Sazuna/UAT_keywords huggingface dataset:
Automatic Satellite Identification in Digital Images. Using a digital camera on the roof of the Royal Observatory, Edinburgh, images are continuously captured of the sky on a nightly basis to image satellites which pass overhead. Such satellites are seen in images as short lines since satellites move much quicker in the sky than stars, and up to 100 satellites can be imaged in one night. Using these images, software was developed (GitHub repository for code &amp; documentation: https://github.com/Jack6228/STM_Final, or DOI: https://doi.org/10.5281/zenodo.7304283.) to use known catalogs of artificial objects which orbit the Earth to determine which satellites can be seen in each image. This was achieved by comparing the expected positions of satellites in the catalog to those observed by the camera to identify matches. Overall, the project was a success and satellites are able to be identified approximately 85% of the time, which could help track space debris in a cheaper manner in a world where space is becoming increasingly more polluted.

Keywords: Observational astronomy, Astronomy software, Astronomy data acquisition, Astronomy data analysis, Artificial satellites, Astronomical instrumentation, Geostationary satellites, Astronomy image processing
QLP Data Release Notes 002: Improved Detrending Algorithm. Light curves feature many kinds of variability, including instrumental systematics, intrinsic stellar variability such as pulsations, and flux changes caused by transiting exoplanets or eclipsing binary stars. Detrending is a key pre-planet-search data processing step that aims to remove variability not due to transits. This data release note describes improvements to the Quick-Look Pipeline's detrending algorithm via the inclusion of quaternion data to remove short-timescale systematics. We describe updates to our procedure, intermediate data products outputted by the algorithm, and improvements to light curve precision.

Keywords: Time series analysis, Light curves, Transit photometry, Exoplanets
Quick-look Pipeline Light Curves for 5.7 Million Stars Observed Over the Second Year of TESS' First Extended Mission. We present High-Level Science Products (HLSPs) containing light curves from MIT's Quick-Look Pipeline (QLP) from the second year of Transiting Exoplanet Survey Satellite (TESS') first Extended Mission (Sectors 40-55; 2021 July-2022 September). In total, 12.2 million per-sector light curves for 5.7 million unique stars were extracted from 10 minutes cadence Full-Frame Images (FFIs) and are made available to the community. As in previous deliveries, QLP HLSPs include both raw and detrended flux time series for all observed stars brighter than TESS magnitude T = 13.5 mag. Starting in Sector 41, QLP also produces light curves for select fainter M dwarfs. QLP has provided the community with one of the largest sources of FFI-extracted light curves to date since the start of the TESS mission.

Keywords: Light curves, Transit photometry, Exoplanets
Two Example GRBs Where Fermi LAT "Extended" Data Gives a Better Photon List than "Photon". When analyzing Fermi LAT data for temporally contained events like gamma-ray bursts (GRBs), the best data type for analyses is "Extended," not "Photon." Although this is already recommended by the online Fermi website, it is easy to overlook and can lead to inferior analyses. Most extended "events" that are temporally and angularly consistent with GRBs are probably photons. While preparing GRB data for other research projects, the authors encountered this counter-intuitive fact several times. The data from two GRBs are presented with a simple analysis as a demonstration.

Keywords: Gamma-ray astronomy, Gamma-ray bursts, Gamma-ray transient sources, Astronomy data acquisition
The Mercury Lines in the Mean Far Ultraviolet Spectrum of HD 209459. The analysis of the coadded high resolution SWP spectrum of the Hg star HD 209459 recorded by the International Ultraviolet Explorer reveals the presence of two resonance lines of Hg II at 1649.92 and 1942.28 Å. The line synthesis of the least blended resonance line at 1942.28 Å, yields a mercury abundance of about 1000 times the solar mercury abundance. The abundances of other element are found to agree fairly well with previous determinations. These results suggest that HD 209459 might be a mild HgMn star. However more abundance determinations from high resolution high signal-to-noise optical spectra are necessary to clarify the status of this interesting object.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Light Curve Analysis of Nine Algol (EA) Eclipsing Binaries Discovered During the Dauban Survey-additional Data. The Research Note entitled Light Curve Analysis of Nine Algol (EA) Eclipsing Binaries Discovered During the Dauban Survey produced composite light curves for each of the nine systems. This analysis identified specific periods, eclipse durations, Johnson V and Sloan g photometric magnitude ranges, and system temperatures. Also in that Research Note the light curves for four of the nine binary systems were presented (V242, V243, V244, and V247). This Research Note presents light curves for the remaining five eclipsing binary systems (V239, V240, V241, V245, and V246).

