bluuebunny/crossref_metadata_2025_split huggingface dataset:
Signposting mutation in some fourteenth- and fifteenth-century music theory treatises
Authors: WHITTAKER ADAM 
Published: March 2017

ABSTRACTThe foundation of the solmisation system, attributed to Guido d'Arezzo, is based upon the application of the syllables ut, re, mi, fa, sol, la, to the musical notes C D E F G A. Later, this system was expanded to incorporate a series of overlapping hexachords made up of these six syllables. These overlapping hexachords could allow a singer to move seamlessly across the regular musical space (the gamut) using only the six syllables (voces) via ‘mutations’. Even though the extent to which this system underpinned diatonic conceptions of musical space is being reconsidered, it seems clear that, at least for some musicians, it played an integral part in music education.Although many theorists discussed the process of hexachordal mutation in their treatises, the approaches towards its exemplification and demonstration were far from uniform, given its conceptual rather than notated function. Johannes Tinctoris's Expositio manus (c.1472) includes a number of musical examples showing hexachordal mutation. His examples, rather unusually, include syllabic annotations to label the points of mutation within the musical notation, a practice that is almost without precedent. This article takes Tinctoris's treatise as a point of departure and compares the approaches taken towards the exemplification of hexachordal mutation in some theoretical texts from the fourteenth and fifteenth centuries, tracking the influence of their approaches forward into the sixteenth century. It considers what some different approaches can tell us about the conceptual function of the hexachord in pedagogy, and what the motives might have been for adopting specific exemplification practices.
The absent first gathering of the Chantilly manuscript
Authors: BENT MARGARET 
Published: March 2017

ABSTRACTThe Chantilly manuscript, probably compiled in the 1410s, is thought to have lost an original first sestern early in its history, as the folio numbers start at 13. Because the table of contents matches the order of pieces in the manuscript and starts with the present first item and at fol. 13, it has been assumed that it post-dates the sestern's loss. But the folio numbers were added to that table not by its original hand, but by a later (Italian) one, and that same hand wrote the foliation for the manuscript; table and foliation were therefore almost certainly provided in the same operation. If the table of contents waspost factum, why is its foliation in a hand different from the incipits? This article argues that the table of contents was in fact prescriptive, drawn up by a different (French) person before the contents were copied, and that the foliation was added both to the index and the body of the manuscript after copying, allowing for a new planned gathering to be added at the beginning, perhaps including the two Cordier rondeaux. This was never completed; what we have is what there was, and nothing was lost. This hypothesis raises further questions about the codicological and chronological relation of the Cordier songs to the index, to that planned gathering, and to the early history of the manuscript, questions to which provisional answers are suggested.
Core-Shell Structure of Intermediate Precipitates in a Nb-Based Z-Phase Strengthened 12% Cr Steel
Authors: Rashidi Masoud , Andrén Hans-Olof , Liu Fang 
Published: March 2017

AbstractIn creep resistant Z-phase strengthened 12% Cr steels, MX (M=Nb, Ta, or V, and X=C and/or N) to Z-phase (CrMN, M=Ta, Nb, or V) transformation plays an important role in achieving a fine distribution of Z-phase precipitates for creep strengthening. Atom probe tomography was employed to investigate the phase transformation in a Nb-based Z-phase strengthened trial steel. Using iso-concentration surfaces with different concentration values, and subtracting the matrix contribution enabled us to reveal the core-shell structure of the transient precipitates between MX and Z-phase. It was shown that Z-phase forms by diffusion of Cr into NbN upon ageing, and Z-phase has a composition corresponding to Cr1+xNb1−xN withx=0.08.
Resolving the Disk-Halo Degeneracy: A look at M74
Authors: Aniyan S. , Freeman K. C. , Arnaboldi M. , Gerhard O. , Coccato L. , Kuijken K. , Merrifield M. 
Published: March 2017

AbstractThe decomposition of the 21 cm rotation curve of galaxies into contribution from the disk and dark halo depends on the adopted mass to light ratio (M/L) of the disk. Given the vertical velocity dispersion (σz) of stars in the disk and its scale height (h), the disk surface density and hence the M/L can be estimated. Earlier works have used this technique to conclude that galaxy disks are submaximal. Here we address an important conceptual problem: σz and h must pertain to the same population. Our analysis concludes that previous studies underestimate the disk surface mass density by ~ 2, sufficient to make a maximal disk for M74 appear like a submaximal disk.
Circumgalactic gas absorption in extremely metal-poor dwarf dalaxies
Authors: Filho M. E. , Almeida J. Sánchez , Tuñón C. Muñoz 
Published: March 2017

