bluuebunny/crossref_metadata_2025_split huggingface dataset:
JUPITER’S PHASE VARIATIONS FROM CASSINI: A TESTBED FOR FUTURE DIRECT-IMAGING MISSIONS
Authors: Mayorga L. C. , Jackiewicz J. , Rages K. , West R. A. , Knowles B. , Lewis N. , Marley M. S. 
Published: December 2016

ABSTRACT
We present empirical phase curves of Jupiter from ∼0° to 140° as measured in multiple optical bandpasses by Cassini/Imaging Science Subsystem (ISS) during the Millennium flyby of Jupiter in late 2000 to early 2001. Phase curves are of interest for studying the energy balance of Jupiter and understanding the scattering behavior of the planet as an exoplanet analog. We find that Jupiter is significantly darker at partial phases than an idealized Lambertian planet by roughly 25% and is not well fit by Jupiter-like exoplanet atmospheric models across all wavelengths. We provide analytic fits to Jupiter’s phase function in several Cassini/ISS imaging filter bandpasses. In addition, these observations show that Jupiter’s color is more variable with phase angle than predicted by models. Therefore, the color of even a near Jupiter-twin planet observed at a partial phase cannot be assumed to be comparable to that of Jupiter at full phase. We discuss how the Wide-Field Infrared Survey Telescope and other future direct-imaging missions can enhance the study of cool giants.
TWO COLOR POPULATIONS OF KUIPER BELT AND CENTAUR OBJECTS AND THE SMALLER ORBITAL INCLINATIONS OF RED CENTAUR OBJECTS
Authors: Tegler S. C. , Romanishin W. , Consolmagno, S. J. G. J. 
Published: December 2016

ABSTRACT
We present new optical colors for 28 Kuiper Belt objects (KBOs) and 35 Centaur objects measured with the 1.8 m Vatican Advanced Technology Telescope and the 4.3 m Discovery Channel Telescope. By combining these new colors with our previously published colors, we increase the sample size of our survey to 154 objects. Our survey is unique in that the uncertainties in our color measurements are less than half the uncertainties in the color measurements reported by other researchers in the literature. Small uncertainties are essential for discerning between a unimodal and a bimodal distribution of colors for these objects as well as detecting correlations between colors and orbital elements. From our survey, it appears red Centaurs have a broader color distribution than gray Centaurs. We find red Centaurs have a smaller orbital inclination angle distribution than gray Centaurs at the 99.3% confidence level. Furthermore, we find that our entire sample of KBOs and Centaurs exhibits bimodal colors at the

confidence level. KBOs and Centaurs with H

V
> 7.0 have bimodal colors at the 99.96% confidence level and KBOs with H

V
< 6.0 have bimodal colors at the 96% confidence level.
ARE THERE MOONLETS NEAR THE URANIAN α AND β RINGS?
Authors: Chancia R. O. , Hedman M. M. 
Published: December 2016

ABSTRACT
The Voyager 2 Radio Science Subsystem occultations of the Uranian α and β rings exhibit quasi-periodic optical depth variations with radial wavelengths that vary with longitude. These patterns may be wakes from small moonlets orbiting exterior to these rings. Based on the observed structures in the rings, we estimate that the moonlets would need to be located ∼100 km exterior to the rings’ semimajor axes (

km for α and

km for β) and be 2–7 km in radius. Such moonlets could help keep the rings confined. Due to their small radii and presumed low albedo, the expected brightness of these moonlets is on the order of the noise in Voyager 2 images.
OSSOS. IV. DISCOVERY OF A DWARF PLANET CANDIDATE IN THE 9:2 RESONANCE WITH NEPTUNE
Authors: Bannister Michele T. , Alexandersen Mike , Benecchi Susan D. , Chen Ying-Tung , Delsanti Audrey , Fraser Wesley C. , Gladman Brett J. , Granvik Mikael , Grundy Will M. , Guilbert-Lepoutre Aurélie , Gwyn Stephen D. J. , Ip Wing-Huen , Jakubik Marian , Jones R. Lynne , Kaib Nathan , Kavelaars J. J. , Lacerda Pedro , Lawler Samantha , Lehner Matthew J. , Lin Hsing Wen , Lykawka Patryk Sofia , Marsset Michael , Murray-Clay Ruth , Noll Keith S. , Parker Alex , Petit Jean-Marc , Pike Rosemary E. , Rousselot Philippe , Schwamb Megan E. , Shankman Cory , Veres Peter , Vernazza Pierre , Volk Kathryn , Wang Shiang-Yu , Weryk Robert 
Published: December 2016

