Search

We use the photometric metallicities provided by the panoramic Pristine survey to study the veracity and derive the metallicities of the numerous stellar streams found by the application of the STREAMFINDER algorithm to the Gaia EDR3 data. All 26 streams present in Pristine show a clear metallicity distribution function, which provides an independent check of the reality of these structures, supporting the reliability of STREAMFINDER in finding streams and the power of Pristine to measure precise metallicities. We further present 6 candidate structures with coherent phase-space and metallicity signals that are very likely streams. The majority of studied streams are very metal-poor (14 structures with [Fe/H], 25 pages, 29 figures, accepted for publication in MNRAS. Updated version has only minor changes compared to initial submission. The metallicity of most streams have marginally changed in the updated version

WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366$-$959\,nm at $R\sim5000$, or two shorter ranges at $R\sim20\,000$. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for $\sim$3 million stars and detailed abundances for $\sim1.5$ million brighter field and open-cluster stars; (ii) survey $\sim0.4$ million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey $\sim400$ neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in $z1$ million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at $z>2$. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator., 41 pages, 27 figures, accepted for publication by MNRAS

Although diffuse interstellar bands (DIBs) were discovered over 100 years ago, for most of them, their origins are still unknown. Investigation on the correlations between different DIBs is an important way to study the behavior and distributions of their carriers. Based on stacking thousands of spectra from the Pristine Inner Galaxy Survey, we study the correlations between two DIBs at 442.8 nm ($\lambda$442.8) and 862.1 nm ($\lambda$862.1), as well as the dust grains, in a range of latitude spanning ${\sim}22^{\circ}$ ($4^{\circ}\,{}\,0.3$ mag. For $|b|\,{>}\,12^{\circ}$, $\lambda$442.8 and $\lambda$862.1 present larger relative strength with respect to the dust grains. A systematic variation of the relative strength between $\lambda$442.8 and $\lambda$862.1 with $|b|$ and $E(B-V)$ concludes that the two DIBs do not share a common carrier. Furthermore, the carrier of $\lambda$862.1 is more abundant at high latitudes than that of $\lambda$442.8. This work can be treated as an example showing the significance and potentials to the DIB research covering a large latitude range., Comment: 13 pages, 14 figures, accepted for publication in MNRAS

Following the idea originally proposed during the ESO-Workshop The Very Large Telescope in 2030, the concept of a high resolution spectrograph for the VLT has been further explored, both for the science and technological aspects. Such an instrument will fill a gap in capabilities amongst the landscape of future instrumentation planned for the next decade. Its key characteristic will be high spectral resolution (R = 60000-80000) with multi-object (50-100) capabilities and, possibly, a stability that would provide high radial velocity precision (∼10m/s). In this work, we describe the science cases and driving science requirements for the instrument. Furthermore we will present some design solutions and technical options considered to meet these requirements.

PURPOSE Major adverse cardiac events (MACEs) because of immune checkpoint inhibitors (ICIs) are infrequent immune-related adverse events (irAEs) that comprise a spectrum of cardiac toxicities with variable manifestations. ICI-related MACEs can lead to significant morbidity and mortality, hence the need to better define presentations of MACEs and their association with noncardiac irAEs in ICI-treated patients. METHODS We conducted a retrospective pooled analysis of MACE captured in the serious adverse events reporting database of the National Cancer Institute–Cancer Therapy Evaluation Program for National Cancer Institute–sponsored investigational clinical trials between June 2015 and December 2019. Patients were eligible if they had been treated with anti–programmed cell death protein-1 (anti–PD-1)/programmed cell death-ligand 1 (anti–PD-L1) alone or with additional anticancer therapies. RESULTS A total of 6,925 participants received anti–PD-(L)1-based therapies; 48% (n = 3,354) were treated with single-agent anti–PD-(L)1 therapy. Of 6,925 patients, 0.6% (n = 40) qualified as ICI-related MACE, with 77.5% (n = 31 of 40) being ≥ grade 3. Myocarditis accounted for 45% (n = 18 of 40) of total ICI-MACEs. Concurrent multisystem involvement with other noncardiac irAEs was seen in 65% (n = 26 of 40). Most patients with myocarditis (83%, n = 15 of 18) had one or more noncardiac irAEs associated. Incidence of MACE was higher with anti–PD-(L)1 + targeted therapies compared with anti–PD-(L)1 + anti–cytotoxic T-cell lymphocyte-4 combinations (2.1% v 0.9%, P = .08). There was a higher incidence of myocarditis with anti–PD-(L)1-based combination therapies versus single-agent anti–PD-(L)1 therapies (0.36%, n = 13 of 3,571 v 0.15%, n = 5 of 3,354, P = .08). Deaths related to myocarditis were identified in 22.5% (n = 4 of 18). All four patients who died had concurrent myositis. CONCLUSION Increasing patient and prescriber awareness in understanding patterns of ICI-MACE and associated noncardiac irAEs should be emphasized. Better characterization of the risk of MACE with the concurrent use of non–ICI-based anticancer therapies with anti–PD-(L)1 treatments is needed.

Stellar ejecta gradually enrich the gas out of which subsequent stars form, making the least chemically enriched stellar systems direct fossils of structures formed in the early universe. Although a few hundred stars with metal content below one thousandth of the solar iron content are known in the Galaxy, none of them inhabit globular clusters, some of the oldest known stellar structures. These show metal content of at least ~0.2 percent of the solar metallicity ([Fe/H] > -2.7). This metallicity floor appears universal and it has been proposed that proto-galaxies that merge into the galaxies we observe today were simply not massive enough to form clusters that survived to the present day. Here, we report the discovery of a stellar stream, C-19, whose metallicity is less than 0.05 per cent the solar metallicity ([Fe/H]=-3.38 +/- 0.06 (stat.) +/- 0.20 (syst.)). The low metallicity dispersion and the chemical abundances of the C-19 stars show that this stream is the tidal remnant of the most metal-poor globular cluster ever discovered, and significantly below the purported metallicity floor: clusters with significantly lower metallicities than observed today existed in the past and contributed their stars to the Milky Way halo., 14 pages, 6 figures, 5 tables. Nature, accepted

We present a search for disturbed, candidate ram pressure stripping galaxies across more than 50 spectroscopically selected SDSS groups and clusters. Forty-eight ram pressure candidates are visually identified in these systems using high quality UNIONS imaging from the Canada-France Hawaii Telescope, covering ~6200 and ~2800 square degrees in the u- and r-bands respectively. Ram pressure candidates are found in groups and clusters spanning a wide range in halo mass and include ~30 ram pressure candidates in the group regime ($M_h < 10^{14}$). The observed frequency of ram pressure candidates shows substantial scatter with group/cluster mass, but on average is larger in clusters ($M_h > 10^{14}\,M_\odot$) than groups ($M_h < 10^{14}\,M_\odot$) by a factor of ~2. We find that ram pressure candidates are most commonly low-mass galaxies and have enhanced star formation rates relative to star-forming field galaxies. The enhancement in star formation is largely independent of galaxy mass and strongest for galaxies in clusters. As a result of the large survey footprint and excellent image quality from UNIONS, we are able to identify disturbed galaxies, potentially affected by ram pressure stripping, across a wide range of host environment., 12 pages, 9 figures, 1 appendix, accepted for publication in MNRAS

We evaluate the rotational velocity of stars observed by the Pristine survey towards the Galactic anticentre, spanning a wide range of metallicities from the extremely metal-poor regime ($\mathrm{[Fe/H]} -1.5$. Furthermore, we detect signatures of a "heated disc", the so-called Splash, at metallicities higher than $\sim-1.5$. Finally, at $\mathrm{[Fe/H]} < -1.5$ our anticentre sample is dominated by a kinematical halo with a net prograde motion., Comment: 18 pages, 14 figures. Accepted for publication in MNRAS

