bluuebunny/crossref_metadata_2025 huggingface dataset:
Ethics and Inequality: A Strategic and Practical View
Authors: Galbraith James K.
Published: September 2016

Deng Xiaoping once said, “Let some get rich first, the others will follow.” This is Angus Deaton's basic view in The Great Escape. Deaton, co-winner of the Leontief Prize in 2014 and winner of the Nobel Prize in 2015, chronicles the rise of almost all of humanity out of conditions of widespread hunger, disease, destitution, and premature death, and into a world where infant and child mortality has fallen sharply, and where heart diseases and even cancers are declining. Consequently, with exceptions related to AIDS and in the poorest countries, life overall is longer and health better than ever before.
Climate Contributions and the Paris Agreement: Fairness and Equity in a Bottom-Up Architecture
Authors: Chan Nicholas
Published: September 2016

One of the chief aspects of last December's landmark Paris Agreement on climate change was the acceptance of the notion that all states would make a “contribution” to the global effort to address climate change. These voluntary, nationally determined, non-binding pledges are the most visible feature of the reorientation of the international climate regime away from its previous emphasis on “top-down” international coordination, and toward a “bottom-up” architecture that provides greater national flexibility in order to induce broader participation. At the same time, however, the agreement to keep the rise in average global temperatures to below 2 degrees Celsius indicates that there is a limit to the quantity of carbon that can be emitted to meet this temperature goal, raising the challenge of how to apportion this carbon “budget” among states. Can a fair distribution of the carbon budget be achieved amid voluntary contributions? This paper first discusses the tension between the top-down distribution that a carbon budget approach generally implies, and the bottom-up institutional elements of the new climate architecture. Second, it reviews the alternative ways in which considerations of fairness have been integrated into the design of the Paris Agreement, and the rise of “national circumstances” as the context for fairness. Finally, this paper points to the increased role for normative argumentation in this bottom-up world, where new norms embedded in the Paris Agreement, especially relating to increases in national ambition, take on greater importance in efforts to achieve an equitable response to climate change.
Self-Interest and the Distant Vulnerable
Authors: Glanville Luke
Published: September 2016

What interests do states have in assisting and protecting vulnerable populations beyond their borders? While some political leaders and commentators promote a circumscribed understanding of the national interest that rules out accepting substantial risks and costs for the sake of the distant vulnerable, others endorse an “enlightened” conception of the national interest that recognizes the long-term utility to be gained by helping them. However, while this notion of “enlightened” self-interest gives states reason to act in some instances, it fails to prompt action in other cases where the suffering of strangers is less strategically important. Some leaders and commentators have responded to this problem by reaching for some other, less material conception of the national interest to justify assisting the distant vulnerable, but they have often struggled to find the language they need. This article finds a solution in the debates about self-interest waged in seventeenth-century Europe. Dissatisfied both with Hobbes's narrow understanding of self-interest and Pufendorf's more “enlightened” understanding, Leibniz defended a more generous and “disinterested” conception, grounded not in considerations of material utility but in the pleasure to be derived from helping those in need. This article demonstrates two ways in which this “disinterested” conception of self-interest can be of use today. First, it provides resources for explaining why states already sometimes act in “disinterested” and altruistic ways. Second, it provides leaders with a tool for persuading people to help the distant vulnerable, even when it appears to be in neither their narrow nor their “enlightened” interests to do so.
Robots and Respect: A Response to Robert Sparrow
Authors: Jenkins Ryan , Purves Duncan
Published: September 2016

Robert Sparrow recently argued in this journal that several initially plausible arguments in favor of the deployment of autonomous weapon systems (AWS) in warfare are in fact flawed, and that the deployment of AWS faces a serious moral objection. Sparrow's argument against AWS relies on the claim that they are distinct from accepted weapons of war in that they either fail to transmit an attitude of respect for enemy combatants or, worse, they transmit an attitude of disrespect. In this reply we argue that this distinction between AWS and widely accepted weapons is illusory, and therefore cannot ground a moral difference between AWS and existing methods of waging war. We also suggest that if deploying conventional soldiers in a given situation would be permissible, but we could expect to cause fewer civilian casualties by instead deploying AWS, then it would be consistent with an intuitive understanding of respect to deploy AWS in this situation.
Atomic and Molecular Phases of the Interstellar Medium
Authors: Mac Low Mordecai-Mark
Published: September 2016

This review covers four current questions in the behavior of the atomic and molecular interstellar medium. These include whether the atomic gas originates primarily in cold streams or hot flows onto galaxies; what the filling factor of cold gas actually is in galactic regions observationally determined to be completely molecular; whether molecular hydrogen determines or merely traces star formation; and whether gravity or turbulence drives the dynamical motions observed in interstellar clouds, with implications on their star formation properties.
Molecules in Action: Extragalactic ISM at high resolution
Authors: Martín Sergio
Published: September 2016

During the last two decade, observations have shown the potential of molecular tracers to get insights into the physical processes taking place in the central regions of active galaxies. However, observations were severely limited by both sensitivity and resolution. This resulted also in a limited sample of bright enough galaxies where molecular species other than carbon monoxide could be observed. Current instruments like ALMA and the upcoming NOEMA are already changing our view of the extragalactic ISM molecular observations. In fact, it is now possible to study the physical properties of individual spatially resolved star forming GMCs in external galaxies, as well as resolving the physical structure of the ISM in the surroundings of AGNs at scales of a few parsecs. Here I quickly review some of the most recent observational studies in the nuclear regions of galaxies which are setting new standards in the ways we can study the extragalactic ISM properties.
Connecting the density structure of molecular clouds with star formation
Authors: Kainulainen Jouni
Published: September 2016