ABSTRACT
We report the discovery and orbit of a new dwarf planet candidate, 2015 RR245, by the Outer Solar System Origins Survey (OSSOS). The orbit of 2015 RR245 is eccentric (e = 0.586), with a semimajor axis near 82 au, yielding a perihelion distance of 34 au. 2015 RR245 has

and absolute magnitude

for an assumed albedo of p

V
= 12%, the object has a diameter of ∼670 km. Based on astrometric measurements from OSSOS and Pan-STARRS1, we find that 2015 RR245 is securely trapped on ten-megayear timescales in the 9:2 mean-motion resonance with Neptune. It is the first trans-Neptunian object (TNO) identified in this resonance. On hundred-megayear timescales, particles in 2015 RR245-like orbits depart and sometimes return to the resonance, indicating that 2015 RR245 likely forms part of the long-lived metastable population of distant TNOs that drift between resonance sticking and actively scattering via gravitational encounters with Neptune. The discovery of a 9:2 TNO stresses the role of resonances in the long-term evolution of objects in the scattering disk and reinforces the view that distant resonances are heavily populated in the current solar system. This object further motivates detailed modeling of the transient sticking population.
ORBITS, DISTANCE, AND STELLAR MASSES OF THE MASSIVE TRIPLE STAR σ ORIONIS
Authors: Schaefer G. H. , Hummel C. A. , Gies D. R. , Zavala R. T. , Monnier J. D. , Walter F. M. , Turner N. H. , Baron F. , Brummelaar T. ten , Che X. , Farrington C. D. , Kraus S. , Sturmann J. , Sturmann L. 
Published: December 2016

ABSTRACT
We present interferometric observations of the σ Orionis triple system using the CHARA Array, NPOI, and VLTI. Using these measurements, we spatially resolve the orbit of the close spectroscopic binary (Aa,Ab) for the first time and present a revised orbit for the wide pair (A,B). Combining the visual orbits with previously published radial velocity measurements and new radial velocities measured at CTIO, we derive dynamical masses for the three massive stars in the system of

= 16.99 ± 0.20

,

= 12.81 ± 0.18

, and

= 11.5 ± 1.2

. The inner and outer orbits in the triple are not coplanar, with a relative inclination of

–127

. The orbital parallax provides a precise distance of 387.5 ± 1.3 pc to the system. This is a significant improvement over previous estimates of the distance to the young σ Orionis cluster.
ALMA HCN AND HCO+ J = 3 − 2 OBSERVATIONS OF OPTICAL SEYFERT AND LUMINOUS INFRARED GALAXIES: CONFIRMATION OF ELEVATED HCN-TO-HCO+ FLUX RATIOS IN AGNS
Authors: Imanishi (今西昌俊) Masatoshi , Nakanishi (中西康一郎) Kouichiro , Izumi (泉拓磨) Takuma 
Published: December 2016