Background Hospice staff encounter distress, physical and psychological pain every day (Pauly, Varcoe, Storch, 2012). Schwartz Centre Rounds (SCR) promote compassionate care and its link to patient experience (Point of Care Foundation). But who cares for the carer? SCR provide space for reflection, and shared experiences (Cullen, 2012) and during COVID-19 this is more vital than ever (Newcomb, 2021); our hospice Schwartz Steering Group was keen to continue SCR online to support colleagues. ‘Reflection helps manage our responses and lives can be enhanced by cultivating compassion in our practice’ (Sanso, Galiana, Oliver et al., 2015). Aims Launch and sustain virtual monthly SCR for staff/volunteers to reflect and connect. Obtain feedback on virtual format through survey. Identify future SCR topics. Help decision making with SCR future facilitation. Methods Steering group identified members confident in video-conferencing, producing supporting guidance for members. Discussion topics identified through feedback. Staff/volunteer speakers approached by steering group member; subsequent briefing discussion and format explanation. Brief online survey emailed to participants. Results 36 members of staff responded to the survey: 55% clinical, 45% non-clinical staff. What participants like about Schwartz: Sense of community/connection. Non-judgmental space. Understanding others’ roles. Aiding own reflection. Learning from others’ views. 19 answered ‘what could be done differently?’ Ten people (from the total of 19) responded to say that they didn’t think anything could be done differently. Themes identified were: Varying date/time to accommodate different working patterns. Taking advance questions. Return to physical meetings for easier interaction, especially before session. Some commented how well an online platform worked, making it accessible to participants offsite. Ideas for future topics: understanding roles; COVID-19’s impact; coping with stress. Conclusion Online SCR transition was largely positively received. Overarching aim to allow people space to reflect, discuss challenging clinical scenarios and receive support. Despite anxiety about ability to connect emotionally remotely, the feedback showed sense of community and non-judgemental space for reflection was not compromised in a potentially isolating time. We aim to alternate face-to-face and remote SCR to improve access for staff/volunteers.

Although true metal-free "Population III" stars have so-far escaped discovery, their nature, and that of their supernovae, is revealed in the chemical products left behind in the next generations of stars. Here we report the detection of an ultra-metal poor star in the Sculptor dwarf spheroidal galaxy, AS0039. With [Fe/H]$_{\rm LTE}=-4.11$, it is the most metal-poor star so far discovered in any external galaxy. Contrary to the majority of Milky Way stars at this metallicity, AS0039 is clearly not enhanced in carbon, with [C/Fe]$_{\rm LTE}=-0.75$ and A(C)=+3.60, making it the lowest detected carbon abundance in any star to date. It furthermore lacks $\alpha$-element uniformity, having extremely low [Mg/Ca]$_{\rm NLTE}=-0.60$ and [Mg/Ti]$_{\rm NLTE}=-0.86$, in stark contrast with the near solar ratios observed in C-normal stars within the Milky Way halo. The unique abundance pattern indicates that AS0039 formed out of material that was predominantly enriched by a $\sim$20$ M_\odot$ progenitor star with an unusually high explosion energy $E=10\times10^{51}$ erg. The star AS0039 is thus one of the first observational evidence for zero-metallicity hypernovae and provides a unique opportunity to investigate the diverse nature of Population III stars., Comment: Accepted in ApJL, 7 pages, 3 figures, 1 table, and an appendix (1 figure and 3 tables)

The most metal-deficient stars hold important clues about the early build-up and chemical evolution of the Milky Way, and carbon-enhanced metal-poor (CEMP) stars are of special interest. However, little is known about CEMP stars in the Galactic bulge. In this paper, we use the large spectroscopic sample of metal-poor stars from the Pristine Inner Galaxy Survey (PIGS) to identify CEMP stars ([C/Fe] > +0.7) in the bulge region and to derive a CEMP fraction. We identify 96 new CEMP stars in the inner Galaxy, of which 62 are very metal-poor ([Fe/H] < -2.0); this is more than a ten-fold increase compared to the seven previously known bulge CEMP stars. The cumulative fraction of CEMP stars in PIGS is $42^{\,+14\,}_{\,-13} \%$ for stars with [Fe/H] < -3.0, and decreases to $16^{\,+3\,}_{\,-3} \%$ for [Fe/H] < -2.5 and $5.7^{\,+0.6\,}_{\,-0.5} \%$ for [Fe/H] < -2.0. The PIGS inner Galaxy CEMP fraction for [Fe/H] < -3.0 is consistent with the halo fraction found in the literature, but at higher metallicities the PIGS fraction is substantially lower. While this can partly be attributed to a photometric selection bias, such bias is unlikely to fully explain the low CEMP fraction at higher metallicities. Considering the typical carbon excesses and metallicity ranges for halo CEMP-s and CEMP-no stars, our results point to a possible deficiency of both CEMP-s and CEMP-no stars (especially the more metal-rich) in the inner Galaxy. The former is potentially related to a difference in the binary fraction, whereas the latter may be the result of a fast chemical enrichment in the early building blocks of the inner Galaxy., 15 pages, 9 figures, accepted for publication in MNRAS

Objectives To update the American Academy of Pediatrics and Society of Critical Care Medicine's 2004 Guidelines and levels of care for PICU. Design A task force was appointed by the American College of Critical Care Medicine to follow a standardized and systematic review of the literature using an evidence-based approach. The 2004 Admission, Discharge and Triage Guidelines served as the starting point, and searches in Medline (Ovid), Embase (Ovid), and PubMed resulted in 329 articles published from 2004 to 2016. Only 21 pediatric studies evaluating outcomes related to pediatric level of care, specialized PICU, patient volume, or personnel. Of these, 13 studies were large retrospective registry data analyses, six small single-center studies, and two multicenter survey analyses. Limited high-quality evidence was found, and therefore, a modified Delphi process was used. Liaisons from the American Academy of Pediatrics were included in the panel representing critical care, surgical, and hospital medicine expertise for the development of this practice guidance. The title was amended to "practice statement" and "guidance" because Grading of Recommendations, Assessment, Development, and Evaluation methodology was not possible in this administrative work and to align with requirements put forth by the American Academy of Pediatrics. Methods The panel consisted of two groups: a voting group and a writing group. The panel used an iterative collaborative approach to formulate statements on the basis of the literature review and common practice of the pediatric critical care bedside experts and administrators on the task force. Statements were then formulated and presented via an online anonymous voting tool to a voting group using a three-cycle interactive forecasting Delphi method. With each cycle of voting, statements were refined on the basis of votes received and on comments. Voting was conducted between the months of January 2017 and March 2017. The consensus was deemed achieved once 80% or higher scores from the voting group were recorded on any given statement or where there was consensus upon review of comments provided by voters. The Voting Panel was required to vote in all three forecasting events for the final evaluation of the data and inclusion in this work. The writing panel developed admission recommendations by level of care on the basis of voting results. Results The panel voted on 30 statements, five of which were multicomponent statements addressing characteristics specific to PICU level of care including team structure, technology, education and training, academic pursuits, and indications for transfer to tertiary or quaternary PICU. Of the remaining 25 statements, 17 reached consensus cutoff score. Following a review of the Delphi results and consensus, the recommendations were written. Conclusions This practice statement and level of care guidance manuscript addresses important specifications for each PICU level of care, including the team structure and resources, technology and equipment, education and training, quality metrics, admission and discharge criteria, and indications for transfer to a higher level of care. The sparse high-quality evidence led the panel to use a modified Delphi process to seek expert opinion to develop consensus-based recommendations where gaps in the evidence exist. Despite this limitation, the members of the Task Force believe that these recommendations will provide guidance to practitioners in making informed decisions regarding pediatric admission or transfer to the appropriate level of care to achieve best outcomes.