AbstractAccretion of metal-poor gas via cold accretion flows has been recently proposed as a means to trigger/sustain star formation in extremely metal-poor dwarf galaxies (XMPs), a scenario in agreement with theoretical predictions. We report on the tentative detection of CaII absorption used to trace the conditions of the gas clouds in the halo of the XMP UGCA 20.
Resolved stellar populations in dSphs. What can they tell us about galaxy evolution?
Authors: Pino Andréz del , Łokas Ewa L. , Hidalgo Sebasian L. , Fouquet Sylvain 
Published: March 2017

AbstractWe present a comprehensive photometric study of the Fornax and the Andromeda II dwarf spheroidal (dSph) galaxies. It is based on the up-to-date deepest photometric data for both galaxies. We have derived their detailed star formation histories (SFHs) as a function of galactocentric radius. This allowed us to analyze in detail the spatial distribution of their different stellar populations.
Star formation history of the galaxy merger Mrk848 with SDSS-IV MaNGA
Authors: Yuan Fang-Ting , Shen Shiyin , Hao Lei , Fernandez Maria Argudo 
Published: March 2017

AbstractWith the 3D data of SDSS-IV MaNGA (Bundy et al. 2015) spectra and multi-wavelength SED modeling, we expect to have a better understanding of the distribution of dust, gas and star formation of galaxy mergers. For a case study of the merging galaxy Mrk848, we use both UV-to-IR broadband SED and the MaNGA integral field spectroscopy to obtain its star formation histories at the tail and core regions. From the SED fitting and full spectral fitting, we find that the star formation in the tail regions are affected by the interaction earlier than the core regions. The core regions show apparently two times of star formation and a strong burst within 500Myr, indicating the recent star formation is triggered by the interaction. The star formation histories derived from these two methods are basically consistent.
Investigating environmental trends in the outer visible edges of dwarf irregular galaxies
Authors: Dunn Jacqueline M. 
Published: March 2017

AbstractThe star formation histories and evolution of 28 dwarf irregular galaxies (dIs) that reside in differing local and global environments are investigated. The shallow gravitational potentials of dwarf galaxies make these objects highly susceptible to changes in morphology or dynamics by external perturbations. Additionally, the lack of more complicated structures such as spiral arms makes environmental effects more easily discernible. Therefore, dIs are ideal candidates for a study of the role of environment in galaxy evolution. The local environment is defined by the local galaxy number density, where high indicates at least one neighbor within 200 kpc and low indicates no neighbors within 1 Mpc. The global environment is classified as either the field or a galaxy group / cluster.Absolute magnitudes, colors, central surface brightnesses, star formation rates and color profiles were compared using photometry from UBVR and Hα imaging. While some environmental trends are noted (galaxies in local high density environments have brighter central and effective surface brightnesses, while those in global high density environments have brighter absolute magnitudes, central and effective surface brightnesses, and higher star formation rates), no systematic environmental trends are seen in the shape of the color profiles or spatial distribution of recent star formation. A lack of environmental trend in star formation and galaxy color indicates that either internal processes dominate the formation and subsequent evolution of the outskirts of dIs, or there is no systematic environmental effect on such. The appearance of environmental effects should be more noticeable at the outermost edges of these systems. The lack of a trend in such implies that the exact nature of the environmental influence varies greatly depending on the exact nature of the interaction occurring.
Not even wrong: A philosophical, historical and ultimately a scientific inquiry into the Schmidt Law
Authors: Madore Barry F. , Carlson Erika K. 
Published: March 2017

AbstractWe introduce a novel approach to interpreting the well-known spatial correlation of gas densities with on-going star formation. Treated as a closed-loop process involving two physically distinct phases the data can be subdivided into regions that are active and those that are quiescent. The active regions can be distinguished by the presence of high-mass, short-lived, but recently-formed OB stars; the quiescent regions are marked by an absence of these stars and they are considered to be recovering from the last star-formation event and are re-collapsing. The relative (areal) frequencies of those two phases are directly proportional to the relative timescales. For four Local Group galaxies, NGC 6822, the Large & Small Magellanic Clouds, and M33, the cloud assembly/collapse timescales are all found to be monotonically decreasing power-law functions of density, with as yet to be explained differences.
What can the occult do for you?
Authors: Holwerda B. W. , Keel W. C. 
Published: March 2017

