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Context. Small bodies in Earth-like orbits, the Arjunas, are good targets for scientific exploration and mining studies as they enable low-cost missions. The subset of such objects that experience recurrent temporarily captured flyby or orbiter events, also called mini-moon episodes, are among the best ranked in terms of accessibility. Only a handful of objects are known to have engaged in such a dynamical behavior. Finding and characterizing more of them may help to expand scientific and commercial research activities in space over the next few decades. Asteroid 2024 PT5 was found recently and belongs to this group of interesting objects. Aims. Here, we investigate the orbital context of 2024 PT5, and its spectral and rotational properties. Methods. We studied the short-term orbital evolution of 2024 PT5 using direct N-body simulations. We identified its spectral class from the visible reflectance spectrum and used photometric observations to derive its rotational properties. Observational data were obtained with the OSIRIS camera spectrograph at the 10.4 m Gran Telescopio Canarias and the Two-meter Twin Telescope. Results. Asteroid 2024 PT5 experiences recurrent co-orbital engagements and mini-moon events of the temporarily captured flyby type. Its visible spectrum is consistent with that of an Sv-type asteroid or perhaps lunar ejecta. Its rotational period could be less than or close to 1 h. Conclusions. The discovery of 2024 PT5 confirms that temporarily captured flybys are relatively frequent and involve objects larger than a few meters, suitable as accessible targets for scientific research activities and commercial mining ventures in space., Comment: 10 pages, 11 figures, 3 tables, 4 appendices, submitted to A&A Letters on 23 October 2024, currently under review (corrected label in Fig. 3 and caption of Fig. D.1)

Context. Natural interstellar objects do not form isolated in deep space, but escape their natal planetary systems. Early removal from their home star systems via close flybys with still-forming planets could be the dominant ejection mechanism. However, dynamically evolved planetary systems such as the Solar System may also be a significant source of natural interstellar objects. Aims. We studied the dynamical evolution of two unusual Solar System hyperbolic comets, C/1980 E1 (Bowell) and C/2024 L5 (ATLAS), to investigate the circumstances that led them to reach moderate Solar System excess hyperbolic speeds. Methods. We used N-body simulations and statistical analyses to explore the planetary encounters that led to the ejection of C/1980 E1 and C/2024 L5, and studied their pre- and post-encounter trajectories. Results. We confirm that C/1980 E1 reached its present path into interstellar space after an encounter with Jupiter at 0.23 au on December 9, 1980. C/2024 L5 was scattered out of the Solar System following a flyby to Saturn at 0.003 au on January 24, 2022. Integrations backward in time show that C/1980 E1 came from the inner Oort cloud but C/2024 L5 could be a former retrograde, inactive Centaur. The receding velocities of C/1980 E1 and C/2024 L5 when entering interstellar space will be 3.8 and 2.8 km/s, moving towards Aries and Triangulum, respectively. Conclusions. Our results for two comets ejected from the Solar System indicate that dynamically evolved planetary systems can be effective sources of interstellar objects and provide constraints on their velocity distribution., Comment: 8 pages, 8 figures, 2 tables. Accepted for publication in Astronomy and Astrophysics

Understanding the intricate quantum spin dynamics of radical pair reactions is crucial for unraveling the underlying nature of chemical processes across diverse scientific domains. In this work, we leverage Trotterization to map coherent radical pair spin dynamics onto a digital gate-based quantum simulation. Our results demonstrated agreement between the idealized noiseless quantum circuit simulation and established master equation approaches for homogeneous radical pair recombination, identifying approximately 15 Trotter steps to be sufficient for faithfully reproducing the coupled spin dynamics of a prototypical system. By utilizing this computational technique to study the dynamics of spin systems of biological relevance, our findings underscore the potential of digital quantum simulation (DQS) of complex radical pair reactions and builds the groundwork towards more utilitarian investigations into their intricate reaction dynamics. We further investigate the effect of realistic error models on our DQS approach, and provide an upper limit for the number of Trotter steps that can currently be applied in the absence of error mitigation techniques before losing simulation accuracy to deleterious noise effects., Comment: 10 pages, 9 figures

