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1. The fate of the interstellar medium in early-type galaxies. III. The mechanism of ISM removal and quenching of star formation

Author: Michałowski, Michał J., Gall, C., Hjorth, J., Frayer, D. T., Tsai, A. -L., Rowlands, K., Takeuchi, T. T., Leśniewska, A., Behrendt, D., Bourne, N., Hughes, D. H., Koprowski, M. P., Nadolny, J., Ryzhov, O., Solar, M., Spring, E., Zavala, J., and Bartczak, P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Understanding how galaxies quench their star formation is crucial for studies of galaxy evolution. Quenching is related to the cold gas decrease. In the first paper we showed that the dust removal timescale in early-type galaxies (ETGs) is about 2.5 Gyr. Here we present carbon monoxide (CO) and 21 cm hydrogen (H I) line observations of these galaxies and measure the timescale of removal of the cold interstellar medium (ISM). We find that all the cold ISM components (dust, molecular and atomic gas) decline at similar rates. This allows us to rule out a wide range of potential ISM removal mechanisms (including starburst-driven outflows, astration, a decline in the number of asymptotic giant branch stars), and artificial effects like stellar mass-age correlation, environmental influence, mergers, and selection bias, leaving ionization by evolved low-mass stars and ionization/outflows by supernovae Type Ia or active galactic nuclei as viable mechanisms. We also provide evidence for an internal origin of the detected ISM. Moreover, we find that the quenching of star formation in these galaxies cannot be explained by a reduction in gas amount alone, because the star formation rates (SFRs) decrease faster (on a timescale of about 1.8 Gyr) than the amount of cold gas. Furthermore, the star formation efficiency of the ETGs (SFE = SFR/MH2) is lower than that of star-forming galaxies, whereas their gas mass fractions (fH2 = MH2/M*) are normal. This may be explained by the stabilization of gas against fragmentation, for example due to morphological quenching, turbulence, or magnetic fields., Comment: Astrophysical Journal, published; 29 pages, 13 figures, 6 tables; V2: matched the published version and typos in the SFR and outflow equations fixed - no change in the conclusions
Published: 2024
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2. The Lockman-SpReSO project. Description, target selection, observations and preliminary results

Author: González-Otero, M., Padilla-Torres, C. P., Cepa, J., González, J. J., Bongiovanni, Á., García, A. M. Pérez, González-Serrano, J. I., Alfaro, E., Avila-Reese, V., Benítez, E., Binette, L., Cerviño, M., Cruz-González, I., de Diego, J. A., Gallego, J., Hernández-Toledo, H., Krongold, Y., Lara-López, M. A., Nadolny, J., Pérez-Martínez, R., Pović, M., Sánchez-Portal, M., Cedrés, B., Dultzin, D., Jiménez-Bailón, E., Martínez, R. Navarro, Negrete, C. A., Pintos-Castro, I., and Valenzuela, O.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Context. Extragalactic surveys are a key tool for better understanding the evolution of galaxies. Both deep and wide-field surveys serve to provide a clearer emerging picture of the physical processes that take place in and around galaxies, and to identify which of these processes are the most important in shaping the properties of galaxies. Aims. The Lockman Spectroscopic Redshift Survey using Osiris (Lockman-SpReSO) aims to provide one of the most complete optical spectroscopic follow-ups of the far-infrared (FIR) sources detected by the \textit{Herschel} Space Observatory in the Lockman Hole (LH) field. The optical spectroscopic study of the FIR-selected galaxies supplies valuable information about the relation between fundamental FIR and optical parameters, including extinction, star formation rate, and gas metallicity. In this article, we introduce and provide an in-depth description of the Lockman-SpReSO project and of its early results. Methods. We selected FIR sources from \textit{Herschel} observations of the central 24 arcmin $\times$ 24 arcmin of the LH field with an optical counterpart up to 24.5 $R_{\rm C}$(AB). The sample comprises 956 \textit{Herschel} FIR sources, plus 188 additional interesting objects in the field. These are point X-ray sources, cataclysmic variable star candidates, high-velocity halo star candidates, radio sources, very red quasi-stellar objects, and optical counterparts of sub-millimetre galaxies. The faint component of the catalogue ($R_{\rm C}(\mathrm{AB})\geq20$) was observed using the OSIRIS instrument on the 10.4 m Gran Telescopio Canarias in multi-object spectroscopy (MOS) mode. The bright component was observed using two multi-fibre spectrographs: the AF2-WYFFOS at the William Herschel Telescope and the HYDRA instrument at the WYIN telescope., Comment: 22 pages, 12 figures
Published: 2022
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3. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author: Marciniak, A., Ďurech, J., Alí-Lagoa, V., Ogłoza, W., Szakáts, R., Müller, T. G., Molnár, L., Pál, A., Monteiro, F., Arcoverde, P., Behrend, R., Benkhaldoun, Z., Bernasconi, L., Bosch, J., Brincat, S., Brunetto, L., Bąk, M. Butkiewicz, Del Freo, F., Duffard, R., Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, M., Geier, S., Golonka, J., Grice, J., Hirsch, R., Horbowicz, J., Jehin, E., Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kecskeméthy, V., Kim, D. -H., Kim, M. -J., Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, N., Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, E., Polakis, T., Richard, F., Rodrigues, T., Rondon, E., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., and Żukowski, K.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Results from the TESS mission showed that previous studies strngly underestimated the number of slow rotators, revealing the importance of studying those asteroids. For most slowly rotating asteroids (P > 12), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. The goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS. In addition to data in the visible range, we also use thermal data from infrared space observatories (IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model (CITPM). This novel method has so far been applied to only a few targets, and in this work we further validate the method. We present the models of 16 slow rotators. All provide good fits to both thermal and visible data. The obtained sizes are on average accurate at the 5% precision, with diameters in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 hours, and the thermal inertia covers a wide range of values, from 2 to <400 SI units, not showing any correlation with the period. With this work we increase the sample of slow rotators with reliable spin and shape models and known thermal inertia by 40%. The thermal inertia values of our sample do not display a previously suggested increasing trend with rotation period, which might be due to their small skin depth., Comment: Accepted to Astronomy & Astrophysics. 10 pages + appendices
Published: 2021
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4. MaNGA galaxies with off-centered spots of enhanced gas velocity dispersion

Author: Pilyugin, L. S., Cedres, B., Zinchenko, I. A., Garcia, A. M. Perez, Lara-Lopez, M. A., Nadolny, J., Nefedyev, Y. A., Gonzalez-Otero, M., Vilchez, J. M., Puertas, S. Duarte, and Martinez, R. Navarro
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Off-centered spots of the enhanced gas velocity dispersion, s, are revealed in some galaxies from the MaNGA survey. Aiming to clarify the origin of the spots of enhanced s, we examine the distributions of the surface brightness, the line-of-sight velocity, the oxygen abundance, the gas velocity dispersion, and the BPT spaxel classification in seven galaxies. We find that the enhanced s spots in six galaxies can be attributed to a (minor) interaction with a satellite. Three galaxies in our sample have a very close satellite. The spots of enhanced s in those galaxies are located at the edge of the galaxy close to the satellite. The spots of enhanced s in three other galaxies are related to bright spots in the photometric B band within the galaxy, which can be due to the projection of a satellite in the line of sight of the galaxy. The oxygen abundances in the spots in these three galaxies are reduced. This suggests that the low-metallicity gas from the satellite is mixed with the interstellar medium of the disk. The spectra of the spaxels within a spot are usually HII-region-like, suggesting that the interaction in those galaxies does not result in appreciable shocks. In contrast, the spot of the enhanced s in the galaxy M-8716-12703 is associated with an off-centered AGN-like radiation distribution. One can suggest that the spot of the enhanced s in the M-8716-12703 galaxy is different in origin, or that the characteristics of gas infall in this case differs from that in other galaxies., Comment: 25 pages, 22 figures, accepted to AA
Published: 2021
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5. (704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body

