Sazuna/UAT_keywords huggingface dataset:
In Search of Infall Motion in Molecular Clumps. IV. Mapping of the Global Infall Sources. We have used the IRAM 30 m telescope to map some targets with HCO+ (1-0) and H13CO+ (1-0) lines in order to search for evidence of gas infall in clumps. In this paper, we report the mapping results for 13 targets. All of these targets show HCO+ emissions, while H13CO+ emissions are observed in 10 of them. The HCO+ integrated intensity maps of 10 targets show clear clumpy structures, and nine targets show clumpy structures in the H13CO+ maps. Using the RADEX radiative transfer code, we estimate the column density of H13CO+, and we determine the abundance ratio [H13CO+]/[H2] to be approximately 10-12-10-10. Based on the asymmetry of the HCO+ line profiles, we identify 11 targets that show blue profiles, while six clumps have evidence of global infall. We use the RATRAN and two-layer models to fit the HCO+ line profiles of these infall sources, and analyze their spatial distribution of the infall velocity. The average infall velocities estimated by these two models are 0.24-1.85 km s-1 and 0.28-1.45 km s-1, respectively. The mass infall rate ranges from approximately 10-5 to 10-2 M ⊙ yr-1, which suggests that intermediate- or high-mass stars may be forming in the target regions.

Keywords: Star formation, Molecular clouds, Interstellar medium, Collapsing clouds
The Closest View of a Fast Coronal Mass Ejection: How Faulty Assumptions Near Perihelion Lead to Unrealistic Interpretations of PSP/WISPR Observations. We report on the closest view of a coronal mass ejection (CME) observed by the Parker Solar Probe (PSP)/ Wide-field Imager for Parker Solar PRobe (WISPR) instrument on 2022 September 5, when PSP was traversing from a distance of 15.3 to 13.5 R ☉ from the Sun. The CME leading edge and an arc-shaped concave-up structure near the core were tracked in the WISPR field of view using the polar coordinate system for the first time. Using the impact distance on the Thomson surface, we measured the average speeds of the CME leading edge and concave-up structure as ≈2500 ± 270 km s-1 and ≈400 ± 70 km s-1 with a deceleration of ≈20 m s-2 for the latter. The use of the plane-of-sky approach yielded an unrealistic speed of more than 3 times this estimate. We also used single viewpoint STEREO/COR-2A images to fit the Graduated Cylindrical Shell (GCS) model to the CME while incorporating the source region location from Extreme-Ultraviolet Imager of Solar Orbiter and estimated a 3D speed of ≈2700 km s-1. We conclude that this CME exhibits the highest speed during the ascending phase of solar cycle 25. This places it in the category of extreme-speed CMEs, which account for only 0.15% of all CMEs listed in the CDAW CME catalog.

Keywords: Solar corona, Solar coronal transients, Solar coronal mass ejections, Solar magnetic reconnection
Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The Core of the Highest-redshift Galaxy Overdensity at z = 7.88 Confirmed by NIRSpec/JWST. The protoclusters in the epoch of reionization, traced by galaxy overdensity regions, are ideal laboratories for studying the process of stellar assembly and cosmic reionization. We present the spectroscopic confirmation of the core of the most distant protocluster at z = 7.88, A2744-z7p9OD, with the James Webb Space Telescope NIRSpec integral field unit spectroscopy. The core region includes as many as four galaxies detected in [O III] 4960 and 5008 Å in a small area of ~3″ × 3″, corresponding to ~11 × 11 kpc, after the lensing magnification correction. Three member galaxies are also tentatively detected in dust continuum in Atacama Large Millimeter/submillimeter Array Band 6, which is consistent with their red ultraviolet continuum slopes, β ~ -1.3. The member galaxies have stellar masses in the range of log(M */M ☉) ~7.6-9.2 and star formation rates of ~3-50 M ☉ yr-1, showing a diversity in their properties. FirstLight cosmological simulations reproduce the physical properties of the member galaxies including the stellar mass, [O III] luminosity, and dust-to-stellar mass ratio, and predict that the member galaxies are on the verge of merging in a few to several tens of Myr to become a large galaxy with M * ~ 6 × 109 M ☉. The presence of a multiple merger and evolved galaxies in the core region of A2744-z7p9OD indicates that environmental effects are already at work 650 Myr after the Big Bang.

