scholarly journals Hunting for the host galaxy groups of binary black holes and the application in constraining Hubble constant

2020 ◽  
Vol 498 (2) ◽  
pp. 1786-1800
Author(s):  
Jiming Yu ◽  
Yu Wang ◽  
Wen Zhao ◽  
Youjun Lu
Keyword(s):  
Black Holes ◽  
Cosmological Parameters ◽  
Hubble Constant ◽  
Host Galaxy ◽  
Full Time ◽  
Host Galaxies ◽  
Binary Black Holes ◽  
Compact Binaries ◽  
Galaxy Groups ◽  
Host Identification

ABSTRACT The discovery of gravitational-wave (GW) signals, produced by the coalescence of stellar-mass binary black holes (SBBHs), opens a new window to study the astrophysical origins and dynamical evolutions of compact binaries. In addition, these GW events can be treated as the standard sirens to constrain various cosmological parameters. Both issues require the host identification for these GW events, with help of the spatial resolution of GW detector networks. In this paper, we investigate the capabilities of various detector networks for identifying the SBBHs’ host galaxy groups, rather than their host galaxies, which can overcome the influence of galaxies’ proper motions in dark matter haloes for measuring the cosmological parameters. In our analysis, the group catalogue of SDSS DR7 with redshift z ∈ (0.01, 0.1) is considered as an example of the application. We find that for the second-generation (2G) detector network, the host galaxy groups of around (0.7–6.9) SBBHs can be identified per year assuming all sources are $30\!-\!30\, \mathrm{M}_{\odot }$ binaries, and that all five detectors in the network are in lock 100 per cent of the time. For the 3G detector network, this number becomes (3.9–40.0) yr−1. We also investigate the potential constraint on the Hubble constant H0 by these GW events, if their redshift information is extracted from the candidates of host galaxy groups. We find that, by 5-yr full time observations, 2G detector network is expected to give a constraint of $\Delta H_0/H_0\sim (1{{\ \rm per\ cent}},\ 4{{\ \rm per\ cent}})$, which can be more than two order smaller if considering the 3G detector network.

scholarly journals On Dark Gravitational Wave Standard Sirens as Cosmological Inference and Forecasting the Constraint on Hubble Constant using Binary Black Holes Detected by Deci-Hertz Observator

2021 ◽  
Author(s):  
Ju Chen ◽  
Changshuo Yan ◽  
Youjun Lu ◽  
Yuetong Zhao ◽  
Junqiang Ge
Keyword(s):  
Black Holes ◽  
Gravitational Wave ◽  
Signal To Noise Ratio ◽  
Cosmological Parameters ◽  
Hubble Constant ◽  
Luminosity Distance ◽  
Host Galaxies ◽  
Binary Black Holes ◽  
Merger Rate ◽  
Electromagnetic Signals

Abstract Gravitational wave (GW) signals from compact binary coalescences can be used as standard sirens to constrain cosmological parameters if its redshift can be measured independently by electromagnetic signals. However, mergers of stellar binary black holes (BBHs) may not have electromagnetic counterparts and thus have no direct redshift measurements. These dark sirens may be still used to statistically constrain cosmological parameters by combining their GW measured luminosity distances and localization with deep redshift surveys of galaxies around it. We investigate this dark siren method to constrain cosmological parameters in details by using mock BBH and galaxy samples. We find that the Hubble constant can be well constrained with an accuracy $\lesssim 1\%$ with a few tens or more BBH mergers at redshift up to $1$ if GW observations can provide accurate estimates of its luminosity distance (with relative error of $\lesssim 0.01$) and localization ($\lesssim 0.1\mathrm{deg}^2$), though the constraint may be significantly biased if the luminosity distance and localization errors are larger. We further generate mock BBH samples, according to current constraints on BBH merger rate and the distributions of BBH properties, and find that Deci-Hertz Observatory (DO) in a half year observation period may detect about one hundred BBHs with signal-to-noise ratio $\varrho \gtrsim 30$, relative luminosity distance error $\lesssim 0.02$, and localization error $\lesssim 0.01\mathrm{deg}^2$. By applying the dark standard siren method, we find that the Hubble constant can be constrained to $\sim 0.1-1\%$ level using these DO BBHs, an accuracy comparable to the constraints obtained by using electromagnetic observations in the near future, thus it may provide insight into the Hubble tension. We also demonstrate that the constraint on the Hubble constant using this dark siren method are robust and do not depend on the choice of the prior for the properties of BBH host galaxies.

