The Javalambre VARiability Survey (J-VAR) is a photometric survey that is being carried out with the 0.8m Javalambre Auxiliary Survey Telescope, located at the Observatorio Astrofisico de Javalambre (Teruel, Spain), using a subset of seven filters from J-PLUS, covering the wavelength range 0.39-0.88 mu m. The scientific objectives of J-VAR are three: characterization of variable stars, detection of supernovae, and detection and characterization of small Solar system objects (SSOs). The main goal of this work is to present the first catalogue of SSOs compiled from the first data release (DR1) of the J-VAR survey, consisting of observations for 101 fields (visited at least 11 times each). We used the ssos pipeline to analyse each epoch (which usually consists of 21 images, except for the high frequency cases) for all the fields in the J-VAR DR1, retrieving the SSOs detected in the survey images. We analysed more than 30 000 images, recovering 131 966 detections, corresponding to a total of 6579 individual Solar system small bodies, similar to 95 per cent of which are located in the Main Belt. We present here two catalogues: individual detections and combined magnitudes. In addition, we show some preliminary results: analysis of colour-colour plots and comparison with the known spectral properties of asteroids, photospectra for some objects observed in all seven filters, and we present a method for constructing partial light curves for objects detected in the high frequency epochs. Finally, we discuss the survey's potential to discover unknown Solar system bodies.

Context. Phase curves of small bodies are useful tools for obtaining their absolute magnitudes and phase coefficients. The absolute magnitude relates to the object's apparent brightness, while the phase coefficient relates to how the light interacts with the surface. Data from multiwavelength photometric surveys, which usually serendipitously observe small bodies, are becoming the cornerstone of large statistical studies of the Solar System. Nevertheless, to our knowledge, all studies have been carried out in visible wavelengths. Aims. We aim to provide the first catalog of absolute magnitudes in near-infrared filters (Y, J, H, and K). We study the applicability of a nonlinear model to these data and compare it with a simple linear model. Methods. We computed the absolute magnitudes using two photometric models: the HG(12)(& lowast;) and the linear model. We employed a combination of Bayesian inference and Monte Carlo sampling to calculate the probability distributions of the absolute magnitudes and their corresponding phase coefficients. We used the combination of four near-infrared photometric catalogs to create our input database. Results. We produced the first catalog of near-infrared magnitudes. We obtained absolute magnitudes for over 10 000 objects (with at least one absolute magnitude measured), with about 180 objects having four absolute magnitudes. We confirm that a linear model that fits the phase curves produces accurate results. Since linear behavior describes the curves well, fitting to a restricted phase angle range (in particular, larger than 9.5 deg) does not substantially affect the results. Finally, we also detect a phase-coloring effect in the near-infrared, as has been observed in visible wavelengths for asteroids and trans-Neptunian objects.

The near-Earth asteroid (98943) Torifune, previously designated 2001 CC21, is the flyby target of the Hayabusa2 extended mission, nicknamed Hayabusa2# (Small Hazardous Asteroid Reconnaissance Probe (SHARP)). The ground-based telescope observations offer a key science input for the mission's scientific investigation. During 2022-2024, this asteroid was at visible apparent magnitudes brighter than 18.5, allowing for a detailed characterization using ground-based telescope observations. We determined its rotation period P = 5.021516 +/- 0.000106 hr and its absolute magnitude H = 18.78 +/- 0.14. The large number of light curves allows us to estimate its axis ratio, its convex shape, and its pole orientation, lambda = 301(degrees) +/- 35(degrees), beta=89(-6)(+1 degrees), and = 5(degrees) +/- 3(degrees), respectively, which indicate a prograde rotation. We report the semiaxis of the equivalent ellipsoid, a = 0.42(0.06)(+0.08) km, b = 0.16(0.04)(+0.05) km, and c = 0.17 +/- 0.03 km. Consequently, the volume-equivalent diameter is D-eq = 0.44 +/- 0.06 km. Using observations conducted simultaneously with four broadband filters, we determined (g - r) = 0.663 +/- 0.022 mag, (r - i) = 0.177 +/- 0.012 mag, and (i - z(s)) = -0.061 +/- 0.032 mag. Additionally, we found that Torifune exhibits no detectable large-scale heterogeneity. We classified the object using a high signal-to-noise ratio spectrum (over the visible and near-infrared region) as Sq-type in the Bus-DeMeo taxonomy. We estimate a mineralogy similar to LL/L ordinary chondrites, with an ol/(ol+px) = 0.60, a Fa content of 28.5 mol%, and a Fs content of 23.4 mol%. The spectral data indicate a surface affected by moderate space weathering effects.

The near-Earth asteroid (98943) Torifune, previously designated 2001 CC_21, is the flyby target of the Hayabusa2 extended mission, nicknamed Hayabusa2# (SHARP: Small Hazardous Asteroid Reconnaissance Probe). The ground-based telescope observations offer a key science input for the mission's scientific investigation. During 2022 - 2024 this asteroid was at visible apparent magnitudes brighter than 18.5, allowing for a detailed characterization using ground-based telescope observations. We determined its rotation period P = 5.021516±0.000106 h and its absolute magnitude H = 18.78 ± 0.14 and. The large number of lightcurves allows to estimate its axes ratio, its convex shape and its pole orientation λ = 301^∘± 35^∘, β = 89^+1_-6^∘ and ϵ = 5^∘± 3^∘ which indicate a prograde rotation. We report the semi-axis of the equivalent ellipsoid, a = 0.42^+0.08_0.06 km, b = 0.16^+0.05_0.04 km, and c = 0.17±0.03 km. Consequently, the volume equivalent diameter is D_eq = 0.44 ± 0.06 km . Using observations conducted simultaneously with four broadband filters, we determined (g-r) = 0.663 ± 0.022 mag, (r-i) = 0.177 ± 0.012 mag, and (i-z_s) = -0.061 ± 0.032 mag. Additionally, we found that Torifune exhibits no detectable large-scale heterogeneity. We classified the object using a high signal-to-noise ratio spectrum (over the visible and near-infrared region) as Sq-type in the Bus-DeMeo taxonomy. We estimate a mineralogy similar to LL/L ordinary chondrites, with an ol/(ol+px) = 0.60, a Fa content of 28.5 mol%, and a Fs content of 23.4 mol%. The spectral data indicate a surface affected by moderate space weathering effects.

