cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
KIC 6951642: a Kepler δ Scuti-𝜸 Dor star affected by rotation and stellar activity in a (possible) single-lined binary system
Creators: name: Samadi-Ghadim, Anya
name: Lampens, Patricia
Publisher: name: Zenodo
Year: 2022
Subjects: Asteroseismology - Techniques: photometric (Fourier) - Stars: variables: δ Scuti - Stars: rotation - Stars: activity - (Stars:) binaries: spectroscopic

description: Introduction: KIC 6951642 has been reported as a candidate hybrid pulsator of type γ Dor – δ Scuti from the first-quarters observations of the Kepler mission. The occurrence of a broad range of very regularly-spaced frequencies in the Fourier spectra of the available light curves and the long-term modulation of its surface brightness furthermore suggest the presence of, respectively, rotational modulation (due to spots) and stellar activity. Methods: We performed an iterative frequency-search of each Fourier spectrum, and searched for regular patterns in them. We applied spectrum synthesis to determine the atmospheric stellar parameters. Furthermore, since KIC 6951642 was announced to be a long-period binary system, we also fitted the radial velocities of our spectra from the high-resolution, high-efficiency spectrograph HERMES (Raskin et al. 2011) with some time delays derived from the light curves to improve the (first) orbit determination. Results: From high-resolution spectroscopy, we found that KIC 6951642 is a fast-rotating, F0-type, (possible) single-lined binary star with a period of ∼4.8 yr. We detected frequencies of type δ Scuti with the strongest mode located at 13.96 d−1, as well as two multiplets with a regular mean frequency spacing of 0.481 d-1 (natural large frequency spacing), and two multiplets with the rotational splitting as large as 0.719 d-1. In the low-frequency (g-mode) regime, we recovered the frequency of 0.721 d−1, as well as the frequency of 0.0087 d−1. We attribute the first one to stellar rotation and the second one to stellar activity with a (possibly magnetic) cycle length of 3.2 yr. We detected g-modes of γ Dor-type with the mean period spacings of 207.6 s in the frequency range of (1.4-1.6) d−1 .
Flux and spectral variability of Mrk 421 during its moderate activity state using NuSTAR: Possible accretion disc contribution?
Creators: name: Mondal, Santanu
name: Rani, Priyanka
name: Stalin, C. S.
name: Chakrabarti, Sandip K.
name: Rakshit, Suvendu
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: The X-ray emission in BL Lac objects is believed to be dominated by synchrotron emission from their relativistic jets. However, when the jet emission is not strong, one could expect signatures of X-ray emission from inverse Compton scattering of accretion disc photons by the corona. Moreover, the observed X-ray variability can also originate in the disc, and gets propagated and amplified by the jet. Here, we present results on the BL Lac object Mrk 421 using the NuSTAR data acquired during 2017 when the source was in a moderate X-ray brightness state. For comparison with high jet activity, we also considered one epoch data in April 2013 during a very high X-ray brightness state. Our aim is to explore the possibility of the signature of accretion disc emission in the overall X-ray emission from Mrk 421. The spectral fitting of the data using the two component advective flow model shows gives (a) the size of the dynamic corona at the base of the jet from ~28 to 10 r$_s$, (b) the disc mass accretion rate from 0.021 to 0.051 $\dot M_{\rm Edd}$, (c) the halo mass accretion rate from 0.22 to 0.35 $\dot M_{\rm Edd}$, and (d) the viscosity parameter of the Keplerian accretion disc from 0.18 $-$ 0.25. In the assumed model, the total flux, disc and jet flux correlate with the radio flux observed during these epochs. We conclude that the spectra of all the epochs of Mrk 421 in 2017 are well described by the accretion disc based two component advective flow model. The estimated disc and jet flux relations with radio flux show that accretion disc can contribute to the observed X-ray emission, when X-ray data (that covers a small portion of the broad band spectral energy distribution of Mrk 421) is considered in isolation. However, the present disc based models are disfavoured with respect to the relativistic jet models when considering the X-ray data in conjunction with data at other wavelengths.
description: 15 pages, 9 figures, 9 tables, accepted for publication in A&A, comments welcome
OʻRTA OSIYO XATTOTLIK SAN'ATI (IX - XVI ASRLAR)
Creators: name: Bo'ronov, Ismoiljon
name: Moʻminov, Xusanboy
Publisher: name: Zenodo
Year: 2024

