cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Breaking the rules at $z\simeq$0.45: the rebel case of RBS 1055
Creators: name: Marinucci, A.
name: Vietri, G.
name: Piconcelli, E.
name: Bianchi, S.
name: Guainazzi, M.
name: Lanzuisi, G.
name: Stern, D.
name: Vignali, C.
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: We report on a long (250 ks) NuSTAR observation of the bright quasar RBS 1055 performed in March 2021, and archival XMM-Newton pointings (185 ks) taken in July 2014. An optical spectrum of the source taken with the Double Spectrograph at the Palomar Observatory, quasi-simultaneous with the NuSTAR observations, is also analyzed. We find that the two-coronae model, in which a warm and hot corona coexist, well reproduces its broad band spectrum, with temperatures kT$_e=0.12^{+0.08}_{-0.03}$ keV, kT$_e=30^{+40}_{-10}$ keV and Thomson optical depths $τ$=30$_{-10}^{+15}$ and $τ$=3.0$_{-1.4}^{+1.0}$ for the former and the latter component, respectively. We confirm the presence of an intense Fe K$α$ emission line (EW=55$\pm$6 eV) and, when a toroidal model is considered for reproducing the Compton reflection, a Compton-thin solution with N$_{\rm H}=(3.2^{+0.9}_{-0.8})\times10^{23}$ cm$^{-2}$ for the circumnuclear reflector is found. The analysis of the optical spectrum reveals a likely peculiar configuration of our line of sight with respect to the nucleus, and the presence of a broad [O III] component, tracing outflows in the NLR, with a velocity shift $v=$1500$\pm100$ km s$^{-1}$, leading to a mass outflow rate $\dot{M}_{\rm out}=25.4\pm1.5$ M$_{\odot}$ yr$^{-1}$ and outflow kinetic power $\dot{E}_{\rm kin}$/L$_{\rm Bol}$ $\sim$0.33%. We estimate the BH mass to be in the range 2.8$\times$10$^{8}$-1.2$\times$10$^{9}$ M$_{\odot}$, according to different BLR emission lines, with an average value of <$M\rm_{BH}$>=6.5$\times$10$^{8}$ M$_{\odot}$. With an Fe K$α$ which is 3$σ$ above the value predicted from the EW-L$_{2-10\ \rm keV}$ relation and an extreme source brightness at 2 keV (a factor 10-15 higher than the one expected from the optical/UV), RBS 1055 confirms to be an outlier in the X-rays, compared to other objects in the same luminosity and redshift range.
description: 11 pages, 10 figures, 4 tables. Accepted for publication in Astronomy & Astrophysics
The conditional colour-magnitude distribution: II. A comparison of galaxy colour and luminosity distribution in galaxy groups
Creators: name: Xu, Haojie
name: Zheng, Zheng
name: Yang, Xiaohu
name: Li, Qingyang
name: Guo, Hong
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: The Conditional Colour-Magnitude Distribution (CCMD) is a comprehensive formalism of the colour-magnitude-halo mass relation of galaxies. With joint modelling of a large sample of SDSS galaxies in fine bins of galaxy colour and luminosity, Xu et al. inferred parameters of a CCMD model that well reproduces colour- and luminosity-dependent abundance and clustering of present-day galaxies. In this work, we provide a test and investigation of the CCMD model by studying the colour and luminosity distribution of galaxies in galaxy groups. An apples-to-apples comparison of group galaxies is achieved by applying the same galaxy group finder to identify groups from the CCMD galaxy mocks and from the SDSS data, avoiding any systematic effect of group finding and mass assignment on the comparison. We find an overall nice agreement in the conditional luminosity function (CLF), the conditional colour function (CCF), and the CCMD of galaxies in galaxy groups inferred from CCMD mock and SDSS data. We also discuss the subtle differences revealed by the comparison. In addition, using two external catalogues constructed to only include central galaxies with halo mass measured through weak lensing, we find that their colour-magnitude distribution shows two distinct and orthogonal components, in line with the prediction of the CCMD model. Our results suggest that the CCMD model provides a good description of halo mass dependent galaxy colour and luminosity distribution. The halo and CCMD mock catalogues are made publicly available to facilitate other investigations.
description: Match with published version. The halo catalogues and CCMD mocks are publicly available at https://www.astro.utah.edu/~zhengzheng/data.html
Urgleptes duffyi Gilmour 1961
Creators: name: Monné, Miguel A.
Publisher: name: Zenodo
Year: 2005
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Coleoptera
Cerambycidae
Urgleptes
Urgleptes duffyi

description: 22. Urgleptes duffyi Gilmour, 1961
Type locality — Mexico, Veracruz: La Buena Ventura. (AMNH). Distribution — Mexico (Veracruz).
 Urgleptes duffyi Gilmour, 1961b: 339, fig. 2; Chemsak et al., 1992: 148 (cat.); Noguera & Chemsak, 1996: 407 (cat.).
description: Published as part of Monné, Miguel A., 2005, Catalogue of the Cerambycidae (Coleoptera) of the Neotropical Region. Part II. Subfamily Lamiinae, pp. 1-760 in Zootaxa 1023 (1) on pages 1-760, DOI: 10.11646/zootaxa.946.1.1, http://zenodo.org/record/5049553
Non-canonical maximum cliques without a design structure in the block graphs of 2-designs
Creators: name: Goryainov, Sergey
name: Konstantinova, Elena V.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Combinatorics (math.CO)
subject: FOS: Mathematics