Keywords: Eclipsing binary stars
Estimating the X-Ray Irradiance of the 2003 October 28 Solar Flare. The 2003 October 28 X24 solar flare was saturated in GOES XRS/A for about 10 minutes, near the peak of the event. By using RHESSI X-ray spectral fits during that same time period, the XRS/A time series of the flare and derived quantities like temperature and emission measure can be estimated.

Keywords: Solar flares, Solar x-ray flares
M31N 2017-01e: Discovery of a Previous Eruption in this Enigmatic Recurrent Nova. We report the discovery of a previously unknown eruption of the recurrent nova M31N 2017-01e that took place on 2012 January 11. The earlier eruption was detected by Pan-STARRS and occurred 1847 days (5.06 yr) prior to the eruption on 2017 January 31 (M31N 2017-01e). The nova has now been seen to have had a total of four recorded eruptions (M31N 2012-01c, 2017-01e, 2019-09d, and 2022-03d) with a mean time between outbursts of just 929.5 ± 6.8 days (2.545 ± 0.019 yr), the second shortest recurrence time known for any nova. We also show that there is a blue variable source (&lt;V&gt; = 20.56 ± 0.17, B - V ≃ 0.045), apparently coincident with the position of the nova, that exhibits a 14.3 days periodicity. Possible models of the system are proposed, but none are entirely satisfactory.

Keywords: Novae, Time domain astronomy, Recurrent novae, Cataclysmic variable stars, Andromeda Galaxy
A New Stellar Companion to GJ 1292. I present the discovery of a new stellar companion to GJ 1292 detected with the NN-EXPLORE Exoplanet and Stellar Speckle Imager at the 3.5 m WIYN Telescope. The companion was detected at an angular separation of 0.″1244, a position angle of 44°, and a delta magnitude of 0.97 at 832 nm. I also estimate a projected separation of 2.09 au, a mass ratio of 0.69, and component spectral types of M2.5 and M3.

Keywords: M dwarf stars, Binary stars, Close binary stars, Low mass stars, Speckle interferometry, Visual binary stars, High angular resolution
Variability and Parameter Dependence of Hard X-Ray Obscuration Around Supermassive Black Holes in Active Galaxies. We investigate hard X-ray obscuration of Active Galactic Nuclei (AGNs) by considering photoionization processes for a number of simulated accretion-disk winds in our magnetohydrodynamic (MHD) framework. To follow up our earlier work on calculating synthetic AGN obscuration functions, we are motivated in this work to expand our examination of the dependences of obscuration on individual parameters associated with MHD wind and coronal X-ray such as: X-ray luminosity L ion, photon index Γ, density of the wind n  o  and its radial gradient p where n ∝ n  o  r -p . We find that AGN appear to undergo a relatively drastic transition from more obscured state (e.g., N H ≳ 1022 cm-2) to unobscured state (i.e., N H ≲ 1022 cm-2) as p approaches to ~1.1 in these calculations. In the current formalism, luminosity is linearly coupled to wind density (i.e., L X ∝ n  o ), and our calculations also indicate AGN become more obscured at higher luminosity. We further discuss the plausibility of the current model in comparison with observations.

Keywords: AGN host galaxies, Magnetohydrodynamics, Radiative magnetohydrodynamics, High energy astrophysics, X-ray active galactic nuclei, Radiative transfer simulations
Gaia Astrometry Challenges the High Central Oxygen Abundance Claimed for the Pulsating Helium-Atmosphere White Dwarf KIC 08626021. The asteroseismic radius determination previously reported for the pulsating helium-atmosphere white dwarf star KIC 08626021 is 6σ discrepant with constraints from Gaia astrometry. This calls into question the other results of the asteroseismic analysis, especially the high (central) oxygen abundance that stellar evolutionary models have been unable to reproduce.

