cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Observed relationships between driver and passenger restraint use in the front and rear seats
Creators: name: Kufera, Joseph A.
name: Auman, Kimberly M.
name: Chavez, Alicia
name: Kerns, Timothy J.
name: Burch, Cynthia
name: Vesselinov, Roumen
Publisher: name: Taylor & Francis
Year: 2022
Subjects: subject: 59999 Environmental Sciences not elsewhere classified
subject: FOS: Earth and related environmental sciences
subject: 69999 Biological Sciences not elsewhere classified
subject: FOS: Biological sciences
subject: Science Policy

description: Seat belt usage has increased substantially since the 1960s, yet driver use continues to affect passenger usage. Recent observational restraint use findings for Maryland will examine the relationship between driver and passenger usage, including adults and children in the rear seat. Analyses were based on observational front and rear seat studies administered in parallel from 2016 to 2019. A statistically rigorous front seat project yielded weighted results among drivers and outboard passengers. A study of adults and children in the rear seat was based on a convenience sample of vehicles. Restraint usage results were presented as frequencies and proportions among occupants with known belt use, along with the 95% confidence interval for overall rates. Overall restraint usage rates averaged 90.9% in the front seat study and 81.1% in the rear seat sample. In vehicles with two front seat occupants and a belted driver, the proportion of belted passengers averaged 93.0% over four years. However, among unbelted drivers, only 41.6% of passengers were belted on average. In the rear seat study, an average of 82.7% were belted in vehicles driven by a restrained driver, differing for children (92.0%) versus adults (70.4%). Analysis of vehicles with an unbelted driver revealed an average of 45.0% of belted rear seat occupants, with a considerable difference for children (65.0%) compared with adults (21.0%). Observational seat belt studies in Maryland in recent years have shown that, despite overall rates above 80%, passenger use in both the front and rear seats is associated with driver restraint use.
Quantifying Properties of Photospheric Magnetic Cancellations in the Quiet Sun Internetwork
Creators: name: Ledvina, Vincent E.
name: Kazachenko, Maria D.
name: Criscuoli, Serena
name: Tilipman, Dennis
name: Ermolli, Ilaria
name: Falco, Mariachiara
name: Guglielmino, Salvatore
name: Jafarzadeh, Shahin
name: van der Voort, Luc Rouppe
name: Zuccarello, Francesca
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: We analyzed spectropolarimetric data from the Swedish 1-meter Solar Telescope to investigate physical properties of small-scale magnetic cancellations in the quiet Sun photosphere. Specifically, we looked at the full Stokes polarization profiles along the Fe I 557.6 nm and of the Fe I 630.1 nm lines measured by CRisp Imaging SpectroPolarimeter (CRISP) to study temporal evolution of the line-of-sight (LOS) magnetic field during 42.5 minutes of quiet Sun evolution. From this magnetogram sequence, we visually identified 38 cancellation events. We then used Yet Another Feature Tracking Algorithm (YAFTA) to characterize physical properties of these magnetic cancellations. We found on average $1.6\times10^{16}$ Mx of magnetic flux cancelled in each event with an average cancellation rate of $3.8\times10^{14}$ Mx s$^{-1}$. The derived cancelled flux is associated with strong downflows, with an average speed of $V_\mathrm{LOS}\approx1.1$ km s$^{-1}$. Our results show that the average lifetime of each event is $9.2$ minutes with an average $44.8\%$ of initial magnetic flux being cancelled. Our estimates of magnetic fluxes provide a lower limit since studied magnetic cancellation events have magnetic field values that are very close to the instrument noise level. We observed no horizontal magnetic fields at the cancellation sites and therefore can not conclude whether the events are associated structures that could cause magnetic reconnection.
description: 19 pages, 18 figures, 2 tables, accepted into ApJ on 06/08/2022
Evaluation of an education intervention for Australian health practitioners to support people with dementia with driving decisions: A pretest-posttest survey
Creators: name: Veerhuis, Nadine
name: Traynor, Victoria
Publisher: name: Taylor & Francis
Year: 2022
Subjects: subject: Medicine
subject: Neuroscience
subject: Sociology
subject: FOS: Sociology
subject: Science Policy

description: Drivers with dementia will at some stage need to stop driving. The timing of driving retirement is informed by the advice of health practitioners, however many find this task complex and challenging as they feel unprepared or lack confidence, having limited training and education on dementia and driving. Few opportunities exist for Australian health practitioners to advance learning about dementia and driving. This study evaluated the impact of a Dementia and Driving Education Module on practitioner self-perceived knowledge, confidence, and competence in supporting people living with dementia with decisions about driving. A single group, pretest-posttest survey was conducted for this study. Health practitioners were recruited over 19 months via email and invited to attend a face-to-face dementia and driving workshop. The workshop comprised of a two-hour Dementia and Driving Education Module including seven learning activities incorporating six vignettes, five self-reflections, one case study and a paper copy of a dementia and driving decision aid. Participants completed a survey prior to, immediately after and six weeks post completion of the education module. A total of 240 health practitioners, from over six disciplines, took part in one of eleven workshops delivered via face-to-face and online across five states of Australia. Significant increases occurred in all outcome measures of perceived knowledge, confidence and competence between baseline and immediately post-education module survey responses and between baseline and six weeks post-survey responses. The Dementia and Driving Education Module and accompanying decision aid demonstrate an efficacious solution for a diverse range of health practitioners to enhance their knowledge, confidence, and competence in supporting people living with dementia with driving retirement decisions.
การตรวจสอบคุณภาพของฝรั่งตัดแต่งพร้อมบริโภคพันธุ์กิมจูในบรรจุภัณฑ์ โดยใช้ฟิล์มไคโตซานอัจฉริยะที่ผสมเอเอ็มพีและแอนโทไซยานิน
Creators: name: จุฑาทิพย์ โพธิ์อุบล
Publisher: name: คณะศิลปศาสตร์และวิทยาศาสตร์ มหาวิทยาลัยเกษตรศาสตร์ วิทยาเขตกำแพง
Year: 2024
Subjects: ไคโตซาน
อะมิโนเมทิลโพรพานอล
แอนโทไซยานิน
ฝรั่ง