Context. Known Mars trojans could be primordial small bodies that have remained in their present-day orbits for the age of the Solar System. Their orbital distribution is strongly asymmetric; there are over a dozen objects at the L5 point and just one at L4, (121514) 1999 UJ7. Most L5 trojans appear to form a collision-induced asteroid cluster, known as the Eureka family. Asteroid 2023 FW14 was recently discovered and it has a robust orbit determination that may be consistent with a Mars trojan status. Aims. Our aim is determine the nature and dynamical properties of 2023 FW14. Methods. We carried out an observational study of 2023 FW14 to derive its spectral class using the OSIRIS camera spectrograph at the 10.4 m Gran Telescopio Canarias. We investigated its possible trojan resonance with Mars using direct N-body simulations. Results. The reflectance spectrum of 2023 FW14 is not compatible with the olivine-rich composition of the Eureka family; it also does not resemble the composition of the Moon, although (101429) 1998 VF31 does. The Eureka family and 101429 are at the L5 point. The spectrum of 2023 FW14 is also different from two out of the three spectra in the literature of the other known L4 trojan, 121514, which are of C-type. The visible spectrum of 2023 FW14 is consistent with that of an X-type asteroid, as is the third spectrum of 121514. Our calculations confirm that 2023 FW14 is the second known L4 Mars trojan although it is unlikely to be primordial; it may remain in its present-day tadpole path for several million years before transferring to a Mars-crossing orbit. It might be a fragment of 121514, but a capture scenario seems more likely. Conclusions. The discovery of 2023 FW14 suggests that regular Mars-crossing asteroids can be captured as temporary Mars trojans., Comment: 6 pages, 4 figures, 2 tables, 2 appendixes. Accepted for publication in Astronomy & Astrophysics, Letters to the Editor

This paper presents a global study of the class $\bf{Q}{\widehat{ES}}$ of all real quadratic polynomial differential systems possessing exactly one elemental infinite singular point and one triple infinite singular point, which is either an infinite nilpotent elliptic-saddle or a nilpotent saddle. This class can be divided into three different families, namely, $\bf{Q}{{\widehat{ES}(A)}}$ of phase portraits possessing three real finite singular points, $\bf{Q}{{\widehat{ES}(B)}}$ of phase portraits possessing one real and two complex finite singular points, and $\bf{Q}{{\widehat{ES}(C)}}$ of phase portraits possessing one real triple finite singular point. Here we provide the complete study of the geometry of these three families. Modulo the action of the affine group and time homotheties, families $\bf{Q}{{\widehat{ES}(A)}}$ and $\bf{Q}{{\widehat{ES}(B)}}$ are three-dimensional and family $\bf{Q}{{\widehat{ES}(C)}}$ is two-dimensional. We study the respective bifurcation diagrams of their closures with respect to specific normal forms, in subsets of real Euclidean spaces. The bifurcation diagram of family $\bf{Q}{{\widehat{ES}(A)}}$ (respectively, $\bf{Q}{{\widehat{ES}(B)}}$ and $\bf{Q}{{\widehat{ES}(C)}}$) yields 1274 (respectively, 89 and 14) subsets with 91 (respectively, 27 and 12) topologically distinct phase portraits for systems in the closure $\overline{\bf{Q}{{\widehat{ES}(A)}}}$ (respectively, $\overline{\bf{Q}{{\widehat{ES}(B)}}}$ and $\overline{\bf{Q}{{\widehat{ES}(C)}}}$) within the representatives of $\bf{Q}{{\widehat{ES}(A)}}$ (respectively, $\bf{Q}{{\widehat{ES}(B)}}$ and $\bf{Q}{{\widehat{ES}(C)}}$) given by a specific normal form., Comment: 112 pages. arXiv admin note: text overlap with arXiv:1303.2525

