cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Substructures in protoplanetary disks imprinted by compact planetary systems
Creators: name: Garrido-Deutelmoser, Juan
name: Petrovich, Cristobal
name: Krapp, Leonardo
name: Kratter, Kaitlin M.
name: Dong, Ruobing
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets ($\sim10-30\;M_\oplus$) and show that long-standing vortices are a prevalent outcome when their inter-planetary separation ($Δa$) falls below $\sim8$ times $H_{\rm p}$ -- the average disk's scale height at the planets locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least $5,000$ orbits in two regimes: i) fully-shared density gaps with elongated vortices around the stable Lagrange points $L_4$ and $L_5$ for the most compact planet pairs ($Δa \lesssim 4.6\; H_{\rm p}$); ii) partially-shared gaps for more widely spaced planets ($Δa \sim 4.6 - 8\;H_{\rm p}$) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to $\sim3$ and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disk's aspects ratios of $h\gtrsim 0.033$ ($h\gtrsim 0.057$). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.
description: 17 pages, 7 figures, 1 table, submitted to The Astrophysical Journal
CO Excitation and Line Energy Distributions in Gas-selected Galaxies
Creators: name: Klitsch, A.
name: Christensen, L.
name: Valentino, F.
name: Kanekar, N.
name: Møller, P.
name: Zwaan, M. A.
name: Fynbo, J. P. U.
name: Neeleman, M.
name: Prochaska, J. X.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: While emission-selected galaxy surveys are biased towards the most luminous part of the galaxy population, absorption selection is a potentially unbiased galaxy selection technique with respect to luminosity. However, the physical properties of absorption-selected galaxies are not well characterised. Here we study the excitation conditions in the interstellar medium (ISM) in damped Ly$α$ (DLA) absorption-selected galaxies. We present a study of the CO spectral line energy distribution (SLED) in four high-metallicity absorption-selected galaxies with previously reported CO detections at intermediate ($z \sim 0.7$) and high ($z \sim 2$) redshifts. We find further evidence for a wide variety of ISM conditions in these galaxies. Two out of the four galaxies show CO SLEDs consistent with that of the Milky Way inner disk. Interestingly, one of these galaxies is at $z \sim 2$ and has a CO SLED below that of main-sequence galaxies at similar redshifts. The other two galaxies at $z>2$ show more excited ISM conditions, with one of them showing thermal excitation of the mid-$J$ (J$=3, 4$) levels, similar to that seen in two massive main-sequence galaxies at these redshifts. Overall, we find that absorption selection traces a diverse population of galaxies.
description: 10 pages, 5 figures, 6 tables, resubmitted to MNRAS after moderate revision
Dolichognatha mandibularis Thorell
Creators: name: Smith, Helen M.
Publisher: name: Zenodo
Year: 2008
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Arachnida
Araneae
Tetragnathidae
Dolichognatha
Dolichognatha mandibularis

description: Dolichognatha mandibularis (Thorell)
Figs 54–60
Paraebius mandibularis Thorell 1894: 44. Holotype ♂, Sumatra, Lampong. In NHRM, examined. Dolichognatha m. Levi 1981: 277.
Comment. It was initially thought that the male of D. mandibularis (from Sumatra) might pair with D. albida (from Sri Lanka and Thailand) as the short and broad palpal conformation is closest to that of D. deelemanae. However, in general appearance the male D. mandibularis (Figs 54–58) is more similar to males of D. incanescens and D. raveni, with a relatively low carapace, similar eye characteristics, and apparently, no macroseta on the prolateral face of the anterior femora. More specimens are required to resolve this issue and for the time being both species are recognised.
Diagnosis. Male. Palpal bulbus short and rounded, palpal tibia distinctly longer than wide, MEA broad distally (Figs 59, 60).
Female. Unknown.
Description. Male (holotype). Carapace (Figs 54, 57, 58): length 0.86, width 0.67, height 0.29; caput not strongly humped, pear-shaped in dorsal view with caput clearly differentiated. Chelicerae (Fig. 54, 57): cheliceral ledge absent or chelicerae may be pushed up so ledge hidden by carapace; two distinct promarginal cheliceral teeth and one large intermediate, three smaller retromarginal teeth plus basal mound. Labium: with anterior hooked spur. Sternum: concave (but indented by damage). Eyes (Figs 54, 57, 58). AME: 0.10, PME: 0.075, ALE: 0.075, PLE: 0.06, AME–AME: 0.02, AME–ALE: 0.04, PME–PME: 0.02, PME–PLE: 0.04, ALE–PLE: 0.01; no reflective tapeta visible. Legs. I: 3.57, II: 3.06, III: 1.63, IV: 1.94; almost all macrosetae missing, no indication of any prolateral macrosetal bases. Abdomen (Figs 55, 56): length 1.14, width 0.59; apex rounded; post-genital mound indistinct (holotype abdomen is separate from opisthosoma and rather damaged). Male palpus: (Figs 59, 60): palpal femur 0.27× carapace length; patella without macroseta, tibia c. 2× as long as wide; embolus tapering; MEA squat, strongly spoon-shaped distally; conductor, embolus and apophysis all more compact than in D. incanescens; bulbus short and rounded, width: length = 1:1.5. Colour in alcohol: almost entirely creamy-white and in parts semi translucent; PME with hint of black around margins; faint trace of trident-shaped mark on dorsal carapace (Fig. 58).
Distribution. Dolichognatha mandibularis is recorded only from the type locality in Sumatra.
description: Published as part of Smith, Helen M., 2008, Synonymy of Homalopoltys (Araneae: Araneidae) with the genus Dolichognatha (Araneae: Tetragnathidae) and descriptions of two new species, pp. 1-24 in Zootaxa 1775 on pages 18-19, DOI: 10.5281/zenodo.182204
Measurement of simplified template cross sections of the Higgs boson produced in association with W or Z bosons in the H $\to$ $\mathrm{b\bar{b}}$ decay channel in proton-proton collisions at $\sqrt{s}$ = 13 TeV
Creators: name: CMS Collaboration
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Physics - Experiment (hep-ex)
subject: FOS: Physical sciences