ABSTRACT
We present the results of our ALMA observations of three active galactic nucleus (AGN)-dominated nuclei in optical Seyfert 1 galaxies (NGC 7469, I Zw 1, and IC 4329 A) and eleven luminous infrared galaxies (LIRGs) with various levels of infrared estimated energetic contributions by AGNs at the HCN and HCO+
J = 3 − 2 emission lines. The HCN and HCO+
J = 3 − 2 emission lines are clearly detected at the main nuclei of all sources, except for IC 4329 A. The vibrationally excited (v
2 = 1f) HCN J = 3 − 2 and HCO+
J = 3 − 2 emission lines are simultaneously covered, and HCN v
2 = 1f J = 3 − 2 emission line signatures are seen in the main nuclei of two LIRGs, IRAS 12112+0305 and IRAS 22491–1808, neither of which shows clear buried AGN signatures in the infrared. If the vibrational excitation is dominated by infrared radiative pumping, through the absorption of infrared 14 μm photons, primarily originating from AGN-heated hot dust emission, then these two LIRGs may contain infrared-elusive, but (sub)millimeter-detectable, extremely deeply buried AGNs. These vibrationally excited emission lines are not detected in the three AGN-dominated optical Seyfert 1 nuclei. However, the observed HCN v
2 = 1f to v = 0 flux ratios in these optical Seyferts are still consistent with the intrinsic flux ratios in LIRGs with detectable HCN v
2 = 1f emission lines. The observed HCN-to-HCO+
J = 3 − 2 flux ratios tend to be higher in galactic nuclei with luminous AGN signatures compared with starburst-dominated regions, as previously seen at J = 1 − 0 and J = 4 − 3.
BVRI PHOTOMETRIC 2015 WD ANALYSIS OF THE SOUTHERN TOTALLY ECLIPSING, SOLAR-TYPE, SHALLOW-CONTACT W UMA BINARY, DD INDUS
Authors: Samec Ronald G. , Norris Cody L. , Hamme Walter Van , Faulkner Danny R. , Hill Robert L. 
Published: December 2016

ABSTRACT
Observations and a 2015 Wilson–Devinney Program analysis are undertaken for the first precision observations of DD Indi. DD Indi is of solar-type (T
1 ∼ 5750 K) and was determined to be a shallow-contact eclipsing binary. It was observed from 2013 June through September at Cerro Tololo InterAmerican Observatory in remote mode. The 24 inch Boller and Chivens reflector, now under management by The Southeastern Association for Resarch in Astronomomy (SARA) was used. Five new eclipse timings were obtained, for three primary and two secondary eclipses. Seven more eclipse timings were calculated from All Sky Automated Survey data. A possibly increasing period was found from all available eclipse timings with a 5 ± 2 × 10−11 × E
2 quadratic term. A BVR
c
I
c simultaneous synthetic light-curve analysis reveals that the system has a mass ratio of ∼0.46, a ∼ 140 K component temperature difference, and two weak cool spots. The Roche Lobe fill-out of this W-type binary is only ∼11%, and an inclination of ∼86° was determined. A time of constant light of ∼16 minutes is measured around phase zero. More detail is included in this report.
OBSERVATIONAL CONSTRAINTS ON FIRST-STAR NUCLEOSYNTHESIS. I. EVIDENCE FOR MULTIPLE PROGENITORS OF CEMP-NO STARS
Authors: Yoon Jinmi , Beers Timothy C. , Placco Vinicius M. , Rasmussen Kaitlin C. , Carollo Daniela , He Siyu , Hansen Terese T. , Roederer Ian U. , Zeanah Jeff 
Published: December 2016

ABSTRACT
We investigate anew the distribution of absolute carbon abundance, A(C) = log ϵ(C), for carbon-enhanced metal-poor (CEMP) stars in the halo of the Milky Way, based on high-resolution spectroscopic data for a total sample of 305 CEMP stars. The sample includes 147 CEMP-s (and CEMP-r/s) stars, 127 CEMP-no stars, and 31 CEMP stars that are unclassified, based on the currently employed [Ba/Fe] criterion. We confirm previous claims that the distribution of A(C) for CEMP stars is (at least) bimodal, with newly determined peaks centered on A(C) = 7.96 (the high-C region) and A(C) = 6.28 (the low-C region). A very high fraction of CEMP-s (and CEMP-r/s) stars belongs to the high-C region, while the great majority of CEMP-no stars resides in the low-C region. However, there exists complexity in the morphology of the A(C)-[Fe/H] space for the CEMP-no stars, a first indication that more than one class of first-generation stellar progenitors may be required to account for their observed abundances. The two groups of CEMP-no stars we identify exhibit clearly different locations in the A(Na)-A(C) and A(Mg)-A(C) spaces, also suggesting multiple progenitors. The clear distinction in A(C) between the CEMP-s (and CEMP-r/s) stars and the CEMP-no stars appears to be as successful, and likely more astrophysically fundamental, for the separation of these sub-classes as the previously recommended criterion based on [Ba/Fe] (and [Ba/Eu]) abundance ratios. This result opens the window for its application to present and future large-scale low- and medium-resolution spectroscopic surveys.
OBSERVATIONAL CONSTRAINTS ON FIRST-STAR NUCLEOSYNTHESIS. II. SPECTROSCOPY OF AN ULTRA METAL-POOR CEMP-no STAR*
Authors: Placco Vinicius M. , Frebel Anna , Beers Timothy C. , Yoon Jinmi , Chiti Anirudh , Heger Alexander , Chan Conrad , Casey Andrew R. , Christlieb Norbert 
Published: December 2016

