bluuebunny/crossref_metadata_2025 huggingface dataset:
Pancreaticobiliary Maljunctions in European Patients with Bile Duct Cysts: Results of the Multicenter Study of the French Surgical Association (AFC)
Authors: Ragot Emilia , Mabrut Jean‐Yves , Ouaïssi Mehdi , Sauvanet Alain , Dokmak Safi , Nuzzo Gennaro , Halkic Nermin , Dubois Remi , Létoublon Christian , Cherqui Daniel , Azoulay Daniel , Irtan Sabine , Boudjema Karim , Pruvot François‐René , Gigot Jean‐François , Kianmanesh Reza ,   Working Group of the French Surgical Association, Adham Mustapha , Doussot Alexandre , Branchereau Sophie , Ayav Ahmet , Balladur Pierre , Adam René , Troisi Roberto I. , Regimbeau Jean Marc‐Amiens , Majno Pietro , Sommacale Daniele , Bouzid Chafik , Falconi Massimo
Published: September 2016

Background

Pancreaticobiliary maljunctions (PBMs) are congenital anomalies of the junction between pancreatic and bile ducts, frequently associated with bile duct cyst (BDC). BDC is congenital biliary tree diseases that are characterized by distinctive dilatation types of the extra‐ and/or intrahepatic bile ducts. Todani’s types I and IVa, in which dilatation involves principally the main bile duct, are the most frequent. PBM induces pancreatic juice reflux into the biliary tract that is supposed to be one of the main factors of biliary cancer degeneration, although the diagnostic criteria of PBM that can be either morphological and/or functional are not well defined especially in Western series.

Objective

The aim of this study was to assess the relative prevalence of PBM in BDC in a large European multicenter study, to analyze the characteristics of PBM and try to propose diagnostic criteria of PBMs based on morphological and/or functional criteria and define the positive, negative predictive values, sensibility and specificity of either criteria.

Results

From 1975 to 2012, 263 patients with BDC were analyzed. Among them, 190 (72.2 %) were considered to present PBM. Types I and IVa had a similar rate of PBM association. According to the “AFC classification,” 57.2 % had a C–P type, 34.5 % a P–C type and 8.3 % a complex type (“anse‐de‐seau”). The median length of the common channel in patients with PBM was 15.8 ± 6.8 mm (range 5–40 mm). The median intrabiliary amylase and lipase levels were 65,249 and 172,104 UI/L, respectively. For the diagnostic of PBM, a common channel length of more than 8 mm and an intrabiliary amylase level superior to 8000 UI/L were associated with a predictive positive value and a specificity of more than 90 %. Synchronous biliary cancer had an incidence of 8.7 % in all patients with BDC and PBM 11.1 % in adults. Compared to type IV, the type I BDC was associated with statistically more cancer patients in the presence of PBM.

Conclusions

Characteristics of PBM associated with BDC in Western population are quite close to reported Eastern series. The results suggest considering both the intrabiliary value of amylase >8000 UI/L and a length of a common channel >8 mm as appropriate values for positive diagnosis of PBM.
Comparison of Oleo‐ vs Petro‐Sourcing of Fatty Alcohols via Cradle‐to‐Gate Life Cycle Assessment
Authors: Shah Jignesh , Arslan Erdem , Cirucci John , O'Brien Julie , Moss Dave
Published: September 2016

Alcohol ethoxylates surfactants are produced via ethoxylation of fatty alcohol (FA) with ethylene oxide. The source of FA could be either palm kernel oil (PKO) or petrochemicals. The study aimed to compare the potential environmental impacts for PKO‐derived FA (PKO‐FA) and petrochemicals‐derived FA (petro‐FA). Cradle‐to‐gate life cycle assessment has been performed for this purpose because it enables understanding of the impacts across the life cycle and impact categories. The results show that petro‐FA has overall lower average greenhouse gas (GHG) emissions (∼2.97 kg CO2e) compared to PKO‐FA (∼5.27 kg CO2e). (1) The practices in land use change for palm plantations, (2) end‐of‐life treatment for palm oil mill wastewater effluent and (3) end‐of‐life treatment for empty fruit bunches are the three determining factors for the environmental impacts of PKO‐FA. For petro‐FA, n‐olefin production, ethylene production and thermal energy production are the main factors. We found the judicious decisions on land use change, effluent treatment and solid waste treatment are key to making PKO‐FA environmentally sustainable. The sensitivity results show the broad distribution for PKO‐FA due to varying practices in palm cultivation. PKO‐FA has higher impacts on average for 12 out of 18 impact categories evaluated. For the base case, when accounted for uncertainty and sensitivity analyses results, the study finds that marine eutrophication, agricultural land occupation, natural land occupation, fossil depletion, particulate matter formation, and water depletion are affected by the sourcing decision. The sourcing of FA involves trade‐offs and depends on the specific practices through the PKO life cycle from an environmental impact perspective.
Coalescence Behavior of Pure and Natural Fat Droplets Characterized via Micromanipulation
Authors: Thiel A. E. , Hartel R. W. , Spicer P. T. , Hendrickson K. J.
Published: September 2016