description: Ushbu maqolada o‘rta asrlarda O‘rta Osiyoga xattotlik san’atining rivojlanishi, arab alifbosiga asoslangan yozuv turlarining takomillashuvi va isloh qilinishi masalalari tahlil etilgan.
The interplay between AGN feedback and precipitation of the intracluster medium in simulations of galaxy groups and clusters
Creators: name: Nobels, Folkert S. J.
name: Schaye, Joop
name: Schaller, Matthieu
name: Bahé, Yannick M.
name: Chaikin, Evgenii
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Using high-resolution hydrodynamical simulations of galaxy clusters, we study the interaction between the brightest cluster galaxy, its supermassive black hole (BH) and the intracluster medium (ICM). We create initial conditions for which the ICM is in hydrostatic equilibrium within the gravitational potential from the galaxy and an NFW dark matter halo. Two free parameters associated with the thermodynamic profiles determine the cluster gas fraction and the central temperature, where the latter can be used to create cool-core or non-cool-core systems. Our simulations include radiative cooling, star formation, BH accretion, and stellar and active galactic nucleus (AGN) feedback. Even though the energy of AGN feedback is injected thermally and isotropically, it leads to anisotropic outflows and buoyantly rising bubbles. We find that the BH accretion rate (BHAR) is highly variable and only correlates strongly with the star formation rate (SFR) and the ICM when it is averaged over more than $1~\rm Myr$. We generally find good agreement with the theoretical precipitation framework. In $10^{13}~\rm M_\odot$ haloes, AGN feedback quenches the central galaxy and converts cool-core systems into non-cool-core systems. In contrast, higher-mass, cool-core clusters evolve cyclically. Episodes of high BHAR raise the entropy of the ICM out to the radius where the ratio of the cooling time and the local dynamical time $t_{\rm cool}/t_{\rm dyn} > 10$, thus suppressing condensation and, after a delay, the BHAR. The corresponding reduction in AGN feedback allows the ICM to cool and become unstable to precipitation, thus initiating a new episode of high SFR and BHAR.
description: 22 pages, 15 figures (including appendix); submitted to MNRAS; Supplementary material is available on Youtube at https://youtu.be/HQhc_mytj0A and online on a single website page at https://home.strw.leidenuniv.nl/~nobels/supplementary_idealised_cluster_paper.php
ООН И ЕЁ РОЛЬ В ЗАЩИТЕ ПРАВ ЧЕЛОВЕКА
Creators: name: Гаффорова, Муниса
Publisher: name: Zenodo
Year: 2024

description: В представленной работе освещается роль Организации Объединённых Наций в защите прав человека, подчеркивая их неотъемлемость и универсальность, а также важность их уважительного отношения. Автор аргументирует значимость прав человека в формировании справедливого и демократического общества, основанного на уважении человеческого достоинства. В работе также обращается внимание на систематические нарушения прав человека и необходимость их борьбы и защиты на мировом уровне. Особое внимание уделяется призыву общественным организациям, правительствам и гражданам к созданию общества, где основной целью является поощрение и защита прав человека.
Probing massive neutrinos with the Minkowski functionals of large-scale structure
Creators: name: Liu, Wei
name: Jiang, Aoxiang
name: Fang, Wenjuan
Publisher: name: arXiv
Year: 2022
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: Massive neutrinos suppress the growth of structure under their free-streaming scales. The effect is most prominent on small scales where the widely-used two-point statistics can no longer capture the full information. In this work, we study the signatures massive neutrinos leave on large-scale structure (LSS) as revealed by its morphological properties, which are fully described by $4$ Minkowski functionals (MFs), and quantify the constraints on the summed neutrino mass $M_ν$ from the MFs, by using publicly available N-body simulations. We find the MFs provide important complementary information, and give tighter constraints on $M_ν$ than the power spectrum. Specifically, depending on whether massive neutrinos are included in the density field (the `m' field) or not (the `cb' field), we find the constraint on $M_ν$ from the MFs with a smoothing scale of $R_G=5 h^{-1}$Mpc is $48$ or $4$ times better than that from the power spectrum. When the MFs are combined with the power spectrum, they can improve the constraint on $M_ν$ from the latter by a factor of 63 for the `m' field and 5 for the `cb' field. Notably, when the `m' field is used, the constraint on $M_ν$ from the MFs can reach $0.0177$eV with a volume of $1(h^{-1}\rm Gpc)^3$, while the combination of the MFs and power spectrum can tighten this constraint to be $0.0133$eV, a $4.5σ$ significance on detecting the minimum sum of the neutrino masses. For the `m' field, we also find the $σ_8$ and $M_ν$ degeneracy is broken with the MFs, leading to stronger constraints on all 6 cosmological parameters considered in this work than the power spectrum.
description: Accepted for publication in JCAP. Changes from the first version: add figure 10, and minor text revisions. Matches accepted version. 33 pages, 10 figures, 2 tables
Validation and interpretation of three-dimensional configuration of a magnetic cloud flux rope
Creators: name: Hu, Qiang
name: Zhu, Chunming
name: He, Wen
name: Qiu, Jiong
name: Jian, Lan K.
name: Prasad, Avijeet
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Plasma Physics (physics.plasm-ph)
subject: Space Physics (physics.space-ph)
subject: FOS: Physical sciences

description: One "strong" magnetic cloud (MC) with the magnetic field magnitude reaching $\sim$ 40 nT at 1 au during 2012 June 16-17 is examined in association with a pre-existing magnetic flux rope (MFR) identified on the Sun. The MC is characterized by a quasi-three dimensional (3D) flux rope model based on in situ measurements from the Wind spacecraft. The magnetic flux contents and other parameters are quantified. In addition, a correlative study with the corresponding measurements of the same structure crossed by the Venus Express (VEX) spacecraft at a heliocentric distance 0.7 au and with an angular separation $\sim 6^\circ$ in longitude is performed to validate the MC modeling results. The spatial variation between the Wind and VEX magnetic field measurements is attributed to the 3D configuration of the structure as featured by a knotted bundle of flux. The comparison of the magnetic flux contents between the MC and the source region on the Sun indicates that the 3D reconnection process accompanying an M1.9 flare may correspond to the magnetic reconnection between the field lines of the pre-existing MFR rooted in the opposite polarity footpoints. Such a process reduces the amount of the axial magnetic flux in the erupted flux rope, by approximately 50\%, in this case.
description: Submitted to ApJ
National Disability Strategy: Beyond 2020 Webinar Report
Creators: name: Fortune, Nicola
Publisher: name: University of Melbourne
Year: 2021
Subjects: Public health not elsewhere classified
People with disability
Public policy
Human rights and justice issues (excl. law)
Public economics - publicly provided goods
Health economics
Health and community services
Community psychology
Social psychology