AbstractInterstellar dust is still a dominant uncertainty in Astronomy, limiting precision in e.g., cosmological distance estimates and models of how light is re-processed within a galaxy. When a foreground galaxy serendipitously overlaps a more distant one, the latter backlights the dusty structures in the nearer foreground galaxy.Such an overlapping or occulting galaxy pair can be used to measure the distribution of dust in the closest galaxy with great accuracy. The STARSMOG program uses Hubble to map the distribution of dust in foreground galaxies in fine (<100 pc) detail. Integral Field Unit (IFU) observations will map the effective extinction curve, disentangling the role of fine-scale geometry and grain composition on the path of light through a galaxy.The overlapping galaxy technique promises to deliver a clear understanding of the dust in galaxies: geometry, a probability function of dimming as a function of galaxy mass and radius, and its dependence on wavelength.
What do galaxies look like beyond 31 mag/arcsec2?
Authors: Cebrián María , Trujillo Ignacio , Fliri Juergen 
Published: March 2017

AbstractDetection of optical surface brightness structures with magnitudes fainter than 30 mag/arcsec2 has remained elusive in current photometric deep surveys. We are conducting a new imaging strategy to cross that frontier and address the study of outskirts of galaxies and theories of galaxy formation.
The halo-to-stellar mass ratio in the S4G
Authors: Díaz-García Simón , Salo Heikki , Laurikainen Eija 
Published: March 2017

AbstractWe use 3.6 μm photometry for 1154 disk galaxies (i < 65°) in the S4G (Sheth et al. 2010). We obtain the average stellar component of the circular velocity (Vdisk) and the mean (dark matter) halo-to-stellar mass ratio (Mhalo/M*) inside the optical radius (Ropt) in bins of total stellar mass (M*, from Muñoz-Mateos et al. 2015), providing observational constraints for galaxy formation models to be tested against. We find the Mhalo/M* − M* relation in good agreement with the best-fit model at z ≈ 0 in ΛCDM cosmological simulations (e.g. Moster 2010), assuming that the dark matter halo within Ropt comprises a constant fraction (~ 4%) of its total mass.
The SFR Efficiency of HI Gas in the Outskirts of Star Forming Galaxies
Authors: Rafelski Marc 
Published: March 2017

AbstractIn order to understand the origin of the decreased star formation rate (SFR) efficiency of neutral atomic hydrogen gas measured in Damped Lyα Systems (DLAs) at z ~ 3, we measure the SFR efficiency of atomic gas at z ~ 1, z ~ 2, and z ~ 3 around star-forming galaxies. We create galaxy stacks in these three redshift bins, and measure the SFR efficiency by combining DLA absorber statistics with the observed rest-frame UV emission in the galaxies’ outskirts. We find that the SFR efficiency of Hi gas is ~ 3% of that predicted by the KS relation. We find no significant evolution in the SFR efficiency with redshift, although simulations and models predict a decreasing SFR efficiency with decreasing metallicity and thus with increasing redshift. We discuss possible explanations for this decreased efficiency without an evolution with redshift.
DAGAL: Detailed Anatomy of Galaxies
Authors: Knapen Johan H. 
Published: March 2017

AbstractThe current IAU Symposium is closely connected to the EU-funded network DAGAL (Detailed Anatomy of Galaxies), with the final annual network meeting of DAGAL being at the core of this international symposium. In this short paper, we give an overview of DAGAL, its training activities, and some of the scientific advances that have been made under its umbrella.
Probing the Baryon Cycle in Galaxy Outskirts
Authors: Davé Romeel 
Published: March 2017

