bluuebunny/crossref_metadata_2025_split huggingface dataset:
Domestic incense use and lung cancer in Asia: a review
Authors: Seow Wei Jie , Lan Qing 
Published: January 2016

Abstract
While there is strong evidence for the association between household air pollution and lung cancer among non-smoking women, the association between domestic incense use and lung cancer risk has been inconsistent. We conducted a systematic review of PubMed articles authored between 1969 and August 25, 2015 before performing a manual review of each study, and found a total of seven published studies on this topic. Most of the studies are case-control in design and did not further stratify by sex and smoking status. Of the seven studies, three reported positive associations, three reported null associations and one study found a negative association between incense use and lung cancer. Only one study reported estimates for non-smoking women. Future studies should be larger in sample size, stratify by both sex and smoking status in their analyses, and collect more detailed information on incense use in order to facilitate the understanding of the association between domestic incense use and lung cancer risk among non-smoking women in Asia.
Effects of manufacturing environments on the residual stresses in a SiC/Ti metal-matrix composite
Authors: Aghdam Mohammad Mohammadi , Morsali Seyed Reza 
Published: January 2016

Abstract
A three-dimensional micromechanical finite element model is developed to study the effects of a manufacturing environment on thermal residual stresses in a SiC/Ti-6Al-4V metal-matrix composite. The model includes a representative volume element consisting of a quarter of SiC fiber covered by relatively thick coating and an interaction layer all of which are surrounded by the Ti-6Al-4V matrix. Stress relaxation due to the viscoplastic behavior of the matrix is accounted for different manufacturing environments, that is, air and nitrogen. The results show that the presented model provides accurate predictions when compared with experimental data. It is possible to use the presented results for appropriate selection of manufacturing parameters. The results suggest that to delay the onset of interface debonding, the best choice is to use cooling rates higher than 0.64 and 0.1°C/s, respectively, for air and nitrogen environments. In order to use simple elastic-plastic models to predict residual stresses within the composite, detailed equivalent stress-free temperatures for various environments, cooling rates, and fiber volume fractions are presented.
OPTICAL SPECTROSCOPY OF SDSS J004054.65-0915268: THREE POSSIBLE SCENARIOS FOR THE CLASSIFICATION. A z ∼ 5 BL LACERTAE, A BLUE FSRQ, OR A WEAK EMISSION LINE QUASAR
Authors: Landoni M. , Zanutta A. , Bianco A. , Tavecchio F. , Bonnoli G. , Ghisellini G. 
Published: January 2016

ABSTRACT
The haunt of high-redshift BL Lacerate objects is day by day more compelling to firmly understand their intrinsic nature and evolution. SDSS J004054.65-0915268 is, at the moment, one of the most distant BL Lac candidates, at z ∼ 5. We present a new optical-near-IR spectrum obtained with ALFOSC-NOT with a new, custom designed dispersive grating aimed to detect broad emission lines that could disprove this classification. In the obtained spectra, we do not detect any emission features and we provide an upper limit to the luminosity of the C iv broad emission line. Therefore, the nature of the object is then discussed, building the overall spectral energy distribution (SED) and fitting it with three different models. Our fits, based on SED modeling with different possible scenarios, cannot rule out the possibility that this source is indeed a BL Lac object, though the absence of optical variability and the lack of strong radio flux seem to suggest that the observed optical emission originates from a thermalized accretion disk.
WISE PHOTOMETRY FOR 400 MILLION SDSS SOURCES
Authors: Lang Dustin , Hogg David W. , Schlegel David J. 
Published: January 2016