For two approaching oil droplets, a region of arrested coalescence lies between full coalescence and total stability. Here the fusion of two droplets begins, but they are stopped from fully relaxing into one spherical droplet. The internal rigidity of the solid fat network within each droplet can provide the resistance necessary to arrest the shape change driven by Laplace pressure. These intermediate doublet structures lead to the partially‐coalesced fat networks important for the desired physical properties of ice cream and whipped topping. The use of micromanipulation techniques allows coalescence events between two oil droplets to be microscopically observed. In this study, oil droplets composed of different fats were manipulated at varying elastic moduli, interfacial tension, and radii. It was seen that increasing the elastic moduli of the droplets or increasing droplet radii resulted in coalescence being arrested earlier. Under these experimental conditions, different interfacial tensions did not change the coalescence behavior between two oil droplets.
Pavement performance evaluation for different combinations of temperature conditions and bituminous mixes
Authors: Ranadive M. S. , Tapase Anand
Published: September 2016

The effectiveness of 2D axisymmetric finite element analysis in predicting the performance of flexible pavements at different temperatures is illustrated in the present study. The critical parameters are examined for variation in thicknesses and material properties of the bituminous layer, to select the right binder grade of bituminous mixes for the particular climatic condition or the selected temperature profile. To observe the effect of decrement in temperature profile of the under layer on the performance of the pavement, variation in modulus of dense bituminous macadam is analyzed for material properties reported as per IRC: 37-2012. For the modern trucks, which usually have more than 0.800 MPa tyre pressure, the right binder grade of bituminous layer comprising a wearing course and dense bituminous macadam is 1700 MPa for 250 mm-thick bituminous layer. When more stiffer binder is used, drastic change in the value of critical parameters is observed. A reduction of 18.98 and 5.25 % in horizontal tensile strain and vertical compressive strain, respectively, is observed at a 200 mm thickness of bituminous layer and around 21.12 and 6.72 % in horizontal tensile strain and vertical compressive strain, respectively, at 250 mm thickness of bituminous layer. As the values of the critical parameters are noticed well within the allowable limits at 200 mm, it is concluded that the use of a stiffer binder for DBM makes the pavement safe as far as fatigue of bituminous layer and rutting in subgrade is concerned with the reduction in thickness of the bituminous layer even at higher temperature. It is observed that the use of waste plastic/rubber is found in safe limits at 250 mm-thick bituminous layer for the selected condition. It is concluded that the use of too soft a bituminous mix results in lowering the structural capacity of the pavement at high temperatures and too hard bituminous mixes would become brittle at low temperatures.
Postoperative septic arthritis with Eikenella corrodens and Streptococcus mitis following arthroscopic anterior cruciate ligament reconstruction in an adolescent
Authors: Hurley Richard K. , Maranich Ashley M. , Schmitz Matthew R.
Published: September 2016

We present a case of postoperative septic arthritis with Eikenella corrodens and Streptococcus mitis following an arthroscopic anterior cruciate ligament reconstruction in an adolescent male with no pertinent medical history. The patient presented to the emergency department nine days after the operation with fever, an elevated white blood cell count, knee pain, and effusion. Arthrocentesis of the knee yielded purulent fluid that tested positive for S. mitis. Repeat intraoperative cultures revealed E. corrodens. In addition to antibiotics, the patient's treatment course included arthroscopic irrigation and debridement in the operating room as well as removal of graft material and fixation devices. To our knowledge, this is the first case of a polymicrobial infection of E. corrodens and S. mitis causing septic arthritis in a teenager following arthroscopic anterior cruciate ligament reconstruction.
Percutaneous cholecystostomy for acute cholecystitis in high‐risk elderly patients
Authors: Lin Wei‐Chen , Chang Chen‐Wang , Chu Cheng‐Hsin
Published: September 2016

Emergency cholecystectomy for acute cholecystitis (AC) is associated with high morbidity and mortality rates in elderly patients with significant comorbidities. The aim of this study was to evaluate percutaneous cholecystostomy for AC in elderly patients with various coexisting diseases. We retrospectively reviewed the records of 4311 patients with AC treated in Mackay Memorial Hospital between the years 2000 and 2015. The clinical course of AC was compared between nonelderly (age ≤70 years) and elderly patients (age >70 years). In total, 67 elderly patients and 32 nonelderly patients received percutaneous cholecystostomy. The rate of percutaneous cholecystostomy increased between the years 2011 and 2015 (from 2.5% to 12.2%) and this procedure was more common in the elderly group (p = 0.009). In addition, the comorbidities of ischemic heart disease and chronic kidney disease were higher in elderly than in nonelderly patients (p = 0.014 and p = 0.015, respectively). The American Society of Anesthesiologists' classification was higher in the elderly patients (p = 0.001). The overall survival‐free rate of recurrent cholecystitis in patients who did not receive cholecystectomy was not significantly different in the two groups. When compared with emergent cholecystectomy in high‐risk elderly patients, percutaneous cholecystostomy resulted in reduced hospital stay and morbidity (p = 0.002 and p = 0.013, respectively). Our results demonstrate that percutaneous cholecystostomy has become a common and early treatment for AC in high‐risk elderly patients with ischemic heart disease or chronic kidney disease. Identifying such patients will possibly improve clinical outcomes, reduce hospital stay and morbidity, and facilitate delayed laparoscopic cholecystectomy.
Pressure fluctuations induced by a hypersonic turbulent boundary layer
Authors: Duan Lian , Choudhari Meelan M. , Zhang Chao
Published: September 2016