In the current paradigm of turbulence-regulated interstellar medium (ISM), star formation rates of entire galaxies are intricately linked to the density structure of the individual molecular clouds. This density structure is essentially encapsulated in the probability distribution function of volume densities (ρ-PDF), which directly affects the star formation rates predicted by analytic models. Contrasting its fundamental role, the ρ-PDF function has remained virtually unconstrained by observations. I describe in this contribution the recent progress in attaining observational constraints for the column density PDFs (N-PDFs) of molecular clouds that function as a proxy of the ρ-PDFs. Specifically, observational works point towards a universal correlation between the shape of the N-PDFs and star formation activity in molecular clouds. The correlation is in place from the scales of a parsec up to the scales of entire galaxies, making it a fundamental, global link between the ISM structure and star formation.
The role of interstellar filaments in regulating the star formation efficiency and shaping the initial mass function
Authors: Könyves Vera , André Philippe
Published: September 2016

Recent surveys at infrared and submillimeter wavelengths with the Spitzer and Herschel space observatories suggest that star formation in dense molecular gas is governed by essentially the same “laws” in nearby Galactic clouds and distant external galaxies. This raises the possibility of a unified picture for star formation in the Universe from individual-cloud scales to galaxy–wide scales. We summarize the star formation scenario favored by Herschel studies of the nearest molecular clouds of the Galaxy which point to the key role of the quasi-universal filamentary structure pervading the cold interstellar medium.
Molecular cloud fragmentation and core collapse
Authors: Basu Shantanu
Published: September 2016

I review some steps in the conversion of molecular cloud gas into stars and planets, with an emphasis in this presentation on the early stage molecular cloud fragmentation that leads to elongated filaments/ribbons. Magnetic fields can play a crucial role in all stages and need to be invoked particularly for early stage fragmentation as well as in late core collapse where it may control disk formation. I also review some elements of hydrodynamic modeling of disk evolution.
SCUBA2 observations of prestellar cores
Authors: Ward-Thompson Derek , Pattle Kate
Published: September 2016

We show data from the SCUBA2 camera on JCMT, of molecular clouds. We focus on starless cores within the clouds. We present data of the Taurus region and show how the environment is affecting some cores' appearance in this region. We compare the SCUBA2 data with Herschel data and discuss the sensitivity of SCUBA2 to surface brightness in the sub-millimetre. We show how this leads to its ability to pick out the densest cores at a given temperature. Hence SCUBA2 preferentially picks out gravitationally bound pre-stellar cores. We discuss the effects of the magnetic field, and how this lends support to a model for the formation and evolution of cores in filamentary molecular clouds.
Theory of Protostellar Disk Formation
Authors: Li Zhi-Yun , Krasnopolsky Ruben , Shang Hsien
Published: September 2016

How large, 100-AU scale, rotationally supported disks form around protostars remains unsettled, both observationally and theoretically. In this contribution, we discuss the theoretical difficulties with disk formation in the presence of a dynamically significant magnetic field and their possible resolutions. These difficulties are caused by the concentration of magnetic field lines close to the forming star by protostellar collapse, and the strong magnetic braking associated with the concentrated field. Possible resolutions include magnetic field-rotation axis misalignment, non-ideal MHD effects, and turbulence. The field-rotation misalignment has been shown to promote disk formation, especially when the field is relatively weak and the misalignment angle is relatively large. Non-ideal MHD effects can enable the formation of small disks at early times. How such disks grow at later times remains to be fully quantified. Turbulence has been found to enable disk formation in a number of simulations, but the exact reason for its beneficial effect is debated.
Star formation rates, laws, thresholds
Authors: Walch Stefanie
Published: September 2016

On scales of ≳ several hundred parsec, there are relatively well defined observed relations between the star formation rate surface density of a galaxy and its gas content. I present a short summary of the so-called ‘star formation laws’ and discuss the most established models to explain their origin. Nevertheless, none of the models can explain the offset of these relations, which requires a low star formation efficiency within the total and/or molecular gas. Stellar feedback is proposed to limit the star formation efficiency locally. I discuss the available feedback mechanisms and show recent simulation results on the evolution of the multi-phase interstellar medium under the influence of gravity, cooling, feedback-driven outflows and heating.
Molecular gas in galaxies: changing conditions from disks to starbursts
Authors: Wilson Christine D.
Published: September 2016

In understanding galaxy evolution, one central question is how star formation is regulated in galaxies. Changes in star formation rates are likely tied to changes in the interstellar medium, particularly the molecular gas which is the fuel for star formation. I will discuss our recent results which use data from the Herschel Space Observatory, the Atacama Large Millimeter/submillimeter Array, and other telescopes to determine the typical density, temperature, and surface density of the molecular gas in various nearby galaxies. Comparing the properties of molecular gas in starburst and other active galaxies with more quiescent spiral disks provides some clues as to how changes in the physical state of the gas, such as mean density, can lead to enhanced star formation rates.
Evolution of the ISM in main-sequence versus starburst galaxies: A motivation for molecular deep fields
Authors: Aravena Manuel
Published: September 2016

In the last decade, significant progress has been made to understand the evolution with redshift of star formation processes in galaxies. Its is now clear that the majority of galaxies at z<3 form a nearly linear correlation between their stellar mass and star formation rates and appear to create most of their stars in timescales of ~1 Gyr. At the highest luminosities, a significant fraction of galaxies deviate from this main-sequence, showing short duty cycles and thus producing most of their stars in a single burst of star formation within ~100 Myr, being likely driven by major merger activity. Despite the large luminosities of starbursts, main-sequence galaxies appear to dominate the star formation density of the Universe at its peak.