description: ศวท: ศิลปศาสตร์ วิทยาศาสตร์และเทคโนโลยี, 1, 1, 23-35
title: Image quality evaluation for FIB‐SEM images
Creators: name: Roldán, Diego
name: Redenbach, Claudia
name: Schladitz, Katja
name: Kübel, Christian
name: Schlabach, Sabine
Publisher: name: Wiley-Blackwell
Year: 2024

description: Focused ion beam scanning electron microscopy (FIB‐SEM) tomography is a serial sectioning technique where an FIB mills off slices from the material sample that is being analysed. After every slicing, an SEM image is taken showing the newly exposed layer of the sample. By combining all slices in a stack, a 3D image of the material is generated. However, specific artefacts caused by the imaging technique distort the images, hampering the morphological analysis of the structure. Typical quality problems in microscopy imaging are noise and lack of contrast or focus. Moreover, specific artefacts are caused by the FIB milling, namely, curtaining and charging artefacts. We propose quality indices for the evaluation of the quality of FIB‐SEM data sets. The indices are validated on real and experimental data of different structures and materials.
Evolution of a Relativistic Outflow and X-ray Corona in the Extreme Changing-Look AGN 1ES 1927+654
Creators: name: Masterson, Megan
name: Kara, Erin
name: Ricci, Claudio
name: García, Javier A.
name: Fabian, Andrew C.
name: Pinto, Ciro
name: Kosec, Peter
name: Remillard, Ronald A.
name: Loewenstein, Michael
name: Trakhtenbrot, Benny
name: Arcavi, Iair
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: 1ES 1927+654 is a paradigm-defying AGN and one of the most peculiar X-ray nuclear transients. In early 2018, this well-known AGN underwent a changing-look event, in which broad optical emission lines appeared and the optical flux increased. Yet, by July 2018, the X-ray flux had dropped by over two orders of magnitude, indicating a dramatic change to the inner accretion flow. With three years of observations with NICER, XMM-Newton, and NuSTAR, we present the X-ray evolution of 1ES 1927+654, which can be broken into three phases-(1) an early super-Eddington phase with rapid variability in X-ray luminosity and spectral parameters, (2) a stable super-Eddington phase at the peak X-ray luminosity, and (3) a steady decline back to the pre-outburst luminosity and spectral parameters. For the first time, we witnessed the formation of the X-ray corona, as the X-ray spectrum transitioned from thermally-dominated to primarily Comptonized. We also track the evolution of the prominent, broad 1 keV feature in the early X-ray spectra and show that this feature can be modeled with blueshifted reflection (z = -0.33) from a single-temperature blackbody irradiating spectrum using xillverTDE, a new flavor of the xillver models. Thus, we propose that the 1 keV feature could arise from reflected emission off the base of an optically thick outflow from a geometrically thick, super-Eddington inner accretion flow, connecting the inner accretion flow with outflows launched during extreme accretion events (e.g. tidal disruption events). Lastly, we compare 1ES 1927+654 to other nuclear transients and discuss applications of xillverTDE to super-Eddington accretors.
description: 25 pages, 10 figures, accepted for publication in ApJ
การศึกษาความเชื่อในสังคมไทยและความเชื่อมั่นในตนเอง ที่มีอิทธิพลต่อความสำเร็จในงานของพนักงาน บริษัทผู้ผลิตและจัดจำหน่ายชิ้นส่วนอิเล็กทรอนิกส์แห่งหนึ่งในจังหวัดปทุมธานี
Creators: name: ณัฐธิดา วงษ์สุข
Publisher: name: คณะศิลปศาสตร์และวิทยาศาสตร์ มหาวิทยาลัยเกษตรศาสตร์ วิทยาเขตกำแพง
Year: 2024
Subjects: ความเชื่อในสังคมไทย
ฮวงจุ้ย
วัตถุมงคล
ความเชื่อมั่นในตนเอง
ความสำเร็จในงาน

description: ศวท: ศิลปศาสตร์ วิทยาศาสตร์และเทคโนโลยี, 1, 1, 36-51
Evidence to Action (E2A) Framework: A Participatory Approach to Action Learning - Summary Guide
Creators: name: Butcher, Stephanie
name: Das, Joyati
name: Dam, Jennifer
name: Fattah, Kazi
name: Hausmann, Susanna
Publisher: name: University of Melbourne
Year: 2021
Subjects: Urban and regional economics

description: This is a Summary Guide to the Evidence to Action Framework developed by the Connected Cities Laboratory at the University of Melbourne and funded by Fondation Botnar.
Evidence to Action (E2A) Framework: A Participatory Approach to Action Learning - Summary Guide
Creators: name: Dam, Jennifer
name: Butcher, Stephanie
name: Fattah, Kazi
name: Hausmann, Susanna
name: Das, Joyati
Publisher: name: University of Melbourne
Year: 2021
Subjects: Urban and regional economics