Direct numerical simulations (DNS) are used to examine the pressure fluctuations generated by a spatially developed Mach 5.86 turbulent boundary layer. The unsteady pressure field is analysed at multiple wall-normal locations, including those at the wall, within the boundary layer (including inner layer, the log layer, and the outer layer), and in the free stream. The statistical and structural variations of pressure fluctuations as a function of wall-normal distance are highlighted. Computational predictions for mean-velocity profiles and surface pressure spectrum are in good agreement with experimental measurements, providing a first ever comparison of this type at hypersonic Mach numbers. The simulation shows that the dominant frequency of boundary-layer-induced pressure fluctuations shifts to lower frequencies as the location of interest moves away from the wall. The pressure wave propagates with a speed nearly equal to the local mean velocity within the boundary layer (except in the immediate vicinity of the wall) while the propagation speed deviates from Taylor’s hypothesis in the free stream. Compared with the surface pressure fluctuations, which are primarily vortical, the acoustic pressure fluctuations in the free stream exhibit a significantly lower dominant frequency, a greater spatial extent, and a smaller bulk propagation speed. The free-stream pressure structures are found to have similar Lagrangian time and spatial scales as the acoustic sources near the wall. As the Mach number increases, the free-stream acoustic fluctuations exhibit increased radiation intensity, enhanced energy content at high frequencies, shallower orientation of wave fronts with respect to the flow direction, and larger propagation velocity.
Giant Molecular Cloud Populations in Nearby Galaxies
Authors: Hughes Annie , Meidt Sharon , Colombo Dario , Schruba Andreas , Schinnerer Eva , Leroy Adam , Wong Tony ,   the PAWS, MAGMA, CANON and M31-CARMA survey teams
Published: September 2016

We present new results from a comparative analysis of the resolved giant molecular cloud (GMC) populations in six nearby galaxies. We show that the GMCs in denser environments–M51, the centre of NGC6946–have greater CO surface brightness and higher velocity dispersions relative to their size than GMCs in less dense environments. We find systematic differences in the GMC mass distribution among galaxies, such that more of the molecular gas in the low-mass galaxies (M33, the Large Magellanic Cloud) and the outer disk of M31 is located in low mass clouds. Using the number density of GMCs in the interarm regions of M51, we argue that GMC destruction in this region is regulated by shear, and that cloud lifetimes there are finite and short, ~20 to 30 Myr. Our results indicate the importance of galactic environment on the evolution of GMCs, and on a galaxy's global pattern of star formation.
Probing star formation relations of mergers and normal galaxies across the CO ladder
Authors: Greve Thomas R.
Published: September 2016

We examine integrated luminosity relations between the IR continuum and the CO rotational ladder observed for local (ultra) luminous infra-red galaxies ((U)LIRGs, LIR ≥ 1011 M⊙) and normal star forming galaxies in the context of radiation pressure regulated star formation proposed by Andrews & Thompson (2011). This can account for the normalization and linear slopes of the luminosity relations (log LIR = α log L'CO + β) of both low- and high-J CO lines observed for normal galaxies. Super-linear slopes occur for galaxy samples with significantly different dense gas fractions. Local (U)LIRGs are observed to have sub-linear high-J (Jup > 6) slopes or, equivalently, increasing LCOhigh-J/LIR with LIR. In the extreme ISM conditions of local (U)LIRGs, the high-J CO lines no longer trace individual hot spots of star formation (which gave rise to the linear slopes for normal galaxies) but a more widespread warm and dense gas phase mechanically heated by powerful supernovae-driven turbulence and shocks.
The Formation and Destruction of Molecular Clouds and Galactic Star Formation
Authors: Inutsuka Shu-ichiro , Inoue Tsuyoshi , Iwasaki Kazunari , Hosokawa Takashi , Kobayashi Masato I. N.
Published: September 2016

We discuss an overall picture of star formation in the Galaxy. Recent high-resolution magneto-hydrodynamical simulations of two-fluid dynamics with cooling/heating and thermal conduction have shown that the formation of molecular clouds requires multiple episodes of supersonic compression. This finding enables us to create a new scenario of molecular cloud formation through interacting shells or bubbles on galactic scales. We estimate the ensemble-averaged growth rate of individual molecular clouds, and predict the associated cloud mass function. This picture naturally explains the accelerated star formation over many million years that was previously reported by stellar age determination in nearby star forming regions. The recent claim of cloud-cloud collisions as a mechanism for forming massive stars and star clusters can be naturally accommodated in this scenario. This explains why massive stars formed in cloud-cloud collisions follows the power-law slope of the mass function of molecular cloud cores repeatedly found in low-mass star forming regions.
Observational studies of the formation and evolution of dense cores
Authors: Tafalla Mario
Published: September 2016

Dense cores are the simplest star-forming sites. They represent the end stage of the fragmentation hierarchy that characterizes molecular clouds, and they likely control the efficiency of star formation via their relatively low numbers. Recent dust continuum observations of entire molecular clouds show that dense cores often lie along large-scale filamentary structures, suggesting that the cores form by some type of fragmentation process in an approximately cylindrical geometry. To understand the formation mechanism of cores, additional kinematic information is needed, and this requires observations in molecular-line tracers of both the dense cores and their surrounding cloud material. Here I present some recent efforts to clarify the kinematic structure of core-forming regions in the nearby Taurus molecular cloud. These new observations show that the filamentary structures seen in clouds are often more complex than suggested by the maps of continuum emission, and that they consist of multiple fiber-like components that have different velocities and sonic internal motions. These components likely arise from turbulent fragmentation of the large-scale flows that generate the filamentary structures. While not all these fiber-like components further fragment to form dense cores, a small group of them does so, likely by gravitational instability. This fragmentation produces characteristic chain-like groups of dense cores that further evolve to form stars.
Small-scale properties of Class 0 protostars from the CALYPSO IRAM-PdBI survey
Authors: Maury Anaëlle , André Philippe , Maret Sébastien , Belloche Arnaud , Codella Claudio , Cabrit Sylvie , Gueth Frédéric ,   CALYPSO collaboration
Published: September 2016

