Low-luminosity AGN and X-Ray Binary Populations in COSMOS Star-forming Galaxies

Fornasini, Francesca M.; Civano, F.; Fabbiano, G.; Elvis, M.; Marchesi, S.; Miyaji, Takeshi; Zezas, A.

doi:10.3847/1538-4357/aada4e

Cited by 43 publications

(47 citation statements)

References 103 publications

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“…The measured evolution of L X (HMXB)/SFR ∝ (1+z) and L X (LMXB)/M ⋆ ∝ (1 + z) 2−3 out to z ≈ 2-4 Aird et al 2017) is only loosely constrained, but consistent with the population synthesis predictions from Fragos et al (2013a); however, see Fornasini et al (2018) for caveats. Extrapolation of the theoretical predictions into the very early Universe at z > ∼ 10, when the Universe was of very low metallicity ( < ∼ 1/10 Z ⊙ ; e.g., based on the Millenium II simulations; Guo et al 2011), indicate that XRBs were likely the most luminous X-ray emitting population in the Universe (e.g., Fragos et al 2013b;Lehmer et al 2016;Madau & Fragos 2017).…”

Section: Introductionsupporting

confidence: 73%

X-Ray Binary Luminosity Function Scaling Relations for Local Galaxies Based on Subgalactic Modeling

Lehmer

Eufrasio

Tzanavaris

et al. 2019

ApJS

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129

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We present new Chandra constraints on the X-ray luminosity functions (XLFs) of X-ray binary (XRB) populations, and their scaling relations, for a sample of 38 nearby galaxies (D = 3.4-29 Mpc). Our galaxy sample is drawn primarily from the Spitzer infrared nearby galaxy survey (SINGS), and contains a wealth of Chandra (5.8 Ms total) and multiwavelength data, allowing for star-formation rates (SFRs) and stellar masses (M ⋆ ) to be measured on subgalactic scales. We divided the 2478 X-ray detected sources into 21 subsamples in bins of specific-SFR (sSFR ≡ SFR/M ⋆ ) and constructed XLFs. To model the XLF dependence on sSFR, we fit a global XLF model, containing contributions from high-mass XRBs (HMXBs), low-mass XRBs (LMXBs), and background sources from the cosmic X-ray background (CXB) that respectively scale with SFR, M ⋆ , and sky area. We find an HMXB XLF that is more complex in shape than previously reported and an LMXB XLF that likely varies with sSFR, potentially due to an age dependence. When applying our global model to XLF data for each individual galaxy, we discover a few galaxy XLFs that significantly deviate from our model beyond statistical scatter. Most notably, relatively low-metallicity galaxies have an excess of HMXBs above ≈10 38 erg s −1 and elliptical galaxies that have relatively rich populations of globular clusters (GCs) show excesses of LMXBs compared to the global model. Additional modeling of how the XRB XLF depends on stellar age, metallicity, and GC specific frequency is required to sufficiently characterize the XLFs of galaxies.

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Section: Introductionsupporting

confidence: 73%

X-Ray Binary Luminosity Function Scaling Relations for Local Galaxies Based on Subgalactic Modeling

Lehmer

Eufrasio

Tzanavaris

et al. 2019

ApJS

Self Cite

129

179

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“…The L X /SFR of the z ∼ 2.3 stacks are higher than, but statistically consistent with, the z ∼ 1.5 stacks. The L X /SFR of the z ∼ 2.3 full sample stack is 2.3σ higher than the M12 value of 3.7 × 10 39 erg s −1 M ⊙ yr and 3.1σ higher than the L10 value of 1.6 × 10 39 erg s −1 M ⊙ yr. Fornasini et al (2018) find that for X-ray stacks with 50 galaxies such as these, L X may be biased to higher values than the true mean by 0.15 dex; 4 however, even accounting for this possible systematic effect, the z ∼ 2.3 stacks have enhanced L X /SFR compared to the L10 and M12 relations. Both the z ∼ 1.5 and z ∼ 2.3 full sample stacks are in good agreement with the L X /SFR values expected from the redshift evolution of the total X-ray binary (XRB) emission measured by Lehmer et al (2016) (shown by the dark gray long-dashed line in Figure 4; hereafter L16) and Aird et al (2017) (shown by the dark gray shortdashed line; hereafter A17).…”

Section: The Redshift Evolution Of Xrbsmentioning

confidence: 84%

The MOSDEF Survey: The Metallicity Dependence of X-Ray Binary Populations at z ∼ 2

