PRELIMINARY ANALYSIS OF
                    <i>WISE</i>
                    /NEOWISE 3-BAND CRYOGENIC AND POST-CRYOGENIC OBSERVATIONS OF MAIN BELT ASTEROIDS

Masiero, J.; Mainzer, Amy; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; Cabrera, Mario S.

doi:10.1088/2041-8205/759/1/l8

Cited by 89 publications

(101 citation statements)

References 15 publications

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“…Since our photometric measurements were carefully calibrated in the Johnson-Cousins system, we obtained Datura's absolute magnitude in V band H = 12.65 ± 0.05, in a very good agreement with H = 12.61 ± 0.12 reported by Wisniewski et al (1997). 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.…”

Section: Introductionsupporting

confidence: 84%

The young Datura asteroid family

Vokrouhlický

Pravec

Ďurech

et al. 2017

A&A

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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.

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Section: Introductionsupporting

confidence: 84%

The young Datura asteroid family

Vokrouhlický

Pravec

Ďurech

et al. 2017

A&A

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“…This will convert ALMA into one of the most important sources of disk-resolved asteroid data, alongside adaptive-optics images and rangeDoppler radar echoes. Tedesco et al 2004;Millis et al 1981;Baier & Weigelt 1983;Drummond & Christou 2008;Ryan & Woodward 2010;Durech et al 2011;Usui et al 2011;Masiero et al 2012). We determine the average value here following the method by Carry et al (2012), by rejecting all the estimates that do not fall within one standard deviation of the average value, then by recomputing the average without these values.…”

Section: Discussionmentioning

confidence: 99%

VLT/SPHERE- and ALMA-based shape reconstruction of asteroid (3) Juno

Viikinkoski

Kaasalainen

Ďurech

et al. 2015

A&A

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We use the recently released Atacama Large Millimeter Array (ALMA) and VLT/SPHERE science verification data, together with earlier adaptive-optics images, stellar occultation, and lightcurve data to model the 3D shape and spin of the large asteroid (3) Juno with the all-data asteroid modelling (ADAM) procedure. These data set limits on the plausible range of shape models, yielding reconstructions suggesting that, despite its large size, Juno has sizable unrounded features moulded by non-gravitational processes such as impacts.

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“…The second difference is that the NEOWISE clusters stretch towards higher p V at lower sizes, which results in a negative slope that is not apparent in the AKARI catalogues. This could be partly due to the contribution of diameters derived from data taken during non-cryogenic phases of the mission and the default values of beaming parameter assumed, namely 1.0 (Masiero et al 2012) and 0.95 (Nugent et al 2015(Nugent et al , 2016. Those values are more representative of medium-sized and large objects (10 km < D < 100 km), whereas smaller bodies tend to require higher beaming parameters (all other variables of the model being equal; see the discussions by Alí-Lagoa et al 2016;Alí-Lagoa & Delbo' 2017).…”

Section: Comparison With U11/h13mentioning

confidence: 99%

The AKARI IRC asteroid flux catalogue: updated diameters and albedos

Alí-Lagoa

Müller

Usui

et al. 2018

A&A

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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.

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PRELIMINARY ANALYSIS OF WISE /NEOWISE 3-BAND CRYOGENIC AND POST-CRYOGENIC OBSERVATIONS OF MAIN BELT ASTEROIDS

Cited by 89 publications

References 15 publications

The young Datura asteroid family

The young Datura asteroid family

VLT/SPHERE- and ALMA-based shape reconstruction of asteroid (3) Juno

The AKARI IRC asteroid flux catalogue: updated diameters and albedos

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