description: Differential cross sections are measured for the standard model Higgs boson produced in association with vector bosons (W, Z) and decaying to a pair of b quarks. Measurements are performed within the framework of the simplified template cross sections. The analysis relies on the leptonic decays of the W and Z bosons, resulting in final states with 0, 1, or 2 electrons or muons. The Higgs boson candidates are either reconstructed from pairs of resolved b-tagged jets, or from single large distance parameter jets containing the particles arising from two b quarks. Proton-proton collision data at $\sqrt{s}$ = 13 TeV, collected by the CMS experiment in 2016-2018 and corresponding to a total integrated luminosity of 138 fb$^{-1}$, are analyzed. The inclusive signal strength, defined as the product of the observed production cross section and branching fraction relative to the standard model expectation, combining all analysis categories, is found to be $μ$ = 1.15 $^{+0.22}_{-0.20}$. This corresponds to an observed (expected) significance of 6.3 (5.6) standard deviations.
description: Replaced with the published version. Added the journal reference and the DOI. All the figures and tables, including additional supplementary figures, can be found at http://cms-results.web.cern.ch/cms-results/public-results/publications/HIG-20-001 (CMS Public Pages)
A Fisher information-based incompatibility criterion for quantum channels
Creators: name: Zhang, Qing-Hua
name: Nechita, Ion
Publisher: name: arXiv
Year: 2022
Subjects: subject: Quantum Physics (quant-ph)
subject: Mathematical Physics (math-ph)
subject: FOS: Physical sciences

description: We introduce a new incompatibility criterion for quantum channels, based on the notion of (quantum) Fisher information. Our construction is based on a similar criterion for quantum measurements put forward by H.~Zhu. We then study the power of the incompatibility criterion in different scenarios. Firstly, we prove the first analytical conditions for the incompatibility of two Schur channels. Then, we study the incompatibility structure of a tuple of depolarizing channels, comparing the newly introduced criterion with the known results from asymmetric quantum cloning.
description: 16 pages, 2 figures
title: Reclaimed wastewater: preventing viral pathogens on plant foods: BfR Opinion No 019/2022 of 8 July 2022
Creators: name: Bundesinstitut Für Risikobewertung
Publisher: name: Bundesbehörden und Einrichtungen im Geschäftsbereich des Bundesministeriums für Ernährung und Landwirtschaft (BMEL)
Year: 2022
Subjects: subject: 000

description: BfR-Stellungnahmen, vol. 2022, no. 019
A Multi-Wavelength Study of the Highly Asymmetrical Debris Disk Around HD 111520
Creators: name: Crotts, Katie A.
name: Draper, Zachary H.
name: Matthews, Brenda C.
name: Duchêne, Gaspard
name: Esposito, Thomas M.
name: Wilner, David
name: Mazoyer, Johan
name: Padgett, Deborah
name: Kalas, Paul
name: Stapelfeldt, Karl
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: We observed the nearly edge-on debris disk system HD 111520 at $J$, $H$, & $K1$ near infrared (NIR) bands using both the spectral and polarization modes of the Gemini Planet Imager (GPI). With these new observations, we have performed an empirical analysis in order to better understand the disk morphology and its highly asymmetrical nature. We find that the disk features a large brightness and radial asymmetry, most prominent at shorter wavelengths. We also find that the radial location of the peak polarized intensity differs on either side of the star by 11 AU, suggesting that the disk may be eccentric, although, such an eccentricity does not fully explain the large brightness and radial asymmetry observed. Observations of the disk halo with HST also show the disk to be warped at larger separations, with a bifurcation feature in the northwest, further suggesting that there may be a planet in this system creating an asymmetrical disk structure. Measuring the disk color shows that the brighter extension is bluer compared to the dimmer extension, suggesting that the two sides have different dust grain properties. This finding, along with the large brightness asymmetry, are consistent with the hypothesis that a giant impact occurred between two large bodies in the northern extension of the disk, although confirming this based on NIR observations alone is not feasible. Follow-up imaging with ALMA to resolve the asymmetry in the dust mass distribution is essential in order to confirm this scenario.
description: 15 pages, 5 figures, 4 tables, accepted for publication in ApJ
Using HITRAN to Model Opacities for Planetary Atmospheres: Test case of Microwave Spectra of NH$_3$, SO$_2$ and PH$_3$
Creators: name: Skinner, Frances M.
name: Hargreaves, Robert J.
name: Gordon, Iouli E.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: The latest version of the HITRAN molecular spectroscopic database, HITRAN2020, has recently been released featuring many updates, including line-by-line broadening parameters (and their temperature dependence) appropriate for the dominant constituents of planetary atmospheres. In this work, line shape codes suitable for calculating microwave spectra have been implemented within the HITRAN Application Programming Interface (HAPI). These new additions allow for spectroscopic calculations of microwave absorbing species pertinent to current and future studies of the atmospheres of Jupiter and Venus, and more generally for the atmospheres of gas giants and rocky planets. The inversion spectrum of the NH$_3$ molecule broadened by H$_2$, He and H$_2$O dominates the microwave region of Jupiter. Whereas for Venus, accurate spectroscopic data of SO$_2$ broadened by CO$_2$ is necessary in order to determine its significance, if any, on the reported detection of PH$_3$ in the Venusian upper cloud deck. Comparisons have been made to available microwave laboratory opacities and the following results illustrate that HITRAN data can be used in conjunction with HAPI to reproduce the existing experimental measurements and provide reliable calculation of planetary opacities. Users should be mindful regarding selection of appropriate parameters in HITRAN and selecting suitable line shape functions in HAPI, depending on the spectral region, target molecular species, as well as ambient chemical and thermodynamic conditions.
description: Accepted to the Monthly Notices of the Royal Astronomical Society (MNRAS) June 2022
Dolichognatha
Creators: name: Smith, Helen M.
Publisher: name: Zenodo
Year: 2008
Subjects: Biodiversity
Taxonomy