description: In this note we answer positively a question of Chris Godsil and Karen Meagher on the existence of a 2-design whose block graph has a non-canonical maximum clique without a design structure.
Stellar migrations and metal flows -- Chemical evolution of the thin disc of a simulated Milky Way analogous galaxy
Creators: name: Vincenzo, Fiorenzo
name: Kobayashi, Chiaki
Publisher: name: arXiv
Year: 2020
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: In order to understand the roles of metal flows in galaxy formation and evolution, we analyse our self-consistent cosmological chemo-dynamical simulation of a Milky Way like galaxy during its thin-disc phase. Our simulated galaxy disc qualitatively reproduces the variation of the dichotomy in [$α$/Fe]-[Fe/H] at different Galactocentric distances as derived by APOGEE-DR16, as well as the stellar age distribution in [$α$/Fe]-[Fe/H] from APOKASC-2. The disc grows from the inside out, with a radial gradient in the star-formation rate during the entire phase. Despite the radial dependence, the outflow-to-infall ratio of metals in our simulated halo shows a time-independent profile scaling with the disc growth. The simulated disc undergoes two modes of gas inflow: (i) an infall of metal-poor and relatively low-[$α$/Fe] gas, and (ii) a radial flow where already chemically-enriched gas moves inwards with an average velocity of $\sim0.7$ km/s. Moreover, we find that stellar migrations mostly happen outwards, on typical time scales of $\sim5$ Gyr. Our predicted radial metallicity gradients agree with the observations from APOGEE-DR16, and the main effect of stellar migrations is to flatten the radial metallicity profiles by 0.05 dex/kpc in the slopes. We also show that the effect of migrations can appear more important in [$α$/Fe] than in the [Fe/H]-age relation of thin-disc stars.
description: Accepted for publication in MNRAS
Kinematically quiet halos around z~2.5 radio galaxies. Keck spectroscopy
Creators: name: Villar-Martin, M.
name: Vernet, J.
name: Alighieri, S. di Serego
name: Fosbury, R.
name: Humphrey, A.
name: Pentericci, L.
Publisher: name: arXiv
Year: 2003
Subjects: subject: Astrophysics (astro-ph)
subject: FOS: Physical sciences

description: We present the results of the kinematic study of the extended gas in a sample of 10 high redshift radio galaxies (z~2.5) based on high signal to noise Keck II and VLT long slit spectroscopy. In addition to the typical high surface brightness kinematically perturbed regions (FWHM and velocity shifts >1000 km/s), we find in all objects giant low surface brightness halos which show quieter kinematics with typical emission line FWHM and velocity shifts of several hundred km/s. The giant halos often extend for more than 100 kpc and sometimes beyond the radio structures. Their emission line specta are typical of high redshift active galaxies. Continuum is also often detected. The halos are enriched with heavy elements at tens of kpc from the active nucleus. The quasar continuum is the dominant source of ionization of the quiescent halos along the radio axis. The detection of giant quiescent halos in all objects suggests that they could be a common ingredient of high redshift radio galaxies. The radio galaxies seem to be embedded within the halos. The nature, origin of the halos and the cosmological implications are also discussed.
description: 23 pages, 10 figures. Accepted for publication in MNRAS
Diffusion in stellar interiors: critical tests of three numerical methods
Creators: name: Meynet, Georges
name: Maeder, Andre
name: Mowlavi, Nami
Publisher: name: arXiv
Year: 2003
Subjects: subject: Astrophysics (astro-ph)
subject: FOS: Physical sciences

description: We describe and discuss the properties of three numerical methods for solving the diffusion equation for the transport of the chemical species and of the angular momentum in stellar interiors. We study through numerical experiments both their accuracy and their ability to provide physical solutions. On the basis of new tests and analyses applied to the stellar astrophysical context, we show that the most robust method to follow the secular evolution is the implicit finite differences method. The importance of correctly estimating the diffusion coefficient between mesh points is emphasized and a procedure for estimating the average diffusion coefficient between a convective and a radiative zone is described.
description: 15 pages, 8 figures. accepted for publication in Astronomy and Astrophysics
The soft X-ray background with Suzaku: I. Milky Way halo
Creators: name: Ueda, Masaki
name: Sugiyama, Hayato
name: Kobayashi, Shogo B.
name: Fukushima, Kotaro
name: Yamasaki, Noriko Y.
name: Sato, Kosuke
name: Matsushita, Kyoko
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We present measurements of the soft X-ray background emission for 130 Suzaku observations at $75^\circ15^\circ$ obtained from 2005 to 2015, covering nearly one solar cycle. In addition to the standard soft X-ray background model consisting of the local hot bubble and the Milky Way Halo (MWH), we include a hot collisional-ionization-equilibrium component with a temperature of $\sim 0.8$ keV to reproduce spectra of a significant fraction of the lines of sight. Then, the scatter in the relation between the emission measure vs. temperature of the MWH component is reduced. Here, we exclude time ranges with high count rates to minimize the effect of the solar wind charge exchange (SWCX). However, the spectra of almost the same lines of sight are inconsistent. The heliospheric SWCX emissions likely contaminate and gives a bias in measurements of temperature and the emission measure of the MWH. Excluding the data around the solar maximum and using the data taken before the end of 2009, at $|b|>35^\circ$ and $105^\circ
description: 20 pages, 16 figures, Accepted for publication in PASJ
Trypanidius albosignatus Melzer 1932
Creators: name: Monné, Miguel A.
Publisher: name: Zenodo
Year: 2005
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Coleoptera
Cerambycidae
Trypanidius
Trypanidius albosignatus