scholarly journals Testing the evolution of correlations between supermassive black holes and their host galaxies using eight strongly lensed quasars

2020 ◽  
Vol 501 (1) ◽  
pp. 269-280
Author(s):  
Xuheng Ding ◽  
Tommaso Treu ◽  
Simon Birrer ◽  
Adriano Agnello ◽  
Dominique Sluse ◽  
...  
Keyword(s):  
Black Holes ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Galactic Nuclei ◽  
Host Galaxy ◽  
Wide Field ◽  
Host Galaxies ◽  
Field Surveys ◽  
Instrumental Resolution ◽  
The Moment

ABSTRACT One of the main challenges in using high-redshift active galactic nuclei (AGNs) to study the correlations between the mass of a supermassive black hole ($\mathcal {M}_{\rm BH}$) and the properties of its active host galaxy is instrumental resolution. Strong lensing magnification effectively increases instrumental resolution and thus helps to address this challenge. In this work, we study eight strongly lensed AGNs with deep Hubble Space Telescope imaging, using the lens modelling code lenstronomy to reconstruct the image of the source. Using the reconstructed brightness of the host galaxy, we infer the host galaxy stellar mass based on stellar population models. $\mathcal {M}_{\rm BH}$ are estimated from broad emission lines using standard methods. Our results are in good agreement with recent work based on non-lensed AGNs, demonstrating the potential of using strongly lensed AGNs to extend the study of the correlations to higher redshifts. At the moment, the sample size of lensed AGNs is small and thus they provide mostly a consistency check on systematic errors related to resolution for non-lensed AGNs. However, the number of known lensed AGNs is expected to increase dramatically in the next few years, through dedicated searches in ground- and space-based wide-field surveys, and they may become a key diagnostic of black holes and galaxy co-evolution.

An accreting < 105M⊙ black hole at the center of dwarf galaxy IC750

2019 ◽  
Vol 15 (S356) ◽  
pp. 376-376
Author(s):  
Ingyin Zaw
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dwarf Galaxies ◽  
Dwarf Galaxy ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Host Galaxies ◽  
Seed Formation ◽  
Maser Emission ◽  
Water Masers

AbstractNuclear black holes in dwarf galaxies are important for understanding the low end of the supermassive black hole mass distribution and the black hole-host galaxy scaling relations. IC 750 is a rare system which hosts an AGN, found in ˜0.5% of dwarf galaxies, with circumnuclear 22 GHz water maser emission, found in ˜3–5% of Type 2 AGNs. Water masers, the only known tracer of warm, dense gas in the center parsec of AGNs resolvable in position and velocity, provide the most precise and accurate mass measurements of SMBHs outside the local group. We have mapped the maser emission in IC 750 and find that it traces a nearly edge-on warped disk, 0.2 pc in diameter. The central black hole has an upper limit mass of ˜1 × 105 M⊙ and a best fit mass of ˜8 × 104 M⊙, one to two orders of magnitude below what is expected from black hole-galaxy scaling relations. This has implications for models of black hole seed formation in the early universe, the growth of black holes, and their co-evolution with their host galaxies.

scholarly journals Supermassive black holes: Coevolution (or not) of black holes and host galaxies

2012 ◽  
Vol 8 (S295) ◽  
pp. 241-256
Author(s):  
John Kormendy
Keyword(s):  
Black Holes ◽  
Galaxy Formation ◽  
Globular Clusters ◽  
Hubble Space Telescope ◽  
Supermassive Black Holes ◽  
Host Galaxy ◽  
Late Time ◽  
Host Galaxies ◽  
Energy Feedback ◽  
Negative Effect

