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Probing the Circumgalactic Medium with Fast Radio Bursts: Insights from CAMELS Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Isabel Medlock, Daisuke Nagai, Priyanka Singh, Benjamin Oppenheimer, Daniel Anglés-Alcázar and Francisco Villaescusa-Navarro
Most diffuse baryons, including the circumgalactic medium (CGM) surrounding galaxies and the intergalactic medium (IGM) in the cosmic web, remain unmeasured and unconstrained. Fast radio bursts (FRBs) offer an unparalleled method to measure the electron dispersion measures (DMs) of ionized baryons. Their distribution can resolve the missing baryon problem and constrain the history of feedback theorized
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Bayesian Synthesis of Astrometric Wobble and Total Light Curves in Close Binary Supermassive Black Holes Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Andjelka B. Kovačević, Yu-Yang Songsheng, Jian-Min Wang and Luka Č. Popović
We test the potential of Bayesian synthesis of upcoming multi-instrument data to extract orbital parameters and individual light curves of close binary supermassive black holes (CB-SMBH) with subparsec separations. Next-generation interferometers, will make possible the observation of astrometric wobbles in CB-SMBH. Combining them with periodic variable time-domain data from surveys like the Vera C
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Deep Synoptic Array Science: First FRB and Host Galaxy Catalog Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Casey J. Law, Kritti Sharma, Vikram Ravi, Ge Chen, Morgan Catha, Liam Connor, Jakob T. Faber, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, James W. Lamb, Paul Rasmussen, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody and Nitika Yadlapalli Yurk
Fast radio bursts (FRBs) are a powerful and mysterious new class of transients that are luminous enough to be detected at cosmological distances. By associating FRBs to host galaxies, we can measure intrinsic and environmental properties that test FRB origin models, in addition to using them as precise probes of distant cosmic gas. The Deep Synoptic Array (DSA-110) is a radio interferometer built to
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Lyα Emission at z = 7–13: Clear Evolution of Lyα Equivalent Width Indicating a Late Cosmic Reionization History Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yuichi Harikane, Yoshiaki Ono, Hiroya Umeda, Yuki Isobe, Yechi Zhang and Yi Xu
We present the evolution of Lyα emission derived from 53 galaxies at z = 6.6–13.2, which have been identified by multiple JWST/NIRSpec spectroscopy programs of Early Release Science, General Observer, Director's Discretionary Time, and Guaranteed Time Observations. These galaxies fall on the star formation main sequence and are typical star-forming galaxies with UV magnitudes of −22.5 ≤ MUV ≤ −17.0
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Study of the Observation Sensitivity of Gamma-Ray Bursts for the HADAR Project Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Zi-hao Zhang, Tian-Lu Chen, You-Liang Feng, Yi-Qing Guo, Yu-Hua Yao, Cheng Liu, Yang-Zhao Ren, Heng-Jiao Liu, Hong-Bo Hu, Qi-Ling Chen, Guang-Guang Xin, Yi Zhang and Qiang Yuan
The High Altitude Detection of Astronomical Radiation (HADAR) is a novel wide-field Cherenkov Telescope. It is designed for gamma-ray astronomy in the energy range of 10 GeV to 100 TeV, with gamma-ray bursts (GRBs) being one of its primary research focuses. To assess its complementary capabilities, this study first presents the Crab sensitivity of HADAR. Then, to compare the sensitivity of GRBs, the
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Exploring the Mpc Environment of the Quasar ULAS J1342+0928 at z = 7.54 Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Sofía Rojas-Ruiz, Chiara Mazzucchelli, Steven L. Finkelstein, Eduardo Bañados, Emanuele Paolo Farina, Bram P. Venemans, Roberto Decarli, Chris J. Willott, Feige Wang, Fabian Walter, Enrico Congiu, Gabriel Brammer and Peter Zeidler
Theoretical models predict that z ≳ 6 quasars are hosted in the most massive halos of the underlying dark matter distribution and thus would be immersed in protoclusters of galaxies. However, observations report inconclusive results. We investigate the 1.1 proper-Mpc2 environment of the z = 7.54 luminous quasar ULAS J1342+0928. We search for Lyman-break galaxy (LBG) candidates using deep imaging from
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Evidence of a Strong 19.5 Hz Flux Oscillation in Swift BAT and Fermi GBM Gamma-Ray Data from GRB 211211A Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Cecilia Chirenti, Simone Dichiara, Amy Lien and M. Coleman Miller
The gamma-ray burst (GRB) GRB 211211A is believed to have occurred due to the merger of two neutron stars or a neutron star and a black hole, despite its duration of more than a minute. Subsequent analysis has revealed numerous interesting properties including the possible presence of a ∼22 Hz quasiperiodic oscillation (QPO) during precursor emission. Here we perform timing analysis of Fermi and Swift
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Sizes of Active Galactic Nucleus Inhomogeneous Disks—Large in Microlensing, Small in Reverberation Mapping Astrophys. J. (IF 4.9) Pub Date : 2024-05-14 Guowei Ren, Mouyuan Sun, Jun-Xian Wang and Zhen-Yi Cai