description: This report is a summary of the webinar panel discussion on the National Disability Strategy held on 24 September 2020.
Th event was organised by the Australian Human Rights Commission and the NHMRC Centre of Research Excellence in Disability and Health, and hosted by The Social Deck via Zoom webinar.
There were three panels and the report summarises the key discussions from each panel as follows:

Panel One: A reflection on the last National Disability StrategyPanel Two: What is needed under the National Disability Strategy?Panel Three: Issues for the new National Disability Strategy
------The Australian Human Rights Commission (AHRC) is an independent statutory organisation, established by an act of Federal Parliament. The AHRC protects and promotes human rights in Australia and internationally – it investigates complaints about discrimination and human rights breaches, conciliates discrimination complaints, holds public inquiries, and develops education resources for schools and workplaces. The AHRC also provides legal advice to courts, makes submissions to parliaments and governments, and initiates research into human rights and discrimination issues. https://humanrights.gov.au/

The Centre of Research Excellence in Disability and Health (CRE-DH) is a world-first research initiative that aims to build knowledge and gather the evidence needed to guide social and health policy reform for people with disability in Australia. The CRE-DH also aims to identify cost-effective policies that improve the health of people with disability in Australia. The CRE-DH is funded by the National Health and Medical Research Council. https://credh.org.au/

The Social Deck is a for-purpose business specialising in strategic communications, stakeholder and community engagement, digital strategy, social marketing campaigns and evaluation. The Social Deck helps organisations to reach and engage people in actions that have a positive impact on society and the environment. https://www.thesocialdeck.com.au/

The report was written by Dr Nicola Fortune from the Centre of Research Excellence in Disability and Health and finalised by 2 December 2020.

https://credh.org.au/reports-and-submissions/
Binary Natal Kicks in the Galactic Center: X-ray Binaries, Hypervelocity Stars, and Gravitational Waves
Creators: name: Hoang, Bao-Minh
name: Naoz, Smadar
name: Sloneker, Melodie
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Theoretical and observational studies suggest that stellar binaries exist in large numbers in galactic nuclei like our own Galactic Center. Neutron stars (NSs), and debatedly, black holes (BHs) and white dwarfs (WDs), receive natal kicks at birth. In this work we study the effect of two successive natal kicks on a population of stellar binaries orbiting the massive black hole (MBH) in our Galactic Center. These natal kicks can significantly alter the binary orbit in a variety of ways, and also the orbit of the binary around the MBH. We found a variety of dynamical outcomes resulting from these kicks, including a steeper cusp of single NSs relative to the initial binary distribution. Furthermore, hypervelocity star and binary candidates, including hypervelocity X-ray binaries, are a common outcome of natal kicks. In addition, we show that the population of X-ray binaries in the Galactic Center can be used as a diagnostic for the BH natal kick distribution. Finally, we estimate the rate of gravitational wave (GW) events triggered by natal kicks, including binary mergers and EMRIs.
description: Accepted to ApJ
One Star to Tag Them All (OSTTA): I. Radial velocities and chemical abundances for 20 poorly studied open clusters
Creators: name: Carrera, R.
name: Casamiquela, L.
name: Bragaglia, A.
name: Carretta, E.
name: Carbajo-Hijarrubia, J.
name: Jordi, C.
name: Alonso-Santiago, J.
name: Balaguer-Nuñez, L.
name: Baratella, M.
name: D'Orazi, V.
name: Lucatello, S.
name: Soubiran, C.
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: Context: Open clusters are ideal laboratories to investigate a variety of astrophysical topics, from the properties of the Galactic disc to stellar evolution models. For this purpose, we need to know their chemical composition in detail. Unfortunately, the number of systems with chemical abundances determined from high resolution spectroscopy remains small. Aims: Our aim is to increase the number of open clusters with radial velocities and chemical abundances determined from high resolution spectroscopy by sampling a few stars in clusters not studied previously. Methods: We obtained high resolution spectra with the FIES spectrograph at NOT for 41 stars belonging to 20 open clusters. These stars have high astrometric membership probabilities, determined from the Gaia second data release. Results: We derived radial velocities for all the observed stars, which were used to confirm their membership to the corresponding clusters. For Gulliver\,37 we cannot be sure the observed star is a real member. We derived atmospheric parameters for the 32 stars considered real cluster members. We discarded five stars because they have very low gravity or atmospheric parameters were not properly constrained due to low signal-to-noise ratio spectra. Therefore, detailed chemical abundances were determined for 28 stars belonging to 17 clusters. For most of them, this is the first chemical analysis available in the literature. Finally, we compared the clusters in our sample to a large population of well studied clusters. The studied systems follow the trends, both chemical and kinematical, described by the majority of open clusters. Worth noticing that the three most metal-poor studied clusters (NGC\,1027, NGC\,1750 and Trumpler 2) are enhanced in Si but not in the other alpha-elements studied (Mg, Ca and Ti).
description: 19 pages Accepted for publication on A&A
Thermodynamic geometry and complexity of black holes in theories with broken translational invariance
Creators: name: Babaei-Aghbolagh, H.
name: Mohammadzadeh, Hosein
name: Yekta, Davood Mahdavian
name: Velni, Komeil Babaei
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Physics - Theory (hep-th)
subject: General Relativity and Quantum Cosmology (gr-qc)
subject: FOS: Physical sciences