AbstractSupermassive black holes (BHs) have been found in 75 galaxies by observing spatially resolved dynamics. The Hubble Space Telescope (HST) revolutionized BH work by advancing the subject from its ‘proof of concept’ phase into quantitative studies of BH demographics. Most influential was the discovery of a tight correlation between BH masses M• and the velocity dispersions σ of stars in the host galaxy bulge components at radii where the stars mostly feel each other and not the BH. Together with correlations between M• and bulge luminosity, with the ‘missing light’ that defines galaxy cores, and with numbers of globular clusters, this has led to the conclusion that BHs and bulges coevolve by regulating each other's growth. This simple picture with one set of correlations for all galaxies dominated BH work in the past decade.New results are now replacing the above, simple story with a richer and more plausible picture in which BHs correlate differently with different kinds of galaxy components. BHs with masses of 105—106M⊙ live in some bulgeless galaxies. So classical (merger-built) bulges are not necessary equipment for BH formation. On the other hand, while they live in galaxy disks, BHs do not correlate with galaxy disks or with disk-grown pseudobulges. They also have no special correlation with dark matter halos beyond the fact that halo gravity controls galaxy formation. This leads to the suggestion that there are two modes of BH feeding, (1) local, secular and episodic feeding of small BHs in largely bulgeless galaxies that involves too little energy feedback to drive BH–host-galaxy coevolution and (2) global feeding in major galaxy mergers that rapidly grows giant BHs in short-duration events whose energy feedback does affect galaxy formation. After these quasar-like phases, maintenance-mode BH feedback into hot, X-ray-emitting gas continues to have a primarily negative effect in preventing late-time star formation when cold gas or gas-rich galaxies get accreted. Finally, the highest-mass galaxies inherit coevolution effects from smaller galaxies; the tightness of their BH correlations is caused mainly by averaging during dissipationless major mergers.

scholarly journals Inferring the population properties of binary black holes from unresolved gravitational waves

2020 ◽  
Vol 496 (3) ◽  
pp. 3281-3290 ◽  
Author(s):  
Rory J E Smith ◽  
Colm Talbot ◽  
Francisco Hernandez Vivanco ◽  
Eric Thrane
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Monte Carlo Study ◽  
Design Sensitivity ◽  
Spin Distribution ◽  
Binary Black Holes ◽  
Compact Binaries ◽  
Compact Binary ◽  
Binary Mergers ◽  
The Universe

ABSTRACT The vast majority of compact binary mergers in the Universe produce gravitational waves that are too weak to yield unambiguous detections; they are unresolved. We present a method to infer the population properties of compact binaries – such as their merger rates, mass spectrum, and spin distribution – using both resolved and unresolved gravitational waves. By eliminating entirely the distinction between resolved and unresolved signals, we eliminate bias from selection effects. To demonstrate this method, we carry out a Monte Carlo study using an astrophysically motivated population of binary black holes. We show that some population properties of compact binaries are well constrained by unresolved signals after about one week of observation with Advanced LIGO at design sensitivity.

scholarly journals Imaging compact supermassive binary black holes with Very Long Baseline Interferometry

2006 ◽  
Vol 2 (S238) ◽  
pp. 269-272 ◽  
Author(s):  
G. B. Taylor ◽  
C. Rodriguez ◽  
R. T. Zavala ◽  
A. B. Peck ◽  
L. K. Pollack ◽  
...  
Keyword(s):  
Black Holes ◽  
Hot Spots ◽  
Very Long Baseline Interferometry ◽  
Radio Galaxy ◽  
Host Galaxy ◽  
Binary Black Holes ◽  
Long Baseline ◽  
Compact Binary ◽  
Binary Black Hole ◽  
Very Long Baseline Array

AbstractWe report on the discovery of a supermassive binary black-hole (SBBH) system in the radio galaxy 0402+379, with a projected separation between the two black holes of just 7.3 pc. This is the most compact SBBH pair yet imaged by more than two orders of magnitude. These results are based upon multi-frequency imaging using the Very Long Baseline Array (VLBA) which reveal two compact, variable, flat-spectrum, active nuclei within the elliptical host galaxy of 0402+379. Multi-epoch observations from the VLBA also provide constraints on the total mass and dynamics of the system. The two nuclei appear stationary while the jets emanating from the weaker of the two nuclei appear to move out and terminate in bright hot spots. The discovery of this system has implications for the number of compact binary black holes that might be sources of gravitational radiation. The VLBI Imaging and Polarimetry Survey (VIPS) currently underway should discover several more SBBHs.

ARE SOME HOST GALAXIES OFSNe IaACTUALLY BLUESHIFTING?