Because the formation of protostars is believed to be closely tied to the angular momentum problem of star formation, characterizing the properties of the youngest disks around Class 0 objects is crucial. However, not much is known on the structure of the youngest protostellar envelopes, on the small scales at which disks and multiple systems are observed around more evolved YSOs, due to a lack of comprehensive high angular resolution observations (probing <100 AU). In order to tackle this issue, we conducted a large observing program with the IRAM Plateau de Bure interferometer (PdBI): the CALYPSO survey, providing us with detailed maps of molecular lines and millimeter continuum emission, probing scales down to ~30–50 au towards a sample of 17 Class 0 protostars. Here we present our analysis of the CALYPSO dust continuum emission maps, constraining disk properties of the Class 0 protostars in our sample. We show that large, r > 50 au, disk structures are not observed in most Class 0 protostars from our sample, which can be described by various envelope models reproducing satisfactorily the intensity distribution of the dust emission at all scales from 50 au to 5000 au.
SMA and ALMA studies of protoplanetary disk formation around low-mass protostars
Authors: Takakuwa Shigehisa , Ohashi Nagayoshi , Yen Hsi-Wei , Chou Ti-Lin , Saigo Kazuya , Saito Masao , Aso Yusuke , Aikawa Yuri , Koyamatsu Shin , Machida Masahiro N. , Takahashi Sanemichi Z. , Tomida Kengo , Tomisaka Kohji
Published: September 2016

We report our systematic survey observations of protostellar sources with the SubMillimeter Array (SMA) and Atacama Large Millimeter/submillimeter Array (ALMA). The purpose of our survey is to investigate formation mechanism of protoplanetary disks, precursors of planetary systems, out of ~1000 AU-scale protostellar envelopes surrounding the protostars. We found that in the early protostars (B335, NGC1333 IRAS 4B), the envelopes do not show significant rotating motions but infalling motions toward the central protostars. In more evolved protostars (L1527 IRS, L1448-mm, L1551 IRS 5), the envelopes are infalling and rotating with the conserved specific angular momenta (that is, vrot ∝ r−1). In most evolved sources (L1551 NE, TMC-1A, L1489 IRS) large-scale (≳100 AU) disks in Keplerian rotation or protoplanetary disks are evident. These results demonstrate a systematic evolutionary trend of envelope gas motions toward the disk formation.
Central Molecular Zone of the Milky Way: Star Formation in an extreme Environment
Authors: Kauffmann Jens
Published: September 2016

The Central Molecular Zone (CMZ; inner ~100 pc) hosts some of the most dense and massive molecular clouds of the Milky Way. These clouds might serve as local templates for dense clouds seen in nearby starburst galaxies or in the early universe. The clouds have a striking feature: they form stars at a very slow pace, considering their mass and high average density. Here we use interferometer data from ALMA and the SMA to show that this slow star formation is a consequence of the cloud density structure: CMZ clouds have a very flat density structure. They might, for example, exceed the average density of the Orion A molecular cloud by an order of magnitude on spatial scales ~5 pc, but CMZ “cores” of ~0.1 pc radius have masses and densities lower than what is found in the Orion KL region. This absence of highest–density gas probably explains the suppression of star formation. The clouds are relatively turbulent, and ALMA observations of H2CO and SiO indicate that the turbulence is induced by high–velocity shocks. We speculate that these shocks might prevent the formation of high–mass cores. It has been argued that the state of CMZ clouds depends on their position along the orbit around Sgr A*. Our incomplete data indicate no evolution in the density structure, and only a modest evolution in star formation activity per unit mass.
Local Physics and Star Formation in Galaxies
Authors: Leroy Adam K. , Bigiel Frank , Hughes Annie , Schinnerer Eva , Usero Antonio ,   the PAWS, EMPIRE, and HERACLES Dense Gas Collaborations
Published: September 2016

A next main step in understanding star formation is to link the sharp but narrow view of Galactic molecular cloud studies to the wider context accessed by less detail by extragalactic work. In this proceeding, we discuss how new technology and large programs at millimeter wavelengths are improving our ability to access physical conditions in the interstellar medium (ISM) of other galaxies. We highlight results from the multi-line survey of Usero et al. (2015), which measured density sensitive lines across nearby galaxy disks, and two new mapping studies of M51: the high resolution Plateau de Bure Arcsecond Whirlpool Survey (PAWS) and the EMPIRE multi-line mapping survey. These results argue for a context-dependent role for gas density in star formation; that is, gas at a particular density does not appear to form stars in a universal way. They also demonstrate the influence of cloud-scale conditions, especially surface density and the velocity dispersion, in setting the small-scale density distribution and highlight gravitational boundedness as a main driver of the ability of gas to form stars. Beyond these specific results, we argue that ability to gauge detailed physical conditions in the star-forming gas of other galaxies promises major advances that will help unify the fields of Galactic and extragalactic star formation in the next few years.
How does metallicity affect the gas and dust properties of galaxies?
Authors: Madden Suzanne C. , Cormier Diane , Rémy-Ruyer Aurélie
Published: September 2016