Author: Hanuš, J., Vernazza, P., Viikinkoski, M., Ferrais, M., Rambaux, N., Podlewska-Gaca, E., Drouard, A., Jorda, L., Jehin, E., Carry, B., Marsset, M., Marchis, F., Warner, B., Behrend, R., Asenjo, V., Berger, N., Bronikowska, M., Brothers, T., Charbonnel, S., Colazo, C., Coliac, J-F., Duffard, R., Jones, A., Leroy, A., Marciniak, A., Melia, R., Molina, D., Nadolny, J., Person, M., Pejcha, O., Riemis, H., Shappee, B., Sobkowiak, K., Soldán, F., Suys, D., Szakats, R., Vantomme, J., Birlan, M., Berthier, J., Bartczak, P., Dumas, C., Dudziński, G., Ďurech, J., Castillo-Rogez, J., Cipriani, F., Fetick, R., Fusco, T., Grice, J., Kaasalainen, M., Kryszczynska, A., Lamy, P., Michalowski, T., Michel, P., Santana-Ros, T., Tanga, P., Vachier, F., Vigan, A., Witasse, O., and Yang, B.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: With an estimated diameter in the 320 to 350 km range, (704) Interamnia is the fifth largest main belt asteroid and one of the few bodies that fills the gap in size between the four largest bodies with $D$ > 400 km (Ceres, Vesta, Pallas and Hygiea) and the numerous smaller bodies with $D$ $\lesssim$ 200 km. However, despite its large size, little is known about the shape and spin state of Interamnia and, therefore, about its bulk composition and past collisional evolution. We aimed to test at what size and mass the shape of a small body departs from a nearly ellipsoidal equilibrium shape (as observed in the case of the four largest asteroids) to an irregular shape as routinely observed in the case of smaller ($D$ $\lesssim$ 200 km) bodies. We observed Interamnia as part of our ESO VLT/SPHERE large program (ID: 199.C-0074) at thirteen different epochs. In addition, several new optical lightcurves were recorded. These data, along with stellar occultation data from the literature, were fed to the All-Data Asteroid Modeling (ADAM) algorithm to reconstruct the 3D-shape model of Interamnia and to determine its spin state. Interamnia's volume-equivalent diameter of 332 $\pm$ 6 km implies a bulk density of $\rho$=1.98 $\pm$ 0.68 gcm$^{-3}$ , which suggests that Interamnia - like Ceres and Hygiea - contains a high fraction of water ice, consistent with the paucity of apparent craters. Our observations reveal a shape that can be well approximated by an ellipsoid, and that is compatible with a fluid hydrostatic equilibrium at the 2 $\sigma$ level. The rather regular shape of Interamnia implies that the size and mass limit, under which the shapes of minor bodies with a high amount of water ice in the subsurface become irregular, has to be searched among smaller ($D$ $\lesssim$ 300km) less massive ($m$ $\lesssim$ 3x10$^{19}$ kg) bodies., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2019
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6. A new non-convex model of the binary asteroid (809) Lundia obtained with the SAGE modelling technique

Author: Bartczak, P., Kryszczyńska, A., Dudziński, G., Polińska, M., Colas, F., Vachier, F., Marciniak, A., Pollock, J., Apostolovska, G., Santana-Ros, T., Hirsch, R., Dimitrow, W., Murawiecka, M., Wietrzycka, P., and Nadolny, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present a new non-convex model of the binary asteroid (809) Lundia. A SAGE (Shaping Asteroids with Genetic Evolution) method using disc-integrated photometry only was used for deriving physical parameters of this binary system. The model of (809) Lundia improves former system's pole solution and gives the ecliptic coordinates of the orbit pole - $\lambda=122^{\circ}$, $\beta=22^{\circ}$, $\sigma=\pm5^{\circ}$ - and the orbital period of $15.41574 \pm 0.00001$ h. For scaling our results we used effective diameter of $D_{eff} = 9.6 \pm 1.1$ km obtained from Spitzer observations. The non-convex shape description of the components permitted a refined calculation of the components' volumes, leading to a density estimation of $2.5\pm0.2$ g/cm$^3$ and macroporosity of 13-23\%. The intermediate-scale features of the model may also offer new clues on the components' origin and evolution.
Published: 2019
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7. Against the biases in spins and shapes of asteroids

Author: Marciniak, A., Pilcher, F., Oszkiewicz, D., Santana-Ros, T., Urakawa, S., Fauvaud, S., Kankiewicz, P., Tychoniec, Ł., Fauvaud, M., Hirsch, R., Horbowicz, J., Kamiński, K., Konstanciak, I., Kosturkiewicz, E., Murawiecka, M., Nadolny, J., Nishiyama, K., Okumura, S., Polińska, M., Richard, F., Sakamoto, T., Sobkowiak, K., Stachowski, G., and Trela, P.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: 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 figures
Published: 2017
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8. Shape and spin determination of Barbarian asteroids

Author: Devogèle, M., Tanga, P., Bendjoya, P., Rivet, J. P., Surdej, J., Hanus, J., Abe, L., Antonini, P., Artola, R. A., Audejean, M., Behrend, R., Berski, F., Bosch, J. G., Bronikowska, M., Carbognani, A., Char, F., Kim, M. -J., Choi, Y. -J., Colazo, C. A., Coloma, J., Coward, D., Durkee, R., Erece, O., Forne, E., Hickson, P., Hirsch, R., Horbowicz, J., Kamiński, K., Kankiewicz, P., Kaplan, M., Kwiatkowski, T., Konstanciak, I., Kruszewki, A., Kudak, V., Manzini, F., Moon, H. -K., Marciniak, A., Murawiecka, M., Nadolny, J., Ogłoza, W., Ortiz, J. L, Oszkiewicz, D., Pallares, H., Peixinho, N., Poncy, R., Reyes, F., Reyes, J. A. de los, Santana-Ros, T., Sobkowiak, K., Pastor, S., Pilcher, F., Quiñones, M. C., Trela, P., and Vernet, D.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. The so-called Barbarian asteroids share peculiar, but common polarimetric properties, probably related to both their shape and composition. They are named after (234) Barbara, the first on which such properties were identified. As has been suggested, large scale topographic features could play a role in the polarimetric response, if the shapes of Barbarians are particularly irregular and present a variety of scattering/incidence angles. This idea is supported by the shape of (234) Barbara, that appears to be deeply excavated by wide concave areas revealed by photometry and stellar occultations. Aims. With these motivations, we started an observation campaign to characterise the shape and rotation properties of Small Main- Belt Asteroid Spectroscopic Survey (SMASS) type L and Ld asteroids. As many of them show long rotation periods, we activated a worldwide network of observers to obtain a dense temporal coverage. Methods. We used light-curve inversion technique in order to determine the sidereal rotation periods of 15 asteroids and the con- vergence to a stable shape and pole coordinates for 8 of them. By using available data from occultations, we are able to scale some shapes to an absolute size. We also study the rotation periods of our sample looking for confirmation of the suspected abundance of asteroids with long rotation periods. Results. Our results show that the shape models of our sample do not seem to have peculiar properties with respect to asteroids with similar size, while an excess of slow rotators is most probably confirmed.
Published: 2017
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9. The Fate of the Interstellar Medium in Early-type Galaxies. III. The Mechanism of Interstellar Medium Removal and the Quenching of Star Formation

Author: Michałowski, Michał J., Gall, C., Hjorth, J., Frayer, D. T., Tsai, A.-l., Rowlands, K., Takeuchi, T. T., Leśniewska, A., Behrendt, D., Bourne, N., Hughes, D. H., Koprowski, M. P., Nadolny, J., Ryzhov, O., Solar, M., Spring, E., Zavala, J., Bartczak, P., Michałowski, Michał J., Gall, C., Hjorth, J., Frayer, D. T., Tsai, A.-l., Rowlands, K., Takeuchi, T. T., Leśniewska, A., Behrendt, D., Bourne, N., Hughes, D. H., Koprowski, M. P., Nadolny, J., Ryzhov, O., Solar, M., Spring, E., Zavala, J., and Bartczak, P.
Published: 2024

10. The Fate of the Interstellar Medium in Early-type Galaxies. II. Observational Evidence for Morphological Quenching*

Author: Leśniewska, Aleksandra, primary, Michałowski, M. J., additional, Gall, C., additional, Hjorth, J., additional, Nadolny, J., additional, Ryzhov, O., additional, and Solar, M., additional
Published: 2023
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11. The Fate of the Interstellar Medium in Early-type Galaxies. II. Observational Evidence for Morphological Quenching*

Author: Leśniewska, Aleksandra, Michałowski, M. J., Gall, C., Hjorth, J., Nadolny, J., Ryzhov, O., Solar, M., Leśniewska, Aleksandra, Michałowski, M. J., Gall, C., Hjorth, J., Nadolny, J., Ryzhov, O., and Solar, M.
Published: 2023

12. Analysis of ice-nucleating particle concentrations measured with the PINE instrument: An automated workflow

Author: Buettner, N., Foesig, R., Vogel, F., Lacher, L., Bogert, P., Nadolny, J., and Moehler, O.
Abstract: The PINE (Portable Ice Nucleation Experiment) instrument is a mobile cloud chamber that allows for continuous and autonomous measurements of ice-nucleating particle (INP) concentrations. PINE simulates mixed-phase cloud formation upon air mass lifting by expanding the sampled air inside the chamber via pressure reduction. It is designed for INP monitoring in ambient air but can also be used for laboratory studies. By design, the automated cycle of sampling and expanding the air within about 5 minutes results in highly time-resolved INP data. This inevitably requires a standardized and automated procedure to process the data allowing direct comparisons between different instruments and measurement sites.We developed a software package for automated data analysis to complete PINE’s workflow. The software package processes the raw data to Level 1 (time series of INP concentrations) and to Level 2 (temperature spectra of INP concentrations) data, provides the results in standardized formats including suitable metadata, and creates overview plots. The package includes two special modules: (1) for the automated data quality control and flagging in compliance with community standards e.g. ACTRIS (Aerosol, Clouds and Trace Gases Research Infrastructure) and (2) to distinguish the target ice crystals from aerosol particles and cloud droplets detected by an optical particle counter (OPC).Using this software package we are able to process the data in near real-time and visualize the results in our PINE community portal. In total the portal already contains data of more than 1000 measurement days at six locations since 2020., The 28th IUGG General Assembly (IUGG2023) (Berlin 2023)
Published: 2023
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13. Development and validation of a new cloud simulation experiment for lab-based aerosol–cloud studies

