cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Gas selection for Xe-based LCP-GEM detectors onboard the CubeSat X-ray observatory NinjaSat
Creators: name: Takeda, T.
name: Tamagawa, T.
name: Enoto, T.
name: Kitaguchi, T.
name: Kato, Y.
name: Mihara, T.
name: Iwakiri, W.
name: Numazawa, M.
name: Zhou, Y.
name: Uchiyama, K.
name: Yoshida, Y.
name: Ota, N.
name: Hayashi, S.
name: Watanabe, S.
name: Jujo, A.
name: Sato, H.
name: Hu, C. P.
name: Takahashi, H.
name: Odaka, H.
name: Tamba, T.
name: Taniguchi, K.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: High Energy Physics - Experiment (hep-ex)
subject: FOS: Physical sciences

description: We present a gas selection for Xe-based gas electron multiplier (GEM) detectors, Gas Multiplier Counters (GMCs) onboard the CubeSat X-ray observatory NinjaSat. To achieve an energy bandpass of 2-50 keV, we decided to use a Xe-based gas mixture at a pressure of 1.2 atm that is sensitive to high-energy X-rays. In addition, an effective gain of over 300 is required for a single GEM so that the 2 keV X-ray signal can be sufficiently larger than the electrical noise. At first, we measured the effective gains of GEM in nine Xe-based gas mixtures (combinations of Xe, Ar, CO2, CH4, and dimethyl ether; DME) at 1.0 atm. The highest gains were obtained with Xe/Ar/DME mixtures, while relatively lower gains were obtained with Xe/Ar/CO2, Xe/Ar/CH4, and Xe+quencher mixtures. Based on these results, we selected the Xe/Ar/DME (75%/24%/1%) mixture at 1.2 atm as the sealed gas for GMC. Then we investigated the dependence of an effective gain on the electric fields in the drift and induction gaps ranging from 100-650 V cm$^{-1}$ and 500-5000 V cm$^{-1}$, respectively, in the selected gas mixture. The effective gain weakly depended on the drift field while it was almost linearly proportional to the induction field: 2.4 times higher at 5000 V cm$^{-1}$ than at 1000 V cm$^{-1}$. With the optimal induction and drift fields, the flight model GMC achieves an effective gain of 460 with an applied GEM voltage of 590 V.
description: 7th international conference on Micro Pattern Gaseous Detectors 2022 - MPGD2022, 3 pages, 2 figures
Chandra & HST Imaging of the Quasars PKS B0106+013 & 3C345: Inverse Compton X-rays and Magnetized Jets
Creators: name: Kharb, Preeti
name: Lister, Matthew
name: Marshall, Herman
name: Hogan, Brandon
Publisher: name: arXiv
Year: 2012
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We present results from deep (70 ks) Chandra ACIS observations and Hubble Space Telescope ACS F475W observations of two highly optically polarized quasars belonging to the MOJAVE blazar sample, viz., PKS B0106+013 and 1641+399 (3C345). These observations reveal X-ray and optical emission from the jets in both sources. X-ray emission is detected from the entire length of the 0106+013 radio jet, which shows clear bends or wiggles - the X-ray emission is brightest at the first prominent kpc jet bend. A picture of a helical kpc jet with the first kpc-scale bend representing a jet segment moving close(r) to our line of sight, and getting Doppler boosted at both radio and X-ray frequencies, is consistent with these observations. The X-ray emission from the jet end however peaks at about 0.4" (~3.4 kpc) upstream of the radio hot spot. Optical emission is detected both at the X-ray jet termination peak and at the radio hot spot. The X-ray jet termination peak is found upstream of the radio hot spot by around 0.2" (~1.3 kpc) in the short projected jet of 3C345. HST optical emission is seen in an arc-like structure coincident with the bright radio hot spot, which we propose is a sharp (apparent) jet bend instead of a terminal point, that crosses our line of sight and consequently has a higher Doppler beaming factor. A weak radio hot spot is indeed observed less than 1" downstream of the bright radio hot spot, but has no optical or X-ray counterpart. By making use of the pc-scale radio and the kpc-scale radio/X-ray data, we derive constraints on the jet Lorentz factors (Gamma_jet) and inclination angles (theta): for a constant jet speed from pc- to kpc-scales, we obtain a Gamma_jet of ~70 for 0106+013, and ~40 for 3C345. On relaxing this assumption, we derive a Gamma_jet of ~2.5 for both the sources. Upper limits on theta of ~13 degrees are obtained for the two quasars. (ABRIDGED)
description: 46 pages, 11 figures, Accepted for publication in ApJ
Graceful exit from inflation and reheating with twin waterfalls
Creators: name: Lee, Hyun Min
name: Menkara, Adriana
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: FOS: Physical sciences

description: We study the hybrid inflation with a pseudo-Nambu-Goldstone boson inflaton and two waterfall scalar fields. The $Z_2$ symmetry for the waterfall fields keeps inflaton potential flat against quantum corrections coming from the waterfall couplings, and it is broken spontaneously in the vacuum without a domain wall problem within the Hubble horizon of our universe. We show that the $Z_2$ invariant Higgs portal couplings to the waterfall fields are responsible for the reheating process, leading to a sufficiently large reheating temperature after inflation. In the presence of an extra $Z'_2$ symmetry, one of the waterfall fields or another singlet scalar field becomes a dark matter candidate. In particular, we find that preheating is sufficient to account for the correct relic density of the waterfall dark matter.
description: 26 pages, 5 figures. arXiv admin note: text overlap with arXiv:2206.05523
Mineralogy and petrology of Quaternary lavas, Snake River plain, Idaho and the cation distribution in natural titanomagnetites
Creators: name: Stout, M. Z.
Publisher: name: University of Calgary
Year: 1975
Subjects: subject: QE 363.2 S74 1975 Microfiche
subject: Mineralogy
subject: Petrology
subject: Geology - Idaho - Snake River

