Past, Present, and Future of the Scaling Relations of Galaxies and Active Galactic Nuclei

D’Onofrio, M.; Marziani, Paola; Chiosi, C.

doi:10.3389/fspas.2021.694554

Cited by 20 publications

(6 citation statements)

References 874 publications

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“…In addition, the derived relation with dynamical mass measurements of MBHs may suffer significant selection bias (Shankar et al 2016). The MBH-host galaxy scaling relation may evolve with redshift as suggested by many authors (e.g., McLure et al 2006;Salviander et al 2007;Merloni et al 2010;Zhang et al 2012;Schulze & Wisotzki 2014;Decarli et al 2018;D'Onofrio et al 2021), which may contain critical information about the coevolution of MBHs with their host galaxies. In this work, we also demonstrate the potential of using GWB "observations" to set strong constraints on the redshift evolution of the MBHhost galaxy relationship.…”

Section: Constraining the Mbh-host Galaxy Relationship From The Gwbmentioning

confidence: 89%

Pulsar Timing Array Detections of Supermassive Binary Black Holes: Implications from the Detected Common Process Signal and Beyond

Chen,

Yu,

2023

ApJ

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Pulsar timing arrays (PTAs) are anticipated to detect the stochastic gravitational-wave background (GWB) from supermassive binary black holes (BBHs) as well as the gravitational waves from individual BBHs. Recently, a common process signal was reported by several PTAs. In this paper, we investigate the constraints on the BBH population model(s) by current PTA observations and further study the detections of both the GWB and individual BBHs by current and future PTAs. We find that the massive black hole–host galaxy scaling relation, an important ingredient of the BBH population model, is required to either evolve significantly with redshift or have a normalization ∼0.86–1.1 dex higher than the empirical ones if the GWB is the same as the common process signal. For both cases, the estimated detection probability for individual BBHs is too small for a positive detection by current PTAs. By involving either the constrained scaling relations or those empirical ones into the BBH population models, we estimate that the GWB may be detected with a signal-to-noise ratio ≳3 by the China Five-hundred-meter Aperture Spherical radio Telescope PTA (CPTA) and the Square Kilometre Array PTA (SKAPTA) after ∼2–3 (or ∼6–11) yr observation if it is the same as (or 1 order of magnitude lower than) the common process signal. The detection time of individual BBHs by CPTA and SKAPTA is close to that of the GWB detection. We show that the BBH population model can be strongly constrained by the number and property distributions of BBHs to be detected by future PTAs.

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Section: Constraining the Mbh-host Galaxy Relationship From The Gwbmentioning

confidence: 89%

Pulsar Timing Array Detections of Supermassive Binary Black Holes: Implications from the Detected Common Process Signal and Beyond

Chen,

Yu,

2023

ApJ

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“…1 To date, only about 150 such supermassive black holes (SMBHs) with M •  10 6 M e have been directly measured in just the nearest and most massive galaxies. 2 With SMBHs expected to reside in the hearts of almost every massive galaxy (Rees 1984), one can take their pick of scaling relations (see Graham 2016;D'Onofrio et al 2021 for informative reviews) to perform black hole mass estimates for large numbers of galaxies in surveys to construct black hole mass functions (e.g., Graham et al 2007;Mutlu-Pakdil et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Discovery of a Planar Black Hole Mass Scaling Relation for Spiral Galaxies

Davis,

Jin 金

2023

ApJL

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Supermassive black holes (SMBHs) are tiny in comparison to the galaxies they inhabit, yet they manage to influence and coevolve along with their hosts. Evidence of this mutual development is observed in the structure and dynamics of galaxies and their correlations with black hole mass (M •). For our study, we focus on relative parameters that are unique to only disk galaxies. As such, we quantify the structure of spiral galaxies via their logarithmic spiral-arm pitch angles (ϕ) and their dynamics through the maximum rotational velocities of their galactic disks (v max). In the past, we have studied black hole mass scaling relations between M • and ϕ or v max, separately. Now, we combine the three parameters into a trivariate M •–ϕ–v max relationship that yields best-in-class accuracy in prediction of black hole masses in spiral galaxies. Because most black hole mass scaling relations have been created from samples of the largest SMBHs within the most massive galaxies, they lack certainty when extrapolated to low-mass spiral galaxies. Thus, it is difficult to confidently use existing scaling relations when trying to identify galaxies that might harbor the elusive class of intermediate-mass black holes (IMBHs). Therefore, we offer our novel relationship as an ideal predictor to search for IMBHs and probe the low-mass end of the black hole mass function by utilizing spiral galaxies. Already with rotational velocities widely available for a large population of galaxies and pitch angles readily measurable from uncalibrated images, we expect that the M •–ϕ–v max fundamental plane will be a useful tool for estimating black hole masses, even at high redshifts.