Comparison of the ISM properties of a wide range of metal poor galaxies with normal metal-rich galaxies reveals striking differences. We find that the combination of the low dust abundance and the active star formation results in a very porous ISM filled with hard photons, heating the dust in dwarf galaxies to overall higher temperatures than their metal-rich counterparts. This results in photodissociation of molecular clouds to greater depths, leaving relatively large PDR envelopes and difficult-to-detect CO cores. From detailed modeling of the low-metallicity ISM, we find significant fractions of CO-dark H2 - a reservoir of molecular gas not traced by CO, but present in the [CII] and [CI]-emitting envelopes. Self-consistent analyses of the neutral and ionized gas diagnostics along with the dust SED is the necessary way forward in uncovering the multiphase structure of galaxies.
AGN feedback and star formation in ETGs: negative and positive feedback
Authors: Ciotti Luca , Ostriker Jeremiah P. , Negri Andrea , Pellegrini Silvia , Posacki Silvia , Novak Greg
Published: September 2016

AGN feedback from supermassive black holes (SMBHs) at the center of early type galaxies is commonly invoked as the explanation for the quenching of star formation in these systems. The situation is complicated by the significant amount of mass injected in the galaxy by the evolving stellar population over cosmological times. In absence of feedback, this mass would lead to unobserved galactic cooling flows, and to SMBHs two orders of magnitude more massive than observed. By using high-resolution 2D hydrodynamical simulations with radiative transport and star formation in state-of-the-art galaxy models, we show how the intermittent AGN feedback is highly structured on spatial and temporal scales, and how its effects are not only negative (shutting down the recurrent cooling episodes of the ISM), but also positive, inducing star formation in the inner regions of the host galaxy.
High Mass Star Formation: Properties of NH3 clumps in Southern Galactic Plane
Authors: Akhter Shaila , Cunningham Maria R. , Harvey-Smith Lisa , Nawaz Mohammad Ali , Jones Paul A. , Purcell Cormac , Walsh Andrew
Published: September 2016

Massive stars are some of the most important objects in the Universe, shaping the evolution of galaxies, creating chemical elements, and hence shaping the evolution of the Universe. However, the processes by which they form, and how they shape their environment during their birth processes, are not well understood. We are using NH3 data from the “The H2O Southern Galactic Plane Survey” (HOPS) to define the positions of dense cores/clumps of gas in the southern Galactic plane that are likely to form stars. We did a comparative study with different methods for finding clumps and found Fellwalker to be the best for this dataset. We detected ~ 500 clumps with mean kinetic temperature ~ 20 K and virial mass ~ 680 solar masses.
A supernova scenario for magnetic fields and rotation measures in galaxies
Authors: Beck Alexander M. , Dolag Klaus
Published: September 2016

We present a model for the seeding and evolution of magnetic fields in galaxies by supernovae (SN). SN explosions during galaxy assembly provide seed fields, which are subsequently amplified by compression, shear flows and random motions. Our model explains the origin of μG magnetic fields within galactic structures. We implement our model in the MHD version of the cosmological simulation code Gadget-3 and couple it with a multi-phase description of the interstellar medium. We perform simulations of Milky Way-like galactic halo formation and analyze the distribution and strength of the magnetic field. We investigate the intrinsic rotation measure (RM) evolution and find RM values exceeding 1000 rad/m2 at high redshifts and RM values around 10 rad/m2 at present-day. We compare our simulations to a limited set of observational data points and find encouraging similarities. In our model, galactic magnetic fields are a natural consequence of the very basic processes of star formation and galaxy assembly.
Detection and measurement of expanding ionized shells around young star clusters
Authors: Beckman John , Fariña Artemi Camps , Cardiel Javier Zaragoza , Font Joan
Published: September 2016

We present a new method (BUBBLY) for detecting expanding components of ionized gas using integral field spectroscopy, showing its capabilities not only in detecting but also in obtaining the key physical parameters of the expanding shells: their expansion velocities and masses. The main advantages are that the detection is performed automatically via software and that we can derive most parameters of the shells, so it is suitable for detailed studies of feedback in nearby galaxies. The software can easily be configured to run on any data cube mapping an emission line over a spatial field. We also present results obtained by running BUBBLY on observations of Hα emission with the Fabry-Perot spectrograph GHαFaS: two sets of spectacular results at widely different spatial scales: the Antennae galaxies show multiple giant bubbles of size ~300pc around the brightest clusters, while inside a region in M33 we find three nested supernova remnants, with which we can study the feedback on the molecular gas surrounding the cluster.
A Statistical Comparison of the Near Infrared Emission with the Hα Emission from the HII regions of NGC4321, NGC4736 and NGC4254
Authors: Beckman J.E. , Chan S.J. , Li A. , Borissova J.
Published: September 2016

We report on our ongoing project “Statistical studies of HII regions in the nearby extra-galaxies”. We present an overview of our detailed study of warm dust in the nearby Galaxy NGC 4321 (M100), measuring the flux values in the 4 Spitzer-IRAC bands of some 275 HII regions in M100. In addition, we present new measurements of the flux values in the 4 Spitzer-IRAC bands of a complete sample of 70 isolated luminous HII regions in NGC 4736 and 157 regions in NGC 4254. We study the relations between the Hα luminosity and the near-IR luminosity and temperature of HII regions in the three galaxies. We estimate the near-IR luminosities and compare them with the Hα luminosities from archive and literature sources. We find a linear relation between the Hα luminosity and the IRAC luminosity for the HII regions, but no apparent relation between the luminosity and the colour temperature of the regions in any of the three galaxies. The colour temperatures of regions especially in M100 and NGC4254 are confined to a surprisingly narrow range, with a small fraction forming a higher temperature tail to the distribution. These results give new insight into the size function and the 3D distribution of the dust in these regions, and we propose scenarios to explain them.
Time evolution of chemistry with fixed physical parameters in TMC-1
Authors: Berczik Peter , Bertsyk Peter , Fehér Orsolya , Harju Jorma , Onishi Toshikazu , Tóth L. Viktor
Published: September 2016