Context. The Arjuna asteroid belt is loosely defined as a diverse group of small asteroids that follow dynamically cold, Earth-like orbits. Most of them are not actively engaged in resonant, co-orbital behavior with Earth. Some of them experience temporary but recurrent horseshoe episodes. Objects in horseshoe paths tend to approach Earth at a low velocity, leading to captures as Earth's temporary satellites or mini-moons. Four such objects have already been identified: 1991 VG, 2006 RH120, 2020 CD3, and 2022 NX1. Here, we focus on 2023 FY3, a recent finding, the trajectory of which might have a co-orbital status and perhaps lead to temporary captures. Aims. We want to determine the physical properties of 2023 FY3 and explore its dynamical evolution. Methods. We carried out an observational study of 2023 FY3 using the OSIRIS camera spectrograph at the 10.4 m Gran Telescopio Canarias, to derive its spectral class, and time-series photometry obtained with QHY411M cameras and two units of the Two-meter Twin Telescope to investigate its rotational state. N-body simulations were also performed to examine its possible resonant behavior. Results. The visible reflectance spectrum of 2023 FY3 is consistent with that of an S-type asteroid; its light curve gives a rotation period of 9.3$\pm$0.6 min, with an amplitude of 0.48$\pm$0.13 mag. We confirm that 2023 FY3 roams the edge of Earth's co-orbital space. Conclusions. Arjuna 2023 FY3, an S-type asteroid and fast rotator, currently exhibits horseshoe-like resonant behavior and in the past experienced mini-moon engagements of the temporarily captured flyby type that may repeat in the future. The spectral type result further confirms that mini-moons are a diverse population in terms of surface composition., Comment: 9 pages, 8 figures, 2 tables, accepted for publication in Astronomy & Astrophysics. Updated after submission of production files

Although the present-day orbital distribution of minor bodies that go around the Sun between the orbit of Neptune and the Kuiper Cliff is well understood, past ~50 au from the Sun, our vision gets blurred as objects become fainter and fainter and their orbital periods span several centuries. Deep imaging using the largest telescopes can overcome the first issue but the problems derived from the second one are better addressed using data analysis techniques. Here, we make use of the heliocentric range and range-rate of the known Kuiper belt objects and their uncertainties to identify structures in orbital parameter space beyond the Kuiper Cliff. The distribution in heliocentric range there closely resembles that of the outer main asteroid belt with a gap at 70 au that may signal the existence of a dynamical analogue of the Jupiter family comets. Outliers in the distribution of mutual nodal distances suggest that a massive perturber is present beyond the heliopause., Comment: 6 pages, 7 figures, 1 table. Accepted for publication in Monthly Notices of the Royal Astronomical Society Letters

We present an observational and numerical study of the borderline hyperbolic comet C/2021 O3 (PANSTARRS) performed during its recent passage through the inner Solar system. Our observations were carried out at OASI and SOAR between 2021 October and 2022 January, and reveal a low level of activity relative to which was measured for other long-period comets. In addition, we observed a decrease in brightness as the comet got closer to the Sun. Our photometric data, obtained as C/2021 O3 approached perihelion on 2022 April 21, show that the comet was much less active than what is usually expected in the cases of long-period comets, with $Af\rho$ values more in line with those of short-period comets (specifically, the Jupiter Family Comets). On the other hand, the observed increase in the value of the spectral slope as the amount of dust in the coma decreased could indicate that the smaller dust particles were being dispersed from the coma by radiation pressure faster than they were injected by possible sublimation jets. The analysis of its orbital evolution suggests that C/2021 O3 could be a dynamically old comet, or perhaps a new one masquerading as a dynamically old comet, with a likely origin in the Solar system., Comment: 8 pages, 7 figures

Near-Earth asteroids (NEAs) that may evolve into impactors deserve detailed threat assessment studies. Early physical characterization of a would-be impactor may help in optimizing impact mitigation plans. We first detected NEA 2023~DZ$_{2}$ on 27--February--2023. After that, it was found to have a Minimum Orbit Intersection Distance (MOID) with Earth of 0.00005~au as well as an unusually high initial probability of becoming a near-term (in 2026) impactor. We aim to perform a rapid but consistent dynamical and physical characterization of 2023~DZ$_{2}$ as an example of a key response to mitigate the consequences of a potential impact. We use a multi-pronged approach, drawing from various methods (observational/computational) and techniques (spectroscopy/photometry from multiple instruments), and bringing the data together to perform a rapid and robust threat assessment.} The visible reflectance spectrum of 2023~DZ$_{2}$ is consistent with that of an X-type asteroid. Light curves of this object obtained on two different nights give a rotation period $P$=6.2743$\pm$0.0005 min with an amplitude $A$=0.57$\pm$0.14~mag. We confirm that although its MOID is among the smallest known, 2023~DZ$_{2}$ will not impact Earth in the foreseeable future as a result of secular near-resonant behaviour. Our investigation shows that coordinated observation and interpretation of disparate data provides a robust approach from discovery to threat assessment when a virtual impactor is identified. We prove that critical information can be obtained within a few days after the announcement of the potential impactor., Comment: Accepted for publication in Astronomy and Astrophysics, 15 pages