The Javalambre VARiability Survey (J-VAR) is a photometric survey that is being carried out with the 0.8m Javalambre Auxiliary Survey Telescope (JAST80), located at the Observatorio Astronómico de Javalambre (OAJ, in Teruel). J-VAR is the time-domain extension of the Javalambre-Photometric Local Universe Survey, J-PLUS, carried out in the same telescope. J-VAR uses a sub-set of seven filters from the J-PLUS set covering the range from 0.395 up to 0.861 microns, including the g,r,i filters from the SDSS set. The main concept of J-VAR is to explore the time-domain capabilities offered by the JAST80, and its strategy is as follows: each field is observed three times, with dithering, in all seven filters, and is revisited a total of ten times whenever the weather conditions allow J-VAR to be executed. This observational strategy, favouring the detection of transient phenomena, is also well-suited for the detection of small bodies (SBs) of the Solar System.Within the 101 fields included in J-VAR Data Release 1 we have recovered more than 130,000 individual detections (an asteroid was detected in one image). These correspond to more than 8,600 objects (a total of 6,572 individual asteroids). The detection of the SBs is done using the SOSS pipeline (Mahlke et al. 2019). Here, we present the first catalog of small bodies of the Solar System observed with J-VAR: we show the calibration method, we present some statistics on the data, and we outline the next steps for future iterations of the catalog.

Past analyses of spectral properties of the inner -belt primitive families in visible wavelengths have uncovered the possible existence of two compositional groups: Erigone-like (highly hydrated) and Polana-like (nearly anhydrous) (Morate et al., 2018). We explore the spectral properties of the Erigone asteroid family in the nearinfrared to probe this hypothesis. To get a closer look at the family, we observed 25 family members over an observational campaign from 2014b-2016b utilizing the NASA Infrared Telescope Facility and the Telescopio Nazionale Galileo. The objects are analyzed by determining the taxonomic classification and spectral gradient values. The spectral gradient results display a compact, primarily reddened range of values in agreement with the primitive types identified through taxonomic classification. Erigone is found to be composed of C- and X -complex types as well as various end -members (L- and T -types). All objects classified as C -complex belong to either Ch- or Cgh-types, types that exhibit hydration in the visible region, aligning with the results of the Erigone family being highly hydrated. We find that trends pointing at the existence of Erigone-like and Polana-like groups in the visible do not appear in the analysis of the near -infrared data. An additional analysis of the Lucy mission target, (52246) Donaldjohanson, was performed and determined to be a probable true member of the Erigone family. Understanding the distribution and extent of hydration in the main asteroid belt contributes to understanding the solar system's evolution. It provides insight into the implications of primitive bodies being a possible source of Earth's water.

Asteroids are the remnant blocks of the early stages of the formation of our Solar System. In particular, those classified as “primitive” are believed to contain the most pristine and almost unprocessed materials (water-bearing minerals, carbon compounds, and organics), and therefore they provide unique information on the formation and evolution of our planetary system, including how water appeared on Earth. Among these objects, primitive near-Earth asteroids (NEAs) are of particular interest. Due to their proximity they are impact hazards to Earth, but they are also the ideal targets for space missions. That is the case of primitive NEAs (101955) Bennu and (162173) Ryugu, primary targets of NASA’s OSIRIS-REx and JAXA’s Hayabusa 2 sample return missions, respectively, currently on their way to encounter the two asteroids. The main asteroid belt, located between the orbits of Mars and Jupiter (2.1-5.2 AU), and in particular collisional families, are currently considered the principal source of NEAs (Bottke et al. 2002; Bottke et al. 2005). In the case of the two primitive NEAs mentioned above, several studies have shown that the most likely source is the Polana collisional family (Campins et al. 2010, 2013), a primitive family located in the inner belt. Other large primitive families in that region are Erigone, Sulamitis, and Clarissa. Smaller primitives families like Klio, Chaldaea, Svea and Chimaera can also be found in the same region (Nesvorny et al. 2015).With the main objective of supporting the science return of OSIRIS-Rex and Hayabusa 2, in 2010 our group started a coordinated effort to characterize the surface composition of primitive asteroids not only in the collisional families of the inner belt, but in the central and outer belt: our PRIMitive Asteroids Spectroscopic Survey (PRIMASS) includes both visible and near-infrared spectra. Up to now, in the frame of PRIMASS, our group has studied several primitive families wihtin the inner main belt: the Polana-Eulalia complex (de León et al. 2016; Pinilla-Alonso et al. 2016), Erigone (Morate et al. 2016), Sulamitis and Clarissa (Morate et al. 2018a), and Klio, Chaldaea, Chimaera, and Svea (Morate et al. 2019). One interesting result was that Erigone. Sulamitis, Klio, Chaldaea, and Chimaera, presented different percentages of asteroids with an absorption band centered at 0.7μm and associated to hydrated silicates, while the Polana, Clarissa, and Svea families showed no signs of hydration. This result remarks the need for spectral characterization as even the families classified all a priori as primitive can show compositional differences.Continuing with our PRIMASS survey, we started the characterization of the families in the central part of the belt (2.50-2.82 AU). According to Nesvorný et al. (2015), there are at least 5 primitive families in that region, and for the present work we have focused on three of them: Padua, Nemesis, and Hoffmeister. As it can be seen in Fig. 1A, they overlap in the (a, i) orbital parameter space, and two of them overlap even in the (a, e) space. This might be indicative of a common origin and interestingly, the three families show a similar age. They also overlap in the (a, H) space (Fig. 1B), which make them an ideal case to see if we can discriminate between members from each family using spectroscopy. According to the taxonomical classification of their largest member using visible spectra, Hoffmeister is classified as a CF type family (neutral to blue spectral slope), Nemesis is a C-type family (neutral slope), and Padua is an X-type (redder slope). The distribution of WISE albedos (Mainzer et al. 2011) of Hoffmeister is rather different from what is seen on Nemesis and Padua (Fig. 1C), also indicative of different composition. Only spectra will help to compositionally characterize these families and to search for the presence of the 0.7 μm absorption band associated to hydration. This will allow us to compare the level of hydration in families from the inner to the outer belt (De Prá et al. 2017) and map the water inventory of the asteroid belt to constrain evolutionary models.Figure 1: A) Distribution of the members of the three primitive collisional families in semimajor axis (a) vs. Eccentricity (top panel) and sine of inclination (bottom panel). The three families clearly overlap in the (a,i) space. B) Distribution of the three families in the absolute magnitude (H) - a space. There are clear overlapping regions where we can test if members of each family can be identified using spectra. C) Distribution of the albedos measured by WISE for the members of the three families.In order to study these three families, we obtained visible spectra for a total of 124 asteroids (44 within the Nemesis and Hoffmeister families, and 36 within the Padua family) using the OSIRIS spectrograph at the 10.4m GTC, located at the Observatorio Del Roque de Los Muchachos (La Palma, Spain). In this work, we will present the first spectroscopic study of the Nemesis, Hoffmeister, and Padua families, and we will compare the results with those obtained for the families located in the inner main belt.