Magnetohydrodynamic turbulence can drive significant temperature fluctuations in the accretion disk of an active galactic nucleus (AGN). As a result, the disk can be highly inhomogeneous and has a half-light radius larger than the static Shakura and Sunyaev disk (SSD), in agreement with quasar microlensing observations. Meanwhile, the accretion-disk sizes can also be determined using continuum reverberation
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The Evolution of Accreting Binaries: From Brown Dwarfs to Supermassive Black Holes Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Alexander J. Dittmann and Geoffrey Ryan
Circumbinary accretion occurs throughout the universe, from the formation of stars and planets to the aftermath of major galactic mergers. We present an extensive investigation of circumbinary accretion disks, studying circular binaries with mass ratios (q ≡ M2/M1) from 0.01 to 1 and at each mass ratio probing the effects of disk thickness and viscosity. We study disks with aspect ratios H/r ∈ {0.1
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Determining the Nanoflare Heating Frequency of an X-Ray Bright Point Observed by MaGIXS Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Biswajit Mondal, P. S. Athiray, Amy R. Winebarger, Sabrina L. Savage, Ken Kobayashi, Stephen Bradshaw, Will Barnes, Patrick R. Champey, Peter Cheimets, Jaroslav Dudík, Leon Golub, Helen E. Mason, David E. McKenzie, Christopher S. Moore, Chad Madsen, Katharine K. Reeves, Paola Testa, Genevieve D. Vigil, Harry P. Warren, Robert W. Walsh and Giulio Del Zanna
Nanoflares are thought to be one of the prime candidates that can heat the solar corona to its multimillion kelvin temperature. Individual nanoflares are difficult to detect with the present generation of instruments, but their presence can be inferred by comparing simulated nanoflare-heated plasma emissions with the observed emission. Using HYDRAD coronal loop simulations, we model the emission from
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Resolved Near-infrared Stellar Photometry from the Magellan Telescope for 13 Nearby Galaxies: J-region Asymptotic Giant Branch Method Distances Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Abigail J. Lee, Andrew J. Monson, Wendy L. Freedman, Barry F. Madore, Kayla A. Owens, Rachael L. Beaton, Coral Espinoza, Tongtian Ren and Yi Ren
We present near-infrared JHK photometry for the resolved stellar populations in 13 nearby galaxies: NGC 6822, IC 1613, NGC 3109, Sextans B, Sextans A, NGC 300, NGC 55, NGC 7793, NGC 247, NGC 5253, Cen A, NGC 1313, and M83, acquired from the 6.5 m Baade–Magellan telescope. We measure distances to each galaxy using the J-region asymptotic giant branch (JAGB) method, a new standard candle that leverages
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Dissipative Dark Substructure: The Consequences of Atomic Dark Matter on Milky Way Analog Subhalos Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Caleb Gemmell, Sandip Roy, Xuejian Shen, David Curtin, Mariangela Lisanti, Norman Murray and Philip F. Hopkins
Using cosmological hydrodynamical zoom-in simulations, we explore the properties of subhalos in Milky Way analogs that contain a subcomponent of atomic dark matter (ADM). ADM differs from cold dark matter (CDM) due to the presence of self-interactions that lead to energy dissipation, analogous to standard model baryons. This model can arise in dark sectors that are natural and theoretically motivated
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Optical Spectroscopy of Type Ia Supernovae by the Carnegie Supernova Projects I and II Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 N. Morrell, M. M. Phillips, G. Folatelli, M. D. Stritzinger, M. Hamuy, N. B. Suntzeff, E. Y. Hsiao, F. Taddia, C. R. Burns, P. Hoeflich, C. Ashall, C. Contreras, L. Galbany, J. Lu, A. L. Piro, J. Anais, E. Baron, A. Burrow, L. Busta, A. Campillay, S. Castellón, C. Corco, T. Diamond, W. L. Freedman, C. Gonzalez, K. Krisciunas, S. Kumar, S. E. Persson, J. Serón, M. Shahbandeh, S. Torres, S. A. Uddin
We present the second and final release of optical spectroscopy of Type Ia supernovae (SNe Ia) obtained during the first and second phases of the Carnegie Supernova Project (CSP-I and CSP-II). The newly released data consist of 148 spectra of 30 SNe Ia observed in the course of CSP-I and 234 spectra of 127 SNe Ia obtained during CSP-II. We also present 216 optical spectra of 46 historical SNe Ia, including
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Parametric Decay of a Kinked Alfvén Wave Packet: 3D Magnetohydrodynamic Simulations Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Maile Marriott and Anna Tenerani
Large amplitude Alfvénic fluctuations, sometimes leading to localized inversions of the magnetic field, called switchbacks, are a common but poorly understood phenomenon in the solar wind. In particular, their origin(s), evolution, and stability within solar wind conditions are yet to be fully understood. Simulations modeling switchbacks have previously studied their stability in 2D. Here, we investigate
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Magnetic Field of Molecular Gas Measured with the Velocity Gradient Technique. II. Curved Magnetic Field in kpc-scale Bubble of NGC 628 Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Mengke Zhao, Jianjun Zhou, Willem A. Baan, Yue Hu, A. Lazarian, Xindi Tang, Jarken Esimbek, Yuxin He, Dalei Li, Weiguang Ji, Zhengxue Chang and Kadirya Tursun