Keywords: Primordial galaxies, Protoclusters
Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days. GJ 367 is a bright (V ≈ 10.2) M1 V star that has been recently found to host a transiting ultra-short period sub-Earth on a 7.7 hr orbit. With the aim of improving the planetary mass and radius and unveiling the inner architecture of the system, we performed an intensive radial velocity follow-up campaign with the HARPS spectrograph-collecting 371 high-precision measurements over a baseline of nearly 3 yr-and combined our Doppler measurements with new TESS observations from sectors 35 and 36. We found that GJ 367 b has a mass of M b = 0.633 ± 0.050 M ⊕ and a radius of R b = 0.699 ± 0.024 R ⊕, corresponding to precisions of 8% and 3.4%, respectively. This implies a planetary bulk density of ρ b = 10.2 ± 1.3 g cm-3, i.e., 85% higher than Earth's density. We revealed the presence of two additional non-transiting low-mass companions with orbital periods of ~11.5 and 34 days and minimum masses of ${M}_{{\rm{c}}}\sin {i}_{{\rm{c}}}$ = 4.13 ± 0.36 M ⊕ and ${M}_{{\rm{d}}}\sin {i}_{{\rm{d}}}$ = 6.03 ± 0.49 M ⊕, respectively, which lie close to the 3:1 mean motion commensurability. GJ 367 b joins the small class of high-density planets, namely the class of super-Mercuries, being the densest ultra-short period small planet known to date. Thanks to our precise mass and radius estimates, we explored the potential internal composition and structure of GJ 367 b, and found that it is expected to have an iron core with a mass fraction of ${0.91}_{-0.23}^{+0.07}$ . How this iron core is formed and how such a high density is reached is still not clear, and we discuss the possible pathways of formation of such a small ultra-dense planet. *Based on observations made with the ESO-3.6 m telescope at La Silla Observatory under programs 1102.C-0923 and 106.21TJ.001.

Keywords: Extrasolar rocky planets, Exoplanet detection methods, Exoplanet systems, Exoplanets
Coronal Heating Rate in the Slow Solar Wind. This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume, with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a minor fraction of the solar wind energy flux, since most of the energy dissipation that feeds the heating and acceleration of the coronal flow occurs much closer to the Sun than the heights probed in the present study, which range from 6.3 to 13.3 R ⊙. The energy deposited to the supersonic wind is then used to explain the observed slight residual wind acceleration and to maintain the plasma in a nonadiabatic state. As derived in the Wentzel-Kramers-Brillouin limit, the present energy transfer rate estimates provide a lower limit, which can be very useful in refining the turbulence-based modeling of coronal heating and subsequent solar wind acceleration.

Keywords: Magnetohydrodynamics, Interplanetary turbulence, The Sun, Solar coronal heating, Solar wind, Solar physics, Solar corona, Magnetohydrodynamical simulations
Proton Temperature Anisotropy within the Interplanetary Coronal Mass Ejections Sheath at 1 au. The sheath plasma of interplanetary coronal mass ejections (ICMEs) is highly compressed, heated, turbulent, and magnetically intense relative to the ambient solar wind. In this Letter, we perform a detailed study of proton temperature anisotropy within the 333 ICME sheath regions observed on board the Wind spacecraft spanning the years 1995-2015. Our observations show that marginal stability thresholds of mirror mode and firehose instabilities predominantly constrain the proton temperature anisotropy within these sheath regions regardless of ICME sheath plasma speed. This is true even when the plasma beta values are less than 2, a parameter space that should have favored the prevalence of parallel firehose and proton cyclotron instabilities according to linear stability analysis. This investigation demonstrates the critical role played by distinct plasma instabilities in shaping the evolution of ICME sheath plasma compared to the broader solar wind environment.