The near-Earth asteroids (NEAs) represent excellent scientific opportunities to study the dynamical and physical properties of small bodies of the Solar System. Moreover, the celestial bodies with sizes lower than one km can be studied using a variety of techniques, thanks to the fact that they come close to Earth orbit.We report the preliminary results of an ongoing observational program for obtaining the visible color indexes of NEAs. Our survey use the MuSCAT2 instrument [1] mounted on the 1.52 m Telescopio Carlos Sánchez located at Teide Observatory (Canary Islands, Spain). The setup allows us to obtain simultaneous imaging in the g (400–550nm), r (550–700 nm), i( 700–820 nm), and zs (820–920nm) bands. The visible colors have proven to be efficient to broadly differentiate between the major compositional groups [2]. Thus, by using MuSCAT2 instrument we can obtain the spectro-photometric classification for a large number of NEOs. The simultaneous imaging allows to study the relation between the rotational properties and the taxonomic type. It can also reveal possible heterogeneous compositions of the observed targets.Fig. 1 The absolute magnitude distribution of NEAs observed with TCS – MuSCAT2 instrumentThe program started in March 2018 with one or two observing nights allocated on every month. A total of 267 spectro-photometric observational sets were collected. They correspond to 198 NEAs with the absolute magnitudes distributed in the range of 12 -24 mag (Fig. 1). Our schedule gave priority to the targets observed by radar, to potentially hazardous asteroids and to those suitable for a space mission. We also considered the newly discovered objects. Most of these are very small objects (in general smaller than 300m) and the opportunities to study them are rare.Fig. 2 The color-color diagrams of objects with known visible colors and spectral classification, used as training sets in the K-Nearest Neighbors algorithm.We used the Photometry Pipeline (PP) software [3] and several Python scripts for reducing the data. We applied the K-Nearest Neighbors (KNN) algorithm to obtain the spectro-photometric classification. For the training set we used the 86 asteroids for which spectral data is also available and the taxonomic type is known ([4], [5]). We grouped the taxonomic classes in seven groups, namely Q-type and S-complex (similar to silicate asteroids), V-type (specific to basaltic objects), A-type (an olivine-dominated composition), B/C-complex (similar to carbonaceous meteorites), X-complex and D-type (reddish surfaces – possible cometary nature). The color-color diagrams of this sample used for training is shown in Fig. 2. The classification results are shown in Fig. 3.Fig 3. The taxonomic distribution of the observed sampleBy assigning a probability for each classification we quantified the effect of color errors. This was derived by applying a Monte-Carlo approach. We generated 10000 simulated values for each of the colors of an asteroid by using a normal distribution where the mean is the observed color and the standard deviation is the color error. The KNN classifier was applied for each of these colors. The reported class is the one predicted in most cases and the probability is the occurrence rate.AcknowledgmentsMP, JL, JdL, and DM acknowledge support from the ESA P3NEOI and NEOROCKS projects. The work of MP, GNS, and RMG was supported by a grant of the Romanian National Authority for Scientific Research – UEFISCDI, project number PN-III-P1-1.1-TE-2019-1504. This work was developed in the framework of EURONEAR collaboration.References[1] Narita, Norio et al.; Journal of Astronomical Telescopes, Instruments, and Systems, Volume 5, id. 015001 (2019).[2] Parker, A.; Icarus, Volume 198, Issue 1, p. 138-155 (2008).[3] Mommert, Michael; Astronomy and Computing, Volume 18, p. 47-53 (2017).[4] Popescu, M et al.; Astronomy & Astrophysics, Volume 627, id.A124, 21 pp (2019).[5] Binzel R. P., et al. 2019, Icarus, 324, 4

In the framework of the Visible NEAs Observations Survey (ViNOS) that uses several telescopes at the Canary Islands observatories since 2018, we observed two super fast rotator NEAs, 2021 NY1 and 2022 AB. We obtained photometry and spectrophotometry of both targets and visible spectroscopy of 2022 AB. Light curves of 2021 NY1 obtained in 4 different nights between Sept. 30 and Oct. 16, 2021 return a rotation period P = 13.3449 ± 0.0013 minutes and a light curve amplitude A = 1.00 mag. We found that 2021 NY1 is a very elongated super fast rotator with an axis ratio a/b ≥ 3.6. We also report colours (g − r) = 0.664 ± 0.013, (r − i) = 0.186 ± 0.013, and (i − zs) = −0.117 ± 0.012 mag. These are compatible with an S-type asteroid. The light curves of 2022 AB obtained on Jan. 5 and Jan. 8, 2021 show a rotation period P = 3.0304 ± 0.0008 minutes, with amplitudes A = 0.52 and A = 0.54 mag. 2022 AB is also an elongated object with axis ratio a/b ≥ 1.6. The obtained colours are (g − r) = 0.400 ± 0.017, (r − i) = 0.133 ± 0.017, and (i − zs) = 0.093 ± 0.016. These colours are similar to those of the X-types, but with an unusually high (g − r) value. Spectra obtained on Jan. 12 and Jan. 14, 2022, are consistent with the reported colours. The spectral upturn over the 0.4 - 0.6 $\mu \mathrm{m}$ region of 2022 AB does not fit with any known asteroid taxonomical class or meteorite spectrum, confirming its unusual surface properties.