We report the detection of the ordered alignment between the magnetic field and kpc-scale bubbles in the nearby spiral galaxy, NGC 628. Applying the Velocity Gradient Technique on CO spectroscopic data from the ALMA-PHANGS, the magnetic field of NGC 628 is measured at the scale of 191 pc (∼4″). The large-scale magnetic field is oriented parallel to the spiral arms and curves around the galactic bubble
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Evolutionary Origin of Ultralong-period Radio Transients Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Yun-Ning Fan, Kun Xu and Wen-Cong Chen
Recently, two ultralong-period radio transients, GLEAM-X J162759.5-523504.3 (J1627) and GPM J1839-10 (J1839), were discovered with spin periods longer than 1000 s. The origin of these two ultralong-period radio transients is intriguing in understanding the spin evolution of neutron stars (NSs). In this work, we examine whether the interaction between strong magnetized NSs and fallback disks can spin
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Photometric Objects Around Cosmic Webs (PAC). VI. High Satellite Fraction of Quasars Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Shanquan Gui, Kun Xu, Y. P. Jing, Donghai Zhao and Hongyu Gao
The Photometric objects Around Cosmic webs (PAC) approach developed in Xu et al. has the advantage of making full use of spectroscopic and deeper photometric surveys. With the merits of PAC, the excess surface density of neighboring galaxies can be measured down to stellar mass 1010.80M⊙ around quasars at redshift 0.8 < zs < 1.0, with the data from the Sloan Digital Sky Survey IV extended Baryon Oscillation
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Properties of the Magellanic Corona Astrophys. J. (IF 4.9) Pub Date : 2024-05-13 Scott Lucchini, Elena D’Onghia and Andrew J. Fox
We characterize the Magellanic Corona, the warm gaseous halo around the Large Magellanic Cloud (LMC). The Corona is a key ingredient in the formation of the Magellanic Stream and has recently been observed in high-ion absorption around the LMC. In this work, we present a suite of high-resolution hydrodynamical simulations to constrain its total mass and temperature prior to the infall of the Magellanic
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TEMPLATES: Characterization of a Merger in the Dusty Lensing SPT0418–47 System Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Jared Cathey, Anthony H. Gonzalez, Sidney Lower, Kedar A. Phadke, Justin Spilker, Manuel Aravena, Matthew Bayliss, Jack E. Birkin, Simon Birrer, Scott Chapman, Håkon Dahle, Christopher C. Hayward, Yashar Hezaveh, Ryley Hill, Taylor A. Hutchison, Keunho J. Kim, Guillaume Mahler, Daniel P. Marrone, Desika Narayanan, Alexander Navarre, Cassie Reuter, Jane R. Rigby, Keren Sharon, Manuel Solimano, Nikolaus
We present JWST and Atacama Large Millimeter/submillimeter Array (ALMA) imaging for the lensing system SPT0418−47, which includes a strongly lensed, dusty, star-forming galaxy at redshift z = 4.225 and an associated multiply imaged companion. The JWST NIRCam and MIRI imaging observations presented in this paper were acquired as part of the Early Release Science program Targeting Extremely Magnified
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Testing the LSST Difference Image Analysis Pipeline Using Synthetic Source Injection Analysis Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 S. Liu, W. M. Wood-Vasey, R. Armstrong, G. Narayan, B. O. Sánchez and The Dark Energy Science Collaboration
We evaluate the performance of the Legacy Survey of Space and Time Science Pipelines Difference Image Analysis (DIA) on simulated images. By adding synthetic sources to galaxies on images, we trace the recovery of injected synthetic sources to evaluate the pipeline on images from the Dark Energy Science Collaboration Data Challenge 2. The pipeline performs well, with efficiency and flux accuracy consistent
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Generation and Life Cycle of Solar Spicules Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Hamid Saleem and Zain H. Saleem
The physical mechanism for the creation of solar spicules is proposed with three stages of their life cycle. It is assumed that at stage I the density hump is formed locally in the x-y plane in the lower chromosphere in the presence of temperature gradients of electrons and ions along the z-axis (the vertical direction). In this region, the density structure of quasi-neutral (ni ≃ ne = n) plasma after
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The First High-contrast Images of Near High-mass X-Ray Binaries with Keck/NIRC2 Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 M. Prasow-Émond, J. Hlavacek-Larrondo, K. Fogarty, É. Artigau, D. Mawet, P. Gandhi, J. F. Steiner, J. Rameau, D. Lafrenière, A. Fabian, D. J. Walton, R. Doyon, B. B. Ren and 彬 任
Although the study of X-ray binaries has led to major breakthroughs in high-energy astrophysics, their circumbinary environment at scales of ∼100–10,000 au has not been thoroughly investigated. In this paper, we undertake a novel and exploratory study by employing direct and high-contrast imaging techniques on a sample of X-ray binaries, using adaptive optics and the vortex coronagraph on Keck/NIRC2