While progress has been impressive, a number of questions are still unanswered. In this paper, I briefly review our current observational understanding of this main-sequence vs starburst galaxy paradigm, and address how future observations will help us to have better insights into the fundamental properties of the interstellar medium of these galaxies. Finally, I show recent attempts to conduct molecular deep field observations and the motivation to perform molecular deep field spectroscopy with the Atacama Large Millimeter/submillimeter Array.
Theoretical considerations for star formation at low and high redshift
Authors: Elmegreen Bruce G.
Published: September 2016

Star formation processes in strongly self-gravitating cloud cores should be similar at all redshifts, forming single or multiple stars with a range of masses determined by local magneto-hydrodynamics and gravity. The formation processes for these cores, however, as well as their structures, temperatures, Mach numbers, etc., and the boundedness and mass distribution functions of the resulting stars, should depend on environment, as should the characteristic mass, density, and column density at which cloud self-gravity dominates other forces. Because the environments for high and low redshift star formation differ significantly, we expect the resulting gas to stellar conversion details to differ also. At high redshift, the universe is denser and more gas-rich, so the active parts of galaxies are denser and more gas rich too, leading to slightly shorter gas consumption timescales, higher cloud pressures, and denser, more massive, bound stellar clusters at the high mass end. With shorter consumption times corresponding to higher relative cosmic accretion rates, and with the resulting higher star formation rates and their higher feedback powers, the ISM has greater turbulent speeds relative to the rotation speeds, thicker gas disks, and larger cloud and star complex sizes at the characteristic Jeans length. The result is a more chaotic appearance at high redshift, bridging the morphology gap between today's quiescent spirals and today's major-mergers, with neither spiral nor major-merger processes actually in play at that time. The result is also a thick disk at early times, and after in-plane accretion from relatively large clump torques, a classical bulge. Today's disks are thinner, and torque-driven accretion is slower outside of inner barred regions. This paper reviews the basic processes involved with star formation in order to illustrate its evolution over time and environment.
Apparent brightness distribution of GRB host galaxies
Authors: Bagoly Zsolt , Rácz István I. , Balázs Lajos G. , Horváth István , Tóth L. Viktor
Published: September 2016

We studied the unbiased optical brightness distribution which was calculated from the survival analysis of host galaxies (HGs) data and its relationship with the Swift GRB data of the host galaxies observed by the Keck telescope. Based on the sample obtained from merging the Swift GRB table and the Keck optical data we also studied the dependence of this distribution on the GRB's data. Finally, we compared the HGs distribution with standard galaxies distribution of the DEEP2 redshift survey and checked the result with the VIPERS catalogue too.
The IMF-SFH connection in massive early-type galaxies
Authors: Ferreras I. , Weidner C. , Vazdekis A. , Barbera F. La
Published: September 2016

The stellar initial mass function (IMF) is one of the fundamental pillars in studies of stellar populations. It is the mass distribution of stars at birth, and it is traditionally assumed to be universal, adopting generic functions constrained by resolved (i.e. nearby) stellar populations (e.g., Salpeter 1955; Kroupa 2001; Chabrier 2003). However, for the vast majority of cases, stars are not resolved in galaxies. Therefore, the interpretation of the photo-spectroscopic observables is complicated by the many degeneracies present between the properties of the unresolved stellar populations, including IMF, age distribution, and chemical composition. The overall good match of the photometric and spectroscopic observations of galaxies with population synthesis models, adopting standard IMF choices, made this issue a relatively unimportant one for a number of years. However, improved models and observations have opened the door to constraints on the IMF in unresolved stellar populations via gravity-sensitive spectral features. At present, there is significant evidence of a non-universal IMF in early-type galaxies (ETGs), with a trend towards a dwarf-enriched distribution in the most massive systems (see, e.g., van Dokkum & Conroy 2010; Ferreras et al. 2013; La Barbera et al. 2013). Dynamical and strong-lensing constraints of the stellar M/L in similar systems give similar results, with heavier M/L in the most massive ETGs (see, e.g., Cappellari et al. 2012; Posacki et al. 2015). Although the interpretation of the results is still open to discussion (e.g., Smith 2014; La Barbera 2015), one should consider the consequences of such a bottom-heavy IMF in massive galaxies.
The WISE Census of Young Stellar Objects and Clusters in Canis Major
Authors: Fischer W. J. , Padgett D. L. , Stapelfeldt K. R.
Published: September 2016