Keywords: Solar wind, Solar coronal mass ejections
Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function. We conduct a systematic tidal disruption event (TDE) demographics analysis using the largest sample of optically selected TDEs. A flux-limited, spectroscopically complete sample of 33 TDEs is constructed using the Zwicky Transient Facility over 3 yr (from 2018 October to 2021 September). We infer the black hole (BH) mass (M BH) with host galaxy scaling relations, showing that the sample M BH ranges from 105.1 M ⊙ to 108.2 M ⊙. We developed a survey efficiency corrected maximum volume method to infer the rates. The rest-frame g-band luminosity function can be well described by a broken power law of $\phi ({L}_{g})\propto {\left[{\left({L}_{g}/{L}_{\mathrm{bk}}\right)}^{0.3}+{\left({L}_{g}/{L}_{\mathrm{bk}}\right)}^{2.6}\right]}^{-1}$ , with L bk = 1043.1 erg s-1. In the BH mass regime of 105.3 ≲ (M BH/M ⊙) ≲ 107.3, the TDE mass function follows $\phi ({M}_{\mathrm{BH}})\propto {M}_{\mathrm{BH}}^{-0.25}$ , which favors a flat local BH mass function ( ${{dn}}_{\mathrm{BH}}/d\mathrm{log}{M}_{\mathrm{BH}}\approx \mathrm{constant}$ ). We confirm the significant rate suppression at the high-mass end (M BH ≳ 107.5 M ⊙), which is consistent with theoretical predictions considering direct capture of hydrogen-burning stars by the event horizon. At a host galaxy mass of M gal ~ 1010 M ⊙, the average optical TDE rate is ≈3.2 × 10-5 galaxy-1 yr-1. We constrain the optical TDE rate to be [3.7, 7.4, and 1.6] × 10-5 galaxy-1 yr-1 in galaxies with red, green, and blue colors.

Keywords: Luminosity function, Supermassive black holes, Black holes, Tidal disruption, Galaxy nuclei, Time domain astronomy
Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm. The first James Webb Space Telescope observations of TRAPPIST-1 c showed a secondary eclipse depth of 421 ± 94 ppm at 15 μm, which is consistent with a bare rock surface or a thin, O2-dominated, low-CO2 atmosphere. Here we further explore potential atmospheres for TRAPPIST-1 c by comparing the observed secondary eclipse depth to synthetic spectra of a broader range of plausible environments. To self-consistently incorporate the impact of photochemistry and atmospheric composition on atmospheric thermal structure and predicted eclipse depth, we use a two-column climate model coupled to a photochemical model and simulate O2-dominated, Venus-like, and steam atmospheres. We find that a broader suite of plausible atmospheric compositions are also consistent with the data. For lower-pressure atmospheres (0.1 bar), our O2-CO2 atmospheres produce eclipse depths within 1σ of the data, consistent with the modeling results of Zieba et al. However, for higher-pressure atmospheres, our models produce different temperature-pressure profiles and are less pessimistic, with 1-10 bar O2, 100 ppm CO2 models within 2.0σ-2.2σ of the measured secondary eclipse depth and up to 0.5% CO2 within 2.9σ. Venus-like atmospheres are still unlikely. For thin O2 atmospheres of 0.1 bar with a low abundance of CO2 (~100 ppm), up to 10% water vapor can be present and still provide an eclipse depth within 1σ of the data. We compared the TRAPPIST-1 c data to modeled steam atmospheres of ≤3 bars, which are 1.7σ-1.8σ from the data and not conclusively ruled out. More data will be required to discriminate between possible atmospheres or more definitively support the bare rock hypothesis.

Keywords: Extrasolar rocky planets, Exoplanet atmospheres
From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion. We present the discovery of the Type II supernova SN 2023ixf in M101 and follow-up photometric and spectroscopic observations, respectively, in the first month and week of its evolution. Our discovery was made within a day of estimated first light, and the following light curve is characterized by a rapid rise (≈5 days) to a luminous peak (M  V  ≈ - 18.2 mag) and plateau (M  V  ≈ - 17.6 mag) extending to 30 days with a fast decline rate of ≈0.03 mag day-1. During the rising phase, U - V color shows blueward evolution, followed by redward evolution in the plateau phase. Prominent flash features of hydrogen, helium, carbon, and nitrogen dominate the spectra up to ≈5 days after first light, with a transition to a higher ionization state in the first ≈2 days. Both the U-V color and flash ionization states suggest a rise in the temperature, indicative of a delayed shock breakout inside dense circumstellar material (CSM). From the timescales of CSM interaction, we estimate its compact radial extent of ~(3-7) × 1014 cm. We then construct numerical light-curve models based on both continuous and eruptive mass-loss scenarios shortly before explosion. For the continuous mass-loss scenario, we infer a range of mass-loss history with 0.1-1.0 M ⊙ yr-1 in the final 2-1 yr before explosion, with a potentially decreasing mass loss of 0.01-0.1 M ⊙ yr-1 in ~0.7-0.4 yr toward the explosion. For the eruptive mass-loss scenario, we favor eruptions releasing 0.3-1 M ⊙ of the envelope at about a year before explosion, which result in CSM with mass and extent similar to the continuous scenario. We discuss the implications of the available multiwavelength constraints obtained thus far on the progenitor candidate and SN 2023ixf to our variable CSM models.