Introduction The asteroid (4660) Nereus is considered one of the most accessible targets for a rendez-vous space mission. It was proposed as a possible target for the NASA Near-Earth Asteroid Rendezvous (NEAR) and for JAXA Hayabusa spacecraft. The lightcurve analysis and the radar shape modeling revealed a long rotational period of ≅ 15.16 ± 0.04 h [1, 2]. The radar [2] and thermal [3] observations report optical albedo values of 0.54 (-0.09, +0.03) and 0.55 ± 0.17 respectively. Coupled with the featureless spectrum [4], Nereus is classified as an E-type object in the Tholen taxonomy. This class has been associated with enstatite achondrite meteorites. During the fall of 2020 and the beginning of 2021, (4660) Nereus made a favorable apparition for observations with ground-based telescopes. It had an apparent magnitude brighter than 18.5 V mag. for about 7 months. The peak brightness was 12.9 on the night of December 7. In this context, we performed an extended characterization using various telescopes. Thus, we report light-curves, spectro-photometric data and spectral observations for Nereus. Observations We obtain the light curve of (4660) Nereus using the T025-BD4SB, a 0.25 m aperture telescope located at the Bucharest Astronomical Institute , Romania. About 65 hours of observations were obtained during 8 nights spread between October 27 and November 25, 2021. These data were acquired using the QHY294M CMOS camera. The color indices in the visible region were determined using the MuSCAT2 instrument of the 1.52 m Telescopio Carlos Sanchez (TCS) located in Tenerife, Spain. This instrument allows simultaneous images with the broad band filters g (0.40 - 0.55 μm), r (0.550 - 0.70 μm), i (0.70 - 0.82 μm), and zs (0.82 - 0.92 μm). As such, we gathered 15.2 hours of data during six nights of observations spread over October 02, 2021 until April 02, 2022. Additional photometry data was obtained using the 2.54 m Isaac Newton Telescope (La Palma, Spain) equipped with Wide Field Camera (WFC). We obtained 6 hrs of photometric observations using the B, V, R Johnson filters, and the r and z SDSS filters during the nights of March 2, and April 18, 2022. The spectrum in the near-infrared region was obtained using the 3.58m Galileo National Telescope (La Palma, Spain). We used the near-infrared camera spectrometer (NICS) with the AMICI prism and a a.5 arcsec slit-width. The configuration allowed a resolving power of R=50 and a spectral interval coverage of 0.8 - 2.45 μm. The photometric data reduction has been made using the Photometry Pipeline [5]. We also used IRAF and MP0 Canopus to cross-check the results. The spectral data was reduced using a dedicated pipeline written in Python. Results First we performed a photometric analysis of the asteroid (4660) Nereus. We determined its period using the Lomb-Scargle Periodogram and we investigated the YORP effect on the asteroid. Subsequently, we obtained the object's phase curve and we computed its absolute magnitude (H) and the slope parameter (G). Then we determined its color indices and we used them for classification. Finally, we reviewed its taxonomic classification based on the new acquired spectrum. Fig 1: Left: The folded lightcurve of (4660) Nereus obtained by combining the data from T025-BD4SB and TCS. Right: Phase curve of (4660) Nereus. The red points are TCS observations while the blue ones are T025-BD4SB. The dotted line represents the H-G model fit. The Lomb-Scargle periodogram peaks at a value of 15.19 hrs. The light-curve corresponding to this period is plotted in Fig. 1. This value is in the range reported by [1] determined a period of 15.1 ± 1.2 h. It is also compatible with the value obtained using radar data [2] of 15.16 ± 0.04 h. Because of its size, (4660) Nereus is subjected to the YORP effect which affects the asteroid's spin rate. We estimate a change of one to four seconds for its rotation period in a range of 10 years. Unfortunately, the previous values for its rotation period have much larger uncertainties. As such, another favorable observing window is needed to quantify this effect. Furthermore, we determine the phase curve of the asteroid in order to obtain its absolute magnitude. In order to do this, we use the Pyedra software [6]. The algorithm allowed us to use the H-G model [7] in order to fit our phase curve (Fig. 1). We obtained the absolute magnitude (H = 18.69 ± 0.18) and the slope parameter (G = 0.209 ± 0.06). In Fig. 1 we show our results. For comparison, [8] reported a value of 18.58 ± 0.06. Fig 2: Left: The color-color diagram of (4660) Nereus compared with the reference data-set (Popescu et al. 2022 - paper in preparation). Right: The near-infrared spectrum of (4660) Nereus and its taxonomic classification. The TCS/MuSCAT2 instrument allowed us to simultaneously obtain the light-curve in all four filters. We found (g-r) = 0.537 ± 0.048, (r-i) = 0.145 ± 0.012, (i-zs) = 0.091 ± 0.017. In addition to these values, we obtained the (B-R) = 1.15 ± 0.05 mag, and ± = 0.043 ± 0.03 mag color indices. The average color values obtained with TCS/MuSCAT2 are compatible with an X-complex classification (Fig. 2). This result complements the spectral classification based on the data obtained with TNG/NICs instrument. The spectrum shown in Fig. 2 is compatible with the Xe type. Acknowledgments The work of MP and RMG was supported by a grant of the Romanian National Authority for Scientific Research -- UEFISCDI, project number PN-III-P1-1.1-TE-2019-1504. The work of MP, JdL, JL, and DM is made in the framework of EU-funded project "NEOROCKS project", SU-SPACE-23-SEC-2019 from the Horizon 2020 - Work Programme 2018-2020. The observations were obtained trough the EURONEAR collaboration. [1] Y. Ishibashi et al, 2000, Earth, Planets and Space [2] Marina Brozovic et al, 2009, Icarus [3] Marco Delb ́o et al, 2003, Icarus [4] Richard P. Binzel et al, 2004, Asteroids II [5] M. Mommert, 2017, Astronomy and Computing [6] M. Colazo et al, 2022, Astronomy and Computing [7] Edward Bowell et al, 1989, Asteroids II [8] Y. Ishibashi et al, 2000, Advances in Space Research