Keywords: White dwarf stars, Stellar cores, Astrometry, Asteroseismology, Astronomical methods
The Aluminum Abundance of HD 209459 from Far Ultraviolet and Optical Spectra. The abundance of aluminum in the atmosphere of HD 209459 is measured by synthesizing selected optical and ultraviolet lines having high quality atomic data. The Al III resonance lines at 1854.12 and 1862.79 Å are reproduced by an aluminum underabundance of about 0.3 times the solar aluminum abundance. The Al II line at 4663.06 Å is properly fit by a solar aluminum abundance. This difference needs confirmation by the modeling of more lines in both spectral regions.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Kepler K2 Observations of the Faint, Understudied Polar SDSS J092122.84+203857.1. SDSS J092122.84+203857.1 is a polar-type cataclysmic variable system, consisting of a strongly magnetized white dwarf that accretes from its red dwarf companion. It is also one of just five polars known to have been observed by Kepler during its K2 mission. We analyzed the K2 short-cadence light curve of J0921 and identified a weak, but highly coherent, signal at a frequency of 17.099 cycles day-1, corresponding with the system's reported orbital period. We see no overall variation in the accretion rate across the K2 observation, and both our measurement of the period and the binned orbital profile are very consistent with previous ground-based data.

Keywords: Cataclysmic variable stars, AM Herculis stars
Witnessing a Galaxy Cluster Merger with JWST and a Chandra X-Ray Temperature Map. The first James Webb Space Telescope (JWST) image released was of galaxy cluster SMACSJ0723.3-7327, a lensing cluster at z = 0.39 showing detail only JWST can provide. While the majority of the focus has been on the brilliantly lensed galaxies at redshifts far beyond it, there is more to the story than it being just a lensing cluster. The Chandra X-ray temperature map tells a tale of a merging cluster with a significant subcluster leaving a wake in the intracluster medium (ICM). This paper presents a high fidelity temperature map of SMACSJ0723.3-7327 using adaptive circular binning, overlaid with the JWST image, showing clear signs of merger activity. As the ICM extends well past the boundaries of the JWST imagery, and no low-frequency radio observations are yet published, a fuller story of this cluster remains to be told. This new X-ray temperature map reveals new details of a moderately distant actively merging cluster.

Keywords: Galaxy clusters, X-ray astronomy, Astronomy data analysis, Spectroscopy, Intracluster medium, Astronomy data visualization
First Release of PLATO Consortium Stellar Limb-darkening Coefficients. We release the first grid of stellar limb-darkening coefficients (LDCs) and intensity profiles (IPs) computed by the consortium of the PLAnetary Transits and Oscillations of stars (PLATO), the next medium-class (M3) mission under development by the European Space Agency to be launched in 2026. We have performed spectral synthesis with TurboSpectrum on a grid of MARCS model atmospheres. Finally, we adopted ExoTETHyS to convolve the high-resolution spectra (R = 2 × 105) with the state-of-the-art response functions for all the PLATO cameras, and computed the LDCs that best approximate the convolved IPs. In addition to the PLATO products, we provide new LDCs and IPs for the Kepler mission, based on the same grid of stellar atmospheric models and calculation procedures. The data can be downloaded from the following link: https://doi.org/10.5281/zenodo.7339706.

Keywords: Exoplanets, Limb darkening, Space telescopes, Transit photometry, Stellar atmospheres
The Behavior of HgMn Stars in the Far-UV-Paper 19: HD 149121. The analysis of three spectra of the Mn Hg Sr star HD 149121 recorded by the SWP camera on board the International Ultraviolet Explorer does not reveal variations of the far-ultraviolet flux of this star over two sets of observations separated by about 6 yr. The synthesis of the Sr II resonance line at 4215.52 Å in a high resolution high signal-to-noise SOPHIE spectrum of HD 149121 yields a large overabundance of about 200 times the solar abundance of strontium and confirms that HD 149121 is a strontium-rich HgMn star.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Re-evaluation of the Effect of Brown Dwarfs' Viewing Geometry using a Bayesian Framework. A brown dwarf's viewing geometry can affect measurements of variability amplitudes and emergent spectra. Historically, this angle was derived by combining rotation periods and $v\,\sin \,i$ assuming that they are statistically independent. Recently, Masuda &amp; Winn showed that this assumption could lead to biased results. The same study presented a solution that properly incorporates the correlation between the equatorial and projected rotational velocities. We use this Bayesian framework to re-calculate the viewing angles of 18 variable brown dwarfs with known $v\,\sin \,i$ values and photometric rotation periods. We find that the viewing angle distributions change most significantly in equator-on cases. We re-derive the correlation coefficients between the viewing angle, variability amplitude, and color anomaly. These results confirm and refine these correlations and highlight the importance of proper posterior sampling to determine the inclination angle of the spin axis.