description: Bibliography: p. 137-143.
Large-Scale Atomistic Simulations of Environmental Effects on the Formation and Properties of Molecular Junctions
Creators: name: French, William R.
name: Iacovella, Christopher R.
name: Cummings, Peter T.
Publisher: name: arXiv
Year: 2012
Subjects: subject: Mesoscale and Nanoscale Physics (cond-mat.mes-hall)
subject: Materials Science (cond-mat.mtrl-sci)
subject: FOS: Physical sciences

description: Using an updated simulation tool, we examine molecular junctions comprised of benzene-1,4-dithiolate bonded between gold nanotips, focusing on the importance of environmental factors and inter-electrode distance on the formation and structure of bridged molecules. We investigate the complex relationship between monolayer density and tip separation, finding that the formation of multi-molecule junctions is favored at low monolayer density, while single-molecule junctions are favored at high density. We demonstrate that tip geometry and monolayer interactions, two factors that are often neglected in simulation, affect the bonding geometry and tilt angle of bridged molecules. We further show that the structures of bridged molecules at 298 and 77 K are similar.
description: To appear in ACS Nano, 30 pages, 5 figures
title: Die Gegenwelt des Erfundenen
title: Fiktionale Texte als Medium biblischer Verheißung
Creators: name: Kutzer, Mirja
Publisher: name: Universität Kassel
Year: 2006
Subjects: subject: 220
subject: Katholische Theologie
subject: Bibelarbeit
subject: Erzähltheorie

description: Dieser Artikel greift eine Sinnlinie der umfassenderen Untersuchung der Verfasserin zum erkenntnistheoretischen Wert von Dichtung für theologisches Denken auf: Mirja Kutzer, In Wahrheit erfunden. Dichtung als Ort theologischer Erkenntnis (ratio fidei 30), Regensburg 2006.
Spectral theory of elliptic differential operators with indefinite weights
Creators: name: Behrndt, Jussi
Publisher: name: arXiv
Year: 2011
Subjects: subject: Spectral Theory (math.SP)
subject: FOS: Mathematics

description: The spectral properties of a class of non-selfadjoint second order elliptic operators with indefinite weight functions on unbounded domains $Ω$ are investigated. It is shown that under an abstract regularity assumption the nonreal spectrum of the associated elliptic operator in $L^2(Ω)$ is bounded. In the special case that $Ω=R^n $decomposes into subdomains $Ω_+$ and $Ω_-$ with smooth compact boundaries and the weight function is positive on $Ω_+$ and negative on $Ω_-$, it turns out that the nonreal spectrum consists only of normal eigenvalues which can be characterized with a Dirichlet-to-Neumann map.
description: to appear in Proc. Roy. Soc. Edinburgh Sect. A
Mineralogy and petrology of some granite rocks in the Canadian Shield north of Fort Chipewyan, Alberta
Creators: name: Klewchuk, P.
Publisher: name: University of Calgary
Year: 1972
Subjects: subject: QE 462 G7 K54 1972
subject: Granite
subject: Petrology - Alberta - Fort Chipewyan
subject: Mineralogy - Alberta - Fort Chipewyan

description: Bibliography: p. 126-134.
The progenitors of Type Ia supernovae with asymptotic giant branch donors
Creators: name: Li, Luhan
name: Liu, Dongdong
name: Wang, Bo
Publisher: name: arXiv
Year: 2023
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Type Ia supernovae (SNe Ia) are among the most energetic events in the Universe. They are excellent cosmological distance indicators due to the remarkable homogeneity of their light curves. However, the nature of the progenitors of SNe Ia is still not well understood. In the single-degenerate model, a carbon-oxygen white dwarf (CO WD) could grow its mass by accreting material from an asymptotic giant branch (AGB) star, leading to the formation of SNe Ia when the mass of the WD approaches to the Chandrasekhar-mass limit, known as the AGB donor channel. In this channel, previous studies mainly concentrate on the wind-accretion pathway for the mass-increase of the WDs. In the present work, we employed an integrated mass-transfer prescription for the semidetached WD+AGB systems, and evolved a number of WD+AGB systems for the formation of SNe Ia through the Roche-lobe overflow process or the wind-accretion process. We provided the initial and final parameter spaces of WD+AGB systems for producing SNe Ia. We also obtained the density distribution of circumstellar matter at the moment when the WD mass reaches the Chandrasekhar-mass limit. Moreover, we found that the massive WD+AGB sample AT 2019qyl can be covered by the final parameter space for producing SNe Ia, indicating that AT 2019qyl is a strong progenitor candidate of SNe Ia with AGB donors.
description: 12 pages, 5 figures, accepted for publication in Res. Astron. Astrophys
Centers and homotopy centers in enriched monoidal categories
Creators: name: Batanin, M.
name: Markl, M.
Publisher: name: arXiv
Year: 2011
Subjects: subject: Algebraic Topology (math.AT)
subject: Category Theory (math.CT)
subject: FOS: Mathematics
subject: Primary 18D10, 18D20, 18D50, secondary 55U40, 55P48