Up to now, only (4) Vesta has been identified as the source of differentiated material, which has been discovered all around the Main Belt region. Most of the basaltic asteroids, identified through spectroscopic measurements, are located in the inner main belt region (2.15-2.5AU) and constitute the Vesta family. These asteroids are indeed dynamically linked to Vesta and share similar spectroscopic properties, showing the absorption bands at 0.92-0.94 micron and 2.0 micron, which are indicative of a basaltic composition. From a dynamical point of view, these objects have proper semimajor axis ap, eccentricity ep and inclination ip in the ranges 2.26 < ap < 2.48, 0.075 < ep <0.122 and 5.6° < ip < 7.9°, respectively (Nesvorny et al. 2015). In addition, a faint absorption band at 0.506 micron, due to a spin forbidden transition of Fe2+, was recently detected also in some V-type asteroids, both members and non-members of the Vesta family (Migliorini et al. 2021). Ground-based observations have shown that few asteroids distributed beyond the 3:1 MMR (Mean Motion Resonance) at 2.5 AU have a basaltic composition (Lazzaro et al. 2000; Hardersen et al. 2004, 2018; Roig et al. 2008; De Sanctis et al. 2011; Solontoi et al. 2012; Ieva et al. 2018; Leith et al. 2017; Migliorini et al. 2018, 2021; Medeiros et al. 2019), although with some differences with respect to Vesta and its family members (Jasmim et al. 2013). Thus, their origin seems to be likely linked to the break-up of large, differentiated objects other than Vesta. Dynamical studies allowed the identification of possible asteroid families, like (221) Eos, (1272) Gefion and (1040) Klumpkea families, which could be the result of the disruption of a differentiated or partly-differentiated parent body. These asteroid families include members with very different spectral types, including basaltic asteroids. Among the asteroids we observed in a previous ground-based campaign, some confirmed V-type asteroids were found to be members of these identified asteroid families, while others lay close to these asteroid families (Migliorini et al. 2021). In the figure below, confirmed basaltic asteroids located beyond 2.5 AU are shown in the proper a- proper I plane and indicated with a circle. Asteroid families are also marked with different colors. Some objects classified as M- (crosses) and A- type (triangles) are also included. We started a new observing campaign to spectrally characterize asteroids selected among the above listed asteroid families, aiming to identify other members with a basaltic composition. In this work we revise the spectral and dynamical properties of basaltic asteroids in the middle and outer main belt, not related to Vesta, and recent observations of asteroids members of the (221) Eos, (1272) Gefion and (1040) Klumpkea families. Figure 1. a-i plane of proper semimajor axis and inclination of the middle (left) and outer (right) main belt. Basaltic asteroids from Migliorini et al. (2021) are shown with circles. Some are identified as members of the asteroids families shaped with different colors, while some are locate close to these families. Some M- type and A- type asteroids, located in the same region, are also reported with crosses and triangles, respectively, for comparison. References De Sanctis M.C. et al. 2011, A&A, 533, A77. Hardersen P.S. et al. 2004, Icarus, 159, 178. Hardersen P.S. et al. 2018, AJ, 156, 11. Ieva S. et al. 2018, MNRAS, 479, 2607. Jasmim F.L. et al. 2013, A&A, 552, A85. Lazzaro D. et al. 2000, Science, 288, 2033. Leith T.B. et al. 2017, Icarus, 205, 61. Medeiros H. et al. 2019, MNRAS, 488, 3866. Migliorini A. et al. 2018, MNRAS, 475, 353. Migliorini A. et al. 2021, MNRAS, 504, 2019. Nesvorny D. et al. 2015, Asteroids IV, p. 895. Roig F. et al. 2008, Icarus, 194, 125. Solontoi M. et al. 2012, Icarus, 218, 571.

An asteroid family is a group of asteroids with similar orbital proper elements (e.g., Nesvorný et al. 2005), which could be fragments formed by large impact events. The heating temperature in primordial bodies is important to form various mineralogies observed in asteroids and meteorites. The short-lived radiogenic heat of 26Al is the plausible heat source for the early stages of planetesimal formation. After 5 Myr of CAIs, 26Al decreases by <1%. Heating temperatures caused by 26Al highly depend on the water-to-rock ratio (W/R) and accretion timing in the planetesimal. W/R can be a good indicator of the formation distance from the Sun. However, it should be noted that W/R can be changed by the differentiation process (Wakita et al. 2011, Neumann et al. 2020, Kurokawa et al. 2022). The taxonomic composition of a family can be a witness to the internal structure of a primordial body, before disruption to become a collisional family. The near-ultraviolet wavelengths (NUV; 0.3-0.5 µm) and 0.7-µm absorption band are sensitive to the presence of phyllosilicates (Feierberg et al. 1985, Vilas and Gaffey 1989). The presence or absence of the 0.7-µm band and the NUV absorption suggest a possible differentiation process. Methods: In this study, in order to cover the NUV to visible wavelength range, using two spectrophotometric surveys, we used SDSS MOC4 (Ivezić et al. 2001) and ECAS (Zellner et al. 1985), for evaluation of the taxonomic configuration of family members. The asteroid family members were classified based on Tholen’s taxonomy (Tholen 1984). Furthermore, the 0.7-µm band (HYD) was evaluated as the slope change between the SDSS r-i filters to i-z filters: HYD=[r-i-(r-i)_sun]-[i-z-(i-z)_sun]. Results: Some of these families had been studied spectroscopically and the fraction of members with 0.7-µm band absorption can be obtained from the literature (Mothé-Diniz et al. 2005, Morate et al. 2016, 2018, 2019, de León et al. 2016, De Prá et al. 2020). Families with negative HYD values have a majority of members with the 0.7-µm band absorption from the spectroscopic studies. Thus, we found the HYD is a good proxy for the 0.7-µm band absorptions, even though the SDSS filters are not optimized for characterizing the 0.7-µm band. Furthermore, a strong correlation (correlation coefficient of -0.69) exists between HYD and the NUV absorption, suggesting that the NUV absorption can be also used for evaluating the presence of Fe-bearing phyllosilicates. The NUV absorption strength decreases from G > C/B > F/CP > P > D, which is in good agreement with the percentage of objects showing 0.7-µm band found by Vilas (1994) and Fornasier et al. (2014). Thus, G types might be dominated by Fe-bearing phyllosilicates in composition, while F types might be dominated by Fe-poor phyllosilicates. The figure shows the taxonomic compositions for primitive asteroid families that have greater than 30 asteroid members. We found several families consist of relatively homogeneous taxonomic types. The collisional families with majority of G type (the highest NUV absorption) are composed of Fe-rich phyllosilicates, and those with majority of F type (the lowest NUV absorption) are composed of Mg-rich phyllosilicates or dehydrated phyllosilicates. There are also intermediate families which consist of variety of taxonomic classes, which may inhere compositional heterogeneity. This heterogeneous families are larger than 200 km, indicating the size of primordial bodies may play a great role to differentiate or produce different lithologies inside the bodies. Figure. Taxonomic structure of primitive asteroid families. References: Nesvorný et al. (2005) Icarus 173, 132-152. Wakita et al. (2011) EPS 63, 1193-1206. Neumann et al. (2020) A&A 633, A117. Kurokawa et al. (2022) AGU Acvances 3, e2021AV000568. Feierberg et al. (1985) Icarus 63, 183-191. Vilas and Gaffey (1989) Science 246, 790-792. Ivezić et al. (2001) Astron. J 122, 2749-2784. Zellner et al. (1985) Icarus 61, 355-416. Tholen (1984) PhD thesis from University of Arizona. Mothé-Diniz et al. (2005) Icarus 174, 54-80. Morate et al. (2016) A&A 586, A129. Morate et al. (2018) A&A 610, A25. Morate et al. (2019) 630, A141. De Prá et al. (2020) A&A 643, A102. Vilas (1994) Icarus 111, 456-467.

