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Dr. Rabus, Markus
Nombre de publicación
Dr. Rabus, Markus
Nombre completo
Rabus, Markus
Facultad
Email
mrabus@ucsc.cl
ORCID
4 results
Research Outputs
Now showing 1 - 4 of 4
- PublicationShape and spin state model of contact binary (388188) 2006 DP14 using combined radar and optical observations(Royal Astronomical Society, 2025)
; ;Cannon, Richard ;Rożek, Agata ;Brozović, Marina ;Pravec, Petr ;Snodgrass, Colin ;Busch, Michael ;Robinson, James ;Donaldson, Abbie ;Holc, Tanja ;Benner, Lance ;Naidu, Shantanu ;Kušnirák, Peter ;Gardener, Daniel ;Kučáková, Hana ;Khalouei, Elahe ;Pollock, Joseph ;Bonavita, Mariangela ;Fatka, Petr ;Hornoch, Kamil ;Sajadian, Sedighe ;Alegre, Lara ;Amadio, Flavia ;Andersen, Michael ;Bozza, Valerio ;Burgdorf, Martin ;Columba, Gabriele ;Dominik, Martin ;Figuera Jaimes, R. ;Hinse, Tobias ;Hundertmark, Markus ;Jørgensen, Uffe ;Longa-Peña, Penelope ;Peixinho, Nuno ;Rahvar, Sohrab ;Rota, Paolo ;Skottfelt, Jesper ;Southworth, JohnTregloan-Reed, JeremyContact binaries are found throughout the solar system. The recent discovery of Selam, the satellite of MBA (152830) Dinkinesh, by the NASA LUCY mission has made it clear that the term ‘contact binary’ covers a variety of different types of bi-modal mass distributions and formation mechanisms. Only by modelling more contact binaries can this population be properly understood. We determined a spin state and shape model for the Apollo group contact binary asteroid (388188) 2006 DP14 using ground-based optical and radar observations collected between 2014 and 2023. Radar delay-Doppler images and continuous wave spectra were collected over two days in February 2014, while 16 lightcurves in the Cousins R and SDSS-r filters were collected in 2014, 2022 and 2023. We modelled the spin state using convex inversion before using the SHAPE modelling software to include the radar observations in modelling concavities and the distinctive neck structure connecting the two lobes. We find a spin state with a period of (5.7860±0.0001) hours and pole solution of 𝜆 = (180±121)◦ and 𝛽 = (−80±7)◦ with morphology indicating a 520 m long bi-lobed shape. The model’s asymmetrical bi-modal mass distribution resembles other small NEA contact binaries such as (85990) 1999 JV6 or (8567) 1996 HW1, which also feature a smaller ‘head’ attached to a larger ‘body’. The final model features a crater on the larger lobe, similar to several other modelled contact binaries. The model’s resolution is 25 m, comparable to that of the radar images used. - PublicationStar-spot activity, orbital obliquity, transmission spectrum, physical properties, and transit time variations of the HATS-2 planetary system(EDP Sciences, 2024)
; ;Biagiotti, F. ;Mancini, L. ;Southworth, J. ;Tregloan-Reed, J. ;Naponiello, L. ;Jørgensen, U. ;Bach-Møller, N. ;Basilicata, M. ;Bonavita, M. ;Bozza, V. ;Burgdorf, M. ;Dominik, M. ;Figuera Jaimes, R. ;Henning, Th. ;Hinse, T. ;Hundertmark, M. ;Khalouei, E. ;Longa-Peña, P. ;Peixinho, N. ;Rahvar, S. ;Sajadian, S. ;Skottfelt, J. ;Snodgrass, C. ;Jongen, Y.Vignes, J.-PAims. Our aim in this paper is to refine the orbital and physical parameters of the HATS-2 planetary system and study transit timing variations and atmospheric composition thanks to transit observations that span more than 10 yr and that were collected using different instruments and pass-band filters. We also investigate the orbital alignment of the system by studying the anomalies in the transit light curves induced by starspots on the photosphere of the parent star. Methods. We analysed new transit events from both ground-based telescopes and NASA’s TESS mission. Anomalies were detected in most of the light curves and modelled as starspots occulted by the planet during transit events. We fitted the clean and symmetric light curves with the JKTEBOP code and those affected by anomalies with the PRISM+GEMC codes to simultaneously model the photometric parameters of the transits and the position, size, and contrast of each starspot. Results. We found consistency between the values we found for the physical and orbital parameters and those from the discovery paper and ATLAS9 stellar atmospherical models. We identified different sets of consecutive starspot-crossing events that temporally occurred in less than five days. Under the hypothesis that we are dealing with the same starspots, occulted twice by the planet during two consecutive transits, we estimated the rotational period of the parent star and, in turn the projected and the true orbital obliquity of the planet. We find that the system is well aligned. We identified the possible presence of transit timing variations in the system, which can be caused by tidal orbital decay, and we derived a low-resolution transmission spectrum. - PublicationAnother shipment of six short-period giant planets from TESS(Royal Astronomical Society., 2023)
