Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations

Pravec, Petr; Harris, Alan W.; Kušnirák, Peter; Galád, Adrián; Hornoch, Kamil

doi:10.1016/j.icarus.2012.07.026

Cited by 192 publications

(216 citation statements)

References 34 publications

Supporting

Mentioning

185

Contrasting

Order By: Relevance

“…The absolute magnitude reported by Pravec et al (2012) is H = 14.270, which is close to the value derived from the lightcurve observations, H = 14.10. Very different values are reported for the albedo: based on the WISE thermal observations, Pravec et al (2012) There are several spectra available for this object.…”

Section: (5143) Heraclessupporting

confidence: 84%

Spectral properties of the largest asteroids associated with Taurid Complex

Popescu

Birlan

Nedelcu

et al. 2014

A&A

View full text Add to dashboard Cite

Context. The Taurid Complex is a massive stream of material in the inner part of the Solar System. It contains objects spanning the range of 10 −6 -10 3 m, considered by some authors to have a common cometary origin. The asteroids belonging to Taurid Complex are on Apollo type orbit, with most of them being flagged as potentially hazardous asteroids. In this context, understanding the nature and the origin of this asteroidal population is not only of scientific interest but also of practical importance. Aims. We aim to investigate the surface mineralogy of the asteroids associated with Taurid Complex using visible and near-infrared spectral data. Compositional linking between these asteroids and meteorites can be derived based on the obtained spectra. Methods. We obtained spectra of six of the largest asteroids (2201, 4183, 4486, 5143, 6063, and 269690) associated with Taurid complex. The observations were made with the IRTF telescope equipped with the spectro-imager SpeX. Their taxonomic classification is made using Bus-DeMeo taxonomy. The asteroid spectra are compared with the meteorite spectra from the Relab database. Mineralogical models were applied to determine their surface composition. All the spectral analysis is made in the context of the already published physical data. Results. Five of the objects studied in this paper present spectral characteristics similar to the S taxonomic complex. The spectra of ordinary chondrites (spanning H, L, and LL subtypes) are the best matches for these asteroid spectra. The asteroid (269690) 1996 RG3 presents a flat featureless spectrum which could be associated to a primitive C-type object. The increased reflectance above 2.1 microns constrains its geometrical albedo to a value around 0.03. Conclusions. While there is an important dynamical grouping among the Taurid Complex asteroids, the spectral data of the largest objects do not support a common cometary origin. Furthermore, there are significant variations between the spectra acquired until now.

show abstract

Section: (5143) Heraclessupporting

confidence: 84%

Spectral properties of the largest asteroids associated with Taurid Complex

Popescu

Birlan

Nedelcu

et al. 2014

A&A

View full text Add to dashboard Cite

show abstract

“…We used the H-G 12 values computed by Oszkiewicz et al (2011), from now on referred to as O11. Vereš et al (2015) (V15) also produced a catalogue of H-G 12 values based on Pan-STARRS photometry and found systematic differences with respect to the Minor Planet Center and O11 absolute magnitudes but not with respect to those obtained by Pravec et al (2012) based only on high-quality photometry. However, O11 and V15 have different strengths (see the discussion in V15), and a considerable fraction of objects in our catalogue are not included in the V15 catalogue.…”