Author: Vogel, F., primary, Lacher, L., additional, Nadolny, J., additional, Saathoff, H., additional, Leisner, T., additional, and Möhler, O., additional
Published: 2022
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14. The OTELO survey as a morphological probe. Last ten Gyr of galaxy evolution The mass–size relation up to z = 2

Author: Nadolny, J., Bongiovanni, Á., Cepa, J., Cerviño, M., Pérez García, A. M., Povic, M., Pérez Martínez, M., De Diego, J. A., Pintos Castro, I., Alfaro, Emilio J., Castañeda, H. O., Gallego, J., González, J. J., González Serrano, J. I., Lara López, M. A., Padilla Torres, C. P., Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Nadolny, J. [0000-0003-1440-9061], Ministerio de Economía y Competitividad (MINECO), Agencia Estatal de Investigación (AEI), National Research Council (NRC), and Ethiopian Space Science and Technology Institute (ESSTI)
Subjects: structure [Galaxies], fundamental parameters [Galaxies], Catalogs, evolution [Galaxies]
Abstract: The catalogue are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/647/A89 Context. The morphology of galaxies provide us with a unique tool for relating and understanding other physical properties and their changes over the course of cosmic time. It is only recently that we have been afforded access to a wealth of data for an unprecedented number galaxies thanks to large and deep surveys. Aims. We present the morphological catalogue of the OTELO survey galaxies detected with the Hubble Space Telescope (HST)-ACS F814W images. We explore various methods applied in previous works to separate early-type (ET) and late-type (LT) galaxies classified via spectral energy distribution (SED) fittings using galaxy templates. Together with this article, we are releasing a catalogue containing the main morphological parameters in the F606W and F814W bands derived for more than 8000 sources. Methods. The morphological analysis is based on the single-Sérsic profile fit. We used the GALAPAGOS2 software to provide multi-wavelength morphological parameters fitted simultaneously in two HST-ACS bands. The GALAPAGOS2 software detects, prepares guess values for GALFIT-M, and provides the best-fitting single-Sérsic model in both bands for each source. Stellar masses were estimated using synthetic rest-frame magnitudes recovered from SED fittings of galaxy templates. The morphological catalogue is complemented with concentration indexes from a separate SExtractor dual, high dynamical range mode. Results. A total of 8812 sources were successfully fitted with single-Sérsic profiles. The analysis of a carefully selected sample of ∼3000 sources up to zphot = 2 is presented in this work, of which 873 sources were not detected in previous studies. We found no statistical evidence for the evolution of the low-mass end of mass–size relation for ET and LT since z = 2. Furthermore, we found a good agreement for the median size evolution for ET and LT galaxies, for a given stellar mass, with the data from the literature. Compared to previous works on faint field galaxies, we found similarities regarding their rest-frame colours as well as the Sérsic and concentration indices. This work was supported by the project Evolution of Galaxies, of reference AYA2014-58861-C3-1-P and AYA2017-88007-C3-1-P, within the "Programa estatal de fomento de la investigacion cientifica y tecnica de excelencia del Plan Estatal de Investigacion Cientifica y Tecnica y de Innovacion (2013-2016)" of the "Agencia Estatal de Investigacion del Ministerio de Ciencia, Innovacion y Universidades", and co-financed by the FEDER "Fondo Europeo de Desarrollo Regional". APG, RPM and MSP was supported by AYA2017-88007-C3-2-P. APG and MC are also supported by the Spanish State Research Agency grant MDM-2017-0737 (Unidad de Excelencia Maria de Maeztu CAB). JAD is grateful for the support from the UNAM-DGAPA-PASPA 2019 program, and the kind hospitality of the IAC. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma. This paper made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/). This paper made use of the Wright (2006) cosmological calculator. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. M.A.L.L. is a DARK-Carlsberg Foundation Fellow (Semper Ardens project CF15-0384). MP acknowledges financial financial support from the Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Innovation and Technology (MInT), and of the Spanish MEC undergrant AYA2016-76682-C3-1-P and PID2019-106027GB-C41 and financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andaluca (SEV-2017-0709). Peerreview
Published: 2021

15. Nonsequential neural network for simultaneous, consistent classification, and photometric redshifts of OTELO galaxies

Author: de Diego, J. A., primary, Nadolny, J., additional, Bongiovanni, Á., additional, Cepa, J., additional, Lara-López, M. A., additional, Gallego, J., additional, Cerviño, M., additional, Sánchez-Portal, M., additional, Ignacio González-Serrano, J., additional, Alfaro, E. J., additional, Pović, M., additional, Pérez García, A. M., additional, Pérez Martínez, R., additional, Padilla Torres, C. P., additional, Cedrés, B., additional, García-Aguilar, D., additional, González, J. J., additional, González-Otero, M., additional, Navarro-Martínez, R., additional, and Pintos-Castro, I., additional
Published: 2021
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16. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author: Marciniak, A., primary, Ďurech, J., additional, Alí-Lagoa, V., additional, Ogłoza, W., additional, Szakáts, R., additional, Müller, T. G., additional, Molnár, L., additional, Pál, A., additional, Monteiro, F., additional, Arcoverde, P., additional, Behrend, R., additional, Benkhaldoun, Z., additional, Bernasconi, L., additional, Bosch, J., additional, Brincat, S., additional, Brunetto, L., additional, Butkiewicz - Bąk, M., additional, Del Freo, F., additional, Duffard, R., additional, Evangelista-Santana, M., additional, Farroni, G., additional, Fauvaud, S., additional, Fauvaud, M., additional, Ferrais, M., additional, Geier, S., additional, Golonka, J., additional, Grice, J., additional, Hirsch, R., additional, Horbowicz, J., additional, Jehin, E., additional, Julien, P., additional, Kalup, Cs., additional, Kamiński, K., additional, Kamińska, M. K., additional, Kankiewicz, P., additional, Kecskeméthy, V., additional, Kim, D.-H., additional, Kim, M.-J., additional, Konstanciak, I., additional, Krajewski, J., additional, Kudak, V., additional, Kulczak, P., additional, Kundera, T., additional, Lazzaro, D., additional, Manzini, F., additional, Medeiros, H., additional, Michimani-Garcia, J., additional, Morales, N., additional, Nadolny, J., additional, Oszkiewicz, D., additional, Pakštienė, E., additional, Pawłowski, M., additional, Perig, V., additional, Pilcher, F., additional, Pinel, P., additional, Podlewska-Gaca, E., additional, Polakis, T., additional, Richard, F., additional, Rodrigues, T., additional, Rondón, E., additional, Roy, R., additional, Sanabria, J. J., additional, Santana-Ros, T., additional, Skiff, B., additional, Skrzypek, J., additional, Sobkowiak, K., additional, Sonbas, E., additional, Stachowski, G., additional, Strajnic, J., additional, Trela, P., additional, Tychoniec, Ł., additional, Urakawa, S., additional, Verebelyi, E., additional, Wagrez, K., additional, Żejmo, M., additional, and Żukowski, K., additional
Published: 2021
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17. MaNGA galaxies with off-centered spots of enhanced gas velocity dispersion

Author: Pilyugin, L. S., primary, Cedrés, B., additional, Zinchenko, I. A., additional, Pérez Garcia, A. M., additional, Lara-López, M. A., additional, Nadolny, J., additional, Nefedyev, Y. A., additional, González-Otero, M., additional, Vílchez, J. M., additional, Duarte Puertas, S., additional, and Navarro Martinez, R., additional
Published: 2021
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18. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marciniak, Anna, Ďurech, Josef, Alí-Lagoa, Víctor, Ogłoza, W., Szakáts, Róbert, Müller, Thomas G., Molnár, László, Pál, András, Monteiro, F., Arcoverde, P., Behrend, Raoul, Benkhaldoun, Zouhair, Bernasconi, Laurent, Bosch, J., Brincat, S., Brunetto, L., Butkiewicz-Bąk, Magdalena, Del Freo, F., Duffard, René, Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, Marin, Geier, Stefan, Golonka, J., Grice, Jonny, Hirsch, R., Horbowicz, J., Jehin, Emmanuel, Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M.K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, Myung-Jin, Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, Nicolás, Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, Edyta, Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, René, Sanabria, J.J., Santana-Ros, Toni, Skiff, B., Skrzypek, J., Sobkowiak, Krzysztof, Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., Żukowski, K., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marciniak, Anna, Ďurech, Josef, Alí-Lagoa, Víctor, Ogłoza, W., Szakáts, Róbert, Müller, Thomas G., Molnár, László, Pál, András, Monteiro, F., Arcoverde, P., Behrend, Raoul, Benkhaldoun, Zouhair, Bernasconi, Laurent, Bosch, J., Brincat, S., Brunetto, L., Butkiewicz-Bąk, Magdalena, Del Freo, F., Duffard, René, Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, Marin, Geier, Stefan, Golonka, J., Grice, Jonny, Hirsch, R., Horbowicz, J., Jehin, Emmanuel, Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M.K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, Myung-Jin, Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, Nicolás, Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, Edyta, Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, René, Sanabria, J.J., Santana-Ros, Toni, Skiff, B., Skrzypek, J., Sobkowiak, Krzysztof, Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., and Żukowski, K.
Abstract: Context. Recent results for asteroid rotation periods from the TESS mission showed how strongly previous studies have underestimated the number of slow rotators, revealing the importance of studying those targets. For most slowly rotating asteroids (those with P > 12 h), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. Also, it is still unclear whether signatures of different surface material properties can be seen in thermal inertia determined from mid-infrared thermal flux fitting. Aims. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. Our goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Methods. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS spacecrafts. In addition to data in the visible range, we also use thermal data from infrared space observatories (mainly IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model. This novel method has so far been applied to only a few targets, and therefore in this work we further validate the method itself. Results. We present the models of 16 slow rotators, including two updated models. All provide good fits to both thermal and visible data.The obtained sizes are on average accurate at the 5% precision level, with diameters found to be in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 h, and the thermal inertia covers a wide range of values, from 2 to <400 J m−2 s−1∕2 K−1, not showing any correlation with the period. Conclusions. With this work we increase the sample of slow rotators with reliable spin and shape models and known thermal inertia by 40%. The thermal inertia values of our sample d
Published: 2021