description: 1. Trypanidius albosignatus Melzer, 1932
Type locality — Brazil, Rio de Janeiro: Itatiaia. (MZSP). Distribution — Brazil (Bahia to Rio de Janeiro).
 Trypanidius albosignatus Melzer, 1932a: 226, pl. 4, fig. 12; Zikán & Zikán, 1944: 37 (distr.); Zikán & Wygodzinsky, 1948: 66 (type); Zajciw, 1972a: 64 (distr.); 1974a: 73 (distr.).
description: Published as part of Monné, Miguel A., 2005, Catalogue of the Cerambycidae (Coleoptera) of the Neotropical Region. Part II. Subfamily Lamiinae, pp. 1-760 in Zootaxa 1023 (1) on pages 1-760, DOI: 10.11646/zootaxa.946.1.1, http://zenodo.org/record/5049553
title: A "cell-free" system to study regulation of focal adhesions and of the connected actin cytoskeleton.
Creators: name: Cattelino, Anna
Publisher: name: The Open University
Year: 2000

description: The exact composition of focal adhesions and the role of single components in their assembly and regulation during dynamic adhesive processes are poorly understood. I have characterised and used a "cell-free" system consisting of ventral plasma membranes (VPMs) prepared from adherent fibroblasts, and found that this subcellular fraction preserves intact focal adhesion components and the connected actin cytoskeleton. Moreover, VPMs show an accumulation of several tyrosine phosphorylated proteins, including tyrosine phosphorylated focal adhesion kinase and paxillin. In particular, a pool of higly phosphorylated paxillin is found in focal adhesions, suggesting an important role for the phosphorylated polypeptide in the mechanism of integrin-mediated adhesion.
With the aim of obtaining new important tools for my studies, I have produced and characterised monoclonal antibodies (mAbs) raised against VPM preparations.
The use of VPM preparations as a "cell-free" system has shown that changes in [Ca2+] can affect integrin behaviour within VPMs. I observed a correlation between integrin localisation and the functional state of the receptors, which can be reversibly modulated either by changes in free [Ca2+], or by function modulating anti-integrin pi mAbs. [Ca2+]-induced integrin redistribution is dependent on the presence of the pi cytoplasmic domain, whereas it is independent from the presence of filamentous actin (F- actin) and focal adhesion components in this experimental system, thus implicating the uncoupling of events relevants for focal adhesion assembly under "cell-free" conditions. Moreover, reconstitution experiments show that a-actinin colocalises and redistributes with pi receptors on VPMs depleted of actin, implicating binding of a-actinin to the receptors. Finally, I found that recruitment of exogenous actin is specifically restricted to focal adhesions under conditions in which new actin polymerisation is inhibited. These data attest the value of the system for further analysis of the molecular mechanisms regulating integrin function and focal adhesions.
Holomorphic matrix models
Creators: name: Lazaroiu, C. I.
Publisher: name: arXiv
Year: 2003
Subjects: subject: High Energy Physics - Theory (hep-th)
subject: Condensed Matter (cond-mat)
subject: Quantum Algebra (math.QA)
subject: FOS: Physical sciences
subject: FOS: Mathematics