description: This is a Summary Guide to the Evidence to Action Framework developed by the Connected Cities Laboratory at the University of Melbourne and funded by Fondation Botnar.
Single Pulse Variability in Gamma-ray Pulsars
Creators: name: Kerr, Matthew
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: The Fermi Large Area Telescope receives $\ll$1 photon per rotation from any $γ$-ray pulsar. However, out of the billions of monitored rotations of the bright pulsars Vela (PSR~J0835$-$4510) and Geminga (PSR~J0633$+$1746), a few thousand have $\geq$2 pulsed photons. These rare pairs encode information about the variability of pulse amplitude and shape. We have cataloged such pairs and find the observed number to be in good agreement with simple Poisson statistics, limiting any amplitude variations to $<$19% (Vela) and $<$22% (Geminga) at 2$σ$ confidence. Using an array of basis functions to model pulse shape variability, the observed pulse phase distribution of the pairs limits the scale of pulse shape variations of Vela to $<$13% while for Geminga we find a hint of $\sim$20% single-pulse shape variability most associated with the pulse peaks. If variations last longer than a single rotation, more pairs can be collected, and we have calculated upper limits on amplitude and shape variations for assumed coherence times up to 100 rotations, finding limits of $\sim$1% (amplitude) and $\sim$3% (shape) for both pulsars. Because a large volume of the pulsar magnetosphere contributes to $γ$-ray pulse production, we conclude that the magnetospheres of these two energetic pulsars are stable over one rotation and very stable on longer time scales. All other $γ$-ray pulsars are too faint for similar analyses. These results provide useful constraints on rapidly-improving simulations of pulsar magnetospheres, which have revealed a variety of large-scale instabilities in the thin equatorial current sheets where the bulk of GeV $γ$-ray emission is thought to originate.
description: 12 pages, accepted in ApJ
Is Fermi 1544-0649 a misaligned blazar? discovering the jet structure with VLBI
Creators: name: Shao, Chengyu
name: Cheng, Xiaopeng
name: Thomas, Tam Pak-Hin
name: Yang, Lili
name: Cui, Yudong
name: Pal, Partha Sarathi
name: Zhang, Zhongli
name: Sohn, Bong Won
name: Sugiyama, Koichiro
name: Chen, Wen
name: Hao, Longfei
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: Fermi J1544-0649 is a transient GeV source first detected during its GeV flares in 2017. Multi-wavelength observations during the flaring time demonstrate variability and spectral energy distribution(SED) that are typical of a blazar. Other than the flare time, Fermi J1544-0649 is quiet in the GeV band and looks rather like a quiet galaxy (2MASX J15441967-0649156) for a decade. Together with the broad absorption lines feature we further explore the "misaligned blazar scenario". We analyzed the Very Long Baseline Array (VLBA) and East Asian VLBI Network (EAVN) data from 2018 to 2020 and discovered the four jet components from Fermi J1544-0649. We found a viewing angle around 3.7° to 7.4°. The lower limit of the viewing angle indicates a blazar with an extremely low duty cycle of the gamma-ray emission, the upper limit of it supports the "misaligned blazar scenario". Follow-up multi-wavelength observations after 2018 show Fermi J1544-0649 remains quiet in GeV, X-ray, and optical bands. Multi-messenger search of neutrinos is also performed, and an excess of 3.1 σ significance is found for this source.
description: Accepted for publication in ApJ. 13 pages, 7 figures
A candle in the wind: a radio filament in the core of the A3562 galaxy cluster
Creators: name: Giacintucci, S.
name: Venturi, T.
name: Markevitch, M.
name: Bourdin, H.
name: Mazzotta, P.
name: Merluzzi, P.
name: Dallacasa, D.
name: Bardelli, S.
name: Sikhosana, S. P.
name: Smirnov, O.
name: Bernardi, G.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Using a MeerKAT observation of the galaxy cluster A3562 (a member of the Shapley Supercluster), we have discovered a narrow, long and straight, very faint radio filament, which branches out at a straight angle from the tail of a radio galaxy located in projection near the core of the cluster. The radio filament spans 200 kpc and aligns with a sloshing cold front seen in the X-rays, staying inside the front in projection. The radio spectral index along the filament appears uniform (within large uncertainties) at $α\simeq -1.5$. We propose that the radio galaxy is located outside the cold front, but dips its tail under the front. The tangential wind that blows there may stretch the radio plasma from the radio galaxy into a filamentary structure. Some reacceleration is needed in this scenario to maintain the radio spectrum uniform. Alternatively, the cosmic ray electrons from that spot in the tail can spread along the cluster magnetic field lines, straightened by that same tangential flow, via anomalously fast diffusion. Our radio filament can provide constraints on this process. We also uncover a compact radio source at the Brightest Cluster Galaxy (BCG) that is 2--3 orders of magnitude less luminous than those in typical cluster central galaxies -- probably an example of a BCG starved of accretion fuel by gas sloshing.
description: 25 pages, 12 figures, accepted for publication in ApJ
Survival of Plant Growth Promoting Rhizobacteria (PGPR)
Creators: name: Yadav, Anurag
name: Yadav, Kusum
Publisher: name: figshare
Year: 2022
Subjects: subject: Microbiology
subject: FOS: Biological sciences