Keywords: Red supergiant stars, Core-collapse supernovae, Type II supernovae, Massive stars, Stellar mass loss, Circumstellar matter, Supergiant stars, Supernovae
Low- and High-energy Neutrinos from SN 2023ixf in M101. Supernova (SN) 2023ixf in M101 is the closest SN explosion observed in the last decade. Therefore, it is a suitable test bed to study the role of jets in powering the SN ejecta. With this aim, we explored the idea that high-energy neutrinos could be produced during the interaction between the jets and the intense radiation field produced in the SN explosion and eventually be observed by the IceCube neutrino telescope. The lack of detection of such neutrinos has significantly constrained both the fraction of stellar collapses that produce jets and/or the theoretical models for neutrino production. Finally, we investigated the possibility of detecting low-energy neutrinos from SN 2023ixf with the Super- and Hyper-Kamiokande experiments, obtaining, in both cases, subthreshold estimates.

Keywords: Supernova neutrinos, Jets
Constraints on the Intergalactic Magnetic Field Strength from γ-Ray Observations of GRB 221009A. Characteristics of the cascade gamma-ray signal resulting from very-high-energy gamma-ray sources, such as gamma-ray bursts, can be used to constrain the strength and structure of intergalactic magnetic fields (IGMFs). There has been a debate on whether GRB 190114C, the first gamma-ray burst with observed TeV photons, can constrain the IGMF. Recently, LHAASO detected the brightest-of-all-time GRB 221009A, which has much larger energy in the TeV band, and the spectrum extends to energy above 10 TeV, providing an unprecedented opportunity to study IGMF. We perform a Monte Carlo simulation of the cascade process with the public ELMAG code, considering the TeV data of GRB 221009A observed by LHAASO. By comparing the resulting cascade emission with the flux limit obtained from Fermi-LAT observations, we infer a limit of B ≥ 10-18.5 G for IGMF. Though this limit may not be as strong as the limit from blazars, it serves as an independent constraint on IGMF from a new class of TeV sources.

Keywords: Gamma-ray bursts, Magnetic fields, High energy astrophysics, Intergalactic medium
High-resolution [O I] Line Spectral Mapping of TW Hya Consistent with X-Ray-driven Photoevaporation. Theoretical models indicate that photoevaporative and magnetothermal winds play a crucial role in the evolution and dispersal of protoplanetary disks and affect the formation of planetary systems. However, it is still unclear what wind-driving mechanism is dominant or if both are at work, perhaps at different stages of disk evolution. Recent spatially resolved observations by Fang et al. of the [O I] 6300 Å spectral line, a common disk wind tracer in TW Hya, revealed that about 80% of the emission is confined to the inner few astronomical units of the disk. In this work, we show that state-of-the-art X-ray-driven photoevaporation models can reproduce the compact emission and the line profile of the [O I] 6300 Å line. Furthermore, we show that the models also simultaneously reproduce the observed line luminosities and detailed spectral profiles of both the [O I] 6300 Å and the [Ne II] 12.8 μm lines. While MHD wind models can also reproduce the compact radial emission of the [O I] 6300 Å line, they fail to match the observed spectral profile of the [O I] 6300 Å line and underestimate the luminosity of the [Ne II] 12.8 μm line by a factor of 3. We conclude that, while we cannot exclude the presence of an MHD wind component, the bulk of the wind structure of TW Hya is predominantly shaped by a photoevaporative flow.

