Asteroids’ Size Distribution and Colors from HITS

Peña, José Martínez; Fuentes, César; Förster, F.; Martínez-Palomera, Jorge; Cabrera-Vives, G.; Maureira, J. C.; Huijse, P.; Estévez, P. A.; Galbany, L.; González–Gaitán, S.; Jaeger, Th. de

doi:10.3847/1538-3881/ab7338

Cited by 13 publications

(13 citation statements)

References 61 publications

(105 reference statements)

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“…Interestingly, this result is well consistent with the possible periodic activity predicted by our model for FRB 121102 (Dai et al 2016;Bagchi 2017), and thus, from the analysis in this paper, can also provide a constraint on R a,out of an EAB (see Figure 3). It is seen from this figure that R a,out always increases with e for a given q and is in the range of ∼ 0.69 AU to ∼ 1.7 AU, which is smaller than that of the solar-system main asteroid belt by a factor of a few (DeMeo & Carry 2014;Peña et al 2020).…”

Section: Conclusion and Discussionmentioning

confidence: 75%

“…The outer radius increases from ∼ 0.13 AU to ∼ 0.26 AU if q is set to be 0.25 to 4. This shows that R a,out of the EAB responsible for FRB 180916.J0158+65 is at least an order of magnitude smaller than that of its solar-system analogue (DeMeo & Carry 2014; Peña et al 2020).…”

Section: Constraint On the Outer Radiusmentioning

confidence: 89%

“…where D is the asteroidal diameter. In the solar system, β 1 ≃ 2.3, β 2 ≃ 4.0 and D br ∼ 6.0 km (Ivezić et al 2001;Davis et al 2002;Yoshida & Nakamura 2007;Ryan et al 2015;Peña et al 2020). In the case of E iso ∝ m, equation ( 10) gives a differential energy distribution of FRBs,…”

Section: A Simple Waymentioning

confidence: 99%

“…This EAB has an inner radius R a,in ≪ R a,out and an inclination angle, implying that its thickness is nearly proportional to radius. In structure, the EAB may thus be analogous to the main asteroid belt in the solar system (DeMeo & Carry 2014;Peña et al 2020) but the two belts could have some different physical parameters. The pulsar and the star, whose masses are taken to be M pulsar and M star respectively, form a binary (see Figure 1) and rotate around the center of mass (i.e., point O), which is also assumed to be the original point of a coordinate system (x, y).…”

Section: Constraints On An Eabmentioning

confidence: 99%

“…As shown by the Sloan Digital Sky Survey (SDSS) data (Ivezić et al 2001;Davis et al 2002), the Subaru Main Belt Asteroid Survey (SMBAS) data (Yoshida & Nakamura 2007), the Spitzer Space Telescope infrared data (Ryan et al 2015), and the High cadence Transient Survey (HiTS) data (Peña et al 2020) of solar system objects, the differential size distribution of the EAB's asteroids can also be assumed to be written as…”

Section: A Simple Waymentioning

confidence: 99%

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Periodic Fast Radio Bursts as a Probe of Extragalactic Asteroid Belts

Dai,

Zhong

2020

Preprint

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The periodic activity of repeating fast radio burst (FRB) 180916.J0158+65 was recently reported by the CHIME/FRB Collaboration team. 28 bursts from this source not only show a ∼ 16-day period with an active phase of ∼ 4.0 days but also indicate a broken power law in differential energy distribution. In this paper, we suggest that FRB 180916.J0158+65-like periodic FRBs would provide a unique probe of extragalactic asteroid belts (EABs), based on our previously-proposed pulsar-EAB impact model, in which repeating FRBs arise from an old-aged, slowly-spinning, moderately-magnetized pulsar traveling through an EAB around another stellar-mass object. These two objects form a binary and thus the observed period is in fact the orbital period. We constrain the EAB's properties by using the observed data of FRB 180916.J0158+65. We find that (1) the outer radius of the EAB is at least an order of magnitude smaller than that of its analogue in the solar system, (2) the differential size distribution of the EAB's asteroids at small diameters (large diameters) is shallower (steeper) than that of solarsystem small objects, and (3) the EAB's total mass is about one to two orders of magnitude smaller than the mass of the main asteroid belt in the solar system.