Context. The near-Earth orbital space is shared by natural objects and space debris that can be temporarily captured in geocentric orbits. Short-term natural satellites are often called mini-moons. Reflectance spectroscopy can determine the true nature of transient satellites because the spectral signatures of spacecraft materials and near-Earth asteroids (NEAs) are different. The recently discovered object 2022 NX1 follows an Earth-like orbit that turns it into a recurrent but ephemeral Earth companion. It has been suggested that 2022 NX1 could have an artificial origin or be lunar ejecta. Aims. Here, we use reflectance spectroscopy and N-body simulations to determine the nature and actual origin of 2022 NX1. Methods. We carried out an observational study of 2022 NX1, using the OSIRIS camera spectrograph at the 10.4 m Gran Telescopio Canarias, to derive its spectral class. N-body simulations were also performed to investigate how it reached NEA space. Results. The reflectance spectrum of 2022 NX1 is neither compatible with an artificial origin nor lunar ejecta; it is also different from the V type of the only other mini-moon with available spectroscopy, 2020 CD3. The visible spectrum of 2022 NX1 is consistent with that of a K-type asteroid, although it could also be classified as an Xk type. Considering typical values of the similar albedo of both K-type and Xk-type asteroids and its absolute magnitude, 2022 NX1 may have a size range of 5 to 15 m. We confirm that 2022 NX1 inhabits the rim of Earth's co-orbital space, the 1:1 mean-motion resonance, and experiences recurrent co-orbital engagements of the horseshoe-type and mini-moon events. Conclusions. The discovery of 2022 NX1 confirms that mini-moons can be larger than a few meters and also that they belong to a heterogeneous population in terms of surface composition., Comment: 8 pages, 7 figures, 2 tables, 3 appendixes. Accepted for publication in Astronomy and Astrophysics: Letters

Context. Most flybys in the Galactic disk are distant, beyond 10,000 AU, and have characteristic velocities of about 70 km/s. However, deep and fast encounters also take place, albeit with lower probability, particularly if one of the objects involved is a stellar remnant ejected during a supernova. WD 0810-353 might be a high velocity white dwarf, and it was recently identified as heading straight for the Solar System; however, the Gaia DR3 data that support its future deep and fast flyby are regarded as suspicious. Aims. Here, we reanalyze the Gaia DR3 data set associated with WD 0810-353 to confirm or reject the reality of its Solar System flyby and also to investigate its possible runaway status. Methods. We studied the evolution of WD 0810-353 forward in time using N-body simulations. We computed the distribution of distances of closest approach and their associated times of perihelion passage. We used a statistical analysis of the kinematics of this object to assess its possible hypervelocity. We compared its mean BP/RP spectrum to those of other well-studied white dwarfs. Results. We confirm that WD 0810-353 is headed for the Solar System, but the actual parameters of the encounter depend strongly on its radial velocity. The Gaia DR3 value of -373.74+/-8.18 km/s is strongly disfavored by our analyses. Its mean BP/RP spectrum suggests a value over ten times higher based on the position of its putative Halpha line. However, spectral matching using other white dwarfs with non-Gaia data indicate a radial velocity in the interval (-60, -70) km/s. Conclusions. These results confirm the future flyby of WD 0810-353 near the Solar System, although the relative velocity could be high enough or the minimum approach distance large enough to preclude any significant perturbation on the Oort cloud., Comment: 10 pages, 9 figures. Accepted for publication in Astronomy and Astrophysics

