L. S. Vygotsky Edited and translated by E. Hanfmann and G. Vakar <b>Thought and Language</b>. Massachusetts Institute of Technology: The M. I. T. Press, and New York and London: John Willey and Sons, Inc., 1962. xxi + 168 pp.

Hinshaw, Virgil

doi:10.1086/288002

Cited by 23 publications

(33 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Here the comoving volume of a given redshift slice dV c /dz is computed (e.g., see Hogg 1999) by assuming WMAP9 parameters Ω M = 0.282, Ω Λ = 0.718, h = 0.697 (Hinshaw et al 2012). The factor dt s /dt o = 1/(1 + z) is the ratio between the clock at the source redshift z, which measures the merger rate, and a clock at the Earth, which measures the detection rate.…”

Section: Detection Of Bh-bh Coalescencesmentioning

confidence: 99%

The Formation and Gravitational-Wave Detection of Massive Stellar Black Hole Binaries

Belczyński

Buonanno

Cantiello

et al. 2014

ApJ

138

View full text Add to dashboard Cite

If binaries consisting of two ∼ 100 M ⊙ black holes exist they would serve as extraordinarily powerful gravitational-wave sources, detectable to redshifts of z ∼ 2 with the advanced LIGO/Virgo groundbased detectors. Large uncertainties about the evolution of massive stars preclude definitive rate predictions for mergers of these massive black holes. We show that rates as high as hundreds of detections per year, or as low as no detections whatsoever, are both possible. It was thought that the only way to produce these massive binaries was via dynamical interactions in dense stellar systems. This view has been challenged by the recent discovery of several 150 M ⊙ stars in the R136 region of the Large Magellanic Cloud. Current models predict that when stars of this mass leave the main sequence, their expansion is insufficient to allow common envelope evolution to efficiently reduce the orbital separation. The resulting black-hole-black-hole binary remains too wide to be able to coalesce within a Hubble time. If this assessment is correct, isolated very massive binaries do not evolve to be gravitational-wave sources. However, other formation channels exist. For example, the high multiplicity of massive stars, and their common formation in relatively dense stellar associations, opens up dynamical channels for massive black hole mergers (e.g., via Kozai cycles or repeated binary-single interactions). We identify key physical factors that shape the population of very massive black-holeblack-hole binaries. Advanced gravitational-wave detectors will provide important constraints on the formation and evolution of very massive stars.

show abstract

Section: Detection Of Bh-bh Coalescencesmentioning

confidence: 99%

The Formation and Gravitational-Wave Detection of Massive Stellar Black Hole Binaries

Belczyński

Buonanno

Cantiello

et al. 2014

ApJ

138

View full text Add to dashboard Cite

show abstract

“…Eq. 1 of Hinshaw et al 1996). That is, we describe the high-latitude sky as a fixed quadrupole pattern plus a statistical distribution of higher-order power given by a Harrison-Zel'dovich power spectrum.…”

Section: Quadrupolementioning

confidence: 99%

Microwave Emission at High Galactic Latitudes in the Four-Year DMR Sky Maps

Kogut

Banday

Bennett

et al. 1996

The Astrophysical Journal

227

195

View full text Add to dashboard Cite

We use the COBE 8 Differential Microwave Radiometers (DMR) 4-year sky maps to model Galactic microwave emission at high latitudes (|b| > 20 • ). Cross-correlation of the DMR maps with Galactic template maps detects fluctuations in the highlatitude microwave sky brightness with the angular variation of the DIRBE farinfrared dust maps and a frequency dependence consistent with a superposition of dust and free-free emission. We find no significant correlations between the DMR maps and various synchrotron templates. On the largest angular scales (e.g., quadrupole), Galactic emission is comparable in amplitude to the anisotropy in the cosmic microwave background (CMB). The CMB quadrupole amplitude, after correction for Galactic emission, has amplitude Q rms = 10.7 µK with random uncertainty 3.6 µK and systematic uncertainty 7.1 µK from uncertainty in our knowledge of Galactic microwave emission.

show abstract

“…We attempt to place these results in a larger context in Section 4, before summarizing in Section 5. Throughout the paper we assume a standard lambda cold dark matter (ΛCDM) cosmology based on the final nineyear WMAP results (Hinshaw et al 2012) in which H 0 = 70.0 km s −1 Mpc −1 , Ω m = 0.279 and Ω Λ = 0.721. mass, size and host galaxy. While there is much evidence to suggest that DLAs are the progenitors of massive spiral galaxies, competing interpretations model them as merging clumps of gas.…”

Section: Introductionmentioning

confidence: 99%

Spatially Resolved Emission of a High-Redshift Dla Galaxy With the Keck/Osiris Ifu

Jorgenson

Wolfe

2014

ApJ

View full text Add to dashboard Cite

We present the first Keck/OSIRIS infrared IFU observations of a high redshift damped Lyman−α (DLA) galaxy detected in the line of sight to a background quasar. By utilizing the Laser Guide Star Adaptive Optics (LGSAO) to reduce the quasar PSF to FWHM∼ 0.15 , we were able to search for and map the foreground DLA emission free from the quasar contamination. We present maps of the Hα and [O III] λλ5007, 4959 emission of DLA2222−0946 at a redshift of z ∼ 2.35. From the composite spectrum over the Hα emission region we measure a star formation rate of 9.5 ± 1.0 M year −1 and a dynamical mass, M dyn = 6.1 × 10 9 M . The average star formation rate surface density is Σ SF R = 0.55 M yr −1 kpc −2 , with a central peak of 1.7 M yr −1 kpc −2 . Using the standard Kennicutt-Schmidt relation, this corresponds to a gas mass surface density of Σ gas = 243 M pc −2 . Integrating over the size of the galaxy we find a total gas mass of M gas = 4.2 × 10 9 M . We estimate the gas fraction of DLA2222−0946 to be f gas ∼ 40%. We detect [N II]λ6583 emission at 2.5σ significance with a flux corresponding to a metallicity of 75% solar. Comparing this metallicity with that derived from the low-ion absorption gas ∼6 kpc away, ∼30% solar, indicates possible evidence for a metallicity gradient or enriched in/outflow of gas. Kinematically, both Hα and [O III] emission show relatively constant velocity fields over the central galactic region. While we detect some red and blueshifted clumps of emission, they do not correspond with rotational signatures that support an edge-on disk interpretation.

show abstract

L. S. Vygotsky Edited and translated by E. Hanfmann and G. Vakar Thought and Language. Massachusetts Institute of Technology: The M. I. T. Press, and New York and London: John Willey and Sons, Inc., 1962. xxi + 168 pp.

Cited by 23 publications

References 0 publications

The Formation and Gravitational-Wave Detection of Massive Stellar Black Hole Binaries

The Formation and Gravitational-Wave Detection of Massive Stellar Black Hole Binaries

Microwave Emission at High Galactic Latitudes in the Four-Year DMR Sky Maps

Spatially Resolved Emission of a High-Redshift Dla Galaxy With the Keck/Osiris Ifu

Contact Info

Product

Resources

About