19. The OTELO survey:Faint end of the luminosity function of [OII]3727 emitters at z=1.43

Author: Cedres, B., Bongiovanni, A., Cervino, M., Nadolny, J., Cepa, J., de Diego, J. A., Perez Garcia, A. M., Gallego, J., Lara-Lopez, M. A., Sanchez-Portal, M., Gonzalez-Serrano, J., Alfaro, E. J., Navarro Martinez, R., Perez Martinez, R., Gonzalez, J. J., Padilla Torres, C. P., Castaneda, H. O., Gonzalez, M., Cedres, B., Bongiovanni, A., Cervino, M., Nadolny, J., Cepa, J., de Diego, J. A., Perez Garcia, A. M., Gallego, J., Lara-Lopez, M. A., Sanchez-Portal, M., Gonzalez-Serrano, J., Alfaro, E. J., Navarro Martinez, R., Perez Martinez, R., Gonzalez, J. J., Padilla Torres, C. P., Castaneda, H. O., and Gonzalez, M.
Abstract: Aims. In this paper, we aim to study the main properties and luminosity function (LF) of the [OII]3727 emitters detected in the OTELO survey in order to characterise the star formation processes in low-mass galaxies at z similar to 1.43 and to constrain the faint-end of the LF.Methods. Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we present several relevant properties of the emitters and discuss the selection biases and uncertainties in the determination of the LF and the star formation rate density (SFRD).Results. We confirmed a total of 60 sources from a preliminary list of 332 candidates as [OII]3727 emitters. Approximately 93% of the emitters have masses in the range of 10(8)(*)) of the LF and explains the discrepancy of our results when compared with those obtained from surveys of much larger volumes. However, we are able to determine the faint-end slope of the LF, namely, alpha=-1.42 +/- 0.06, by sampling the LF down to similar to 1 dex lower than in previous works. We present our calculation of the SFRD of our sample and compare it to the value obtained in previous studies from the literature.
Published: 2021

20. Optical feedback cavity enhanced absorption spectroscopy: effective adjustment of the feedback-phase

Author: Habig, J. C., Nadolny, J., Meinen, J., Saathoff, H., and Leisner, T.
Published: 2012
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21. The OTELO survey

Author: Cedrés, B., primary, Bongiovanni, Á., additional, Cerviño, M., additional, Nadolny, J., additional, Cepa, J., additional, de Diego, J. A., additional, Pérez García, A. M., additional, Gallego, J., additional, Lara-López, M. A., additional, Sánchez-Portal, M., additional, González-Serrano, J. I., additional, Alfaro, E. J., additional, Navarro Martínez, R., additional, Pérez Martínez, R., additional, González, J. J., additional, Padilla Torres, C. P., additional, Castañeda, H. O., additional, and González, M., additional
Published: 2021
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22. (704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body

Author: Dudziński, G., Podlewska-Gaca, E., Bartczak, P., Benseguane, S, Ferrais, M., Jorda, L., Hanuš, J., Vernazza, P., Rambaux, N., Carry, B., Marchis, F., Marsset, M., Viikinkoski, M., Brož, M., Fetick, R., Drouard, A., Fusco, T., Birlan, M., Jehin, E., Berthier, J., Castillo-Rogez, J., Cipriani, F., Colas, F., Dumas, C., Kryszczynska, A., Lamy, P., Le Coroller, H, Marciniak, A., Michalowski, T., Michel, P., Santana-Ros, T., Tanga, P., Vachier, F., Vigan, A., Witasse, O., Yang, Bin, Ďurech, J., Kaasalainen, M., Le Coroller, H., Ševeček, P., Dudzinski, G., DeMeo, F., Durech, J., Grice, J., Gillon, M., Benkhaldoun, Z., Szakats, R., Hirsch, R., Duffard, R., Chapman, A., Maestre, J., Carbognani, Albino, Barghini, D., Gardiol, D., Martino, M. Di, Valsecchi, G., Trivero, P., Buzzoni, A., Rasetti, S., Selvestrel, D., Knapic, C., Londero, E., Zorba, S., Volpicelli, C., Carlo, M. Di, Vaubaillon, J., Marmo, C., Valeri, D., Zanotti, F., Morini, M., Demaria, P., Zanda, B., Bouley, S., Rault, J., Maquet, L., Warner, B., Behrend, R., Asenjo, V., Berger, N., Bronikowska, M., Brothers, T., Charbonnel, S., Colazo, C., Coliac, J.-F., Jones, A., Leroy, A., Melia, R., Molina, D., Nadolny, J., Person, M., Pejcha, O., Riemis, H., Shappee, B., Sobkowiak, K., Soldán, F., Suys, D., Vantomme, J., Ministry of Education, Youth and Sports (Czech Republic), European Commission, National Aeronautics and Space Administration (US), National Centre for Research and Development (Poland), National Research, Development and Innovation Office (Hungary), Hungarian Academy of Sciences, Université de Liège, Centre National de la Recherche Scientifique (France), Gordon and Betty Moore Foundation, National Science Foundation (US), The Ohio State University, Chinese Academy of Sciences, Villum Fonden, Astronomical Institute of Charles University, Charles University [Prague], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Tampere University of Technology [Tampere] (TUT), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Adam Mickiewicz University in Poznań (UAM), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Geneva Observatory, University of Geneva [Switzerland], Asociación Astronómica Astro Henares, Centro de Recursos Asociativos El Cerro, Institute of Geology [Poznan], Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Observatorio Astronómico de Córdoba (OAC), Universidad Nacional de Córdoba [Argentina], Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), Department of Geological Sciences [Bloomington], Indiana University [Bloomington], Indiana University System-Indiana University System, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Astronomical Observatory [Poznan], Observatorio Amanecer de Arrakis, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Laboratoire associé de Reconnaissance cellulaire et amélioration des plantes, Institut National de la Recherche Agronomique (INRA), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, European Space Research and Technology Centre (ESTEC), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Department of Mathematics [Tampere], Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Northeastern University [Shenyang], Charles University [Prague] (CU), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), SETI Institute, Center for Solar System Studies (CS3), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Observatoire de Durtal, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), L'Uranoscope de l'Ile de France, Observatoire de Gretz-Armainvilliers, Anunaki Observatory, Thirty Meter Telescope Observatory, NASA-California Institute of Technology (CALTECH), Agence Spatiale Européenne = European Space Agency (ESA), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Señal [Alicante] (DFESTS), Universidad de Alicante, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), European Southern Observatory [Santiago] (ESO), Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), and Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: asteroids, 010504 meteorology & atmospheric sciences, Dwarf planet, Irregular shape, Minor (linear algebra), FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Techniques: high angular resolution, photometric, Impact crater, Methods: observational, law, Física Aplicada, 0103 physical sciences, high angular resolutiontechniques, observational [Methods], individual, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, (704) Interamnia -methods, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Interamnia, photometric [Techniques], observational -techniques, Minor planets, Astronomy and Astrophysics, individual: (704) [Asteroids], Ellipsoid, high angular resolution [Techniques], Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], individual: (704) Interamnia [Minor planets, asteroids], Stellar occultation, Asteroids: individual: (704), Hydrostatic equilibrium, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract: Full list of authors: Hanuš, J.; Vernazza, P.; Viikinkoski, M.; Ferrais, M.; Rambaux, N.; Podlewska-Gaca, E.; Drouard, A.; Jorda, L.; Jehin, E.; Carry, B.; Marsset, M.; Marchis, F.; Warner, B.; Behrend, R.; Asenjo, V.; Berger, N.; Bronikowska, M.; Brothers, T.; Charbonnel, S.; Colazo, C. Coliac, J. -F.; Duffard, R.; Jones, A.; Leroy, A.; Marciniak, A.; Melia, R.; Molina, D.; Nadolny, J.; Person, M.; Pejcha, O.; Riemis, H.; Shappee, B.; Sobkowiak, K.; Soldán, F.; Suys, D.; Szakats, R.; Vantomme, J.; Birlan, M.; Berthier, J.; Bartczak, P.; Dumas, C.; Dudziński, G.; Ďurech, J.; Castillo-Rogez, J.; Cipriani, F.; Fetick, R.; Fusco, T.; Grice, J.; Kaasalainen, M.; Kryszczynska, A.; Lamy, P.; Michalowski, T.; Michel, P.; Santana-Ros, T.; Tanga, P.; Vachier, F.; Vigan, A.; Witasse, O.; Yang, B., With an estimated diameter in the 320 350 km range, (704) Interamnia is the fifth largest main belt asteroid and one of the few bodies that fills the gap in size between the four largest bodies with D >400 km (Ceres, Vesta, Pallas and Hygiea) and the numerous smaller bodies with diameter 200 km. However, despite its large size, little is known about the shape and spin state of Interamnia and, therefore, about its bulk composition and past collisional evolution. Aims. We aimed to test at what size and mass the shape of a small body departs from a nearly ellipsoidal equilibrium shape (as observed in the case of the four largest asteroids) to an irregular shape as routinely observed in the case of smaller (D 200 km) bodies. Methods. We observed Interamnia as part of our ESO VLT/SPHERE large program (ID: 199.C-0074) at thirteen different epochs. In addition, several new optical lightcurves were recorded. These data, along with stellar occultation data from the literature, were fed to the All-Data Asteroid Modeling algorithm to reconstruct the 3D-shape model of Interamnia and to determine its spin state. Results. Interamnia s volume-equivalent diameter of 332 6 km implies a bulk density of = 1.98 0.68 g cm3, which suggests that Interamnia like Ceres and Hygiea contains a high fraction of water ice, consistent with the paucity of apparent craters. Our observations reveal a shape that can be well approximated by an ellipsoid, and that is compatible with a fluid hydrostatic equilibrium at the 2 level. Conclusions. The rather regular shape of Interamnia implies that the size and mass limit, under which the shapes of minor bodies with a high amount of water ice in the subsurface become irregular, has to be searched among smaller (D 300 km) less massive (m 3 1019 kg) bodies. © 2020 EDP Sciences. All rights reserved., This work has been supported by the Czech Science Foundation through grant 18-09470S (J.H., J.D.) and by the Charles University Research program No. UNCE/SCI/023. This research was supported by INTER-EXCELLENCE grant LTAUSA18093 from the Czech Ministry of Education, Youth, and Sports (J.H. and O.P.). The research of O.P. is additionally supported by Horizon 2020 ERC Starting Grant "Cat-In-hAT" (grant agreement #803158) and award PRIMUS/SCI/17 from Charles University. P.V., A.D., and B.C. were supported by CNRS/INSU/PNP. M.M. was supported by the National Aeronautics and Space Administration under Grant No. 80NSSC18K0849 issued through the Planetary Astronomy Program. This work was supported by the National Science Centre, Poland, through grant no. 2014/13/D/ST9/01818 (A.M.). The research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378 (SBNAF). This project has been supported by the GINOP-2.3.2-15-2016-00003 and NKFIH K125015 grants of the Hungarian National Research, Development and Innovation Office (NKFIH) and by the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences. TRAPPIST-North is a project funded by the University of Liege, in collaboration with Cadi Ayyad University of Marrakech (Morocco). TRAPPIST-South is a project funded by the Belgian FNRS under grant FRFC 2.5.594.09. F.E.J. is a FNRS Senior Research Associate. ASAS-SN thanks the Las Cumbres Observatory and its staff for its continuing support of the ASAS-SN project. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University and NSF grant AST-1515927. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), the Villum Foundation, and George Skestos.
Published: 2020