description: Appendix. Dolichognatha specimens examined as part of this study (and not detailed in text).
Repository & Sex Data Notes
reg. no.
AM KS57548 1 Ψ USA: S.C. Oconee County, Chattooga Det. Dolichognatha pentagona, M. Kuntner
R., 1.5 mi S Russell Brudge (sic) on Rt 2002. No reflective tapeta visible. 28, 1580 ft elevation, 18 July 1998.
description: Published as part of Smith, Helen M., 2008, Synonymy of Homalopoltys (Araneae: Araneidae) with the genus Dolichognatha (Araneae: Tetragnathidae) and descriptions of two new species, pp. 1-24 in Zootaxa 1775 on page 24, DOI: 10.5281/zenodo.182204
Detailed properties of gravitational-wave mergers from flyby perturbations of wide binary black holes in the field
Creators: name: Raveh, Yael
name: Michaely, Erez
name: Perets, Hagai Binyamin
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Wide black hole binaries (wide-BBHs; $\geqslant 10^3$ AU) in the field can be perturbed by random stellar flybys that excite their eccentricities. Once a wide binary is driven to a sufficiently small pericenter approach, gravitational wave (GW) emission becomes significant, and the binary inspirals and merges. In our previous study, using simplified models for wide-BBHs, we found that successive flybys lead to significant merger fractions of wide-BBHs in less than Hubble time, making the flyby perturbation mechanism a relevant contributor to the production rate of GW-sources. However, the exact rates and detailed properties of the resulting GW sources depend on the wide binary progenitors. In this paper we use detailed population synthesis models for the initial wide-BBH population, considering several populations corresponding to different natal-kick models and metallicities, and then follow the wide-BBHs evolution due to flyby perturbations and GW-emission. We show that the cumulative effect of flybys is conductive for the production of GW sources in non-negligible rates of $1-20$ Gpc$^{-3}$ yr$^{-1}$, which are sensitive to the natal kicks model. Such rates are relevant to the observationally inferred rate. Our models, now derived from detailed population of binaries, provide the detailed properties of the produced GW-sources, including mass-functions and delay times. The GW mergers are circularized when enter the aLIGO band; have a preference for high velocity dispersion host galaxies (in particular ellipticals); have a relatively uniform delay-time distribution; and likely have mildly correlated (less than isolated evolution channels and more than dynamical channels) prograde spin-spin and spin-orbits.
description: 13 pages, 8 figures
Mapping the dispersion of the occupied and unoccupied band structure in photoexcited 1T-TiSe$_2$
Creators: name: Huber, Maximilian
name: Lin, Yi
name: Dale, Nicholas
name: Sailus, Renee
name: Tongay, Sefaattin
name: Kaindl, Robert A.
name: Lanzara, Alessandra
Publisher: name: arXiv
Year: 2022
Subjects: subject: Strongly Correlated Electrons (cond-mat.str-el)
subject: FOS: Physical sciences

description: Charge density waves (CDW) are states of broken symmetry with a periodic modulation of charge and lattice typically leading to the opening of a gap in the band structure. In the model CDW system 1T-TiSe$_2$ such a gap opens up between its Se$_{4p}$ valence and Ti$_{3d}$ conduction band, accompanied by a change of dispersion. These changes are crucial in understanding the CDW phase, as they provide a measure of the Se$_{4p}$-Ti$_{3d}$ hybridization strength and characteristic mechanistic features. Using time- and angle-resolved photoelectron spectroscopy (trARPES), the unoccupied band structure is populated with near-infrared (NIR) pump pulses which allows to to directly visualize the parabolically-shaped Ti$_{3d}$ conduction band. Furthermore, we observe a transient change of effective mass in the Se$_{4p}$ valence band following photoexcitation. This occurs alongside an overall reduction due to weakening of the CDW phase and is accompanied by an oscillating component with the frequency of the characteristic A$_{1g}$ phonon. These observations, enabled by trAPRES, highlight the importance of the lattice contributions in establishing the CDW order in 1T-TiSe$_2$.
description: 4 figures
Submersible Gathered Evidence of a Vulnerable Marine Ecosystem at the Melchior Islands, Western Antarctic Peninsula (Subarea 48.1) - multimedia
Creators: name: Lockhart, Susanne
name: Potter, Shaylyn
name: Venus, Chris
name: Weller, Kara
name: Izendooren, Remy
Publisher: name: Zenodo
Year: 2024
Subjects: Occurrence
Observation
VULNERABLE MARINE ECOSYSTEM
VME
CCAMLR
ANTARCTICA
SPONGES
SEA FANS/SEA WHIPS
SEA ANEMONES
LAMP SHELLS
SEA SQUIRTS