Keywords: Inclination, Stellar rotation, Brown dwarfs, Bayesian statistics
A Partial Disintegration of Active Centaur/Comet P/2020 MK4?. Centaur P/2020 MK4 (a = 6.19 au, e = 0.011) was discovered in 2020 and quickly brightened to V ~ 18.5. As of early 2022 November, no astrometric observations had been reported in 2021 or 2022. The object should have been easily found had it retained its 2020 absolute magnitude. We find that P/2020 MK4 now appears as an ~10″ wide low surface brightness coma, with a faint (r ~ 24.9) point-like source. The rates of brightening and fading of P/2020 MK4 are both much slower than the larger Centaur 29P/Schwassmann-Wachmann 1, which is on a similar orbit. Perhaps the image morphology and unusual brightening and fading of P/2020 MK4 were due to a partial disintegration event.

Keywords: Comets, Centaur group, Comae
Fastcc: Fast Color Corrections for Broadband Radio Telescope Data. Broadband receiver data need color corrections applying to correct for the different source spectra across their wide bandwidths. The full integration over a receiver bandpass may be computationally expensive and redundant when repeated many times. Color corrections can be applied, however, using a simple quadratic fit based on the full integration instead. Here we describe fastcc and interpcc, quick Python and IDL codes that return, respectively, color correction coefficients for different power-law spectral indices and modified blackbodies for various Cosmic Microwave Background related experiments. The codes are publicly available, and can be easily extended to support additional telescopes.

Keywords: CMBR detectors, Radio receivers, Astronomy data analysis, Photometry
Gaia22eor: Symbiotic Star V2756 Sgr Detected in a Deep Eclipse. V2756 Sgr is a long-known S-type symbiotic binary that was recently detected in ~1 mag eclipse-like fading by the Gaia satellite. This behavior was reported as a Gaia Science Alert under the designation Gaia22eor. V2756 Sgr has not been reported as an eclipsing symbiotic system. In this contribution, we have investigated the recent light curves of this target obtained by Gaia and ASAS-SN survey and supplemented these data by the photometry from the ASAS survey and DASCH archive. In addition, low-resolution BP/RP spectra from Gaia were examined. Based on the presented analysis, we conclude that the observed fading is indeed an eclipse of the hot component of V2756 Sgr by the cool giant. The data also allowed us to refine the orbital period to 725 ± 3 days.

Keywords: Eclipsing binary stars, Symbiotic binary stars, Gaia, Photometry
Polarimetry of the Total Lunar Eclipse on 2022 November 8. We have measured the degree of linear polarization of the Moon during its total eclipse on 2022 November 8, and found P ≈ -2% in the V filter. The plane of preferential polarization was oriented at ~36° counting clockwise from the lunar equator. These measurements suggest global asymmetry in the spatial distribution of aerosol particles in the uppermost atmosphere of Earth, with their net linear polarization being P ≈ -6.5%.

Keywords: Lunar eclipses, Earth atmosphere, The Moon, Polarimetry, Atmospheric science
PERISTOLE: Package That Generates Time Delay Plots Caused by Gravitational Lensing. We present PERISTOLE to study the various time delays associated with the pulsar rotation and other general relativistic aspects of binary pulsars. It is made available as an open-source python package which takes some parameters of the double pulsar system as input and outputs the rotational and latitudinal lensing delays along with the geometric and Shapiro delays that arise due to gravitational lensing. This package was intended to provide a way to quickly analyze, evaluate and study the differences between variations of the same systems and also to quantify the consequences that different parameters have over the system. Through this research note, we briefly describe the motivation behind PERISTOLE and showcase its capabilities using the only double pulsar system ever found, J0737-3039.

Keywords: Astroinformatics, Binary pulsars, Astronomy software
The Behavior of HgMn Stars in the Far UV-Paper 20: HD 14228. The analysis of three spectra of the Mn Hg Sr star HD 14228 recorded by the SWP camera on board the International Ultraviolet Explorer does not reveal variations of the far-ultraviolet flux over a nine years time interval. The analysis of the TESS lightcurve of HD 14228 confirms a very short period of 0.34 day already reported in the literature. This periodicity, attributed to rotation, could be a mode of radial pulsation too.

Keywords: Mercury-manganese stars, Chemically peculiar stars
On the Angle of Sunset. We calculate the angle ψ between the Sun path at sunset and the horizon to be $\psi =\arctan \left[\sqrt{1-\tfrac{{\sin }^{2}\delta }{{\cos }^{2}\phi }}\ \tan (90^\circ -\phi )\right]$ , where δ is the decl. of the Sun, and ϕ is the latitude of the place. We dub this angle the ghorub angle, after غروب, the Arabic word for sunset.