Section: Thermal Modellingmentioning

confidence: 99%

The AKARI IRC asteroid flux catalogue: updated diameters and albedos

Alí-Lagoa

Müller

Usui

et al. 2018

A&A

View full text Add to dashboard Cite

The AKARI IRC All-sky survey provided more than twenty thousand thermal infrared observations of over five thousand asteroids. Diameters and albedos were obtained by fitting an empirically calibrated version of the standard thermal model to these data. After the publication of the flux catalogue in October 2016, our aim here is to present the AKARI IRC all-sky survey data and discuss valuable scientific applications in the field of small body physical properties studies. As an example, we update the catalogue of asteroid diameters and albedos based on AKARI using the near-Earth asteroid thermal model (NEATM). We fit the NEATM to derive asteroid diameters and, whenever possible, infrared beaming parameters. We fit groups of observations taken for the same object at different epochs of the survey separately, so we compute more than one diameter for approximately half of the catalogue. We obtained a total of 8097 diameters and albedos for 5170 asteroids, and we fitted the beaming parameter for almost two thousand of them. When it was not possible to fit the beaming parameter, we used a straight line fit to our sample's beaming parameter-versus-phase angle plot to set the default value for each fit individually instead of using a single average value. Our diameters agree with stellar-occultation-based diameters well within the accuracy expected for the model. They also match the previous AKARI-based catalogue at phase angles lower than 50 degrees, but we find a systematic deviation at higher phase angles, at which near-Earth and Mars-crossing asteroids were observed. The AKARI IRC All-sky survey is an essential source of information about asteroids, especially the large ones, since, it provides observations at different observation geometries, rotational coverages and aspect angles. For example, by comparing in more detail a few asteroids for which dimensions were derived from occultations, we discuss how the multiple observations per object may already provide three-dimensional information about elongated objects even based on an idealised model like the NEATM. Finally, we enumerate additional expected applications for more complex models, especially in combination with other catalogues.

show abstract

“…We also assigned an uncertainty of 0.25 to these values. This is the observed scatter of MPC H values in this size range (see Table 3 of Pravec et al 2012).…”

Section: Debiased Datura-family Populationmentioning

confidence: 72%

“…First, we note that our accurate H for brighter Datura objects are systematically larger than the magnitude values reported by Minor Planet Center (MPC) by 0.34 ± 0.05. This is a well understood mismatch discussed by Pravec et al (2012). We assumed this correction applies also for fainter Datura members.…”

Section: Debiased Datura-family Populationmentioning

confidence: 95%

“…This accurate measurement of Datura's absolute magnitude helped us to improve its size and albedo measurements, D 8.2 km and p V 0.29, obtained during the post-cryogenic phase of the WISE spacecraft (see, Masiero et al 2012), who used an uncertain absolute magnitude value 12.5 from the Minor Planet Center (MPC) catalog. This problem has been thoroughly analyzed by Pravec et al (2012), who developed a correction procedure. Using their technique we find Datura's size of 8.17 km and its geometric albedo slightly lower, p V = 0.24.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The young Datura asteroid family

Vokrouhlický

Pravec

Ďurech

et al. 2017

A&A

View full text Add to dashboard Cite

Context. Asteroid families are the outcomes of disruption or cratering events on a size and energy scales that are not reproducible in laboratory experiments. Overall structure, as well as properties of individual members, in the old families could have been changed since their formation. Therefore young families preserve best the characteristics of the initial event. Aims. We study the most suitable known asteroid family with an age of less than 1 Myr, the Datura family. We aim (i) to obtain information about rotation state and shape of the largest members in the family; and (ii) to constrain its debiased population down to couple of hundreds of meters in size. Methods. We have analyzed the up-to-date catalog of orbital elements of main belt asteroids. We evaluated the detection efficiency of Catalina Sky Survey (CSS) in regard to detections of members in the Datura family, and we have used our photometric observations and lightcurve inversion methods to determine the rotation states and shapes of the largest members of the family. Results. We determined rotation periods of the seven largest members of the Datura family, and we also derived accurate mean absolute magnitudes for six of them. Except for the largest fragment (1270) Datura, the asteroids tend to have long rotation periods and large amplitude of the lightcurve, witnessing an elongated shape. For the four largest asteroids, our observations allow us to resolve rotation pole and a rough shape. All of them are prograde-rotating and have the latitude of the rotation pole >50 • . Our search in orbital catalogs resulted in the discovery of many small, sub-kilometer members of the Datura family. Using the CSS detection efficiency, we inverted this information into the debiased population of Datura family members. We show that the mass and angular momentum content in small fragments is negligible compared to the largest fragment (1270) Datura. These findings may help to constrain the formation mechanism of the family.

show abstract

Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations

Cited by 192 publications

References 34 publications

Spectral properties of the largest asteroids associated with Taurid Complex

Spectral properties of the largest asteroids associated with Taurid Complex

The AKARI IRC asteroid flux catalogue: updated diameters and albedos

The young Datura asteroid family

Contact Info

Product

Resources

About