23. (704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body

Author: Hanuš, J., primary, Vernazza, P., additional, Viikinkoski, M., additional, Ferrais, M., additional, Rambaux, N., additional, Podlewska-Gaca, E., additional, Drouard, A., additional, Jorda, L., additional, Jehin, E., additional, Carry, B., additional, Marsset, M., additional, Marchis, F., additional, Warner, B., additional, Behrend, R., additional, Asenjo, V., additional, Berger, N., additional, Bronikowska, M., additional, Brothers, T., additional, Charbonnel, S., additional, Colazo, C., additional, Coliac, J.-F., additional, Duffard, R., additional, Jones, A., additional, Leroy, A., additional, Marciniak, A., additional, Melia, R., additional, Molina, D., additional, Nadolny, J., additional, Person, M., additional, Pejcha, O., additional, Riemis, H., additional, Shappee, B., additional, Sobkowiak, K., additional, Soldán, F., additional, Suys, D., additional, Szakats, R., additional, Vantomme, J., additional, Birlan, M., additional, Berthier, J., additional, Bartczak, P., additional, Dumas, C., additional, Dudziński, G., additional, Ďurech, J., additional, Castillo-Rogez, J., additional, Cipriani, F., additional, Fetick, R., additional, Fusco, T., additional, Grice, J., additional, Kaasalainen, M., additional, Kryszczynska, A., additional, Lamy, P., additional, Michalowski, T., additional, Michel, P., additional, Santana-Ros, T., additional, Tanga, P., additional, Vachier, F., additional, Vigan, A., additional, Witasse, O., additional, and Yang, B., additional
Published: 2020
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24. A new non-convex model of the binary asteroid (809) Lundia obtained with the SAGE modelling technique

Author: Bartczak, P. (P.), Kryszczyńska, A. (A.), Dudziński, G. (G.), Polińska, M. (M.), Colas, F. (F.), Vachier, F. (F.), Marciniak, A. (A.), Pollock, J. (J.), Apostolovska, G. (G.), Santana-Ros, T. (T.), Hirsch, R. (R.), Dimitrow, W. (W.), Murawiecka, M. (M.), Wietrzycka, P. (P.), Nadolny, J. (J.), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), and Institut de Mécanique Céleste et de Calcul des Ephémérides [IMCCE]
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Space and Planetary Science, 0103 physical sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: We present a new non-convex model of the binary asteroid (809) Lundia. A SAGE (Shaping Asteroids with Genetic Evolution) method using disc-integrated photometry only was used for deriving physical parameters of this binary system. The model of (809) Lundia improves former system's pole solution and gives the ecliptic coordinates of the orbit pole - $\lambda=122^{\circ}$, $\beta=22^{\circ}$, $\sigma=\pm5^{\circ}$ - and the orbital period of $15.41574 \pm 0.00001$ h. For scaling our results we used effective diameter of $D_{eff} = 9.6 \pm 1.1$ km obtained from Spitzer observations. The non-convex shape description of the components permitted a refined calculation of the components' volumes, leading to a density estimation of $2.5\pm0.2$ g/cm$^3$ and macroporosity of 13-23\%. The intermediate-scale features of the model may also offer new clues on the components' origin and evolution.
Published: 2017

25. Simulating measurements for a cable radiation study

Author: Harms, P., Mittra, R., and Nadolny, J.
Subjects: Electromagnetic compatibility -- Models, Shielding (Electricity) -- Models, Numerical analysis -- Methods, Time-domain analysis -- Usage, Business, Computers, Electronics, Electronics and electrical industries
Abstract: Accurate numerical simulations are needed for analyzing and developing better electrical interconnects and electromagnetic compatibility (EMC) measurement systems. Numerical simulations enable one to predict the field behavior and compute voltages, currents, impedances and other parameters of interest for a given structure such as cable shielding. In this work, a numerical simulation is used to analyze measured data from a cable radiation study. The finite-difference time-domain (FDTD) and the method-of-moments-based Numerical Electromagnetics Code (NEC) are used to compute the total radiated power from the cable, and the results are shown to be in agreement with measured data. A numerical study is carried out in this paper to demonstrate the usefulness of the method at aiding the design of a measurement system without much additional experimental work.
Published: 1996

