Photometry and models of selected main belt asteroids

Marciniak, A.; Bartczak, P.; Santana-Ros, T.; Michałowski, Tadeusz; Antonini, P.; Behrend, R.; Bembrick, C.; Bernasconi, L.; Borczyk, W.; Colas, F.; Coloma, J. M.; Crippa, R.; Esseiva, N.; Fagas, M.; Fauvaud, M.; Fauvaud, S.; Ferreira, Desiree Della Monica; Bertelsen, R. P. Hein; Higgins, David; Hirsch, R.; Kajava, J. J. E.; Kamiński, K.; Kryszczyńska, A.; Kwiatkowski, T.; Manzini, F.; Michałowski, J.; Michalowski, Michal; Paschke, A.; Polińska, M.; Poncy, R.; Roy, R.; Santacana, G.; Sobkowiak, K.; Stasik, M.; Starczewski, S.; Velichko, F. P.; Wücher, H.; Zafar, T.

doi:10.1051/0004-6361/201219542

Cited by 28 publications

(12 citation statements)

References 31 publications

(28 reference statements)

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“…mff.cuni.cz/projects/damit/ (Ďurech et al 2010). (c) Available from the ISAM service http://isam.astro.amu.edu.pl (see Marciniak et al 2012, for details). (d) Downloaded from the Dawn Public Data site http://dawndata.igpp.ucla.edu/tw.jsp?section= geometry/ShapeModels flux densities and absolute calibration error bars compiled in the SBNAF thermal infrared database (IRDB).…”

Section: Datamentioning

confidence: 99%

Thermal properties of large main-belt asteroids observed byHerschelPACS

Alí-Lagoa

Müller

Kiss

et al. 2020

A&A

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Non-resolved thermal infrared observations enable studies of thermal and physical properties of asteroids via thermo-physical models provided the shape and rotational properties of the target are well determined. We used calibration-programme Herschel PACS data (70, 100, 160 μm) and state-of-the-art shape models derived from adaptive-optics observations and/or optical light curves to constrain for the first time the thermal inertia of twelve large main-belt asteroids. We also modelled previously well-characterised targets such as (1) Ceres or (4) Vesta as they constitute important benchmarks. Using the scale as a free parameter, most targets required a re-scaling ~5% consistent with what would be expected given the absolute calibration error bars. This constitutes a good cross-validation of the scaled shape models, although some targets required larger re-scaling to reproduce the IR data. We obtained low thermal inertias typical of large main belt asteroids studied before, which continues to give support to the notion that these surfaces are covered by fine-grained insulating regolith. Although the wavelengths at which PACS observed are longwards of the emission peak for main-belt asteroids, they proved to be extremely valuable to constrain size and thermal inertia and not too sensitive to surface roughness. Finally, we also propose a graphical approach to help examine how different values of the exponent used for scaling the thermal inertia as a function of heliocentric distance (i.e. temperature) affect our interpretation of the results.

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Section: Datamentioning

confidence: 99%

Thermal properties of large main-belt asteroids observed byHerschelPACS

Alí-Lagoa

Müller

Kiss

et al. 2020

A&A

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“…During more than fifteen years of station operation optimal observing and reduction procedures have been established and substantial experience has been gained both in asteroid photometry and modelling (see [24] for the description of the station and reduction procedures, and e.g. Marciniak et al [22] for lightcurves and models).…”

Section: Observing Campaignmentioning

confidence: 99%

Against the biases in spins and shapes of asteroids

Marciniak

Pilcher²,

Oszkiewicz

et al. 2015

Planetary and Space Science

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Physical studies of asteroids depend on an availability of lightcurve data. Targets that are easy to observe and analyse naturally have more data available, so their synodic periods are confirmed from multiple sources. Also, thanks to availability of data from a number of apparitions, their spin and shape models can often be obtained. Almost half of bright (H<=11 mag) main-belt asteroid population with known lightcurve parameters have rotation periods considered long (P>12 hours) and are rarely chosen for photometric observations. There is a similar selection effect against asteroids with low lightcurve amplitudes (a_max<=0.25 mag). As a result such targets, though numerous in this brightness range, are underrepresented in the sample of spin and shape modelled asteroids. In the range of fainter targets such effects are stronger. These selection effects can influence what is now known about asteroid spin vs. size distribution, on asteroid internal structure and densities and on spatial orientation of asteroid spin axes. To reduce both biases at the same time, we started a photometric survey of a substantial sample of those bright main-belt asteroids that displayed both features: periods longer than 12 hours, and amplitudes that did not exceed 0.25 magnitude. First we aim at finding synodic periods of rotation, and after a few observed apparitions, obtaining spin and shape models. As an initial result of our survey we found that a quarter of the studied sample (8 out of 34 targets) have rotation periods different from those widely accepted. We publish here these newly found period values with the lightcurves. The size/frequency plot might in reality look different in the long-period range. Further studies of asteroid spins, shapes, and structure should take into account serious biases that are present in the parameters available today.Comment: Published in Planetary and Space Science. 13 pages, 20 figure

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“…The model images shown in Figure 2 were obtained using the DAMIT online tool 21 (see also the Interactive Service for Asteroid Models 22 ; Marciniak et al 2012). This tool provides a prediction of the projected appearance of the asteroid on the sky as viewed from Earth in equatorial coordinate orientation at any observed Julian date.…”

Section: Comparison To Damit Shape Modelmentioning

confidence: 99%

The 2014 Alma Long Baseline Campaign: Observations of Asteroid 3 Juno at 60 Kilometer Resolution

Partnership¹,

Hunter

Kneißl

et al. 2015

ApJ

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We present Atacama Large Millimeter/submillimeter Array (ALMA) 1.3 mm continuum images of the asteroid 3 Juno obtained with an angular resolution of 0. 042 ″ (60 km at 1.97 AU). The data were obtained over a single 4.4 hr interval, which covers 60% of the 7.2 hr rotation period, approximately centered on local transit. A sequence of 10 consecutive images reveals continuous changes in the asteroidʼs profile and apparent shape, in good agreement with the sky projection of the three-dimensional model of the Database of Asteroid Models from Inversion Techniques. We measure a geometric mean diameter of 259 ± 4 km, in good agreement with past estimates from a variety of techniques and wavelengths. Due to the viewing angle and inclination of the rotational pole, the southern hemisphere dominates all of the images. The median peak brightness temperature is 215 ± 13 K, while the median over the whole surface is 197 ± 15 K. With the unprecedented resolution of ALMA, we find that the brightness temperature varies across the surface with higher values correlated to the subsolar point and afternoon areas and lower values beyond the evening terminator. The dominance of the subsolar point is accentuated in the final four images, suggesting a reduction in the thermal inertia of the regolith at the corresponding longitudes, which are possibly correlated to the location of the putative large impact crater. These results demonstrate ALMAʼs potential to resolve thermal emission from the surface of main belt asteroids and to measure accurately their position, geometric shape, rotational period, and soil characteristics.

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Photometry and models of selected main belt asteroids

Cited by 28 publications

References 31 publications

Thermal properties of large main-belt asteroids observed byHerschelPACS

Thermal properties of large main-belt asteroids observed byHerschelPACS

Against the biases in spins and shapes of asteroids

The 2014 Alma Long Baseline Campaign: Observations of Asteroid 3 Juno at 60 Kilometer Resolution

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