description: We consider a theory of centers and homotopy centers of monoids in monoidal categories which themselves are enriched in duoidal categories. Duoidal categories (introduced by Aguillar and Mahajan under the name 2-monoidal categories) are categories with two monoidal structures which are related by some, not necessary invertible, coherence morphisms. Centers of monoids in this sense include many examples which are not `classical.' In particular, the 2-category of categories is an example of a center in our sense. Examples of homotopy center (analogue of the classical Hochschild complex) include the Gray-category Gray of 2-categories, 2-functors and pseudonatural transformations and Tamarkin's homotopy 2-category of dg-categories, dg-functors and coherent dg-transformations.
description: 52 pages
Star formation in the dwarf Seyfert galaxy NGC 4395: Evidence for both AGN and SNe feedback?
Creators: name: Nandi, Payel
name: Stalin, C. S.
name: Saikia, D. J.
name: Muneer, S.
name: Mountrichas, George
name: Wylezalek, Dominika
name: Sagar, R.
name: Kissler-Patig, Markus
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present a detailed multi-wavelength study of star formation in the dwarf galaxy NGC 4395 which hosts an active galactic nucleus (AGN). From our observations with the Ultra-Violet Imaging Telescope, we have compiled a catalogue of 284 star forming (SF) regions, out of which we could detect 120 SF regions in H$α$ observations. Across the entire galaxy, we found the extinction corrected star formation rate (SFR) in the far ultra-violet (FUV) to range from 2.0 $\times$ 10$^{-5}$ M$_\odot$yr$^{-1}$ to 1.5 $\times$ 10$^{-2}$ M$_\odot$yr$^{-1}$ with a median of 3.0 $\times$ 10$^{-4}$ M$_\odot$yr$^{-1}$ and age to lie in the range of $\sim$ 1 to 98 Myr with a median of 14 Myr. In H$α$ we found the SFR to range from 7.2 $\times$ 10$^{-6}$ M$_\odot$yr$^{-1}$ to 2.7 $\times$ 10$^{-2}$ M$_\odot$yr$^{-1}$ with a median of 1.7 $\times$ 10$^{-4}$ M$_\odot$yr$^{-1}$ and age to lie between 3 to 6 Myr with a median of 5 Myr. The stellar ages derived from H$α$ show a gradual decline with galactocentric distance. We found three SF regions close to the center of NGC~4395 with high SFR both from H$α$ and UV which could be attributed to feedback effects from the AGN. We also found six other SF regions in one of the spiral arms having higher SFR. These are very close to supernovae remnants which could have enhanced the SFR locally. We obtained a specific SFR (SFR per unit mass) for the whole galaxy 4.64 $\times$ 10$^{-10}$ yr$^{-1}$.
description: 10 pages, 11 figures, Accepted for publication in ApJ
Design of a "Digital Atlas Vme Electronics" (DAVE) Module
Creators: name: Goodrick, Maurice
name: Robinson, Dave
name: Shaw, Rick
name: Postranecky, Martin
name: Warren, Matthew
Publisher: name: arXiv
Year: 2011
Subjects: subject: Instrumentation and Detectors (physics.ins-det)
subject: High Energy Physics - Experiment (hep-ex)
subject: FOS: Physical sciences

description: ATLAS-SCT has developed a new ATLAS trigger card, 'Digital Atlas Vme Electronics' ("DAVE"). The unit is designed to provide a versatile array of interface and logic resources, including a large FPGA. It interfaces to both VME bus and USB hosts. DAVE aims to provide exact ATLAS CTP (ATLAS Central Trigger Processor) functionality, with random trigger, simple and complex deadtime, ECR (Event Counter Reset), BCR (Bunch Counter Reset) etc. being generated to give exactly the same conditions in standalone running as experienced in combined runs. DAVE provides additional hardware and a large amount of free firmware resource to allow users to add or change functionality. The combination of the large number of individually programmable inputs and outputs in various formats, with very large external RAM and other components all connected to the FPGA, also makes DAVE a powerful and versatile FPGA utility card
description: 8 pages, 4 figures, TWEPP-2011; E-mail: mp@hep.ucl.ac.uk
Detecting and Characterizing Young Quasars. III. The Impact of Gravitational Lensing Magnification
Creators: name: Yue, Minghao
name: Eilers, Anna-Christina
name: Simcoe, Robert A.
name: Belli, Sirio
name: Davies, Frederick B.
name: DePalma, David
name: Hennawi, Joseph F.
name: Mason, Charlotte A.
name: Muñoz, Julian B.
name: Nelson, Erica J.
name: Tacchella, Sandro
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We test the impact of gravitational lensing on the lifetime estimates of seven high-redshift quasars at redshift $z\gtrsim6$. The targeted quasars are identified by their small observed proximity zone sizes, which indicate extremely short quasar lifetimes $(t_Q\lesssim10^5 \text{ yrs})$. However, these estimates of quasar lifetimes rely on the assumption that the observed luminosities of the quasars are intrinsic and not magnified by gravitational lensing, which would bias the lifetime estimates towards younger ages. In order to test possible effects of gravitational lensing, we obtain high-resolution images of the seven quasars with the {\em Hubble Space Telescope (HST)} and look for signs of strong lensing. We do not find any evidence of strong lensing, i.e., all quasars are well-described by point sources, and no foreground lensing galaxy is detected. We estimate that the strong lensing probabilities for these quasars are extremely small $(\sim1.4\times10^{-5})$, and show that weak lensing changes the estimated quasar lifetimes by only $\lesssim0.2$ dex. We thus confirm that the short lifetimes of these quasars are intrinsic. The existence of young quasars indicates a high obscured fraction, radiatively inefficient accretion, and/or flickering light curves for high-redshift quasars. We further discuss the impact of lensing magnification on measurements of black hole masses and Eddington ratios of quasars.
description: 14 pages, 4 figures, 3 tables. Accepted by the Astrophysical Journal
Graphene Transistor as a Probe for Streaming Potential
Creators: name: Newaz, A. K. M.
name: Markov, D. A.
name: Prasai, D.
name: Bolotin, K. I.
Publisher: name: arXiv
Year: 2012
Subjects: subject: Mesoscale and Nanoscale Physics (cond-mat.mes-hall)
subject: FOS: Physical sciences