26. Shape and spin determination of Barbarian asteroids

Author: Natural Sciences and Engineering Research Council of Canada, European Commission, Fundação para a Ciência e a Tecnologia (Portugal), National Science Centre (Poland), Devogèle, M., Tanga, P., Bendjoya, P., Rivet, J.P., Surdej, J., Hanuš, J., Abe, L., Antonini, P., Artola, R.A., Audejean, M., Behrend, R., Berski, F., Bosch, J.G., Bronikowska, M., Carbognani, A., Char, F., Kim, M. J., Choi, Y.J., Colazo, C.A., Coloma, J., Coward, D., Durkee, R., Erece, O., Forne, E., Hickson, P., Hirsch, R., Horbowicz, J., Kamiński, K., Kankiewicz, P., Kaplan, M., Kwiatkowski, T., Konstanciak, I., Kruszewki, A., Kudak, V., Manzini, F., Moon, H.K., Marciniak, A., Murawiecka, M., Nadolny, J., Ogłoza, W., Ortiz, José Luis, Oszkiewicz, D., Pallares, H., Peixinho, N., Poncy, R., Reyes, F., de los Reyes, J.A., Santana-Ros, Toni, Sobkowiak, K., Pastor, S., Natural Sciences and Engineering Research Council of Canada, European Commission, Fundação para a Ciência e a Tecnologia (Portugal), National Science Centre (Poland), Devogèle, M., Tanga, P., Bendjoya, P., Rivet, J.P., Surdej, J., Hanuš, J., Abe, L., Antonini, P., Artola, R.A., Audejean, M., Behrend, R., Berski, F., Bosch, J.G., Bronikowska, M., Carbognani, A., Char, F., Kim, M. J., Choi, Y.J., Colazo, C.A., Coloma, J., Coward, D., Durkee, R., Erece, O., Forne, E., Hickson, P., Hirsch, R., Horbowicz, J., Kamiński, K., Kankiewicz, P., Kaplan, M., Kwiatkowski, T., Konstanciak, I., Kruszewki, A., Kudak, V., Manzini, F., Moon, H.K., Marciniak, A., Murawiecka, M., Nadolny, J., Ogłoza, W., Ortiz, José Luis, Oszkiewicz, D., Pallares, H., Peixinho, N., Poncy, R., Reyes, F., de los Reyes, J.A., Santana-Ros, Toni, Sobkowiak, K., and Pastor, S.
Abstract: Context. The so-called Barbarian asteroids share peculiar, but common polarimetric properties, probably related to both their shape and composition. They are named after (234) Barbara, the first on which such properties were identified. As has been suggested, large scale topographic features could play a role in the polarimetric response, if the shapes of Barbarians are particularly irregular and present a variety of scattering/incidence angles. This idea is supported by the shape of (234) Barbara, that appears to be deeply excavated by wide concave areas revealed by photometry and stellar occultations. Aims. With these motivations, we started an observation campaign to characterise the shape and rotation properties of Small Main-Belt Asteroid Spectroscopic Survey (SMASS) type L and Ld asteroids. As many of them show long rotation periods, we activated a worldwide network of observers to obtain a dense temporal coverage. Methods. We used light-curve inversion technique in order to determine the sidereal rotation periods of 15 asteroids and the convergence to a stable shape and pole coordinates for 8 of them. By using available data from occultations, we are able to scale some shapes to an absolute size. We also study the rotation periods of our sample looking for confirmation of the suspected abundance of asteroids with long rotation periods. Results. Our results show that the shape models of our sample do not seem to have peculiar properties with respect to asteroids with similar size, while an excess of slow rotators is most probably confirmed.© 2017 ESO.
Published: 2017

27. Shape and spin determination of Barbarian asteroids

Author: Devogèle, M., primary, Tanga, P., additional, Bendjoya, P., additional, Rivet, J. P., additional, Surdej, J., additional, Hanuš, J., additional, Abe, L., additional, Antonini, P., additional, Artola, R. A., additional, Audejean, M., additional, Behrend, R., additional, Berski, F., additional, Bosch, J. G., additional, Bronikowska, M., additional, Carbognani, A., additional, Char, F., additional, Kim, M.-J., additional, Choi, Y.-J., additional, Colazo, C. A., additional, Coloma, J., additional, Coward, D., additional, Durkee, R., additional, Erece, O., additional, Forne, E., additional, Hickson, P., additional, Hirsch, R., additional, Horbowicz, J., additional, Kamiński, K., additional, Kankiewicz, P., additional, Kaplan, M., additional, Kwiatkowski, T., additional, Konstanciak, I., additional, Kruszewki, A., additional, Kudak, V., additional, Manzini, F., additional, Moon, H.-K., additional, Marciniak, A., additional, Murawiecka, M., additional, Nadolny, J., additional, Ogłoza, W., additional, Ortiz, J. L., additional, Oszkiewicz, D., additional, Pallares, H., additional, Peixinho, N., additional, Poncy, R., additional, Reyes, F., additional, de los Reyes, J. A., additional, Santana-Ros, T., additional, Sobkowiak, K., additional, Pastor, S., additional, Pilcher, F., additional, Quiñones, M. C., additional, Trela, P., additional, and Vernet, D., additional
Published: 2017
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28. Dynamic art technological sources for contemporary works: the artist interview and the installation process

Author: Stigter, S., Dubois, H., Townsend, J.H., Nadolny, J., Eyb-Green, S., Kroustallis, S., Neven, S., and AHM (FGw)
Abstract: The artist interview has become an important resource for the conservation of contemporary art. The installation of an artwork in collaboration with the artist is an even more valuable research tool. However, as with the artist interview, it needs critical assessment, because first-hand information is gained but also co-constructed. Different ways of presenting the artwork can be explored in dialogue with the artist, as was experienced with Jan Dibbets’ conceptual and variable artwork 'All shadows that occurred to me in… are marked with tape' (1969) in the collection of the Kröller-Müller Museum.
Published: 2014

29. Against the biases in spins and shapes of asteroids

Author: Marciniak, A., primary, Pilcher, F., additional, Oszkiewicz, D., additional, Santana-Ros, T., additional, Urakawa, S., additional, Fauvaud, S., additional, Kankiewicz, P., additional, Tychoniec, Ł., additional, Fauvaud, M., additional, Hirsch, R., additional, Horbowicz, J., additional, Kamiński, K., additional, Konstanciak, I., additional, Kosturkiewicz, E., additional, Murawiecka, M., additional, Nadolny, J., additional, Nishiyama, K., additional, Okumura, S., additional, Polińska, M., additional, Richard, F., additional, Sakamoto, T., additional, Sobkowiak, K., additional, Stachowski, G., additional, and Trela, P., additional
Published: 2015
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30. 'To prepare white excellent...': reconstructions investigating the influence of washing, grinding and decanting of stack-process lead white on pigment composition and particle size

Author: Stols-Witlox, M., Megens, L., Carlyle, L., Eyb-Green, S., Townsend, J.H., Clarke, M., Nadolny, J., Kroustallis, S., and History of Arts
Published: 2012

31. Identifying 16th-century paints on silver using a contemporary manuscript

Author: Davidowitz, T., Beentjes, T., van Bennekom, J., Creange, S., Eyb-Green, S., Townsend, J.H., Clarke, M., Nadolny, J., Kroustallis, S., and History of Arts
Abstract: The BnF Ms. Fr. 640 manuscript, written by an anonymous French goldsmith at the end of the 16th century, can be found in the collection of the Bibliothèque nationale de France in Paris. It describes the process of producing metal life-casts in great detail, from the preparation of the moulds to applying the final decorative paint layers. While the practice of applying translucent paints, otherwise referred to as ‘cold enamels’, to a metal substrate has long been used as an alternative to traditional enamelling, the result is extremely vulnerable to damage and subsequent restorations. It is perhaps for this reason that no significant research has yet been published on this subject. The Merkel tablepiece by Wenzel Jamnitzer (currently in the collection of the Rijksmuseum, Amsterdam) appears to have a great deal of intact original paint, which provides a good basis for study. Using the paint recipes and methods in the manuscript as a guideline, analytical techniques including X-ray fluorescence, X-ray diffraction and gas chromatography with mass spectrometry, as well as polarised light microscopy and ultraviolet light, were used to identify the pigments and binders on the Merkel tablepiece.
Published: 2012

32. Hans Heysen’s art materials: an investigation into suppliers, knowledge and choice

Author: Dubois, H, Townsend, J, Nadolny, J, Eyb-Green, S, Kroustallis, S, Neven, S, TSE, NA, Heysen, R, Dubois, H, Townsend, J, Nadolny, J, Eyb-Green, S, Kroustallis, S, Neven, S, TSE, NA, and Heysen, R
Abstract: The Cedars, belonging to the estate of the renowned Australian landscape painter Hans Heysen (1877–1968), in the Adelaide Foothills, South Australia, was transformed into a museum in the early 1990s. Consisting of the artist’s home, studio and personal collections, it has provided a rich source for research into the artist’s sources of supplies, his technical knowledge and choices of material. During his lifetime, he maintained meticulous financial receipts, invoices and correspondence, and the collection includes his notebooks, trade directories and catalogues, and a significant study collection of related works and art materials. This evidence makes for a better understanding of Heysen’s technical practice, the making of his works of art and the merchandising, distribution and uptake of art materials in the British colony of South Australia. Previously, very little was known of the history of trading in art materials in Adelaide. The use of complementary written and object-based sources served to identify both patterns in Heysen’s purchases of artists’ materials and his preferred suppliers of materials. Between 1898 and 1918, there were no businesses trading exclusively in artists’ materials in South Australia, so Heysen bought materials through hardware and building suppliers, stationers and music sellers. Study of financial records along with exhibition catalogues and trade directories together with remaining artists‘ materials in Heysen studio confirmed the predominant presence of British manufactured artists’ materials that had been suspected. Suppliers advertising in exhibition catalogues indicate that Winsor & Newton was the principal brand of paints available in Adelaide.
Published: 2014

33. Optical feedback cavity enhanced absorption spectroscopy: effective adjustment of the feedback-phase

Author: Habig, J. C., primary, Nadolny, J., additional, Meinen, J., additional, Saathoff, H., additional, and Leisner, T., additional
Published: 2011
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34. EMI Design of Shielded Cable Assemblies.

Author: Nadolny, J.
Published: 2007
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35. Extracting CAD models for quantifying noise coupling between vias in PCB layouts.

Author: Luan, S., Fan, J., Liu, W., Xiao, F., Knighten, J., Smith, N., Alexander, R., Nadolny, J., Kami, Y., and Drewniak, J.
Published: 2002
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36. Electrical modeling of high speed interconnection links.

