bluuebunny/crossref_metadata_2025_split huggingface dataset:
Changes in glaciation of the Balkhash–Alakol basin, central Asia, over recent decades
Authors: Severskiy I. , Vilesov E. , Armstrong R. , Kokarev A. , Kogutenko L. , Usmanova Z. , Morozova V. , Raup B. 
Published: March 2016

AbstractWe describe changes in glaciers of the Balkhash-Alakol basin, central Asia, and analyse unified glacier inventories of the Zailiyskiy-Kungei and Jungar glacier systems and the Chinese part of the Ili river basin, as well as mass-balance monitoring data from Tsentralniy Tuyuksu glacier for the period 1957-2014. In spite of significant inter-basin differences, glaciation of the three glacial systems in the Ili river basin within Kazakhstan as well as within Chinese territory is changing simultaneously and similarly. Differences in the rates of glacier degradation are small and are affected primarily by the orientation of the flanks of the mountain ridges. Since the mid-1950s, glaciation of the region has remained degraded and, on average over the period examined, glaciers shrank at a rate of about 0.8% a-1 in area and about 1 % a-1 in ice volume. Glacial systems in large basins such as Balkhash-Alakol change simultaneously, linearly and at similar rates. The average rates of glacier reduction of the Zailiyskiy-Kungei, Jungar and upper Ili glacier systems for the period 1955/56-2008 amounted to 0.76%, 0.75% and 0.73% a-1 respectively.
Synthesis, characterization, and anti-plasmodial activity of 2,6-substituted benzothiazole derivatives
Authors: Sadhasivam Gnanavel , Kulanthai Kannan , Rajamani Sowmiya , Perumal Pachiappan 
Published: March 2016

<p class="Abstract">Six compounds of benzothiazole derivatives were synthesized, and structures were confirmed by FT-IR, <sup>1</sup>H-NMR, <sup>13</sup>C-NMR and LC-MS. The resulting compounds were evaluated for anti-plasmodial activity against <em>Plasmodium falciparum</em> by Giemsa stain. Among them the compounds 3b and 4 showed potent anti-plasmodial activity against <em>P. falciparum</em>. The com-pounds 3a, 5a, 5b also showed moderate anti-plasmodial activity. The structure-activity relationships of benzothiazole derivatives also discussed which were useful for exploring and developing benzothiazole derivatives as novel anti-malarial drugs.</p><p> </p>
DENSE GAS IN MOLECULAR CORES ASSOCIATED WITH PLANCK GALACTIC COLD CLUMPS
Authors: Yuan (袁敬华) Jinghua , Wu Yuefang , Liu Tie , Zhang Tianwei , Li Jin Zeng , Liu Hong-Li , Meng Fanyi , Chen Ping , Hu Runjie , Wang Ke 
Published: March 2016

ABSTRACT
We present the first survey of dense gas toward Planck Galactic Cold Clumps (PGCCs). Observations in the J = 1–0 transitions of HCO+ and HCN toward 621 molecular cores associated with PGCCs were performed using the Purple Mountain Observatory’s 13.7 m telescope. Among them, 250 sources were detected, including 230 cores detected in HCO+ and 158 in HCN. Spectra of the J = 1–0 transitions from 12CO, 13CO, and C18O at the centers of the 250 cores were extracted from previous mapping observations to construct a multi-line data set. The significantly low detection rate of asymmetric double-peaked profiles, together with the good consistency among central velocities of CO, HCO+, and HCN spectra, suggests that the CO-selected Planck cores are more quiescent than classical star-forming regions. The small difference between line widths of C18O and HCN indicates that the inner regions of CO-selected Planck cores are no more turbulent than the exterior. The velocity-integrated intensities and abundances of HCO+ are positively correlated with those of HCN, suggesting that these two species are well coupled and chemically connected. The detected abundances of both HCO+ and HCN are significantly lower than values in other low- to high-mass star-forming regions. The low abundances may be due to beam dilution. On the basis of an inspection of the parameters given in the PGCC catalog, we suggest that there may be about 1000 PGCC objects that have a sufficient reservoir of dense gas to form stars.
SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M
⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES
Authors: Jontof-Hutter Daniel , Ford Eric B. , Rowe Jason F. , Lissauer Jack J. , Fabrycky Daniel C. , Laerhoven Christa Van , Agol Eric , Deck Katherine M. , Holczer Tomer , Mazeh Tsevi 
Published: March 2016