The region where the main asteroid belt is now located may have started empty, to become populated early in the history of the Solar system with material scattered outward by the terrestrial planets and inward by the giant planets. These dynamical pathways toward the main belt may still be active today. Here, we present results from a data mining experiment aimed at singling out present-day members of the main asteroid belt that may have reached the belt during the last few hundred years. Probable newcomers include 2003 BM1, 2007 RS62, 457175 (2008 GO98), 2010 BG18, 2010 JC58, 2010 JV52, 2010 KS6, 2010 LD74, 2010 OX38, 2011 QQ99, 2013 HT149, 2015 BH103, 2015 BU525, 2015 RO127, 2015 RS139, 2016 PC41, 2016 UU231, 2020 SA75, 2020 UO43, and 2021 UJ5, all of them in the outer belt. Some of these candidates may have been inserted in their current orbits after experiencing relatively recent close encounters with Jupiter. We also investigated the likely source regions of such new arrivals. Asteroid 2020 UO43, if real, has a non-negligible probability of having an origin in the Oort cloud or even interstellar space. Asteroid 2003 BM1 may have come from the neighborhood of Uranus. However, most newcomers -- including 457175, 2011 QQ99, and 2021 UJ5 -- might have had an origin in Centaur orbital space. The reliability of these findings is assessed within the context of the uncertainties of the available orbit determinations., Comment: 37 pages, 14 figures, 10 tables, 3 appendices. Accepted for publication in Celestial Mechanics and Dynamical Astronomy (bibtex part improved)

NASA's Transiting Exoplanet Survey Satellite (TESS) is performing a homogeneous survey of the sky from space in search of transiting exoplanets. The collected data are also being used for detecting passing Solar system objects, including 17 new outer Solar system body candidates located at geocentric distances in the range 80-200 au, that need follow-up observations with ground-based telescope resources for confirmation. Here, we present results of a proof-of-concept mini-survey aimed at recovering two of these candidates that was carried out with the 4.2 m William Herschel Telescope and a QHY600L CMOS camera mounted at its prime focus. For each candidate attempted, we surveyed a patch of sky of over one square degree around its expected coordinates in Sloan r'. The same location was revisited in five consecutive or nearly consecutive nights, reaching S/N > 4 at r' < 23 mag. We focused on the areas of sky around the circumpolar TESS candidates located at equatorial coordinates (07:00:15, +86:55:19), 202.8 au from Earth, and (06:39:47, +83:43:54) at 162.1 au, but we could not recover either of them at r' < 23 mag. Based on the detailed analysis of the acquired images, we confirm that either both candidates are much fainter than predicted or that they are false positives., Comment: 5 pages, 2 figures, 1 table. Accepted for publication in Monthly Notices of the Royal Astronomical Society Letters. Revised to match published version

Asymmetric debris discs have been found around stars other than the Sun; asymmetries are sometimes attributed to perturbations induced by unseen planets. The presence or absence of asymmetries in our own trans-Neptunian belt remains controversial. The study of sensitive tracers in a sample of objects relatively free from the perturbations exerted by the four known giant planets and most stellar flybys may put an end to this debate. The analysis of the distribution of the mutual nodal distances of the known extreme trans-Neptunian objects (ETNOs) that measure how close two orbits may get to each other could be such a game changer. Here, we use a sample of 51 ETNOs together with random shufflings of this sample and two unbiased scattered-disc orbital models to confirm a statistically significant (62 sigma) asymmetry between the shortest mutual ascending and descending nodal distances as well as the existence of multiple highly improbably (p < 0.0002) correlated pairs of orbits with mutual nodal distances as low as 0.2 au at 152 au from the Solar system's barycentre or 1.3 au at 339 au. We conclude that these findings fit best with the notion that trans-Plutonian planets exist., Comment: 5 pages, 3 figures, 1 table. Accepted for publication in Monthly Notices of the Royal Astronomical Society Letters. Revised to match published version