description: The plant growth promoting rhizobacteria (PGPR) are a group of bacteria that enhance plant growth by varied mechanisms. These bacteria colonize plant roots and deliver plant growth promoting effect in rhizosphere; therefore used as biofertilizers or biopesticides. Considering their beneficial effects the concept of rhizosphere tailoring is in agriculture practice from several decades. Bioinoculants introduced in the field face the survival threat due to several reasons. Therefore, their growth study is imperative for crop improvement. Better survival of PGPR in soil requires selection of appropriate bioinoculant strain, a good understanding of soil and rhizosphere bacterial population dynamics. Since the survival of rhizobacteria in the environment is regulated by physical, chemical and biological stresses, therefore, the use of environmentally adaptive strains has been advocated. Non-cultural counterpart of the soil microorganisms also plays a vital role in shaping the PGPR population dynamics that also influence culturable PGPRs. Bioinoculant survival has been further augmented by using appropriate carrier material and by using composite inoculation of two and more ecologically distinct strains.
The Lyman Alpha Reference Sample XIII: High-Angular Resolution 21cm HI observations of Ly$α$ emitting galaxies
Creators: name: Reste, A. Le
name: Hayes, M.
name: Cannon, J. M.
name: Herenz, E. C.
name: Melinder, J.
name: Menacho, V.
name: Östlin, G.
name: Puschnig, J.
name: Rivera-Thorsen, T. E.
name: Kunth, D.
name: Velikonja, N.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: The Ly$α$ emission line is one of the main observables of galaxies at high redshift, but its output depends strongly on the neutral gas distribution and kinematics around the star-forming regions where UV photons are produced. We present observations of Ly$α$ and 21-cm HI emission at comparable scales with the goal to qualitatively investigate how the neutral interstellar medium (ISM) properties impact Ly$α$ transfer in galaxies. We have observed 21-cm HI at the highest angular resolution possible (~ 3" beam) with the VLA in two local galaxies from the Lyman Alpha Reference Sample. We contrast this data with HST Ly$α$ imaging and spectroscopy, and MUSE and PMAS ionized gas observations. In LARS08, high intensity Ly$α$ emission is co-spatial with high column density HI where dust content is the lowest. The Ly$α$ line is strongly redshifted, consistent with velocity redistribution which allows Ly$α$ escape from high column density neutral medium with low dust content. In eLARS01, high intensity Ly$α$ emission is located in regions of low column density HI, below the HI data sensitivity limit ($<2\times10^{20}\,$cm$^{-2}$). The perturbed ISM distribution with low column density gas in front of the Ly$α$ emission region plays an important role in the escape. In both galaxies, the faint Ly$α$ emission ($\sim 1\times10^{-16}$erg.s$^{-1}$cm$^{-2}$arcsec$^{-2}$) traces intermediate H$α$ emission regions where HI is found, regardless of the dust content. Dust seems to modulate, but not prevent, the formation of a faint Ly$α$ halo. This study suggests the existence of scaling relations between dust, H$α$, HI, and Ly$α$ emission in galaxies.
description: 28 pages, 14 figures, accepted for publication in ApJ
Dust Grain Growth & Dusty Supernovae in Low-Metallicity Molecular Clouds
Creators: name: Martínez-González, Sergio
name: Wünsch, Richard
name: Tenorio-Tagle, Guillermo
name: Silich, Sergiy
name: Szécsi, Dorottya
name: Palouš, Jan
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present 3-D hydrodynamical models of the evolution of superbubbles powered by stellar winds and supernovae from young coeval massive star clusters within low metallicity ($Z = 0.02$Z$_{\odot}$), clumpy molecular clouds. We explore the initial stages of the superbubble evolution, including the occurrence of pair-instability and core-collapse supernovae. Our aim is to study the occurrence of dust grain growth within orbiting dusty clumps, and in the superbubble's swept-up supershell. We also aim to address the survival of dust grains produced by sequential supernovae. The model accounts for the star cluster gravitational potential and self-gravity of the parent cloud. It also considers radiative cooling (including that induced by dust) and a state-of-the-art population synthesis model for the coeval cluster. As shown before, a superbubble embedded into a clumpy medium becomes highly distorted, expanding mostly due to the hot gas streaming through low density channels. Our results indicate that in the case of massive ($\sim10^7$M$_{\odot}$) molecular clouds, hosting a super star cluster ($\sim5.6\times10^5$M$_{\odot}$), grain growth increments the dust mass at a rate $\sim4.8\times10^{-5}$M$_{\odot}$ yr$^{-1}$ during the first $2.5$Myr of the superbubble's evolution, while the net contribution of pair-instability and core-collapse supernovae to the superbubble's dust budget is $\sim1200$M$_{\odot} (M_{SC}/5.6\times10^{5}$M$_{\odot})$, where $M_{SC}$ is the stellar mass of the starburst. Therefore, dust grain growth and dust injection by supernovae lead to create, without invoking a top-heavy initial mass function, massive amounts of dust within low-metallicity star-forming molecular clouds, in accordance with the large dust mass present in galaxies soon after the onset of cosmic reionization.
description: 8 pages, 4 figures. Accepted for publication in The Astrophysical Journal
Risk Factors of Non-specific Low Back Pain in a Rural Community of Bangladesh (extended data)
Creators: name: Md. Abu Shahin
name: Rijwan Bhuiyan
name: Rowsan Ara
name: Md. Nazrul Islam
name: Minhaj Rahim Choudhury
name: Haq, Syed Atiqul
name: Zaman, Mohammad Mostafa
Publisher: name: Zenodo
Year: 2022

description: Risk Factors of Non-specific Low Back Pain in a Rural Community of Bangladesh (extended data) Questionnaires used to collect data (Bangla and English)
ปัจจัยที่มีอิทธิพลต่อการตัดสินใจซื้อเครื่องดื่มทางเลือกเพื่อสุขภาพและความงาม
Creators: name: ไข่มุกด์ วิกรัยศักดา
Publisher: name: คณะศิลปศาสตร์และวิทยาศาสตร์ มหาวิทยาลัยเกษตรศาสตร์ วิทยาเขตกำแพง
Year: 2024
Subjects: เครื่องดื่มทางเลือกเพื่อสุขภาพและความงาม
การตัดสินใจซื้อ
ส่วนประสมทางการตลาด
ผู้บริโภค