ABSTRACT
We report on the first high-resolution spectroscopic analysis of HE 0020–1741, a bright (V = 12.9), ultra metal-poor (

= −4.1), carbon-enhanced (

= +1.7) star selected from the Hamburg/ESO Survey. This star exhibits low abundances of neutron-capture elements (

= −1.1) and an absolute carbon abundance A(C) = 6.1; based on either criterion, HE 0020–1741 is subclassified as a carbon-enhanced metal-poor star without enhancements in neutron-capture elements (CEMP-no). We show that the light-element abundance pattern of HE 0020–1741 is consistent with predicted yields from a massive (M =

), primordial-composition, supernova (SN) progenitor. We also compare the abundance patterns of other ultra metal-poor stars from the literature with available measures of C, N, Na, Mg, and Fe abundances with an extensive grid of SN models (covering the mass range

), in order to probe the nature of their likely stellar progenitors. Our results suggest that at least two classes of progenitors are required at

, as the abundance patterns for more than half of the sample studied in this work (7 out of 12 stars) cannot be easily reproduced by the predicted yields.
THE SCALING RELATIONS AND STAR FORMATION LAWS OF MINI-STARBURST COMPLEXES
Authors: Nguyễn-Lu’o’ng Quang , Nguyễn Hans V. V. , Motte Fredérique , Schneider Nicola , Fujii Michiko , Louvet Fabien , Hill Tracey , Sanhueza Patricio , Chibueze James O. , Didelon Pierre 
Published: December 2016

ABSTRACT
The scaling relations and star formation laws for molecular cloud complexes (MCCs) in the Milky Way are investigated. MCCs are mostly large (R > 50 pc), massive (∼106

) gravitationally unbound cloud structures. We compare their masses

, mass surface densities

, radii R, velocity dispersions σ, star formation rates (SFRs), and SFR densities

with those of structures ranging from cores, clumps, and giant molecular clouds, to MCCs, and galaxies, spanning eight orders of magnitudes in size and 13 orders of magnitudes in mass. This results in the following universal relations:

Variations in the slopes and coefficients of these relations are found at individual scales, signifying different physics acting at different scales. Additionally, there are breaks at the MCC scale in the

relation and between starburst and normal star-forming objects in the

and

–

relations. Therefore, we propose to use the Schmidt–Kennicutt diagram to distinguish starburst from normal star-forming structures by applying a

threshold of ∼100

pc−2 and a

threshold of 1

yr−1 kpc−2. Mini-starburst complexes are gravitationally unbound MCCs that have enhanced

(>1

yr−1 kpc−2), probably caused by dynamic events such as radiation pressure, colliding flows, or spiral arm gravitational instability. Because of dynamical evolution, gravitational boundedness does not play a significant role in regulating the star formation activity of MCCs, especially the mini-starburst complexes, which leads to the dynamical formation of massive stars and clusters. We emphasize the importance of understanding mini-starbursts in investigating the physics of starburst galaxies.
STRONG-LENSING ANALYSIS OF THE POWERFUL LENSING CLUSTER MACS J2135.2-0102 (z = 0.33)
Authors: Zitrin Adi , Broadhurst Tom 
Published: December 2016