We describe results of a planetary defense exercise conducted during the close approach to Earth by the near-Earth asteroid (99942) Apophis during 2020 December–2021 March. The planetary defense community has been conducting observational campaigns since 2017 to test the operational readiness of the global planetary defense capabilities. These community-led global exercises were carried out with the support of NASA’s Planetary Defense Coordination Office and the International Asteroid Warning Network. The Apophis campaign is the third in our series of planetary defense exercises. The goal of this campaign was to recover, track, and characterize Apophis as a potential impactor to exercise the planetary defense system including observations, hypothetical risk assessment and risk prediction, and hazard communication. Based on the campaign results, we present lessons learned about our ability to observe and model a potential impactor. Data products derived from astrometric observations were available for inclusion in our risk assessment model almost immediately, allowing real-time updates to the impact probability calculation and possible impact locations. An early NEOWISE diameter measurement provided a significant improvement in the uncertainty on the range of hypothetical impact outcomes. The availability of different characterization methods such as photometry, spectroscopy, and radar provided robustness to our ability to assess the potential impact risk.

This work presents the analysis of seven mutual events of the Patroclus–Menoetius system (PMS) observed during the last season of mutual events, in 2017–2018. We compare the obtained light curves with those predicted using Grundy et al. and discuss the differences in the timing of the events and the drop of magnitude. Based on models of these observations, we present a collection of orbital parameters that provide the best fit for the observed events and compare the new solutions for the orbit of the system with solutions provided in the literature. Furthermore, we also discuss an interesting finding in the light curve of the only superior event in our collection. This light curve (the one with the best signal-to-noise ratio in our data set) shows the imprint of a possible crater in the south pole of Menoetius as deep as a fourth of its radius.

Primitive asteroids (PAs) are characterized by dark surfaces (albedo < 10%) dominated by carbon compounds. Their reflectance spectra are similar to those of carbonaceous chondrites (CCs), the most pristine meteorites in our records, abundant in hydrated minerals and organics. Studying these life-forming materials in PAs and CCs is important to answer how water and life appeared on Earth. PAs present rather featureless spectra in visible and near-infrared wavelengths (from 0.5 to 2.5 microns). The most diagnostic and reliable region to study hydrated mineralogies and organics is the 3 microns region. However, observing at those wavelengths is extremely complicated using ground-based telescopes due to Earth's atmosphere, and so, the 3-microns feature can only be appropriately studied using space telescopes (e.g. AKARI). Another feature in visible wavelengths around 0.7 µm, thus accessible from the Earth, is related to the Fe2+ Fe3+ iron transition in hydrated mineralogies (Vilas 1994, Fornasier et al. 2014, Morate et al. 2016). However, this band is shallow. Hiroi et al (1998) have proposed a correlation between the 3 microns band and the UV absorption based on the meteorite spectra. In our work, we aim to explore the near UV (NUV hereafter) behavior of PAs and try to relate it with the main characteristics in the visible (0.7 micron band and slope). To accomplish this objective we have observed and explored spectral data for more than a hundred primitive asteroids with different taxonomies using the 3.58-m Telescopio Nazionale Galileo and the 2.54-m Isaac Newton Telescope located at the Roque de Los Muchachos Observatory. All the spectra go down to ~0.35 microns (near-UV or NUV). The ground-based reflectance spectroscopy in NUV needs special cautions such as airmass, and solar analogs (Tatsumi et al. accepted). In addition, we have explored the Hubble Space Telescope archive thanks to the Archival Research Visitor Program from ESA, finding also some primitive asteroids observed at UV. We also selected ~100 PAs from the MoOJA catalog (Morate et al. 2021), that have 5 filters between 0.35 and 0.55 microns and other 7 from 0.55 to 1 microns. This set of filters allows us to obtain information about how strong is the NUV absorption, to characterize the 0.7-micron band, and to compute several spectral slopes. Results: we have found a correlation of 77% between the difference of spectral slopes between 0.4 - 0.55 microns and 0.55-0.7 microns (associated with the absorption in the UV) and the difference of spectral slopes between 0.55 - 0.7 microns and 0.7-0.9 microns (associated with iron transition at 0.7 microns), see Figure 1. Therefore, this drop in reflectance in the NUV can be used as a proxy for the phyllosilicates to measure the hydration degree of asteroids. Moreover, there are Fe-rich and Mg-rich phases among phyllosilicates, which reflect the amount of water present during their formation. On other hand, we have found a way to describe the beginning of the NUV drop, and among different taxonomies, there is a difference in the wavelength statistically significant, see Figure 2. Gaia DR3 will provide thousands of low-resolution slit-less spectra of asteroids in the range of 0.35 - 0.90 microns before the meeting. This will constitute the largest dataset of asteroid spectra down to the NUV and we are going to also present how the thousands of asteroid spectra look like in our spectral slope space. Figure 1. Slope change at 0.55 microns (computed as slope between 0.39 and 0.55 microns minus slope between 0.55 and 0.7) versus slope change at 0.7 microns (computed as slope between 0.55 and 0.7 minus slope between 0.7 and 0.9). The Pearson correlation coeficient between both variables is 0.77. Figure 2. Histogram for the wavelength where the drop in reflectance downwards UV wavelengths begins for C, B, G and F taxonomies. We can see 2 main groups: one around 0.4 microns composed by F and B types and the other around 0.55 containing mainly C and G types. REFERENCES Fornasier, S., Lantz, C., Barucci, M. A., & Lazzarin, M. 2014, Icarus, 233, 163 Hiroi, T. and Zolensky, E.M.: 1998, Antarctic Meteorites XXIII; 23, 30. Morate, D., de León, J., De Prá, M., et al. 2016, A&A, 586, A129 Tatsumi, E., Tinaut-Ruano, F., de León, J., et al. 2022, A&A, accepted Vilas, F. 1994, Icarus, 111, 456