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Can Jupiter’s Atmospheric Metallicity Be Different from the Deep Interior? Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Simon Müller and Ravit Helled
Updated formation and structure models of Jupiter predict a metal-poor envelope. This is at odds with the two to three times solar metallicity measured by the Galileo probe. Additionally, Juno data imply that water and ammonia are enriched. Here, we explore whether Jupiter could have a deep radiative layer separating the atmosphere from the deeper interior. The radiative layer could be caused by a
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KFVM-WENO: A High-order Accurate Kernel-based Finite Volume Method for Compressible Hydrodynamics Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Ian C. T. May and Dongwook Lee
This paper presents a fully multidimensional kernel-based reconstruction scheme for finite volume methods applied to systems of hyperbolic conservation laws, with a particular emphasis on the compressible Euler equations. Nonoscillatory reconstruction is achieved through an adaptive-order weighted essentially nonoscillatory (WENO) method cast into a form suited to multidimensional reconstruction. A
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Insights into the Galactic Bulge Chemodynamical Properties from Gaia Data Release 3 Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Xiaojie Liao, Zhao-Yu Li, Iulia Simion, Juntai Shen, Robert Grand, Francesca Fragkoudi and Federico Marinacci
We explore the chemodynamical properties of the Galaxy in the azimuthal velocity Vϕ and metallicity [Fe/H] space using red giant stars from Gaia Data Release 3. The row-normalized Vϕ–[Fe/H] maps form a coherent sequence from the bulge to the outer disk, clearly revealing the thin/thick disk and the Splash. The metal-rich stars display bar-like kinematics, while the metal-poor stars show dispersion-dominated
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Dynamical Properties of Magnetized Low-angular-momentum Accretion Flows around a Kerr Black Hole Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Indu K. Dihingia and Yosuke Mizuno
An essential factor for determining the characteristics of an accretion flow is its angular momentum. According to the angular momentum of the flow, semi-analytical analysis suggests various types of accretion solutions. It is critical to test these with numerical simulations, using the most advanced framework available (general relativistic magnetohydrodynamics), to understand how the flow changes
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Relativistic Jet Ejections from Slim Disks Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Hajime Inoue
A mechanism for the ejection of relativistic jets from slim disks is studied. Since radiation pressure is dominant in the slim disk, radiative energy flows along the pressure gradient in the vertical direction. The divergence of the radiative flux tells us that the flow of radiative energy from a bottom layer near the equatorial plane is absorbed by another layer above the boundary surface. The absorbed
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Oscillating Dark Energy in Light of the Latest Observations and Its Impact on the Hubble Tension Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Mehdi Rezaei
In this paper, we have performed a comparative study of different types of oscillating dark energy (DE) models using the Metropolis algorithm of Markov Chain Monte Carlo. Eight different oscillating parameterizations are examined herein that have demonstrated considerable ability to fit the overall cosmological observations, including the Pantheon sample of Type Ia supernovae, baryon acoustic oscillations
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Forming Mercury from Excited Initial Conditions Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Jennifer Scora, Diana Valencia, Alessandro Morbidelli and Seth Jacobson
Mercury is notoriously difficult to form in Solar System simulations, due to its small mass and iron-rich composition. Smooth particle hydrodynamics simulations of collisions have found that a Mercury-like body could be formed by one or multiple giant impacts, but due to the chaotic nature of collisions, it is difficult to create a scenario where such impacts will take place. Recent work has found
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On the Formation of the W-shaped O ii Lines in Spectra of Type I Superluminous Supernovae Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Sei Saito, Masaomi Tanaka, Paolo A. Mazzali, Stephan Hachinger and Kenta Hotokezaka
H-poor Type I superluminous supernovae (SLSNe I) are characterized by O ii lines around 4000–4500 Å in pre-/near-maximum spectra, the so-called W-shaped O ii lines. As these lines are from relatively high excitation levels, they have been considered a sign of nonthermal processes, which may provide a hint of the power sources of SLSNe I. However, the conditions for these lines to appear have not been