Millennials are a powerful workforce group and are quickly becoming established business leaders, consumers, and investors. Yet, millennials are often described as a uniformly homogeneous generation, despite mounting evidence of variances across their private and workplace behaviors, attitudes and preferences, and personal values. This article examines the personal value orientations of millennials in the Unites States, reporting consistencies, variations, and contrasts based on a large sample drawn from seven diverse universities. Results of this article suggest more similarities across a national population of millennials than differences, suggesting a national identity among American millennials. Practical implications of our findings and future research are discussed.

Knowledge of the ages of the stars formed over a galaxy's lifetime is fundamental to an understanding of its formation and evolution. However, stellar ages are difficult to obtain since they cannot be measured from observations, but require comparison with stellar models1. Alternatively, age distributions can be derived by applying the robust technique of colour-magnitude diagram fitting2, which until now has been used primarily to study nearby galaxies. Accurate distances to individual Milky Way stars now provided by the Gaia spacecraft mission3 have allowed us to derive ages from a thick-disk colour-magnitude diagram and from the two-sequenced colour-magnitude diagram of the kinematically hot local halo4, whose blue sequence has been linked to a major accretion event, Gaia-Enceladus5,6. Because accurate stellar ages were lacking, the time of the merger and its role in our Galaxy's early evolution remained unclear. Here we show that the stars in both halo sequences share identical age distributions, and are older than most of the thick-disk stars. The sharp halo age distribution cutoff at ten billion years ago can be identified with the time of accretion of Gaia-Enceladus to the Milky Way. Together with state-of-the-art cosmological simulations of galaxy formation7, these robust ages allow us to order the early sequence of events that shaped our Galaxy. We identify the red-sequence stars as the first stars formed within the Milky Way progenitor, and their kinematics indicate that these stars constitute the long-sought in situ halo of the Milky Way.

2668 Background: Immune checkpoint inhibitors (CPI) are known to rarely cause new onset diabetes (CPI DM). While rare, this adverse event is quite challenging for patients and clinicians to manage. Therefore, it is important to identify risk factors and clinical characteristics. This is the first comprehensive, multi-institutional study of CPI-DM across multiple agents and cancer types. Methods: The NCI Cancer Therapy Program (CTEP) database of adverse events (AEs) was queried for AEs related to diabetes (Grade 3 or 4 hyperglycemia, Acidosis including Diabetic Ketoacidosis (DKA), glucose intolerance and diabetes mellitus) among 6,925 patients who had been treated with a PD-(L)1 inhibitor alone or in combination from 6/2015 to 12/2019. Each AE report was reviewed and classified as due to CPI DM, new onset type 2 diabetes mellitus (T2DM), T2DM exacerbation without medication non-compliance, existing DM with medication non-compliance, or association with steroids (SDM). CPI DM was diagnosed based on: evidence of insulin deficiency either through presentation in DKA or low c-peptide with need for long term basal bolus insulin to maintain euglycemia and/or positive islet autoantibodies. Results: In total, there were 82 cases with at least one of these AEs; 41 had CPI-DM, 22 had SDM, 1 had new T2DM, 4 had T2DM exacerbation, 3 had medication noncompliance and 11 had acidosis not attributable to diabetes or had insufficient data. After excluding non-hyperglycemic acidosis, 57.8% had CPI-DM. Furthermore, if not on steroids and in good compliance with diabetes medications, 89.1% had CPI-DM. The incidence of CPI-DM was 0.59%; it was most common on combination PD-1/CTLA-4 inhibitor therapy (0.85%, 15/1767), followed by PD-(L)1 inhibitor monotherapy (0.54%, 18/3354), followed by CPIs combined with additional agents including chemotherapy and targeted agents (0.44%, 8/1804)(p = 0.25). Hospitalization was required for 87.5% of CPI-DM cases with 74.3% of those requiring an inpatient endocrine consult. All but one CPI-DM case had an endocrine consult at as either an inpatient or outpatient. Conclusions: While rare, this cohort shows the large health care burden of CPI-DM and that any hyperglycemia, and especially marked hyperglycemia, should be treated as CPI-DM until proven otherwise. [Table: see text]

2508 Background: MACE due to ICIs are infrequent immune-related adverse events (irAEs) that comprise a spectrum of cardiac toxicities with variable manifestations. ICI-related MACE can lead to significant morbidity and mortality, hence the need to better define presentations of MACE and their association with non-cardiac irAEs in ICI-treated patients. Methods: We conducted a retrospective pooled analysis of MACE captured in the serious adverse events reporting database of the NCI-CTEP for NCI-sponsored investigational clinical trials between 6/2015-12/2019. Patients (pts) were eligible if they had been treated with anti-programmed cell death protein-1/programmed death-ligand 1 (anti-PD-[L]1) alone or in combination with additional anti-cancer therapies. Results: A total of 6,925 pts received anti-PD-(L)1-based therapies; 48% (n = 3354) were treated with single-agent anti-PD-(L)1 therapy. Of 6925 pts, 0.6% (n = 40) qualified as ICI-related MACE. Myocarditis accounted for 45% (n = 18/40) of total ICI-MACE. Approximately 77.5% (n = 31/40) of MACE were ≥ grade 3. Multi-system organ involvement with other non-cardiac irAEs was seen in 65% (n = 26/40). Most pts with myocarditis (83%, n = 15/18) had one or more non-cardiac irAEs associated; non-cardiac irAEs were observed in 50% (n = 11/22) of non-myocarditis MACE. Incidence of MACE was higher with anti-PD-(L)1 + targeted therapies vs. anti-PD-(L)1 + anti-CTLA-4 (2.1% vs. 0.09%, p = 0.08). Most of these were non-myocarditis MACE. There was a significantly higher incidence of myocarditis with anti-PD-(L)1-based combinations vs. single-agent anti-PD-(L)1 therapies (0.39%, n = 13/3341 vs. 0.14%, n = 5/3566, p = 0.04. Most pts with myocarditis had been treated with anti-PD-1-based combinations (72%, n = 13/18); the most common combination being anti-PD1+ anti-CTLA-4 (92%, n = 12/13). Pts with myocarditis presented after a median of 2 ICI doses and after a median of 35 days from the initial ICI administration. In pts with myocarditis, a concurrent or preceding history of myositis was present in 53% (n = 8/15). Deaths related to myocarditis were identified in 22.5% (n = 4/18). All four patients who died had concurrent myositis, with three having concurrent transaminitis. Conclusions: Our results represent the first report of a comprehensive pooled analysis of ICI-MACE obtained from NCI CTEP-sponsored investigational clinical trials. Based on our results, increasing patient and prescriber awareness in understanding patterns of ICI-MACE and associated non-cardiac irAEs should be emphasized. Furthermore, better characterization of the risk and patterns of non-myocarditis MACE with the use of anti-PD(L)-1 ICIs concurrently with non-ICI-based anti-cancer therapies is needed.