The photometric data returned by WISE, the Wide-field Infrared Survey Explorer, can be used to search the sky for young stellar objects (YSOs) away from the molecular clouds studied in detail by Spitzer and Herschel. We present updated results for a 100 deg2 region centered on Canis Major, including a look at the clustering properties of YSOs in the region.
Dust Extinction toward SN 2014J in M82
Authors: Gao Jian , Jiang B. W. , Li Aigen
Published: September 2016

We derive the extinction toward SN 2014J, a Type Ia supernova in M82, as a function of wavelength from the far ultraviolet to the near infrared by modeling the observed color excesses in terms of a mixture of silicate and graphite. With Av ≈ 1.9 mag and RV ≈ 1.7-1.8, the derived extinction law differs substantially from those of the Galaxy and the Magellanic clouds.
Properties of the ISM in UV-luminous galaxies: clues from the low-redshift universe
Authors: Gonçalves Thiago S.
Published: September 2016

How is gas converted into stars across cosmic time? Observations of star-forming galaxies at high redshift indicate that the conditions of the interstellar medium (ISM) were remarkably distinct from typical spirals in the local universe. Nevertheless, these observations are biased towards objects brighter than L*, due to the large luminosity distances involved. Here I present a survey targeting the molecular gas in galaxies at low redshift (z ~ 0.2) with ISM conditions remarkably similar to those observed at earlier epochs, including high star formation rates and lower metallicities. CO observations performed with CARMA indicate that these galaxies follow the same star-formation law as local spirals and other galaxies at the same redshift, albeit at much higher densities. We also present recent results from our ALMA program studying galaxies down to 12 + log(O/H) ~ 8, and discuss the implications of these data to our understanding of the molecular gas reservoir and the conversion factor between CO luminosity and gas mass in environments that are simultaneously low in metal content and extremely dense.
SWAN: NGC 253's Nucleated Star Bursting Environment
Authors: Gorski Mark , Ott Jürgen , Meier David , Momjian Emmanuel , Walter Fabian , Rand Richard
Published: September 2016

We present the first results from SWAN: “Survey of Water and Ammonia in Nearby galaxies”. Nearby galaxies are conveniently located to probe molecular gas properties on scales of 10 to 200 pc, which are appropriate for the study of Giant Molecular Clouds (GMCs). The resolution of the Very Large Array in D and C configurations corresponds to a few 10s of parsecs in these galaxies. To advance studies of galaxy evolution it is paramount to understand how processes in the molecular Interstellar Medium(ISM) and star formation are linked on these scales. We have observed the metastable transitions of ammonia and the 22GHz water maser line in four nearby galaxies: NGC 253, IC 342, NGC 2146, and NGC 6946 using the VLA. These galaxies were chosen to span an order of magnitude in star formation rate, and a range of galactic ecosystems. We use the ammonia transitions to derive kinetic temperatures, which exposes the heating and cooling balance of the ISM. We then aim to relate these conditions to energetic feedback from star formation as indicated by water masers.

Currently, our analysis is focused on NGC 253. NGC 253 is a barred spiral starburst galaxy with a nucleated star formation rate (SFR) of ≈ 3M⊙ per year. We use a distance of 3.9Mpc for analysis. We have observed ammonia transitions (1,1) to (5,5) and the 22GHz water maser line with a resolution of ≈63pc. We have identified nine regions across the nucleated starburst for study. The ammonia (3,3) line appears to be masing in the centermost 200pc. We have identified two regions of water maser emission. The first region is a minor axis extension, about the center of the galaxy, and is very close to the outflow. By means of these measurements, we gain an understanding of the molecular ISM associated with the nucleated starburst environment in NGC 253.
Chemical Tracers of Pre-Brown Dwarf Cores Formed Through Turbulent Fragmentation
Authors: Holdship Jonathan , Viti Serena
Published: September 2016

A gas-grain time dependent chemical code, UCL_CHEM, has been used to investigate the possibility of using chemical tracers to differentiate between the possible formation mechanisms of brown dwarfs. We model the formation of a pre-brown dwarf core through turbulent fragmentation by following the depth-dependent chemistry in a molecular cloud through the step change in density associated with an isothermal shock and the subsequent freefall collapse once a bound core is produced. Trends in the fractional abundance of molecules commonly observed in star forming cores are then explored to find a diagnostic for identifying brown dwarf mass cores formed through turbulence. We find that the cores produced by our models would be bright in CO and NH3 but not in HCO+. This differentiates them from models using purely freefall collapse as such models produce cores that would have detectable transitions from all three molecules.
ALFALFA Hα Reveals How Galaxies Use Their Hi Fuel
Authors: Jaskot Anne , Oey Sally , Salzer John , Van Sistine Angie , Bell Eric , Haynes Martha
Published: September 2016