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Infall Motions in the Hot Core Associated with the Hypercompact H ii Region G345.0061+01.794 B Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Toktarkhan Komesh, Guido Garay, Christian Henkel, Aruzhan Omar, Robert Estalella, Zhandos Assembay, Dalei Li, Andrés Guzmán, Jarken Esimbek, Jiasheng Huang, Yuxin He, Nazgul Alimgazinova, Meiramgul Kyzgarina, Shukirgaliyev Bekdaulet, Nurman Zhumabay and Arailym Manapbayeva
We report high angular resolution observations, made with the Atacama Large Millimeter Array in band 6, of high excitation molecular lines of and SO2 and of the H29α radio recombination line toward the G345.0061+01.794 B HC H ii region in order to investigate the physical and kinematical characteristics of its surroundings. Emission was detected in all observed components of the J = 14 →13 rotational
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Optical Photometric Indicators of Galaxy Cluster Relaxation Astrophys. J. (IF 4.9) Pub Date : 2024-05-12 Madeline C. Casas, Ky Putnam, Adam B. Mantz, Steven W. Allen and Taweewat Somboonpanyakul
The most dynamically relaxed clusters of galaxies play a special role in cosmological studies as well as astrophysical studies of the intracluster medium (ICM) and active galactic nucleus feedback. While high-spatial-resolution imaging of the morphology of the ICM has long been the gold standard for establishing a cluster’s dynamical state, such data are not available from current or planned surveys
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Variability of Blue Supergiants in the LMC with TESS Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Linhao Ma, Cole Johnston, Earl Patrick Bellinger, Selma E. de Mink
The blue supergiant (BSG) problem, namely, the overabundance of BSGs inconsistent with classical stellar evolution theory, remains an open question in stellar astrophysics. Several theoretical explanations have been proposed, which may be tested by their predictions for the characteristic time variability. In this work, we analyze the light curves of a sample of 20 BSGs obtained from the Transiting
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X-Ray and Radio Monitoring of the Neutron Star Low-mass X-Ray Binary 1A 1744-361: Quasiperiodic Oscillations, Transient Ejections, and a Disk Atmosphere Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Mason Ng, Andrew K. Hughes, Jeroen Homan, Jon M. Miller, Sean N. Pike, Diego Altamirano, Peter Bult, Deepto Chakrabarty, D. J. K. Buisson, Benjamin M. Coughenour, Rob Fender, Sebastien Guillot, Tolga Güver, Gaurava K. Jaisawal, Amruta D. Jaodand, Christian Malacaria, James C. A. Miller-Jones, Andrea Sanna, Gregory R. Sivakoff, Tod E. Strohmayer, John A. Tomsick, Jakob van den Eijnden
We report on X-ray (NICER/NuSTAR/MAXI/Swift) and radio (MeerKAT) timing and spectroscopic analysis from a 3 month monitoring campaign in 2022 of a high-intensity outburst of the dipping neutron star low-mass X-ray binary 1A 1744−361. The 0.5–6.8 keV NICER X-ray hardness–intensity and color–color diagrams of the observations throughout the outburst suggest that 1A 1744−361 spent most of its outburst
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The Mass Density of Mg ii Absorbers from the Australian Dark Energy Survey Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Asif Abbas, Christopher W. Churchill, Glenn G. Kacprzak, Christopher Lidman, Susanna Guatelli, Sabine Bellstedt
We present an all-southern sky survey for Mg ii λλ2796, 2803 doublet absorbers in 951 z < 4 active galactic nucleus/quasar spectra from the Australian Dark Energy Survey. The spectral resolution ranges from R = 1400 to 1700 over the wavelengths 3700–8800 Å. The survey has a 5σ detection completeness of 50% and above for rest-frame equivalent widths W r (2796) ≥ 0.3 Å. We studied 656 Mg ii absorption
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The Mass Dependence of Hα Emission and Stellar Spindown for Fully Convective M Dwarfs Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Emily K. Pass, David Charbonneau, David W. Latham, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Jessica Mink
Fully convective M dwarfs typically remain rapidly rotating and magnetically active for billions of years, followed by an abrupt and mass-dependent transition to slow rotation and quiescence. A robust understanding of this process is complicated by difficulties in estimating M dwarf ages and potential dependencies on other variables such as birth environment or metallicity. To isolate the effect of
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MHD Simulation in Galactic Center Region with Radiative Cooling and Heating Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Kensuke Kakiuchi, Takeru. K. Suzuki, Shu-ichiro Inutsuka, Tsuyoshi Inoue, Jiro Shimoda
We investigate the role of magnetic field on the gas dynamics in a galactic bulge region by three-dimensional simulations with radiative cooling and heating. While a high-temperature corona with T > 106 K is formed in the halo regions, the temperature near the midplane is ≲104 K following the thermal equilibrium curve determined by the radiative cooling and heating. Although the thermal energy of the
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Active Galactic Nuclei Selection and Demographics: A New Age with JWST/MIRI Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Jianwei Lyu, Stacey Alberts, George H. Rieke, Irene Shivaei, Pablo G. Pérez-González, Fengwu Sun, Kevin N. Hainline, Stefi Baum, Nina Bonaventura, Andrew J. Bunker, Eiichi Egami, Daniel J. Eisenstein, Michael Florian, Zhiyuan Ji, Benjamin D. Johnson, Jane Morrison, Marcia Rieke, Brant Robertson, Wiphu Rujopakarn, Sandro Tacchella, Jan Scholtz, Christopher N. A. Willmer