description: The relationship between thermodynamics and the Lloyd bound on the holographic complexity for a black hole has been of interest. We consider $D$ dimensional anti-de Sitter black holes with hyperbolic geometry as well as black holes with momentum relaxation that have a minimum for temperature and mass. We show that the singular points of the thermodynamic curvature of the black holes, as thermodynamic systems, correspond to the zero points of the action and volume complexity at the Lloyd bound. For such black holes with a single horizon, the complexity of volume and the complexity of action at minimum mass and minimum temperature are zero, respectively. We show that the thermodynamic curvature diverges at these minimal values. Because of the behaviour of action complexity and thermodynamic curvature at minimum temperature, we propose the action complexity as an order parameter of the black holes as thermodynamic systems. Also, we derive the critical exponent related to the thermodynamic curvature in different dimensions.
description: 14 pages, 10 figures
The Heliospheric Ambipolar Potential Inferred from Sunward-Propagating Halo Electrons
Creators: name: Horaites, Konstantinos
name: Boldyrev, Stanislav
Publisher: name: arXiv
Year: 2022
Subjects: subject: Space Physics (physics.space-ph)
subject: FOS: Physical sciences

description: We provide evidence that the sunward-propagating half of the solar wind electron halo distribution evolves without scattering in the inner heliosphere. We assume the particles conserve their total energy and magnetic moment, and perform a "Liouville mapping" on electron pitch angle distributions measured by the Parker Solar Probe SPAN-E instrument. Namely, we show that the distributions are consistent with Liouville's theorem if an appropriate interplanetary potential is chosen. This potential, an outcome of our fitting method, is compared against the radial profiles of proton bulk flow energy. We find that the inferred potential is responsible for nearly 100% of the proton acceleration in the solar wind at heliocentric distances 0.18-0.79 AU. These observations combine to form a coherent physical picture: the same interplanetary potential accounts for the acceleration of the solar wind protons as well as the evolution of the electron halo. In this picture the halo is formed from a sunward-propagating population that originates somewhere in the outer heliosphere by a yet-unknown mechanism.
Disc dichotomy signature in the vertical distribution of [Mg/Fe] and the delayed gas infall scenario
Creators: name: Spitoni, E.
name: Børsen-Koch, V. Aguirre
name: Verma, K.
name: Stokholm, A.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: The analysis of the APOGEE data suggests the existence of a clear distinction between two sequences of disc stars in the [$α$/Fe] vs. [Fe/H] abundance ratio space. We aim to test if the two-infall chemical evolution models designed to reproduce these two sequences in the solar neighbourhood are also capable to predict the disc bimodality observed in the vertical distribution of [Mg/Fe] in APOGEE DR16 data. Along with the predicted chemical composition of SSPs born at different Galactic times in the solar vicinity, we provide their maximum vertical height |zmax| above the Galactic plane computed assuming the relation between the vertical action and stellar age in thin disc stars. The predicted vertical distribution of the [Mg/Fe] abundance ratio is in agreement with the one observed combining the APOGEE DR16 data and the astroNN catalogue (stellar ages, orbital parameters) for stars younger than 8 Gyr (only low-$α$ sequence stars). Including the high-$α$ disc component, the dichotomy in the vertical [Mg/Fe] abundance distribution is reproduced considering the observational cut in the Galactic height of |z| < 2 kpc. However, our model predicts a too flat growth of the |zmax| as a function of [Mg/Fe] for high-$α$ objects in contrast with the median values from APOGEE data. Possible explanations for such a tension are: i) the data sample with |z| < 2 kpc is more likely contaminated by halo stars, causing the median values to be kinematically hotter, ii) external perturbations such as minor mergers could have heated up the disc, and the heating of the orbits cannot be modelled by only scattering processes. Assuming for the data a disc dissection based on chemistry, the observed |zmax| distributions for high-$α$ and low-$α$ sequences are in good agreement with our model predictions if we consider in the calculation the errors in the vertical action estimates.
description: Accepted for publication in Astronomy and Astrophysics (A&A), 17 pages, 15 figures
Full superconducting gap in the candidate topological superconductor In$_{1-x}$Pb$_x$Te for x = 0.2
Creators: name: Smylie, M. P.
name: Kobayashi, Kaya
name: Dans, J. Z.
name: Hebbeker, H.
name: Chapai, R.
name: Kwok, W. -K.
name: Welp, U.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Superconductivity (cond-mat.supr-con)
subject: FOS: Physical sciences