description: Description*

Imagery to support a proposed VME based on high abundances of VME indicator taxa that fall within the range of previously registered VMEs. The site is off the east coast of Lambda Island, Melchior Islands, Western Antarctic Peninsula. Video imagery was taken via submersible deployed by Seabourn Venture crewed by scientist and volunteer citizen science pilots. Data on the relative percent cover of all VME indicator taxa was sourced and analysed in the same manner as VMEs added to CCAMLR’s registry in 2018 (SC-CCAMLR-XXXVII) and 2022 (SC-CCAMLR-41) using all data from WG-EMM-18/35, WG-EMM-22/34Rev1 and WG-EMM-22/46Rev1 for a direct comparison. The present site clusters with previously registered VMEs. The site supports many large hexactinellid sponges and small bamboo corals. Notable also, is the presence of the rare and little-known hydroid, Candelabrum sp. – a VME indicator taxa that is particularly vulnerable to fishing gear as they can extend metres into the water column.

Method step description: 

DaVinci Resolve 18 was used to combine separate files where necessary and for editing. 

Clean-up followed the same methodology as was used for analyzing the submarine footage for the successful nomination of VMEs in WG-EMM-22/46Rev1 to remove unusable sequences. For the Lambda Is footage that meant the removal of any sequences where the submersible was too far from the wall, where the visibility was poor and when the submersible was stationary. Footage from Dive A was the longest resulting video after the completion of this clean-up procedure (Table 1), thus it became the footage that was analysed.

Footage was color adjusted within DaVinci Resolve 18.

The analysis methodology also followed that which was used in WG-EMM-22/46Rev1. To compare the relative percent abundance of VME indicator taxa to that of non-VME taxa and bare substrate at the Lambda Is site, frames were exported at regular intervals (30 secs) beginning at 0:00.

The resulting series of images were then imported into the program PAPARA(ZZ)I (Marcon & Purser,  2017). Within this program images were further enhanced by adjusting brightness, contrast and gamma. As recommended by the authors, the usable area was then defined for each image allowing the exclusion of dark or blurred edges.

Once images were prepared in this way, an array of 100 random points was overlayed. Each point in each image was assigned one of three designations: VME indicator taxa, non-VME taxa or bare substrate.
Globular Clusters UVIT Legacy Survey (GlobULeS) I. FUV-optical Color-Magnitude Diagrams for Eight Globular Clusters
Creators: name: Sahu, Snehalata
name: Subramaniam, Annapurni
name: Singh, Gaurav
name: Yadav, Ramakant
name: Valcarce, Aldo R.
name: Choudhury, Samyaday
name: Rani, Sharmila
name: Prabhu, Deepthi S.
name: Chung, Chul
name: Côté, Patrick
name: Leigh, Nathan
name: Geller, Aaron M.
name: Chatterjee, Sourav
name: Rao, N. Kameswara
name: Bandyopadhyay, Avrajit
name: Shara, Michael
name: Dalessandro, Emanuele
name: Pandey, Gajendra
name: Postma, Joesph E.
name: Hutchings, John
name: Simunovic, Mirko
name: Stetson, Peter B.
name: Thirupathi, Sivarani
name: Puzia, Thomas
name: Sohn, Young-Jong
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: We present the first results of eight Globular Clusters (GCs) from the AstroSat/UVIT Legacy Survey program GlobULeS based on the observations carried out in two FUV filters (F148W and F169M). The FUV-optical and FUV-FUV color-magnitude diagrams (CMDs) of GCs with the proper motion membership were constructed by combining the UVIT data with HST UV Globular Cluster Survey (HUGS) data for inner regions and Gaia Early Data Release (EDR3) for regions outside the HST's field. We detect sources as faint as F148W $\sim$ 23.5~mag which are classified based on their locations in CMDs by overlaying stellar evolutionary models. The CMDs of 8 GCs are combined with the previous UVIT studies of 3 GCs to create stacked FUV-optical CMDs to highlight the features/peculiarities found in the different evolutionary sequences. The FUV (F148W) detected stellar populations of 11 GCs comprises 2,816 Horizontal Branch (HB) stars (190 Extreme HB candidates), 46 post-HB (pHB), 221 Blue Straggler Stars (BSS), and 107 White Dwarf (WD) candidates. We note that the blue HB color extension obtained from F148W$-$G color and the number of FUV detected EHB candidates are strongly correlated with the maximum internal Helium (He) variation within each GC, suggesting that the FUV-optical plane is the most sensitive to He abundance variations in the HB. We discuss the potential science cases that will be addressed using these catalogues including HB morphologies, BSSs, pHB, and, WD stars.
description: Accepted for publication in MNRAS; 24 pages, 20 Figures, 6 Tables
Sidydrassus Esyunin & Tuneva 2002
Creators: name: Fomichev, Alexander A.
Publisher: name: Zenodo
Year: 2022
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Arachnida
Araneae
Gnaphosidae
Sidydrassus