Atomic hydrogen traces the raw material from which molecular clouds and stars form. With 565 galaxies from the ALFALFA Hα survey, a statistically complete subset of the ALFALFA survey, we examine the processes that affect galaxies' abilities to access and consume their Hi gas. On galaxy-wide scales, Hi gas fractions correlate only weakly with instantaneous specific star formation rates (sSFRs) but tightly with galaxy color. We show that a connection between dust and Hi content, arising from the fundamental mass-metallicity-Hi relation, leads to this tight color correlation. We find that disk galaxies follow a relation between stellar surface density and Hi depletion time, consistent with a scenario in which higher mid-plane pressure leads to more efficient molecular cloud formation from Hi. In contrast, spheroids show no such trend. Starbursts, identified by Hα equivalent width, do not show enhanced Hi gas fractions relative to similar mass non-starburst galaxies. The starbursts' shorter Hi depletion times indicate more efficient consumption of Hi, and galaxy interactions drive this enhanced star formation efficiency in several starbursts. Interestingly, the most disturbed starbursts show greater enhancements in Hi gas fraction, which may indicate an excess of Hi at early merger stages. At low galaxy stellar masses, the triggering mechanism for starbursts is less clear; the high scatter in efficiency and sSFR among low-mass galaxies may result from periodic bursts. We find no evidence for depleted Hi reservoirs in starbursts, which suggests that galaxies may maintain sufficient Hi to fuel multiple starburst episodes.
Possible density dependent local variations in the IMF
Authors: Kavila Indulekha , George Babitha
Published: September 2016

A robust feature of turbulent fragmentation theories is a universal Salpeter like slope (2.2 -2.4), for the mass spectrum of the fragments, at the high mass end. This is so due to the scale-free nature of turbulence and gravity. There are reports of top heavy / flatter Initial Mass Functions (IMF), inferred for many regions where we expect star formation to take place in gas clouds with comparatively higher gas density. Also, a higher Star Formation Efficiency (SFE) for regions of higher gas density has been proposed, to understand the formation of bound stellar systems in which dark matter is not a significant factor affecting the internal dynamics. In turbulent fragmentation models for star formation, we do not expect the mass of the stellar cluster to influence the maximum stellar mass directly and thereby imply a relation between the maximum stellar mass and the cluster mass. However, such a relation may be expected from statistical considerations. In this context, we explore the density dependence of the IMF, that would arise due to denser clouds producing more massive clusters due to the density dependence of the SFE.
High-Redshift Protoclusters Traced by Submillimeter Galaxies
Authors: Menéndez-Delmestre Karín , Capak Peter , Sheth Kartik
Published: September 2016

Clustering analysis indicate that at z ~ 2 submm-selected galaxies (SMGs) reside in very massive halos (MDM > 5 × 1013), suggesting that SMGs trace high-density environments that evolve into rich galaxy clusters. Conversely, recent work suggests that SMGs are tracers of a broader range of environments, including structures with more modest masses caught in highly active periods; since galaxies in these structures are likely caught during episodes of peak starbursts, SMGs may be tracers of a wider range of environments beyond the progenitors of todays very rich clusters, opening a window for a more complete exploration of the details underpinning the process of galaxy evolution in concert with the assembly of the large scale structure (LSS). We have undertaken a large observing program comprising deep narrow-band Ly-alpha imaging and multi-object spectroscopy using Palomar/Keck/Magellan/Gemini telescopes to probe for galaxy overdensities in SMG environments at z ~ 1 − 5. With ~200 spectroscopically-confirmed Ly-alpha emitters, we are in a position to gauge the level of galaxy overdensity in these regions.
What is a GMC? Are observers and simulators discussing the same star-forming clouds?
Authors: Pan Hsi-An , Fujimoto Yusuke , Tasker Elizabeth J.
Published: September 2016

Observations and simulations have now reached the point where the giant molecular cloud (GMCs) populations can be studied over a whole galaxy. This is immensely helpful for understanding star formation. Yet, are these two groups really comparing the same objects? While simulators work in 6D (x, y, z, vx, vy, vz) position-position-position (PPP) space, observers see 2 + 1D (RA, Dec, vlos) projected properties along the line of sight, identifying clouds in position-position-velocity (PPV) space. In this research we generated PPP and PPV data for a high-resolution simulated galaxy and compared the identified clouds in both data sets. The results show that 70% of the clouds have a single counterpart in each data structure. Cloud boundaries of these clouds are indeed the same. Scatter of the derived cloud properties (radius and velocity dispersion) between PPP and PPV are typically within a factor of two. However, this small scatter can make it difficult to determine if a cloud is truly gravitationally bound.
Galactic spiral generation in tidal encounters
Authors: Pettitt Alex R. , Tasker Elizabeth J. , Wadsley James W.
Published: September 2016

The existence of grand design spiral galaxies in the universe is still a standing problem. The passage of a small companion is known to be able to induce spiral structures in disc galaxies, but there remains questions over how relevant this mechanism is to the galaxies observed in the real universe. Our study aims to address two key points regarding such interactions; the limiting mass companion needed to drive tidal spiral structures, and the differences between the resulting gas and stellar morphology. We find the minimum mass of a companion to be as low as 5% of the stellar mass of the galaxy, and that the arms formed in the gas and the stars display very minor dynamical and morphological differences.
Core mass function: a comparison study between Orion A and other massive filamentary clouds.
Authors: Ren Zhiyuan , Li Di
Published: September 2016

As a giant compact filamentary cloud, Orion A has a similar morphology with those more distant filaments in infrared dark clouds as revealed in Herschel surveys. We compared their core mass functions and found a similar power law index of N(>m)∝ m−1.0 for the high-mass end, which may possibly indicates a common case for massive filamentary clouds. We also show that the measured mass function for a certain cloud would largely depend on its distance, thus call for caution in interpreting individual measurements of CMF.
CaII Quasar Absorbers: Statistics, Metals, Dust, and Associated Galaxies
Authors: Turnshek David A. , Sardane Gendith M. , Rao Sandhya M.
Published: September 2016