ABSTRACT
We present photometry of images from the Wide-Field Infrared Survey Explorer (WISE) of over 400 million sources detected by the Sloan Digital Sky Survey (SDSS). We use a “forced photometry” technique, using measured SDSS source positions, star–galaxy classification, and galaxy profiles to define the sources whose fluxes are to be measured in the WISE images. We perform photometry with The Tractor image modeling code, working on our “unWISE” coaddds and taking account of the WISE point-spread function and a noise model. The result is a measurement of the flux of each SDSS source in each WISE band. Many sources have little flux in the WISE bands, so often the measurements we report are consistent with zero given our uncertainties. However, for many sources we get 3σ or 4σ measurements; these sources would not be reported by the “official” WISE pipeline and will not appear in the WISE catalog, yet they can be highly informative for some scientific questions. In addition, these small-signal measurements can be used in stacking analyses at the catalog level. The forced photometry approach has the advantage that we measure a consistent set of sources between SDSS and WISE, taking advantage of the resolution and depth of the SDSS images to interpret the WISE images; objects that are resolved in SDSS but blended together in WISE still have accurate measurements in our photometry. Our results, and the code used to produce them, are publicly available at http://unwise.me.
OBSERVATION OF TWO NEW L4 NEPTUNE TROJANS IN THE DARK ENERGY SURVEY SUPERNOVA FIELDS
Authors: Gerdes D. W. , Jennings R. J. , Bernstein G. M. , Sako M. , Adams F. , Goldstein D. , Kessler R. , Hamilton S. , Abbott T. , Abdalla F. B. , Allam S. , Benoit-Lévy A. , Bertin E. , Brooks D. , Buckley-Geer E. , Burke D. L. , Capozzi D. , Rosell A. Carnero , Kind M. Carrasco , Carretero J. , Cunha C. E. , D’Andrea C. B. , Costa L. N. da , DePoy D. L. , Desai S. , Dietrich J. P. , Doel P. , Eifler T. F. , Neto A. Fausti , Flaugher B. , Frieman J. , Gaztanaga E. , Gruen D. , Gruendl R. A. , Gutierrez G. , Honscheid K. , James D. J. , Kuehn K. , Kuropatkin N. , Lahav O. , Li T. S. , Maia M. A. G. , March M. , Martini P. , Miller C. J. , Miquel R. , Nichol R. C. , Nord B. , Ogando R. , Plazas A. A. , Romer A. K. , Roodman A. , Sanchez E. , Santiago B. , Schubnell M. , Sevilla-Noarbe I. , Smith R. C. , Soares-Santos M. , Sobreira F. , Suchyta E. , Swanson M. E. C. , Tarlé G. , Thaler J. , Walker A. R. , Wester W. , Zhang Y. ,   The DES Collaboration
Published: January 2016

ABSTRACT
We report the discovery of the eighth and ninth known Trojans in stable orbits around Neptune’s leading Lagrange point, L4. The objects 2014 QO441 and 2014 QP441 were detected in data obtained during the 2013–14 and 2014–15 observing seasons by the Dark Energy Survey, using the Dark Energy Camera (DECam) on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory. Both are in high-inclination orbits (18.°8 and 19.°4, respectively). With an eccentricity of 0.104, 2014 QO441 has the most eccentric orbit of the 11 known stable Neptune Trojans. Here we describe the search procedure and investigate the objects’ long-term dynamical stability and physical properties.
THE OFFSET AND HOST LIGHT DISTRIBUTIONS OF LONG GAMMA-RAY BURSTS: A NEW VIEW FROM HST OBSERVATIONS OF SWIFT BURSTS
Authors: Blanchard Peter K. , Berger Edo , Fong Wen-fai 
Published: January 2016

ABSTRACT
We present the results of an extensive Hubble Space Telescope imaging study of 105, mostly Swift, long-duration gamma-ray bursts (LGRBs) spanning

, which were localized using relative astrometry from ground- and space-based afterglow observations. We measure the distribution of LGRB offsets from their host centers and their relation to the underlying host light distribution. We find that the host-normalized offsets of LGRBs are more centrally concentrated than expected for an exponential disk profile,

= 0.63, and in particular they are more concentrated than the underlying surface brightness profiles of their host galaxies and more concentrated than supernovae. The fractional flux distribution, with a median of 0.78, indicates that LGRBs prefer some of the brightest locations in their host galaxies but are not as strongly correlated as previous studies indicated. Importantly, we find a clear correlation between offset and fractional flux, where bursts at offsets

exclusively occur at fractional fluxes

, while bursts at

have a uniform fractional flux distribution. This indicates that the spatial correlation of LGRBs with bright star-forming regions seen in the full sample is dominated by the contribution from bursts at small offset and that LGRBs in the outer parts of galaxies show no preference for unusually bright regions. We conclude that LGRBs strongly prefer the bright, inner regions of their hosts, indicating that the star formation taking place there is more favorable for LGRB progenitor production. This indicates that environmental factors beyond metallicity, such as binary interactions or IMF differences, may operate in the central regions of LGRB hosts.
THE EFFECTS OF GRAIN SIZE AND TEMPERATURE DISTRIBUTIONS ON THE FORMATION OF INTERSTELLAR ICE MANTLES
Authors: Pauly Tyler , Garrod Robin T. 
Published: January 2016