Introduction Bedtime procrastination, the volitional delay of going to bed without any external circumstances causing the delay, is associated with poor sleep outcomes. Alleviating bedtime procrastination is an important target for interventions to promote adequate sleep, yet the social cognitive, biological, and behavioural determinants of bedtime procrastination are poorly understood. The present study aimed to conduct a systematic review, narrative synthesis, and meta-analysis of (1) the underlying determinants of bedtime procrastination, and (2) the strength and direction of the relationship between bedtime procrastination and sleep outcomes. Methods A database search was conducted through CINAHL, EMBASE, PsychINFO, PubMed, Scopus and Web of Science, using keywords related to procrastination, delay, bedtime and sleep. Results A total of 2087 records were identified, and 38 publications met the inclusion criteria. Random-effects meta-analysis for bedtime procrastination and sleep outcomes is ongoing. Preliminary findings suggest self-regulation, self-control and chronotype are the most prominent determinants. Conclusion Future research should expand focus to identify a broader range of determinants. Given that there are multiple benefits to a theory-based approach to behaviour change interventions, further research exploring determinants will be able to guide the development of interventions targeting bedtime procrastination. Support (If Any)

The early Universe presented a star formation environment that was almost devoid of heavy elements. The lowest metallicity stars thus provide a unique window into the earliest Galactic stages, but are exceedingly rare and difficult to find. Here we present the discovery of an ultra-metal-poor star, Pristine_221.8781+9.7844, using narrow-band Ca H&K photometry from the Pristine survey. Follow-up medium and high-resolution spectroscopy confirms the ultra-metal-poor nature of Pristine_221.8781+9.7844 ([Fe/H] = -4.66 +/- 0.13 in 1D LTE) with an enhancement of 0.3-0.4 dex in alpha-elements relative to Fe, and an unusually low carbon abundance. We derive an upper limit of A(C) = 5.6, well below typical A(C) values for such ultra metal-poor stars. This makes Pristine_221.8781+9.7844 one of the most metal-poor stars; in fact, it is very similar to the most metal-poor star known (SDSS J102915+172927). The existence of a class of ultra metal-poor stars with low(er) carbon abundances suggest that there must have been several formation channels in the early Universe through which long-lived, low-mass stars were formed., Re-submitted to MNRAS after minor revisions

International audience; We present an update on the overall integration progress of the WEAVE next-generation spectroscopy facility for the William Herschel Telescope (WHT), now scheduled for first light in early-2021, with almost all components now arrived at the observatory. We also present a summary of the current planning behind the 5-year initial phase of survey operations, and some detailed end-to-end science simulations that have been implemented to evaluate the final on-sky performance after data processing. WEAVE will provide optical ground-based follow up of ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2-degree prime focus field of view at the WHT, with a buffered pick-and-place positioner system hosting 1000 multi-object (MOS) fibres, 20 mini integral field units, or a single large IFU for each observation. The fibres are fed to a single (dual-beam) spectrograph, with total of 16k spectral pixels, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R~5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R~20000.

Elemental abundances of the most metal-poor stars reflect the conditions in the early Galaxy and the properties of the first stars. We present a spectroscopic follow-up of two ultra metal-poor stars ([Fe/H], Comment: 17 pages, 11 figures, accepted for publication in MNRAS

We present the high-resolution spectroscopic analysis of two new extremely metal-poor stars (EMPS) candidates in the dwarf spheroidal galaxy Sextans. These targets were pre-selected from medium resolution spectra centered around the Ca II triplet in the near-infrared and followed-up at higher resolution with VLT/UVES. We confirm their low metallicities with [Fe/H]=-2.95 and [Fe/H]=-3.01, placing them among the most metal-poor stars known in Sextans. The abundances of 18 elements, including C, Na, the alpha-elements, Fe-peak, and neutron capture elements, are determined. In particular, we present the first measurements of Zn in a classical dwarf at extremely low metallicity. There has been previous hints of a large scatter in the abundance ratios of the Sextans stellar population around [Fe/H] -3 when compared to other galaxies. We took the opportunity of this work to re-analyse the full sample of EMPS and find a Milky-Way -like plateau and a normal dispersion at fixed metallicity., Accepted for publication in A&A. 14 pages, 10 figures

Context: The accretion history of the Milky Way is still unknown, despite the recent discovery of stellar systems that stand out in terms of their energy-angular momentum space, such as Gaia-Enceladus-Sausage. In particular, it is still unclear how these groups are linked and to what extent they are well-mixed. Aims: We investigate the similarities and differences in the properties between the prograde and retrograde (counter-rotating) stars and set those results in context by using the properties of Gaia-Enceladus-Sausage, Thamnos/Sequoia, and other suggested accreted populations. Methods: We used the stellar metallicities of the major large spectroscopic surveys (APOGEE, Gaia-ESO, GALAH, LAMOST, RAVE, SEGUE) in combination with astrometric and photometric data from Gaia's second data-release. We investigated the presence of radial and vertical metallicity gradients as well as the possible correlations between the azimuthal velocity, $v_\phi,$ and metallicity, [M/H], as qualitative indicators of the presence of mixed populations. Results: We find that a handful of super metal-rich stars exist on retrograde orbits at various distances from the Galactic center and the Galactic plane. We also find that the counter-rotating stars appear to be a well-mixed population, exhibiting radial and vertical metallicity gradients on the order of $\sim$ -0.04 dex/kpc and -0.06 dex/kpc, respectively, with little (if any) variation when different regions of the Galaxy are probed. The prograde stars show a $v_\phi$-[M/H] relation that flattens -- and, perhaps, even reverses as a function of distance from the plane. Retrograde samples selected to roughly probe Thamnos and Gaia-Enceladus-Sausage appear to be different populations yet they also appear to be quite linked, as they follow the same trend in terms of the eccentricity versus metallicity space., Comment: 16 pages, accepted for publication in A&A

We use the second Gaia data release to dissect the Milky Way disc in phase-space and relative ages. We confirm and report the existence of multiple velocity moving groups at low azimuthal velocities and angular momenta, below Arcturus, regularly separated by ∼18−20 km s−1 in azimuthal velocity. Such features were predicted to exist more than ten years ago, based on the reaction of the Milky Way to a perturbation in the disc undergoing phase-mixing. These structures appear slightly younger than their phase-space surroundings and reach up to high (solar) metallicities, which argues against an extra-galactic origin. We also identify, in terms of relative age, many of the classical ridges in the plane of azimuthal velocity versus Galactocentric radius, which are traditionally associated with resonance features. These ridges are also younger than their phase-space surroundings in accordance with predictions from recent state-of-the-art cosmological hydrodynamical simulations of Milky Way-like galaxies. We study the response of dynamically young and old stellar disc populations to resonances from an analytic model of a large bar which, remarkably, reproduces qualitatively the trends seen in the data for the classical ridges close to circularity. Our results reinforce the idea that the Galactic disc is being shaped by both internal and external perturbations, along with the fact that while absolute isochrone ages have to be taken with great care, exploring the dynamical structure of the disc in stellar ages, especially with future asteroseismic data, will provide much stronger constraints than metallicity and abundance trends alone.

The Milky Way bulge is an important tracer of the early formation and chemical enrichment of the Galaxy. The abundances of different iron-peak elements in field bulge stars can give information on the nucleosynthesis processes that took place in the earliest supernovae. Cobalt (Z=27) and copper (Z=29) are particularly interesting.We aim to identify the nucleosynthesis processes responsible for the formation of the iron-peak elements Co and Cu. Methods. We derived abundances of the iron-peak elements cobalt and copper in 56 bulge giants, 13 of which were red clump stars. High-resolution spectra were obtained using FLAMES-UVES at the ESO Very Large Telescope by our group in 2000-2002, which appears to be the highest quality sample of high-resolution data on bulge red giants obtained in the literature to date. Over the years we have derived the abundances of C, N, O, Na, Al, Mg; the iron-group elements Mn and Zn; and neutron-capture elements. In the present work we derive abundances of the iron-peak elements cobalt and copper. We also compute chemodynamical evolution models to interpret the observed behaviour of these elements as a function of iron. The sample stars show mean values of [Co/Fe]~0.0 at all metallicities, and [Cu/Fe]~0.0 for [Fe/H]>-0.8 and decreasing towards lower metallicities with a behaviour of a secondary element. We conclude that [Co/Fe] varies in lockstep with [Fe/H], which indicates that it should be produced in the alpha-rich freezeout mechanism in massive stars. Instead [Cu/Fe] follows the behaviour of a secondary element towards lower metallicities, indicating its production in the weak s-process nucleosynthesis in He-burning and later stages. The chemodynamical models presented here confirm the behaviour of these two elements (i.e. [Co/Fe] vs. [Fe/H]~constant and [Cu/Fe] decreasing with decreasing metallicities)., Accepted to Astronomy & Astrophysics

