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1. CRIRES$^{+}$ on sky at the ESO Very Large Telescope

Author: Dorn, R. J., Bristow, P., Smoker, J. V., Rodler, F., Lavail, A., Accardo, M., Ancker, M. van den, Baade, D., Baruffolo, A., Courtney-Barrer, B., Blanco, L., Brucalassi, A., Cumani, C., Follert, R., Haimerl, A., Hatzes, A., Haug, M., Heiter, U., Hinterschuster, R., Hubin, N., Ives, D. J., Jung, Y., Jones, M., Kirchbauer, J-P., Klein, B., Kochukhov, O., Korhonen, H. H., Köhler, J., Lizon, J-L., Moins, C., Molina-Conde, I., Marquart, T., Neeser, M., Oliva, E., Pallanca, L., Pasquini, L., Paufique, J., Piskunov, N., Reiners, A., Schneller, D., Schmutzer, R., Seemann, U., Slumstrup, D., Smette, A., Stegmeier, J., Stempels, E., Tordo, S., Valenti, E., Valenzuela, J. J., Vernet, J., Vinther, J., and Wehrhahn, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The CRyogenic InfraRed Echelle Spectrograph (CRIRES) Upgrade project CRIRES$^{+}$ extended the capabilities of CRIRES. It transformed this VLT instrument into a cross-dispersed spectrograph to increase the wavelength range that is covered simultaneously by up to a factor of ten. In addition, a new detector focal plane array of three Hawaii 2RG detectors with a 5.3 $\mu$m cutoff wavelength replaced the existing detectors. Amongst many other improvements, a new spectropolarimetric unit was added and the calibration system has been enhanced. The instrument was installed at the VLT on Unit Telescope 3 at the beginning of 2020 and successfully commissioned and verified for science operations during 2021, partly remotely from Europe due to the COVID-19 pandemic. The instrument was subsequently offered to the community from October 2021 onwards. This article describes the performance and capabilities of the upgraded instrument and presents on sky results., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2023
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2. MATISSE, the VLTI mid-infrared imaging spectro-interferometer