description: ศวท: ศิลปศาสตร์ วิทยาศาสตร์และเทคโนโลยี, 1, 1, 52-65
ปัจจัยที่มีผลต่อการเลือกรับชมสื่อออนไลน์บนแพลตฟอร์มยูทูบในประเทศไทย กรณีศึกษา นักแคสเกมและวีทูบเบอร์
Creators: name: ชิดชนก สิทธิคงศักดิ์
Publisher: name: คณะศิลปศาสตร์และวิทยาศาสตร์ มหาวิทยาลัยเกษตรศาสตร์ วิทยาเขตกำแพง
Year: 2024
Subjects: การเลือกรับชมสื่อออนไลน์
พฤติกรรมการใช้สื่อ
แพลตฟอร์มยูทูบ นักแคสเกม
วีทูบเบอร์

description: ศวท: ศิลปศาสตร์ วิทยาศาสตร์และเทคโนโลยี, 1, 1, 66-86
New theoretical Period-Luminosity-Metallicity relations for RR Lyrae in the Rubin-LSST filters
Creators: name: Marconi, Marcella
name: Molinaro, Roberto
name: Dall'Ora, Massimo
name: Ripepi, Vincenzo
name: Musella, Ilaria
name: Bono, Giuseppe
name: Braga, Vittorio
name: Di Criscienzo, Marcella
name: Fiorentino, Giuliana
name: Leccia, Silvio
name: Monelli, Matteo
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: The revolutionary power of future Rubin-LSST observations will allow us to significantly improve the physics of pulsating stars, including RR Lyrae. In this context, an updated theoretical scenario predicting all the relevant pulsation observables in the corresponding photometric filters is mandatory. The bolometric light curves based on a recently computed extensive set of nonlinear convective pulsation models for RR Lyrae stars, covering a broad range in metal content and transformed into the Rubin-LSST photometric system. Predicted Rubin-LSST mean magnitudes and pulsation amplitudes have been adopted to built the Bailey diagrams (luminosity amplitude vs period) and the color-color diagrams in these bands. The current findings indicate that the gLSST-rLSST, rLSST-iLSST colors obey to a well defined linear relation with the metal content. Moreover, the Period Luminosity relations display in the reddest filters (rLSST,iLSST,zLSST,yLSST) a significant dependence on the assumed metal abundance. In particular, more metal-rich RR Lyrae are predicted to be fainter at fixed period. Metal-dependent Period-Wesenheit relations for different combinations of optical and NIR filters are also provided. These represent powerful tools to infer individual distances independently of reddening uncertainties, once the metal abundance is known and no relevant deviations from the adopted extinction law occur. Finally, we also derived new linear and quadratic absolute magnitude metallicity relations (gLSST vs [Fe/H]) and the metallicity coefficient is consistent with previous findings concerning the B and the V band.
description: Accepted for publication on ApJ
Regional Research and Innovation for City Climate Action: Global Synthesis Report
Creators: name: Hadfield, Paris
name: OKE, CATHY
name: Verbeeck, Jorn
Publisher: name: University of Melbourne
Year: 2021
Subjects: Urban policy
Environment policy

description: This document summarises insights from a global database of city climate change mitigation and adaptation actions drawn from a random sample of cities committed to the Global Covenant of Mayors for Climate and Energy (GCoM) by region. Actions in the database were extracted from publicly available climate action strategy documents published in English between 2016 and mid-2020. The database assesses the content and comprehensiveness of proposed city climate actions aggregated by region, including how research and innovation is integrated in the strategies and common focus areas. The data is not intended to be statistically representative of city climate actions in the respective regions. The research was conducted by the Connected Cities Lab at the University of Melbourne for GCoM, in partnership with Ironbark Sustainability.
Youth Employment Study: Findings from the first survey
Creators: name: Dimov, Stefanie
name: KAVANAGH, ANNE
name: Shields, Marissa
name: Badji, Samia
name: LAMONTAGNE, ANTHONY
name: VAUGHAN, CATHERINE
name: PETRIE, DENNIS
name: KING, TANIA
name: DICKINSON, HELEN
Publisher: name: University of Melbourne
Year: 2021
Subjects: Occupational and workplace health and safety

description: The Youth Employment Study is a study of Australian youth, aged 15 to 25, looking for work during the COVID-19 pandemic. An overview of findings relating to looking for work and previous work, employment programs, wellbeing, housing, and financial stresses is summarised along with recommendations arising from the findings (Recommendations 1-5).
Chemical and Physical Characterization of the Isolated Protostellar Source CB68: FAUST. IV
Creators: name: Imai, Muneaki
name: Oya, Yoko
name: Svoboda, Brian
name: members, FAUST
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: Chemical diversity of low-mass protostellar sources has so far been recognized, and environmental effects are invoked as its origin. In this context, observations of isolated protostellar sources without influences of nearby objects are of particular importance. Here, we report chemical and physical structures of the low-mass Class 0 protostellar source IRAS 16544$-$1604 in the Bok globule CB68, based on 1.3 mm ALMA observations at a spatial resolution of $\sim$70~au that were conducted as part of the large program FAUST. Three interstellar saturated complex organic molecules (iCOMs), CH$_3$OH, HCOOCH$_3$, and CH$_3$OCH$_3$, are detected toward the protostar. The rotation temperature and the emitting region size for CH$_3$OH are derived to be $131\pm11$~K and $\sim$10~au, respectively. The detection of iCOMs in close proximity to the protostar indicates that CB68 harbors a hot corino. The kinematic structure of the C$^{18}$O, CH$_3$OH, and OCS lines is explained by an infalling-rotating envelope model, and the protostellar mass and the radius of the centrifugal barrier are estimated to be $0.08-0.30$~$M_\odot$ and $< 30$ au, respectively. The small radius of the centrifugal barrier seems to be related to the small emitting region of iCOMs. In addition, we detect emission lines of c-C$_3$H$_2$ and CCH associated with the protostar, revealing a warm carbon chain chemistry (WCCC) on a 1000~au scale. We therefore find that the chemical structure of CB68 is described by a hybrid chemistry. The molecular abundances are discussed in comparison with those in other hot corino sources and reported chemical models.
description: 43 pages, 4 tables, 12 figures
Pollenia margarita Schluesslmayr & Sivell, 2021, nov.sp.
Creators: name: Schluesslmayr, Gerhard
name: Sivell, Olga
Publisher: name: Zenodo
Year: 2021
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Diptera
Polleniidae
Pollenia
Pollenia margarita