Metal-poor stars are important tools for tracing the early history of the Milky Way, and for learning about the first generations of stars. Simulations suggest that the oldest metal-poor stars are to be found in the inner Galaxy. Typical bulge surveys, however, lack low metallicity ([Fe/H] < -1.0) stars because the inner Galaxy is predominantly metal-rich. The aim of the Pristine Inner Galaxy Survey (PIGS) is to study the metal-poor and very metal-poor (VMP, [Fe/H] < -2.0) stars in this region. In PIGS, metal-poor targets for spectroscopic follow-up are selected from metallicity-sensitive CaHK photometry from the CFHT. This work presents the ~250 deg^2 photometric survey as well as intermediate-resolution spectroscopic follow-up observations for ~8000 stars using AAOmega on the AAT. The spectra are analysed using two independent tools: ULySS with an empirical spectral library, and FERRE with a library of synthetic spectra. The comparison between the two methods enables a robust determination of the stellar parameters and their uncertainties. We present a sample of 1300 VMP stars -- the largest sample of VMP stars in the inner Galaxy to date. Additionally, our spectroscopic dataset includes ~1700 horizontal branch stars, which are useful metal-poor standard candles. We furthermore show that PIGS photometry selects VMP stars with unprecedented efficiency: 86%/80% (lower/higher extinction) of the best candidates satisfy [Fe/H] < -2.0, as do 80%/63% of a larger, less strictly selected sample. We discuss future applications of this unique dataset that will further our understanding of the chemical and dynamical evolution of the innermost regions of our Galaxy., accepted for publication in MNRAS, 17 pages, 9 figures

A chemo-dynamical analysis of 115 metal-poor candidate stars selected from the narrow-band Pristine photometric survey is presented based on CFHT high-resolution ESPaDOnS spectroscopy. We have discovered 28 new bright (V < 15) stars with [Fe/H] < −2.5 and 5 with [Fe/H] < −3.0 for success rates of 40 (28/70) and 19 per cent (5/27), respectively. A detailed model atmosphere analysis is carried out for the 28 new metal-poor stars. Stellar parameters were determined from SDSS photometric colours, Gaia DR2 parallaxes, MESA/MIST stellar isochrones, and the initial Pristine survey metallicities, following a Bayesian inference method. Chemical abundances are determined for 10 elements (Na, Mg, Ca, Sc, Ti, Cr, Fe, Ni, Y, and Ba). Most stars show chemical abundance patterns that are similar to the normal metal-poor stars in the Galactic halo; however, we also report the discoveries of a new r-process-rich star, a new CEMP-s candidate with [Y/Ba] > 0, and a metal-poor star with very low [Mg/Fe]. The kinematics and orbits for all of the highly probable metal-poor candidates are determined by combining our precision radial velocities with Gaia DR2 proper motions. Some stars show unusual kinematics for their chemistries, including planar orbits, unbound orbits, and highly elliptical orbits that plunge deeply into the Galactic bulge (Rperi < 0.5 kpc); also, eight stars have orbital energies and actions consistent with the Gaia-Enceladus accretion event. This paper contributes to our understanding of the complex chemo-dynamics of the metal-poor Galaxy, and increases the number of known bright metal-poor stars available for detailed nucleosynthetic studies.

This is an erratum to the paper ‘The Pristine survey – VI. The first three years of medium-resolution follow-up spectroscopy of Pristine EMP star candidates’ (2019, MNRAS, 490, 2241–2253). In the original version of this paper, the author Rafael Garcia-Dias was incorrectly listed. This has now been corrected and the author’s apologise for the error.

The Pristine survey uses narrow-band photometry to derive precise metallicities down to the extremely metal-poor regime ([Fe/H] < -3), and currently consists of over 4 million FGK-type stars over a sky area of $\sim 2~500\, \mathrm{deg}^2$. We focus our analysis on a subsample of $\sim 80~000$ main sequence turnoff stars with heliocentric distances between 6 and 20 kpc, which we take to be a representative sample of the inner halo. The resulting metallicity distribution function (MDF) has a peak at [Fe/H] = -1.6, and a slope of $��$(LogN)/$��[Fe/H] = 1.0 \pm 0.1$ in the metallicity range of -3.4 < [Fe/H] < -2.5. This agrees well with a simple closed-box chemical enrichment model in this range, but is shallower than previous spectroscopic MDFs presented in the literature, suggesting that there may be a larger proportion of metal-poor stars in the inner halo than previously reported. We identify the Monoceros/TriAnd/ACS/EBS/A13 structure in metallicity space in a low latitude field in the anticenter direction, and also discuss the possibility that the inner halo is dominated by a single, large merger event, but cannot strongly support or refute this idea with the current data. Finally, based on the MDF of field stars, we estimate the number of expected metal-poor globular clusters in the Milky Way halo to be 5.4 for [Fe/H] < -2.5 and 1.5 for [Fe/H] < -3, suggesting that the lack of low metallicity globular clusters in the Milky Way is not due simply to statistical undersampling., 17 pages, 12 figures, 5 tables, accepted for publication in MNRAS

Our Galaxy is known to contain a central boxy/peanut-shaped bulge, yet the importance of a classical, pressure-supported component within the central part of the Milky Way is still being debated. It should be most visible at low metallicity, a regime that has not yet been studied in detail. Using metallicity-sensitive narrow-band photometry, the Pristine Inner Galaxy Survey (PIGS) has collected a large sample of metal-poor ([Fe/H] < -1.0) stars in the inner Galaxy to address this open question. We use PIGS to trace the metal-poor inner Galaxy kinematics as function of metallicity for the first time. We find that the rotational signal decreases with decreasing [Fe/H], until it becomes negligible for the most metal-poor stars. Additionally, the velocity dispersion increases with decreasing metallicity for -3.0 < [Fe/H] < -0.5, with a gradient of -44 $\pm$ 4 km$\,$s$^{-1}\,$dex$^{-1}$. These observations may signal a transition between Galactic components of different metallicities and kinematics, a different mapping onto the boxy/peanut-shaped bulge for former disk stars of different metallicities and/or the secular dynamical and gravitational influence of the bar on the pressure-supported component. Our results provide strong constraints on models that attempt to explain the properties of the inner Galaxy., 5 pages + appendices, accepted to MNRAS Letters

The orbits of the least chemically enriched stars open a window on the formation of our Galaxy when it was still in its infancy. The common picture is that these low-metallicity stars are distributed as an isotropic, pressure-supported component since these stars were either accreted from the early building blocks of the assembling Milky Way, or were later brought by the accretion of faint dwarf galaxies. Combining the metallicities and radial velocities from the Pristine and LAMOST surveys and Gaia DR2 parallaxes and proper motions for an unprecedented large and unbiased sample of very metal-poor stars at $[Fe/H]\leq-2.5$ we show that this picture is incomplete. This sample shows strong statistical evidence (at the $5.0\sigma$ level) of asymmetry in their kinematics, favouring prograde motion. Moreover, we find that $31\%$ of the stars that currently reside in the disk do not venture outside of the disk plane throughout their orbit. The discovery of this population implies that a significant fraction of stars with iron abundances $[Fe/H]\leq-2.5$ formed within or concurrently with the Milky Way disk and that the history of the disk was quiet enough to allow them to retain their disk-like orbital properties., Comment: Submitted to MNRAS letter, 5 pages with 1 figure. Appendices A and B with 3 figures