Understanding the coevolution of supermassive black holes and their host systems requires a comprehensive census of active galactic nuclei (AGNs) behavior across a wide range of redshift, luminosity, obscuration level, and galaxy properties. We report significant progress with JWST toward this goal from the Systematic Mid-infrared Instrument Legacy Extragalactic Survey (SMILES). Based on comprehensive
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Feedback and Galaxy Dynamics: A Study of Turbulence and Star Formation in 34 Galaxies Using the PHANGS Survey Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Bruce G. Elmegreen
The correlation between interstellar turbulent speed and local star formation rate surface density, ΣSFR, is studied using CO observations in the PHANGS survey. The local velocity dispersion of molecular gas, σ, increases with ΣSFR, but the virial parameter, α vir, is about constant, suggesting the molecular gas remains self-gravitating. The correlation arises because σ depends on the molecular surface
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Hubble Space Telescope Images of SN 1987A: Evolution of the Ejecta and the Equatorial Ring from 2009 to 2022 Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Sophie Rosu, Josefin Larsson, Claes Fransson, Peter Challis, Tuomas Kangas, Robert P. Kirshner, Stephen S. Lawrence, Peter Lundqvist, Mikako Matsuura, Jesper Sollerman, George Sonneborn, Linda Tenhu
Supernova (SN) 1987A offers a unique opportunity to study how a spatially resolved SN evolves into a young SN remnant. We present and analyze Hubble Space Telescope (HST) imaging observations of SN 1987A obtained in 2022 and compare them with HST observations from 2009 to 2021. These observations allow us to follow the evolution of the equatorial ring (ER), the rapidly expanding ejecta, and emission
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The Heavy Metal Survey: The Evolution of Stellar Metallicities, Abundance Ratios, and Ages of Massive Quiescent Galaxies since z ∼ 2 Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Aliza G. Beverage, Mariska Kriek, Katherine A. Suess, Charlie Conroy, Sedona H. Price, Guillermo Barro, Rachel Bezanson, Marijn Franx, Brian Lorenz, Yilun Ma, Lamiya A. Mowla, Imad Pasha, Pieter van Dokkum, Daniel R. Weisz
We present the elemental abundances and ages of 19 massive quiescent galaxies at z ∼ 1.4 and z ∼ 2.1 from the Keck Heavy Metal Survey. The ultradeep LRIS and MOSFIRE spectra were modeled using a full-spectrum stellar population fitting code with variable abundance patterns. The galaxies have iron abundances between [Fe/H] = −0.5 and −0.1 dex, with typical values of −0.2 [−0.3] at z ∼ 1.4 [z ∼ 2.1]
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Polarization Holes as an Indicator of Magnetic Field−Angular Momentum Alignment. I. Initial Tests Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Lijun Wang, Zhuo Cao, Xiaodan Fan, Hua-bai Li
The formation of protostellar disks is still a mystery, largely due to the difficulties in observations that can constrain theories. For example, the 3D alignment between the rotation of the disk and the magnetic fields (B-fields) in the formation environment is critical in some models, but so far it is impossible to observe. Here we study the possibility of probing the alignment between B-field and
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The MUSE Ultra Deep Field (MUDF). V. Characterizing the Mass–Metallicity Relation for Low-mass Galaxies at z ∼ 1–2 Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Mitchell Revalski, Marc Rafelski, Alaina Henry, Matteo Fossati, Michele Fumagalli, Rajeshwari Dutta, Norbert Pirzkal, Alexander Beckett, Fabrizio Arrigoni Battaia, Pratika Dayal, Valentina D’Odorico, Elisabeta Lusso, Kalina V. Nedkova, Laura J. Prichard, Casey Papovich, Celine Peroux
Using more than 100 galaxies in the MUSE Ultra Deep Field with spectroscopy from the Hubble Space Telescope’s (HST) Wide Field Camera 3 and the Very Large Telescope’s Multi Unit Spectroscopic Explorer, we extend the gas-phase mass–metallicity relation (MZR) at z ≈ 1–2 down to stellar masses of M ⋆ ≈ 107.5 M ⊙. The sample reaches 6 times lower in stellar mass and star formation rate (SFR) than previous
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Runaway OB Stars in the Small Magellanic Cloud. III. Updated Kinematics and Insights into Dynamical versus Supernova Ejections Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Grant D. Phillips, M. S. Oey, Maria Cuevas, Norberto Castro, Rishi Kothari
We use the kinematics of field OB stars to estimate the frequencies of runaway stars generated by the dynamical ejection scenario (DES), the binary supernova scenario (BSS), and the combined two-step mechanism. We update the proper motions for field OB and OBe stars in the Small Magellanic Cloud (SMC) using Gaia DR3. Our sample now contains 336 stars from the Runaways and Isolated O-Type Star Spectroscopic
