Abstract:Studies indicate strong evidence of a scaling relation in the local Universe between the supermassive black hole mass (MBH) and the stellar mass of their host galaxies (M⋆). They even show similar histories across cosmic times of their differential terms: the star formation rate (SFR) and black hole accretion rate (BHAR). However, a clear picture of this coevolution is far from being understood. We selected an X-ray sample of active galactic nuclei (AGN) up to z = 2.5 in the miniJPAS footprint. Their X-ray to … Show more
“…Although, λ sBHAR is often used as a proxy of the Eddington ratio, it is important to acknowledge that the calculation of AGN bolometric luminosity and the inherent scatter in the relation between black hole mass, M BH , and M * , may introduce variations in λ sBHAR compared to the Eddington ratio, as indicated by previous studies (Lopez et al 2023;Mountrichas & Buat 2023). Nevertheless, our primary objective is to explore potential disparities in the distributions of λ sBHAR between type 1 and type 2 AGN.…”
Section: Specific Black Hole Accretion Rate Of Type 1 and 2 Agnmentioning
It is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, M BH , and the galaxy bulge or stellar mass, M * . The cosmic evolution of this relation, though, is still a matter of debate. In this work, we examine the M BH −M * relation, using 687 X-ray luminous (median log [L X,2−10keV (ergs −1 )] = 44.3), broad-line active galactic nuclei (AGN), at 0.2 < z < 4.0 (median z ≈ 1.4) that lie in the XMM-XXL field. Their M BH and M * range from 7.5 < log [M BH (M )] < 9.5 and 10 < log [M * (M )] < 12, respectively. Most of the AGN live in star-forming galaxies and their Eddington ratios range from 0.01 to 1, with a median value of 0.06. Our results show that M BH and M * are correlated (r = 0.47 ± 0.21, averaged over different redshift intervals). Our analysis also shows that the mean ratio of the M BH and M * does not evolve with redshift, at least up to z = 2 and has a value of log(M BH /M * ) = −2.44. The majority of the AGN (75%) are in a SMBH mass growth-dominant phase. In these systems, the M BH −M * correlation is weaker and their M * tends to be lower (for the same M BH ) compared to systems that are in a galaxy mass growth phase. Our findings suggest that the growth of black hole mass occurs first, while the early stellar mass assembly may not be so efficient.
“…Although, λ sBHAR is often used as a proxy of the Eddington ratio, it is important to acknowledge that the calculation of AGN bolometric luminosity and the inherent scatter in the relation between black hole mass, M BH , and M * , may introduce variations in λ sBHAR compared to the Eddington ratio, as indicated by previous studies (Lopez et al 2023;Mountrichas & Buat 2023). Nevertheless, our primary objective is to explore potential disparities in the distributions of λ sBHAR between type 1 and type 2 AGN.…”
Section: Specific Black Hole Accretion Rate Of Type 1 and 2 Agnmentioning
It is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, M BH , and the galaxy bulge or stellar mass, M * . The cosmic evolution of this relation, though, is still a matter of debate. In this work, we examine the M BH −M * relation, using 687 X-ray luminous (median log [L X,2−10keV (ergs −1 )] = 44.3), broad-line active galactic nuclei (AGN), at 0.2 < z < 4.0 (median z ≈ 1.4) that lie in the XMM-XXL field. Their M BH and M * range from 7.5 < log [M BH (M )] < 9.5 and 10 < log [M * (M )] < 12, respectively. Most of the AGN live in star-forming galaxies and their Eddington ratios range from 0.01 to 1, with a median value of 0.06. Our results show that M BH and M * are correlated (r = 0.47 ± 0.21, averaged over different redshift intervals). Our analysis also shows that the mean ratio of the M BH and M * does not evolve with redshift, at least up to z = 2 and has a value of log(M BH /M * ) = −2.44. The majority of the AGN (75%) are in a SMBH mass growth-dominant phase. In these systems, the M BH −M * correlation is weaker and their M * tends to be lower (for the same M BH ) compared to systems that are in a galaxy mass growth phase. Our findings suggest that the growth of black hole mass occurs first, while the early stellar mass assembly may not be so efficient.
“…At high redshift, it is hard to resolve the central AGN emission from the host galaxy. SED observations, modeling, and fitting are indispensable to investigate the physical properties of these high-redshift AGNs and their host galaxies (e.g., Merloni et al 2010;Bongiorno et al 2014;Suh et al 2019;López et al 2023).…”
We present a UV to millimeter spectral energy distribution (SED) analysis of 16 hyperluminous, dust-obscured quasars at z ∼ 3, selected by the Wide-field Infrared Survey Explorer. We aim to investigate the physical properties of these quasars, with a focus on their molecular gas content. We decompose the SEDs into three components: stellar, cold dust, and active galactic nucleus (AGN). By doing so, we are able to derive and analyze the relevant properties of each component. We determine the molecular gas mass from CO line emission based on Atacama Large Millimeter/submillimeter Array (ALMA) observations. By including ALMA observations in the multiwavelength SED analysis, we derive the molecular gas fractions, gas depletion timescales, and star formation efficiencies (SFEs). Their sample median and 16th–84th quartile ranges are
f
gas
∼
0.33
−
0.17
+
0.33
, t
depl ∼
39
−
28
+
85
Myr, and SFE ∼
297
−
195
+
659
K km s−1 pc−2, respectively. Compared to main-sequence galaxies, they have lower molecular gas content and higher SFEs, similar to quasars in the literature. This suggests that the gas in these quasars is rapidly depleted, likely as the result of intense starburst activity and AGN feedback. The observed correlations between these properties and the AGN luminosities further support this scenario. Additionally, we infer the black hole to stellar mass ratio and black hole mass growth rate, which indicate significant central black hole mass assembly over short timescales. Our results are consistent with the scenario that our sample represents a short transition phase toward unobscured quasars.
It is well known that supermassive black holes (SMBHs) and their host galaxies undergo a process of co-evolution. Feedback from active galactic nuclei (AGNs) plays an important role in this symbiosis. To study the effect of AGN feedback on the host galaxy, one popular method is to study the star formation rate (SFR) as a function of the X-ray luminosity (LX). However, hydrodynamical simulations suggest that the cumulative impact of AGN feedback on a galaxy is encapsulated in the mass of the SMBH, MBH, rather than the LX. In this study, we compare the SFRs of AGN and non-AGN galaxies as a function of LX, MBH, the Eddington ratio (nEdd), and the specific black hole accretion rate (λsBHAR). For that purpose, we used 122 X-ray AGN in the XMM-XXL field and 3371 galaxies from the VIPERS survey to calculate the SFRnorm parameter, defined as the ratio of the SFR of AGN to the SFR of non-AGN galaxies with similar stellar mass, M*, and redshift. Our datasets span a redshift range of 0.5 ≤ z ≤ 1.2. The results show that the correlation between SFRnorm and MBH is stronger compared to that between SFRnorm and LX. A weaker correlation is found between SFRnorm and λsBHAR. No correlation is detected between SFRnorm and nEdd. These results corroborate the notion that the MBH is a more robust tracer of the cumulative impact of the AGN feedback, compared to the instantaneous accretion rate (LX). Thus, it may serve as a better predictive parameter of changes in the SFR of the host galaxy.
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