description: High-pressure synthesis techniques have allowed for the growth of samples on the indium-rich side of (Pb,In)Te, which have increased superconducting transition temperatures compared to lead-rich compounds. In this study we present measurements of the temperature dependence of the London penetration depth $Δλ(T)$ in the compound In$_{0.8}$Pb$_{0.2}$Te, which shows a bulk $T_{c,onset}$ of $\sim4.75$ K. The results indicate fully gapped BCS-like behavior, ruling out odd-parity, topologically nontrivial $A_{2u}$ pairing; however, odd-parity $A_{1u}$ pairing is still possible. Critical field values measured below 1 K and other superconducting parameters are also presented.
description: 8 pages, 9 figures
Microbulk Micromegas in non-flammable mixtures of argon and neon at high pressure
Creators: name: Iguaz, F. J.
name: Dafni, T.
name: Canellas, C.
name: Castel, J. F.
name: Cebrián, S.
name: Garza, J. G.
name: Irastorza, I. G.
name: Luzón, G.
name: Mirallas, H.
name: Chóliz, E. Ruiz
Publisher: name: arXiv
Year: 2022
Subjects: subject: Instrumentation and Detectors (physics.ins-det)
subject: FOS: Physical sciences

description: We report on a systematic characterization of microbulk Micromegas readouts in high-pressure Ar+1%iC4H10 and Ne+2%iC4H10 mixtures. Experimental data on gain, electron transmission and energy resolution are presented for a wide range of drift and amplification voltages and pressures from 1 bar to 10 bar for argon and from 5 bar to 10 bar in neon, in steps of 1 bar. Maximum gains higher than 1.7e3 (1.7e4) in argon (neon) are measured for all pressures, remarkably without the significant decrease with pressure typically observed in other amplification structures. A competitive energy resolution at 22.1 keV, but with a slight degradation with pressure, is observed:from 10.8% at 1 bar to 15.6% FWHM at 10 bar in argon and from 8.3% at 5 bar to 15.0% FWHM at1 10 bar in neon. The experimental setup, procedure and the results will be presented and discussed in detail. The work is motivated by the TREX-DM experiment, that is operating in the Laboratorio Subterráneo de Canfranc with the mentioned mixtures, although the results may be of interest for other applications of time projection chambers at high pressures.
description: 11 pages, 8 figures, prepared for JINST, minor changes in th text, added a reference
On energetics and progenitors of Odd Radio Circles: A causal connection with tidal disruption of stars?
Creators: name: Omar, A.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Odd Radio Circles or ORCs are recently discovered edge-brightened, low surface brightness circular radio sources. The progenitors and astrophysical processes responsible for their origins are presently debated. Some ORCs are host-less and some appear to be hosted in distant quiescent galaxies. Two plausible explanations consider ORCs as nearby supernova remnants with sizes a few hundred parsec in the intragroup medium of the local group of galaxies or alternatively shocked halos of a few hundred kpc extent around distant galaxies. The input shock energy required to create ORCs of a few hundred kpc size is estimated in a range of $10^{55} - 10^{59}$ erg. It is shown here that the cumulative energy in unbound debris ejected from multiple ($10^{5} - 10^{9}$) tidal disruption events over $\sim100$ Myr period around a central massive black hole can meet the required energies to generate ORCs around some galaxies, which have recently undergone a merger. The potential hosts for ORCs are identified here as abundant post-starburst galaxies at intermediate redshifts having massive black holes. A causal connection between ORC around quiescent galaxies and tidal disruption may find support in the observed dominance of tidal disruption events in post-starburst galaxies.
description: 5 pages, Accepted version in MNRAS Letters, Several new references added and some new analysis presented in this version
Ariel stellar characterisation: I -- homogeneous stellar parameters of 187 FGK planet host stars Description and validation of the method
Creators: name: Magrini, L.
name: Danielski, C.
name: Bossini, D.
name: Rainer, M.
name: Turrini, D.
name: Benatti, S.
name: Brucalassi, A.
name: Tsantaki, M.
name: Mena, E. Delgado
name: Sanna, N.
name: Biazzo, K.
name: Campante, T. L.
name: Van der Swaelmen, M.
name: Sousa, S. G.
name: Helminiak, K. G.
name: Neitzel, A. W.
name: Adibekyan, V.
name: Bruno, G.
name: Casali, G.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: In 2020 the European Space Agency selected Ariel as the next mission to join the space fleet of observatories to study planets outside our Solar System. Ariel will be devoted to the characterisation of a thousand planetary atmospheres, for understanding what exoplanets are made of, how they formed and how they evolve. To achieve the last two goals all planets need to be studied within the context of their own host stars, which in turn have to be analysed with the same technique, in a uniform way. We present the spectro-photometric method we have developed to infer the atmospheric parameters of the known host stars in the Tier 1 of the Ariel Reference Sample. Our method is based on an iterative approach, which combines spectral analysis, the determination of the surface gravity from {\em Gaia} data, and the determination of stellar masses from isochrone fitting. We validated our approach with the analysis of a control sample, composed by members of three open clusters with well-known ages and metallicities. We measured effective temperature, Teff, surface gravity, logg, and the metallicity, [Fe/H], of 187 F-G-K stars within the Ariel Reference Sample. We presented the general properties of the sample, including their kinematics which allows us to separate them between thin and thick disc populations. A homogeneous determination of the parameters of the host stars is fundamental in the study of the stars themselves and their planetary systems. Our analysis systematically improves agreement with theoretical models and decreases uncertainties in the mass estimate (from 0.21+/-0.30 to 0.10+/-0.02 M_sun), providing useful data for the Ariel consortium and the astronomical community at large.
description: Accepted for publication in A&A, 13 pages, 14 figures, Tables A1 and A2 in the Appendix will be available at CDS and can be requested by email to: laura.magrini@inaf.it
The [CII] and FIR properties of z>6 radio-loud quasars
Creators: name: Khusanova, Yana
name: Bañados, Eduardo
name: Mazzucchelli, Chiara
name: Rojas-Ruiz, Sofía
name: Momjian, Emmanuel
name: Walter, Fabian
name: Decarli, Roberto
name: Venemans, Bram
name: Farina, Emanuele Paolo
name: Meyer, Romain
name: Wang, Feige
name: Yang, Jinyi
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: There are only five radio-loud quasars currently known within 1 Gyr from the Big Bang ($z>6$) and the properties of their host galaxies have not been explored in detail. We present a NOrthern Extended Millimeter Array (NOEMA) survey of [CII] (158 $μ$m) and underlying continuum emission of four $z>6$ radio-loud quasars, revealing their diverse properties. J0309+2717 ($z=6.10$) has a bright [CII] line and underlying continuum, implying a starburst with a star-formation rate SFR=$340-1200$ $M_\odot$ yr$^{-1}$. J1429+5447 ($z=6.18$) has a SFR=$520-870$ $M_{\odot}$yr$^{-1}$ and its [CII] profile is consistent with two Gaussians, which could be interpreted as a galaxy merger. J1427+3312 ($z=6.12$) has a moderate SFR=$30-90$ $M_\odot$ yr$^{-1}$. Notably, this is a broad absorption line quasar and we searched for the presence of high-velocity outflows in the host galaxy. Although the NOEMA data reveal a tentative broad component of the [CII] line as wide as $\sim$1400~km~s$^{-1}$, the sensitivity of our current data is not sufficient to confirm it. Finally, P172+18 ($z=6.82$) is undetected in both [CII] and continuum, implying a SFR$<22-40$ $M_{\odot}$yr$^{-1}$. The broad range of SFRs is similar to what is observed in radio-quiet quasars at similar redshifts. If radio jets do not significantly contribute to both [CII] and IR luminosities, this suggest no feedback from the jet on the star formation in the host galaxy.
description: submitted to A&A
Primary care data and linkage: Australian dataset identification and capacity building
Creators: name: CANAWAY, RACHEL
name: BOYLE, DOUGLAS
name: MANSKI-NANKERVIS, JO-ANNE
name: GRAY, KATHLEEN
Publisher: name: University of Melbourne
Year: 2021
Subjects: Primary health care
Public health not elsewhere classified
Health surveillance

