Characterization of neural entrainment to speech with and without slow spectral energy fluctuations in laminar recordings in monkey A1

NeuroImage ◽  
2017 ◽  
Vol 150 ◽  
pp. 344-357 ◽  
Author(s):  
Benedikt Zoefel ◽  
Jordi Costa-Faidella ◽  
Peter Lakatos ◽  
Charles E. Schroeder ◽  
Rufin VanRullen
Author(s):  
Yohei Koizumi ◽  
Masayuki Kuzuhara ◽  
Masashi Omiya ◽  
Teruyuki Hirano ◽  
John Wisniewski ◽  
...  

Abstract We present the optical spectra of 338 nearby M dwarfs, and compute their spectral types, effective temperatures (Teff), and radii. Our spectra were obtained using several optical spectrometers with spectral resolutions that range from 1200 to 10000. As many as 97% of the observed M-type dwarfs have a spectral type of M3–M6, with a typical error of 0.4 subtype, among which the spectral types M4–M5 are the most common. We infer the Teff of our sample by fitting our spectra with theoretical spectra from the PHOENIX model. Our inferred Teff is calibrated with the optical spectra of M dwarfs whose Teff have been well determined with the calibrations that are supported by previous interferometric observations. Our fitting procedures utilize the VO absorption band (7320–7570 Å) and the optical region (5000–8000 Å), yielding typical errors of 128 K (VO band) and 85 K (optical region). We also determine the radii of our sample from their spectral energy distributions. We find most of our sample stars have radii of <0.6 R⊙, with the average error being 3%. Our catalog enables efficient sample selection for exoplanet surveys around nearby M-type dwarfs.


2020 ◽  
Vol 492 (3) ◽  
pp. 3459-3464 ◽  
Author(s):  
Maurizio Salaris ◽  
Chris Usher ◽  
Silvia Martocchia ◽  
Emanuele Dalessandro ◽  
Nate Bastian ◽  
...  

ABSTRACT The existence of star-to-star light-element abundance variations (multiple populations, MPs) in massive Galactic and extragalactic star clusters older than about 2 Gyr is by now well established. Photometry of red giant branch (RGB) stars has been and still is instrumental in enabling the detection and characterization of cluster MPs, through the appropriate choices of filters, colours, and colour combinations that are mainly sensitive to N and – to a lesser degree – C stellar surface abundances. An important issue not yet properly addressed is that the translation of the observed widths of the cluster RGBs to abundance spreads must account for the effect of the first dredge-up on the surface chemical patterns, hence on the spectral energy distributions of stars belonging to the various MPs. We have filled this gap by studying theoretically the impact of the dredge-up on the predicted widths of RGBs in clusters hosting MPs. We find that for a given initial range of N abundances, the first dredge-up reduces the predicted RGB widths in N-sensitive filters compared to the case when its effect on the stellar spectral energy distributions is not accounted for. This reduction is a strong function of age and has also a dependence on metallicity. The net effect is an underestimate of the initial N-abundance ranges from RGB photometry if the first dredge-up is not accounted for in the modelling, and also the potential determination of spurious trends of N-abundance spreads with age.


Author(s):  
Amanda L. Heiderman ◽  
Neal J. Evans

AbstractCharacterization of how dense molecular cores evolve into stars has historically been made through observational changes in their 2 to 25 μm spectral energy distribution (SED) or bolometric temperature via the Class system. Linking these observational classes to a physical protostellar phase or Stages in a consistent manner remains challenging. In order to provide a uniform indicator of whether an observationally classified embedded protostar candidate is likely to be a physical phase Stage 0 or I protostar, we performed an HCO+(J=3-2) survey of Class 0+I and Flat SED young stellar objects (YSOs) in the Spitzer nearby (D < 500 pc) Gould Belt cloud surveys. We use criteria from van Kempen et al.(2009) to classify sources as Stage 0+I or bona fide protostars and find 84% of our HCO+ detected sources meet that criteria. We recommend 0.54 Myr as an evolutionary timescale for these embedded protostars. We discuss trends in our sample with spatial distribution, molecular cloud extinction, spectral index, and bolometric temperature and luminosity.


2017 ◽  
Vol 599 ◽  
pp. A51 ◽  
Author(s):  
◽  
N. Aghanim ◽  
M. Ashdown ◽  
J. Aumont ◽  
C. Baccigalupi ◽  
...  

The characterization of the Galactic foregrounds has been shown to be the main obstacle in thechallenging quest to detect primordial B-modes in the polarized microwave sky. We make use of the Planck-HFI 2015 data release at high frequencies to place new constraints on the properties of the polarized thermal dust emission at high Galactic latitudes. Here, we specifically study the spatial variability of the dust polarized spectral energy distribution (SED), and its potential impact on the determination of the tensor-to-scalar ratio, r. We use the correlation ratio of the CBBℓ angular power spectra between the 217 and 353 GHz channels as a tracer of these potential variations, computed on different high Galactic latitude regions, ranging from 80% to 20% of the sky. The new insight from Planck data is a departure of the correlation ratio from unity that cannot be attributed to a spurious decorrelation due to the cosmic microwave background, instrumental noise, or instrumental systematics. The effect is marginally detected on each region, but the statistical combination of all the regions gives more than 99% confidence for this variation in polarized dust properties. In addition, we show that the decorrelation increases when there is a decrease in the mean column density of the region of the sky being considered, and we propose a simple power-law empirical model for this dependence, which matches what is seen in the Planck data. We explore the effect that this measured decorrelation has on simulations of the BICEP2-Keck Array/Planck analysis and show that the 2015 constraints from these data still allow a decorrelation between the dust at 150 and 353 GHz that is compatible with our measured value. Finally, using simplified models, we show that either spatial variation of the dust SED or of the dust polarization angle are able to produce decorrelations between 217 and 353 GHz data similar to the values we observe in the data.