description: Pollenia margarita nov.sp. (Figs 1-18)
M a t e r i a l e x a m i n e d: Holotype ♁, AUSTRIA: Lower Austria, Nationalpark Donau-Auen, Lobau, Mühlleiten E Vienna, 48.162N / 16,564E, 150 m a.s.l., 30.03.2021, leg. & det. G. Schlüsslmayr. Holotype in Natural History Museum London. Paratypes: same locality and date as for holotype: 2♁♁. 1 Paratype in Biologiezentrum Linz (LI).
A d d i t i o n a l m a t e r i a l: AUSTRIA: LowerAustria, NationalparkDonau-Auen, Orth an der Donau, 48.128N / 16.708E, 150 m a.s.l., 30.03.2021, 1 ♁; Lower Austria, Nationalpark Donau-Auen, Stopfenreuth, 48.14N / 16.90E, 145 m a.s.l., 30.03.2021, 2♁♁, leg. & det. G. Schlüsslmayr.
description: Published as part of Schluesslmayr, Gerhard & Sivell, Olga, 2021, Pollenia margarita, a new species of Pollenia ROBINEAU-DESVOIDY, 1830 from Austria (Diptera, Polleniidae), pp. 413-419 in Linzer biologische Beiträge 53 (1) on page 413, DOI: 10.5281/zenodo.13153685
A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). VII. Redshift Evolution of Radio Galaxy Environments at z=0.3-1.4
Creators: name: Uchiyama, Hisakazu
name: Yamashita, Takuji
name: Nagao, Tohru
name: Ichikawa, Kohei
name: Toba, Yoshiki
name: Ishikawa, Shogo
name: Kubo, Mariko
name: Kajisawa, Masaru
name: Kawaguchi, Toshihiro
name: Kawakatu, Nozomu
name: Lee, Chien-Hsiu
name: Noboriguchi, Akatoki
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We examine the redshift evolution of density environments around 2,163 radio galaxies with the stellar masses of $\sim10^{9}-10^{12} M_\odot$ between redshifts of $z=0.3-1.4$, based on the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) and Faint Images of the Radio Sky at Twenty-cm (FIRST). We use the $k$-nearest neighbor method to measure the local galaxy number density around our radio galaxy sample. We find that the overdensities of the radio galaxies are weakly but significantly anti-correlated with redshift. This is consistent with the known result that the relative abundance of less-massive radio galaxies increases with redshift, because less-massive radio galaxies reside in relatively low density regions. Massive radio galaxies with stellar mass of $M_* >10^{11}M_\odot$ are found in high density environments compared with the control sample galaxies with radio-non-detection and matched-stellar-mass. Less-massive radio galaxies with $M_* <10^{11}M_\odot$ reside in average density environments. The fraction of the radio galaxies associated with the neighbors within a typical major merger scale, $<70$ kpc, is higher than (comparable to) that of the control galaxies at $M_* >10^{11}M_\odot$ ($M_* <10^{11}M_\odot$). We also find that the local densities around the radio galaxies are anti-correlated with the radio luminosities and black hole mass accretion rates at fixed stellar mass. These findings suggest that massive radio galaxies have matured through galaxy mergers in the past, and have supermassive black holes whose mass accretion almost ceased at $z>1.4$, while less-massive radio galaxies undergo active accretion just at this epoch, as they have avoided such merger events.
description: 14 pages, 8 figures, ApJ accepted
Magnetic Field of Molecular Gas Measured with the Velocity Gradient Technique I. Orion A
Creators: name: Zhao, Mengke
name: Zhou, Jianjun
name: Hu, Yue
name: Lazarian, A.
name: Tang, Xindi
name: Baan, Willem A.
name: Esimbek, Jarken
name: He, Yuxin
name: Li, Dalei
name: Ji, Weiguang
name: Tursun, Kadirya
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Magnetic fields play an important role in the evolution of molecular clouds and star formation. Using the Velocity Gradient Technique (VGT) model, we measured the magnetic field in Orion A using the 12CO, 13CO, and C18O (1-0) emission lines at a scale of 0.07 pc. The measured B-field shows an east-west orientation that is perpendicular to the integral shaped filament of Orion A at large scale. The VGT magnetic fields obtained from 13CO and C18O are in agreement with the B-field that is measured from the Planck 353 GHz dust polarization at a scale of 0.55 pc. Removal of density effects by using a Velocity Decomposition Algorithm can significantly improve the accuracy of the VGT in tracing magnetic fields with the 12CO (1-0) line. The magnetic field strength of seven sub-clouds, OMC-1, OMC-2, OMC-3, OMC-4, OMC-5, L 1641-N, and NGC 1999 has also been estimated with the Davis-Chandrasekhar-Fermi (DCF) and MM2 technique, and these are found to be in agreement with previous results obtained from dust polarization at far-infrared and sub-millimeter wavelengths. At smaller scales, the VGT proves a good method to measure magnetic fields.
description: 15 pages, 6 figures, accepted to ApJ
Toward fully compressible numerical simulations of stellar magneto-convection with the RAMSES code
Creators: name: Cuissa, José R. Canivete
name: Teyssier, Romain
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: Numerical simulations of magneto-convection have greatly expanded our understanding of stellar interiors and stellar magnetism. Recently, fully compressible hydrodynamical simulations of full-star models have demonstrated the feasibility of studying the excitation and propagation of pressure and internal gravity waves in stellar interiors, which would allow for a direct comparison with asteroseismological measurements. However, the impact of magnetic fields on such waves has not been taken into account yet in three-dimensional simulations. We conduct a proof of concept for the realization of three-dimensional, fully compressible, magneto-hydrodynamical numerical simulations of stellar interiors with the RAMSES code. We adapted the RAMSES code to deal with highly subsonic turbulence, typical of stellar convection, by implementing a well-balanced scheme in the numerical solver. We then ran and analyzed three-dimensional hydrodynamical and magneto-hydrodynamical simulations with different resolutions of a plane-parallel convective envelope on a Cartesian grid. Both hydrodynamical and magneto-hydrodynamical simulations develop a quasi-steady, turbulent convection layer from random density perturbations introduced over the initial profiles. The convective flows are characterized by small-amplitude fluctuations around the hydrodynamical equilibrium of the stellar interior, which is preserved over the whole simulation time. Using our compressible well-balanced scheme, we were able to model flows with Mach numbers as low as $\mathcal{M} \sim 10^{-3}$, but even lower Mach number flows are possible in principle. In the magneto-hydrodynamical runs, we observe an exponential growth of magnetic energy consistent with the action of a small-scale dynamo. (Abridged)
description: accepted for publication on A&A
ALMA reveals extended cool gas and hot ionized outflows in a typical star-forming galaxy at $z=7.13$
Creators: name: Akins, Hollis
name: Fujimoto, Seiji
name: Finlator, Kristian
name: Watson, Darach
name: Knudsen, Kirsten
name: Richard, Johan
name: Bakx, Tom
name: Hashimoto, Takuya
name: Inoue, Akio
name: Matsuo, Hiroshi
name: Michalowski, Michal
name: Tamura, Yoichi
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present spatially-resolved morphological properties of [CII] 158 $μ$m, [OIII] 88 $μ$m, dust, and rest-frame ultraviolet (UV) continuum emission for A1689-zD1, a strongly lensed, sub-L* galaxy at $z=7.13$, by utilizing deep Atacama Large Millimeter/submillimeter Array (ALMA) and Hubble Space Telescope (HST) observations. While the [OIII] line and UV continuum are compact, the [CII] line is extended up to a radius of $r \sim 12$ kpc. Using multi-band rest-frame far-infrared (FIR) continuum data ranging from 52-400 $μ$m, we find an average dust temperature and emissivity index of $T_{\rm dust} = 41^{+17}_{-14}$ K and $β= 1.7^{+1.1}_{-0.7}$, respectively, across the galaxy. We find slight differences in the dust continuum profiles at different wavelengths, which may indicate that the dust temperature decreases with distance. We map the star-formation rate (SFR) via IR and UV luminosities and determine a total SFR of $37\pm 1~M_\odot~{\rm yr}^{-1}$ with an obscured fraction of $87\%$. While the [OIII] line is a good tracer of the SFR, the [CII] line shows deviation from the local $L_{\rm [CII]}$-SFR relations in the outskirts of the galaxy. Finally, we observe a clear difference in the line profile between [CII] and [OIII], with significant residuals ($\sim 5σ$) in the [OIII] line spectrum after subtracting a single Gaussian model. This suggests a possible origin of the extended [CII] structure from the cooling of hot ionized outflows. The extended [CII] and high-velocity [OIII] emission may both contribute in part to the high $L_{\rm [OIII]}$/$L_{\rm [CII]}$ ratios recently reported in $z>6$ galaxies.
description: 22 pages, 14 figures, accepted to ApJ, presented at AAS240
Barriers and enablers in the development of the COVID-19 Management and Operational Plan for People with Disability
Creators: name: Green, Celia
name: DICKINSON, HELEN
name: CAREY, GEMMA
Publisher: name: University of Melbourne
Year: 2021
Subjects: Public policy
Public health not elsewhere classified
People with disability