description: Sidydrassus Esyunin & Tuneva, 2002
Type species: Drassus shumakovi Spassky, 1934 from Kalmykia (Russia).
Diagnosis. The genus is most similar to Drassodes Westring, 1851 in having straight and pointed RTA, oval tegulum with well visible sinusoidal sperm duct, thick and straight embolus and membranous conductor in males and dual receptacles in females. The males of Sidydrassus can be distinguished from those of Drassodes by the thick embolus and the large median apophysis (vs. filamentous embolus and small median apophysis in Drassodes). The females of Sidydrassus differ from those of Drassodes in having cross-inclined epigynal fovea (vs. rounded in Drassodes). The males of Sidydrassus are also similar to those of Talanites Simon, 1893 in having non filamentous embolus and large median apophysis, but can be separated from it by having long and straight RTA (vs. short and curved in Talanites), medially situated embolus (vs. prolaterally situated embolus in the type species, T. fervidus Simon, 1893) and elongated distal part of the cymbium (vs. short and rounded in Talanites).
Description. Total length: male 6.9–10.5, female 7.8–11.0. Carapace length: male 3.1–4.6, female 3.5–4.0; width: male 2.15–3.1; female 2.45–2.9. Carapace yellow-brown or light brown. Sternum yellow-brown to yellow. Chelicerae brown. Legs yellow to yellow-brown. Abdomen beige or cream-coloured. Spinnerets yellow or yellowbeige. Chelicera with three promarginal teeth (Figs 7–12). Male palp. Femur 2–2.5 times longer than patella. Patella slightly shorter than tibia. Retrolateral tibial apophysis as long as tibia or 2–4 times shorter. Cymbium drop-shaped, longer than tibia. Tibia and cymbium bear several strong spines. Tegulum 1.5–1.8 times longer than wide. Sperm duct C-shaped or sinusoidal. Median apophysis well-developed. Conductor membranous, translucent. Embolic base thick. Embolus short, with a slightly curved tip. Epigyne. Fovea cross-inclined, slit-shaped or wide and round. Median plate in form of an inverted triangle or pentagonal. Receptacles dual: the anterior one spherical, the posterior one flattened.
Composition. Sidydrassus rogue, S. saiynovi sp. n., S. shumakovi and S. tianschanicus.
Distribution. The southern part of Russian Plain, the Caucasus, Iran and Central Asia.
description: Published as part of Fomichev, Alexander A., 2022, A survey of the East Palaearctic Gnaphosidae (Araneae). 12. A review of Sidydrassus Esyunin & Tuneva, 2002, pp. 260-272 in Zootaxa 5194 (2) on page 261, DOI: 10.11646/zootaxa.5194.2.7, http://zenodo.org/record/7147403
title: On the multi-dimensional microparticle fractionation in a sharp-corner serpentine microchannel
Creators: name: Blahout, Sebastian
Publisher: name: UNSPECIFIED
Year: 2022

description: In this thesis, the multi-dimensional fractionation of particles smaller than 10μm with respect to their size and density is investigated inside a sharp-corner serpentine microchannel by means of experimental as well as numerical methods. The motivation for research on multi-dimensional particle fractionation methods is twofold. First, particles with highly specified characteristics are the basis for various products of several different industries. Second, due to environmental or sustainability requirements, particles with defined properties are targeted to be extracted from a bulk quantity. Passive microfluidic approaches have a large potential to provide such fractionation methods, due to their simplicity and parallelizability. One of these approaches is fractionation in sharp-corner serpentine microchannels. This approach is investigated in the present thesis. Long-exposure measurements are performed to investigate the general behavior of particles of several sizes and different densities at various bulk Reynolds numbers (chapter 4). Besides the confirmation of the high potential of the used method to fractionate micron sized particles with regard to their size, the results also reveal the potential to fractionate particles solely with regard to their density. Furthermore, it is demonstrated that the used method is suitable to focus sub-micron particles on distinct trajectories. The reconstruction of three-dimensional particle distributions additionally reveals that micron particles with different sizes and densities not only move on trajectories that are spatially separated in-plane, but also out-of-plane (chapter 5). Astigmatism Particle Tracking Velocimetry measurements also enable to determine a size fractionation performance of nearly 100%. To surpass qualitative descriptions of the force contributions that are relevant for the particle motion inside a serpentine microchannel, numerical simulations are performed (chapter 6). A detailed evaluation of the simulation results reveals that the contributions of the shear-gradient force and depending on the particle size also the drag force are dominant for the motion of a particle inside a serpentine loop under the investigated conditions. Moreover, a new extension of micro Particle Image Velocimetry is presented that provides the opportunity to measure the bulk dynamics of both phases of a suspension flow simultaneously (chapter 7). For this, a labelling procedure is used to create suspension particles with a ring-shaped particle image. A comparison with Gaussian and plateau-shaped particle images showed the superior characteristics of such ring-shaped particle images with respect to measurement accuracy.
Radioactively-Powered Gamma-Ray Transient Associated with a Kilonova from Neutron Star Merger
Creators: name: Chen, Meng-Hua
name: Hu, Rui-Chong
name: Liang, En-Wei
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: AAssociation of GW170817/GRB170817A/AT2017gfo provides the first direct evidence for neutron star mergers as significant sources of $r$-process nucleosynthesis. A gamma-ray transient (GRT) would be powered by the radioactive decay of the freshly-synthesized $r$-process elements. By analyzing the composition and gamma-ray opacity of the kilonova ejecta in details, we calculate the lightcurve and spectrum of the GRT for a range of spherically symmetric merger ejecta models with mass $M_{\rm ej}=0.001 \sim 0.05M_{\odot}$ and expansion velocity $v_{\rm ej}= 0.1\sim 0.4c$. It is found that the peak of the GRT lightcurve depends on $M_{\rm ej}$ and $v_{\rm ej}$ as $t_{\rm pk} \approx 0.5~{\rm days} ~ (M_{\rm ej}/0.01M_{\odot})^{1/2}(v_{\rm ej}/0.1c)^{-1}$ and $L_{\rm pk} \approx 2.0\times10^{41} ~{\rm erg~s} ^{-1} (M_{\rm ej}/0.01M_{\odot})^{1/2}(v_{\rm ej}/0.1c)$. Most radiating photons are in the $100-3000$ keV band and the spectrum peaks at about 800~keV for different nuclear physics inputs. The line features are blurred out by the Doppler broadening effect. Adopting the ejecta parameters reported in literature, we examine the detection probability of the possible GRT associated with AT2017gfo. We show that the GRT cannot be convincingly detected neither with current nor with the proposed missions in the MeV band, such as ETCC and AMEGO. The low gamma-ray flux, together with the extremely low event rate at local universe, makes a discovery of GRTs a great challenge.
description: 16 pages, 7 figures. Accepted for publication in the ApJ Letters
Formation of periodic FRB in binary systems with eccentricity
Creators: name: Barkov, Maxim V.
name: Popov, Sergei B.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Long-term periodicity in the rate of flares is observed for two repeating sources of fast radio bursts (FRBs). In this paper We present a hydrodynamical modeling of a massive binary consisting of a magnetar and an early-type star. We model the interaction of the pulsar wind from the magnetar with an intense stellar wind. It is shown that only during a fraction of the orbital period radio emission can escape the system. This explains the duty cycle of the two repeating FRB sources with periodic activity. The width of the transparency window depends on the eccentricity, stellar wind properties, and the viewing angle. To describe properties of the known sources it is necessary to assume large eccentricities $\gtrsim 0.5$. We apply the maser cyclotron mechanism of the radio emission generation to model spectral properties of the sources. The produced spectrum is not wide: $Δν/ν\sim 0.2$ and the typical frequency depends on the radius of the shock where the emission is generated. The shock radius changes along the orbit. This, together with changing parameters of the medium, allows us to explain the frequency drift during the phase of visibility. Frequency dependence of the degree of polarization at few GHz can be a consequence of a small scale turbulence in the shocked stellar wind. It is much more difficult to explain huge ($\sim 10^5$ [rad/m$^2$]) and variable value of the rotation measure observed for FRB 121102. We suggest that this can be explained if the supernova explosion which produced the magnetar happened near a dense interstellar cloud with $n \sim100$ cm$^{-3}$.
description: 12 pages, 9 figures, accepted by MNRAS
Sidydrassus saiynovi Fomichev 2022, sp. n.
Creators: name: Fomichev, Alexander A.
Publisher: name: Zenodo
Year: 2022
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Arachnida
Araneae
Gnaphosidae
Sidydrassus
Sidydrassus saiynovi