Author(s):  
Raffaele Volpe ◽  
Philippe Devinant ◽  
Azeddine Kourta

The increasing demand for such vehicles as station wagons or minivans has focused aerodynamic research for drag reduction on squareback models of which, the one proposed by Ahmed et al. [1] is one of the most used. The presented study aims at finely characterize the natural wake of a 1:1 squareback Ahmed body with experimental measurements, in order to draw possible strategies for drag reduction. Our analysis focused both on the detection of the mean wake topology, by means of 2D PIV as well as parietal pressure measurements, and on the study of the spectral fluctuations of velocity and pressures. The experimental results exhibit a left/right bistable behavior for the wake, highly sensitive to the incoming wind yaw angle, so that, most generally, the mean aerodynamic field shows an asymmetric behavior due to the predominance of one of the two stable positions. The characterization of the mean wake by averaging the fields on the whole acquisition time can then be biased and show an asymmetrical wake. Then, as far as the symmetric average field is of interest, it is relevant to study separately each topology using conditional averaging, and then build a symmetrical field by averaging the two bistable phases. The analysis shows that the well-known symmetrical wake and the corresponding rear pressure field derive from a random rotation of the toric recirculation bubble, which can induce instantaneous pressure losses of about 25%. The bistability does not affect the spectral energy distribution. Our results show a spectral activity mostly at low frequencies. In particular, we found in measurements along the vertical symmetry plane a peak at StH = 0.07, indicating the presence of the “bubble pumping” phenomenon, whereas pressure measurements at vehicle mid-height indicate the existence of vortex shedding.


2019 ◽  
pp. 122315EQS188M
Author(s):  
Ashly Cabas ◽  
Adrian Rodriguez-Marek

Input motions used in seismic site response analyses are commonly selected based on similarities between the shear wave velocity (Vs) at the recording station, and the reference depth at the site of interest (among other aspects such as the intensity of the expected ground motion). This traditional approach disregards the influence of the attenuation in the shallow crust on site response. Given that this attenuation (damping) can be characterized by the distance-independent high-frequency attenuation parameter 0, a Vs-0 correction framework for input motions is proposed to render them compatible with the assumed properties of the reference depth at the site. The proposed correction factors were applied to a subset of recordings from the KiK-net database, and compared to traditional deconvolution. Results indicate that Vs-0 corrected motions outperform deconvolved motions in the characterization of the spectral energy in the high-frequency range. However, motions recorded at sites with soft deposits are not good candidates for the Vs-0 correction approach. Vs-0 corrections also affect amplification functions which are important in the assessment of site-specific seismic hazards.


2021 ◽  
Author(s):  
Bryce T. Bolin ◽  
Wing-Huen Ip ◽  
Frank J. Masci ◽  
George Helou

&lt;p&gt;Near-Earth asteroid population models predict a small population of asteroids located entirely within the orbit of Venus. We report the discovery of the first inner-Venus asteroid (IVA), 2020 AV&lt;sub&gt;2&lt;/sub&gt;, was first detected by the Zwicky Transient Facility (ZTF) on the Samuel Oschin Telescope 48-inch telescope at Palomar Observatory on 2020 January 4. Recovery observations by the Spectral Energy Distribution Machine on the Palomar 60-inch Telescope and the Lulin Optical Telescope at Lulin Observatory in late 2021 November greatly extended its orbit to ~330 days confirm its location inside the orbit of Venus and allowing for detail investigation of its dynamical evolution. In addition, a comparison with the NEO model reveals its likely source location in agreement with recent spectroscopic observations. In addition, we provide an estimate of our observational completeness for detecting inner-Venus asteroids with ZTF with implications on the expected number of their detection.&lt;/p&gt;


2017 ◽  
Vol 33 (3) ◽  
pp. 917-941 ◽  
Author(s):  
Ashly Cabas ◽  
Adrian Rodriguez-Marek

Input motions used in seismic site response analyses are commonly selected based on similarities between the shear wave velocity ( V S) at the recording station, and the reference depth at the site of interest (among other aspects such as the intensity of the expected ground motion). This traditional approach disregards the influence of the attenuation in the shallow crust on site response. Given that this attenuation (damping) can be characterized by the distance-independent high-frequency attenuation parameter κ0, a V S -κ0 correction framework for input motions is proposed to render them compatible with the assumed properties of the reference depth at the site. The proposed correction factors were applied to a subset of recordings from the KiK-net database, and compared to traditional deconvolution. Results indicate that V S -κ0 corrected motions outperform deconvolved motions in the characterization of the spectral energy in the high-frequency range. However, motions recorded at sites with soft deposits are not good candidates for the V S -κ0 correction approach. V S -κ0 corrections also affect amplification functions which are important in the assessment of site-specific seismic hazards.


2008 ◽  
Vol 120 (865) ◽  
pp. 328-338 ◽  
Author(s):  
Nanyao Lu ◽  
Paul S. Smith ◽  
Charles W. Engelbracht ◽  
Alberto Noriega-Crespo ◽  
Jane Morrison ◽  
...  

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