description: This is a study of holomorphic matrix models, the matrix models which underlie the conjecture of Dijkgraaf and Vafa. I first give a systematic description of the holomorphic one-matrix model. After discussing its convergence sectors, I show that certain puzzles related to its perturbative expansion admit a simple resolution in the holomorphic set-up. Constructing a `complex' microcanonical ensemble, I check that the basic requirements of the conjecture (in particular, the special geometry relations involving chemical potentials) hold in the absence of the hermicity constraint. I also show that planar solutions of the holomorphic model probe the entire moduli space of the associated algebraic curve. Finally, I give a brief discussion of holomorphic $ADE$ models, focusing on the example of the $A_2$ quiver, for which I extract explicitly the relevant Riemann surface. In this case, use of the holomorphic model is crucial, since the Hermitian approach and its attending regularization would lead to a singular algebraic curve, thus contradicting the requirements of the conjecture. In particular, I show how an appropriate regularization of the holomorphic $A_2$ model produces the desired smooth Riemann surface in the limit when the regulator is removed, and that this limit can be described as a statistical ensemble of `reduced' holomorphic models.
description: 45 pages, reference added
Studying Anisotropy of Compressible Magnetohydrodynamic Turbulence by Synchrotron Polarization Intensity
Creators: name: Wang, Ru-Yue
name: Zhang, Jian-Fu
name: Xiang, Fu-Yuan
Publisher: name: arXiv
Year: 2020
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Based on statistical analysis of synchrotron polarization intensity, we study the anisotropic properties of compressible magnetohydrodynamic (MHD) turbulence. The second-order normalized structure function, quadrupole ratio modulus and anisotropic coefficient are synergistically used to characterize the anisotropy of the polarization intensity. On the basis of pre-decomposition data cubes, we first explore the anisotropy of the polarization intensity in different turbulence regimes and find that the most significant anisotropy occurs in the sub-Alfvénic regime. Using post-decomposition data cubes in this regime, we then study the anisotropy of the polarization intensity from Alfvén, slow and fast modes. Statistics of polarization intensity from Alfvén and slow modes demonstrate the significant anisotropy while statistics of polarization intensity from fast modes show isotropic structures, which is consistent with the earlier results provided in Cho & Lazarian (2002). As a result, both quadrupole ratio modulus and anisotropic coefficient for polarization intensities can quantitatively recover the anisotropy of underlying compressible MHD turbulence. The synergistic use of the two methods helps enhance the reliability of the magnetic field measurement.
description: 13 pages with 12 Figures and 1 Table. Accepted by ApJ
Smoke on the wind: dust nucleation in archetype colliding wind pinwheel WR104
Creators: name: Soulain, A.
name: Lamberts, A.
name: Millour, F.
name: Tuthill, P.
name: Lau, R. M.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: A handful of binary Wolf-Rayet stars are known to harbour spectacular spiral structures spanning a few hundred AU. These systems host some of the highest dust production rates in the Universe and are therefore interesting candidates to address the origin of the enigmatic dust excess observed across galactic evolution. The substantial interaction between the winds of the Wolf-Rayet star and its companion constitutes a unique laboratory to study the mechanisms of dust nucleation in a hostile environment. Using the grid-based $\texttt{RAMSES}$ code, we investigate this problem by performing a 3D hydrodynamic simulation of the inner region of the prototypical spiral nebula around WR104. We then process the $\texttt{RAMSES}$ results using the radiative transfer code $\texttt{RADMC3d}$ to generate a candidate observable scene. This allows us to estimate the geometrical parameters of the shocked region. We link those quantities to the specific chemical pathway for dust nucleation, where the hydrogen-rich companion's wind catalyses dust formation. The scaling laws we derive constitute a unique tool that can be directly compared to observations. Depending on the dust nucleation locus, the velocity field reveals a differential wind speed. Thus, the initial dust speed could be more balanced between the speeds of the two stellar winds ($\sim$1600 km/s). With $\texttt{RADMC3d}$, we provide constraints on the dust nucleation radius for different combinations of dust-to-gas ratio, hydrogen enrichment and dust grain properties. Finally, our models reveal that dust may escape beyond the boundaries of the spiral due to hydrodynamical instabilities in the wind collision zone.
Accretion Flow Evolution of a New Black Hole Candidate MAXI J1348-630 During the 2019 Outburst
Creators: name: Jana, Arghajit
name: Debnath, Dipak
name: Chatterjee, Debjit
name: Chatterjee, Kaushik
name: Chakrabarti, Sandip Kumar
name: Naik, Sachindra
name: Bhowmick, Riya
name: Kumari, Neeraj
Publisher: name: arXiv
Year: 2020
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Galactic black hole candidate MAXI~J1348-630 was recently discovered by {\it MAXI} and {\it Swift}/BAT satellites during its first outburst in 2019 January which continued for $\sim4$ months. We study the spectral and timing properties of the source in detail. The combined $1-150$ keV {\it Swift}/XRT, {\it Swift}/BAT and {\it MAXI}/GSC spectra are investigated with the two component advective flow (TCAF) solution. Physical flow parameters of TCAF, such as the Keplerian disk accretion rate, the sub-Keplerian halo accretion rate, the shock location and the shock compression ratio are estimated from our spectral fits. Based on the variation of flux in soft and hard X-ray ranges, the hardness ratio, TCAF model fitted accretion rates and accretion rate ratio (ARR), we show how the sources evolved through four spectral states viz. hard, hard-intermediate, soft-intermediate and soft states in rising and declining states. Low-frequency quasi-periodic oscillations (QPO) are observed in two observations during the rising phase of the outburst. From the spectral analysis, we estimate the mass of the black hole to be $9.1^{+1.6}_{-1.2}$ $M_{\odot}$. We also find that the viscous timescale in this outburst is $\sim 3.5$ days. The distance of the source is also estimated as $5-10$ kpc from state transition luminosity.
description: 15 Pages, 6 Figures, 2 Tables (Accepted for Publication in ApJ)
A Quantum Algorithm for Dynamic Mode Decomposition Integrated with a Quantum Differential Equation Solver
Creators: name: Mizuno, Yuta
name: Komatsuzaki, Tamiki
Publisher: name: arXiv
Year: 2023
Subjects: subject: Quantum Physics (quant-ph)
subject: FOS: Physical sciences

description: We present a quantum algorithm that analyzes time series data simulated by a quantum differential equation solver. The proposed algorithm is a quantum version of the dynamic mode decomposition algorithm used in diverse fields such as fluid dynamics and epidemiology. Our quantum algorithm can also compute matrix eigenvalues and eigenvectors by analyzing the corresponding linear dynamical system. Our algorithm handles a broad range of matrices, in particular those with complex eigenvalues. The complexity of our quantum algorithm is $O(\operatorname{poly}\log N)$ for an $N$-dimensional system. This is an exponential speedup over known classical algorithms with at least $O(N)$ complexity. Thus, our quantum algorithm is expected to enable high-dimensional dynamical systems analysis and large matrix eigenvalue decomposition, intractable for classical computers.
You want me to do what? : ethical dilemmas for sign language interpreters in Canadian post-secondary education
Creators: name: West, Miriam
Publisher: name: The University of British Columbia
Year: 2011

description: Personal discussions with American Sign Language/English interpreters who work in post-secondary settings and the institutional employees who contract their services revealed discrepancies between the services interpreters typically provide and the services the institutional employees typically expect of interpreters. At the centre of this relationship are guidelines, established to assist in the provision of services for d/Deaf and hard of hearing students. While the guidelines sought to introduce standards and improve service provision, countering guidelines with the AVLIC Code of Ethics and Guidelines for Professional Conduct revealed inconsistencies that served to place interpreters in ethical dilemmas. The role of the institutional employee, responsible for contracting interpreting services, is key to students attaining not only appropriate services, but a more inclusive education. Given the current models of service delivery though, the chances of an institutional employee having the necessary knowledge, and employment status, to provide this kind of support is low. In the spirit of improving the working relationships between and among interpreters, and institutional employees, the first step is recognizing that the guidelines serve to place both at a disadvantage. Perhaps the most challenging, problems are embedded in the guidelines making it difficult for any one stakeholder to discern. With an awareness of the discrepancies, stakeholders will have the tools to better understand each other’s positions and the means to build more constructive working relationships.
YOUTH EXTENSION PROGRAMS: A JOINT BUSINESS AND LAND GRANT UNIVERSITY APPROACH
Creators: name: Riggins, Steven K.
name: Riggins, Steven K.
Publisher: name: Unknown
Year: 1978
Subjects: Teaching/Communication/Extension/Profession