We present a set of time dependent chemical evolution models (based on the UMIST† astrochemistry 2012 code, Woodall et al. (2007); McElroy et al. (2013) for a range of initial physical cloud parameters: 10 K < T < 20 K; 103 cm−3 < n(H2) < 5 · 104 cm−3; 1 < AV < 10 and with estimated values of scaled interstellar ultraviolet radiation field. Our computation model included the full UMIST gas-phase reaction network for 467 species Garrod et al. (2008), Graedel et al. (1982). We compare our chemical model results with the relative abundances of: CO, CH, OH, HCO+, HCN, HNC, NH3, N2H+ and H2CO molecules. We find significant time dependent variations of the chemical ratios of: X(NH3/H2); X(HCO+/H2) and X(HCO+/NH3). We derive an ammonia age spread for the parts of TMC-1 (Taurus Molecular Cloud-1) that looks more complex than previous estimated showed. Age estimates based on X(NH3/H2); X(HCO+/H2) and X(HCO+/NH3) were compared in 3 selected positions, and were found to be very similar (with ±9% differences).
Quantifying the Magnetic Alignment of Hi and Dust in the Diffuse ISM
Authors: Clark S.E. , Peek J.E.G. , Hill J. Colin , Putman M.E.
Published: September 2016

Sensitive, high resolution observations of Galactic neutral hydrogen (Hi) reveal an intricate network of slender linear features, much as sensitive surveys of dust in Galactic molecular clouds reveal ubiquitous filamentary structure. Across the high Galactic latitude sky, diffuse Histructures are aligned with the interstellar magnetic field, as revealed by background starlight polarization (Clark, Peek, & Putman 2014) and by Planck 353 GHz polarized dust emission (Clark et al. 2015). These discoveries were enabled by the Rolling Hough Transform, a recently developed, open source machine vision algorithm.
OH as a Probe of The Milky Way's Hidden Gas: First Results from SPLASH
Authors: Dawson J. R. , Walsh A. J. ,   The SPLASH Team
Published: September 2016

SPLASH (the Southern Parkes Large-Area Survey in Hydroxyl) is a deep survey of ground-state OH absorption and emission from the Galactic Plane, as well as an unbiased search for OH masers. Key early results include the detection of a rich and complex distribution of diffuse, optically thin OH with strongly non-thermal excitation temperatures, and the detection of numerous new maser sources. The survey aims to use OH as a probe of CO-dark H2 ISM Galactic scales, with future plans including comprehensive comparisons with CO and Hi, as well as non-LTE excitation modelling of the four ground-state lines.
A Green Bank Telescope Search for Highly Extended HI Disks Around Spiral Galaxies
Authors: Ford H. Alyson , Bregman Joel N.
Published: September 2016

Recent UV absorption line studies suggest that a large fraction of missing baryons are in the warm ionized and neutral phases, with about half of Milky Way-mass galaxies containing absorption systems with HI column densities of 1018 cm−2 or greater. This HI gas, which would have been difficult to detect with previous instruments, could be a significant contributor to the missing baryons. The Green Bank Telescope (GBT) presents a unique opportunity to detect this emission. We present results from GBT 21 cm observations of a sample of ten nearby optically luminous spirals, which reveal extended HI gas in half of our sample. The column densities of this extended HI are typically ~ 1 × 1019 cm−2, as measured at distances of 100 kpc from the center of the galaxies.
A Global View of Molecule-Forming Clouds in the Galaxy
Authors: Gibson Steven J. , Howard Ward S. , Jolly Christian S. , Newton Jonathan H. , Bell Aaron C. , Spraggs Mary E. , Hughes J. Marcus , Tagliaboschi Aaron M. , Brunt Christopher M. , Taylor A. Russell , Stil Jeroen M. , Dame Thomas M.
Published: September 2016

We have mapped cold atomic gas in 21cm line H i self-absorption (HISA) at arcminute resolution over more than 90% of the Milky Way's disk. To probe the formation of H2 clouds, we have compared our HISA distribution with CO J = 1-0 line emission. Few HISA features in the outer Galaxy have CO at the same position and velocity, while most inner-Galaxy HISA has overlapping CO. But many apparent inner-Galaxy HISA-CO associations can be explained as chance superpositions, so most inner-Galaxy HISA may also be CO-free. Since standard equilibrium cloud models cannot explain the very cold H i in many HISA features without molecules being present, these clouds may instead have significant CO-dark H2.
Investigating formation of isolated intermediate/massive YSOs in the LMC
Authors: Harada Ryohei , Onishi Toshikazu , Hughes Annie , Meixner Margaret , Sewilo Marta , Indebetouw Remy , Nayak Omnarayani , Tokuda Kazuki , Morioka Yuuki , Fukui Yasuo , Kawamura Akiko , Wong Tony , Bernard Jean-Philippe
Published: September 2016

High-mass stars usually form in giant molecular clouds (GMCs) as part of a young stellar cluster, but some isolated O/B stars are observed. What are the initial conditions that lead to the formation of these objects? The aim of this study is to measure the distribution and basic physical properties of the neutral gas associated with isolated intermediate- and high-mass young stellar objects (YSOs) in the Large Magellanic Cloud.