ABSTRACT
We present a light-traces-mass (LTM) strong-lensing model of the massive lensing cluster MACS J2135.2-0102 (z = 0.33; hereafter MACS2135), known in part for hosting the cosmic eye galaxy lens. MACS2135 is also known to multiply lens a z = 2.3 sub-millimeter galaxy near the brightest cluster galaxy (BCG), as well as a prominent, triply imaged system at a large radius of ∼37″ south of the BCG. We use the latest available Hubble imaging to construct an accurate lensing model for this cluster, identifying six new multiply imaged systems with the guidance of our LTM method, so that we have roughly quadrupled the number of lensing constraints. We determine that MACS2135 is among the top lensing clusters known, comparable in size to the Hubble Frontier Fields. For a source at

, we find an effective Einstein radius of

, enclosing

. We make our lens model, including mass and magnification maps, publicly available, in anticipation of searches for high-z galaxies with the James Webb Space Telescope, for which this cluster is a compelling target.
ASTROSAT/LAXPC REVEALS THE HIGH-ENERGY VARIABILITY OF GRS 1915+105 IN THE χ CLASS
Authors: Yadav J S , Misra Ranjeev , Chauhan Jai Verdhan , Agrawal P C , Antia H M , Pahari Mayukh , Dedhia Dhiraj , Katoch Tilak , Madhwani P. , Manchanda R K , Paul B , Shah Parag , Ishwara-Chandra C H 
Published: December 2016

ABSTRACT
We present the first quick look analysis of data from nine AstroSat's Large Area X-ray Proportional Counter (LAXPC) observations of GRS 1915+105 during 2016 March when the source had the characteristics of being in the Radio-quiet χ class. We find that a simple empirical model of a disk blackbody emission, with Comptonization and a broad Gaussian Iron line can fit the time-averaged 3–80 keV spectrum with a systematic uncertainty of 1.5% and a background flux uncertainty of 4%. A simple dead time corrected Poisson noise level spectrum matches well with the observed high-frequency power spectra till 50 kHz and as expected the data show no significant high-frequency (

) features. Energy dependent power spectra reveal a strong low-frequency (2–8 Hz) quasi-periodic oscillation and its harmonic along with broadband noise. The QPO frequency changes rapidly with flux (nearly 4 Hz in ∼5 hr). With increasing QPO frequency, an excess noise component appears significantly in the high-energy regime (

keV). At the QPO frequencies, the time-lag as a function of energy has a non-monotonic behavior such that the lags decrease with energy till about 15–20 keV and then increase for higher energies. These first-look results benchmark the performance of LAXPC at high energies and confirms that its data can be used for more sophisticated analysis such as flux or frequency-resolved spectro-timing studies.
A COMPREHENSIVE SEARCH FOR STELLAR BOWSHOCK NEBULAE IN THE MILKY WAY: A CATALOG OF 709 MID-INFRARED SELECTED CANDIDATES
Authors: Kobulnicky Henry A. , Chick William T. , Schurhammer Danielle P. , Andrews Julian E. , Povich Matthew S. , Munari Stephan A. , Olivier Grace M. , Sorber Rebecca L. , Wernke Heather N. , Dale Daniel A. , Dixon Don M. 
Published: December 2016