Context. Saturn has an excess of irregular moons. This is thought to be the result of past collisional events. Debris produced during such episodes in the neighborhood of a host planet can evolve into co-orbitals trapped in quasi-satellite and/or horseshoe resonant states. A recently announced centaur, 2013 VZ70, follows an orbit that could be compatible with those of prograde Saturn's co-orbitals. Aims. We perform an exploration of the short-term dynamical evolution of 2013 VZ70 to confirm or reject a co-orbital relationship with Saturn. A possible connection with Saturn's irregular moon population is also investigated. Methods. We studied the evolution of 2013 VZ70 backward and forward in time using N-body simulations, factoring uncertainties into the calculations. We computed the distribution of mutual nodal distances between this centaur and a sample of moons. Results. We confirm that 2013 VZ70 is currently trapped in a horseshoe resonant state with respect to Saturn but that it is a transient co-orbital. We also find that 2013 VZ70 may become a quasi-satellite of Saturn in the future and that it may experience brief periods of capture as a temporary irregular moon. This centaur might also pass relatively close to known irregular moons of Saturn. Conclusions. Although an origin in trans-Neptunian space is possible, the hostile resonant environment characteristic of Saturn's neighborhood favors a scenario of in situ formation via impact, fragmentation, or tidal disruption as 2013 VZ70 can experience encounters with Saturn at very low relative velocity. An analysis of its orbit within the context of those of the moons of Saturn suggests that 2013 VZ70 could be related to the Inuit group. Also, the mutual nodal distances of 2013 VZ70 and the moons Fornjot and Thrymr are below the first percentile of the distribution., Comment: 10 pages, 8 figures, 5 tables, 1 appendix. Accepted for publication in Astronomy and Astrophysics. Abstract abridged. After language edition

Quantum walks are dynamic systems with a wide range of applications in quantum computation and quantum simulation of analog systems, therefore it is of common interest to understand what changes from an isolated process to one embedded in an environment. In the present work, we analyze the decoherence in a three-state uni-dimensional quantum walk. The approaches taken into consideration to account for the environment effects are phase and amplitude damping Kraus operators, unitary noise on the coin space, and broken links.

It is still an open question how the Solar system is structured beyond 100 au from the Sun. Our understanding of this vast region remains very limited and only recently we have become aware of the existence there of a group of enigmatic bodies known as the extreme trans-Neptunian objects (ETNOs) that have large orbits with perihelia beyond the orbit of Neptune. Four ETNOs -- Sedna, Leleakuhonua, 2012 VP113, and 2013 SY99 -- have perihelia beyond 50 au. The study of the ETNOs may provide much needed information on how this remote region is organized. Here, we apply machine-learning techniques to the sample of 40 known ETNOs to identify statistically significant clusters that may signal the presence of true dynamical groupings and study the distribution of the mutual nodal distances of the known ETNOs that measure how close two orbits can get to each other. Machine-learning techniques show that the known ETNOs may belong to four different populations. Results from the analysis of the distribution of nodal distances show that 41 per cent of the known ETNOs have at least one mutual nodal distance smaller than 1.45 au (1st percentile of the distribution), perhaps hinting at past interactions. In this context, the peculiar pair of ETNOs made of 505478 (2013 UT15) and 2016 SG58 has a mutual ascending nodal distance of 1.35 au at 339 au from the Sun. In addition, the known ETNOs exhibit a highly statistically significant asymmetry between the distributions of object pairs with small ascending and descending nodal distances that might be indicative of a response to external perturbations., Comment: 17 pages, 19 figures, 1 table, 3 appendices. Accepted for publication in Monthly Notices of the Royal Astronomical Society