ABSTRACT
We infer dynamical masses in eight multiplanet systems using transit times measured from Kepler's complete data set, including short-cadence data where available. Of the 18 dynamical masses that we infer, 10 pass multiple tests for robustness. These are in systems Kepler-26 (KOI-250), Kepler-29 (KOI-738), Kepler-60 (KOI-2086), Kepler-105 (KOI-115), and Kepler-307 (KOI-1576). Kepler-105 c has a radius of 1.3 R
⊕ and a density consistent with an Earth-like composition. Strong transit timing variation (TTV) signals were detected from additional planets, but their inferred masses were sensitive to outliers or consistent solutions could not be found with independently measured transit times, including planets orbiting Kepler-49 (KOI-248), Kepler-57 (KOI-1270), Kepler-105 (KOI-115), and Kepler-177 (KOI-523). Nonetheless, strong upper limits on the mass of Kepler-177 c imply an extremely low density of ∼0.1 g cm−3. In most cases, individual orbital eccentricities were poorly constrained owing to degeneracies in TTV inversion. For five planet pairs in our sample, strong secular interactions imply a moderate to high likelihood of apsidal alignment over a wide range of possible eccentricities. We also find solutions for the three planets known to orbit Kepler-60 in a Laplace-like resonance chain. However, nonlibrating solutions also match the transit timing data. For six systems, we calculate more precise stellar parameters than previously known, enabling useful constraints on planetary densities where we have secure mass measurements. Placing these exoplanets on the mass–radius diagram, we find that a wide range of densities is observed among sub-Neptune-mass planets and that the range in observed densities is anticorrelated with incident flux.
KILOPARSEC MASS/LIGHT OFFSETS IN THE GALAXY PAIR-Lyα EMITTER LENS SYSTEM SDSS J1011+0143*
Authors: Shu Yiping , Bolton Adam S. , Moustakas Leonidas A. , Stern Daniel , Dey Arjun , Brownstein Joel R. , Burles Scott , Spinrad Hyron 
Published: March 2016

ABSTRACT
We report the discovery of significant mass/light offsets in the strong gravitational lensing system SDSS J1011+0143. We use the high-resolution Hubble Space Telescope (HST) F555W- and F814W-band imaging and Sloan Digital Sky Survey (SDSS) spectroscopy of this system, which consists of a close galaxy pair with a projected separation of

at z
lens ∼ 0.331 lensing an Lyα emitter (LAE) at z
source = 2.701. Comparisons between the mass peaks inferred from lens models and light peaks from HST imaging data reveal significant spatial mass/light offsets as large as 1.72 ± 0.24 ± 0.34 kpc in both filter bands. Such large mass/light offsets, not seen in isolated field lens galaxies and relaxed galaxy groups, may be related to the interactions between the two lens galaxies. The detected mass/light offsets can potentially serve as an important test for the self-interacting dark matter model. However, other mechanisms such as dynamical friction on spatially differently distributed dark matter and stars could produce similar offsets. Detailed hydrodynamical simulations of galaxy–galaxy interactions with self-interacting dark matter could accurately quantify the effects of different mechanisms. The background LAE is found to contain three distinct star-forming knots with characteristic sizes from 116 to 438 pc. It highlights the power of strong gravitational lensing in probing the otherwise too faint and unresolved structures of distance objects below subkiloparsec or even 100 pc scales through its magnification effect.
BEAM-FORMING ERRORS IN MURCHISON WIDEFIELD ARRAY PHASED ARRAY ANTENNAS AND THEIR EFFECTS ON EPOCH OF REIONIZATION SCIENCE
Authors: Neben Abraham R. , Hewitt Jacqueline N. , Bradley Richard F. , Dillon Joshua S. , Bernardi G. , Bowman J. D. , Briggs F. , Cappallo R. J. , Corey B. E. , Deshpande A. A. , Goeke R. , Greenhill L. J. , Hazelton B. J. , Johnston-Hollitt M. , Kaplan D. L. , Lonsdale C. J. , McWhirter S. R. , Mitchell D. A. , Morales M. F. , Morgan E. , Oberoi D. , Ord S. M. , Prabu T. , Shankar N. Udaya , Srivani K. S. , Subrahmanyan R. , Tingay S. J. , Wayth R. B. , Webster R. L. , Williams A. , Williams C. L. 
Published: March 2016