ABSTRACT
Computational models of interstellar gas-grain chemistry have historically adopted a single dust-grain size of 0.1 micron, assumed to be representative of the size distribution present in the interstellar medium. Here, we investigate the effects of a broad grain-size distribution on the chemistry of dust-grain surfaces and the subsequent build-up of molecular ices on the grains, using a three-phase gas-grain chemical model of a quiescent dark cloud. We include an explicit treatment of the grain temperatures, governed both by the visual extinction of the cloud and the size of each individual grain-size population. We find that the temperature difference plays a significant role in determining the total bulk ice composition across the grain-size distribution, while the effects of geometrical differences between size populations appear marginal. We also consider collapse from a diffuse to a dark cloud, allowing dust temperatures to fall. Under the initial diffuse conditions, small grains are too warm to promote grain-mantle build-up, with most ices forming on the mid-sized grains. As collapse proceeds, the more abundant, smallest grains cool and become the dominant ice carriers; the large population of small grains means that this ice is distributed across many grains, with perhaps no more than 40 monolayers of ice each (versus several hundred assuming a single grain size). This effect may be important for the subsequent processing and desorption of the ice during the hot-core phase of star formation, exposing a significant proportion of the ice to the gas phase, increasing the importance of ice-surface chemistry and surface–gas interactions.
IMPLICATION OF FORMATION MECHANISMS OF HC5N IN TMC-1 AS STUDIED BY 13C ISOTOPIC FRACTIONATION
Authors: Taniguchi Kotomi , Ozeki Hiroyuki , Saito Masao , Sakai Nami , Nakamura Fumitaka , Kameno Seiji , Takano Shuro , Yamamoto Satoshi 
Published: January 2016

ABSTRACT
We observed the J = 9 − 8 and 16 − 15 rotational transitions of the normal species and five 13C isotopologues of HC5N to study its formation mechanisms toward the cyanopolyyne peak in Taurus Molecular Cloud-1, with the 45-m radio telescope of the Nobeyama Radio Observatory. We detected the five 13C isotopologues with high signal-to-noise ratios between 12 and 20, as well as the normal species. The abundance ratios of the five 13C isotopologues of HC5N are found to be 1.00:0.97:1.03:1.05:1.16 (±0.19) (1σ) for [H13CCCCCN]:[HC13CCCCN]:[HCC13CCCN]:[HCCC13CCN]:[HCCCC13CN]. We do not find any significant differences among the five

isotopologues. The averaged [HC5N]/[13C isotopologues] abundance ratio is determined to be 94 ± 6 (1σ), which is slightly higher than the local interstellar elemental 12C/13C ratio of 60–70. Possible formation pathways are discussed on the basis of these results.
IGRINS NEAR-IR HIGH-RESOLUTION SPECTROSCOPY OF MULTIPLE JETS AROUND LkHα 234*
Authors: Oh Heeyoung , Pyo Tae-Soo , Yuk In-Soo , Park Byeong-Gon , Park Chan , Chun Moo-Young , Pak Soojong , Kim Kang-Min , Oh Jae Sok , Jeong Ueejeong , Yu Young Sam , Lee Jae-Joon , Kim Hwihyun , Hwang Narae , Kaplan Kyle , Pavel Michael , Mace Gregory , Lee Hye-In , Le Huynh Anh Nguyen , Lee Sungho , Jaffe Daniel T. 
Published: January 2016

ABSTRACT
We present the results of high-resolution near-IR spectroscopy toward the multiple outflows around the Herbig Be star LkHα 234 using the Immersion Grating Infrared Spectrograph. Previous studies indicate that the region around LkHα 234 is complex, with several embedded young stellar objects and the outflows associated with them. In simultaneous H- and K-band spectra from HH 167, we detected 5 [Fe ii] and 14 H2 emission lines. We revealed a new [Fe ii] jet driven by radio continuum source VLA 3B. Position–velocity diagrams of the H2 1−0 S(1) λ2.122 μm line show multiple velocity peaks. The kinematics may be explained by a geometrical bow shock model. We detected a component of H2 emission at the systemic velocity (V
LSR = −10.2 km s−1) along the whole slit in all slit positions, which may arise from the ambient photodissociation region. Low-velocity gas dominates the molecular hydrogen emission from knots A and B in HH 167, which is close to the systemic velocity; [Fe ii] emission lines are detected farther from the systemic velocity, at V
LSR = −100–−130 km s−1. We infer that the H2 emission arises from shocked gas entrained by a high-velocity outflow. Population diagrams of H2 lines imply that the gas is thermalized at a temperature of 2500–3000 K and the emission results from shock excitation.
THE OFF-CENTERED SEYFERT-LIKE COMPACT EMISSION IN THE NUCLEAR REGION OF NGC 3621
Authors: Menezes R. B. , Steiner J. E. , Silva Patrícia da 
Published: January 2016