description: This paper reports on a joint business-Agricultural Economics Department extension program for youth carried out by the University of Kentucky and the Kentucky Council of Cooperatives. This paper concludes that the benefits to the department easily exceed the effort required and that relevant joint programs are alive and well.
Cluster formation induced by a cloud--cloud collision in [DBS2003]179
Creators: name: Kuwahara, Sho
name: Torii, Kazufumi
name: Mizuno, Norikazu
name: Fujita, Shinji
name: Kohno, Mikito
name: Fukui, Yasuo
Publisher: name: arXiv
Year: 2019
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: [DBS2003]179 is a super star cluster in the Galaxy discovered by deep near infrared observations. We carried out CO J=1-0 and J=3-2 observations of the region of [DBS2003]179 with NANTEN2, ASTE and the Mopra 22m telescope. We identified and mapped two molecular clouds which are likely associated with the cluster. The association is evidenced by the spatial correlation with the 8 micron Spitzer image, and a high ratio of the two transitions of 12CO (J=3-2 to J=1-0). The two clouds show complementary distribution in space and bridge features connecting them in velocity. We frame a hypothesis that the two clouds collided with each other 1-2 Myr ago, and the collision compressed the interface layer, triggering the formation of the cluster. This offers an additional piece of evidence for a super star cluster formed by cloud--cloud collision alongside of the four super star clusters including Wd2, NGC3603, RCW38 and R136. The findings indicate that the known super star clusters having closely associated dust emission are formed by cloud-cloud collision, lending support for the important role of cloud--cloud collision in high-mass star formation.
description: 32 pages, 16 figures
Shocks in the outflow of the RS Oph 2021 eruption observed with X-ray gratings
Creators: name: Orio, Marina
name: Behar, Ehud
name: Luna, Juan
name: Drake, Jeremy
name: Gallagher, Jay
name: Nichols, Joy S.
name: Ness, Jan-Uwe
name: Dobrotka, Andrej
name: Mikolajewska, Joanna
name: Della Valle, Massimo
name: Ignace, Rico
name: Rahin, Roy
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: The 2021 outburst of the symbiotic recurrent nova RS Oph was observed with the Chandra High Energy Transmission Gratings (HETG) on day 18 after optical maximum and with XMM-Newton and its Reflection Grating Spectrographs (RGS) on day 21, before the supersoft X-ray source emerged and when the emission was due to shocked ejecta. The absorbed flux in the HETG 1.3-31 Angstrom range was 2.6 x 10(-10) erg/cm(-2)/s, three orders of magnitude lower than the gamma-ray flux measured on the same date. The spectra are well fitted with two components of thermal plasma in collisional ionization equilibrium, one at a temperature ~0.75 keV, and the other at temperature in the 2.5-3.4 keV range. With the RGS we measured an average flux 1.53 x 10(-10) erg/cm(-2)/s in the 5-35 Angstrom range, but the flux in the continuum and especially in the lines in the 23-35 Angstrom range decreased during the 50 ks RGS exposure by almost 10%, indicating short term variability on hours' time scale. The RGS spectrum can be fitted with three thermal components, respectively at plasma temperature between 70 and 150 eV, 0.64 keV and 2.4 keV. The post-maximum epochs of the exposures fall between those of two grating spectra observed in the 2006 eruption on days 14 and 26: they are consistent with a similar spectral evolution, but in 2021 cooling seems to have been more rapid. Iron is depleted in the ejecta with respect to solar values, while nitrogen is enhanced.
description: In press in the Astrophysical Journal
Changing jellyfish populations: Trends in large marine ecosystems
Creators: name: Brotz, Lucas
Publisher: name: Fisheries Centre. University of British Columbia
Year: 2012