Introduction. The NEO Rapid Observation, Characterization and Key Simulations (NEOROCKS) project is funded (2020-2023) through the H2020 European Commission programme to improve our knowledge on near-Earth objects by connecting expertise in performing small body astronomical observations and the related modelling needed to derive their dynamical and physical properties. The Instituto de Astrofísica de Canarias (IAC), and in particular members of the Solar System Group, participate in the NEOROCKS project and currently are devoted to one specific task: to collect observational data, mainly in the visible and near-infrared wavelength regions, of NEAs that have been observed in the past using the Arecibo Planetary Radar. In this work we present preliminary results, focusing on those targets for which the signal-to-noise ratio is satisfactorily high. Observations. Our observations include spectroscopy, color photometry and lightcurves. They are performed using the facilities located at the Observatorios de Canarias (OOCC), including the El Teide Observatory in the island of Tenerife and the El Roque de los Muchachos Observatory in the island of La Palma. Visible and near-infrared spectra are mainly obtained using the 10.4-m Gran Telescopio de Canarias (GTC) and its visible (OSIRIS) and near-infrared (EMIR) spectrographs. We also use the ALFOSC spectrograph at the 2.5-m Nordic Optical Telescope (NOT). Visible color photometry is obtained using the MuSCAT2 instrument at the 1.5-m Telescopio Carlos Sánchez (TCS). The setup allows us to obtain simultaneous imaging in the g, r, i, and zs visible bands. Time-series photometry in the visible is obtained using several telescopes, including the 46-cm TAR2, 80-cm IAC-80, and 1-m Jacobus Kapteyn Telescope (JKT). Results. Spectra in the visible and/or the near-infrared wavelengths, as well as color photometry in the visible, allow us to taxonomically classify the targets and to infer their composition. In the case of having no albedo measurements for any given object, we can also use the taxonomy to have an estimation of the albedo based on the spectral class, and therefore determine the size of the asteroid. Lightcurves allow us to both get the asteroid rotational period and, together with radar data, to obtain the shape and the spin axis orientation of the target. In this way, a full characterization can be obtained for every asteroid observed within this program. So far, we have obtained spectra/colors/lightcurves in the visible for more than 100 NEAs. In this work, we present our most updated results. Acknowledgements. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 870403.

Research into the orbital and physical properties near-Earth asteroids (NEAs) is important as these objects can reveal information about the origin and history of our planetary system. Here we present our findings regarding the physical characteristics of the near Earth asteroids (NEAs) 2005 UD and 2001 SG286. The 2005 UD is currently a possible target for the DESTINY+ space mission, along with (3200) Phaeton which seems to share similar dynamic and physical characteristics. However, compared to Phaethon, there is still limited data available regarding 2005 UD. On the other hand, 2001 SG286 is another very interesting object, feasible as target for a sample-return mission which required additional observations to firmly establish its nature and composition. In order to obtain the light-curves of these objects, we used the 2.5m Issac Newton Telescope (INT) equipped with Wide Field Camera CCD4 and the Sloan photometric filters. The visible spectrum of 2005 UD was captured using the INT with the Intermediate Dispersion Spectrograph (IDS) instrument. Furthermore, we used the 3.58m Telescopio Nazionale Galileo (TNG) equipped with the NICS instrument and the AMICI prism disperser to capture its infrared spectrum. The spectrum of 2001 SG286 was acquired using the 10.4m Gran Telescopio Canarias equipped with Optical System for Imaging and low Resolution Integrated Spectroscopy (OSIRIS) instrument. The observations of both objects were made during their recent favorable approaches (October 2018 for 2005 UD and October 2020 for 2001 SG 286). For photometric data reduction we used the PHOTOMETRY PIPELINE by Michael Mommert and the MPO CANOPUS software with the reference stars from the GAIA and APASS catalogues, respectively. The nightly zero points were found to be consistent up to 0.1 magnitudes. MPO Canopus was finally used for the rotation period analysis, using the FALC (Fourier Analysis of Light Curves) algorithm. The light-curve plots are shown below. The “Reduced Magnitude” on the Y axis represents the Sloan filter magnitude values that have been corrected from sky magnitudes to unity distance by applying –5 * log(rR) to the initial measurements, where r is the Earth-asteroid distance and R is the Sun-asteroid distance. The X axis represents the rotational phase. For 2005 UD, we found that a trimodal solution with a period of 7.85 hours is the best fit with polynomial orders ranging from 3 to 8, taking into account the INT data. This solution was previously suggested by Moskovitz in his presentation at PERC Int'l Symposium on Dust & Parent Bodies 2019 (IDP 2019) as a valid possibility, besides the predominant value of 5.23 hours currently found in the literature [1]. As for 2001 SG286, our analysis indicates that it is a non-principal axis slow rotator (tumbler), with overlapped rotational periods of 12.3 and 18.45 hours. Although we searched for a binary solution, we could not get a compelling result. Moreover, probabilistically there is a low chance of finding a companion given that the majority of binary asteroids are fast rotators. 2005 UD presents a C-type spectrum according to Bus-DeMeo classification. In this case, we used the infrared data to calculate the thermal excess according to the thermal model described by Rivkin et al [2]. By further applying the aforementioned model and taking into account the heliocentric distance of the object at the time of the observation, we determined the geometrical albedo of 2005 UD to be pV = 0.06, which is in agreement to the latest estimate of Masiero et al [3]. On the other hand, the high quality spectral data obtained with GTC allowed us to firmly determine that 2001 SG286 is an S-type asteroid according to Bus-DeMeo classification, a result which is not in agreement with previous studies[4][5]. References: 1. B. Warner and R. Stephens “Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2019 July-September”, Minor Planet Bull. 2020 Jan;47(1):23-34. 2. A.S. Rivkin et al. “Constraining near-Earth object albedos using near-infrared spectroscopy”, Icarus 175 (2005) 175–180. 3. J. R. Masiero et al. “Asteroid Diameters and Albedos from NEOWISE Reactivation Mission Years 4 and 5”, The Planetary Science Journal, 1:5, 2020 March 4. Binzel et al. “Dynamical and compositional assessment of near-Earth object mission targets”, Meteoritics & Planetary Science 39, Nr 3, 351–366 (2004) 5. Popescu, M. et al. “Spectral properties of eight near-Earth asteroids”, A&A 535, A15 (2011) Acknowledgements: The work of RMG, and MP was supported by a grant of the Romanian National Authority for Scientific Research – UEFISCDI, project number PN-III-P1-1.1- TE-2019-1504. The work of MP, JdL, JL, is made in the framework of EU-funded project ”NEOROCKS - The NEO Rapid Observation, Characterization and Key Simulations project”, SU-SPACE-23-SEC-2019 from the Horizon 2020 - Work Programme 2018-2020, under grant agreement No 870403

