An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
We present a new empirical framework modeling the metallicity and star formation history (SFH) dependence of X-ray luminous ( L ≳ 10 ^36 erg s ^−1 ) point-source population X-ray luminosity functions (XLFs) in normal galaxies. We expect that the X-ray point-source populations are dominated by X-ray...
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2024-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ad8de7 |
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| author | Bret D. Lehmer Erik B. Monson Rafael T. Eufrasio Amirnezam Amiri Keith Doore Antara Basu-Zych Kristen Garofali Lidia Oskinova Jeff J. Andrews Vallia Antoniou Robel Geda Jenny E. Greene Konstantinos Kovlakas Margaret Lazzarini Chris T. Richardson |
| author_facet | Bret D. Lehmer Erik B. Monson Rafael T. Eufrasio Amirnezam Amiri Keith Doore Antara Basu-Zych Kristen Garofali Lidia Oskinova Jeff J. Andrews Vallia Antoniou Robel Geda Jenny E. Greene Konstantinos Kovlakas Margaret Lazzarini Chris T. Richardson |
| author_sort | Bret D. Lehmer |
| collection | DOAJ |
| description | We present a new empirical framework modeling the metallicity and star formation history (SFH) dependence of X-ray luminous ( L ≳ 10 ^36 erg s ^−1 ) point-source population X-ray luminosity functions (XLFs) in normal galaxies. We expect that the X-ray point-source populations are dominated by X-ray binaries (XRBs), with contributions from supernova remnants near the low luminosity end of our observations. Our framework is calibrated using the collective statistical power of 3731 X-ray detected point sources within 88 Chandra-observed galaxies at D ≲ 40 Mpc that span broad ranges of metallicity ( Z ≈ 0.03–2 Z _⊙ ), SFH, and morphology (dwarf irregulars, late types, and early types). Our best-fitting models indicate that the XLF normalization per unit stellar mass declines by ≈2–3 dex from 10 Myr to 10 Gyr, with a slower age decline for low-metallicity populations. The shape of the XLF for luminous X-ray sources ( L ≳ 10 ^38 erg s ^−1 ) significantly steepens with increasing age and metallicity, while the lower-luminosity XLF appears to flatten with increasing age. Integration of our models provides predictions for X-ray scaling relations that agree very well with past results presented in the literature, including, e.g., the L _X –SFR– Z relation for high-mass XRBs in young stellar populations as well as the L _X / M _⋆ ratio observed in early-type galaxies that harbor old populations of low-mass XRBs. The model framework and data sets presented in this paper further provide unique benchmarks that can be used for calibrating binary population synthesis models. |
| format | Article |
| id | doaj-art-925b21583c3f46348d4a85f31b072e0a |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-925b21583c3f46348d4a85f31b072e0a2024-12-13T06:59:43ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01977218910.3847/1538-4357/ad8de7An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in GalaxiesBret D. Lehmer0https://orcid.org/0000-0003-2192-3296Erik B. Monson1https://orcid.org/0000-0001-8473-5140Rafael T. Eufrasio2https://orcid.org/0000-0002-2987-1796Amirnezam Amiri3https://orcid.org/0000-0002-8553-1964Keith Doore4https://orcid.org/0000-0001-5035-4016Antara Basu-Zych5https://orcid.org/0000-0001-8525-4920Kristen Garofali6https://orcid.org/0000-0002-9202-8689Lidia Oskinova7https://orcid.org/0000-0003-0708-4414Jeff J. Andrews8https://orcid.org/0000-0001-5261-3923Vallia Antoniou9https://orcid.org/0000-0001-7539-1593Robel Geda10https://orcid.org/0000-0003-1509-9966Jenny E. Greene11https://orcid.org/0000-0002-5612-3427Konstantinos Kovlakas12https://orcid.org/0000-0003-3684-964XMargaret Lazzarini13https://orcid.org/0000-0003-3252-352XChris T. Richardson14https://orcid.org/0000-0002-3703-0719Department of Physics, University of Arkansas , 226 Physics Building, 825 West Dickson Street, Fayetteville, AR 72701, USA ; lehmer@uark.edu; Arkansas Center for Space and Planetary Sciences, University of Arkansas , 332 N. Arkansas Avenue, Fayetteville, AR 72701, USADepartment of Astronomy and Astrophysics, 525 Davey Lab, The Pennsylvania State University , University Park, PA 16802, USADepartment of Physics, University of Arkansas , 226 Physics Building, 825 West Dickson Street, Fayetteville, AR 72701, USA ; lehmer@uark.eduDepartment of Physics, University of Arkansas , 226 Physics Building, 825 West Dickson Street, Fayetteville, AR 72701, USA ; lehmer@uark.eduDepartment of Physics, University of