description: This report explores the barriers and enablers that led to the development of the Management and Operational Plan for People with Disability, the Federal Government’s National Action Plan for protecting people with disability during the pandemic. The report provides a descriptive account of findings from interviews with key stakeholders involved in the development of the Action Plan.
Early in the COVID-19 pandemic, Australians with disability were identified as a vulnerable population due to increased risk of morbidity and mortality as a result of underlying health conditions, potential exposures to multiple support workers and informal carers, and ‘social determinants of health’ impacts such as discrimination and social exclusion. Despite this, people with disability were largely ignored in the Federal Government’s initial COVID-19 policy response. Consequently, the disability sector rapidly mobilised to lobby for the Federal Government to create a disability specific policy response, which resulted in the Commonwealth Department of Health forming an Advisory Group and associated Roundtable to help inform the development of a response. Despite an initial lack of action to protect people with disability by the Federal Government, there were a number of enablers that helped both draw policy makers attention to the issue and facilitated a relatively rapid policy response once policy makers were on board. The process of developing the COVID-19 disability policy response was seen by stakeholders as a mostly positive experience. Many members of the groups expressed a desire for the structures (Advisory Committee and Roundtable), which had been established during 2020 to continue once the immediate threat of the pandemic is over. However, it was also identified that to continue in an effective manner there would need to be a tight focus for the group(s) to avoid confusion over the purpose and direction moving forward. While there were positive aspects to the development of the Action Plan, there were also a number of barriers identified that hindered its execution. Many of these barriers are long standing issues in the disability-health policy interface rather than new issues and these were further exacerbated in the context of the COVID-19 pandemic. Overall, there was positive engagement with the sector once the Advisory Committee and Roundtable were established, however fully implementing responses was more challenging due to issues such as lack of collection of data on which to base decisions and ongoing difficulties in the disability health interface.
SRI LANKA’S AGRI-FOOD TRADE: STRUCTURE, OPPORTUNITIES, CHALLENGES & IMPACTS OF COVID-19
Creators: name: Dissanayaka, Nimesha
name: Thibbotuwana, Manoj
name: Dissanayaka, Nimesha
name: Thibbotuwana, Manoj
Publisher: name: Unknown
Year: 2021
Subjects: subject: Agricultural and Food Policy
subject: Trade flow analysis
subject: COVID-19
subject: barriers to trade
subject: trade patterns
subject: food security

