Caballero identified the star 2MASS 19281982-2640123 as a potential Sun-like star from which the WOW! signal could have originated. We conducted a search for artificial narrowband (2.79 Hz/1.91 Hz), drifting (±4 Hz s−1) technosignatures from this source using the turboSETI pipeline, from 1–2 GHz, using simultaneous multi-telescope observations with both the Robert C. Byrd Green Bank Telescope and the newly refurbished Allen Telescope Array on 2022 May 21. Both telescope observations had an overlap of 580 s. While blind searches using radio telescopes have been conducted in the general field of view in which the WOW! signal was first detected, this is the first time a targeted search has been done. No technosignature candidates were detected.
The American Astronomical Society (AAS), established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. Its membership of about 7,000 individuals also includes physicists, mathematicians, geologists, engineers, and others whose research and educational interests lie within the broad spectrum of subjects comprising contemporary astronomy. The mission of the AAS is to enhance and share humanity's scientific understanding of the universe.
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ISSN: 2515-5172
Research Notes of the AAS is a non-peer reviewed, indexed and secure record of works in progress, comments and clarifications, null results, or timely reports of observations in astronomy and astrophysics.
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Karen I. Perez et al 2022 Res. Notes AAS 6 197
A. Loeb et al 2024 Res. Notes AAS 8 39
We have conducted an extensive towed-magnetic-sled survey during the period 2023 June 14–28, over the seafloor about 85 km north of Manus Island, Papua New Guinea, centered around the calculated path of the bolide CNEOS 2014 January 8 (IM1). We found about 850 spherules of diameter 0.05–1.3 mm in our samples. They were analyzed by microXRF, Electron Probe Microanalyzer and ICP Mass spectrometry. We identified 22% of the spherules as the product of planetary igneous differentiation and labeled them as D-type spherules. A small portion of the D-spherules show an excess of Be, La and U, by up to three orders of magnitude relative to the solar system standard of CI chondrites, and a composition pattern that is distinctly different from coal fly ash.
Sanja Lazarević et al 2024 Res. Notes AAS 8 107
We report the Australian Square Kilometre Array Pathfinder discovery of a new Galactic supernova remnant (SNR) candidate G308.73+1.38, which we name Raspberry. This new SNR candidate has an angular size of 207 × 167, and we measure a total integrated flux of 407 ± 50 mJy. We estimate Raspberry's most likely diameter of 10–30 pc which would place it at a distance 3–5 kpc, in the near side of the Milky Way's Scutum–Centaurus Arm. We also find a Stokes-V point source close to the center of Raspberry with a ∼5σ significance. This point source may be the remaining compact source, a neutron star, or possibly a pulsar, formed during the initial supernova event.
Sangeeta Kumar and Maïssa Salama 2024 Res. Notes AAS 8 123
We present mass estimates and companion demographics on stellar multiples within 25 pc, using a survey of stars of all spectral types done by Robo-AO and supplemented by Gaia. The survey combined direct imaging by Robo-AO, a robotic adaptive optics instrument for 2 m class telescopes, to detect tight companions (<4'' separation) and with Gaia astrometry to detect wider co-moving companions. We estimated the masses for 267 companions using empirical relations and, for a subset of 97, dynamical mass estimates. We utilized previous mass–magnitude models using contrasts measured from Gaia and Robo-AO to estimate the mass and also used the orvara python package, a Markov Chain Monte Carlo orbit fitter using the companion astrometry and Hipparcos-Gaia proper motion accelerations, to estimate dynamical masses. We compare agreements and discrepancies in mass estimates from these two methods.
Carmen Choza et al 2024 Res. Notes AAS 8 37
We describe archival observations and analysis of the HD 110067 planetary system using the Green Bank Telescope (GBT) as part of the Breakthrough Listen search for technosignatures. The star hosts six sub-Neptune planets in resonant orbits, and we tune the drift rate range of our search to match the properties of the system derived by Luque et al. Our observations cover frequencies from 1 to 11.2 GHz, using the GBT's L, S, C, and X-band receivers, to an equivalent isotropic radiated power limit of ∼3 × 1012 W. No technosignatures were found, but this unusual system remains an interesting target for future technosignature searches.
Zhoujian Zhang 2024 Res. Notes AAS 8 114
AF Lep b is a rare directly imaged exoplanet with properties consistent with core-accretion evolution models. Using its precise dynamical mass and spectroscopically inferred bolometric luminosity alongside the Spiegel & Burrows evolution models, I determined an initial entropy >8.7 kB/baryon at 3σ and an age of 12 ± 4 Myr for AF Lep b. Comparing this planet's age to the isochrone age (24 ± 3 Myr) of its host association, the β Pictoris moving group (BPMG), suggests AF Lep b formed 12 ± 5 Myr later than its host star. Alternatively, the BPMG's updated kinematic age ( Myr) implies that AF Lep b formed 5 ± 5 Myr after its host star's formation, aligning more closely with protoplanetary disk dispersal timescales. The sensitivities of our findings to the planet's mass and luminosity are discussed. AF Lep b uniquely facilitates the constraints of its initial entropy and formation epoch, paving the way for similar insights into forthcoming exoplanet discoveries.