description: We explore the dependence of electrical transport in a graphene field effect transistor (GraFET) on the flow of the liquid within the immediate vicinity of that transistor. We find large and reproducible shifts in the charge neutrality point of GraFETs that are dependent on the fluid velocity and the ionic concentration. We show that these shifts are consistent with the variation of the local electrochemical potential of the liquid next to graphene that are caused by the fluid flow (streaming potential). Furthermore, we utilize the sensitivity of electrical transport in GraFETs to the parameters of the fluid flow to demonstrate graphene-based mass flow and ionic concentration sensing. We successfully detect a flow as small as~70nL/min, and detect a change in the ionic concentration as small as ~40nM.
description: 6 pages, 4 figures
Internal kinematics and structure of the bulge globular cluster NGC 6569
Creators: name: Pallanca, Cristina
name: Leanza, Silvia
name: Ferraro, Francesco R.
name: Lanzoni, Barbara
name: Dalessandro, Emanuele
name: Cadelano, Mario
name: Vesperini, Enrico
name: Origlia, Livia
name: Mucciarelli, Alessio
name: Valenti, Elena
name: Miola, Andrea
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: In the context of a project aimed at characterizing the properties of star clusters in the Galactic bulge, here we present the determination of the internal kinematics and structure of the massive globular cluster NGC 6569. The kinematics has been studied by means of an unprecedented spectroscopic dataset acquired in the context of the ESO-VLT Multi-Instrument Kinematic Survey (MIKiS) of Galactic globular clusters, combining the observations from four different spectrographs. We measured the line-of-sight velocity of a sample of almost 1300 stars distributed between ~0.8" and 770" from the cluster center. From a sub-sample of high-quality measures, we determined the velocity dispersion profile of the system over its entire radial extension (from ~ 5" to ~ 200" from the center), finding the characteristic behavior usually observed in globular clusters, with a constant inner plateau and a declining trend at larger radii. The projected density profile of the cluster has been obtained from resolved star counts, by combining high-resolution photometric data in the center, and the Gaia EDR3 catalog radially extended out to ~20' for a proper sampling of the Galactic field background. The two profiles are properly reproduced by the same King model, from which we estimated updated values of the central velocity dispersion, main structural parameters (such as the King concentration, the core, half-mass, and tidal radii), total mass, and relaxation times. Our analysis also reveals a hint of ordered rotation in an intermediate region of the cluster (40"
description: Accepted for publication in The Astrophysical Journal; 21 pages, 10 figures, 4 tables
Community response to the Alaska native claims settlement act : Seldovia, Alaska
Creators: name: Reed, Carolyn Elizabeth
Publisher: name: University of Calgary
Year: 1979
Subjects: subject: E 93 R42 1979 Microfiche
subject: Indians of North America - Alaska - Legal status, Laws, etc.
subject: Indians of North America - Alaska - Claims
subject: Indians of North America - Alaska - Land transfer
subject: Indians of North America - Social conditions
subject: Indians of North America - Economic conditions

description: Bibliography: p. 101-105.
Giant planet engulfment by evolved giant stars: light curves, asteroseismology, and survivability
Creators: name: O'Connor, Christopher E.
name: Bildsten, Lars
name: Cantiello, Matteo
name: Lai, Dong
Publisher: name: arXiv
Year: 2023
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: About ten percent of Sun-like ($1$-$2 M_\odot$) stars will engulf a $1$-$10 M_{\rm J}$ planet as they expand during the red giant branch (RGB) or asymptotic giant branch (AGB) phase of their evolution. Once engulfed, these planets experience a strong drag force in the star's convective envelope and spiral inward, depositing energy and angular momentum. For these mass ratios, the inspiral takes $\sim 10$-$10^{2}$ years ($\sim 10^{2}$-$10^{3}$ orbits); the planet undergoes tidal disruption at a radius of $\sim R_\odot$. We use the Modules for Experiments in Stellar Astrophysics (MESA) software instrument to track the stellar response to the energy deposition while simultaneously evolving the planetary orbit. For RGB stars, as well as AGB stars with $M_{\rm p} \lesssim 5 M_{\rm J}$ planets, the star responds quasistatically but still brightens measurably on a timescale of years. In addition, asteroseismic indicators, such as the frequency spacing or rotational splitting, differ before and after engulfment. For AGB stars, engulfment of a $M_{\rm p} \gtrsim 5 M_{\rm J}$ planet drives supersonic expansion of the envelope, causing a bright, red, dusty eruption similar to a "luminous red nova." Based on the peak luminosity, color, duration, and expected rate of these events, we suggest that engulfment events on the AGB could be a significant fraction of low-luminosity red novae in the Galaxy. We do not find conditions where the envelope is ejected prior to the planet's tidal disruption, complicating the interpretation of short-period giant planets orbiting white dwarfs as survivors of common-envelope evolution.
description: 24 pages, 11 figures, 1 table. Accepted to ApJ
Net-proton probability distribution in heavy ion collisions
Creators: name: Braun-Munzinger, P.
name: Friman, B.
name: Karsch, F.
name: Redlich, K.
name: Skokov, V.
Publisher: name: arXiv
Year: 2011
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: FOS: Physical sciences