;Joseph E. Rodriguez ;Samuel N. Quinn ;Andrew Vanderburg ;George Zhou ;Jason D. Eastman ;Erica Thygesen ;Bryson Cale ;David R. Ciardi ;Phillip A. Reed ;Ryan J. Oelkers ;Karen A. Collins ;Allyson Bieryla ;David W. Latham ;Erica J. Gonzales ;B. Scott Gaudi ;Coel Hellier ;Matias I. Jones ;Rafael Brahm ;Kirill Sokolovsky ;Jack Schulte ;Gregor Srdoc ;John Kielkopf ;Ferran Grau Horta ;Bob Massey ;Phil Evans ;Denise C. Stephens ;Kim K. McLeod ;Nikita Chazov ;Vadim Krushinsky ;Mourad Ghachoui ;Boris S. Safonov ;Cayla M. Dedrick ;Dennis Conti ;Didier Laloum ;Steven Giacalone ;Carl Ziegler ;Pere Guerra Serra ;Ramon Naves Nogues ;Felipe Murgas ;Edward J. Michaels ;George R. Ricke ;Roland K. Vanderspek ;Sara Seager ;Joshua N. Winn ;Jon M. Jenkins ;Brett Addison ;Owen Alfaro ;D. R. Anderson ;Elias Aydi ;Thomas G. Beatty ;Timothy R. Bedding ;Alexander A. Belinski ;Zouhair Benkhaldoun ;Perry Berlind ;Cullen H. Blake ;Michael J. Bowen ;Brendan P. Bowler ;Andrew W. Boyle ;Dalton Branson ;Cesar Briceño ;Michael L. Calkins ;Emma Campbell ;Jessie L. Christiansen ;Laura Chomiuk ;Kevin I. Collins ;Matthew A.Cornachione ;Ahmed Daassou ;Courtney D. Dressing ;Gilbert A. Esquerdo ;Dax L. Feliz ;William Fong ;Akihiko Fukui ;Tianjun Gan ;Holden Gill ;Maria V. Goliguzova ;Jarrod Hansen ;Thomas Henning ;Eric G. Hintz ;Melissa J. Hobson ;Jonathan Horner ;Chelsea X. Huang ;David J. James ;Jacob S. Jensen ;amson A. Johnson ;Andres Jordan Stephen R. Kane ;Khalid Barkaoui ;Myung-Jin Kim ;Kingsley Kim ;Rudolf B. Kuhn ;Nicholas Law ;Pablo Lewin ;Hui-Gen Liu ;Michael B. Lund ;Andrew W. Mann ;Nate McCrady ;Matthew W. Mengel ;Jessica Mink ;Lauren G. Murphy ;Norio Narita ;Patrick Newman ;Jack Okumura ;Hugh P. Osborn ;Martin Paegert ;Enric Palle ;Joshua Pepper ;Peter Plavchan ;Alexander A. Popov; ;Jessica Ranshaw ;Jennifer A. Rodriguez ;Dong-Goo Roh ;Michael A. Reefe ;Arjun B. Savel ;Richard P. Schwarz ;Avi Shporer ;Robert J. Siverd ;David H. Sliski ;Keivan G. Stassun ;Daniel J. Stevens ;Abderahmane Soubkiou ;Eric B. Ting ;C. G. Tinney ;Noah Vowell ;Payton Walton ;R. G. West ;Maurice L. Wilson ;Robert A. Wittenmyer ;Justin M. Wittrock ;Shania Wolf ;Jason T. Wright ;Hui ZhangEvan ZobelWe present the discovery and characterization of six short-period, transiting giant planets from NASA’s Transiting Exoplanet Survey Satellite (TESS) – TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642), TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), and TOI-2497 (TIC 97568467). All six planets orbit bright host stars (8.9 - PublicationPhysical properties of near-Earth asteroid (2102) Tantalus from multiwavelength observations(Monthly Notices of the Royal Astronomical Society, 2022)
;Rozek, Agata ;Lowry, Stephen C. ;Rozitis, Benjamin ;Dover, Lord R. ;Taylor, Patrick A. ;Virkki, Anne ;Green, Simon F. ;Snodgrass, Colin ;Fitzsimmons, Alan ;Campbell-White, Justyn ;Sajadian, Sedighe ;Bozza, Valerio ;Burgdorf, Martin J. ;Dominik, Martin ;Jaimes, R. Figuera ;Hinse, Tobias C. ;Hundertmark, Markus ;Jørgensen, Uffe G. ;Longa-Peña, Penélope; ;Rahvar, Sohrab ;Skottfelt, JesperSouthworth, JohnBetween 2010 and 2017, we have collected new optical and radar observations of the potentially hazardous asteroid (2102) Tantalus from the ESO NTT and Danish telescopes at the La Silla Observatory, and from the Arecibo planetary radar. The object appears to be nearly spherical, showing a low-amplitude light-curve variation and limited large-scale features in the radar images. The spin-state is difficult to constrain with the available data; including a certain light-curve subset significantly changes the spin-state estimates, and the uncertainties on period determination are significant. Constraining any change in rotation rate was not possible, despite decades of observations. The conv e x light curv e-inv ersion model, with rotational pole at λ = 210 ◦ ± 41 ◦ and β = −30 ◦ ± 35 ◦, is more flattened than the two models reconstructed by including radar observations: with prograde ( λ = 36 ◦ ± 23 ◦, β = 30 ◦ ± 15 ◦), and with retrograde rotation mode ( λ = 180 ◦ ± 24 ◦, β = −30 ± 16 ◦). Using data from WISE , we were able to determine that the prograde model produces the best agreement in size determination between radar and thermophysical modelling. Radar measurements indicate possible variation in surface properties, suggesting one side might have lower radar albedo and be rougher at the centimetre-to-decimetre scale than the other. However, further observations are needed to confirm this. Thermophysical analysis indicates a surface co v ered in fine-grained regolith, consistent with radar albedo, and polarisation ratio measurements. Finally, geophysical investigation of the spin-stability of Tantalus shows that it could be exceeding its critical spin-rate via cohesive forces.