Author: Lopez, B., Lagarde, S., Petrov, R. G., Jaffe, W., Antonelli, P., Allouche, F., Berio, P., Matter, A., Meilland, A., Millour, F., Robbe-Dubois, S., Henning, Th., Weigelt, G., Glindemann, A., Agocs, T., Bailet, Ch., Beckmann, U., Bettonvil, F., van Boekel, R., Bourget, P., Bresson, Y., Bristow, P., Cruzalèbes, P., Eldswijk, E., Caujolle, Y. Fanteï, Herrera, J. C. González, Graser, U., Guajardo, P., Heininger, M., Hofmann, K. -H., Kroes, G., Laun, W., Lehmitz, M., Leinert, C., Meisenheimer, K., Morel, S., Neumann, U., Paladini, C., Percheron, I., Riquelme, M., Schoeller, M., Stee, Ph., Venema, L., Woillez, J., Zins, G., Ábrahám, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Alonso, J., Augereau, J. -C., Böhm, A., Bazin, G., Beltran, J., Bensberg, A., Boland, W., Brast, R., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J. -M., Connot, C., Conzelmann, R. D., Danchi, W. -C., Delbo, M., Drevon, J., Dominik, C., van Duin, A., Ebert, M., Eisenhauer, F., Flament, S., Frahm, R., Rosas, V. Gámez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Glazenborg, A., Gonté, F. Y. J., Guitton, F., de Haan, M., Hanenburg, H., Haubois, X., Hocdé, V., Hogerheijde, M., ter Horst, R., Hron, J., Hummel, C. A., Hubin, N., Huerta, R., Idserda, J., Isbell, J. W., Ives, D., Jakob, G., Jaskó, A., Jochum, L., Klarmann, L., Klein, R., Kragt, J., Kuindersma, S., Kokoulina, E., Labadie, L., Lacour, S., Leftley, J., Poole, R. Le, Lizon, J. -L., Lopez, M., Mérand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Menut, J. L., Mohr, L., Mosoni, L., Navarro, R., Nussbaum, E., Pallanca, L., Pantin, E., Pasquini, L., Duc, T. Phan, Pott, J. -U., Pozna, E., Richichi, A., Ridinger, A., Rigal, F., Rivinius, Th., Roelfsema, R., Rohloff, R. -R., Rousseau, S., Salabert, D., Schertl, D., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., Toledo, P., Tristram, K., Tromp, N., Vakili, F., Varga, J., Vinther, J., Waters, L. B. F. M., Wittkowski, M., Wolf, S., Wrhel, F., and Yoffe, G.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Context:Optical interferometry is at a key development stage. ESO's VLTI has established a stable, robust infrastructure for long-baseline interferometry for general astronomical observers. The present second-generation instruments offer a wide wavelength coverage and improved performance. Their sensitivity and measurement accuracy lead to data and images of high reliability. Aims:We have developed MATISSE, the Multi AperTure mid-Infrared SpectroScopic Experiment, to access high resolution imaging in a wide spectral domain and explore topics such: stellar activity and mass loss; planet formation and evolution in the gas and dust disks around young stars; accretion processes around super massive black holes in AGN. Methods:The instrument is a spectro-interferometric imager covering three atmospheric bands (L,M,N) from 2.8 to 13.0 mu, combining four optical beams from the VLTI's telscopes. Its concept, related observing procedure, data reduction and calibration approach are the product of 30 years of instrumental research. The instrument utilizes a multi-axial beam combination that delivers spectrally dispersed fringes. The signal provides the following quantities at several spectral resolutions: photometric flux, coherent fluxes, visibilities, closure phases, wavelength differential visibilities and phases, and aperture-synthesis imaging. Results:We provide an overview of the physical principle of the instrument and its functionalities, the characteristics of the delivered signal, a description of the observing modes and of their performance limits. An ensemble of data and reconstructed images are illustrating the first acquired key observations. Conclusion:The instrument has been in operation at Cerro Paranal, ESO, Chile since 2018, and has been open for science use by the international community since April 2019. The first scientific results are being published now., Comment: 24 pages, 26 figures, submitted to Astronomy & Astrophysics
Published: 2021
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3. COSMOS2020: A panchromatic view of the Universe to $z\sim10$ from two complementary catalogs

Author: Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J. R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P. U., Gould, K. M. L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Fevre, O. Le, Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Sneppen, A., Smolcic, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W. -H., and Zamorani, G.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data has been collected in the COSMOS field. This paper describes the collection, processing, and analysis of this new imaging data to produce a new reference photometric redshift catalog. Source detection and multi-wavelength photometry is performed for 1.7 million sources across the $2\,\mathrm{deg}^{2}$ of the COSMOS field, $\sim$966,000 of which are measured with all available broad-band data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The $i<21$ sources have sub-percent photometric redshift accuracy and even the faintest sources at $25
Published: 2021
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4. Mid-infrared circumstellar emission of the long-period Cepheid l Carinae resolved with VLTI/MATISSE