ABSTRACT
We analyze an optical data cube of the nuclear region of NGC 3621, taken with the integral field unit of the Gemini Multi-object Spectrograph. We found that the previously detected central line emission in this galaxy actually comes from a blob, located at a projected distance of 2.″14 ± 0.″08 (70.1 ± 2.6 pc) from the stellar nucleus. Only diffuse emission was detected in the rest of the field of view, with a deficit of emission at the position of the stellar nucleus. Diagnostic diagram analysis reveals that the off-centered emitting blob has a Seyfert 2 spectrum. We propose that the line-emitting blob may be a “fossil” emission-line region or a light “echo” from an active galactic nucleus (AGN), which was significantly brighter in the past. Our estimates indicate that the bolometric luminosity of the AGN must have decreased by a factor of ∼13–500 during the past ∼230 yr. A second scenario to explain the morphology of the line-emitting areas in the nuclear region of NGC 3621 involves no decrease of the AGN bolometric luminosity and establishes that the AGN is highly obscured toward the observer but not toward the line-emitting blob. The third scenario proposed here assumes that the off-centered line-emitting blob is a recoiling supermassive black hole, after the coalescence of two black holes. Finally, an additional hypothesis is that the central X-ray source is not an AGN, but an X-ray binary. This idea is consistent with all the scenarios we proposed.
STRUCTURE OF THE ACCRETION DISK IN THE LENSED QUASAR Q2237+0305 FROM MULTI-EPOCH AND MULTI-WAVELENGTH NARROWBAND PHOTOMETRY
Authors: Muñoz J. A. , Vives-Arias H. , Mosquera A. M. , Jiménez-Vicente J. , Kochanek C. S. , Mediavilla E. 
Published: January 2016

ABSTRACT
We present estimates for the size and the logarithmic slope of the disk temperature profile of the lensed quasar Q2237+0305, independent of the component velocities. These estimates are based on six epochs of multi-wavelength narrowband images from the Nordic Optical Telescope. For each pair of lensed images and each photometric band, we determine the microlensing amplitude and chromaticity using pre-existing mid-IR photometry to define the baseline for no microlensing magnification. A statistical comparison of the combined microlensing data (6 epochs × 5 narrow bands × 6 image pairs) with simulations based on microlensing magnification maps gives Bayesian estimates for the half-light radius of

lt-day, and p = 0.95 ± 0.33 for the exponent of the logarithmic temperature profile

. This size estimate is in good agreement with most recent studies. Other works based on the study of single microlensing events predict smaller sizes, but could be statistically biased by focusing on high-magnification events.
THE EVOLUTION OF THE ELECTRIC CURRENT DURING THE FORMATION AND ERUPTION OF ACTIVE-REGION FILAMENTS
Authors: Wang Jincheng , Yan Xiaoli , Qu Zhongquan , Xue Zhike , Xiang Yongyuan , Li Hao 
Published: January 2016

ABSTRACT
We present a comprehensive study of the electric current related to the formation and eruption of active region filaments in NOAA AR 11884. The vertical current on the solar surface was investigated by using vector magnetograms (VMs) observed by HMI on board the Solar Dynamics Observatory. To obtain the electric current along the filament's axis, we reconstructed the magnetic fields above the photosphere by using nonlinear force-free field extrapolation based on photospheric VMs. Spatio-temporal evolutions of the vertical current on the photospheric surface and the horizontal current along the filament's axis were studied during the long-term evolution and eruption-related period, respectively. The results show that the vertical currents of the entire active region behaved with a decreasing trend and the magnetic fields also kept decreasing during the long-term evolution. For the eruption-related evolution, the mean transverse field strengths decreased before two eruptions and increased sharply after two eruptions in the vicinity of the polarity inversion lines underneath the filament. The related vertical current showed different behaviors in two of the eruptions. On the other hand, a very interesting feature was found: opposite horizontal currents with respect to the current of the filament's axis appeared and increased under the filament before the eruptions and disappeared after the eruptions. We suggest that these opposite currents were carried by the new flux emerging from the photosphere bottom and might be the trigger mechanism for these filament eruptions.
ON THE BEAM INDUCED QUASI-INSTABILITY TRANSFORMATION OF THE DAMPED APERIODIC MODE IN THE INTERGALACTIC MEDIUM
Authors: Kolberg U. , Schlickeiser R. , Yoon P. H. 
Published: January 2016