Author: De Geest, J., Sercu, S., and Nadolny, J.
Published: 2001
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37. d-Fructose-l-sorbose interconversions. Access to 5-thio-d-fructose and interaction with the d-fructose transporter, GLUT5

Author: Tatibouet, A., Lefoix, M., Nadolny, J., Martin, O. R., Rollin, P., Yang, J., and Holman, G. D.
Published: 2001
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38. (704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body

Author: Hanuš, J., Vernazza, P., Viikinkoski, M., Ferrais, M., Rambaux, N., Podlewska-Gaca, E., Drouard, A., Jorda, L., Jehin, E., Carry, B., Marsset, M., Marchis, F., Warner, B., Behrend, R., Asenjo, V., Berger, N., Bronikowska, M., Brothers, T., Charbonnel, S., Colazo, C., Coliac, J.-F., Duffard, R., Jones, A., Leroy, A., Marciniak, A., Melia, R., Molina, D., Nadolny, J., Person, M., Pejcha, O., Riemis, H., Shappee, B., Sobkowiak, K., Soldán, F., Suys, D., Szakats, R., Vantomme, J., Birlan, M., Berthier, J., Bartczak, P., Dumas, C., Dudziński, G., Ďurech, J., Castillo-Rogez, J., Cipriani, F., Fetick, R., Fusco, T., Grice, J., Kaasalainen, M., Kryszczynska, A., Lamy, P., Michalowski, T., Michel, P., Santana-Ros, T., Tanga, P., Vachier, F., Vigan, A., Witasse, O., Yang, B., Hanuš, J., Vernazza, P., Viikinkoski, M., Ferrais, M., Rambaux, N., Podlewska-Gaca, E., Drouard, A., Jorda, L., Jehin, E., Carry, B., Marsset, M., Marchis, F., Warner, B., Behrend, R., Asenjo, V., Berger, N., Bronikowska, M., Brothers, T., Charbonnel, S., Colazo, C., Coliac, J.-F., Duffard, R., Jones, A., Leroy, A., Marciniak, A., Melia, R., Molina, D., Nadolny, J., Person, M., Pejcha, O., Riemis, H., Shappee, B., Sobkowiak, K., Soldán, F., Suys, D., Szakats, R., Vantomme, J., Birlan, M., Berthier, J., Bartczak, P., Dumas, C., Dudziński, G., Ďurech, J., Castillo-Rogez, J., Cipriani, F., Fetick, R., Fusco, T., Grice, J., Kaasalainen, M., Kryszczynska, A., Lamy, P., Michalowski, T., Michel, P., Santana-Ros, T., Tanga, P., Vachier, F., Vigan, A., Witasse, O., and Yang, B.
Abstract: Context. With an estimated diameter in the 320–350 km range, (704) Interamnia is the fifth largest main belt asteroid and one of the few bodies that fills the gap in size between the four largest bodies with D > 400 km (Ceres, Vesta, Pallas and Hygiea) and the numerous smaller bodies with diameter ≤200 km. However, despite its large size, little is known about the shape and spin state of Interamnia and, therefore, about its bulk composition and past collisional evolution. Aims. We aimed to test at what size and mass the shape of a small body departs from a nearly ellipsoidal equilibrium shape (as observed in the case of the four largest asteroids) to an irregular shape as routinely observed in the case of smaller (D ≤ 200 km) bodies. Methods. We observed Interamnia as part of our ESO VLT/SPHERE large program (ID: 199.C-0074) at thirteen different epochs. In addition, several new optical lightcurves were recorded. These data, along with stellar occultation data from the literature, were fed to the All-Data Asteroid Modeling algorithm to reconstruct the 3D-shape model of Interamnia and to determine its spin state. Results. Interamnia’s volume-equivalent diameter of 332 ± 6 km implies a bulk density of ρ = 1.98 ± 0.68 g cm−3, which suggests that Interamnia – like Ceres and Hygiea – contains a high fraction of water ice, consistent with the paucity of apparent craters. Our observations reveal a shape that can be well approximated by an ellipsoid, and that is compatible with a fluid hydrostatic equilibrium at the 2σ level. Conclusions. The rather regular shape of Interamnia implies that the size and mass limit, under which the shapes of minor bodies with a high amount of water ice in the subsurface become irregular, has to be searched among smaller (D ≤ 300 km) less massive (m ≤ 3 × 1019 kg) bodies.

39. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author: Marciniak, A., Ďurech, J., Alí-Lagoa, V., Ogłoza, W., Szakáts, R., Müller, T. G., Molnár, L., Pál, A., Monteiro, F., Arcoverde, P., Behrend, R., Benkhaldoun, Z., Bernasconi, L., Bosch, J., Brincat, S., Brunetto, L., Butkiewicz - Bąk, M., Del Freo, F., Duffard, R., Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, M., Geier, S., Golonka, J., Grice, J., Hirsch, R., Horbowicz, J., Jehin, E., Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, M.-J., Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, N., Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, E., Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., Żukowski, K., Marciniak, A., Ďurech, J., Alí-Lagoa, V., Ogłoza, W., Szakáts, R., Müller, T. G., Molnár, L., Pál, A., Monteiro, F., Arcoverde, P., Behrend, R., Benkhaldoun, Z., Bernasconi, L., Bosch, J., Brincat, S., Brunetto, L., Butkiewicz - Bąk, M., Del Freo, F., Duffard, R., Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, M., Geier, S., Golonka, J., Grice, J., Hirsch, R., Horbowicz, J., Jehin, E., Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, M.-J., Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, N., Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, E., Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., and Żukowski, K.
Abstract: Context. Recent results for asteroid rotation periods from the TESS mission showed how strongly previous studies have underestimated the number of slow rotators, revealing the importance of studying those targets. For most slowly rotating asteroids (those with P > 12 h), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. Also, it is still unclear whether signatures of different surface material properties can be seen in thermal inertia determined from mid-infrared thermal flux fitting. Aims. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. Our goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Methods. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS spacecrafts. In addition to data in the visible range, we also use thermal data from infrared space observatories (mainly IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model. This novel method has so far been applied to only a few targets, and therefore in this work we further validate the method itself. Results. We present the models of 16 slow rotators, including two updated models. All provide good fits to both thermal and visible data.The obtained sizes are on average accurate at the 5% precision level, with diameters found to be in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 h, and the thermal inertia covers a wide range of values, from 2 to <400 J m−2 s−1∕2 K−1, not showing any correlation with the period. Conclusions. With this wor

40. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author: Marciniak, A., Ďurech, J., Alí-Lagoa, V., Ogłoza, W., Szakáts, R., Müller, T. G., Molnár, L., Pál, A., Monteiro, F., Arcoverde, P., Behrend, R., Benkhaldoun, Z., Bernasconi, L., Bosch, J., Brincat, S., Brunetto, L., Butkiewicz - Bąk, M., Del Freo, F., Duffard, R., Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, M., Geier, S., Golonka, J., Grice, J., Hirsch, R., Horbowicz, J., Jehin, E., Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, M.-J., Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, N., Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, E., Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., Żukowski, K., Marciniak, A., Ďurech, J., Alí-Lagoa, V., Ogłoza, W., Szakáts, R., Müller, T. G., Molnár, L., Pál, A., Monteiro, F., Arcoverde, P., Behrend, R., Benkhaldoun, Z., Bernasconi, L., Bosch, J., Brincat, S., Brunetto, L., Butkiewicz - Bąk, M., Del Freo, F., Duffard, R., Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, M., Geier, S., Golonka, J., Grice, J., Hirsch, R., Horbowicz, J., Jehin, E., Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, M.-J., Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, N., Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, E., Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., and Żukowski, K.
Abstract: Context. Recent results for asteroid rotation periods from the TESS mission showed how strongly previous studies have underestimated the number of slow rotators, revealing the importance of studying those targets. For most slowly rotating asteroids (those with P > 12 h), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. Also, it is still unclear whether signatures of different surface material properties can be seen in thermal inertia determined from mid-infrared thermal flux fitting. Aims. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. Our goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Methods. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS spacecrafts. In addition to data in the visible range, we also use thermal data from infrared space observatories (mainly IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model. This novel method has so far been applied to only a few targets, and therefore in this work we further validate the method itself. Results. We present the models of 16 slow rotators, including two updated models. All provide good fits to both thermal and visible data.The obtained sizes are on average accurate at the 5% precision level, with diameters found to be in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 h, and the thermal inertia covers a wide range of values, from 2 to <400 J m−2 s−1∕2 K−1, not showing any correlation with the period. Conclusions. With this wor

41. Extracting CAD models for quantifying noise coupling between vias in PCB layouts

Author: Luan, S., primary, Fan, J., additional, Liu, W., additional, Xiao, F., additional, Knighten, J., additional, Smith, N., additional, Alexander, R., additional, Nadolny, J., additional, Kami, Y., additional, and Drewniak, J., additional
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42. Electrical modeling of high speed interconnection links

Author: De Geest, J., primary, Sercu, S., additional, and Nadolny, J., additional
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43. Analyzing shielded connectors using feature transfer impedance

Author: Dunwoody, S., primary, Nadolny, J., additional, and Kelly, K., additional
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44. Anticipating EMI using transfer functions and signal integrity information.

Author: Chen Wang, Drewniak, J.L., and Nadolny, J.
Published: 2003
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45. Experimental and FDTD study of the EMI performance of an open-pin-field connector for modules-on-backplanes.

Author: Xiaoning Ye, Nadolny, J., Drewniak, J.L., DuBroff, R.E., VanDoren, T.P., and Hubing, T.H.
Published: 2000
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46. EMI associated with inter-board connection for module-on-backplane and stacked-card configurations.