description: We compute net-proton probability distributions in heavy ion collisions within the hadron resonance gas model. The model results are compared with data taken by the STAR Collaboration in Au-Au collisions at sqrt(s_{NN})= 200 GeV for different centralities. We show that in peripheral Au-Au collisions the measured distributions, and the resulting first four moments of net-proton fluctuations, are consistent with results obtained from the hadron resonance gas model. However, data taken in central Au-Au collisions differ from the predictions of the model. The observed deviations can not be attributed to uncertainties in model parameters. We discuss possible interpretations of the observed deviations.
description: 4 pages, 2 figures
Identification and Characterization of a Large Sample of Distant Active Dwarf Galaxies in XMM-SERVS
Creators: name: Zou, Fan
name: Brandt, W. N.
name: Ni, Qingling
name: Zhu, Shifu
name: Alexander, David M.
name: Bauer, Franz E.
name: Chen, Chien-Ting J.
name: Luo, Bin
name: Sun, Mouyuan
name: Vignali, Cristian
name: Vito, Fabio
name: Xue, Yongquan
name: Yan, Wei
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Active dwarf galaxies are important because they contribute to the evolution of dwarf galaxies and can reveal their hosted massive black holes. However, the sample size of such sources beyond the local universe is still highly limited. In this work, we search for active dwarf galaxies in the recently completed XMM-Spitzer Extragalactic Representative Volume Survey (XMM-SERVS). XMM-SERVS is currently the largest medium-depth X-ray survey covering 13 $\mathrm{deg}^2$ in three extragalactic fields, which all have well-characterized multi-wavelength information. After considering several factors that may lead to misidentifications, we identify 73 active dwarf galaxies at $z<1$, which constitutes the currently largest X-ray-selected sample beyond the local universe. Our sources are generally less obscured than predictions based on the massive-AGN (active galactic nucleus) X-ray luminosity function and have a low radio-excess fraction. We find that our sources reside in similar environments to inactive dwarf galaxies. We further quantify the accretion distribution of the dwarf-galaxy population after considering various selection effects and find that it decreases with X-ray luminosity, but redshift evolution cannot be statistically confirmed. Depending upon how we define an AGN, the active fraction may or may not show a strong dependence on stellar mass. Their Eddington ratios and X-ray bolometric corrections significantly deviate from the expected relation, which is likely caused by several large underlying systematic biases when estimating the relevant parameters for dwarf galaxies. Throughout this work, we also highlight problems in reliably measuring photometric redshifts and overcoming strong selection effects for distant active dwarf galaxies.
description: 34 pages, 21 figures, 6 tables, accepted for publication in ApJ
Digital power measurement
Creators: name: Hriskevich, Brian (Robert Brian James)
Publisher: name: University of Calgary
Year: 1978
Subjects: subject: TK 275 H73 1978 Microfiche
subject: Power plants - Measurement
subject: Electronic digital processing - Power-plants
subject: Analog-to-digital converters
subject: Electric filters - Noise

description: Bibliography: p. 104-105.
Muons in EASs with $E_0 = 10^{19}$ eV according to data of the Yakutsk Array
Creators: name: Glushkov, A. V.
name: Lebedev, K. G.
name: Sabourov, A. V.
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: Lateral distribution functions of particles in extensive air showers with the energy $E_0 \simeq 10^{19}$ eV recorded by ground-based and underground scintillation detectors with a threshold of $E_μ \simeq 1.0 \times \secθ$ GeV at the Yakutsk array during the continuous observations from 1986 to 2016 have been analyzed using events with zenith angles $θ\le 60^{\circ}$ functions have been compared to the predictions obtained with the QGSJet01 hadron interaction model by applying the CORSIKA code. The entire dataset indicates that cosmic rays consist predominantly of protons.
description: 11 pages, 5 figures, 2 tables. Accepted for publication in JETP Letters (v.117, no.4, 2023), minor typos fixed
Two-fingered grasp planning for randomized bin-picking : determining the best pick
Creators: name: Dupuis, Donna C.
Publisher: name: University of British Columbia
Year: 2009

description: For many years, the manufacturing industry has pursued a commercially viable, vision-guided, robotic bin-picking system. The goal of such a system is to select a target part and a corresponding grasp from a pile of jumbled parts. Strategic planning of this selection to reduce the risk of a failed grasp attempt would increase the system's reliability, and, thus, its commercial viability, and is the focus of this thesis. Specifically, this work aims to find the best pick; namely, the best combination of a target part and corresponding grasp. The primary contribution of this work is a novel method for generating many high-quality, rated, pick options for a given vision-guided robotic bin-picking cycle, enabling the selection of the best pick. The method is tailored for a two-fingered (antipodal) gripper, typically used in industry; however, it may be extended to other gripper types (i.e., three-fingered). The method is broken down into two stages: (1) offline generation of many high-quality, two-fingered grasps for a given part, and (2) online evaluation of these grasps in the context of the pile to determine a collision-free set of rated picks, and, ultimately, the most desirable pick. In evaluating grasps online, the effect of gripper finger clearance is considered to further minimize the risk of collision when executing the selected pick. Subsidiary contributions of this work include: (1) an automatic grasp-generation method to sample the space of all two-fingered grasps for the target part, (2) a metric function for evaluating grasps, and (3) a measure of the robustness of a grasp. The proposed method for pick selection is validated using stereo data of a real pile of parts. We compare the use of a small set of nominal grasps for pick selection (an approach typical in industry) to the use of an extensive evaluated grasp set generated using the proposed method. Our experimental results show that, in the majority of cases, the use of our method results in more valid and higher quality picks.
Amplitudes for the analysis of the decay $J/ψ\to K^{+} K^{-} π^0$
Creators: name: Guo, Peng
name: Mitchell, Ryan
name: Shepherd, Matthew
name: Szczepaniak, Adam P.
Publisher: name: arXiv
Year: 2011
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: High Energy Physics - Experiment (hep-ex)
subject: FOS: Physical sciences