We summarize results from our recent SDSS survey for CaII quasar absorbers. The survey finds 435 absorbers at z<1.34, which corresponds to ~9 Gyrs of the Universe's history. Two CaII absorber populations are identified, which we call weak and strong. Metal abundance ratios derived from normalized composite spectra show that weak absorbers can be identified with halo-like gas, while strong absorbers are a mix of halo+disk-like gas. Consistent with these abundance ratio results, fluxed composites show that strong absorbers are ~6 times more reddened than weak absorbers (i.e., they contain more dust). Four individual examples of galaxies associated with CaII absorption are found in the SDSS images, and three are star forming galaxies (SFGs). Image composites show that galaxies associated with strong absorbers have mean luminosity-weighted impact parameters, b, which are ~2.4 times smaller than the weak absorbers (bstrong ~ 19 kpc versus bweak 45 kpc). Studies of CaII absorbers suggest links to molecular clouds, SFGs, and circumgalactic gas (CGG).
WISE properties of OH megamaser galaxies: Guide for future FAST OHM survey?
Authors: Zhang J.S. , Wang J.Z. , Li D. , Zhu Q.F.
Published: September 2016

All 119 OH maser galaxies (110 out of them are megamasers, i.e., LOH > 10 L⊙, OHMs) published so far were compiled and were cross-identified with the Wide-Field Infrared Survey Explorer (WISE) catalog. Our aim is to investigate intrinsic middle-infrared properties of OH maser galaxies and try to find some hints on sample selections on OHM surveys through the coming Five hundred aperture spherical telescope (FAST). In addition, enormous potentials for OHM surveys by future FAST are investigated, based on its innovative designs and its expected best sensitivity among single dish telescopes.
Binary stars on the galaxy SFH
Authors: Zhang F. , Li L. , Han Z.
Published: September 2016

Using the Yunnan-II evolutionary population synthesis models comprising binary stars, we find that the inclusion of binary stars can raise the derived stellar metallicity Z* and/or age t (degeneracy problem), raise the stellar mass M*, lower the gaseous metallicity Zgas and star formation rate (SFR) of galaxies. This means that a few stars form recently in galaxies, while more stars form during the entire evolution process when considering binary stars. If the degeneracy between t and Z* can be broken, its effect on the feedback process and star formation history can be determined.
Verantwortungsbewusstsein stärken
Authors: Siegler Sarah
Published: September 2016

Zusammenfassung. Durch die Arbeit mit hilfsbedürftigen Personen stehen Pflegende tagtäglich in einem besonderen Verantwortungsverhältnis. Zu erkennen, dass Pflegende in der Lage sind eigenständig Entscheidungen zu treffen, Gründe anzugeben und auch dementsprechend zu handeln, sind grundlegende Bedingungen pflegerischer Verantwortung. Bereits in der Gesundheits- und Krankenpflegeausbildung sollte innerhalb des Ethikunterrichts auf die volle Verantwortungsübernahme vorbereitet werden.
Spiritualität und Ethik: Autonomie oder Symbiose?
Authors: Knoll Franziskus
Published: September 2016

Zusammenfassung. Spiritualität ist bisher noch kein Thema innerhalb der deutschen Pflegeethik. In Diskursen wird Spiritualität häufig in eins gesetzt mit Religion und die sollte im Zuge ethische Entscheidungsfindungen doch weitgehend außen vor bleiben; es sei denn, Pflegende haben es mit Menschen zu tun, die explizit ihre religiösen Rechte einfordern. Vor diesem Hintergrund möchte der vorliegende Beitrag für die Relevanz der spirituellen Dimension des Mensch-Seins im ethischen Diskurs sensibilisieren.
Ethische Bildung in der Altenpflege
Authors: Brodehl Reinhard
Published: September 2016

Zusammenfassung. Der ethische Ansatz von Ricoeur reflektiert in Verbindung mit dem Sorgebegriff Heideggers die Dimension um das Selbst, den Anderen und die Pflegeinstitution. Weil Institutionen untrennbar mit dem Privat- und Berufsleben verwoben sind und sie auf das Selbst und den Anderen eine ’deontische Macht’ ausüben, stellt die kritische Reflexion dazu einen Schwerpunkt dar. Für die Einführung in die Ethik eignet sich als Transfer das Märchen von den ’Bremer Stadtmusikanten’, dessen Kenntnis vorausgesetzt wird.
Orientierung schaffen
Authors: Behrendt Daniel , Welzel Patrick
Published: September 2016

Zusammenfassung. Aktuell wird vielfach über Ansätze einer demenzorientierte Umgebungsgestaltung in Altenpflegeeinrichtungen berichtet und diskutiert. Aber wie sieht es mit der Implementierung der Ergebnisse in der Praxis aus? In einem Projekt an der Krankenpflegeschule des Städtischen Klinikums Dessau stellen sich Schülerinnen und Schüler der Gesundheits- und Krankenpflege dieser Herausforderung und suchen am Beispiel einer stationären Altenpflegeeinrichtung nach praktikablen Möglichkeiten der Umsetzung.
Targeting the metabolic pathway of human colon cancer overcomes resistance to TRAIL-induced apoptosis
Authors: Carr Ryan M , Qiao Guilin , Qin Jianzhong , Jayaraman Sundararajan , Prabhakar Bellur S , Maker Ajay V
Published: September 2016