Keywords: Computational astronomy, Protoplanetary disks, Classical T Tauri stars
Sizes and Mass Profiles of Candidate Massive Galaxies Discovered by JWST at 7 &lt; z &lt; 9: Evidence for Very Early Formation of the Central 100 pc of Present-day Ellipticals. The first JWST data revealed an unexpected population of red galaxies that appear to have redshifts of z ~ 7-9 and high masses of M * ≳ 1010 M ☉. Here we fit Sérsic profiles to the F200W NIRCam images of the 13 massive galaxy candidates of Labbé et al., to determine their structural parameters. Satisfactory fits were obtained for nine galaxies. We find that their effective radii are extremely small, ranging from r e ~ 80 pc to r e ~ 300 pc, with a mean of &lt;r e&gt; ≈ 150 pc. For their apparent stellar masses, the galaxies are smaller than any other galaxy population that has been observed at any other redshift. We use the fits to derive circularized three-dimensional stellar mass profiles of the galaxies, and compare these to the mass profiles of massive quiescent galaxies at z ~ 2.3 and nearby elliptical galaxies. Despite the fact that the high-redshift galaxies have 10-20 times smaller half-light radii than their putative descendants, the central stellar densities are very similar. The most straightforward interpretation is that the dense compact inner regions of the most massive ellipticals today were already in place ~600 Myr after the Big Bang. We caution that the redshifts and masses of the galaxies remain to be confirmed, and that the complex NIRCam point-spread function is not yet fully characterized.

Keywords: James Webb Space Telescope, High-redshift galaxies, Galaxy evolution
High-resolution Spectroscopic Metallicities of Milky Way Cepheid Standards and Their Impact on the Leavitt Law and the Hubble Constant. Milky Way Cepheid variables with accurate Hubble Space Telescope photometry have been established as standards for primary calibration of the cosmic distance ladder to achieve a percent-level determination of the Hubble constant (H 0). These 75 Cepheid standards are the fundamental sample for investigation of possible residual systematics in the local H 0 determination due to metallicity effects on their period-luminosity relations. We obtained new high-resolution (R ~ 81,000), high-signal-to-noise (S/N ~ 50-150) multiepoch spectra of 42 out of 75 Cepheid standards using the ESPaDOnS instrument at the 3.6 m Canada-France-Hawaii Telescope. Our spectroscopic metallicity measurements are in good agreement with the literature values with systematic differences up to 0.1 dex due to different metallicity scales. We homogenized and updated the spectroscopic metallicities of all 75 Milky Way Cepheid standards and derived their multiwavelength (GVIJHK  s ) period-luminosity-metallicity and period-Wesenheit-metallicity relations using the latest Gaia parallaxes. The metallicity coefficients of these empirically calibrated relations exhibit large uncertainties due to low statistics and a narrow metallicity range (Δ[Fe/H] = 0.6 dex). These metallicity coefficients are up to 3 times better constrained if we include Cepheids in the Large Magellanic Cloud and range between -0.21 ± 0.07 and -0.43 ± 0.06 mag dex-1. The updated spectroscopic metallicities of these Milky Way Cepheid standards were used in the Cepheid-supernovae distance ladder formalism to determine H 0 = 72.9 ± 1.0 km s-1 Mpc-1, suggesting little variation (~0.1 km s-1 Mpc-1) in the local H 0 measurements due to different Cepheid metallicity scales.

Keywords: Hubble constant, Cepheid variable stars, Stellar pulsations, Distance indicators
Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia. The Gaia mission has detected many white dwarfs (WDs) in binary and triple configurations, and while observations suggest that triple-stellar systems are common in our Galaxy, not much attention was devoted to WDs in triples. For stability reasons, these triples must have hierarchical configurations, i.e., two stars are on a tight orbit (the inner binary), with the third companion on a wider orbit about the inner binary. In such a system, the two orbits torque each other via the eccentric Kozai-Lidov mechanism, which can alter the orbital configuration of the inner binary. We simulate thousands of triple-stellar systems for over 10 Gyr, tracking gravitational interactions, tides, general relativity, and stellar evolution up to their WD fate. As demonstrated here, three-body dynamics coupled with stellar evolution is a critical channel to form tight WD binaries or merge a WD binary. Among these triples, we explore their manifestations as cataclysmic variables, Type Ia supernovae, and gravitational-wave events. The simulated systems are then compared to a sample of WD triples selected from the Gaia catalog. We find that including the effect of mass-loss-induced kicks is crucial for producing a distribution of the inner binary-tertiary separations that is consistent with Gaia observations. Lastly, we leverage this consistency to estimate that, at minimum, 30% of solar-type stars in the local 200 pc were born in triples.

Keywords: Astrodynamics, Theoretical models, Binary stars, White dwarf stars, Gravitational wave sources, Three-body problem, Trinary stars, Cataclysmic variable stars, Common envelope evolution, Stellar evolution