description: We construct an analytical model for two channel, two-body scattering amplitudes, and then apply it in the description of the three-body $J/ψ\to K^+K^-π^0$ decay. In the construction of the partial wave amplitudes, we combine the low energy resonance region with the Regge asymptotic behavior determined from direct two-body production. We find that resonance production in the $Kπ$ channel in $J/ψ$ decays seems to differ from that observed in direct $Kπ$ production, while the mass distribution in the $K\bar K$ channel may be compatible.
Multifractal Height Cross-Correlation Analysis: A New Method for Analyzing Long-Range Cross-Correlations
Creators: name: Kristoufek, Ladislav
Publisher: name: arXiv
Year: 2012
Subjects: subject: Statistical Finance (q-fin.ST)
subject: Data Analysis, Statistics and Probability (physics.data-an)
subject: FOS: Economics and business
subject: FOS: Physical sciences

description: We introduce a new method for detection of long-range cross-correlations and multifractality - multifractal height cross-correlation analysis (MF-HXA) - based on scaling of qth order covariances. MF-HXA is a bivariate generalization of the height-height correlation analysis of Barabasi & Vicsek [Barabasi, A.L., Vicsek, T.: Multifractality of self-affine fractals, Physical Review A 44(4), 1991]. The method can be used to analyze long-range cross-correlations and multifractality between two simultaneously recorded series. We illustrate a power of the method on both simulated and real-world time series.
description: 6 pages, 4 figures
Radiative Neutron Capture on Carbon-14 in Effective Field Theory
Creators: name: Rupak, Gautam
name: Fernando, Lakma
name: Vaghani, Akshay
Publisher: name: arXiv
Year: 2012
Subjects: subject: Nuclear Theory (nucl-th)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Nuclear Experiment (nucl-ex)
subject: FOS: Physical sciences

description: The cross section for radiative capture of neutron on carbon-14 is calculated using the model-independent formalism of halo effective field theory. The dominant contribution from E1 transition is considered, and the cross section is expressed in terms of elastic scattering parameters of the effective range expansion. Contributions from both resonant and non-resonant interaction are calculated. Significant interference between these leads to a capture contribution that deviates from simple Breit-Wigner resonance form.
description: 14 pages, 6 figures
Workshop On Digital Image Processing Of Spm(Afm,Sem) Data Using Imagej And Gwyddion
Creators: name: Jany, Benedykt R.
Publisher: name: Zenodo
Year: 2016
Subjects: Digital Image Processing
Workshop
SPM
SEM
AFM

description: Workshop on Digital Image Processing of SPM(AFM,SEM) data using ImageJ and Gwyddion

Marian Smoluchowski Institute of Physics Jagiellonian University Krakow Poland 12.05.2016

Organized by Dr Benedykt R. Jany

Examples and Exercises

The free software could be downloaded from:

ImageJ/FIJI

http://fiji.sc/

Gwyddion

http://gwyddion.net/

LibreOffice

https://www.libreoffice.org/
The AMBRE Project: r-process elements in the Milky Way thin and thick discs
Creators: name: Guiglion, G.
name: De Laverny, P.
name: Recio-Blanco, A.
name: Prantzos, N.
Publisher: name: Les Ulis : EDP Sciences
Year: 2018
Subjects: subject: Galaxy: abundances
subject: Galaxy: stellar content
subject: Methods: data analysis
subject: Stars: abundances
subject: 520