Colon cancer is a leading cause of cancer-related mortality for which targeted therapy is needed; however, trials using apoptosis-inducing ligand monotherapy to overcome resistance to apoptosis have not shown clinical responses. Since colon cancer cells selectively uptake and rapidly metabolize glucose, a property utilized for clinical staging, we investigated mechanisms to alter glucose metabolism in order to selectively target the cancer cells and to overcome evasion of apoptosis. We demonstrate TRAIL (tumor necrosis factor-related apoptosis-inducing ligand) resistance in the majority of human colon cancers tested and utilize the glucose analog 2-deoxy-d-glucose to sensitize TRAIL-resistant gastrointestinal adenocarcinoma cells, and not normal gastrointestinal epithelial cells, to TRAIL-induced apoptosis through enhanced death receptor 5 expression, downstream modulation of MAPK signaling and subsequent miRNA expression modulation by increasing the expression of miR-494 via MEK activation. Further, established human colon cancer xenografts treated with this strategy experience anti-tumor responses. These findings in colon adenocarcinoma support further investigation of manipulation of cellular energetics to selectively overcome resistance to apoptosis and to impart tumor regressions in established colon cancer tumors.
Mutational signatures of ionizing radiation in second malignancies
Authors: Behjati Sam , Gundem Gunes , Wedge David C. , Roberts Nicola D. , Tarpey Patrick S. , Cooke Susanna L. , Van Loo Peter , Alexandrov Ludmil B. , Ramakrishna Manasa , Davies Helen , Nik-Zainal Serena , Hardy Claire , Latimer Calli , Raine Keiran M. , Stebbings Lucy , Menzies Andy , Jones David , Shepherd Rebecca , Butler Adam P. , Teague Jon W. , Jorgensen Mette , Khatri Bhavisha , Pillay Nischalan , Shlien Adam , Futreal P. Andrew , Badie Christophe ,   ICGC Prostate Group, Cooper Colin S. , Eeles Rosalind A. , Easton Douglas , Foster Christopher , Neal David E. , Brewer Daniel S. , Hamdy Freddie , Lu Yong-Jie , Lynch Andrew G. , Massi Charlie E. , Ng Anthony , Whitaker Hayley C. , Yu Yongwei , Zhang Hongwei , Bancroft Elizabeth , Berney Dan , Camacho Niedzica , Corbishley Cathy , Dadaev Tokhir , Dennis Nening , Dudderidge Tim , Edwards Sandra , Fisher Cyril , Ghori Jilur , Gnanapragasam Vincent J. , Greenman Christopher , Hawkins Steve , Hazell Steven , Howat Will , Karaszi Katalin , Kay Jonathan , Kote-Jarai Zsofia , Kremeyer Barbara , Kumar Pardeep , Lambert Adam , Leongamornlert Daniel , Livni Naomi , Luxton Hayley , Matthews Lucy , Mayer Erik , Merson Susan , Nicol David , Ogden Christopher , O’Meara Sarah , Pelvender Gill , Shah Nimish C. , Tavare Simon , Thomas Sarah , Thompson Alan , Verrill Claire , Warren Anne , Zamora Jorge , McDermott Ultan , Bova G. Steven , Richardson Andrea L. , Flanagan Adrienne M. , Stratton Michael R. , Campbell Peter J.
Published: September 2016

Ionizing radiation is a potent carcinogen, inducing cancer through DNA damage. The signatures of mutations arising in human tissues following in vivo exposure to ionizing radiation have not been documented. Here, we searched for signatures of ionizing radiation in 12 radiation-associated second malignancies of different tumour types. Two signatures of somatic mutation characterize ionizing radiation exposure irrespective of tumour type. Compared with 319 radiation-naive tumours, radiation-associated tumours carry a median extra 201 deletions genome-wide, sized 1–100 base pairs often with microhomology at the junction. Unlike deletions of radiation-naive tumours, these show no variation in density across the genome or correlation with sequence context, replication timing or chromatin structure. Furthermore, we observe a significant increase in balanced inversions in radiation-associated tumours. Both small deletions and inversions generate driver mutations. Thus, ionizing radiation generates distinctive mutational signatures that explain its carcinogenic potential.
Local and thalamic origins of correlated ongoing and sensory-evoked cortical activities
Authors: Cohen-Kashi Malina Katayun , Mohar Boaz , Rappaport Akiva N. , Lampl Ilan
Published: September 2016

Thalamic inputs of cells in sensory cortices are outnumbered by local connections. Thus, it was suggested that robust sensory response in layer 4 emerges due to synchronized thalamic activity. To investigate the role of both inputs in the generation of correlated cortical activities, we isolated the thalamic excitatory inputs of cortical cells by optogenetically silencing cortical firing. In anaesthetized mice, we measured the correlation between isolated thalamic synaptic inputs of simultaneously patched nearby layer 4 cells of the barrel cortex. Here we report that in contrast to correlated activity of excitatory synaptic inputs in the intact cortex, isolated thalamic inputs exhibit lower variability and asynchronous spontaneous and sensory-evoked inputs. These results are further supported in awake mice when we recorded the excitatory inputs of individual cortical cells simultaneously with the local field potential in a nearby site. Our results therefore indicate that cortical synchronization emerges by intracortical coupling.
Quantum dot spin coherence governed by a strained nuclear environment
Authors: Stockill R. , Le Gall C. , Matthiesen C. , Huthmacher L. , Clarke E. , Hugues M. , Atatüre M.
Published: September 2016