description: This report details the findings of a study commissioned by the Australian Health Research Alliance (AHRA) in 2018 as part of its objective to increase data use by healthcare professionals and other stakeholders to improve health outcomes. Drawing primarily from survey and interview data from 62 custodians and users of primary care data used for secondary purposes in Australia, the study explored the primary care-related datasets considered available in Australia and their data linkage status; the quality frameworks being used to assess primary care datasets; and the stakeholder perceptions of enablers and barriers to strategically building benefit and capacity of primary care data use
A deep survey of short GRB host galaxies over $z\sim0-2$: implications for offsets, redshifts, and environments
Creators: name: O'Connor, B.
name: Troja, E.
name: Dichiara, S.
name: Beniamini, P.
name: Cenko, S. B.
name: Kouveliotou, C.
name: Gonzalez, J. Becerra
name: Durbak, J.
name: Gatkine, P.
name: Kutyrev, A.
name: Sakamoto, T.
name: Sanchez-Ramirez, R.
name: Veilleux, S.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: A significant fraction (30\%) of well-localized short gamma-ray bursts (sGRBs) lack a coincident host galaxy. This leads to two main scenarios: \textit{i}) that the progenitor system merged outside of the visible light of its host, or \textit{ii}) that the sGRB resided within a faint and distant galaxy that was not detected by follow-up observations. Discriminating between these scenarios has important implications for constraining the formation channels of neutron star mergers, the rate and environments of gravitational wave sources, and the production of heavy elements in the Universe. In this work, we present the results of our observing campaign targeted at 31 sGRBs that lack a putative host galaxy. Our study effectively doubles the sample of well-studied sGRB host galaxies, now totaling 72 events of which $28\%$ lack a coincident host to deep limits ($r$\,$\gtrsim$\,$26$ or $F110W$\,$\gtrsim$\,$27$ AB mag), and represents the largest homogeneously selected catalog of sGRB offsets to date. We find that 70\% of sub-arcsecond localized sGRBs occur within 10 kpc of their host's nucleus, with a median projected physical offset of $5.6$ kpc. Using this larger population, we discover an apparent redshift evolution in their locations: bursts at low-$z$ occur at $2\times$ larger offsets compared to those at $z$\,$>$\,$0.5$. This evolution could be due to a physical evolution of the host galaxies themselves or a bias against faint high-$z$ galaxies. Furthermore, we discover a sample of hostless sGRBs at $z$\,$\gtrsim$\,$1$ that are indicative of a larger high-$z$ population, constraining the redshift distribution and disfavoring log-normal delay time models.
description: Accepted by MNRAS
Pegasus V -- a newly discovered ultra-faint dwarf galaxy on the outskirts of Andromeda
Creators: name: Collins, Michelle L. M.
name: Charles, Emily J. E.
name: Martínez-Delgado, David
name: Monelli, Matteo
name: Karim, Noushin
name: Donatiello, Giuseppe
name: Tollerud, Erik J.
name: Boschin, Walter
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: We report the discovery of an ultra-faint dwarf in the constellation of Pegasus. Pegasus~V (Peg~V) was initially identified in the public imaging data release of the DESI Legacy Imaging Surveys and confirmed with deep imaging from Gemini/GMOS-N. The colour-magnitude diagram shows a sparse red giant branch (RGB) population and a strong over-density of blue horizontal branch stars. We measure a distance to Peg~V of $D=692^{+33}_{-31}$~kpc, making it a distant satellite of Andromeda with $M_V=-6.3\pm0.2$ and a half-light radius of $r_{\rm half}=89\pm41$~pc. It is located $\sim260$~kpc from Andromeda in the outskirts of its halo. The RGB is well-fit by a metal-poor isochrone with [Fe/H]$=-3.2$, suggesting it is very metal poor. This, combined with its blue horizontal branch could imply that it is a reionisation fossil. This is the first detection of an ultra-faint dwarf outside the deep Pan-Andromeda Archaeological Survey area, and points to a rich, faint satellite population in the outskirts of our nearest neighbour.
description: Submitted to MNRAS Letters. 6 pages, 4 figures. Comments welcome
The high energy spectrum of Proxima Centauri simultaneously observed at X-ray and FUV wavelengths
Creators: name: Fuhrmeister, B.
name: Zisik, A.
name: Schneider, P. C.
name: Robrade, J.
name: Schmitt, J. H. M. M.
name: Predehl, P.
name: Czesla, S.
name: France, K.
name: Muñoz, A. García
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: The M dwarf Proxima~Centauri is known to be magnetically active and it hosts a likely Earth-like planet in its habitable zone. Understanding the characteristics of stellar radiation by understanding the properties of the emitting plasma is of paramount importance for a proper assessment of the conditions on Proxima~Centauri~b and exoplanets around M dwarfs in general. We determine the temperature structure of the coronal and transition region plasma of Proxima Centauri from simultaneous X-ray and far-ultraviolet (FUV) observations. The differential emission measure distribution (DEM) was constructed for flaring and quiescent periods by analysing optically thin X-ray and FUV emission lines. Four X-ray observations of Proxima Centauri were conducted by the LETGS instrument on board of the Chandra X-ray Observatory and four FUV observations were carried out using the Hubble STIS spectrograph. From the X-ray light curves, we determined a variation of the quiescent count rate by a factor of two within 20\% of the stellar rotation period. To obtain the DEM, 18 optically thin emission lines were analysed (12 X-ray and six FUV). The flare fluxes differ from the quiescence fluxes by factors of 4-20 (FUV) and 1-30 (X-ray). The temperature structure of the stellar corona and transition region was determined for both the quiescence and flaring state by fitting the DEM(T) with Chebyshev polynomials for a temperature range $\log$T = 4.25 - 8. Compared to quiescence, the emission measure increases during flares for temperatures below 0.3\,MK (FUV dominated region) and beyond 3.6\,MK (X-ray dominated region). The reconstructed DEM shape provides acceptable line flux predictions compared to the measured values. We provide synthetic spectra at 1-1700 Å, which may be considered as representative for the high-energy irradiation of Proxima~Cen~b during quiescent and flare periods.
description: 12 pages, 11 figures, accepted to A&A
Evidence to Action (E2A) Framework: A Participatory Approach to Action Learning
Creators: name: Dam, Jennifer
name: Butcher, Stephanie
name: Das, Joyati
name: Fattah, Kazi
name: Hausmann, Susanna
Publisher: name: University of Melbourne
Year: 2021
Subjects: Urban and regional economics