Author: Hocdé, V., Nardetto, N., Matter, A., Lagadec, E., Mérand, A., Cruzalèbes, P., Meilland, A., Millour, F., Lopez, B., Berio, P., Weigelt, G., Petrov, R., Isbell, J. W., Jaffe, W., Kervella, P., Glindemann, A., Schöller, M., Allouche, F., Gallenne, A., de Souza, A. Domiciano, Niccolini, G., Kokoulina, E., Varga, J., Lagarde, S., Augereau, J. -C., van Boekel, R., Bristow, P., Henning, Th., Hofmann, K. -H., Zins, G., Danchi, W. -C., Delbo, M., Dominik, C., Rosas, V. Gámez, Klarmann, L., Hron, J., Hogerheijde, M. R., Meisenheimer, K., Pantin, E., Paladini, C., Robbe-Dubois, S., Schertl, D., Stee, P., Waters, R., Lehmitz, M., Bettonvil, F., Heininger, M., Woillez, J., Wolf, S., Yoffe, G., Szabados, L., Chiavassa, A., Borgniet, S., Breuval, L., Javanmardi, B., Ábrahám, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Agócs, T., Alonso, J., Antonelli, P., Böhm, A., Bailet, C., Bazin, G., Beckmann, U., Beltran, J., Boland, W., Bourget, P., Brast, R., Bresson, Y., Burtscher, L., Buter, R., Castillo, R., Chelli, A., Cid, C., Clausse, J. -M., Connot, C., Conzelmann, R. D., De Haan, M., Ebert, M., Elswijk, E., Fantei, Y., Frahm, R., Gabasch, A., Garces, E., Girard, P., Glazenborg, A., Gonté, F. Y. J., Herrera, J. C. González, Graser, U., Guajardo, P., Guitton, F., Hanenburg, H., Haubois, X., Hubin, N., Huerta, R., Idserda, J., Ives, D., Jakob, G., Jaskó, A., Jochum, L., Klein, R., Kragt, J., Kroes, G., Kuindersma, S., Labadie, L., Laun, W., Poole, R. Le, Leinert, C., Lizon, J. -L., Lopez, M., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Mohr, L., Morel, S., Mosoni, L., Navarro, R., Neumann, U., Nußbaum, E., Pallanca, L., Pasquini, L., Percheron, I., Duc, T. Phan, Pott, J. -U., Pozna, E., Ridinger, A., Rigal, F., Riquelme, M., Rivinius, Th., Roelfsema, R., Rohloff, R. -R., Rousseau, S., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., ter Horst, R., Tromp, N., Vakili, F., van Duin, A., Venema, L. B., Vinther, J., Wittkowski, M., and Wrhel, F.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: The nature of circumstellar envelopes (CSE) around Cepheids is still a matter of debate. The physical origin of their infrared (IR) excess could be either a shell of ionized gas, or a dust envelope, or both. This study aims at constraining the geometry and the IR excess of the environment of the long-period Cepheid $\ell$ Car (P=35.5 days) at mid-IR wavelengths to understand its physical nature. We first use photometric observations in various bands and Spitzer Space Telescope spectroscopy to constrain the IR excess of $\ell$ Car. Then, we analyze the VLTI/MATISSE measurements at a specific phase of observation, in order to determine the flux contribution, the size and shape of the environment of the star in the L band. We finally test the hypothesis of a shell of ionized gas in order to model the IR excess. We report the first detection in the L band of a centro-symmetric extended emission around l Car, of about 1.7$R_\star$ in FWHM, producing an excess of about 7.0\% in this band. In the N band, there is no clear evidence for dust emission from VLTI/MATISSE correlated flux and Spitzer data. On the other side, the modeled shell of ionized gas implies a more compact CSE ($1.13\pm0.02\,R_\star$) and fainter (IR excess of 1\% in the L band). We provide new evidences for a compact CSE of $\ell$ Car and we demonstrate the capabilities of VLTI/MATISSE for determining common properties of CSEs. While the compact CSE of $\ell$ Car is probably of gaseous nature, the tested model of a shell of ionized gas is not able to simultaneously reproduce the IR excess and the interferometric observations. Further Galactic Cepheids observations with VLTI/MATISSE are necessary for determining the properties of CSEs, which may also depend on both the pulsation period and the evolutionary state of the stars., Comment: 13 pages, 8 figures, accepted in Astronomy and Astrophysics
Published: 2021
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5. The asymmetric inner disk of the Herbig Ae star HD 163296 in the eyes of VLTI/MATISSE: evidence for a vortex?