The interaction between a confined electron and the nuclei of an optically active quantum dot provides a uniquely rich manifestation of the central spin problem. Coherent qubit control combines with an ultrafast spin–photon interface to make these confined spins attractive candidates for quantum optical networks. Reaching the full potential of spin coherence has been hindered by the lack of knowledge of the key irreversible environment dynamics. Through all-optical Hahn echo decoupling we now recover the intrinsic coherence time set by the interaction with the inhomogeneously strained nuclear bath. The high-frequency nuclear dynamics are directly imprinted on the electron spin coherence, resulting in a dramatic jump of coherence times from few tens of nanoseconds to the microsecond regime between 2 and 3 T magnetic field and an exponential decay of coherence at high fields. These results reveal spin coherence can be improved by applying large magnetic fields and reducing strain inhomogeneity.
Relationships between pathology and crystal structure in breast calcifications: an in situ X-ray diffraction study in histological sections
Authors: Scott Robert , Stone Nicholas , Kendall Catherine , Geraki Kalotina , Rogers Keith
Published: September 2016

Calcifications are not only one of the most important early diagnostic markers of breast cancer, but are also increasingly believed to aggravate the proliferation of cancer cells and invasion of surrounding tissue. Moreover, this influence appears to vary with calcification composition. Despite this, remarkably little is known about the composition and crystal structure of the most common type of breast calcifications, and how this differs between benign and malignant lesions. We sought to determine how the phase composition and crystallographic parameters within calcifications varies with pathology, using synchrotron X-ray diffraction. This is the first time crystallite size and lattice parameters have been measured in breast calcifications, and we found that these both parallel closely the changes in these parameters with age observed in fetal bone. We also discovered that these calcifications contain a small proportion of magnesium whitlockite, and that this proportion increases from benign to in situ to invasive cancer. When combined with other recent evidence on the effect of magnesium on hydroxyapatite precipitation, this suggests a mechanism explaining observations that carbonate levels within breast calcifications are lower in malignant specimens.
Single-cell transcriptome and epigenomic reprogramming of cardiomyocyte-derived cardiac progenitor cells
Authors: Chen Xin , Chakravarty Tushar , Zhang Yiqiang , Li Xiaojin , Zhong Jiang F. , Wang Charles
Published: September 2016

The molecular basis underlying the dedifferentiation of mammalian adult cardiomyocytes (ACMs) into myocyte-derived cardiac progenitor cells (mCPCs) during cardiac tissue regeneration is poorly understood. We present data integrating single-cell transcriptome and whole-genome DNA methylome analyses of mouse mCPCs to understand the epigenomic reprogramming governing their intrinsic cellular plasticity. Compared to parental cardiomyocytes, mCPCs display epigenomic reprogramming with many differentially-methylated regions, both hypermethylated and hypomethylated, across the entire genome. Correlating well with the methylome, our single-cell transcriptomic data show that the genes encoding cardiac structure and function proteins are remarkably down-regulated in mCPCs, while those for cell cycle, proliferation, and stemness are significantly up-regulated. In addition, implanting mCPCs into infarcted mouse myocardium improves cardiac function with augmented left ventricular ejection fraction. This dataset suggests that the cellular plasticity of mammalian cardiomyocytes is the result of a well-orchestrated epigenomic reprogramming and a subsequent global transcriptomic alteration. Understanding cardiomyocyte epigenomic reprogramming may enable the design of future clinical therapies that induce cardiac regeneration, and prevent heart failure.
Novel O-GlcNAcylation on Ser40 of canonical H2A isoforms specific to viviparity
Authors: Hirosawa Mitsuko , Hayakawa Koji , Yoneda Chikako , Arai Daisuke , Shiota Hitoshi , Suzuki Takehiro , Tanaka Satoshi , Dohmae Naoshi , Shiota Kunio
Published: September 2016

We report here newly discovered O-linked-N-acetylglucosamine (O-GlcNAc) modification of histone H2A at Ser40 (H2AS40Gc). The mouse genome contains 18 H2A isoforms, of which 13 have Ser40 and the other five have Ala40. The combination of production of monoclonal antibody and mass spectrometric analyses with reverse-phase (RP)-high performance liquid chromatography (HPLC) fractionation indicated that the O-GlcNAcylation is specific to the Ser40 isoforms. The H2AS40Gc site is in the L1 loop structure where two H2A molecules interact in the nucleosome. Targets of H2AS40Gc are distributed genome-wide and are dramatically changed during the process of differentiation in mouse trophoblast stem cells. In addition to the mouse, H2AS40Gc was also detected in humans, macaques and cows, whereas non-mammalian species possessing only the Ala40 isoforms, such as silkworms, zebrafish and Xenopus showed no signal. Genome database surveys revealed that Ser40 isoforms of H2A emerged in Marsupialia and persisted thereafter in mammals. We propose that the emergence of H2A Ser40 and its O-GlcNAcylation linked a genetic event to genome-wide epigenetic events that correlate with the evolution of placental animals.