Fornasini

Kriek

Shivaei³

et al. 2019

ApJ

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Population synthesis models predict that high-mass X-ray binary (HMXB) populations produced in low metallicity environments should be more X-ray luminous, a trend supported by studies of nearby galaxies. This trend may be responsible for the observed increase of the X-ray luminosity (L X ) per star formation rate (SFR) with redshift due to the decrease of metallicity (Z) at fixed stellar mass as a function of redshift. To test this hypothesis, we use a sample of 79 z ∼ 2 star-forming galaxies with oxygen abundance measurements from the MOSDEF survey, which obtained rest-frame optical spectra for ∼ 1500 galaxies in the CANDELS fields at 1.37 < z < 3.80. Using Chandra data from the AEGIS-X Deep, Deep Field North, and Deep Field South surveys, we stack the X-ray data at the galaxy locations in bins of redshift and Z because the galaxies are too faint to be individually detected. In agreement with previous studies, the average L X /SFR of our z ∼ 2 galaxy sample is enhanced by ≈ 0.4 − 0.8 dex relative to local HMXB L X -SFR scaling relations. Splitting our sample by Z, we find that L X /SFR and Z are anti-correlated with 97% confidence. This observed Z dependence for HMXB-dominated galaxies is consistent both with the local L X -SFR-Z relation and a subset of population synthesis models. Although the statistical significance of the observed trends is weak due to the low X-ray statistics, these results constitute the first direct evidence connecting the redshift evolution of L X /SFR and the Z dependence of HMXBs.

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“…Chen et al 2013;Hickox et al 2014;Lanzuisi et al 2017;Yang et al 2017). However, Yang et al (2017) show, via partial correlation (PCOR) analyses , that BHAR is actually more strongly related to host-galaxy total stellar mass (M ) than SFR (also see Fornasini et al 2018 for a similar conclusion). Their results suggest that the apparent BHAR-SFR relation is only a secondary effect resulting from a primary BHAR-M relation and the star formation main sequence.…”

Section: Introductionmentioning

confidence: 88%

“…As explained in Section 1, the BHAR quantity is designed to approximate long-term average SMBH accretion rate, and has been widely adopted in the studies of AGN-galaxy relations (e.g. Chen et al 2013;Hickox et al 2014;Yang et al 2017Yang et al , 2018aFornasini et al 2018). Some works proposed to recover the full distribution of BHAR as a function of galaxy properties (e.g.…”

Section: Black Hole Accretion Ratementioning

confidence: 99%

Evident black hole-bulge coevolution in the distant universe

Yang

Brandt

Alexander

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACT Observations in the local universe show a tight correlation between the masses of supermassive black holes (SMBHs; M BH ) and host-galaxy bulges (M bulge ), suggesting a strong connection between SMBH and bulge growth.However, direct evidence for such a connection in the distant universe remains elusive. We have studied sample-averaged SMBH accretion rate (BHAR) for bulge-dominated galaxies at z = 0.5-3. While previous observations found BHAR is strongly related to host-galaxy stellar mass (M ) for the overall galaxy population, our analyses show that, for the bulge-dominated population, BHAR is mainly related to SFR rather than M . This BHAR-SFR relation is highly significant, e.g. 9.0σ (Pearson statistic) at z = 0.5-1.5. Such a BHAR-SFR connection does not exist among our comparison sample of galaxies that are not bulge dominated, for which M appears to be the main determinant of SMBH accretion. This difference between the bulge-dominated and comparison samples indicates that SMBHs only coevolve with bulges rather than the entire galaxies, explaining the tightness of the local M BH −M bulge correlation. Our best-fitting BHAR-SFR relation for the bulge-dominated sample is log BHAR = log SFR − (2.48 ± 0.05) (solar units). The best-fitting BHAR/SFR ratio (10 −2.48 ) for bulge-dominated galaxies is similar to the observed M BH /M bulge values in the local universe. Our results reveal that SMBH and bulge growth are in lockstep, and thus non-causal scenarios of merger averaging are unlikely the origin of the M BH −M bulge correlation. This lockstep growth also predicts that the M BH −M bulge relation should not have strong redshift dependence.

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Low-luminosity AGN and X-Ray Binary Populations in COSMOS Star-forming Galaxies

Cited by 43 publications

References 103 publications

X-Ray Binary Luminosity Function Scaling Relations for Local Galaxies Based on Subgalactic Modeling

X-Ray Binary Luminosity Function Scaling Relations for Local Galaxies Based on Subgalactic Modeling

The MOSDEF Survey: The Metallicity Dependence of X-Ray Binary Populations at z ∼ 2

Evident black hole-bulge coevolution in the distant universe

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