaxies. Our model quantifies how X-ray emission from hot gas and XRB populations vary as functions of host stellar-population age. We find that (1) the ratio Lₓ/M⋆ declines by a factor of ∼1000 from 0–10 Gyr and (2) the X-ray SED becomes harder with increasing age, consistent with a scenario in which the hot gas contribution to the X-ray SED declines quickly for ages above 10 Myr. When dividing our sample into subsets based on metallicity, we find some indication that Lₓ/M⋆ is elevated for low-metallicity galaxies, consistent with recent studies of X-ray scaling relations. However, additional statistical constraints are required to quantify both the age and metallicity dependence of X-ray emission from star-forming galaxies.The Chandra Deep Field-South and North surveys (CDFs) provide unique windows into the cosmic history of X-ray emission from normal (non-active) galaxies. Scaling relations of normal galaxy X-ray luminosity (Lₓ) with star formation rate (SFR) and stellar mass (M⋆) have been used to show that the formation rates of lowmass and high-mass X-ray binaries (LMXBs and HMXBs, respectively) evolve with redshift across z ≈ 0–2 following LHMXB/SFR ∝ (1 + z) and Lₗₘₓ/M⋆ ∝ (1 + z) ²−³. However, these measurements alone do not directly reveal the physical mechanisms behind the redshift evolution of X-ray binaries (XRBs). We derive star-formation histories for a sample of 344 normal galaxies in the CDFs, using spectral energy distribution (SED) fitting of FUV-to-FIR photometric data, and construct a self-consistent, age-dependent model of the Xray emission from the galaxies. Our model quantifies how X-ray emission from hot gas and XRB populations vary as functions of host stellar-population age. We find that (1) the ratio Lₓ/M⋆ declines by a factor of ∼1000 from 0–10 Gyr and (2) the X-ray SED becomes harder with increasing age, consistent with a scenario in which the hot gas contribution to the X-ray SED declines quickly for ages above 10 Myr. When dividing our sample into subsets based on metallicity, we find some indication that Lₓ/M⋆ is elevated for low-metallicity galaxies, consistent with recent studies of X-ray scaling relations. However, additional statistical constraints are required to quantify both the age and metallicity dependence of X-ray emission from star-forming galaxies.) with star formation rate (SFR) and stellar mass (M⋆) have been used to show that the formation rates of lowmass and high-mass X-ray binaries (LMXBs and HMXBs, respectively) evolve with redshift across z ≈ 0–2 following LHMXB/SFR ∝ (1 + z) and Lₗₘₓ/M⋆ ∝ (1 + z) ²−³. However, these measurements alone do not directly reveal the physical mechanisms behind the redshift evolution of X-ray binaries (XRBs). We derive star-formation histories for a sample of 344 normal galaxies in the CDFs, using spectral energy distribution (SED) fitting of FUV-to-FIR photometric data, and construct a self-consistent, age-dependent model of the Xray emission from the galaxies. Our model quantifies how X-ray emission from hot gas and XRB populations vary as functions of host stellar-population age. We find that (1) the ratio Lₓ/M⋆ declines by a factor of ∼1000 from 0–10 Gyr and (2) the X-ray SED becomes harder with increasing age, consistent with a scenario in which the hot gas contribution to the X-ray SED declines quickly for ages above 10 Myr. When dividing our sample into subsets based on metallicity, we find some indication that Lₓ/M⋆ is elevated for low-metallicity galaxies, consistent with recent studies of X-ray scaling relations. However, additional statistical constraints are required to quantify both the age and metallicity dependence of X-ray emission from star-forming galaxies.en_US
dc.description.sponsorshipWe thank the anonymous referee for their helpful comments, which have improved the quality of this paper. We gratefully acknowledge financial support from the NASA Astrophysics Data Analysis Program (ADAP) grant 80NSSC20K0444 (W.G.,B.D.L.,K.D.,R.T.E.) and Chandra X-ray Center (CXC) grant AR9-20008X (W.G.,B.D.L.). W.N.B. acknowledges support from the V.M. Willaman Endowment. T.F. acknowledges support from the Swiss National Science Foundation Professorship grant (project number PP00P2 176868). K.G. is supported by an appointment to the NASA Postdoctoral Program at NASA Goddard Space Flight Center, administered by Universities Space Research Association under contract with NASA. B.L. acknowledges financial support from the National Natural Science Foundation of China grant 11991053, China Manned Space Project grants NO. CMS-CSST-2021-A05 and NO. CMS-CSST-2021-A06. Y.Q.X. acknowledges support from NSFC-12025303, 11890693, 11421303, the CAS Frontier Science Key Research Program (QYZDJ-SSW-SLH006), the K.C. Wong Education Foundation, and the science research grants from the China Manned Space Project with NO. CMSCSST-2021-A06. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5- 26555. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Centro de Astrobiologia (CAB/INTA), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC), and the Arkansas High Performance Computing Center, which is funded through multiple National Science Foundation grants and the Arkansas Economic Development Commission. The material is based upon work supported by NASA under award number 80GSFC21M0002.en_US
dc.description.urihttps://arxiv.org/abs/2112.03194en_US
dc.format.extent23 pagesen_US
dc.genrejournal articlesen_US
dc.genrepreprintsen_US
dc.identifierdoi:10.13016/m2xilc-msjs
dc.identifier.urihttp://hdl.handle.net/11603/24019
dc.language.isoen_USen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Center for Space Sciences and Technology
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.en_US
dc.rightsAttribution 4.0 International (CC BY 4.0)*
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/*
dc.titleThe Stellar Age Dependence of X-ray Emission from Normal Star-Forming Galaxies in the GOODS Fieldsen_US
dc.typeTexten_US
dcterms.creatorhttps://orcid.org/0000-0001-8525-4920en_US

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