description: Sidydrassus saiynovi sp. n.
Figs 1, 7, 13–15, 19–21, 44
Type. KAZAKHSTAN: Mangystau Oblast: holotype ♂ (ISEA, 001.8936), Ustyurt Nature Reserve, Mamekkazgan Guard Post, near Karazhar Well, 43°24’52”N, 54°33’48”E, takyr, 70 m, 12– 14.04.2018, A.A. Fomichev.
Etymology. The specific name is a patronym honouring Mr Berik Saiynov (Zhanaozen, Kazakhstan), a research fellow from the Ustyurt Nature Reserve, who helped the author to organize an expedition to Ustyurt Plateau, during which this new species was collected.
Diagnosis. In having the large median apophysis (Ma) without a prolateral bent branch, the male of the new species resembles that of S. tianschanicus, from which it differs in having the RTA of the same length as tibia (vs. twice shorter in S. tianschanicus), the embolus (Em) bent prolaterad (vs. straight in S. tianschanicus) and the median apophysis twice as short as the embolus (vs. equal to it in S. tianschanicus) (cf. Figs 13–15, 20 and 16–18, 23).
Description. Male. Total length 7.8. Carapace: 3.55 long, 2.45 wide. Colouration. Carapace and sternum yellow-brown. Labium, endites and chelicerae brown. Coxae pale yellow. Legs pale yellow. Palps pale yellow, cymbium brown. Abdomen beige, ventrally lighter. Spinnerets pale yellow. Leg measurements: I: 3.15, 1.65, 2.8, 2.45, 1.7 (11.75). II: 2.95, 1.4, 2.65, 2.35, 1.65 (11.0). III: 2.85, 1.3, 2.25, 2.4, 1.65 (10.45). IV: 3.6, 1.5, 3.0, 3.7, 1.85 (13.65). Leg spination: I: Fe d1-1-0 p0-1-1; Ti v1-2-0; Mt v2-0-0. II: Fe d1-1-0 p0-1-2; Ti v0-2-0; Mt v3-0-0. III: Fe d1-1-1 p0-1-1 r0-1-1; Ti d1-0-0 p2-0-1 r1-0-1 v2-2-2; Mt d1-2-0 p1-1-0 r1-1-0 v2-2-0. IV: Fe d1-1-1 p0-1-1 r0-1-1; Ti d1-0-1 p1-1-1 r2-0-1 v2-2-2; Mt d1-2-0 p1-1-0 r1-1-0 v2-0-2.
Palp as in Figs 13–15, 19–21. Tegulum (Te) 1.8 times longer than wide. Sperm duct (Sd) clearly visible in ventral view. Median apophysis (Ma) slightly bent prolaterad. Membrane of median apophysis (Mm) well developed. Triangular membrane between embolus and median apophysis reduced. Conductor (Cn) originates at a 11 o’clock position. Embolus (Em) twice as long as median apophysis, with a thick base (Eb) and prolaterally curved apex.
Female unknown.
Distribution. Known only from the type locality in Ustyurt Plateau (Fig. 44).
description: Published as part of Fomichev, Alexander A., 2022, A survey of the East Palaearctic Gnaphosidae (Araneae). 12. A review of Sidydrassus Esyunin & Tuneva, 2002, pp. 260-272 in Zootaxa 5194 (2) on pages 261-264, DOI: 10.11646/zootaxa.5194.2.7, http://zenodo.org/record/7147403
Comment on "On the relations between large-scale models of superfluid helium-4" [Phys. Fluids 33, 127124 (2021]"
Creators: name: Nemirovskii, Sergey K.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Quantum Gases (cond-mat.quant-gas)
subject: Other Condensed Matter (cond-mat.other)
subject: FOS: Physical sciences