AbstractGalaxies are born and grow within a cosmic ecosystem, in which they receive material from surrounding intergalactic gas via gravitationally-driven inflows and expel material via powerful galactic outflows. These processes, collectively referred to as the baryon cycle, are increasingly believed to govern galaxy growth over cosmic time. I discuss new insights on the baryon cycle using analytic models and hydrodynamical simulations of galaxy evolution, particularly emphasizing how galaxy outskirts are the prime locale within which to observe these processes in action by examining observational tracers such as rest-ultraviolet absorption lines and the neutral and molecular gas content of galaxies.
Antitruncations
Authors: Beckman John , Borlaff Alejandro , Eliche-Moral M. Carmen , Font Joan , Erwin Peter 
Published: March 2017

AbstractSince 1970 surface brightness profiles of disc galaxies were classified as Type-I, single falling exponentials, or Type-II, broken exponentials with steeper decline in the outskirts. For the past decade Type-III profiles, (antitruncations), with a shallower fall-off in the outskirts, have been shown to occur in a significant fraction of galaxy discs. Here we give a brief overview, characterizing these profiles and their distribution with galaxy type, with a look at recent explanations of their causes, and how they fit into the picture of galaxy evolution.
The evolution of S0s with UV bright rings A SWIFT-UVOT study
Authors: Rampazzo R. , Mazzei P. , Marino A. , Trinchieri G. , Uslenghi M. , Wolter A. 
Published: March 2017

AbstractWe report about an ongoing study of the evolution of 24 S0s with UV-bright ring/arm-like structures observed with SWIFT-UVOT and interpreted via SPH simulations with chemo-photometric implementation.
Dynamical modelling of galactic disc outskirts
Authors: Athanassoula E. 
Published: March 2017

AbstractI review briefly some dynamical models of structures in the outer parts of disc galaxies, including models of polar rings, tidal tails and bridges. I then discuss the density distribution in the outer parts of discs. For this, I compare observations to results of a model in which the disc galaxy is in fact the remnant of a major merger, and find good agreement. This comparison includes radial profiles of the projected surface density and of stellar age, as well as time evolution of the break radius and of the inner and outer disc scale lengths. I also compare the radial projected surface density profiles of dynamically motivated mono-age populations and find that, compared to older populations, younger ones have flatter density profiles in the inner region and steeper in the outer one. The break radius, however, does not vary with stellar age, again in good agreement with observations.
The atomic gas in outer disks in semi-analytic models of galaxy formation
Authors: Fu Jian , Luo Yu 
Published: March 2017

AbstractWe use semi-analytic models of galaxy formation L-Galaxies based on ΛCDM cosmology to study the HI gas component in galaxy outskirts. We adopt the radially-resolved version of the models by Fu et al. (2013), which includes both atomic and molecular gas component in interstellar medium. This model has been recently updated by Luo et al. (2016) to include cold gas stripping in the outer disk regions of the satellite galaxies by ram pressure. In our models, we can perfectly reproduce the HI size-mass relation, which is discovered by Broeils & Rhee (1997) and confirmed by many subsequent observations. In our model, the reason for such tight correlation between HI size and mass is atomic-molecular phase conversion in high gas surface density regions while HI ionization in low gas surface density region, which leads to very narrow distribution of HI mean surface density. The models also reproduce the universal exponential HI radial profiles in galaxy outskirts found by Bluedisk (Wang et al. 2013), which arises from cold gas accretion onto the galaxy disks in exponentially profiles.
Gravitationally Lensed CO and Dust at High Redshift: New LMT/GTM Images and Spectra of Sub-Millimeter Galaxies
Authors: Lowenthal J. D. , Harrington K. , Berman D. , Yun M. , Cybulski R. , Wilson G. W. , Aretxaga I. , Chavez M. , De la Luz V. , Erickson N. , Ferrusca D. , Gallup A. , Hughes D. , Montaña A. , Narayanan G. , Sánchez-Argüelles D. , Schloerb F. P. , Souccar K. , Terlevich E. , Terlevich R. , Zeballos M. , Zavala J. A. 
Published: March 2017

