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102. THE INCIDENCE OF COOL GAS IN ∼1013 M ☼ HALOSThis paper includes data gathered with the 2.5 m du Pont telescope located at Las Campanas Observatory, Chile and with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium.
103. HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS IN THE LEAST EVOLVED GALAXIES: LEO IVThis paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
104. Ophiuchus 1622–2405: Not a Planetary-Mass BinaryThis paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory Chile.
105. Calibrating Type Ia Supernovae Using the Planetary Nebula Luminosity Function. I. Initial ResultsThe WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatory. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
106. The Keck+Magellan Survey for Lyman Limit Absorption. I. The Frequency Distribution of Super Lyman Limit SystemsThis paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
107. The Deuterium-to-Hydrogen Abundance Ratio toward the QSO SDSS J155810.16–003120.0This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
108. Subarcsecond Mid-Infrared Imaging of Dust in the Bipolar Nebula Hen 3-401This paper is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (US), the Particle Physics and Astronomy Research Council (UK), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina).
109. A Starfish Preplanetary Nebula:The phrase “preplanetary nebula,” which refers to an object in the evolutionary phase immediately preceding the planetary nebula phase, is used in this paper in place of the more commonly used “proto-planetary nebula,” because the term “proto-planetary” is widely used to refer to disks around pre-main-sequence stars. Since the term protoplanet is used by the planet and planet formation communities to refer to planets undergoing formation, the use of the term “protoplanetary nebula” to refer to a completely different kind of object is an unfortunate choice, which compounds our inconvenience of having the historically inherited misnomer “planetary nebula.” We believe, therefore, that it is important to replace the term “proto-planetary nebula” (in this work and future studies) with “preplanetary nebula,” which is both unique (in the planetary community, the term “preplanet” is not used, and never will be) and correct in its meaning. IRAS 19024+0044
110. H2 Imaging of Three Proto-Planetary and Young Planetary NebulaeThe paper is based on observations obtained at the Gemini Observatory with the Adaptive Optics System Hokupa’a/QUIRC, developed and operated by the University of Hawaii Adaptive Optics Group, with support from the National Science Foundation. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), Comisión Nacional de Investigación Científica y Tecnológica (CONICYT; Chile), the Australian Research Council (Australia), Laboratório Nacional de Astrofísica (CNPq; Brazil), and Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET; Argentina).
111. A Luminous Lyα-emitting Galaxy at Redshift z = 6.535: Discovery and Spectroscopic ConfirmationThe data presented in this paper were obtained at the Kitt Peak National Observatory, the Gemini Observatory, and the W. M. Keck Observatory. Kitt Peak National Observatory, National Optical Astronomy Observatory, is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation (NSF). The Gemini Observatory is operated by AURA under a cooperative agreement with the NSF on behalf of the Gemini partnership: the NSF (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council, CNPq (Brazil), and CONICET (Argentina). The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
112. The Physical Properties and Effective Temperature Scale of O-Type Stars as a Function of Metallicity. I. A Sample of 20 Stars in the Magellanic CloudsBased on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with programs 6417, 7739, 8633, and 9412. This paper also draws heavily from data obtained from the data archive at STScI.
113. The Absorption and Emission Kinematics in the z = 0.7450 Mg II Absorber toward Q1331+17This paper is based on observations collected with the Very Large Telescope at the European Southern Observatory, Chile, as part of ESO programs 67.A-0334 and 68.A-0170.
114. Probing Dark Energy and Modifications of Gravity with Ground-based millimeter-wavelength Line Intensity Mapping.
115. The Influence of Stellar Rotation in Binary Systems on Core-collapse Supernova Progenitors and Multimessenger Signals.
116. ALMA-LEGUS. II. The Influence of Subgalactic Environments on Molecular Cloud Properties.
117. Probing Supermassive Black Hole Seed Scenarios with Gravitational-wave Measurements.
118. Resolving the Periods of the Asynchronous Polar 1RXS J083842.1–282723.
119. Discovery of Kiloparsec-scale Semirelativistic Fe K α Complex Emission in NGC 5728.
120. Can Fallback Accretion on the Magnetar Model Power the X-Ray Flares Simultaneously Observed with Gamma Rays of Gamma-Ray Bursts?