Context. Centaurs go around the Sun between the orbits of Jupiter and Neptune. Only a fraction of the known centaurs have been found to display comet-like features. Comet 29P/Schwassmann-Wachmann 1 is the most remarkable active centaur. It orbits the Sun just beyond Jupiter in a nearly circular path. Only a handful of known objects follow similar trajectories. Aims. We present photometric observations of 2020 MK4, a recently found centaur with an orbit not too different from that of 29P, and we perform a preliminary exploration of its dynamical evolution. Methods. We analyzed broadband Cousins R and Sloan g', r', and i' images of 2020 MK4 acquired with the Jacobus Kapteyn Telescope and the IAC80 telescope to search for cometary-like activity, and to derive its surface colors and size. Its orbital evolution was studied using direct N-body simulations. Results. Centaur 2020 MK4 is neutral-gray in color and has a faint, compact cometary-like coma. The values of its color indexes, (g'-r')=0.42+/-0.04 and (r'-i')=0.17+/-0.04, are similar to the solar ones. A lower limit for the absolute magnitude of the nucleus is Hg=11.30+/-0.03 mag which, for an albedo in the range of 0.1-0.04, gives an upper limit for its size in the interval (23, 37) km. Its orbital evolution is very chaotic and 2020 MK4 may be ejected from the Solar System during the next 200 kyr. Comet 29P experienced relatively close flybys with 2020 MK4 in the past, sometimes when they were temporary Jovian satellites. Conclusions. We confirm the presence of a coma of material around a central nucleus. Its surface colors place this centaur among the most extreme members of the gray group. Although its past, present, and future dynamical evolution resembles that of 29P, more data are required to confirm or reject a possible connection between the two objects and perhaps others., Comment: 15 pages, 15 figures, 6 tables, 3 appendixes. Accepted for publication in Astronomy and Astrophysics. Abstract abridged. After A&A language editing

Jupiter co-orbital comets have orbits that are not long-term stable. They may experience flybys with Jupiter close enough to trigger tidal disruptions like the one suffered by comet Shoemaker-Levy 9. Our aim was to study the activity and dynamical evolution of the Jupiter co-orbital comet P/2019 LD2 (ATLAS). We present results of an observational study carried out with the 10.4m Gran Telescopio Canarias (GTC) that includes image analyses using a MC dust tail fitting code to characterize its activity, and spectroscopic studies to search for gas emission. We also present N-body simulations to explore its orbital evolution. Images of LD2 obtained on 2020 May 16 show a conspicuous coma and tail. The spectrum does not exhibit any evidence of CN, C2, or C3 emission. The comet brightness in a 2.6 arcsec aperture is r'=19.34+/-0.02 mag, with colors (g'-r')=0.78+/-0.03, (r'-i')=0.31+/-0.03, and (i'-z')=0.26+/-0.03. The temporal dependence of the dust loss rate can be parameterized by a Gaussian having a FWHM of 350 days and a maximum of 60 kg/s reached on 2019 August 15. The total dust loss rate is 1.9e09 kg. LD2 is now following what looks like a short arc of a quasi-satellite cycle that started in 2017 and will end in 2028. On 2063 January 23, it will experience a very close encounter with Jupiter at 0.016 au. Its probability of escaping the solar system during the next 0.5 Myr is 0.53+/-0.03. LD2 is a kilometer-sized object, in the size range of the Jupiter-family comets, with a typical comet-like activity likely linked to sublimation of crystalline water ice and clathrates. Its origin is still an open question. We report a probability of LD2 having been captured from interstellar space during the last 0.5 Myr of 0.49+/-0.02, 0.67+/-0.06 during the last 1 Myr, 0.83+/-0.06 over 3 Myr, and 0.91+/-0.09 during the last 5 Myr., Comment: To be published in Astronomy & Astrophysics. 10 pages, 8 figures

Context. The paths followed by the known extreme trans-Neptunian objects (ETNOs) effectively avoid direct gravitational perturbations from the four giant planets, yet their orbital eccentricities are in the range between 0.69-0.97. Solar system dynamics studies show that such high values of the eccentricity can be produced via close encounters or secular perturbations. In both cases, the presence of yet-to-be-discovered trans-Plutonian planets is required. Aims. If the high eccentricities of the known ETNOs are the result of relatively recent close encounters with putative planets, the mutual nodal distances of sizeable groups of ETNOs with their assumed perturber may still be small enough to be identifiable geometrically. In order to confirm or reject this possibility, we used Monte Carlo random search techniques. Methods. Two arbitrary orbits may lead to close encounters when their mutual nodal distance is sufficiently small. We generated billions of random planetary orbits with parameters within the relevant ranges and computed the mutual nodal distances with a set of randomly generated orbits with parameters consistent with those of the known ETNOs and their uncertainties. We monitored which planetary orbits had the maximum number of potential close encounters with synthetic ETNOs and we studied the resulting distributions. Results. We provide narrow ranges for the orbital parameters of putative planets that may have experienced orbit-changing encounters with known ETNOs. Conclusions. Our calculations suggest that more than one perturber is required if scattering is the main source of orbital modification for the known ETNOs. Perturbers might not be located farther than 600 AU and they have to follow moderately eccentric and inclined orbits to be capable of experiencing close encounters with multiple known ETNOs., Comment: 12 pages, 5 figures, 3 tables, 5 appendixes. Accepted for publication in Astronomy and Astrophysics Letters. Abstract abridged