Author: Varga, J., Hogerheijde, M., van Boekel, R., Klarmann, L., Petrov, R., Waters, L. B. F. M., Lagarde, S., Pantin, E., Berio, Ph., Weigelt, G., Robbe-Dubois, S., Lopez, B., Millour, F., Augereau, J. -C., Meheut, H., Meilland, A., Henning, Th., Jaffe, W., Bettonvil, F., Bristow, P., Hofmann, K. -H., Matter, A., Zins, G., Wolf, S., Allouche, F., Donnan, F., Schertl, D., Dominik, C., Heininger, M., Lehmitz, M., Cruzalèbes, P., Glindemann, A., Meisenheimer, K., Paladini, C., Schöller, M., Woillez, J., Venema, L., Kokoulina, E., Yoffe, G., Ábrahám, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Agócs, T., Antonelli, P., Böhm, A., Bailet, C., Bazin, G., Beckmann, U., Beltran, J., Boland, W., Bourget, P., Brast, R., Bresson, Y., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J. -M., Connot, C., Conzelmann, R. D., Danchi, W. -C., De Haan, M., Delbo, M., Ebert, M., Elswijk, E., Fantei, Y., Frahm, R., Rosas, V. Gámez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Gonté, F. Y. J., Herrera, J. C. González, Graser, U., Guajardo, P., Guitton, F., Haubois, X., Hron, J., Hubin, N., Huerta, R., Isbell, J. W., Ives, D., Jakob, G., Jaskó, A., Jochum, L., Klein, R., Kragt, J., Kroes, G., Kuindersma, S., Labadie, L., Laun, W., Poole, R. Le, Leinert, C., Lizon, J. -L., Lopez, M., Mérand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Mohr, L., Morel, S., Mosoni, L., Navarro, R., Neumann, U., Nußbaum, E., Pallanca, L., Pasquini, L., Percheron, I., Pott, J. -U., Pozna, E., Ridinger, A., Rigal, F., Riquelme, M., Rivinius, Th., Roelfsema, R., Rohloff, R. -R., Rousseau, S., Schuhler, N., Schuil, M., Soulain, A., Stee, P., Stephan, C., ter Horst, R., Tromp, N., Vakili, F., van Duin, A., Vinther, J., Wittkowski, M., and Wrhel, F.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. The inner few au region of planet-forming disks is a complex environment. High angular resolution observations have a key role in understanding the disk structure and the dynamical processes at work. Aims. In this study we aim to characterize the mid-infrared brightness distribution of the inner disk of the young intermediate-mass star HD 163296, from VLTI/MATISSE observations. Methods. We use geometric models to fit the data. Our models include a smoothed ring, a flat disk with inner cavity, and a 2D Gaussian. The models can account for disk inclination and for azimuthal asymmetries as well. We also perform numerical hydro-dynamical simulations of the inner edge of the disk. Results. Our modeling reveals a significant brightness asymmetry in the L-band disk emission. The brightness maximum of the asymmetry is located at the NW part of the disk image, nearly at the position angle of the semimajor axis. The surface brightness ratio in the azimuthal variation is $3.5 \pm 0.2$. Comparing our result on the location of the asymmetry with other interferometric measurements, we confirm that the morphology of the $r<0.3$ au disk region is time-variable. We propose that this asymmetric structure, located in or near the inner rim of the dusty disk, orbits the star. For the physical origin of the asymmetry, we tested a hypothesis where a vortex is created by Rossby wave instability, and we find that a unique large scale vortex may be compatible with our data. The half-light radius of the L-band emitting region is $0.33\pm 0.01$ au, the inclination is ${52^\circ}^{+5^\circ}_{-7^\circ}$, and the position angle is $143^\circ \pm 3^\circ$. Our models predict that a non-negligible fraction of the L-band disk emission originates inside the dust sublimation radius for $\mu$m-sized grains. Refractory grains or large ($\gtrsim 10\ \mu$m-sized) grains could be the origin for this emission., Comment: accepted for publication in A&A
Published: 2020
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6. Molecfit: A general tool for telluric absorption correction. I. Method and application to ESO instruments