ABSTRACT
Accurate antenna beam models are critical for radio observations aiming to isolate the redshifted 21 cm spectral line emission from the Dark Ages and the Epoch of Reionization (EOR) and unlock the scientific potential of 21 cm cosmology. Past work has focused on characterizing mean antenna beam models using either satellite signals or astronomical sources as calibrators, but antenna-to-antenna variation due to imperfect instrumentation has remained unexplored. We characterize this variation for the Murchison Widefield Array (MWA) through laboratory measurements and simulations, finding typical deviations of the order of ±10%–20% near the edges of the main lobe and in the sidelobes. We consider the ramifications of these results for image- and power spectrum-based science. In particular, we simulate visibilities measured by a 100 m baseline and find that using an otherwise perfect foreground model, unmodeled beam-forming errors severely limit foreground subtraction accuracy within the region of Fourier space contaminated by foreground emission (the “wedge”). This region likely contains much of the cosmological signal, and accessing it will require measurement of per-antenna beam patterns. However, unmodeled beam-forming errors do not contaminate the Fourier space region expected to be free of foreground contamination (the “EOR window”), showing that foreground avoidance remains a viable strategy.
SEARCH FOR HYPERLUMINOUS INFRARED DUST-OBSCURED GALAXIES SELECTED WITH WISE AND SDSS
Authors: Toba Y. , Nagao T. 
Published: March 2016

ABSTRACT
We aim to search for hyperluminous infrared (IR) galaxies (HyLIRGs) with IR luminosity

> 1013
L
☉ by applying the selection method of dust-obscured galaxies (DOGs). They are spatially rare but could correspond to a maximum phase of cosmic star formation (SF) and/or active galactic nucleus (AGN) activity; hence, they are a crucial population for understanding the SF and mass assembly history of galaxies. Combining the optical and IR catalogs obtained from the Sloan Digital Sky Survey (SDSS) and Wide-field Infrared Survey Explorer (WISE), we performed the extensive HyLIRGs survey; we selected 5311 IR-bright DOGs with i − [22] > 7.0 and flux at 22 μm > 3.8 mJy in 14,555 deg2, where i and [22] are i-band and 22 μm AB magnitudes, respectively. Among them, 67 DOGs have reliable spectroscopic redshifts that enable us to estimate their total IR luminosity based on the spectral energy distribution fitting. Consequently, we successfully discovered 24 HyLIRGs among the 67 spectroscopically confirmed DOGs. We found that (i) i − [22] color of IR-bright DOGs correlates with the total IR luminosity and (ii) the surface number density of HyLIRGs is >0.17 deg−2. A large fraction (∼73%) of IR-bright DOGs with i − [22] > 7.5 show

> 1013
L
☉, and the DOG criterion we adopted could be independently effective against the “W1W2-dropout method,” based on four WISE bands, for searching hyperluminous IR populations of galaxies.
GIANT Hα NEBULA SURROUNDING THE STARBURST MERGER NGC 6240*
Authors: Yoshida Michitoshi , Yagi Masafumi , Ohyama Youichi , Komiyama Yutaka , Kashikawa Nobunari , Tanaka Hisashi , Okamura Sadanori 
Published: March 2016