The aim of this study was to describe the variation in antibiotic prescribing practices for uncomplicated community-acquired pneumonia across the continuum of care for hospitalized pediatric patients to better inform future efforts at standardizing antibiotic therapy throughout a single hospitalization. This is a retrospective cohort study involving 4 hospitals caring for children aged 3 months to 18 years, hospitalized between January 1, 2011, and December 31, 2012, with diagnosis of uncomplicated pneumonia and without complex chronic medical conditions. Data collected include antibiotics prescribed before hospitalization, at the emergency department (ED) encounter, during hospitalization, and at hospital discharge. Six hundred nine children met inclusion criteria, with a mean age of 5.3 years and median length of stay of 2 days. Emergency department providers prescribed narrow-spectrum therapy 27% of the time, whereas discharging providers prescribed narrow-spectrum therapy 56% of the time. Third- and fourth-generation cephalosporins were less often prescribed in the preadmission setting and at discharge but were more often prescribed in the ED and inpatient setting. There was an association between inpatient prescription of broad-spectrum antibiotics when a blood culture was obtained, when broad-spectrum antibiotics were prescribed in the ED, and with increasing length of stay. Broad-spectrum antibiotic therapy for community-acquired pneumonia, especially third- and fourth-generation cephalosporins, often originates in the ED. When initiated in this setting, it is likely to be continued in the inpatient setting.

We present detailed chemical abundances for 99 red-giant branch stars in the centre of the Sculptor dwarf spheroidal galaxy, obtained from high-resolution VLT/FLAMES spectroscopy. This includes abundances of Li (detected in 1 out of 99 stars), Na, $\alpha$-elements (O, Mg, Si, Ca Ti), iron-peak elements (Sc, Cr, Fe, Co, Ni, Zn), r- and s-process elements (Ba, La, Nd, Eu). The sample, covering -2.3< [Fe/H], Comment: Accepted for publication in A&A, 21 pages, 16 figures, +Appendix (in total 34 pages)

We present the analysis of the FLAMES dataset targeting the central 25 arcmin region of the Sextans dSph. This dataset is the third major part of the high resolution spectroscopic section of the ESO large program 171.B-0588(A) obtained by the Dwarf galaxy Abundances and Radial-velocities Team (DART). Our sample is composed of red giant branch stars down to the level of the horizontal branch in Sextans. It allows to address questions related to both stellar nucleosynthesis and galaxy evolution. We provide metallicities for 81 stars, which cover the wide [Fe/H]=$-$3.2 to $-$1.5 dex range. The abundances of 10 other elements are derived: Mg, Ca, Ti, Sc, Cr, Mn, Co, Ni, Ba, and Eu. Despite its small mass, Sextans is a chemically evolved system, with evidence for the contribution of core-collapse and Type Ia supernovae as well as low metallicity AGBs. This new FLAMES sample offers a sufficiently large number of stars with chemical abundances derived at high accuracy to firmly establish the existence of a plateau in [$\alpha$/Fe] at $\sim 0.4$ dex, followed by a decrease above [Fe/H]$\sim-2$ dex. This is in stark similarity with the Fornax and Sculptor dSphs despite their very different masses and star formation histories. This suggests that these three galaxies had very similar star formation efficiencies in their early formation phases, probably driven by the early accretion of smaller galactic fragments, until the UV-background heating impacted them in different ways. The parallel between the Sculptor and Sextans dSph is also striking when considering Ba and Eu. Finally, as to the iron-peak elements, the decline of [Co/Fe] and [Ni/Fe] above [Fe/H]$\sim -2$ implies that the production yields of Ni and Co in SNeIa is lower than that of Fe. The decrease in [Ni/Fe] favours models of SNeIa based on the explosion of double degenerate sub-Chandrasekhar mass white dwarfs., Comment: Accepted for publication in A&A. All tables included

Using Gaia DR2, we trace the Anticenter Stream (ACS) in various stellar populations across the sky and find that it is kinematically and spatially decoupled from the Monoceros Ring. Using stars from {\sc lamost} and {\sc segue}, we show that the ACS is systematically more metal-poor than Monoceros by $0.1$ dex with indications of a narrower metallicity spread. Furthermore, the ACS is predominantly populated of old stars ($\sim 10\,\rm{Gyr}$), whereas Monoceros has a pronounced tail of younger stars ($6-10\, \rm{Gyr}$) as revealed by their cumulative age distributions. Put togehter, all of this evidence support predictions from simulations of the interaction of the Sagittarius dwarf with the Milky Way, which argue that the Anticenter Stream (ACS) is the remains of a tidal tail of the Galaxy excited during Sgr's first pericentric passage after it crossed the virial radius, whereas Monoceros consists of the composite stellar populations excited during the more extended phases of the interaction. We suggest that the ACS can be used to constrain the Galactic potential, particularly its flattening, setting strong limits on the existence of a dark disc. Importantly, the ACS can be viewed as a stand-alone fossil of the chemical enrichment history of the Galactic disc., Comment: 6 pages, 6 Figure, submitted to MNRAS, comments welcome

The technique of color-magnitude diagram (CMD) fitting is a well recognized method that has been used for over 20 years to determine detailed star formation histories (SFH) for Local Group galaxies (Gallart et al. 2005; Tolstoy et al. 2009). The accurate distances for large stellar samples provided in Gaia DR2, together with the precise, homogeneous Gaia photometry, is enabling for the first time to apply the CMD-fitting technique to the different morphological components of our own Galaxy and to robustly derive their SFHs and age distributions using only the Gaia photometric information of millions of stars. This provides answers to long lasting questions regarding the formation and evolution of the disk and halo components of the Milky Way, for which the determination of stellar ages was necessary. In this presentation we discuss two examples resulting from our ongoing work. 1. Thanks to the CMD fitting method, a SFH profile across the Galactic disk has been obtained for the first time: we have constructed CMDs and computed SFHs for a number of layers parallel to the Milky Way plane, at different heights up to Z=2 Kpc above and below the plane, and close to the solar radius. We call these SFHs 'dynamically evolved SFHs' because the stellar sample present in each volume is potentially affected by stellar migration and blurring. Several epochs of enhanced star formation (~10, 6 and 2 ago) can be observed close to the plane, up to |Z| ~ 400 pc. At larger distances from the plane, the younger star forming epochs gradually diminish their relative strength. This results in a smooth change in the SFR(t) as a function of height |Z|, with mean age increasing with |Z|. The distinct epoch of star formation between 13 and 8 Gyr ago may correspond to the formation of the thick disk. 2. The CMD of the kinematically selected Milky Way halo population published from Gaia DR2 data (Babusiaux et al. 2018) showed two enigmatic sequences running parallel in color from the main sequence to the sub-giant and red-giant branch, indicating the presence of two distinct subpopulations. The blue sequence has been associated with a major accretion event experienced by the Milky Way early in its history (Helmi et al. 2018; Haywood et al. 2018), while the red sequence has been associated with the thick disk (Haywood et al. 2018) by the similarity in chemical composition. We have derived age distributions for the two halo sequences and for a thick disk stellar sample. The age distributions clearly demonstrate that the two sequences in the halo CMD are composed by stars that are coeval and formed at the earliest possible times in the life of the Universe. The difference in color is a result of the red and blue sequence stars having different metallicities. The inferred age distributions also clearly show that the thick disc population includes a stellar population that is younger than the two halo populations. These results, allow us to tightly constrain that the merger occurred 10 Gyr ago, and to conclude that the red sequence is composed by stars formed in the Milky Way during its first ~ 3 Gyr of evolution, right before the merger with Gaia-Enceladus took place, and heated to halo-like kinematics by the impact. The associated infalling gas would have contributed to maintain and stoke star formation in the early disk up to a second epoch of maximum inferred intensity 9.5 Gyr ago. &nbsp