As part of the SAGE Spitzer Legacy program for the LMC, we have identified and confirmed YSOs using Spitzer IRAC photometry and IRS spectroscopy. By examining the spatial coincidence between the YSOs and 12CO(1–0) emission detected by the NANTEN mapping survey, we identified more than one hundred intermediate/massive YSOs in the LMC that appear to be isolated, i.e. not associated with CO emission. Deeper follow-up CO observations by our team with the higher resolution by Mopra Telescope (beam=30”) detected CO emission at the YSO positions for ~80% of the isolated LMC YSOs. We obtained ALMA data of some of the targets during Cycle 2. We targeted a small but representative (in terms of their association with neutral gas tracers) sample of the isolated high-mass YSOs that we have been studying in the LMC. All of our 12 targets are separated by more than 200 pc from known CO clouds. Our analysis of the ALMA data shows that a compact molecular cloud whose mass is a few thousand solar masses or smaller is associated with most of the YSOs.
The Real Solar Neighborhood Protostars
Authors: Heiderman Amanda L. , Evans Neal J.
Published: September 2016

Characterization of how dense molecular cores evolve into stars has historically been made through observational changes in their 2 to 25 μm spectral energy distribution (SED) or bolometric temperature via the Class system. Linking these observational classes to a physical protostellar phase or Stages in a consistent manner remains challenging. In order to provide a uniform indicator of whether an observationally classified embedded protostar candidate is likely to be a physical phase Stage 0 or I protostar, we performed an HCO+(J=3-2) survey of Class 0+I and Flat SED young stellar objects (YSOs) in the Spitzer nearby (D < 500 pc) Gould Belt cloud surveys. We use criteria from van Kempen et al.(2009) to classify sources as Stage 0+I or bona fide protostars and find 84% of our HCO+ detected sources meet that criteria. We recommend 0.54 Myr as an evolutionary timescale for these embedded protostars. We discuss trends in our sample with spatial distribution, molecular cloud extinction, spectral index, and bolometric temperature and luminosity.
Results from the Herschel Gould Belt Survey in the Ophiuchus Main Cloud
Authors: Ladjelate Bilal , André Philippe , Könyves Vera , Men'shchikov Alexander ,   the HGBS team
Published: September 2016

As part of the Herschel Gould Belt Survey (HGBS), the Ophiuchus molecular cloud was imaged in the submillimeter range. Here, we summarize and briefly discuss the main results.
The HerMES Local Luminosity Function
Authors: Marchetti Lucia , Vaccari Mattia , Franceschini Alberto
Published: September 2016

We exploit the Herschel Extragalactic Multi-Tiered Survey (HerMES) dataset along with ancillary multi-wavelength photometry and spectroscopy from the Spitzer Data Fusion to provide the most accurate determination to date of the local (0.02<z<0.5) Far-Infrared Luminosity and Star Formation Rate Function. We present and compare our results with model predictions as well as other multi-wavelength estimates of the local star formation rate density.
The Herschel Point Source Catalogue
Authors: Marton G. , Schulz B. , Altieri B. , Calzoletti L. , Kiss Cs. , Lim T. , Lu N. , Paladini R. , Papageorgiou A. , Pearson C. , Rector J. , Shupe D. , Valtchanov I. , Verebélyi E. , Xu K.
Published: September 2016

The Herschel Space Observatory was the fourth cornerstone mission in the European Space Agency (ESA) science programme with excellent broad band imaging capabilities in the sub-mm and far-infrared part of the spectrum. Although the spacecraft finished its observations in 2013, it left a large legacy dataset that is far from having been fully scrutinised and still has a large potential for new scientific discoveries. This is specifically true for the photometric observations of the PACS and SPIRE instruments. Some source catalogues have already been produced by individual observing programs, but there are many observations that risk to remain unexplored. To maximise the science return of the SPIRE and PACS data sets, we are in the process of building the Herschel Point Source Catalogue (HPSC) from all primary and parallel mode observations. Our homogeneous source extraction enables a systematic and unbiased comparison of sensitivity across the different Herschel fields that single programs will generally not be able to provide. The catalogue will be made available online through archives like the Herschel Science Archive (HSA), the Infrared Science Archive (IRSA), and the Strasbourg Astronomical Data Center (CDS).
Mass–metallicity relation for AKARI-FMOS infrared luminous galaxies at z ~ 0.9
Authors: Oi Nagisa , Matsuhara Hideo , Goto Tomotsugu , Pearson Chris , Buat Véronique , Malkan Matthew A.
Published: September 2016

We study the mass–metallicity relation and fundamental relation (FMR) for infrared bright galaxies (IR galaxies) at z ~ 0.9 discovered by AKARI NEP-Deep survey. The main result of this work is that metallicity of IR galaxies surprisingly match optical selected galaxies at a given mass even their star formation rates are different, which may imply that optical and IR selected galaxies follow similar star formation histories, and the starbursts in the IR galaxies do not give a strong impact in changing metallicity because of the short duration time.
A Full Virial Analysis of the Prestellar Cores in the Ophiuchus Molecular Cloud
Authors: Pattle Kate , Ward-Thompson Derek
Published: September 2016