John E. Moores et al 2024 Res. Notes AAS 8 120
A complete understanding of methane in the atmosphere of Mars requires information on putative sources. Organic carbon derived from meteoritic sources, such as interplanetary dust particles (IDPs), over geologic time is the best-defined source of organic carbon on the surface of Mars. Here we examine two different mechanisms for degrading this material to produce methane (1) Ultraviolet photolysis and (2) thermal decomposition. Neither of these mechanisms can produce sufficient methane under realistic assumptions to explain observed methane at Gale Crater, suggesting that IDPs are not the primary source material producing methane on Mars.
Marcel Drechsler et al 2023 Res. Notes AAS 7 1
We report the discovery of a broad, 15 long filamentary [O iii] emission nebulosity some 12 southeast of the M31 nucleus. This nebulosity is not detected in Hα and has no obvious emission counterparts in X-ray, UV, optical, infrared, and radio surveys. To our knowledge, this emission feature has not been previously reported in the literature. We briefly discuss its possible origin.
Ai-Ying Zhou 2024 Res. Notes AAS 8 110
Gaia DR3 revealed 748,058 pulsating variable stars of mixed DSCT∣GDOR∣SXPHE types. This project undertakes a comprehensive examination to validate and distinguish these stars using Transiting Exoplanet Survey Satellite data. Aiming for reliable catalogs of bona fide δ Scuti and γ Doradus stars, I have validated 1715 δ Scuti stars, 1403 γ Doradus stars, and identified 260 eclipsing binaries, one RR Lyrae star, and 460+ rotating variables from an initial sample of 16,690 objects. Notably, 15 of the newfound eclipsing binaries harbor pulsating γ Doradus components.
Julie Moquin et al 2024 Res. Notes AAS 8 138
Magnetic reconnection is the underlying cause of stellar flares which are linked to regions of high magnetic activity, like star spots. To understand trends in stellar activity, we need to study how it is heightened by rapid rotation and deep convection in young low-mass stars. We analyze light curves of such stars observed by the Transiting Exoplanet Survey Satellite to investigate trends in flare timing with starspot modulation signals. Trends in flare properties and spot modulation can provide a means to "localize" which face of a star flares more frequently and better understand their association with active regions. We present an analysis of light curves from M and K dwarfs with no companions from five nearby and young moving groups spanning ages ∼20–150 Myr. We discuss a technique to analyze the distribution of flares and star spots and describe our results, which reveal a tentative correlation.
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Naga Varun Yelagandula 2024 Res. Notes AAS 8 142
This is to address the criticism expressed in the article (Goedbloed & Poedts 2024) referred to as GP[24] about the work (Yelagandula 2023) referred to as Y[23]. It will be shown that the dispersion relation obtained in Y[23] is indeed correct within the framework of the ZSER model discussed in Y[23] despite the correct criticism of GP[24] about the electrodynamic boundary condition.
Anthony Nuñez et al 2024 Res. Notes AAS 8 144
We identified discrepancies between the rotation measure (RM) catalogs by Clegg et al. and Minter & Spangler and their corresponding rows in the Van Eck et al. consolidated catalog. The discrepancies, in the case of Minter & Spangler, are caused by the improper coordinate conversions between J2000 and B1950 Equatorial coordinate systems used between the catalogs. The discrepancies associated with Clegg et al. are due to differences in the number of significant figures reported between the original and consolidated catalogs, which result in overlapping points in the consolidated catalog. These errors affect studies that rely on the accuracy of the coordinate data. After proper unit conversions, we found that coordinate values differed by up to 1° between the Minter & Spangler and consolidated catalogs. Employing a combination of manual data extraction and automated coordinate conversion tools, we corrected and updated those RM coordinate values to align with the standardized format used in the Van Eck et al. consolidated catalog.
A. J. P. Aparicio and J. M. Vaquero 2024 Res. Notes AAS 8 143
The Leonid meteor shower is renowned for its scientific and public interest. In a search for meteorological data from Portuguese stations, records on an observation of the Leonids in 1869 from the Lisbon Geophysical Observatory "Infante Dom Luiz" were found. Given their potential value, a digital version with metadata is provided in the present note (the recovered data are available on doi:10.5281/zenodo.11221019). The observation took place from 9 PM on 1869 November 13 to 6 AM on November 14, local time in Lisbon, with mostly clear skies and 4–5 observers covering completely the sky. They recorded 1980 meteors, noting Zodiacal Light visibility and detailing meteor counts every five minutes.
Dylan S. Caudill et al 2024 Res. Notes AAS 8 139
We present results of a study on the identification of M-dwarf flares using K2 and TESS data. Our sample includes objects observed simultaneously by these two missions, so that we can also compare how flares are identified in the two sets of data. We implement two open-source Python packages, Lightkurve and PyVAN, to work in unison to easily access the data and determine variability in the light curves of 39 M-dwarfs. We identified 13 flare detections in the TESS data while K2 did not provide any reliable detections of flares. We describe the shortcomings of the K2 data that prevented these flares from being identified.
Jarod A. DeSpain et al 2024 Res. Notes AAS 8 140
We report the discovery of cometary activity from minor planet 2011 UG104, which we classify as a Jupiter Family Comet (JFC). This discovery was aided by our Artificial Intelligence (AI) classification system: TailNet. JFC's, short-period comets with eccentric Jupiter-crossing orbits, originate from the Kuiper Belt and thus give us unique insight into the composition and distribution of volatiles in the outer solar system, past and present. Our AI assistant TailNet first classified 2011 UG104 as active, which was affirmed by Citizen Scientists on our NASA Partner Program Active Asteroids. Through further archival image searches our science team found evidence of activity on 2011 UG104 on three separate observations from 2021 February to 2021 April (818 < f < 950).