J/A+A/674/A50 Near-Earth Object (NEO) properties (Deshapriya+, 2023)
Clustering the properties of Near-Earth Objects:
physico-dynamical links among NEOs.
Deshapriya J.D.P., Perna D., Bott N., Hasselmann P.H., Granvik M., Dotto E.,
Fulchignoni M., Giunta A., Perozzi E., Ieva S., Petropoulou V.,
Mazzotta Epifani E.
<Astron. Astrophys. 674, A50 (2023)>
=2023A&A...674A..50D 2023A&A...674A..50D (SIMBAD/NED BibCode)
ADC_Keywords: Minor planets ; Optical
Keywords: minor planets, asteroids: general - techniques: spectroscopic -
methods: statistical
Abstract:
Near-Earth Objects (NEOs) are being discovered at an ever increasing
rate. However, their physical characterisation significantly lags
behind. In particular, the taxonomic classification of newly
discovered NEOs is of great importance to better understand the
population of NEOs.
In this context, our goal is to probe potential links between orbital
properties of NEOs and their composition. We investigate whether we
can make a reasonable guess about the taxonomic class of an NEO upon
its discovery with a decent orbital accuracy.
We used G-mode multivariate statistical clustering method to find
homogeneous clusters in a dataset composed of orbital elements of
NEOs. We adopted two approaches using 2 sets of variables as inputs to
the G-mode method. In each approach, we analysed the available
taxonomic distribution of resulting clusters to find potential
correlations with several unique parameters that distinctively
characterise NEOs. We then applied a dynamical model on the same
clusters to trace their escape regions.
Approach 1 led us to obtain NEO clusters that can be linked to a
primitive composition, and this result was further strengthened by
the dynamical model, which mapped outer-belt sources as escape regions
for these clusters. We remark the finding of a cluster akin to S-type
NEOs in highly eccentric orbits during the same Approach 1. Two
clusters: one with small NEOs in terrestrial-like orbits and one with
relatively high inclinations were found to be common to both
approaches. Approach 2 revealed three clusters only separable by their
arguments of perihelion and, together they compose the majority of
known Atira asteroids.
For an NEO whose orbit is relatively well determined, we propose a
model to determine whether the taxonomy of an NEO is siliceous or
primitive if the orbital elements of the NEO fall within the presented
combinations of inclination, eccentricity and semi-major axis ranges.
Description:
The file dataset.dat contains the data of NEOs that were used to
obtain the results of this paper. Orbital are sourced from the IAU
Minor Planet Center (MPC) at
https://www.minorplanetcenter.net/iau/mpc.html and NASA Small-Body
Database (SBDB) at https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/.
The taxonomic data are sourced from published literature based on
spectroscopic surveys (Perna et al., 2018, Planetary and Space
Science, 157, 82; Binzel et al. 2019, Icarus, 324, 41; Devogele et
al., 2019AJ....158..196D 2019AJ....158..196D, Cat. J/AJ/158/196; Ieva et al.
2020A&A...644A..23I 2020A&A...644A..23I, Cat. J/A+A/644/A23; Simion et al.,
2021MNRAS.508.1128S 2021MNRAS.508.1128S; Hromakina et al. 2021A&A...656A..89H 2021A&A...656A..89H) as well as
spectrophotometric surveys (Lin et al., 2018, Planetary and Space
Science, 152, 116). Albedo data are sourced mainly from the neowise
dataset (Mainzer et al., 2019, NASA Planetary Data System) whenever
available.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
dataset.dat 248 14132 Data of NEOs that were used to obtain the
results of this paper
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See also:
B/astorb : Orbits of Minor Planets (Bowell+ 2014)
https://www.minorplanetcenter.net/iau/mpc.html : MPC Home Page
https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/ : SBDB Home Page
Byte-by-byte Description of file: dataset.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- Number ?=0 NEO number
8- 24 A17 --- Name NEO name (0 for none)
26- 35 A10 --- Design NEO designation (0 for none)
37 I1 --- Unc [0/5] MPC "U" parameter which gives the
uncertainty of the orbit of the NEO (1)
39 I1 --- orbitType [1/4] Dynamical orbital type (2)
41- 60 F20.16 deg i NEO orbit inclination (the angle with respect
to x-y ecliptic plane)
62- 79 F18.16 --- e NEO orbit eccentricity
81- 99 F19.16 au a NEO orbit semi-major axis
101-118 F18.16 au q NEO orbit perihelion
120-138 F19.16 au Q NEO orbit aphelion
140-161 E22.17 au eMOID Minimum orbit intersection distance with
respect to Earth
163-169 A7 --- Taxo NEO taxonomic class
171-188 F18.15 mag H NEO absolute magnitude
190-208 F19.16 --- TJ Tisserand Parameter of the NEO with respect
to Jupiter
210-227 F18.16 % Albedo ? Geometric albedo of the NEO
229-248 F20.16 deg omega Argument of the perihelion of the NEO
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Note (1): This is also called the condition code in the SBDB.
This is an integer in the range 0 to 9, where 0 indicates a very
small uncertainty and 9 an extremely large uncertainty.
In practice, U is rarely larger than 6.
Note (2): Dynamical orbital type as follows:
1 = Atiras
2 = Atens
3 = Apollos
4 = Amors
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History:
From Jasinghege Don Prasanna Deshapriya, prasanna.deshapriya(at)inaf.it
Acknowledgements:
We acknowledge the financial support from Agenzia Spaziale Italiana
(ASI, contract No. 2017-37-H.0 CUP F82F17000630005). We also
acknowledge funding from the European Union's Horizon 2020 research
and innovation programme under grant agreement No. 870403. This work
has made use of the python astroquery library (Ginsburg et al.,
2019AJ....157...98G 2019AJ....157...98G).
(End) Patricia Vannier [CDS] 03-Apr-2023