ABSTRACT
Highly relativistic electron–positron pair beams considerably affect the spontaneously emitted field fluctuations in the unmagnetized intergalactic medium (IGM). In view of the considered small density ratio of beam and background plasma, a perturbative treatment is employed in order to derive the spectral balance equations for the fluctuating fields from first principles of plasma kinetic theory that are covariantly correct within the limits of special relativity. They self-consistently account for the competing effects of spontaneous and induced emission and absorption in the perturbed thermal plasma. It is found that the presence of the beam transforms the growth rate of the dominating transverse damped aperiodic mode into an effective growth rate that displays positive values in certain spectral regions if beam velocity and wave vector are perpendicular or almost perpendicular to each other. This corresponds to a quasi-instability that induces an amplification of the fluctuations for these wavenumbers. Such an effect can greatly influence the cosmic magnetogenesis as it affects the strengths of the spontaneously emitted magnetic seed fields in the IGM, thereby possibly lowering the required growth time and effectivity of any further amplification mechanism such as an astrophysical dynamo.
SHADOW OF A COLOSSUS: A z = 2.44 GALAXY PROTOCLUSTER DETECTED IN 3D Lyα FOREST TOMOGRAPHIC MAPPING OF THE COSMOS FIELD
Authors: Lee Khee-Gan , Hennawi Joseph F. , White Martin , Prochaska J. Xavier , Font-Ribera Andreu , Schlegel David J. , Rich R. Michael , Suzuki Nao , Stark Casey W. , Fèvre Olivier Le , Nugent Peter E. , Salvato Mara , Zamorani Gianni 
Published: January 2016

ABSTRACT
Using moderate-resolution optical spectra from 58 background Lyman-break galaxies and quasars at

within a 11.′5 × 13.′5 area of the COSMOS field (

projected area density or

mean transverse separation), we reconstruct a 3D tomographic map of the foreground Lyα forest absorption at 2.2 < z < 2.5 with an effective smoothing scale of

comoving. Comparing with 61 coeval galaxies with spectroscopic redshifts in the same volume, we find that the galaxy positions are clearly biased toward regions with enhanced intergalactic medium (IGM) absorption in the tomographic map. We find an extended IGM overdensity with deep absorption troughs at z = 2.45 associated with a recently discovered galaxy protocluster at the same redshift. Based on simulations matched to our data, we estimate the enclosed dark matter mass within this IGM overdensity to be

, and argue based on this mass and absorption strength that it will form at least one z ∼ 0 galaxy cluster with

, although its elongated nature suggests that it will likely collapse into two separate clusters. We also point out a compact overdensity of six MOSDEF galaxies at z = 2.30 within a

radius and Δz ∼ 0.006, which does not appear to have a large associated IGM overdensity. These results demonstrate the potential of Lyα forest tomography on larger volumes to study galaxy properties as a function of environment, as well as revealing the large-scale IGM overdensities associated with protoclusters or other features of large-scale structure.
NEPTUNE’S DYNAMIC ATMOSPHERE FROM KEPLER K2 OBSERVATIONS: IMPLICATIONS FOR BROWN DWARF LIGHT CURVE ANALYSES
Authors: Simon Amy A. , Rowe Jason F. , Gaulme Patrick , Hammel Heidi B. , Casewell Sarah L. , Fortney Jonathan J. , Gizis John E. , Lissauer Jack J. , Morales-Juberias Raul , Orton Glenn S. , Wong Michael H. , Marley Mark S. 
Published: January 2016

ABSTRACT
Observations of Neptune with the Kepler Space Telescope yield a 49 day light curve with 98% coverage at a 1 minute cadence. A significant signature in the light curve comes from discrete cloud features. We compare results extracted from the light curve data with contemporaneous disk-resolved imaging of Neptune from the Keck 10-m telescope at 1.65 microns and Hubble Space Telescope visible imaging acquired nine months later. This direct comparison validates the feature latitudes assigned to the K2 light curve periods based on Neptune's zonal wind profile, and confirms observed cloud feature variability. Although Neptune's clouds vary in location and intensity on short and long timescales, a single large discrete storm seen in Keck imaging dominates the K2 and Hubble light curves; smaller or fainter clouds likely contribute to short-term brightness variability. The K2 Neptune light curve, in conjunction with our imaging data, provides context for the interpretation of current and future brown dwarf and extrasolar planet variability measurements. In particular we suggest that the balance between large, relatively stable, atmospheric features and smaller, more transient, clouds controls the character of substellar atmospheric variability. Atmospheres dominated by a few large spots may show inherently greater light curve stability than those which exhibit a greater number of smaller features.