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ELUCID. VIII. Simulating the Coma Galaxy Cluster to Calibrate Model and Understand Feedback Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Xiong Luo, Huiyuan Wang, Weiguang Cui, Houjun Mo, RenJie Li, Yipeng Jing, Neal Katz, Romeel Davé, Xiaohu Yang, Yangyao Chen, Hao Li, Shuiyao Huang
We conducted an investigation of the Coma cluster of galaxies by running a series of constrained hydrodynamic simulations with GIZMO-SIMBA and GADGET-3 based on initial conditions reconstructed from the SDSS survey volume in the ELUCID project. We compared simulation predictions and observations for galaxies, intracluster medium (ICM) and intergalactic medium (IGM) in and around the Coma cluster to
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Intrinsic Mass–Richness Relation of Clusters from THE THREE HUNDRED Hydrodynamic Simulations Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Mingjing Chen, Weiguang Cui, Wenjuan Fang, Zhonglue Wen
The main systematics in cluster cosmology is the uncertainty in the mass–observable relation. In this paper, we focus on the most direct cluster observable in optical surveys, i.e., richness, and constrain the intrinsic mass–richness (MR) relation of clusters in THE THREE HUNDRED hydrodynamic simulations with two runs: GIZMO-SIMBA and GADGET-X. We find that modeling the richness at a fixed halo mass
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On Innermost Stable Spherical Orbits near a Rotating Black Hole: A Numerical Study of the Particle Motion near the Plunging Region Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Ondřej Kopáček, Vladimír Karas
According to general relativity, astrophysical black holes are described by a small number of parameters. Apart from the mass of the black hole (M), among the most interesting characteristics is the spin (a), which determines the degree of rotation, i.e., the angular momentum of the black hole. The latter is observationally constrained by the spectral and timing properties of the radiation signal emerging
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Extinction Values toward Embedded Planets in Protoplanetary Disks Estimated from Hydrodynamic Simulations Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Felipe Alarcón, Edwin A. Bergin, Gabriele Cugno
Upcoming new coronographs with deeper contrast limits, together with planned and current high-contrast imaging campaigns, will push the detectability limit of protoplanets. These planet-hunting campaigns present a new opportunity to characterize protoplanets and their surrounding environments. However, there are clear uncertainties as to what the extinction levels are at different regions of protoplanetary
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Regions of Suppressed Diffusion around Supernova Remnants? Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Yiwei Bao, Pasquale Blasi, Yang Chen
The recent discovery of the so-called TeV halos has attracted much attention. The morphology of the emission requires that the region is characterized by severe suppression of the diffusion coefficient. This finding raises many questions as to its origin: (1) is the suppressed diffusion to be attributed to instabilities induced by the same radiating particles? (2) or does it actually show that the
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Influence of the Gravitational Darkening Effect on the Spectrum of a Hot, Rapidly Rotating Neutron Star. II. Iron Lines Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Agnieszka Majczyna, Jerzy Madej, Agata Różańska, Mirosław Należyty
Rapidly rotating neutron stars are similar to highly flattened ellipsoids. Observed spectra of flattened stars must exhibit effects of nonspherical shape and gravitational darkening. We examined in detail the influence of both effects on the observed central energies and profiles of lines of highly ionized iron, Fe xxv and Fe xxvi. We note that the gravitational darkening effect does not change the
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The Interaction between Stars and Past AGN Disk: Possible Explanation for the Kinematic Distributions of S-stars in the Galactic Center Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Xiao Fan, Qingwen Wu, Jiancheng Wu, Xiangli Lei, Mengye Wang, Fulin Li
The presence of young stars, aged around several million years and situated within the range of ∼0.04–1 pc from our Galactic center raises a question about their origins and dynamical evolutions. Their kinematics provide an opportunity to explore their formation or possible subsequent dynamical evolution. If Sagittarius A* was active in the past as suggested by several observations, the accretion disk
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The Study of Mode-switching Behavior of PSR J0614+2229 Using the Parkes Ultra–wide-bandwidth Receiver Observations Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Yanqing Cai, Shijun Dang, Rai Yuen, Lunhua Shang, Feifei Kou, Jianping Yuan, Lei Zhang, Zurong Zhou, Na Wang, Qingying Li, Zhigang Wen, Wenming Yan, Shuangqiang Wang, Shengnan Sun, Habtamu Menberu Tedila, Shuo Xiao, Xin Xu, Rushuang Zhao, Qijun Zhi, Aijun Dong, Bing Zhang, Wei Li, Yingying Ren, Yujia Liu
In this paper we present a detailed single-pulse and polarization study of PSR J0614+2229 based on the archived data observed on 2019 August 15 (MJD 58710) and 2019 September 12 (MJD 58738) using the ultra−wide-bandwidth low-frequency receiver on the Parkes radio telescope. The single-pulse sequences show that this pulsar switches between two emission states, in which the emission of state A occurs