description: We comment on the paper by M. Sýkora, M. Pavelka, M. La Mantia, D. Jou, and M. Grmela "On the relations between large-scale models of superfluid helium-4," Physics of Fluids, 33(12):127124(2021), where the authors have developed a formalism for describing a coarse-grained flow of superfluid helium. This formalism is greatly based on the Hall-Vinen-Bekarevich-Khalatnikov (HVBK) model. We strongly disagree with the use of the HVBK equation approach for the case of the three-dimensional quantum turbulence and expose our objections in this comment. We discuss the HVBK method and also criticize the so-called vortex bundles model, which serves as a basis for using the HVBK method in a three-dimensional quantum turbulence.
description: 2 pages, 11 11 references
Imaging of the Quiet Sun in the Frequency Range of 20-80 MHz
Creators: name: Zhang, PeiJin
name: Zucca, Pietro
name: Kozarev, Kamen
name: Carley, Eoin
name: Wang, ChuanBing
name: Franzen, Thomas
name: Dabrowski, Bartosz
name: Krankowski, Andrzej
name: Magdalenic, Jasmina
name: Vocks, Christian
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Space Physics (physics.space-ph)
subject: FOS: Physical sciences

description: Radio emission of the quiet Sun is considered to be due to thermal bremsstrahlung emission of the hot solar atmosphere. The properties of the quiet Sun in the microwave band have been well studied, and they can be well described by the spectrum of bremsstrahlung emission. In the meter-wave and decameter-wave bands, properties of the quiet Sun have rarely been studied due to the instrumental limitations. In this work, we use the LOw Frequency ARray (LOFAR) telescope to perform high quality interferometric imaging spectroscopy observations of quiet Sun coronal emission at frequencies below 90~MHz. We present the brightness temperature spectrum, and size of the Sun in the frequency range of 20-80~MHz. We report on dark coronal regions with low brightness temperature that persist with frequency. The brightness temperature spectrum of the quiet Sun is discussed and compared with the bremsstrahlung emission of a coronal model and previous quiet Sun observations.
description: 20 pages
title: Pharaonic Obsessions: Ancient Egypt, an Australian Story
Creators: name: Richards, Candace
Publisher: name: The University of Sydney
Year: 2021

description: Pharaonic Obsessions: Ancient Egypt, an Australian Story explores the modern history of Egyptology through the lens of Australian collecting practices, showcasing the University of Sydney’s significant holdings of ancient Egyptian material culture. Conceptually divided into two themes, ‘objects of obsession’ and ‘sites of obsession’, this exhibition examines the stories of prominent Australians who helped shape the University’s collection, and investigates the reception of ancient Egyptian heritage in Australian society from the mid-19th to the mid-20th century. Historic photography, rare books, poster art and social history collections are entwined within the displays of ancient artefacts to explicitly place the collection in its colonial framework.
Diagnostic functions of solar coronal magnetic fields from radio observations
Creators: name: Tan, Baolin
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: In solar physics, it is a big challenge to measure the magnetic fields directly from observations in the upper solar atmosphere, including the chromosphere and corona. Radio observations are regarded as the most feasible approach to diagnose the magnetic field in solar chromosphere and corona. However, because of the complexity and diversity of the emission mechanisms, the previous studies have only presented the implicit diagnostic functions of the magnetic field for specific mechanism from solar radio observations. This work collected and sorted out all methods for diagnosing coronal magnetic field from solar radio observations, which are expressed as a set of explicit diagnostic functions. In particular, this work supplemented some important diagnostic methods missed in other reviews. This set of diagnostic functions can completely cover all regions of the solar chromosphere and corona, including the quiet region, active region and flaring source regions. At the same time, it also includes incoherent radiation such as bremsstrahlung emission of thermal plasma above the quiet region, cyclotron and gyro-synchrotron emissions of magnetized hot plasma and mildly relativistic nonthermal electrons above the active regions, as well as coherently plasma emission around flaring source regions. Using this set of diagnostic functions and the related broadband spectral solar radio imaging observations, we can derive the magnetic fields of almost all regions in the solar atmosphere,which may help us to make full use of the spectral imaging observations of the new generation solar radio telescopes (such as MUSER, EVOSA and the future FASR, etc.) to study the solar activities, and provide a reliable basis for the prediction of disastrous space weather events.
description: 19 pages, accepted by RAA
Quantum Tomography and Schwinger's Picture of Quantum Mechanics
Creators: name: Ciaglia, Florio M.
name: Di Cosmo, Fabio
name: Ibort, Alberto
name: Marmo, Giuseppe
Publisher: name: arXiv
Year: 2022
Subjects: subject: Quantum Physics (quant-ph)
subject: Mathematical Physics (math-ph)
subject: FOS: Physical sciences