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Section: Conclusion and Discussionmentioning

confidence: 75%

Section: Constraint On the Outer Radiusmentioning

confidence: 89%

Section: A Simple Waymentioning

confidence: 99%

Section: Constraints On An Eabmentioning

confidence: 99%

Section: A Simple Waymentioning

confidence: 99%

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Periodic Fast Radio Bursts as a Probe of Extragalactic Asteroid Belts

Dai,

Zhong

2020

Preprint

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How we can mine asteroids for space food

Pilles,

Nicklin,

Pearce

2024

International Journal of Astrobiology

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To deeply explore the solar system, it will be necessary to become less reliant on the resupply tether to Earth. An approach explored in this study is to convert hydrocarbons in asteroids to human edible food. After comparing the experimental pyrolysis breakdown products, which were able to be converted to biomass using a consortia, it was hypothesized that equivalent chemicals found on asteroids could also be converted to biomass with the same nutritional content as the pyrolyzed products. This study is a mathematical exercise that explores the potential food yield that could be produced from these methodologies. This study uses the abundance of aliphatic hydrocarbons in the Murchison meteorite (>35 ppm) as a baseline for the calculations, representing the minimum amount of organic matter that could theoretically be attributed to biomass production. Calculations for the total carbon in solvent-insoluble organic matter (IOM) represent the maximum amount of organic matter that could theoretically be attributed to food production. These two values will provide a range of realistic yields to determine how much food could theoretically be extractable from an asteroid. The results of this study found that if only the aliphatic hydrocarbons can be converted into biomass (minimum scenario) the resulting mass of edible biomass extractable from asteroid Bennu ranges from 5.070 × 107 g to 2.390 × 108 g. If the biomass extraction process, however, is more efficient, and all IOM is converted into edible biomass (maximum scenario), then the mass of edible biomass extractable from asteroid Bennu ranges from 1.391 × 109 g to 6.556 × 109 g. This would provide between 5.762 × 108 and 1.581 × 1010 calories that is enough to support between 600 and 17 000 astronaut life years. The asteroid mass needed to support one astronaut for one year is between 160 000 metric tons and 5000 metric tons. Based on these results, this approach of using carbon in asteroids to provide a distributed food source for humans appears promising, but there are substantial areas of future work.

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Enabling discoveries of Solar System objects in large alert data streams

Le Montagner,

Peloton,

Carry

et al. 2023

A&A

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Context. With the advent of large-scale astronomical surveys, such as the Zwicky Transient Facility (ZTF) and the forthcoming Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST), the number of alerts generated by transient, variable, and moving astronomical objects is growing rapidly, reaching millions of alerts per night. Concerning the minor planets of the Solar System, their identification requires linking the alerts for many observations over a potentially lengthy period of time, leading to a very large combinatorial number. Aims. The goal is to demonstrate how a third-party module dedicated to the identification of new minor planets of the Solar System can be integrated with the Fink alert broker real-time operations, which deals with massive alert data streams produced by large-scale surveys. Methods. Our analysis takes advantage of the scientific surplus brought on by the Fink alert broker classification capabilities to first reduce the 111 275 131 processed alerts from ZTF between November 2019 and December 2022 (755 observation nights) to only 389 530 new Solar System alert candidates over the same period. We implemented a simple, yet pedagogical linking algorithm called Fink-FAT to create trajectory candidates in real time from alert data and extract orbital parameters. The analysis was validated on ZTF alert packets linked to confirmed Solar System objects from the Minor Planet Center (MPC) database. Finally, the candidates were confronted with follow-up observations. Results. Between November 2019 and December 2022, Fink-FAT extracted 327 new orbits from candidate Solar System objects at the time of the observations, of which 65 had still remained unreported in the MPC database as of March 2023. After two late follow-up observation campaigns of six orbit candidates, four were associated with known minor planets of the Solar System, and two still remain unknown. In terms of performance, Fink-FAT took under 3 h to link alerts into trajectory candidates and to extract the orbital elements over the three years of Fink data, using a modest hardware configuration. Conclusions. Despite a much lower efficiency than present linking algorithms, Fink-FAT reaches a high level of purity in reconstructing orbits and it runs fast, making it suitable for the real-time discovery of new minor planets. Fink-FAT is deployed in the Fink broker and analyzes, in real time, the alert data from the ZTF survey by regularly extracting new candidates for Solar System objects. Tests of scalability also show that Fink-FAT is capable of handling the even larger volume of alert data that will be sent by the Rubin Observatory’s real-time difference image analysis processing.

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Asteroids’ Size Distribution and Colors from HITS

Cited by 13 publications

References 61 publications

Periodic Fast Radio Bursts as a Probe of Extragalactic Asteroid Belts

Periodic Fast Radio Bursts as a Probe of Extragalactic Asteroid Belts

How we can mine asteroids for space food

Enabling discoveries of Solar System objects in large alert data streams

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