description: DIRECTOR'S FORWARD. ABSTRACT. INTRODUCTION. Definition of "Jellyfish". Problem Statement. Challenges of Studying Jellyfish Populations. Impacts of Jellyfish Blooms. Invasive Species. MATERIALS AND METHODS. Large Marine Ecosystem Approach. 1950 Baseline. The Jellyfish Chronicles. Data Selection. Abundance Trend. Scoring Chronicles. Identifying Invasive Species. Fuzzy Expert System. Uncertainty. RESULTS. Effects of Invasive Species. Effects of Jellyfish Overexploitation. DISCUSSION. Defining an ‘Increase’. Species Invasions. Taxonomic Concerns. LME #1 – East Bering Sea. LME #2 – Gulf of Alaska. LME #3 – California Current. LME #4 – Gulf of California. LME #5 – Gulf of Mexico. LME #6 – Southeast U.S. Continental Shelf. LME #7 – Northeast U.S. Continental Shelf. LME #8 – Scotian Shelf. LME #9 – Newfoundland-Labrador Shelf. LME #10 – Insular Pacific-Hawaiian. LME #11 – Pacific Central-American Coastal. LME #12 – Caribbean Sea. LME #13 – Humboldt Current. LME #14 – Patagonian Shelf. LME #15 – South Brazil Shelf. LME #16 – East Brazil Shelf. LME #18 – West Greenland Shelf. LME #21 – Norwegian Sea. LME #22 – North Sea. LME #23 – Baltic Sea. LME #24 – Celtic-Biscay Shelf. LME #25 – Iberian Coastal. LME #26 – Mediterranean Sea. LME #28 – Guinea Current. LME #29 – Benguela Current. LME #30 – Agulhas Current. LME #31 – Somali Coastal Current. LME #32 – Arabian Sea. LME #34 – Bay of Bengal. LME #35 – Gulf of Thailand. LME #36 – South China Sea. LME #40 – Northeast Australian Shelf. LME #41 – East Central Australian Shelf. LME #42 – Southeast Australian Shelf. LME #47 – East China Sea. LME #48 – Yellow Sea. LME #49 – Kuroshio Current. LME #50 – Sea of Japan. LME #51 – Oyashio Current. LME #52 – Sea of Okhotsk. LME #53 – West Bering Sea. LME #60 – Faroe Plateau. LME #61 – Antarctic. LME #62 – Black Sea. LME #63 – Hudson Bay. CONCLUSIONS. REFERENCES. APPENDICES. Appendix A - Jellyfish Chronicles. Appendix B - Belief Indexes.
Urgleptes euprepes
Creators: name: Monné, Miguel A.
Publisher: name: Zenodo
Year: 2005
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Coleoptera
Cerambycidae
Urgleptes
Urgleptes euprepes

description: 23. Urgleptes euprepes (Bates, 1885)
Type locality — Mexico, Oaxaca?. (MNHN). Distribution — Mexico (Oaxaca?).
 Lepturges euprepes Bates, 1885: 404.
 Urgleptes euprepes; Gilmour, 1959d: 8; Chemsak et al., 1992: 148 (cat.); Noguera & Chemsak, 1996: 407 (cat.).
description: Published as part of Monné, Miguel A., 2005, Catalogue of the Cerambycidae (Coleoptera) of the Neotropical Region. Part II. Subfamily Lamiinae, pp. 1-760 in Zootaxa 1023 (1) on pages 1-760, DOI: 10.11646/zootaxa.946.1.1, http://zenodo.org/record/5049553
On the connection between AGN radiative feedback and massive black hole spin
Creators: name: Bollati, Francesco
name: Lupi, Alessandro
name: Dotti, Massimo
name: Haardt, Francesco
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present a novel implementation for active galactic nucleus (AGN) feedback through ultra-fast winds in the code gizmo. Our feedback recipe accounts for the angular dependence of radiative feedback upon black hole spin. We self-consistently evolve in time i) the gas accretion process from resolved scales to an unresolved AGN disc, ii) the evolution of the spin of the massive black hole (MBH), iii) the injection of AGN-driven winds into the resolved scales, and iv) the spin-induced anisotropy of the overall feedback process. We test our implementation by following the propagation of the wind-driven outflow into a homogeneous medium, and we compare the results against simple analytical models. Then, we consider an isolated galaxy setup and there we study the impact of the AGN feedback on the evolution of the MBH and the of the host galaxy. We find that: i) AGN feedback limits the gas inflow that powers the MBH, with a consequent weak impact on the host galaxy characterized by a star formation (SF) suppression of about a factor of two in the nuclear region; ii) the impact of AGN feedback on the host galaxy and on MBH growth is primarily determined by the AGN luminosity, rather than by its angular pattern set by the MBH spin; iii) the imprint of the angular pattern of the AGN radiation emission manifest in a more clear way at high accretion rates. At such high rates the more isotropic angular patterns, proper to higher spin values, sweep away gas in the nuclear region more easily, hence causing a slower MBH mass and spin growths and a higher quenching of the SF. We argue that the influence of spin-dependent anisotropy of AGN feedback on MBH and galaxy evolution is likely to be relevant in those scenarios characterized by high and prolonged MBH accretion episodes and by high AGN wind-galaxy coupling. Such conditions are more frequently met in galaxy mergers and/or high redshift galaxies.
The Stellar-mass Function of Long Gamma-Ray Burst Host Galaxies
Creators: name: Lan, Guang-Xuan
name: Wei, Jun-Jie
name: Li, Ye
name: Zeng, Hou-Dun
name: Wu, Xue-Feng
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: Long gamma-ray bursts (GRBs) have been discussed as a potential tool to probe the cosmic star formation rate (SFR) for a long time. Some studies found an enhancement in the GRB rate relative to the galaxy-inferred SFR at high redshifts, which indicates that GRBs may not be good tracers of star formation. However, in these studies, the GRB rate measured at any redshift is an average over all galaxies at that epoch. A deep understanding of the connection between GRB production and environment also needs to characterize the population of GRB host galaxies directly. Based on a complete sample of GRB hosts, we constrain the stellar-mass function (SMF) of GRB hosts, and examine redshift evolution in the GRB host population. Our results confirm that a strong redshift evolution in energy (with an evolution index of $δ=2.47^{+0.73}_{-0.89}$) or in density ($δ=1.82^{+0.22}_{-0.59}$) is needed in order to account for the observations. The GRB host SMF can be well described by the Schechter function with a power-law index $ξ\approx-1.10$ and a break mass $M_{b,0}\approx4.9\times10^{10}$ ${\rm M}_\odot$, independent of the assumed evolutionary effects. This is the first formulation of the GRB host SMF. The observed discrepancy between the GRB rate and the galaxy-inferred SFR may also be explained by an evolving SMF.
description: 9 pages, 3 figures, 2 tables. Updated to match the published version in ApJ
title: The Masses of the Neutron Stars in Cen X-3 and Vela X-1.
Creators: name: Ash, Timothy David Curtis
Publisher: name: The Open University
Year: 1999