description: This paper analyses Sri Lanka’s opportunities and challenges in agri-food trade amid COVID-19. Among the many impending crises that are gradually unfolding, the challenge of rising food insecurity resulting from the COVID-19 and the measures to contain it can be considered as one of the most critical. Therefore, Sri Lanka, as a middle-income country, should immediately identify the emerging trade patterns, opportunities, and challenges to face the upcoming trade competitiveness due to COVID-19. The paper presents an overview of Sri Lanka’s agricultural trade flows in the world. It describes Sri Lanka’s main import and export partners of the country, market characteristics, shifting of main export destinations, the export potential of Sri Lanka’s agricultural products to other countries. It analyses the immediate impact of the COVID-19 pandemic on Sri Lanka’s import and export sectors, and the barriers to the trade of agricultural products in Sri Lanka. Results indicate that in addition to the main export agriculture commodities such as tea, there might be other emerging agri-food products with a high potential to grow. Identifying such products and potential export markets would be important for the expansion of international trade in new arenas.
Unusual gas structure in an otherwise normal spiral galaxy hosting GRB 171205A / SN 2017iuk
Creators: name: Arabsalmani, M.
name: Roychowdhury, S.
name: Renaud, F.
name: Burkert, A.
name: Emsellem, E.
name: Floc'h, E. Le
name: Pian, E.
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 study the structure of atomic hydrogen (HI) in the host galaxy of GRB 171205A / SN 2017iuk at z=0.037 through HI 21cm emission line observations with the Karl G. Jansky Very Large Array. These observations reveal unusual morphology and kinematics of the HI in this otherwise apparently normal galaxy. High column density, cold HI is absent from an extended North-South region passing by the optical centre of the galaxy, but instead is extended towards the South, on both sides of the galaxy. Moreover, the HI kinematics do not show a continuous change along the major axis of the galaxy as expected in a classical rotating disk. We explore several scenarios to explain the HI structure and kinematics in the galaxy: feedback from a central starburst and/or an active galactic nucleus, ram pressure stripping, accretion, and tidal interaction from a companion galaxy. All of these options are ruled out. The most viable remaining explanation is the penetrating passage of a satellite through the disk only a few Myr ago, redistributing the HI in the GRB host without yet affecting its stellar distribution. It can also lead to the rapid formation of peculiar stars due to a violent induced shock. The location of GRB 171205A in the vicinity of the distorted area suggests that its progenitor star(s) originated in extreme conditions that share the same origin as the peculiarities in HI. This could explain the atypical location of GRB 171205A in its host galaxy.
description: This is the Accepted Manuscript version of an article accepted for publication in The Astronomical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The manuscript has 8 pages and 2 figures
SN 2016dsg: A Thermonuclear Explosion Involving A Thick Helium Shell
Creators: name: Dong, Yize
name: Valenti, Stefano
name: Polin, Abigail
name: Boyle, Aoife
name: Flörs, Andreas
name: Vogl, Christian
name: Kerzendorf, Wolfgang
name: Sand, David
name: Jha, Saurabh
name: Wyrzykowski, Lukasz
name: Bostroem, K.
name: Pearson, Jeniveve
name: McCully, Curtis
name: Andrew, Jennifer
name: Benettii, Stefano
name: Blondin, Stephane
name: Galbany, Lluís
name: Gromadzki, Mariusz
name: Hosseinzadeh, Griffin
name: Howell, D. Andrew
name: Inserra, Cosimo
name: Jencson, Jacob
name: Lundquist, M.
name: Lyman, Joseph
name: Magee, Mark
name: Maguire, Kate
name: Meza, Nicolas
name: Srivastav, Shubham
name: Taubenberger, Stefan
name: Terwel, J
name: Wyatt, Samuel
name: Young, David
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: A thermonuclear explosion triggered by a helium-shell detonation on a carbon-oxygen white dwarf core has been predicted to have strong UV line blanketing at early times due to the iron-group elements produced during helium-shell burning. We present the photometric and spectroscopic observations of SN 2016dsg, a sub-luminous peculiar Type I SN consistent with a thermonuclear explosion involving a thick He shell. With a redshift of 0.04, the $i$-band peak absolute magnitude is derived to be around -17.5. The object is located far away from its host, an early-type galaxy, suggesting it originated from an old stellar population. The spectra collected after the peak are unusually red, show strong UV line blanketing and weak O I $λ$7773 absorption lines, and do not evolve significantly over 30 days. An absorption line around 9700-10500 Åis detected in the near-infrared spectrum and is likely from the unburnt helium in the ejecta. The spectroscopic evolution is consistent with the thermonuclear explosion models for a sub-Chandrasekhar mass white dwarf with a thick helium shell, while the photometric evolution is not well described by existing models.
description: accepted for publication in ApJ