Author: Smette, A., Sana, H., Noll, S., Horst, H., Kausch, W., Kimeswenger, S., Barden, M., Szyszka, C., Jones, A. M., Gallenne, A., Vinther, J., Ballester, P., and Taylor, J.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Context: The interaction of the light from astronomical objects with the constituents of the Earth's atmosphere leads to the formation of telluric absorption lines in ground-based collected spectra. Correcting for these lines, mostly affecting the red and infrared region of the spectrum, usually relies on observations of specific stars obtained close in time and airmass to the science targets, therefore using precious observing time. Aims: We present molecfit, a tool for correcting for telluric absorption lines based on synthetic modelling of the Earth's atmospheric transmission. Molecfit is versatile and can be used with data obtained with various ground-based telescopes and instruments. Methods: Molecfit combines a publicly available radiative transfer code, a molecular line database, atmospheric profiles, and various kernels to model the instrument line spread function. The atmospheric profiles are created by merging a standard atmospheric profile representative of a given observatory's climate, of local meteorological data, and of dynamically retrieved altitude profiles for temperature, pressure, and humidity. We discuss the various ingredients of the method, its applicability, and its limitations. We also show examples of telluric line correction on spectra obtained with a suite of ESO Very Large Telescope (VLT) instruments. Results: Compared to previous similar tools, molecfit takes the best results for temperature, pressure, and humidity in the atmosphere above the observatory into account. As a result, the standard deviation of the residuals after correction of unsaturated telluric lines is frequently better than 2% of the continuum. Conclusion: Molecfit is able to accurately model and correct for telluric lines over a broad range of wavelengths and spectral resolutions. (Abridged), Comment: 18 pages, 13 figures, 5 tables, accepted for publication in Astronomy and Astrophysics
Published: 2015
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7. Flux calibration of medium-resolution spectra from 300 nm to 2500 nm: Model reference spectra and telluric correction

Author: Moehler, S., Modigliani, A., Freudling, W., Giammichele, N., Gianninas, A., Gonneau, A., Kausch, W., Lancon, A., Noll, S., Rauch, T., and Vinther, J.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: While the near-infrared wavelength regime is becoming more and more important for astrophysics there is a marked lack of spectrophotometric standard star data that would allow the flux calibration of such data. Furthermore, flux calibrating medium- to high-resolution \'echelle spectroscopy data is challenging even in the optical wavelength range, because the available flux standard data are often too coarsely sampled. We will provide standard star reference data that allow users to derive response curves from 300nm to 2500nm for spectroscopic data of medium to high resolution, including those taken with \'echelle spectrographs. In addition we describe a method to correct for moderate telluric absorption without the need of observing telluric standard stars. As reference data for the flux standard stars we use theoretical spectra derived from stellar model atmospheres. We verify that they provide an appropriate description of the observed standard star spectra by checking for residuals in line cores and line overlap regions in the ratios of observed (X-shooter) spectra to model spectra. The finally selected model spectra are then corrected for remaining mismatches and photometrically calibrated using independent observations. The correction of telluric absorption is performed with the help of telluric model spectra.We provide new, finely sampled reference spectra without telluric absorption for six southern flux standard stars that allow the users to flux calibrate their data from 300 nm to 2500 nm, and a method to correct for telluric absorption using atmospheric models., Comment: Reference spectra available at CDS. Published in A&A 568, A9, 2014
Published: 2014
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8. Molecfit: A Package for Telluric Absorption Correction

Author: Kausch, W., Noll, S., Smette, A., Kimeswenger, S., Horst, H., Sana, H., Jones, A., Barden, M., Szyszka, C., and Vinther, J.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Correcting for the sky signature usually requires supplementary calibration data which are very expensive in terms of telescope time. In addition, the scheduling flexibility is restricted as these data have to be taken usually directly before/after the science observations due to the high variability of the telluric absorption which depends on the state and the chemical composition of the atmosphere at the time of observations. Therefore, a tool for sky correction, which does not require this supplementary calibration data, saves a significant amount of valuable telescope time and increases its efficiency. We developed a software package aimed at performing telluric feature corrections on the basis of synthetic absorption spectra., Comment: 23rd Annual Astronomical Data Analysis Software and Systems (ADASS) Conference; to be published in ASP Conference Proceedings; 4 pages, 2 figures
Published: 2014