description: This thesis deals with observations, and subsequent analysis made of the high-mass X-ray binary systems Cen X-3 and Vela X-l. By making precise radial velocity measurements of the supergiant components, and combining these results with previous X-ray data, the masses of the neutron star components can be determined. The mass of the neutron star in Cen X-3 is found to be 1.21±0.21Mo, while the mass of the neutron star in Vela X-l is found to be 1.77+0.55-0.29Mⵙ. The thesis concludes with an account of an attempt to detect radio emission from the Vela X-l bowshock.
Urgleptes franciscanus
Creators: name: Monné, Miguel A.
Publisher: name: Zenodo
Year: 2005
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Coleoptera
Cerambycidae
Urgleptes
Urgleptes franciscanus

description: 25. Urgleptes franciscanus (Melzer, 1935)
Type locality — Brazil, São Paulo: São Paulo (Jabaquara). (MZSP). Distribution — Brazil (Minas Gerais to Rio Grande do Sul).
 Lepturges franciscanus Melzer, 1935: 202; Zikán & Wygodzinsky, 1948: 57 (type); Buck, 1959: 606 (distr.).
 Urgleptes franciscanus; Gilmour, 1962a: 21; Zajciw, 1972a: 65 (distr.).
description: Published as part of Monné, Miguel A., 2005, Catalogue of the Cerambycidae (Coleoptera) of the Neotropical Region. Part II. Subfamily Lamiinae, pp. 1-760 in Zootaxa 1023 (1) on pages 1-760, DOI: 10.11646/zootaxa.946.1.1, http://zenodo.org/record/5049553
Coherent Coupling of a Diamond Tin-Vacancy Center to a Tunable Open Microcavity
Creators: name: Herrmann, Yanik
name: Fischer, Julius
name: Brevoord, Julia M.
name: Sauerzapf, Colin
name: Wienhoven, Leonardo G. C.
name: Feije, Laurens J.
name: Pasini, Matteo
name: Eschen, Martin
name: Ruf, Maximilian
name: Weaver, Matthew J.
name: Hanson, Ronald
Publisher: name: arXiv
Year: 2023
Subjects: subject: Quantum Physics (quant-ph)
subject: FOS: Physical sciences

description: Efficient coupling of optically active qubits to optical cavities is a key challenge for solid-state-based quantum optics experiments and future quantum technologies. Here we present a quantum photonic interface based on a single Tin-Vacancy center in a micrometer-thin diamond membrane coupled to a tunable open microcavity. We use the full tunability of the microcavity to selectively address individual Tin-Vacancy centers within the cavity mode volume. Purcell enhancement of the Tin-Vacancy center optical transition is evidenced both by optical excited state lifetime reduction and by optical linewidth broadening. As the emitter selectively reflects the single-photon component of the incident light, the coupled emitter-cavity system exhibits strong quantum nonlinear behavior. On resonance, we observe a transmission dip of 50 % for low incident photon number per Purcell-reduced excited state lifetime, while the dip disappears as the emitter is saturated with higher photon number. Moreover, we demonstrate that the emitter strongly modifies the photon statistics of the transmitted light by observing photon bunching. This work establishes a versatile and tunable platform for advanced quantum optics experiments and proof-of-principle demonstrations towards quantum networking with solid-state qubits.
description: 15 pages, 12 figures
Electronic and Magnetic Structure of Infinite-layer $\textrm{NdNiO}_2$: Trace of Antiferromagnetic Metal
Creators: name: Liu, Zhao
name: Ren, Zhi
name: Zhu, W.
name: Wang, Z. F.
name: Yang, Jinlong
Publisher: name: arXiv
Year: 2019
Subjects: subject: Strongly Correlated Electrons (cond-mat.str-el)
subject: FOS: Physical sciences

description: The recent discovery of Sr-doped infinite-layer nickelate $\textrm{NdNiO}_2$ [D. Li et al. Nature 572, 624 (2019)] offers an exciting platform for investigating unconventional superconductivity in nickelatebased compounds. In this work, we present a first-principles calculations for the electronic and magnetic properties of undoped parent $\textrm{NdNiO}_2$. Intriguingly, we found that: 1) the paramagnetic phase has complex Fermi pockets with 3D characters near the Fermi level; 2) by including electronelectron interactions, 3d-electrons of Ni tend to form $(π, π, π)$ antiferromagnetic ordering at low temperatures; 3) with moderate interaction strength, 5d-electrons of Nd contribute small Fermi pockets that could weaken the magnetic order akin to the self-doping effect. Our results provide a plausible interpretation for the experimentally observed resistivity minimum and Hall coefficient drop. Moreover, we elucidate that antiferromagnetic ordering in $\textrm{NdNiO}_2$ is relatively weak, arising from the small exchange coupling between 3d-electrons of Niand also hybridization with 5d-electrons of Nd.
description: 7 pages, 5 figures
The resonance perturbations of the (39991) Iochroma family
Creators: name: Rosaev, Alexey
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: The dynamics of a very young compact asteroid cluster associated with asteroid 39991 Iochroma is studied. It is shown that Iochroma family lies between the two three body resonances 3J-1M-3 and 5J 3S-2. In this paper we have determined the position of these resonances and the boundary between them. We have included the orbital elements approximations which may be useful in the future study of the dynamics of the family. Additionally, we report on a new candidate member, namely asteroid 2016 UT3.
description: 14 pages, 6 figures
IS PRODUCTION FOR MARKET WINDOWS A VIABLE ALTERNATIVE FOR LIMITED RESOURCE FARMERS
Creators: name: Collette, Ardea
name: Wall, G. Brian
name: Collette, Ardea
name: Wall, G. Brian
Publisher: name: Unknown
Year: 1978
Subjects: subject: Farm Management
subject: Marketing
subject: FOS: Economics and business