During the image acquisition process, noise is usually added to the data mainly due to physical limitations of the acquisition sensor, and also regarding imprecisions during the data transmission and manipulation. In that sense, the resultant image needs to be processed to attenuate its noise without losing details. Non-learning-based strategies such as filter-based and noise prior modeling have been adopted to solve the image denoising problem. Nowadays, learning-based denoising techniques showed to be much more effective and flexible approaches, such as Residual Convolutional Neural Networks. Here, we propose a new learning-based non-blind denoising technique named Attention Residual Convolutional Neural Network (ARCNN), and its extension to blind denoising named Flexible Attention Residual Convolutional Neural Network (FARCNN). The proposed methods try to learn the underlying noise expectation using an Attention-Residual mechanism. Experiments on public datasets corrupted by different levels of Gaussian and Poisson noise support the effectiveness of the proposed approaches against some state-of-the-art image denoising methods. ARCNN achieved an overall average PSNR results of around 0.44dB and 0.96dB for Gaussian and Poisson denoising, respectively FARCNN presented very consistent results, even with slightly worsen performance compared to ARCNN., Comment: Published in: 2020 33rd SIBGRAPI Conference on Graphics, Patterns and Images (SIBGRAPI)

Both Earth and Mars host populations of co-orbital minor bodies. A large number of present-day Mars co-orbitals is probably associated with the fission of the parent body of Mars Trojan 5261 Eureka (1990 MB) during a rotation-induced YORP break-up event. Here, we use the statistical distributions of the Tisserand parameter and the relative mean longitude of Mars co-orbitals with eccentricity below 0.2 to estimate the importance of rotation-induced Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) break-up events in Martian co-orbital space. Machine-learning techniques (k-means++ and agglomerative hierarchical clustering algorithms) are applied to assess our findings. Our statistical analysis identified three new Mars Trojans: 2009 SE, 2018 EC4 and 2018 FC4. Two of them, 2018 EC4 and 2018 FC4, are probably linked to Eureka but we argue that 2009 SE may have been captured, so it is not related to Eureka. We also suggest that 2020 VT1, a recent discovery, is a transient Martian co-orbital of the horseshoe type. When applied to Earth co-orbital candidates with eccentricity below 0.2, our approach led us to identify some clustering, perhaps linked to fission events. The cluster with most members could be associated with Earth quasi-satellite 469219 Kamo`oalewa (2016 HO3) that is a fast rotator. Our statistical analysis identified two new Earth co-orbitals: 2020 PN1, that follows a horseshoe path, and 2020 PP1, a quasi-satellite that is dynamically similar to Kamo`oalewa. For both Mars and Earth co-orbitals, we found pairs of objects whose values of the Tisserand parameter differ by very small amounts, perhaps hinting at recent disruption events. Clustering algorithms and numerical simulations both suggest that 2020 KZ2 and Kamo`oalewa could be related., Comment: 19 pages, 22 figures, 16 tables, 1 appendix. Includes minor style-related changes to match the version published by Monthly Notices of the Royal Astronomical Society

Despite the coined quantum walk being a closed quantum system under a unitary evolution, its Hilbert space can be divided in two sub-spaces, which makes it possible for one to analyze one of the subsystems (the coin or the walker) as an open system in contact with a reservoir. In the present work we calculate the asymptotic reduced density matrix of the coin space of the three-state quantum walk in an infinite line, and use that result to analyze the entanglement between the chirality, and position space. We calculate the von Neumann entropy and the entanglement temperature per mean energy of the system in the asymptotic limit.