Identification and Characterization of a Large Sample of Distant Active Dwarf Galaxies in XMM-SERVS

Zou, Fan; Brandt, W. N.; Ni, Qingling; Zhu, Shifu; Alexander, David M.; Bauer, Franz E.; Chen, Chien-Ting J.; Luo, Bin; Sun, Mouyuan; Vignali, Cristian; Vito, Fabio; Xue, Yongquan; Yan, Wei

doi:10.3847/1538-4357/acce39

“…A similar analysis of our sample shows inconsistent results, with luminosities ranging from L X ≈ 10 38-44 regardless of galaxy mass for both the low-metallicity and control samples. We note that the XMM-SERVS survey used in Zou et al (2023) has significant improvements in sensitivity over a large subset of the targets reported here, and that the work probes a larger range of redshifts (z < 1).…”

Section: Comparison With Previous Studiesmentioning

confidence: 89%

“…We can further compare with the Zou et al (2023) study of dwarf galaxies in the XMM-SERVS field. Their sample shows a relatively small distribution of X-ray luminosities (L X ≈ 10 40-42 erg s −1 ) for their lowest-mass targets (M * ≈ 10 7 M e ), with much greater variation (L X ≈ 10 40-44 erg s −1 ) in higher masses (M * ≈ 10 9 M e ; see Figure 6 in Zou et al 2023).…”

Section: Comparison With Previous Studiesmentioning

confidence: 99%

“…We can further compare with the Zou et al (2023) study of dwarf galaxies in the XMM-SERVS field. Their sample shows a relatively small distribution of X-ray luminosities (L X ≈ 10 40-42 erg s −1 ) for their lowest-mass targets (M * ≈ 10 7 M e ), with much greater variation (L X ≈ 10 40-44 erg s −1 ) in higher masses (M * ≈ 10 9 M e ; see Figure 6 in Zou et al 2023). A similar analysis of our sample shows inconsistent results, with luminosities ranging from L X ≈ 10 38-44 regardless of galaxy mass for both the low-metallicity and control samples.…”

Section: Comparison With Previous Studiesmentioning

confidence: 99%

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Exploring X-Ray Properties of Low-metallicity Dwarf Galaxies

Cann,

Weaver,

Pfeifle

et al. 2024

ApJ

0

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One of the primary outstanding questions in extragalactic astronomy is the formation and early evolution of the supermassive black holes that are seen in nearly every massive galaxy. Low-metallicity dwarf galaxies may offer the most representative local analogs to pristine early galaxies, making them a vital tool in probing black hole seed models through the study of the intermediate-mass black holes (IMBHs) possibly hosted therein; though these dwarf galaxies, and the IMBHs they may host, are typically not as well-studied in this context as their higher-metallicity and higher-mass counterparts. In this paper, we explore the X-ray properties of a sample of 37 low-metallicity dwarf galaxies using archival XMM observations, and we compare the properties of this population against a representative sample of higher-metallicity counterparts. We report the detection of 10 sources with 0.3–10 keV luminosity in excess of 1040 erg s−1 within the low-metallicity sample, which we highlight for followup as potential IMBH candidates. Finally, we discuss the differing multiwavelength scaling relations (e.g., L X–L W2, L X–star formation rate) between the two galaxy populations, as well as the sample’s L X as a function of metallicity.

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“…The uniformity of the K s -band data across XMM-SERVS allows the mass-completeness curve for all three XMM-SERVS fields to be virtually identical (e.g., Figure 11 in Zou et al 2023). Therefore, we simply combine all galaxies residing in XMM-SERVS to estimate our mass-completeness curve without fear that it will change from field to field.…”

Section: Data and Samplementioning

confidence: 99%

Investigating the Star Formation Rates of Active Galactic Nucleus Hosts Relative to the Star-forming Main Sequence

Cristello,

Zou,

Brandt

et al. 2024

ApJ

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A fundamental question in galaxy and black hole evolution remains how galaxies and their supermassive black holes have evolved together over cosmic time. Specifically, it is still unclear how the position of X-ray active galactic nucleus (AGN) host galaxies with respect to the star-forming main sequence (MS) may change with the X-ray luminosity (L X) of the AGN or the stellar mass (M ⋆) of the host galaxy. We use data from the XMM-Spitzer Extragalactic Representative Volume Survey (XMM-SERVS) to probe this issue. XMM-SERVS is covered by the largest medium-depth X-ray survey (with superb supporting multiwavelength data) and thus contains the largest sample to date for study. To ensure consistency, we locally derive the MS from a large reference galaxy sample. In our analysis, we demonstrate that the turnover of the galaxy MS does not allow reliable conclusions to be drawn for high-mass AGNs, and we establish a robust safe regime where the results do not depend upon the choice of MS definition. Under this framework, our results indicate that less massive AGN host galaxies ( log M ⋆ ∼ 9.5 – 10.5 M ⊙ ) generally possess enhanced star formation rates compared to their normal-galaxy counterparts while the more massive AGN host galaxies ( log M ⋆ ∼ 10.5 – 11.5 M ⊙ ) lie on or below the star-forming MS. Further, we propose an empirical model for how the placement of an AGN with respect to the MS (SFRnorm) evolves as a function of both M ⋆ and L X.

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“…We apply a lower cut for z because photo-zs are less reliable when too small (e.g., see Appendix C of Zou et al 2021), and the peculiar motions become nonnegligible as well. We limit >  M log 9.5 because dwarf AGNs usually have much less reliable measurements and require special treatment (e.g., Zou et al 2023). We apply the same upper cuts as in Yang et al (2018) for both M å and z because very few sources can exceed these thresholds.…”

Section: Sample Constructionmentioning

confidence: 99%

Mapping the Growth of Supermassive Black Holes as a Function of Galaxy Stellar Mass and Redshift

Zou,

Yu,

Brandt

et al. 2024

ApJ

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The growth of supermassive black holes is strongly linked to their galaxies. It has been shown that the population mean black hole accretion rate ( BHAR ¯ ) primarily correlates with the galaxy stellar mass (M ⋆) and redshift for the general galaxy population. This work aims to provide the best measurements of BHAR ¯ as a function of M ⋆ and redshift over ranges of 109.5 < M ⋆ < 1012 M ⊙ and z < 4. We compile an unprecedentedly large sample with 8000 active galactic nuclei (AGNs) and 1.3 million normal galaxies from nine high-quality survey fields following a wedding cake design. We further develop a semiparametric Bayesian method that can reasonably estimate BHAR ¯ and the corresponding uncertainties, even for sparsely populated regions in the parameter space. BHAR ¯ is constrained by X-ray surveys sampling the AGN accretion power and UV-to-infrared multiwavelength surveys sampling the galaxy population. Our results can independently predict the X-ray luminosity function (XLF) from the galaxy stellar mass function (SMF), and the prediction is consistent with the observed XLF. We also try adding external constraints from the observed SMF and XLF. We further measure BHAR ¯ for star-forming and quiescent galaxies and show that star-forming BHAR ¯ is generally larger than or at least comparable to the quiescent BHAR ¯ .

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Identification and Characterization of a Large Sample of Distant Active Dwarf Galaxies in XMM-SERVS

Cited by 7 publications

References 126 publications

Exploring X-Ray Properties of Low-metallicity Dwarf Galaxies

Exploring X-Ray Properties of Low-metallicity Dwarf Galaxies

Investigating the Star Formation Rates of Active Galactic Nucleus Hosts Relative to the Star-forming Main Sequence

Mapping the Growth of Supermassive Black Holes as a Function of Galaxy Stellar Mass and Redshift

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