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“…Even though galaxy formation and evolution is thought to depend on a number of different factors and processes, galaxies show remarkably tight correlations between some of their basic stellar and dynamical properties (e.g., Binggeli & Jerjen 1997;Tassis et al 2008). These scaling relations have been extensively studied for different galaxy types, in a range of environments, and in particular in light of a possible evolution with time (see, e.g., D'Onofrio et al 2021, for a recent review). A few examples of well-established galaxy scaling relations are the velocity-luminosity or Tully-Fisher relation (Tully & Fisher 1977;Courteau et al 2007), the Faber-Jackson relation (Faber & Jackson 1976), the Kormendy relation (Kormendy 1977), the fundamental plane of galaxies (e.g., Djorgovski & Davis 1987;Dressler et al 1987;Cappellari et al 2006;La Barbera et al 2008), the bulge-to-black hole mass relation (Magorrian et al 1998) and the mass-radius relation (Chiosi et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Radial velocities and stellar population properties of 56 MATLAS dwarf galaxies observed with MUSE

Heesters

Müller

Marleau

et al. 2023

A&A

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Dwarf galaxies have been extensively studied in the Local Group, in nearby groups, and selected clusters, giving us a robust picture of their global stellar and dynamical properties, such as their circular velocity, stellar mass, surface brightness, age, and metallicity in particular locations in the Universe. Intense study of these properties has revealed correlations between them, called the scaling relations, including the well-known universal stellar mass-metallicity relation. However, since dwarfs play a role in a vast range of different environments, much can be learned about galaxy formation and evolution through extending the study of these objects to various locations. We present MUSE spectroscopy of a sample of 56 dwarf galaxies as a follow-up to the MATLAS survey in low- to moderate-density environments beyond the Local Volume. The dwarfs have stellar masses in the range of M*/M⊙ = 106.1–109.4 and show a distance range of D = 14–148 Mpc, the majority of which (75%) are located in the range targeted by the MATLAS survey (10–45 Mpc). We thus report a 75% success rate for the semi-automatic identification of dwarf galaxies (79% for dwarf ellipticals) in the MATLAS survey on the subsample presented here. Using pPXF full spectrum fitting, we determine their line-of-sight velocity and can match the majority of them with their massive host galaxy. Due to the observational setup of the MATLAS survey, the dwarfs are located in the vicinity of massive galaxies. Therefore, we are able to confirm their association through recessional velocity measurements. Close inspection of their spectra reveals that ∼30% show clear emission lines, and thus star formation activity. We estimate their stellar population properties (age and metallicity) and compare our results with other works investigating Local Volume and cluster dwarf galaxies. We find that the dwarf galaxies presented in this work show a systematic offset from the universal stellar mass-metallicity relation toward lower metallicities at the same stellar mass. A similar deviation is present in other works in the stellar mass range probed in this work and might be attributed to the use of different methodologies for deriving the metallicity.

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Past, Present, and Future of the Scaling Relations of Galaxies and Active Galactic Nuclei

Cited by 20 publications

References 874 publications

Pulsar Timing Array Detections of Supermassive Binary Black Holes: Implications from the Detected Common Process Signal and Beyond

Pulsar Timing Array Detections of Supermassive Binary Black Holes: Implications from the Detected Common Process Signal and Beyond

Discovery of a Planar Black Hole Mass Scaling Relation for Spiral Galaxies

Radial velocities and stellar population properties of 56 MATLAS dwarf galaxies observed with MUSE

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