ABSTRACT
We revealed the detailed structure of a vastly extended Hα-emitting nebula (“Hα nebula”) surrounding the starburst/merging galaxy NGC 6240 by deep narrow-band imaging observations with the Subaru Suprime-Cam. The extent of the nebula is ∼90 kpc in diameter and the total Hα luminosity amounts to L
Hα
≈ 1.6 × 1042 erg s−1. The volume filling factor and the mass of the warm ionized gas are ∼10−4–10−5 and ∼5 × 108
M
⊙, respectively. The nebula has a complicated structure, which includes numerous filaments, loops, bubbles, and knots. We found that there is a tight spatial correlation between the Hα nebula and the extended soft-X-ray-emitting gas, both in large and small scales. The overall morphology of the nebula is dominated by filamentary structures radially extending from the center of the galaxy. A large-scale bipolar bubble extends along the minor axis of the main stellar disk. The morphology strongly suggests that the nebula was formed by intense outflows—superwinds—driven by starbursts. We also found three bright knots embedded in a looped filament of ionized gas that show head-tail morphologies in both emission-line and continuum, suggesting close interactions between the outflows and star-forming regions. Based on the morphology and surface brightness distribution of the Hα nebula, we propose the scenario that three major episodes of starburst/superwind activities, which were initiated ∼102 Myr ago, formed the extended ionized gas nebula of NGC 6240.
SN REFSDAL: PHOTOMETRY AND TIME DELAY MEASUREMENTS OF THE FIRST EINSTEIN CROSS SUPERNOVA
Authors: Rodney S. A. , Strolger L.-G. , Kelly P. L. , Bradač M. , Brammer G. , Filippenko A. V. , Foley R. J. , Graur O. , Hjorth J. , Jha S. W. , McCully C. , Molino A. , Riess A. G. , Schmidt K. B. , Selsing J. , Sharon K. , Treu T. , Weiner B. J. , Zitrin A. 
Published: March 2016

ABSTRACT
We present the first year of Hubble Space Telescope imaging of the unique supernova (SN) “Refsdal,” a gravitationally lensed SN at z = 1.488 ± 0.001 with multiple images behind the galaxy cluster MACS J1149.6+2223. The first four observed images of SN Refsdal (images S1–S4) exhibited a slow rise (over ∼150 days) to reach a broad peak brightness around 2015 April 20. Using a set of light curve templates constructed from SN 1987A-like peculiar Type II SNe, we measure time delays for the four images relative to S1 of 4 ± 4 (for S2), 2 ± 5 (S3), and 24 ± 7 days (S4). The measured magnification ratios relative to S1 are 1.15 ± 0.05 (S2), 1.01 ± 0.04 (S3), and 0.34 ± 0.02 (S4). None of the template light curves fully captures the photometric behavior of SN Refsdal, so we also derive complementary measurements for these parameters using polynomials to represent the intrinsic light curve shape. These more flexible fits deliver fully consistent time delays of 7 ± 2 (S2), 0.6 ± 3 (S3), and 27 ± 8 days (S4). The lensing magnification ratios are similarly consistent, measured as 1.17 ± 0.02 (S2), 1.00 ± 0.01 (S3), and 0.38 ± 0.02 (S4). We compare these measurements against published predictions from lens models, and find that the majority of model predictions are in very good agreement with our measurements. Finally, we discuss avenues for future improvement of time delay measurements—both for SN Refsdal and for other strongly lensed SNe yet to come.
THE FIRST GEV OUTBURST OF THE RADIO-LOUD NARROW-LINE SEYFERT 1 GALAXY PKS 1502+036
Authors: Paliya Vaidehi S. , Stalin C. S. 
Published: March 2016

ABSTRACT
The γ-ray-loud narrow-line Seyfert 1 (γ-NLSy1) galaxy PKS 1502+036 (z = 0.409) exhibited its first γ-ray outburst on 2015 December 20. In the energy range of 0.1–300 GeV, the highest flux measured by the Fermi-Large Area Telescope is (3.90 ± 1.52) × 10−6