We use SCUBA-2, HARP C18O J= 3 → 2, Herschel and IRAM N2H+ J= 1 → 0 observations of the Ophiuchus molecular cloud to identify and characterise the properties of the starless cores in the region. The SCUBA-2, HARP and Herschel data were taken as part of the JCMT and Herschel Gould Belt Surveys. We determine masses and temperatures and perform a full virial analysis on our cores, and find that our cores are all either bound or virialised, with gravitational energy and external pressure energy on average of similar importance in confining the cores. There is wide variation from region to region, with cores in the region influenced by B stars (Oph A) being substantially gravitationally bound, and cores in the most quiescent region (Oph C) being pressure-confined. We observe dissipation of turbulence in all our cores, and find that this dissipation is more effective in regions which do not contain outflow-driving protostars. Full details of this analysis are presented by Pattle et al. (2015).
Multiphase ISM in low luminosity radio galaxies: A case study of NGC 708
Authors: Sahu Sheetal K , Pandey S K , Chaware L , Pandge M B
Published: September 2016

We present a multi-wavelength study of a nearby radio loud elliptical galaxy NGC 708, selected from the Bologna B2 sample of radio galaxies. We obtained optical broad band and narrow images from IGO 2m telescope (Pune, India). We supplement the multi-wavelength coverage of the observation by using X-ray data from Chandra, infrared data from 2MASS, Spitzer and WISE and optical image from DSS and HST. In order to investigate properties of interstellar medium, we have generated unsharp-masked, color, residual, quotient, dust extinction, Hα emission maps. From the derived maps it is evident that cool gas, dust, warm ionized Hα and hot X-ray gas are spatially associated with each other. We investigate the inner and outer photometric and kinematic properties of the galaxy using surface brightness profiles. From X-ray 2d beta model, unsharp masking, surface brightness profiles techniques, it is evident that pair of X-ray cavities are present in this system and which are ~5.6 Kpc away from the central X-ray source.
Molecular Gas Excitation and Chemistry in VV 114 and NGC 1614 with ALMA
Authors: Saito Toshiki , Iono Daisuke , Ueda Junko , Yun Min S. , Nakanishi Kouichiro , Sugai Hajime , Imanishi Masatoshi , Hagiwara Yoshiaki , Kaneko Hiroyuki , Motohara Kentaro , Espada Daniel , Yamashita Takuji , Lee Minju , Michiyama Tomonari , Kawabe Ryohei
Published: September 2016

We present high resolution molecular line observations of dusty AGN and starburst in nearby luminous infrared galaxies (LIRGs), VV 114 (band 3/4/7) and NGC 1614 (band 3/6/7/9), with ALMA. Multi-frequency imaging from 4.8 GHz to 691 GHz of NGC 1614 allows us to study spatial properties of the radio-to-FIR continuum and multiple CO transitions, and we find the CO excitation up to Jupp = 6 can be explained by a single ISM model powered by nuclear starbursts. Our processing line imaging survey for VV 114 detected at least 30 molecular lines which show different chemical composition from region to region. Multi-molecule imaging helps us to diagnose the chemical differences of dusty ISM, while multi-transition imaging allows us to investigate gas physical conditions affected by nuclear activities directly.
ALMA Observations of a High-density Core in Taurus: Dynamical Gas Interaction at the Possible Site of a Multiple Star Formation
Authors: Tokuda Kazuki , Onishi Toshikazu , Saigo Kazuya , Kawamura Akiko , Fukui Yasuo , Matsumoto Tomoaki , Inutsuka Shu-ichiro , Machida Masahiro N. , Tomida Kengo , Tachihara Kengo
Published: September 2016

It is crucially important to observe dense cores in order to investigate the initial condition of star formation since protostars are formed via dynamical collapse of dense cores, inhering the physical properties from their natal dense cores. Here we present the results of ALMA Cycle 0 and Cycle 1 observations of dust continuum emission and molecular rotational lines toward a dense core, MC27 (aka L1521F), which is considered to be very close to the first protostellar core phase. We revealed the spatial/velocity structures of the core are very complex and and suggest that the star formation is highly dynamical.
Star formation in Taurus Auriga Perseus and California nebulae
Authors: Tóth L. Viktor , Zahorecz Sarolta , Marton Gabor , Doi Yasuo , Onishi Toshikazu , Tokuda Kazuki
Published: September 2016

Star formation and interstellar medium (ISM) structure were investigated in the Taurus, Auriga, Perseus and California (TAP) nearby star forming regions. Properties of the cold ISM was derived using AKARI FIR all sky maps, the Osaka-1.85m CO survey focusing to the all-sky Planck catalogue of Galactic Cold Clumps (PGCC). As many as 1041 infrared point sources were classified as young stellar object (YSO) based on multiband photometric data, and 384 of those are associated to a PGCC object. About 30% of the TAP PGCC clumps have associated YSOs.
Dust Temperatures and Opacities in the Central Parsec of the Galactic Center Modeled from Analysis of Multi-wavelength Mid-infrared Images
Authors: Varosi F. , Gezari D. , Dwek E. , Telesco C.
Published: September 2016

We have analyzed multi-wavelength mid-infrared images of the central parsec of the Galactic Center using a two-temperature line-of-sight (LOS) radiative transfer model at each pixel of the images, giving maps of temperatures, luminosities and opacities of the hot, warm, cold (dark) dust components. The data consists of images at nine wavelengths in the mid-infrared (N-band and Q-band) from the Thermal Region Camera and Spectrograph (T-ReCS) instrument operating at the Gemini South Observatory. The results of the LOS modeling indicate that the extinction optical depth is quite large and varies substantially over the FOV.