description: Context. The chemical evolution of neutron capture elements in the Milky Way disc is still a matter of debate. There is a lack of statistically significant catalogues of such element abundances, especially those of the r-process. Aims. We aim to understand the chemical evolution of r-process elements in Milky Way disc. We focus on three pure r-process elements Eu, Gd, and Dy. We also consider a pure s-process element, Ba, in order to disentangle the different nucleosynthesis processes. Methods. We take advantage of high-resolution FEROS, HARPS, and UVES spectra from the ESO archive in order to perform a homogeneous analysis on 6500 FGK Milky Way stars. The chemical analysis is performed thanks to the automatic optimization pipeline GAUGUIN. We present abundances of Ba (5057 stars), Eu (6268 stars), Gd (5431 stars), and Dy (5479 stars). Based on the [α/Fe] ratio determined previously by the AMBRE Project, we chemically characterize the thin and the thick discs, and a metal-rich α-rich population. Results. First, we find that the [Eu/Fe] ratio follows a continuous sequence from the thin disc to the thick disc as a function of the metallicity. Second, in thick disc stars, the [Eu/Ba] ratio is found to be constant, while the [Gd/Ba] and [Dy/Ba] ratios decrease as a function of the metallicity. These observations clearly indicate a different nucleosynthesis history in the thick disc between Eu and Gd-Dy. The [r/Fe] ratio in the thin disc is roughly around +0.1 dex at solar metallicity, which is not the case for Ba. We also find that the α-rich metal-rich stars are also enriched in r-process elements (like thick disc stars), but their [Ba/Fe] is very different from thick disc stars. Finally, we find that the [r/α] ratio tends to decrease with metallicity, indicating that supernovae of different properties probably contribute differently to the synthesis of r-process elements and α-elements. Conclusions. We provide average abundance trends for [Ba/Fe] and [Eu/Fe] with rather small dispersions, and for the first time for [Gd/Fe] and [Dy/Fe]. This data may help to constrain chemical evolution models of Milky Way r- and s-process elements and the yields of massive stars. We emphasize that including yields of neutron-star or black hole mergers is now crucial if we want to quantitatively compare observations to Galactic chemical evolution models.
Gemini Near Infrared Spectrograph -- Distant Quasar Survey: Augmented Spectroscopic Catalog and a Prescription for Correcting UV-Based Quasar Redshifts
Creators: name: Matthews, Brandon M.
name: Dix, Cooper
name: Shemmer, Ohad
name: Brotherton, Michael S.
name: Myers, Adam D.
name: Andruchow, I.
name: Brandt, W. N.
name: Gallagher, S. C.
name: Green, Richard
name: Lira, Paulina
name: McLane, Jacob N.
name: Plotkin, Richard M.
name: Richards, Gordon T.
name: Runnoe, Jessie C.
name: Schneider, Donald P.
name: Strauss, Michael A.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Quasars at $z~{\gtrsim}~1$ most often have redshifts measured from rest-frame ultraviolet emission lines. One of the most common such lines, C IV $λ1549$, shows blueshifts up to ${\approx}~5000~\rm{km~s^{-1}}$, and in rare cases even higher. This blueshifting results in highly uncertain redshifts when compared to redshift determinations from rest-frame optical emission lines, e.g., from the narrow [O III] $λ5007$ feature. We present spectroscopic measurements for 260 sources at $1.55~{\lesssim}~z~{\lesssim}~3.50$ having $-28.0~{\lesssim}~M_i~{\lesssim}~-30.0$ mag from the Gemini Near Infrared Spectrograph - Distant Quasar Survey (GNIRS-DQS) catalog, augmenting the previous iteration which contained 226 of the 260 sources whose measurements are improved upon in this work. We obtain reliable systemic redshifts based on [O III] $λ5007$ for a subset of 121 sources which we use to calibrate prescriptions for correcting UV-based redshifts. These prescriptions are based on a regression analysis involving C IV full-width-at-half-maximum intensity and equivalent width, along with the UV continuum luminosity at a rest-frame wavelength of 1350 A. Applying these corrections can improve the accuracy and the precision in the C IV-based redshift by up to ${\sim}~850~\rm{km~s^{-1}}$ and ${\sim}~150~\rm{km~s^{-1}}$, respectively, which correspond to ${\sim}~8.5$ Mpc and ${\sim}~1.5$ Mpc in comoving distance at $z~=~2.5$. Our prescriptions also improve the accuracy of the best available multi-feature redshift determination algorithm by ${\sim}~100~\rm{km~s^{-1}}$, indicating that the spectroscopic properties of the C IV emission line can provide robust redshift estimates for high-redshift quasars. We discuss the prospects of our prescriptions for cosmological and quasar studies utilizing upcoming large spectroscopic surveys.
description: 20 pages (AASTeX 6.3.1), 8 figures, accepted for publication in ApJ
Exact Solutions v.s. Perturbative Calculations of Finite $Φ^{3}$-$Φ^{4}$ Hybrid-Matrix-Model
Creators: name: Kanomata, Naoyuki
name: Sako, Akifumi
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Physics - Theory (hep-th)
subject: FOS: Physical sciences
subject: 81T32, 81T75