, which is the highest γ-ray flux ever detected from this object. The associated spectral shape is soft (Γ0.1–300 GeV = 2.57 ± 0.17) and this corresponds to an isotropic γ-ray luminosity of (1.2 ± 0.6) × 1048 erg s−1. We generate the broadband spectral energy distribution (SED) during the GeV flare and reproduce it using a one-zone leptonic emission model. The optical-UV spectrum can be explained by a combination of synchrotron and accretion disk emission, whereas the X-ray-to-γ-ray SED can be satisfactorily reproduced by inverse-Compton scattering of thermal photons that originated from the torus. The derived SED parameters hint that the increase in the bulk Lorentz factor is a major cause of the flare and the location of the emission region is estimated as being outside the broad-line region but still inside the torus. A comparison of the GeV-flaring SED of PKS 1502+036 with that of two other γ-NLSy1 galaxies, namely, 1H 0323+342 (z = 0.061) and PMN J0948+0022 (z = 0.585), and also with flat spectrum radio quasar (FSRQ) 3C 279 (z = 0.536), has led to the conclusion that the GeV-flaring SEDs of γ-NLSy1 galaxies resemble FSRQs and a major fraction of their bolometric luminosities are emitted at γ-ray energies.
DEGENERACY BETWEEN LENSING AND OCCULTATION IN THE ANALYSIS OF SELF-LENSING PHENOMENA
Authors: Han Cheongho 
Published: March 2016

ABSTRACT
More than 40 years after the first discussion, the detection of a self-lensing phenomenon within a binary system where the brightness of a background star is magnified by its foreground companion was recently reported. It is expected that the number of self-lensing binary detections will be increased by a wealth of data from current and future survey experiments. In this paper, we introduce a degeneracy in the interpretation of self-lensing light curves. The degeneracy is intrinsic to self-lensing binaries for which both magnification by lensing and de-magnification by occultation occur simultaneously and are caused by the difficulty in separating the contribution of the lensing-induced magnification from the observed light curve. We demonstrate the severity of this degeneracy by presenting examples of self-lensing light curves that suffer from it. We also present the relation between the lensing parameters of the degenerate solutions. This degeneracy is an important obstacle in accurately determining self-lensing parameters and thus characterizing binaries.
THE K2-ESPRINT PROJECT. II. SPECTROSCOPIC FOLLOW-UP OF THREE EXOPLANET SYSTEMS FROM CAMPAIGN 1 OF K2*
Authors: Eylen Vincent Van , Nowak Grzegorz , Albrecht Simon , Palle Enric , Ribas Ignasi , Bruntt Hans , Perger Manuel , Gandolfi Davide , Hirano Teriyuki , Sanchis-Ojeda Roberto , Kiilerich Amanda , Prieto-Arranz Jorge , Badenas Mariona , Dai Fei , Deeg Hans J. , Guenther Eike W. , Montañés-Rodríguez Pilar , Narita Norio , Rogers Leslie A. , Béjar Víctor J. S. , Shrotriya Tushar S. , Winn Joshua N. , Sebastian Daniel 
Published: March 2016

ABSTRACT
We report on Doppler observations of three transiting planet candidates that were detected during Campaign 1 of the K2 mission. The Doppler observations were conducted with FIES, HARPS-N, and HARPS. We measure the mass of EPIC 201546283b, and provide constraints and upper limits for EPIC 201295312b and EPIC 201577035b. EPIC 201546283b is a warm Neptune orbiting its host star in 6.77 days and has a radius of

and a mass of

, which leads to a mean density of

. EPIC 201295312b is smaller than Neptune with an orbital period of 5.66 days, a radius of

, and we constrain the mass to be below

at 95% confidence. We also find a long-term trend indicative of another body in the system. EPIC 201577035b, which was previously confirmed as the planet K2-10b, is smaller than Neptune, orbiting its host star in 19.3 days, with a radius of

. We determine its mass to be

, with a 95% confidence upper limit at

, and a mean density of

. These measurements join the relatively small collection of planets smaller than Neptune with measurements or constraints of the mean density. Our code for performing K2 photometry and detecting planetary transits is now publicly available.
TEMPORAL EVOLUTION OF THE VELA PULSAR’S PULSE PROFILE
Authors: Palfreyman J. L. , Dickey J. M. , Ellingsen S. P. , Jones I. R. , Hotan A. W. 
Published: March 2016