Keywords: The Sun, Astrometry
Pre-maximum Evolution of the Classical Nova YZ Reticuli. The pre-maximum evolution of a nova is the last frontier in studying such objects. YZ Reticuli 2020 is the only nova whose X-ray flash was detected. The X-ray flash occurs immediately after the onset of thermonuclear runaway, so its physical properties impose severe constraints on the nova model. We discuss what we can learn from the early phase observations.

Keywords: X-ray astronomy, High energy astrophysics, White dwarf stars, Cataclysmic variable stars, Classical novae
The Relation between Gas-phase Metallicity and Stellar Mass Surface Density in Post-starburst E+A and E+A+ Galaxies within the Coma Cluster Observed by the SDSS-IV MaNGA Survey. We present an analysis of the Mass-Metallicity Relation (MZR) in 29 post-starburst galaxies in the Coma Cluster. Outward from the central dominant galaxy, NGC 4889, we conducted a conical survey of all galaxies observed by the Sloan Digital Sky Survey Data Release 17 (SDSS DR17) Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey within a 5° radius and redshift constraints 0.013 &lt; z &lt; 0.033. We identified 21 E+A galaxies and 8 "E+A+ galaxies" whose spectra matched the criteria of an E+A galaxy, but contain Balmer emission lines, indicating star formation. We utilized the MaNGA data to calculate each galaxy's star formation rate densities, gas-phase metallicity and stellar mass. We then compared the MZR between E+A galaxies and E+A+ galaxies to observe how varying star formation rates alter this relation.

Keywords: Post-starburst galaxies, Early-type galaxies, E+A galaxies, Galaxy evolution, Galaxies
Life on Titan May Signal Early Life in the Universe. The temperature of the cosmic microwave background was equal to the surface temperature of Saturn's moon Titan, 94 K, at a redshift z = 33.5, after the first galaxies formed. Titan-like objects would have maintained this surface temperature for tens of Myr irrespective of their distance from a star. Titan has the potential for the chemistry of familiar life in its subsurface water ocean, as well new forms of life in the rivers, lakes and seas of liquid methane and ethane on its surface. The potential future discovery of life on Titan would open the possibility that the earliest lifeforms emerged in metal-rich environments of the earliest galaxies in the universe, merely 100 Myr after the big bang.

Keywords: Astrobiology, Population III stars
Update on Global Helioseismic Observations of the Solar Torsional Oscillation 167: Command not found.. We present an up-to-date latitude-time map of the solar zonal flows at 0.99 R ⊙ from global helioseismology using data from the Global Oscillation Network Group, the Michelson Doppler Imager, and the Helioseismic and Magnetic Imager.

Keywords: Helioseismology, Solar physics, Solar rotation
Planetary Line-to-accretion Luminosity Scaling Relations: Extrapolating to Higher-order Hydrogen Lines. Aoyama et al. provided scaling relations between hydrogen-line luminosities and the accretion luminosity for planetary-mass objects. These fits should be an improvement over blind extrapolations of stellar relations. The fits go up only to the n = 8 electron energy level, but higher-n Balmer lines have been observed in the near-UV with UVES. We extend the scaling relations to higher-n levels for the Balmer and other series by fitting the fit coefficients (a, b) themselves and extrapolating them. Within the assumption of an accretion shock as the source of line emission, these fits should be robust for accreting planetary-mass objects.

Keywords: Accretion, H I line emission, Scaling relations, Classical T Tauri stars, Exoplanet formation, Extrasolar gaseous giant planets
The Implications of Ultra-Faint Dwarf Galaxy Reticulum II on the Common Envelope Jets Supernova r-process Scenario. We show that the common envelope jets supernova (CEJSN) r-process scenario is compatible with very recent observationally determined properties of the stars in the ultra faint dwarf (UFD) galaxy Reticulum II that are strongly enhanced in r-process elements. These new results, like efficient mixing of the r-process elements in the Reticulum II galaxy, have some implications on the CEJSN r-process scenario for UFD galaxies. In particular, the energetic jets efficiently mix with the common envelope ejecta and then with the entire interstellar medium of Reticulum II. The compatibility that we find between the scenario and new observations suggests that the CEJSN r-process scenario supplies a non-negligible fraction of the r-process elements.

Keywords: Neutron stars, Core-collapse supernovae, Nucleosynthesis, R-process, Stellar jets, Massive stars