description: The E2A Framework is a tool that proposes essential elements and methodologies through which Fondation Botnar and their program partners can frame and operationalise a formal learning agenda at an organisational and program level. It also provides guidance on integrating an evidence building plan, including a learning and evaluation strategy across programs.
Submission to the National Disability Strategy: Beyond 2020 Stage 2 Consultations
Creators: name: Davy, Laura
name: KAVANAGH, ANNE
name: DICKINSON, HELEN
name: Llewellyn, Gwynnyth
name: CAREY, GEMMA
name: PETRIE, DENNIS
name: BUTTERWORTH, PETER
name: Smith-Merry, Jennifer
name: BADLAND, HANNAH
name: Stancliffe, Roger
Publisher: name: University of Melbourne
Year: 2021
Subjects: Welfare, insurance, disability and social security law
Public policy
Social policy

description: This submission was led by Dr Laura Davy on behalf of investigators within the Centre of Research Excellence in Disability and Health (CRE-DH) funded by the National Health and Medical Research Council, in October 2020
The Centre of Research Excellence in Disability and Health (CRE-DH) aims to identify cost-effective policies to improve the health of people with disabilities in Australia.
Given the majority stakeholder view that the vision and outcome areas of the current National Disability Strategy are still the right ones, this submission focuses on the implementation and governance of the next iteration of the Strategy.
The submission addresses the following three areas:
1. Leadership of people with disability