IntroductionThe notion of identity has shaped the behavior of individuals throughout the course of time, and is "arguably more fundamental to the conception of humanity than any other notion" (Gioia, 1998, p. 17). Theories of identity and social identity suggest that individual behavior is regulated by a sense of who one perceives oneself to be and the memberships in various groups one perceives important. As noted by Ashforth and Mael (1989), a referent organization may provide the answer to an individual's question of "Who am I?" Multiple scholars have offered definitions of organizational identification to explain the association individuals have with their respective organizations. Even though these definitions may differ to some extent, it is broadly agreed that organizational identification demands some sort of deep association between the individual and an organization, in which the individual recognizes him- or herself as sharing communal attributes with a specific group or organization (Ashforth and Mael, 1989; Dutton, Dukerich and Harquail, 1994; Pratt, 1998).Extant research explicates one specific basis for individual identity that is of particular interest here, one's moral identity. Moral identity has been conceptualized as a "set of common moral traits likely to be central to most people's moral self-definition" (Aquino and Reed, 2002, p. 1424). In particular, the importance of one's moral identity to one's self concept has been linked to inter-group relations (Aquino, Ray, and Reed, 2003), charitable giving (Reynolds and Ceranic, 2007) and truth-telling (Aquino, Ray and Reed, 2003), as well as higher levels of moral engagement (Detert, Trevino and Sweitzer, 2008). Research has also shown that the relationship between one's moral identity and behavior in specific circumstances is not fixed and immutable (Appiah, 2008). Behavior contrary to a person's self-concept can be triggered by external factors such as ambient sounds or smells and internal conditions such as fatigue (Appiah, 2008), conditions that threaten safety and security (Narvaez, 2008), the behaviors of others (Haidt, 2007; Haidt and Bjorkland, 2008a, b) and the "frame" or context within which one conceptualizes the circumstances or situation (Tenbrunsel and Messick, 2004; Tennbrunsel and Smith Crowe, 2008).In addition to literature on the concept of individual moral identity, researchers have begun to address the notion of organizational moral identity. Although prior works have investigated congruence in terms of fit and identification in organizations (Haslam, 2001; Hatch and Schultz, 1997, 2000, 2002), organizational research has not explicitly explored congruence in terms of moral identity. Here, we suggest that this congruence or incongruence will affect productive behaviors such as citizenship behaviors as well as counterproductive behaviors such as organizational deviance in organizations. Perhaps more importantly, we argue that specific "types" of congruence and incongruence will likely impact these behaviors in unique ways. Thus, our paper has the potential to advance scholar-practitioners' understanding of: (1) how individual moral identity and organizational moral identity interact to predict important outcomes, and (2) how congruence and incongruence between the individual and the organization will impact behavioral outcomes related to organizational citizenship behavior and deviant behavior in organizations.In the sections that follow, we first review the definition and theoretical background of individual moral identity and extend the concept of moral identity to the organizational level. Then we examine the concepts of moral identity congruence/incongruence and delineate the different types of congruence/incongruence, linking each of these to specific types of productive and counterproductive behaviors through propositions that detail these expected relationships.Moral identityWe define ethics or morality (terms we will use interchangeably) as the values, rules, principles, obligations and concerns that allow individuals and organizations to interact in complicated societies and pursue their individual and common purposes while respecting the purposes of others. …

Abundances of the volatile elements S and Zn have now been measured in around 80 individual stars in the Sculptor dwarf spheroidal galaxy, covering the metallicity range $-2.4\leq\text{[Fe/H]}\leq-0.9$. These two elements are of particular interest as they are not depleted onto dust in gas, and their ratio, [S/Zn], has thus commonly been used as a proxy for [$\alpha$/Fe] in Damped Lyman-$\alpha$ systems. The S abundances in Sculptor are similar to other $\alpha$-elements in this galaxy, consistent with S being mainly created in core-collapse supernovae, but also having some contribution from supernovae Type Ia. However, our results show that Zn and Fe do not trace all the same nucleosynthetic production channels. In particular, (contrary to Fe) Zn is not significantly produced by supernovae Type Ia. Thus, [S/Zn] cannot be reliably used as a proxy for [$\alpha$/Fe]. We propose [O/S] as a function of [S/H] as a possible alternative. At higher metallicities, the values of [S/Zn] measured in Damped Lyman-$\alpha$ systems are inconsistent with those in local dwarf galaxies, and are more compatible with the Milky Way disk. Low-metallicity Damped Lyman-$\alpha$ systems are, however, consistent with the most metal-poor stars in Local Group dwarf spheroidal galaxies. Assuming that the dust depletions of S and Zn are negligible, our comparison indicates that the star formation histories of Damped Lyman-$\alpha$ systems are on average different from both the Milky Way and the Sculptor dwarf spheroidal galaxy., Comment: Accepted for publication in A&A

International audience; We present an update on the overall construction progress of the WEAVE next-generation spectroscopy facility for the William Herschel Telescope (WHT), now that all the major fabrication contracts are in place. We also present a summary of the current planning behind the 5-year initial phase of survey operations, and some detailed end-to-end science simulations that have been effected to evaluate the final on-sky performance after data processing. WEAVE will provide optical ground-based follow up of ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2-degree prime focus field of view at the WHT, with a buffered pick-and-place positioner system hosting 1000 multi-object (MOS) fibres, 20 integral field units, or a single large IFU for each observation. The fibres are fed to a single (dual-beam) spectrograph, with total of 16k spectral pixels, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R 5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R 20000. The project has experienced some delays in procurement and now has first light expected for the middle of 2019.

Despite the huge amount of photometric and spectroscopic efforts targetting the Galactic bulge over the past few years, its age distribution remains controversial owing to both the complexity of determining the age of individual stars and the difficult observing conditions. Taking advantage of the recent release of very deep, proper-motion-cleaned colour--magnitude diagrams (CMDs) of four low reddening windows obtained with the Hubble Space Telescope (HST), we used the CMD-fitting technique to calculate the star formation history (SFH) of the bulge at -2deg > b > -4deg along the minor axis. We find that over 80 percent of the stars formed before 8 Gyr ago, but that a significant fraction of the super-solar metallicity stars are younger than this age. Considering only the stars that are within reach of the current generation of spectrographs (i.e. V < 21), we find that 10 percent of the bulge stars are younger than 5 Gyr, while this fraction rises to 20-25 percent in the metal-rich peak. The age-metallicity relation is well parametrized by a linear fit implying an enrichment rate of dZ/dt ~ 0.005 Gyr$^{-1}$. Our metallicity distribution function accurately reproduces that observed by several spectroscopic surveys of Baade's window, with the bulk of stars having metal-content in the range [Fe/H] ~ -0.7 to ~0.6, along with a sparse tail to much lower metallicities., MNRAS, in press (accepted March 27th, 2018)

Oxygen and zinc in the Galactic bulge are key elements for the understanding of the bulge chemical evolution. Oxygen-to-iron abundance ratios provide a most robust indicator of the star formation rate and chemical evolution of the bulge. Zinc is enhanced in metal-poor stars, behaving as an $\alpha$-element, and its production may require nucleosynthesis in hypernovae. Most of the neutral gas at high redshift is in damped Lyman-alpha systems (DLAs), where Zn is also observed to behave as an alpha-element. The aim of this work is the derivation of the alpha-element oxygen, together with nitrogen, and the iron-peak element zinc abundances in 417 bulge giants, from moderate resolution (R~22,000) FLAMES-GIRAFFE spectra. For stars in common with a set of UVES spectra with higher resolution (R~45,000), the data are intercompared. The results are compared with literature data and chemodynamical models., Comment: accepted on 21/02/2018

The purpose of this chapter is to examine the proliferation of scientific management and then to consider its effect on business and society. Our examination begins with a brief survey of various management approaches that emerged in the early twentieth century. We focus on Frederick Taylor, the originator of scientific management, as the person with the greatest influence on management scholarship. We assert that the propagation of scientific management in all sectors of business and society is so pervasive that is it ubiquitous, making it exceedingly difficult to consciously detect or question. We examine how core ideas from scientific management have facilitated the dehumanization of stakeholders in management scholarship and practice. We then discuss how dehumanizing tendencies — informed by the hidden ubiquity of scientific management — have permeated research in corporate social responsibility and management theory. We conclude with suggestions for integrating humanity into management theory.