ABSTRACT
We identify 709 arc-shaped mid-infrared nebula in 24 μm Spitzer Space Telescope or 22 μm Wide Field Infrared Explorer surveys of the Galactic Plane as probable dusty interstellar bowshocks powered by early-type stars. About 20% are visible at 8 μm or at shorter mid-infrared wavelengths. The vast majority (660) have no previous identification in the literature. These extended infrared sources are strongly concentrated near the Galactic mid-plane, with an angular scale height of ∼0.°6. All host a symmetrically placed star implicated as the source of a stellar wind sweeping up interstellar material. These are candidate “runaway” stars potentially having high velocities in the reference frame of the local medium. Among the 286 objects with measured proper motions, we find an unambiguous excess with velocity vectors aligned with the infrared morphology—kinematic evidence that many of these are “runaway” stars with large peculiar motions responsible for the bowshock signature. We discuss a population of “in situ” bowshocks (∼103 objects) that face giant H ii regions where the relative motions between the star and ISM may be caused by bulk outflows from an overpressured bubble. We also identify ∼58 objects that face 8 μm bright-rimmed clouds and apparently constitute a sub-class of in situ bowshocks where the stellar wind interacts with a photoevaporative flow (PEF) from an eroding molecular cloud interface (i.e., “PEF bowshocks”). Orientations of the arcuate nebulae exhibit a correlation over small angular scales, indicating that external influences such as H ii regions are responsible for producing some bowshock nebulae. However, the vast majority of the nebulae in this sample appear to be isolated (499 objects) from obvious external influences.
LARGE SUPER-FAST ROTATOR HUNTING USING THE INTERMEDIATE PALOMAR TRANSIENT FACTORY
Authors: Chang Chan-Kao , Lin Hsing-Wen , Ip Wing-Huen , Prince Thomas A. , Kulkarni Shrinivas R. , Levitan David , Laher Russ , Surace Jason 
Published: December 2016

ABSTRACT
In order to look for large super-fast rotators, in late 2014 and early 2015, five dedicated surveys covering ∼188 deg2 in the ecliptic plane have been carried out in the R-band, with ∼10 minute cadence using the intermediate Palomar Transient Factory. Among 1029 reliable rotation periods obtained from the surveys, we discovered 1 new large super-fast rotator, (40511) 1999 RE88, and 18 other candidates. (40511) 1999 RE88 is an S-type inner main-belt asteroid with a diameter of D = 1.9 ± 0.3 km, a rotation period of P = 1.96 ± 0.01 hr, and a light curve amplitude of Δm ∼ 1.0 mag. To maintain such fast rotation, an internal cohesive strength of ∼780 Pa is required. Combining all known large super-fast rotators, their cohesive strengths all fall in the range of 100–1000 Pa of lunar regolith. However, the number of large super-fast rotators seems to be far less than the whole asteroid population. This might indicate a peculiar asteroid group for them. Although the detection efficiency for a long rotation period is greatly reduced due to our two-day observation time span, the spin-rate distributions of this work show consistent results with Chang et al. (2015), after considering the possible observational bias in our surveys. It shows a number decrease with an increase of spin rate for asteroids with a diameter of 3 ⩽ D ⩽ 15 km, and a number drop at a spin rate of f = 5 rev day−1 for asteroids with D ⩽ 3 km.
DETECTION OF POLARIZED QUASI-PERIODIC MICROSTRUCTURE EMISSION IN MILLISECOND PULSARS
Authors: De Kishalay , Gupta Yashwant , Sharma Prateek 
Published: December 2016

ABSTRACT
Microstructure emission, involving short timescale, often quasi-periodic, intensity fluctuations in subpulse emission, is well known in normal period pulsars. In this Letter, we present the first detections of quasi-periodic microstructure emission from millisecond pulsars (MSPs), from Giant Metrewave Radio Telescope observations of two MSPs at 325 and 610 MHz. Similar to the characteristics of microstructure observed in normal period pulsars, we find that these features are often highly polarized and exhibit quasi-periodic behavior on top of broader subpulse emission, with periods of the order of a few μs. By measuring their widths and periodicities from single pulse intensity profiles and their autocorrelation functions, we extend the microstructure timescale–rotation period relationship by more than an order of magnitude down to rotation periods ∼5 ms, and find it to be consistent with the relationship derived earlier for normal pulsars. The similarity of behavior is remarkable, given the significantly different physical properties of MSPs and normal period pulsars, and rules out several previous speculations about the possible different characteristics of microstructure in MSP radio emission. We discuss the possible reasons for the non-detection of these features in previous high time resolution MSP studies along with the physical implications of our results, both in terms of a geometric beam sweeping model and temporal modulation model for micropulse production.