121. Modeling the Multiwavelength Spectral Energy Distributions of the Fermi-4LAC Bright Flat-spectrum Radio Quasars.
122. Cosmic Tidal Reconstruction in Redshift Space.
123. Constraining Neutrino Cosmologies with Nonlinear Reconstruction.
124. Redshifted Iron Emission and Absorption Lines in the Chandra X-Ray Spectrum of Centaurus A.
125. Star Formation from Galaxies to GlobulesInvited paper, based on the Heineman Prize lecture presented at the 199th meeting of the American Astronomical Society in 2002 January.
126. Boomerang Returns UnexpectedlyA paper about a boomerang by an Australian and his mates.
127. The Nature of LINERsObservations reported in this paper were obtained with the Multiple Mirror Telescope, which is operated jointly by the Smithsonian Astrophysical Observatory and the University of Arizona.
128. The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XXIII. Proper-motion Catalogs and Internal Kinematics.
129. Universal Relations for the Increase in the Mass and Radius of a Rotating Neutron Star.
130. Infrared Line Emissions from Atoms and Atomic Ions in NGC 7027: Improved Wavelength Determinations for Infrared Metal Lines and a Probable Detection of Zn 5+.
131. Surveying the Giant H ii Regions of the Milky Way with SOFIA. IV. Sgr D, W42, and a Reassessment of the Giant H ii Region Census.
132. A Blueprint for the Milky Way's Stellar Populations. IV. A String of Pearls—the Galactic Starburst Sequence.
133. Magnetic Activity–Rotation–Age–Mass Relations in Late-pre-main-sequence Stars.
134. You Are What You Eat: The Circumgalactic Medium around BreakBRD Galaxies Has Low Mass and Angular Momentum.
135. Magnetic Helicity Flux across Solar Active Region Photospheres. II. Association of Hemispheric Sign Preference with Flaring Activity during Solar Cycle 24.
136. A Stochastic Theory of the Hierarchical Clustering. II. Halo Progenitor Mass Function and Large-scale Bias.
137. Magnetic Helicity Signature and Its Role in Regulating Magnetic Energy Spectra and Proton Temperatures in the Solar Wind.
138. Tidal Disruptions of Main-sequence Stars. II. Simulation Methodology and Stellar Mass Dependence of the Character of Full Tidal Disruptions.
139. Tidal Disruptions of Main-sequence Stars. I. Observable Quantities and Their Dependence on Stellar and Black Hole Mass.
140. Substructure at High Speed. I. Inferring the Escape Velocity in the Presence of Kinematic Substructure.
141. Substructure at High Speed. II. The Local Escape Velocity and Milky Way Mass with Gaia eDR3.
142. Self-similarities and Power Laws in the Time-resolved Spectra of GRB 190114C, GRB 130427A, GRB 160509A, and GRB 160625B.
143. Filtration of Interstellar Neutral Helium by Elastic and Charge Exchange Collisions in Heliospheric Boundaries.
144. Kinematics of the Ursa Major Molecular CloudsThis paper is dedicated to Dr. James Jay Klavetter.
145. Magnetohydrodynamic Accretion–Ejection: Jets Launched by a Nonisotropic Accretion-disk Dynamo. II. A Dynamo Tensor Defined by the Disk Coriolis Number.
146. Global 21 cm Signal Extraction from Foreground and Instrumental Effects. II. Efficient and Self-consistent Technique for Constraining Nonlinear Signal Models.
147. Magnetic Field Structure in Spheroidal Star-forming Clouds. II. Estimating Field Structure from Observed Maps.
148. A Large X-Ray Outburst in Mira AWe dedicate this paper to the memory of Janet A. Mattei, who inspired this work and made these observations possible for many years.
149. A Detailed Analysis of GW190521 with Phenomenological Waveform Models.
150. Three-dimensional Reconstruction of Coronal Plasma Properties from a Single Perspective.
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