description: Fresh-market vegetable production has been advocated as a means of improving incomes of small farmers in northern Florida and southern Georgia. The role ~f price variability, price flexibility and income elasticities in improving price expectations and evaluating crop selection is discussed. These concepts are applied to the analysis of poten- _tial "market windows" for area growers.
COMMUNICATION WITH SMALL FARM OPERATORS
Creators: name: Colette, Arden W.
name: Colette, Arden W.
Publisher: name: Unknown
Year: 1978
Subjects: subject: Farm Management
subject: Small Farm
subject: Communication
subject: Attitudes

description: Change in· small farm operations will not be achieved without communication. Communication will·. be · successful only if primary consideration is given to the characteristics ., attitudes and needs of the target audience. The content of the message and how it is perceived by the target audience is critical to the success of the program. Innovations should be simple, compatable with existing enterprises, and have a relative advantage over current pract;i.ces. Interpersonal channels of communication are the most effective in achieving adoption of new ideas. The more the change agent is oriented towa:r:d the target audience the more successful the program.
A note on a straight gravity tunnel through a rotating body
Creators: name: Simonič, Aleksander
Publisher: name: arXiv
Year: 2020
Subjects: subject: Popular Physics (physics.pop-ph)
subject: FOS: Physical sciences

description: It is well-known that the straight gravity tunnel between any two different positions on a non-rotating Earth, which has uniform density, is traversable, i.e., an object initially at rest will reach its destination through the gravity tunnel in both directions. Moreover, the time taken to fall is always constant. These facts are no longer true if rotation is allowed. The aim of this note is to derive the necessary and sufficient condition for traversability of straight gravity tunnels through a rotating physical body with spherically symmetric gravitational field. Fall-through times are expressed in a closed form for linear and constant gravitational fields. In conclusion, these models are compared to numerically obtained data using the internal structure of the Earth.
Constraints on Dark Matter from Dynamical Heating of Stars in Ultrafaint Dwarfs. Part 1: MACHOs and Primordial Black Holes
Creators: name: Graham, Peter W.
name: Ramani, Harikrishnan
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: High Energy Physics - Theory (hep-th)
subject: FOS: Physical sciences

description: We place limits on dark matter made up of compact objects significantly heavier than a solar mass, such as MACHOs or primordial black holes (PBHs). In galaxies, the gas of such objects is generally hotter than the gas of stars and will thus heat the gas of stars even through purely gravitational interactions. Ultrafaint dwarf galaxies (UFDs) maximize this effect. Observations of the half-light radius in UFDs thus place limits on MACHO dark matter. We build upon previous constraints with an improved heating rate calculation including both direct and tidal heating, and consideration of the heavier mass range above $10^4 \, M_\odot$. Additionally we find that MACHOs may lose energy and migrate in to the center of the UFD, increasing the heat transfer to the stars. UFDs can constrain MACHO dark matter with masses between about $10 M_\odot$ and $10^8 M_\odot$ and these are the strongest constraints over most of this range.
description: 19 Pages, 6 Figures
Urgleptes freudei Gilmour 1959
Creators: name: Monné, Miguel A.
Publisher: name: Zenodo
Year: 2005
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Coleoptera
Cerambycidae
Urgleptes
Urgleptes freudei

description: 26. Urgleptes freudei Gilmour, 1959
Type locality — Brazil. (ZSMC). Distribution — Brazil.
 Urgleptes freudei Gilmour, 1959d: 8, fig. 4.
description: Published as part of Monné, Miguel A., 2005, Catalogue of the Cerambycidae (Coleoptera) of the Neotropical Region. Part II. Subfamily Lamiinae, pp. 1-760 in Zootaxa 1023 (1) on pages 1-760, DOI: 10.11646/zootaxa.946.1.1, http://zenodo.org/record/5049553
Variable star classification with a Multiple-Input Neural Network
Creators: name: Szklenár, T.
name: Bódi, A.
name: Tarczay-Nehéz, D.
name: Vida, K.
name: Mező, Gy.
name: Szabó, R.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: In this experiment, we created a Multiple-Input Neural Network, consisting of Convolutional and Multi-layer Neural Networks. With this setup the selected highest-performing neural network was able to distinguish variable stars based on the visual characteristics of their light curves, while taking also into account additional numerical information (e.g. period, reddening-free brightness) to differentiate visually similar light curves. The network was trained and tested on OGLE-III data using all OGLE-III observation fields, phase-folded light curves and period data. The neural network yielded accuracies of 89--99\% for most of the main classes (Cepheids, $δ$ Scutis, eclipsing binaries, RR Lyrae stars, Type-II Cepheids), only the first-overtone Anomalous Cepheids had an accuracy of 45\%. To counteract the large confusion between the first-overtone Anomalous Cepheids and the RRab stars we added the reddening-free brightness as a new input and only stars from the LMC field were retained to have a fixed distance. With this change we improved the neural network's result for the first-overtone Anomalous Cepheids to almost 80\%. Overall, the Multiple-input Neural Network method developed by our team is a promising alternative to existing classification methods.