9. An atmospheric radiation model for Cerro Paranal. I. The optical spectral range

Author: Noll, S., Kausch, W., Barden, M., Jones, A. M., Szyszka, C., Kimeswenger, S., and Vinther, J.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract: The Earth's atmosphere affects ground-based astronomical observations. Scattering, absorption, and radiation processes deteriorate the signal-to-noise ratio of the data received. For scheduling astronomical observations it is, therefore, important to accurately estimate the wavelength-dependent effect of the Earth's atmosphere on the observed flux. In order to increase the accuracy of the exposure time calculator of the European Southern Observatory's (ESO) Very Large Telescope (VLT) at Cerro Paranal, an atmospheric model was developed as part of the Austrian ESO In-Kind contribution. It includes all relevant components, such as scattered moonlight, scattered starlight, zodiacal light, atmospheric thermal radiation and absorption, and non-thermal airglow emission. This paper focuses on atmospheric scattering processes that mostly affect the blue (< 0.55 mum) wavelength regime, and airglow emission lines and continuum that dominate the red (> 0.55 mum) wavelength regime. While the former is mainly investigated by means of radiative transfer models, the intensity and variability of the latter is studied with a sample of 1186 VLT FORS1 spectra. For a set of parameters such as the object altitude angle, Moon-object angular distance, ecliptic latitude, bimonthly period, and solar radio flux, our model predicts atmospheric radiation and transmission at a requested resolution. A comparison of our model with the FORS1 spectra and photometric data for the night-sky brightness from the literature, suggest a model accuracy of about 20%. This is a significant improvement with respect to existing predictive atmospheric models for astronomical exposure time calculators., Comment: 23 pages, 21 figures, accepted for publication in A&A
Published: 2012
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10. X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope

Author: Vernet, Joel, Dekker, H., D'Odorico, S., Kaper, L., Kjaergaard, P., Hammer, F., Randich, S., Zerbi, F., Groot, P. M., Hjorth, J., Guinouard, I., Navarro, R., Adolfse, T., Albers, P. W., Amans, J. -P., Andersen, J. J., Andersen, M. I., Binetruy, P., Bristow, P., Castillo, R., Chemla, F., Christensen, L., Conconi, P., Conzelmann, R., Dam, J., De Caprio, V., Postigo, A. De Ugarte, Delabre, B., Di Marcantonio, P., Downing, M., Elswijk, E., Finger, G., Fischer, G., Flores, H., Francois, P., Goldoni, P., Guglielmi, L., Haigron, R., Hanenburg, H., Hendriks, I., Horrobin, M., Horville, D., Jessen, N. C., Kerber, F., Kern, L., Kiekebusch, M., Kleszcz, P., Klougart, J., Kragt, J., Larsen, H. H., Lizon, J. -L., Lucuix, C., Mainieri, V., Manuputy, R., Martayan, C., Mason, E., Mazzoleni, R., Michaelsen, N., Modigliani, A., Moehler, S., Møller, P., Sørensen, A. Norup, Nørregaard, P., Peroux, C., Patat, F., Pena, E., Pragt, J., Reinero, C., Riga, F., Riva, M., Roelfsema, R., Royer, F., Sacco, G., Santin, P., Schoenmaker, T., Spano, P., Sweers, E., Ter Horst, R., Tintori, M., Tromp, N., van Dael, P., van der Vliet, H., Venema, L., Vidali, M., Vinther, J., Vola, P., Winters, R., Wistisen, D., Wulterkens, G., and Zacchei, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: X-shooter is the first 2nd generation instrument of the ESO Very Large Telescope(VLT). It is a very efficient, single-target, intermediate-resolution spectrograph that was installed at the Cassegrain focus of UT2 in 2009. The instrument covers, in a single exposure, the spectral range from 300 to 2500 nm. It is designed to maximize the sensitivity in this spectral range through dichroic splitting in three arms with optimized optics, coatings, dispersive elements and detectors. It operates at intermediate spectral resolution (R~4,000 - 17,000, depending on wavelength and slit width) with fixed echelle spectral format (prism cross-dispersers) in the three arms. It includes a 1.8"x4" Integral Field Unit as an alternative to the 11" long slits. A dedicated data reduction package delivers fully calibrated two-dimensional and extracted spectra over the full wavelength range. We describe the main characteristics of the instrument and present its performance as measured during commissioning, science verification and the first months of science operations., Comment: accepted for publication in A&A
Published: 2011
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11. Iridescent plumage in a juvenile dromaeosaurid theropod dinosaur