description: There is a matrix model corresponding to a scalar field theory called Grosse-Wulkenhaar model, which is renormalizable by adding a harmonic oscillator potential to scalar $Φ^{4}$ theory on Moyal spaces. There are more unknowns in $Φ^{4}$ matrix model than in $Φ^{3}$ matrix model, for example, in terms of integrability. We then construct a one-matrix model ($Φ^{3}$-$Φ^{4}$ Hybrid-Matrix-Model) with multiple potentials, which is a combination of a $3$-point interaction and a $4$-point interaction, where the $3$-point interaction of $Φ^{3}$ is multiplied by some positive definite diagonal matrix $M$. This model is solvable due to the effect of this $M$. In particular, the connected $\displaystyle\sum_{i=1}^{B}N_{i}$-point function $G_{|a_{N_{1}}^{1}\cdots a_{N_{1}}^{1}|\cdots|a_{1}^{B}\cdots a_{N_{B}}^{B}|}$ of $Φ^{3}$-$Φ^{4}$ Hybrid-Matrix-Model is studied in detail. This $\displaystyle\sum_{i=1}^{B}N_{i}$-point function can be interpreted geometrically and corresponds to the sum over all Feynman diagrams (ribbon graphs) drawn on Riemann surfaces with $B$ boundaries (punctures). Each $|a_{1}^{i}\cdots a_{N_{i}}^{i}|$ represents $N_{i}$ external lines coming from the $i$-th boundary (puncture) in each Feynman diagram. First, we construct Feynman rules for $Φ^{3}$-$Φ^{4}$ Hybrid-Matrix-Model and calculate perturbative expansions of some multipoint functions in ordinary methods. Second, we calculate the path integral of the partition function $\mathcal{Z}[J]$ and use the result to compute exact solutions for $1$-point function $G_{|a|}$ with $1$-boundary, $2$-point function $G_{|ab|}$ with $1$-boundary, $2$-point function $G_{|a|b|}$ with $2$-boundaries, and $n$-point function $G_{|a^{1}|a^{2}|\cdots|a^{n}|}$ with $n$-boundaries. They include contributions from Feynman diagrams corresponding to nonplanar Feynman diagrams or higher genus surfaces.
description: 28 pages. Typos were corrected, three references were added, and an annotation was added in Section 3
Optical color of Type Ib and Ic supernovae and implications for their progenitors
Creators: name: Jin, Harim
name: Yoon, Sung-Chul
name: Blinnikov, Sergei
Publisher: name: arXiv
Year: 2023
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Type Ib and Ic supernovae (SNe Ib/Ic) originate from hydrogen-deficient massive star progenitors, of which the exact properties are still much debated. Using the SN data in the literature, we investigate the optical $B-V$ color of SNe Ib/Ic at the $V-$band peak and show that SNe Ib are systematically bluer than SNe Ic. We construct SN models from helium-rich and helium-poor progenitors of various masses using the radiation hydrodynamics code STELLA and discuss how the $B-V$ color at the $V-$band peak is affected by $^{56}$Ni to ejecta mass ratios, $^{56}$Ni mixing and presence/absence of the helium envelope. We argue that the dichotomy in the amounts of helium in the progenitors plays the primary role in making the observed systematic color difference at the optical peak, in favor of the most commonly invoked SN scenario that SNe Ib and SNe Ic progenitors are helium-rich and helium-poor, respectively.
description: Accepted for publication in ApJ. 16 pages
The spin-down accretion regime of Galactic ultra-luminous X-ray pulsar Swift J0243.6+6124
Creators: name: Liu, Jiren
name: Ji, Long
name: Ge, MIngyu
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: The relative high fluxes of the Galactic ultra-luminous X-ray pulsar Swift J0243 allow a detailed study of its spin-down regime in quiescence state, for a first time. After the 2017 giant outburst, its spin frequencies show a linear decreasing trend with some variations due to minor outbursts. The linear spin-down rate is $\sim-1.9\times10^{-12}$ Hz/s during the period of lowest luminosity, from which one can infer a dipole field $\sim1.75\times10^{13}$ G. The $\dotν-L$ relation during the spin-down regime is complex, and the $\dotν$ is close to 0 when the luminosity reaches both the high end ($L_{38}\sim0.3$) and the lowest value ($L_{38}\sim0.03$). The luminosity of zero-torque is different for the giant outburst and other minor outbursts. It is likely due to different accretion flows for different types of outburst, as evidenced by the differences of the spectra and pulse profiles at a similar luminosity for different types of outburst (giant or not). The pulse profile changes from double peaks in the spin-up state to a single broad peak in the low spin-down regime, indicating the emission beam/region is larger in the low spin-down regime. These results show that accretion is still ongoing in the low spin-down regime for which the neutron star is supposed to be in a propeller state.
description: 7 pages, 7 figs, to appear in ApJ, comments welcome
Properties of the dense cores and filamentary structures in the Vela C molecular cloud
Creators: name: Li, Xue-Mei
name: Zhang, Guo-Yin
name: Men'shchikov, Alexander
name: Li, Jin-Zeng
name: Zhang, Chang
name: Wu, Zhong-Zu
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: The initial and boundary conditions of the Galactic star formation in molecular clouds are not well understood. In an effort to shed new light on this long-standing problem, we measured properties of dense cores and filamentary structures in the Vela C molecular cloud, observed with Herschel. We applied the getsf extraction method to separate the components of sources and filaments from each other and their backgrounds, before detecting, measuring, and cataloging the structures. The cores and filamentary structures constitute 40% of the total mass of Vela C, most of the material is in the low-density molecular background cloud. We selected 570 reliable cores, of which 149 are the protostellar cores and 421 are the starless cores. Almost 78% of the starless cores were identified with the gravitationally bound prestellar cores. The exponent of the CMF (alpha = 1.35) is identical to that of the Salpeter IMF. We selected 68 filaments with at least one side that appeared not blended with adjacent structures. The filament widths are in the range of 0.15 pc to 0.63 pc, and have a median value of W = 0.3(0.11) pc. The surface densities of filaments are well correlated with their contrasts and linear densities. Within uncertainties of the filament instability criterion, many filaments may well be both supercritical and subcritical. A large fraction of filaments may definitely be considered supercritical, in which are found 94 prestellar cores, 83 protostellar cores, and only 1 unbound starless core. Taking into account the uncertainties, the supercritical filaments contain only prestellar and protostellar cores. Our findings support the idea that there exists a direct relationship between the CMF and IMF and that filaments play a key role in the formation of prestellar cores, which is consistent with the previous Herschel results.
description: 15 pages, 12 figures, 3 tables, accepted for publication in A&A
The Changing pattern of the Canada-West Indies trade, 1966-1976
Creators: name: Hendrickson, Maurice Augustus
Publisher: name: University of Calgary
Year: 1978
Subjects: subject: HF 3228 W4 H44 1978 Microfiche
subject: Canada - Commerce - West Indies, British
subject: West Indies, British - Commerce - Canada

description: Bibliography: p. 185-192.