Author: Ye, X., Nadolny, J., Drewniak, J.L., Hubing, T.H., Vaudoren, T.P., and DuBroff, D.E.
Published: 1999
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47. Analyzing shielded connectors using feature transfer impedance.

Author: Dunwoody, S., Nadolny, J., and Kelly, K.
Published: 1998
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48. The OTELO survey as a morphological probe. Last ten Gyr of galaxy evolution. The mass--size relation up to z=2

Author: Miguel Cerviño, Ricardo Pérez Martínez, Jordi Cepa, Emilio J. Alfaro, Jakub Nadolny, Héctor O. Castañeda, Irene Pintos-Castro, José A. de Diego, J. Jesús González, Maritza A. Lara-López, Miguel Sánchez-Portal, Mirjana Pović, Ana María Pérez García, Carmen P. Padilla Torres, Jesús Gallego, Ángel Bongiovanni, J. Ignacio González-Serrano, Universidad de Cantabria, Ministerio de Economía y Competitividad (España), European Commission, Agencia Estatal de Investigación (España), Carlsberg Foundation, Ministerio de Ciencia, Innovación y Universidades (España), Universidad Nacional Autónoma de México, Ministry of Science and Technology (Ethiopia), Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Nadolny, J. [0000-0003-1440-9061], Pérez Martínez, R. [0000-0002-9127-5522], González, J. J. [0000-0002-3724-1583], Povic, M. [0000-0002-9766-6110], Ministerio de Economía y Competitividad (MINECO), Agencia Estatal de Investigación (AEI), Centre National de la Recherche Scientifique (CNRS), National Research Council (NRC), and Ethiopian Space Science and Technology Institute (ESSTI)
Subjects: Astrofísica, Galaxies: fundamental parameters, Relation (database), Stellar mass, structure [Galaxies], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxies: structure, 0103 physical sciences, Range (statistics), Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Mode (statistics), Galaxies: evolution, Astronomy and Astrophysics, Catalogues, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Astronomía, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Morphological analysis, fundamental parameters [Galaxies], Spectral energy distribution, Catalogs
Abstract: [Context]: The morphology of galaxies provide us with a unique tool for relating and understanding other physical properties and their changes over the course of cosmic time. It is only recently that we have been afforded access to a wealth of data for an unprecedented number galaxies thanks to large and deep surveys. [Aims]: We present the morphological catalogue of the OTELO survey galaxies detected with the Hubble Space Telescope (HST)-ACS F814W images. We explore various methods applied in previous works to separate early-type (ET) and late-type (LT) galaxies classified via spectral energy distribution (SED) fittings using galaxy templates. Together with this article, we are releasing a catalogue containing the main morphological parameters in the F606W and F814W bands derived for more than 8000 sources. [Methods]: The morphological analysis is based on the single-Sérsic profile fit. We used the GALAPAGOS2 software to provide multi-wavelength morphological parameters fitted simultaneously in two HST-ACS bands. The GALAPAGOS2 software detects, prepares guess values for GALFIT-M, and provides the best-fitting single-Sérsic model in both bands for each source. Stellar masses were estimated using synthetic rest-frame magnitudes recovered from SED fittings of galaxy templates. The morphological catalogue is complemented with concentration indexes from a separate SExtractor dual, high dynamical range mode. [Results]: A total of 8812 sources were successfully fitted with single-Sérsic profiles. The analysis of a carefully selected sample of ∼3000 sources up to zphot = 2 is presented in this work, of which 873 sources were not detected in previous studies. We found no statistical evidence for the evolution of the low-mass end of mass-size relation for ET and LT since z = 2. Furthermore, we found a good agreement for the median size evolution for ET and LT galaxies, for a given stellar mass, with the data from the literature. Compared to previous works on faint field galaxies, we found similarities regarding their rest-frame colours as well as the Sérsic and concentration indices. ©, This work was supported by the project Evolution of Galaxies, of reference AYA2014-58861-C3-1-P and AYA2017-88007-C3-1-P, within the "Programa estatal de fomento de la investigacion cientifica y tecnica de excelencia del Plan Estatal de Investigacion Cientifica y Tecnica y de Innovacion (2013-2016)" of the "Agencia Estatal de Investigacion del Ministerio de Ciencia, Innovacion y Universidades", and co-financed by the FEDER "Fondo Europeo de Desarrollo Regional". APG, RPM and MSP was supported by AYA2017-88007-C3-2-P. APG and MC are also supported by the Spanish State Research Agency grant MDM-2017-0737 (Unidad de Excelencia Maria de Maeztu CAB). JAD is grateful for the support from the UNAM-DGAPA-PASPA 2019 program, and the kind hospitality of the IAC. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma. This paper made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/). This paper made use of the Wright (2006) cosmological calculator. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. M.A.L.L. is a DARK-Carlsberg Foundation Fellow (Semper Ardens project CF15-0384). MP acknowledges financial financial support from the Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Innovation and Technology (MInT), and of the Spanish MEC undergrant AYA2016-76682-C3-1-P and PID2019-106027GB-C41 and financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andaluca (SEV-2017-0709).
Published: 2021

49. The OTELO Survey: The Star Formation Rate Evolution of Low-mass Galaxies

Author: Ricardo Pérez-Martínez, Jakub Nadolny, B. Cedrés, Mauro González-Otero, José A. de Diego, Maritza A. Lara-López, J. Ignacio González-Serrano, Jesús Gallego, Carmen P. Padilla Torres, A. M. Pérez-García, Ángel Bongiovanni, Jordi Cepa, Rocío Navarro Martínez, Miguel Sánchez-Portal, Miguel Cerviño, J. Jesús González, Emilio J. Alfaro, Cedrés, B. [0000-0002-7382-6407], Gallego, J. [0000-0003-1439-7697], Nadolny, J. [0000-0003-1440-9061], Lara López, M. A. [0000-0001-7327-3489], Agence Nationale de la Recherche (ANR), Universidad de Cantabria, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, European Space Agency, Agence Nationale de la Recherche (France), and Agencia Estatal de Investigación (España)
Subjects: Astrofísica, Observational cosmology, Stellar mass, FOS: Physical sciences, Starburst galaxies, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, Number density, 010308 nuclear & particles physics, Star formation, Luminosity function, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Astronomía, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Low Mass
Abstract: We present the analysis of a sample of Hα, Hβ, and [O ii] emission line galaxies from the OTELO survey, with masses typically below and redshifts between z ∼ 0.4 and 1.43. We study the star formation rate, star formation rate density, and their number density and evolution with redshift. We obtain a robust estimate of the specific star formation rate - stellar mass relation based on the lowest-mass sample published so far. We also determine a flat trend of the star formation rate density (SFRD) and number density with redshift. Our results suggest a scenario of no evolution of the number density of galaxies, regardless of their masses, up to redshift z ∼ 1.4. This implies a gradual change of the relative importance of the star-forming processes, from high-mass galaxies to low-mass galaxies, with decreasing redshift. We also find little or no variation of the SFRD in the redshift range of 0.4 < z < 1.43., This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2014 - 58861 - C3 - 1 - P, AYA2014 - 58861 - C3 - 2 - P, AYA2014 - 58861 - C3 - 3 - P, AYA2013 - 46724 - P, AYA2017 - 88007 - C3 - 1 - P, AYA2017 - 88007 - C3 - 2, MDM - 2017 - 0737 (Unidad de Excelencia Maria de Maeztu, CAB). A.P.G. acknowledge support from ESA through the Faculty of the European Space Astronomy Centre (ESAC)-Funding reference ESAC_549/2019. E.J.A. acknowledges funding from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709) and from grant PGC2018-095049-B-C21. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. This study makes use of data from AEGIS, a multi-wavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA, and other telescopes and supported in part by the NSF, NASA, and the STFC. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This research was supported by a grant from the Agence Nationale de la Recherche ANR-07-BLAN-0228.
Published: 2021

50. Binary progenitor systems for Type Ic supernovae.

Author: Solar M, Michałowski MJ, Nadolny J, Galbany L, Hjorth J, Zapartas E, Sollerman J, Hunt L, Klose S, Koprowski M, Leśniewska A, Małkowski M, Nicuesa Guelbenzu AM, Ryzhov O, Savaglio S, Schady P, Schulze S, de Ugarte Postigo A, Vergani SD, Watson D, and Wróblewski R
Abstract: Core-collapse supernovae are explosions of massive stars at the end of their evolution. They are responsible for metal production and for halting star formation, having a significant impact on galaxy evolution. The details of these processes depend on the nature of supernova progenitors, but it is unclear if Type Ic supernovae (without hydrogen or helium lines in their spectra) originate from core-collapses of very massive stars (>30 M ⊙ ) or from less massive stars in binary systems. Here we show that Type II (with hydrogen lines) and Ic supernovae are located in environments with similar molecular gas densities, therefore their progenitors have comparable lifetimes and initial masses. This supports a binary interaction for most Type Ic supernova progenitors, which explains the lack of hydrogen and helium lines. This finding can be implemented in sub-grid prescriptions in numerical cosmological simulations to improve the feedback and chemical mixing., (© 2024. The Author(s).)
Published: 2024
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