AbstractWe have assembled a new sample of some of the most FIR-luminous galaxies in the Universe and have imaged them in 1.1 mm dust emission and measured their redshifts 1 < z < 4 via CO emission lines using the 32-m Large Millimeter Telescope / Gran Telescopio Milimétrico (LMT/GTM). Our sample of 31 submm galaxies (SMGs), culled from the Planck and Herschel all-sky surveys, includes 14 of the 21 most luminous galaxies known, with LFIR > 1014L⊙ and SFR > 104M⊙/yr. These extreme inferred luminosities – and multiple / extended 1.1 mm images – imply that most or all are strongly gravitationally lensed, with typical magnification μ ~ 10 × . The gravitational lensing provides two significant benefits: (1) it boosts the S/N, and (2) it allows investigation of star formation and gas processes on sub-kpc scales.
Halo K-Giant Stars from LAMOST: Kinematics and Galactic Mass Estimate
Authors: Bird Sarah A. 
Published: March 2017

AbstractWe analyze line-of-sight velocities of over 3000 halo K-giant stars from the second data release of the spectral survey LAMOST (Zhao et al. 2012). We find a nearly constant velocity dispersion profile, with no large dips or peaks, in a Galactocentric radial range of 10–30 kpc, in accord with earlier analyses (Battaglia et al. 2005, 2006; Xue et al. 2008, 2014) (see Fig. 1). Previous studies of halo star radial velocity dispersions in a reference frame centered on the Galactic Center have detected dips within this radial range (Sommer-Larsen et al. 1994; Kafle et al. 2012, 2014). We use the stars to make estimates of the enclosed mass out to 40 kpc from the Galactic Center using the method of Evans et al. (2011). Tens of thousands of such stars are expected to become available to this analysis by the end of the five-year survey.
Understanding biases when fitting disk truncations
Authors: Cardiel Nicolás , Marino Raffaella A. , Pascual Sergio , Ceballos M. Teresa , de Paz Armando Gil , Sánchez Sebastián F. 
Published: March 2017

AbstractTruncations in the stellar population at the edges of disk galaxies are thought to be a common morphological feature (e.g., Erwin et al. 2005; and more recently Marino et al. 2016). In fact, using imaging data from the SDSS, Pohlen & Trujillo (2006) showed that only ~ 10% of face-on to intermediate inclined, nearby, late-type (Sb-Sdm) spiral galaxies have a normal/standard purely exponential disk down to the noise limit. In situations like these, the simultaneous fit of two lines, joined or not at an intermediate point (the break radius), constitutes a natural step towards the modelling of radial variation in surface brightness, metallicity, or any other relevant parameter. This work shows the results of simple simulations in which the simultaneous fit to two joined lines is compared to the simultaneous fit of two independent lines (i.e., two lines that do not necessarily coincide at an intermediate point), and also to the traditional single ordinary least squares fit. These simulations reveal some biases that should be taken into account when facing these kind of fitting procedures.
A VLT/FORS2 spectroscopic survey of individual stars in a transforming dwarf galaxy
Authors: Battaglia G. , Kacharov N. , Rejkuba M. 
Published: March 2017

AbstractUnderstanding the properties of dwarf galaxies is important not only to put them in their proper cosmological context, but also to understand the formation and evolution of the most common type of galaxies. Dwarf galaxies are divided into two main classes, dwarf irregulars (dIrrs) and dwarf spheroidals (dSphs), which differ from each other mainly because the former are gas-rich objects currently forming stars, while the latter are gas-deficient with no on-going star formation. Transition types (dT) are thought to represent dIs in the process of losing their gas, and can therefore shed light into the possible process of dwarf irregulars (dIrrs) becoming gas-deficient, passively evolving galaxies. Here we present preliminary results from our wide-area VLT/FORS2 MXU spectroscopic survey of the Phoenix dT, from which we obtained line-of-sight velocities and metallicities from the nIR Ca II triplet lines for a large sample of individual Red Giant Branch stars.
HI in the outskirts of Nearby Spirals
Authors: Brinks Elias , Portas António 
Published: March 2017

AbstractWe analyse nine galaxies taken from the THINGS survey to investigate the H I extent of spiral galaxy disks. We exploit the high spatial and velocity resolution, and the sensitivity of THINGS to investigate where the atomic gas disks end and what might shape their outskirts. We find that the atomic gas surface density across most of the disk is constant at 5 to 10 M⊙ pc−2 and declines at large radius. The shape of the H I distribution can be described by a Sérsic–type function with a slope index n = 0.18 – 0.36. The H I column density at which radial profiles turn over is found to be at too high a level for it to be caused by ionisation by a meta–galactic UV field. Instead we suggest the H I extent is rather set by how galaxy disks form.