Arkansas , 226 Physics Building, 825 West Dickson Street, Fayetteville, AR 72701, USA ; lehmer@uark.edu; Arkansas Center for Space and Planetary Sciences, University of Arkansas , 332 N. Arkansas Avenue, Fayetteville, AR 72701, USACenter for Space Science and Technology, University of Maryland Baltimore County , 1000 Hilltop Circle, Baltimore, MD 21250, USA; NASA Goddard Space Flight Center , Code 662, Greenbelt, MD 20771, USANASA Goddard Space Flight Center , Code 662, Greenbelt, MD 20771, USA; William H. miller III Department of Physics and Astronomy, Johns Hopkins University , Baltimore, MD 21218, USAInstitute for Physics and Astronomy University of Potsdam , Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, GermanyDepartment of Physics, University of Florida , 2001 Museum Road, Gainesville, FL 32611, USADepartment of Physics & Astronomy, Texas Tech University , Box 41051, Lubbock, TX 79409-1051, USA; Center for Astrophysics ∣ Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USADepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USADepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USAInstitute of Space Sciences (ICE, CSIC) , Campus UAB, Carrer de Can Magrans s/n, E-08193, Barcelona, Spain; Institut d’Estudis Espacials de Catalunya (IEEC) , Edifici RDIT, Campus UPC, 08860 Castelldefels (Barcelona), SpainDepartment of Physics & Astronomy, California State University Los Angeles , Los Angeles, CA 90032, USADepartment of Physics & Astronomy, Elon University , 100 Campus Drive, Elon, NC 27244, USAWe present a new empirical framework modeling the metallicity and star formation history (SFH) dependence of X-ray luminous ( L ≳ 10 ^36 erg s ^−1 ) point-source population X-ray luminosity functions (XLFs) in normal galaxies. We expect that the X-ray point-source populations are dominated by X-ray binaries (XRBs), with contributions from supernova remnants near the low luminosity end of our observations. Our framework is calibrated using the collective statistical power of 3731 X-ray detected point sources within 88 Chandra-observed galaxies at D ≲ 40 Mpc that span broad ranges of metallicity ( Z ≈ 0.03–2 Z _⊙ ), SFH, and morphology (dwarf irregulars, late types, and early types). Our best-fitting models indicate that the XLF normalization per unit stellar mass declines by ≈2–3 dex from 10 Myr to 10 Gyr, with a slower age decline for low-metallicity populations. The shape of the XLF for luminous X-ray sources ( L ≳ 10 ^38 erg s ^−1 ) significantly steepens with increasing age and metallicity, while the lower-luminosity XLF appears to flatten with increasing age. Integration of our models provides predictions for X-ray scaling relations that agree very well with past results presented in the literature, including, e.g., the L _X –SFR– Z relation for high-mass XRBs in young stellar populations as well as the L _X / M _⋆ ratio observed in early-type galaxies that harbor old populations of low-mass XRBs. The model framework and data sets presented in this paper further provide unique benchmarks that can be used for calibrating binary population synthesis models.https://doi.org/10.3847/1538-4357/ad8de7X-ray binary starsStellar evolutionary modelsGalaxy evolutionStar formationSpectral energy distributionX-ray astronomy |
| spellingShingle | Bret D. Lehmer Erik B. Monson Rafael T. Eufrasio Amirnezam Amiri Keith Doore Antara Basu-Zych Kristen Garofali Lidia Oskinova Jeff J. Andrews Vallia Antoniou Robel Geda Jenny E. Greene Konstantinos Kovlakas Margaret Lazzarini Chris T. Richardson An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies The Astrophysical Journal X-ray binary stars Stellar evolutionary models Galaxy evolution Star formation Spectral energy distribution X-ray astronomy |
| title | An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies |
| title_full | An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies |
| title_fullStr | An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies |
| title_full_unstemmed | An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies |
| title_short | An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies |
| title_sort | empirical framework characterizing the metallicity and star formation history dependence of x ray binary population formation and emission in galaxies |
| topic | X-ray binary stars Stellar evolutionary models Galaxy evolution Star formation Spectral energy distribution X-ray astronomy |
| url | https://doi.org/10.3847/1538-4357/ad8de7 |
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