Context. There have been conflicting results with respect to the extent that radial migration has played in the evolution of the Galaxy. Additionally, observations of the solar neighborhood have shown evidence of a merger in the past history of the Milky Way that drives enhanced radial migration. Aims. We attempt to determine the relative fraction of stars that have undergone significant radial migration by studying the orbital properties of metal-rich ([Fe/H] > 0.1) stars within 2 kpc of the Sun. We also aim to investigate the kinematic properties, such as velocity dispersion and orbital parameters, of stellar populations near the Sun as a function of [Mg/Fe] and [Fe/H], which could show evidence of a major merger in the past history of the Milky Way. Methods. We used a sample of more than 3000 stars selected from the fourth internal data release of the Gaia-ESO Survey. We used the stellar parameters from the Gaia-ESO Survey along with proper motions from PPMXL to determine distances, kinematics, and orbital properties for these stars to analyze the chemodynamic properties of stellar populations near the Sun. Results. Analyzing the kinematics of the most metal-rich stars ([Fe/H] > 0.1), we find that more than half have small eccentricities (e< 0.2) or are on nearly circular orbits. Slightly more than 20% of the metal-rich stars have perigalacticons R> 7 kpc. We find that the highest [Mg/Fe], metal-poor populations have lower vertical and radial velocity dispersions compared to lower [Mg/Fe] populations of similar metallicity by ~10 km s. The median eccentricity increases linearly with [Mg/Fe] across all metallicities, while the perigalacticon decreases with increasing [Mg/Fe] for all metallicities. Finally, the most [Mg/Fe]-rich stars are found to have significant asymmetric drift and rotate more than 40 km s slower than stars with lower [Mg/Fe] ratios. Conclusions. While our results cannot constrain how far stars have migrated, we propose that migration processes are likely to have played an important role in the evolution of the Milky Way, with metal-rich stars migrating from the inner disk toward to solar neighborhood and past mergers potentially driving enhanced migration of older stellar populations in the disk.© ESO, 2018., The authors thank Ivan Minchev for a useful discussion and the anonymous referee for useful comments. M.R.H. and A.R.B. received financial support from ANR, reference 14-CE33-0014-01. S.F. and T.B. acknowledge support from the project grant >The New Milky Way> from the Knut and Alice Wallenberg Foundation. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell' Istruzione, dell' Universita' e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and NASA's Astrophysics Data System.

We revisited barium abundance in a sample of giant stars in the dwarf spheroidal Fornax galaxy. Non-local thermodynamic equilibrium (NLTE) synthesis was used to derive the barium abundance from two Ba II lines. Our new NLTE result for barium shows that in the range of metallicities from -1 to -0.5 the abundance of this element is almost the same as in the stars of the Milky Way. We conclude that the evolution of barium abundance in the dSph Fornax galaxy resembles that of the Milky Way at the epoch of the corresponding metallicity level., Comment: 5 pages, 2 figures

We report an abundance analysis for the highly r-process-enhanced (r-II) star CS 29497-004, a very metal-poor giant with Teff = 5013K and [Fe/H]=-2.85, whose nature was initially discovered in the course of the HERES project. Our analysis is based on high signal-to-noise, high-resolution (R~75000) VLT/UVES spectra and MARCS model atmospheres under the assumption of local thermodynamic equilibrium, and obtains abundance measurements for a total of 46 elements, 31 of which are neutron-capture elements. As is the case for the other 25 r-II stars currently known, the heavy-element abundance pattern of CS 29497-004 well-matches a scaled Solar System second peak r-process-element abundance pattern. We confirm our previous detection of Th, and demonstrate that this star does not exhibit an "actinide boost". Uranium is also detected (log e(U) =-2.20+/-0.30), albeit with a large measurement error that hampers its use as a precision cosmo-chronometer. Combining the various elemental chronometer pairs that are available for this star, we derive a mean age of 12.2+/-3.7 Gyr using the theoretical production ratios from waiting-point approximation models (Kratz et al. 2007). We further explore the high-entropy wind model (Farouqi et al. 2010) production ratios arising from different neutron richness of the ejecta (Y_e), and derive an age of 13.7+/-4.4 Gyr for a best-fitting Y_e=0.447. The U/Th nuclei-chronometer is confirmed to be the most resilient to theoretical production ratios and yields an age of 16.5+:-6.6 Gyr. Lead (Pb) is also tentatively detected in CS 29497-004, at a level compatible with a scaled Solar r-process, or with the theoretical expectations for a pure r-process in this star., Comment: 24 pages, 15 figures, accepted in Astronomy and Astrophysics

The Canada-France Imaging Survey (CFIS) will map the northern high Galactic latitude sky in the $u$-band ("CFIS-u", 10,000$\, {\rm deg^2}$) and in the $r$-band ("CFIS-r", 5,000$\, {\rm deg^2}$), enabling a host of stand-alone science investigations, and providing some of the ground-based data necessary for photometric redshift determination for the Euclid mission. In this first contribution we present the $u$-band component of the survey, describe the observational strategy, and discuss some first highlight results, based on approximately one third of the final area. We show that the Galactic anticenter structure is distributed continuously along the line of sight, out to beyond 20 kpc, and possesses a metallicity distribution that is essentially identical to that of the outer disk sampled by APOGEE. This suggests that it is probably a buckled disk of old metal-rich stars, rather than a stream or a flare. We also discuss the future potential for CFIS-u in discovering star-forming dwarf galaxies around the Local Group, the characterization of the white dwarf and blue straggler population of the Milky Way, as well as its sensitivity to low-surface brightness structures in external galaxies., 12 pages, 11 figures, accepted for publication in ApJ

From ESO VLT/FLAMES/GIRAFFE spectra, abundance measurements of Zn have been made in ≈100 individual red giant branch (RGB) stars in the Sculptor dwarf spheroidal galaxy. This is the largest sample of individual Zn abundance measurements within a stellar system beyond the Milky Way. In the observed metallicity range, -2.7 ≤ [Fe/H] ≤ -0.9, the general trend of Zn abundances in Sculptor is similar to that of α-elements. That is, super-solar abundance ratios of [Zn/Fe] at low metallicities, which decrease with increasing [Fe/H], eventually reaching subsolar values. However, at the higher metallicities in Sculptor, [Fe/H] ≳ -1.8, we find a significant scatter, -0.8 ≲ [Zn/Fe] ≲ +0.4, which is not seen in any α-element. Our results are consistent with previous observations of a limited number of stars in Sculptor and in other dwarf galaxies. These results suggest that zinc has a complex nucleosynthetic origin, behaving neither completely like an α- nor an iron-peak element. Based on observations made with ESO/VLT/FLAMES at the La Silla Paranal observatory under program ID 092.B-0194(A).Tables 2-4 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/606/A71

IAU Commission 29 - Stellar Spectra has been one of the IAU commissions from the onset, until its dissolution at the most recent IAU General Assembly in Honolulu in 2015. This commission belonged to IAU Division G (“Stars and Stellar Physics”), the latter committed with fostering research in stellar astrophysics. Within the general field of stellar astrophysics, stellar spectroscopy plays a key role, as stellar spectra are a powerful tool providing a view into the detailed physical properties of stars and the physical processes occuring within them.