Near-Earth objects (NEOs) deserve our attention because they pose an impact risk for Earth. A good example is the Chicxulub impactor that produced the Cretaceous/Tertiary mass extinction event 65 Myr ago (Bottke et al. 2007). Up to now, more than 1 milion of asteroids have been discovered, and about 28,700 are cataloged as NEOs. This number steadily increases every month. Even if this currently known population of NEOs does not pose a direct threat to humanity within the next century, we are not able to assert that tomorrow we will not discover an asteroid capable of wiping out life on Earth in the next years. Within the NEO population there is a subclass defined potentially hazardous asteroids (PHAs). These are objects with an orbit that can make close approaches to the Earth (whose minimum orbit intersection distance, or MOID, to Earth’s orbit is smaller than 0.05 AU), and large enough (absolute magnitude H ≤ 22, or equivalent diameter above ∼140 m, assuming the average NEO albedo of 0.14) to cause significant regional damage in the event of impact. Currently, more than 2200 NEAs are classified as PHAs. Any mitigation strategy designed for a potential impact is dependent on the ability to determine the asteroid’s physical properties (Perna et al. 2016): the damage produced by a possible collision will mainly depend on the speed of the impact, the size of the object, and its composition. In this context, the knowledge of the physical properties of PHAs is still poor, with less than 15% having their taxonomies determined (∼300 objects). Due to this, improving our understanding on PHAs and their composition is essential for planning space-missions aimed to develop preventive actions against potential impacts (e. g. Cheng et al. 2018). For the present work, we have investigated the physical nature of several PHAs, using data obtained within the framework of the Visible NEAs Observations Survey (ViNOS). We analyzed and characterized a sample comprised of 14 of these objects. To conduct this study, we obtained visible spectra of these 14 PHAs in the 0.5-0.9 μm region using the 2.5m Nordic Optical Telescope, located at the El Roque De Los Muchachos Observatory in La Palma (Spain). The resulting spectra were combined with their corresponding near-infrared counterparts, available in the literature from SMASS. We performed a taxonomical classification of the spectra, and computed several diagnostic spectral parameters (slopes, band centres, and band area ratios). We also compared the spectra with laboratory spectra of meteorites from the RELAB database. Among the studied sample of PHAs, approximately 90% of the objects (13 out of 14) were classified as silicaceous (S-types and subclasses). Only one object, 489486, was classified as carbonaceous. Five of the studied PHAs did not previously have taxonomical classifications. The comparisons of the silicaceous PHAs with meteoritic spectra all yielded ordinary chondrites (OCs) as the best match for meteoritic analogs, and the computed mineralogy of all of our targets is consistent with this results (see Fig. 1). Fig. 1. Distribution of the studied asteroids BAR versus Band Center I space. The enclosed regions are taken from Dunn et al. (2013), which follow the results of Gaffey et al. (1993), Burbine et al. (2001), and Cloutis et al. (2010). Asteroids with two NIR spectra, and thus, two sets of spectral parameters, are connected by a dashed line. The numbers represent the corresponding object (when repeated, refers to its second spectrum).

The Javalambre Photometric Local Universe Survey (J-PLUS) is an observational campaign that aims to obtain photometry in 12 ultraviolet-visible filters (0.3–1 μm) of ∼8 500 deg2 of the sky observable from Javalambre (Teruel, Spain). Due to its characteristics and strategy of observation, this survey will let us analyze a great number of Solar System small bodies, with improved spectrophotometric resolution with respect to previous large-area photometric surveys in optical wavelengths.The main goal of this work is to present here the first catalog of magnitudes and colors of minor bodies of the Solar System compiled using the first data release (DR1) of the J-PLUS observational campaign: the Moving Objects Observed from Javalambre (MOOJa) catalog.Using the compiled photometric data we obtained very-low-resolution reflectance (photospectra) spectra of the asteroids. We first used a σ-clipping algorithm in order to remove outliers and clean the data. We then devised a method to select the optimal solar colors in the J-PLUS photometric system. These solar colors were computed using two different approaches: on one hand, we used different spectra of the Sun, convolved with the filter transmissions of the J-PLUS system, and on the other, we selected a group of solar-type stars in the J-PLUS DR1, according to their computed stellar parameters. Finally, we used the solar colors to obtain the reflectance spectra of the asteroids.We present photometric data in the J-PLUS filters for a total of 3 122 minor bodies (3 666 before outlier removal), and we discuss the main issues of the data, as well as some guidelines to solve them.

We present NIR spectra of 19 asteroids in the Sulamitis family as part of our survey of primitive inner belt asteroid families. The spectra were obtained with NASA's Infrared Telescope Facility and the Telescopio Nazionale Galileo between January 2017 and February 2020. We find spectral homogeneity in our sample despite the diversity within the family observed at visible wavelengths. The average Sulamitis spectrum is flat with a spectral slope of 0.89 + 0.26%/1000 angstrom between 0.95 and 2.3 mu m. We show that the Sulamitis family is spectrally similar to other inner belt families in the NIR, despite differences between families seen in the visible wavelength range. We also compare our obtained spectra with asteroids (101955) Bennu and (162173) Ryugu to show that the Sulamitis family is a plausible source of Ryugu.