description: In this paper the problem of tomographic reconstruction of states is investigated within the so-called Schwinger's picture of Quantum Mechanics in which a groupoid is associated with every quantum system. The attention is focused on spin tomography: In this context the groupoid of interest is the groupoid of pairs over a finite set. In a nutshell, this groupoid is made up of transitions between all possible pairs of outcomes belonging to a finite set. In addition, these transitions possess a partial composition rule, generalizing the notion of groups. The main goal of the paper consists in providing a reconstruction formula for states on the groupoid-algebra associated with the observables of the system. Using the group of bisections of this groupoid, which are special subsets in one-to-one correspondence with the outcomes, a frame is defined and it is used to prove the validity of the tomographic reconstruction. The special case of the set of outcomes being the set of integers modulo n, with n odd prime, is considered in detail. In this case the subgroup of discrete affine linear transformations, whose graphs are linear subspaces of the groupoid, provides a \textit{quorum} in close analogy with the continuos case.
description: 32 pages
Frequency analysis of KIC 1573174 : shedding light on the nature of HADS stars
Creators: name: Lv, Chenglong
name: Esamdin, Ali
name: Pascual-Granado, Javier
name: Yang, Taozhi
name: Shen, Dongxiang
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: We propose that KIC 1573174 is a quadruple-mode $δ$ Scuti star with pulsation amplitudes between those of the HADS (high-amplitude Delta Scuti star) group and average low-amplitude pulsators. The radial modes detected in this star provide a unique opportunity to exploit asteroseismic techniques up to their limits. Detailed frequency analysis is given for the light curve from the Kepler mission. The variation of the light curve is dominated by the strongest mode with a frequency of F0 = 7.3975 $\rm{d^{-1}}$, as shown by Fourier analysis of long cadence data (Q1-Q17, spanning 1460 days), indicating that the target is a $δ$ Scuti star. The other three independent modes with F1 = 9.4397 d$^{-1}$, F2 = 12.1225 d$^{-1}$ and F3 = 14.3577 d$^{-1}$, have ratios of $P_{1}$ / $P_{0}$, $P_{2}$ / $P_{0}$ and $P_{3}$ / $P_{0}$ estimated as 0.783, 0.610 and 0.515, which indicate that KIC 1573174 is a quadruple-mode $δ$ Scuti star. A different approach has been used to determine the $O-C$ through the study of phase modulation. The change of period $(1/P)~dP/dt$ is obtained resulting in $-1.14 \times 10^{-6}~\text{yr}^{-1}$ and $-4.48 \times 10^{-6}~\text{yr}^{-1}$ for F0 and F1 respectively. Based on frequency parameters (i.e., F0, F1, F2, and F3), a series of theoretical models were conducted by employing the stellar evolution code MESA. The ratio of observed $f_{1}/f_{2}$ is larger than that of the model, which may be caused by the rotation of the star. We suggest high-resolution spectral observation is highly desired in the future to further constrain models.
description: 15 pages, 8 figures, accepted for publication in ApJ
Sonnenfleckenzeichnung unnummeriert.
Zeichnung von Flecken und Fackelflächen zur Ermittlung der Sonnenaktivität am 20.07.1943, erstellt von F. Succi, Privatastronom in Rom
Creators: name: [s.n.]
Publisher: name: [s.n.]
Year: 1943

description: Bleistiftzeichnung mit Tinte und Farbstift, erstellt als Zeichnung nach eigener Vorlage in Rom. Instrument: unbekannt
Supplementary Files for the paper: Genome-wide association analyses reveals copy number variant regions associated with reproduction and disease traits in Canadian Holstein cattle. By Oliveira et al.
Creators: name: Rojas de Oliveira, Hinayah
name: Chud, Tatiane C. S.
name: A. Oliveira Junior, Gerson
name: C. Hermisdorff, Isis
name: G. Narayana, Saranya
name: Rochus, Christina M.
name: M. Butty, Adrien
name: Malchiodi, Francesca
name: Stothard, Paul
name: Miglior, Filippo
name: Baes, Christine F.
name: Schenkel, Flavio S.
Publisher: name: figshare
Year: 2024
Subjects: classificationCode: 300305
subject: Animal reproduction and breeding

description: Supplementary files for the paper titled: Genome-wide association analyses reveals copy number variant regions associated with reproduction and disease traits in Canadian Holstein cattle, published in the Journal of Dairy Sciences by Oliveira et al.
Milky Way thin and thick disk kinematics with GAIA EDR3 and RAVE DR5
Creators: name: Vieira, Katherine
name: Carraro, Giovanni
name: Korchagin, Vladimir
name: Lutsenko, Artem
name: Girard, Terrence M.
name: van Altena, William
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present a detailed analysis of kinematics of the Milky Way disk in solar neighborhood using GAIA DR3 catalog. To determine the local kinematics of the stellar disks of the Milky Way galaxy we use a complete sample of 278,228 red giant branch (RGB) stars distributed in a cylinder, centered at the Sun with a 1 kpc radius and half-height of 0.5 kpc. We determine separately the kinematical properties of RGB stars for each Galactic hemisphere in search for possible asymmetries. The kinematical properties of the RGB stars reveal the existence of two kinematically distinct components: the thin disk with mean velocities ${V_R}, {V_ϕ}, {V_Z}$ of about -1, -239, 0 km s$^{-1}$ correspondingly and velocity dispersions $σ_R, σ_ϕ, σ_Z$ of 31, 20 and 11 km s$^{-1}$, and the Thick disk with mean velocities components of about +1, -225, 0 km s$^{-1}$, and velocity dispersions of 49, 35, and 22 km s$^{-1}$. We find that up to 500 pc height above/below the galactic plane, Thick disk stars comprise about half the stars of the disk. Such high amount of RGB stars with Thick disk kinematics points at the secular evolution scenario origin for the Thick disk of the Milky Way galaxy.
description: 14 pages, 9 figures