Facilitating the participation of people with disability and their representative organisations in the development and implementation of law and policy that impacts them is an obligation under Article 4 of the United Nations Convention on the Rights of Persons with Disabilities (CRPD). People with disability must be represented in all aspects of the Strategy’s governance structures and agenda setting and decision-making processes.
2. Coordination of the Strategy

 Reviews of the current Strategy showed that it was not effectively implemented across all levels and portfolios of government. Outlining government responsibilities is not enough; the effective coordination of government responsibilities for implementing the Strategy by an appropriately resourced and representative agency or body is also necessary.
3. Quality data collection and reporting

Collecting quality data to inform policy development and implementation is an obligation under Article 31 of the CRPD. Funding will need to be allocated to developing suitable national data frameworks and to the oversight, collection and analysis of this data. The CRE-DH has developed the Disability and Wellbeing Monitoring Framework to measure and track inequalities between people with and without disability in relation to the social determinants of health and wellbeing which may be a valuable input to the development of a monitoring framework for the next Strategy.

Further information
www.credh.org.au
Submission to the National Disability Strategy: Beyond 2020
Creators: name: Davy, Laura
name: KAVANAGH, ANNE
name: DICKINSON, HELEN
name: Llewellyn, Gwynnyth
name: CAREY, GEMMA
name: PETRIE, DENNIS
name: BUTTERWORTH, PETER
name: Smith-Merry, Jennifer
name: BADLAND, HANNAH
name: Stancliffe, Roger
Publisher: name: University of Melbourne
Year: 2021
Subjects: Welfare, insurance, disability and social security law
Public policy
Social policy

description: This submission is made on behalf of investigators within the Centre of Research Excellence in Disability and Health (CRE-DH) funded by the National Health and Medical Research Council.
The Centre of Research Excellence in Disability and Health(CRE-DH) aims to identify cost-effective policies to improvethe health of people with disabilities in Australia.Given the majority stakeholder view that the vision and outcome areas of the current National Disability Strategy are still the right ones, this submission focuses on the implementation and governance of the next iteration of the Strategy. The submission addresses in particular the following three areas:
1. Leadership of people with disability
Facilitating the participation of people with disability and their representative organisations in the development and implementation of law and policy that impacts them is an obligation under Article 4 of the United Nations Convention on the Rights of Persons with Disabilities (CRPD). People with disability must be represented in all aspects of the Strategy’s governance structures and agenda setting and decision-making processes.
2. Coordination of the Strategy Reviews of the current Strategy showed that it was not effectively implemented across all levels and portfolios of government. Outlining government responsibilities is not enough; the effective coordination of government responsibilities for implementing the Strategy by an appropriately resourced and representative agency or body is also necessary.
3. Quality data collection and reporting Collecting quality data to inform policy development and implementation is an obligation under Article 31 of the CRPD. Funding will need to be allocated to developing suitable national data frameworks and to the oversight, collection and analysis of this data. The CRE-DH has developed the Disability and Wellbeing Monitoring Framework to measure and track inequalities between people with and without disability in relation to the social determinants of health and wellbeing which may be a valuable input to the development of a monitoring framework for the next Strategy.

www.credh.org.au
Long Term X-Ray Spectral Variation of the Wolf-Rayet Binary WR 102-1 in the Galactic bulge: evidence for wind distortion in the binary
Creators: name: Nagatsuka, Tomoki
name: Sugawara, Yasuharu
name: Ebisawa, Ken
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: WR~102-1 was detected by Suzaku as a conspicuous point source in the 6.7 keV intensity map of the central region of the Milky Way. The source was suggested as a possible Wolf-Rayet binary based on its X-ray and infrared spectral characteristics. The iron line emission is expected to originate in the Wolf-Rayet star's dynamic stellar-wind when colliding the companion's mild stellar wind. Here, we report the result of a long-term X-ray monitoring of WR~102-1 since 1998 using archival data of ASCA, XMM-Newton, Chandra, Suzaku, and Swift to reveal variations of the iron K-emission line and the circumstellar absorption. Consequently, we have detected significant redshifts of the iron K-emission line from the XMM-Newton observation in March 2003 and the Suzaku observation in September 2006. Furthermore, when the red-shift was observed, which suggests that the Wolf-Rayet star was in front of the companion star, the circumstellar absorption values were smaller than other periods. These results appear contrary to the expectation if the Wolf-Rayet's stellar wind is spherically symmetric, but may be understood if the Wolf-Rayet star's stellar wind is significantly distorted due to the rapid orbital motion near the periastron.
description: 6 pages, 4 figures