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The Huge Magnetic Toroids in the Milky Way Halo Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 J. Xu, J. L. Han
The magnetic fields in our Milky Way can be revealed by the distribution of Faraday rotation measures (RMs) of radio sources behind the Galaxy and of radio pulsars inside the Galaxy. Based on the antisymmetry of the Faraday sky in the inner Galaxy to the Galactic coordinates, the magnetic field toroids above and below the Galactic plane with reversed field directions exist in the Galactic halo and
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Primordial Black Hole–Neutron Star Merger Rate in Modified Gravity Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Saeed Fakhry, Maryam Shiravand, Marzieh Farhang
In this work, we investigate the merger rate of primordial black hole–neutron star (PBH-NS) binaries in two widely studied modified gravity (MG) models: Hu–Sawicki f(R) gravity and the normal branch of Dvali–Gabadadze–Porrati gravity. In our analysis, we take into account the effects of MG on the halo properties, including halo mass function, halo concentration parameter, halo density profile, and
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21 cm Intensity Mapping with the DSA-2000 Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Ruby Byrne, Nivedita Mahesh, Gregg W. Hallinan, Liam Connor, Vikram Ravi, T. Joseph W. Lazio
Line-intensity mapping is a promising probe of the Universe’s large-scale structure. We explore the sensitivity of the DSA-2000, a forthcoming array consisting of over 2000 dishes, to the statistical power spectrum of neutral hydrogen’s 21 cm emission line. These measurements would reveal the distribution of neutral hydrogen throughout the near-redshift Universe without necessitating resolving individual
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Fast, Simple, and Accurate Time Series Analysis with Large Language Models: An Example of Mean-motion Resonances Identification Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Evgeny A. Smirnov
Classical machine learning has been actively utilized in astronomy to address various challenges, including predicting orbital stability, classifying asteroids, galaxies, and other objects, and analyzing images. However, the emerging trend in artificial intelligence involves the use of large language models such as GPT-4 and ChatGPT. These models are trained on a large corpus of text and can perform
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Pressure Balance and Energy Budget of the Nuclear Superbubble of NGC 3079 Astrophys. J. (IF 4.9) Pub Date : 2024-05-10 Jiang-Tao Li, Wei Sun, Li Ji, Yang Yang
Superbubbles in the nuclear region of galaxies could be produced by active galactic nuclei (AGN) or nuclear starburst via different driving forces. We report analysis of the multiwavelength data of the kiloparsec-scale nuclear superbubble in NGC 3079 in order to probe the mechanisms driving the expansion of the superbubble. Based on the Chandra X-ray observations, we derive the hot-gas thermal pressure
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Discovery of a Second Eclipsing, Bursting Neutron Star Low-mass X-Ray Binary in the Globular Cluster Terzan 6 Astrophys. J. (IF 4.9) Pub Date : 2024-05-09 Maureen van den Berg, Jeroen Homan, Craig O. Heinke, David A. Pooley, Rudy Wijnands, Arash Bahramian, James C. A. Miller-Jones
We have analyzed Chandra and Suzaku observations of the globular cluster Terzan 6, made when the recurrent transient GRS 1747–312 was in quiescence. Our analysis reveals the presence of a second eclipsing, bursting neutron star low-mass X-ray binary in the central regions of the cluster, in addition to GRS 1747–312. The new source, which we name Terzan 6 X2, is located only ∼0.″7 away from GRS 1747–312
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Bayesian Survey of the Dense Matter Equation of State Built upon Skyrme Effective Interactions Astrophys. J. (IF 4.9) Pub Date : 2024-05-09 Mikhail V. Beznogov, Adriana R. Raduta
The nonrelativistic model of nuclear matter (NM) with zero-range Skyrme interactions is employed within a Bayesian approach in order to study the behavior of the neutron star (NS) equation of state (EOS). A minimal number of constraints from nuclear physics and ab initio calculations of pure neutron matter (PNM) are imposed together with causality and a lower limit on the maximum mass of an NS to all
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Probing Electromagnetic Gravitational-wave Emission Coincidence in a Type I Binary-driven Hypernova Family of Long Gamma-Ray Bursts at Very High Redshift Astrophys. J. (IF 4.9) Pub Date : 2024-05-09 C. L. Bianco, M. T. Mirtorabi, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, Y. Wang, M. Della Valle, Liang Li, S. R. Zhang
The repointing time of the X-Ray Telescope (XRT) instrument on the Neil Gehrels Swift Observatory satellite has posed challenges in observing and studying the early X-ray emissions within ≈40 s after a gamma-ray burst (GRB) trigger. To address this issue, we adopt a novel approach that capitalizes on the cosmological time dilation in GRBs with redshifts ranging from 3 to 9. Applying this strategy to