ABSTRACT
The mechanisms of emission and changes in rotation frequency (“glitching”) of the Vela pulsar (J0835−4510) are not well understood. Further insight into these mechanisms can be achieved by long-term studies of integrated pulse width, timing residuals, and bright-pulse rates. We have undertaken an intensive observing campaign of Vela and collected over 6000 hr of single-pulse data. The data shows that the pulse width changes with time, including marked jumps in width after micro-glitches (frequency changes). The abundance of bright pulses also changes after some micro-glitches, but not all. The secular changes in pulse width have three possible cyclic periods that match with X-ray periodicities of a helical jet that are interpreted as free precession.
AN ULTRAMASSIVE 1.28 M⊙ WHITE DWARF IN NGC 2099*
Authors: Cummings Jeffrey D. , Kalirai Jason S. , Tremblay P.-E. , Ramirez-Ruiz Enrico , Bergeron P. 
Published: March 2016

ABSTRACT
With the Keck I Low-Resolution Imaging Spectrometer we have observed nine white dwarf candidates in the very rich open cluster NGC 2099 (M37). The spectroscopy shows seven to be DA white dwarfs, one to be a DB white dwarf, and one to be a DZ white dwarf. Three of these DA white dwarfs are consistent with singly evolved cluster membership: an ultramassive (1.28

) and two intermediate-mass (0.70 and 0.75

) white dwarfs. Analysis of their cooling ages allows us to calculate their progenitor masses and establish new constraints on the initial–final mass relation. The intermediate-mass white dwarfs are in strong agreement with previous work over this mass regime. The ultramassive white dwarf has V = 24.5, ∼2 mag fainter than the other two remnants. The spectrum of this star has lower quality, so the derived stellar properties (e.g.,

, log g) have uncertainties that are several times higher than the brighter counterparts. We measure these uncertainties and establish the star’s final mass as the highest-mass white dwarf discovered thus far in a cluster, but we are unable to calculate its progenitor mass because at this high mass and cooler

its inferred cooling age is highly sensitive to its mass. At the highest temperatures, however, this sensitivity of cooling age to an ultramassive white dwarf’s mass is only moderate. This demonstrates that future investigations of the upper-mass end of the initial–final mass relation must identify massive, newly formed white dwarfs (i.e., in young clusters with ages 50–150 Myr).
SDSS J085431.18+173730.5: THE FIRST COMPACT ELLIPTICAL GALAXY HOSTING AN ACTIVE NUCLEUS
Authors: Paudel Sanjaya , Hilker Michael , Ree Change Hee , Kim Minjin 
Published: March 2016

ABSTRACT
We report the discovery of a rare compact early-type galaxy, SDSS J085431.18+173730.5 (hereafter cE_AGN). It has a half-light radius of R

e
= 490 pc and a brightness of M

r
= −18.08 mag. Optical spectroscopy available from the Sloan Digital Sky Survey (SDSS) reveals the presence of prominent broad-line emissions with the Hα broad component width of FWHM = 2400 km s−1. The black hole (BH) mass, as estimated from the luminosity and width of the broad Hα emission, is 2.1 × 106

. With the help of surface photometry, we perform a detailed analysis of the structural properties. The observed light distribution is best modeled with a double Sérsic function. Fixing the outer component as an exponential disk, we find that the inner component has a Sérsic index of n = 1.4. Considering the inner component as bulge/spheroidal we find that cE_AGN remains consistent in both the BH mass–bulge mass relation and the BH mass–bulge Sérsic index relation. Given these observational properties, we discuss its possible origin investigating the surrounding environment where it is located.
El coloquio de los Perros a la luz de la poética del Pinciano
Authors: Canals Piñas Jordi 
Published: March 2016

La novela cervantina que conocemos con el título de Coloquio de los Pe"os (CP), cierra la colección de Novelas Ejemplares publicadas en 1613. Aunque puede considerarse parte integrante de el casamiento Engañoso (CE), penúltima narración del volumen, mantienen ambas una casi total autonomía.