2000 ◽  
Vol 15 (40) ◽  
pp. 2357-2362 ◽  
Author(s):  
D. BASU
Keyword(s):  
Cosmological Parameters ◽  
Spectral Lines ◽  
Host Galaxy ◽  
Correct Identification ◽  
Host Galaxies ◽  
Tentative Model ◽  
Modern Cosmology ◽  
Type Ia ◽  
Supernova Explosions ◽  
Alternative Identification

Supernova explosions of type Ia (SNe Ia) are now extensively used as "standard candles" in modern cosmology, viz. in constructing the Hubble's diagram and hence in determining various cosmological parameters. One of the most important quantities used in such analyses is the redshift of the host galaxy, which, in its turn, is determined by identifying the observed spectral lines with search lines known in the laboratory. The importance of the correct identification is therefore appreciated. The present work considers the possibility of misidentification of the observed lines. Alternative identification at higher wavelengths leads to blueshifts. Its implication in modern cosmology is discussed. A tentative model of the universe to interpret the results is proposed.

scholarly journals Do Nuclear Star Clusters and Supermassive Black Holes Follow the Same Host-Galaxy Correlations?

2012 ◽  
Vol 2012 ◽  
pp. 1-11 ◽  
Author(s):  
Peter Erwin ◽  
Dimitri Alexei Gadotti
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Careful Analysis ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
Host Galaxy ◽  
Mass Ratio ◽  
Host Galaxies ◽  
Order Of Magnitude ◽  
The Masses

Studies have suggested that there is a strong correlation between the masses of nuclear star clusters (NSCs) and their host galaxies, a correlation which is said to be an extension of the well-known correlations between supermassive black holes (SMBHs) and their host galaxies. But careful analysis of disk galaxies—including 2D bulge/disk/bar decompositions—shows that while SMBHs correlate with the stellar mass of thebulgecomponent of galaxies, the masses of NSCs correlate much better with thetotalgalaxy stellar mass. In addition, the mass ratioMNSC/M⋆, totfor NSCs in spirals (at least those with Hubble types Sc and later) is typically an order of magnitude smaller than the mass ratioMBH/M⋆, bulof SMBHs. The absence of a universal “central massive object” correlation argues against common formation and growth mechanisms for both SMBHs and NSCs. We also discuss evidence for a break in the NSC-host galaxy correlation, galaxies with Hubble types earlier than Sbc appear to host systematically more massive NSCs than do types Sc and later.

scholarly journals The Assembly of the First Massive Black Holes

2020 ◽  
Vol 58 (1) ◽  
pp. 27-97 ◽  
Author(s):  
Kohei Inayoshi ◽  
Eli Visbal ◽  
Zoltán Haiman
Keyword(s):  
Black Holes ◽  
First Generation ◽  
Stellar Mass ◽  
Host Galaxy ◽  
Initial Growth ◽  
Host Galaxies ◽  
Potential Wells ◽  
Massive Black Holes ◽  
History Of ◽  
Gas Accretion

The existence of ∼109M⊙ supermassive black holes (SMBHs) within the first billion years of the Universe has stimulated numerous ideas for the prompt formation and rapid growth of black holes (BHs) in the early Universe. Here, we review ways in which the seeds of massive BHs may have first assembled, how they may have subsequently grown as massive as ∼109M⊙, and how multimessenger observations could distinguish between different SMBH assembly scenarios. We conclude the following: ▪  The ultrarare ∼109 M⊙ SMBHs represent only the tip of the iceberg. Early BHs likely fill a continuum from the stellar-mass (∼10M⊙) to the supermassive (∼109) regimes, reflecting a range of initial masses and growth histories. ▪  Stellar-mass BHs were likely left behind by the first generation of stars at redshifts as high as ∼30, but their initial growth typically was stunted due to the shallow potential wells of their host galaxies. ▪  Conditions in some larger, metal-poor galaxies soon became conducive to the rapid formation and growth of massive seed holes, via gas accretion and by mergers in dense stellar clusters. ▪  BH masses depend on the environment (such as the number and properties of nearby radiation sources and the local baryonic streaming velocity) and on the metal enrichment and assembly history of the host galaxy. ▪  Distinguishing between assembly mechanisms will be difficult, but a combination of observations by the Laser Interferometer Space Antenna (probing massive BH growth via mergers) and by deep multiwavelength electromagnetic observations (probing growth via gas accretion) is particularly promising.

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