Author: Croudace, A. D., Shen, C., Lü, J., Brusatte, Steve, and Vinther, J.
Abstract: Colour reconstructions have provided new insights into the lives of dinosaurs and other extinct animals, by predicting colouration patterns from fossilised pigment-bearing organelles called melanosomes. Although these methods have become increasingly popular, only a small number of dinosaurs have been studied using these techniques, which require exceptional preservation of fossil feathers, leaving open key questions such as whether dinosaurs changed their plumagepatterns during ontogeny. Here we reconstruct the feather colouration of an approximately one-year-old individual of the Early Cretaceous dromaeosaurid theropod Wulong bohaiensis, which to our knowledge is the first unequivocal juvenile paravian for which aspects of the original colour has been predicted. Using quadratic discriminant analysis (QDA) and multinomial logistic regression (MLR) on the most comprehensive available datasets, we find strong evidence for iridescent plumage of the forelimb and hindlimb remiges and grey plumage on other portions of the body. This suggests that some juvenile paravians used shiny iridescent feathers for signalling purposes, possibly even before reachingsomatic or sexual maturity, and thus we can conclude that this paravian used iridescent signalling for intraspecific communication other than sexual signalling. Finally, our results show that when analysing fossil datasets that are entirely comprised of solid and cylindrical melanosomes QDA consistently outperforms MLR, providing more accurate and higher classification probability colour predictions.
Published: 2023

12. CRIRES+ on sky at the ESO Very Large Telescope

Author: Dorn, R. J., primary, Bristow, P., additional, Smoker, J. V., additional, Rodler, F., additional, Lavail, A., additional, Accardo, M., additional, van den Ancker, M., additional, Baade, D., additional, Baruffolo, A., additional, Courtney-Barrer, B., additional, Blanco, L., additional, Brucalassi, A., additional, Cumani, C., additional, Follert, R., additional, Haimerl, A., additional, Hatzes, A., additional, Haug, M., additional, Heiter, U., additional, Hinterschuster, R., additional, Hubin, N., additional, Ives, D. J., additional, Jung, Y., additional, Jones, M., additional, Kaeufl, H.-U., additional, Kirchbauer, J.-P., additional, Klein, B., additional, Kochukhov, O., additional, Korhonen, H. H., additional, Köhler, J., additional, Lizon, J-L., additional, Moins, C., additional, Molina-Conde, I., additional, Marquart, T., additional, Neeser, M., additional, Oliva, E., additional, Pallanca, L., additional, Pasquini, L., additional, Paufique, J., additional, Piskunov, N., additional, Reiners, A., additional, Schneller, D., additional, Schmutzer, R., additional, Seemann, U., additional, Slumstrup, D., additional, Smette, A., additional, Stegmeier, J., additional, Stempels, E., additional, Tordo, S., additional, Valenti, E., additional, Valenzuela, J. J., additional, Vernet, J., additional, Vinther, J., additional, and Wehrhahn, A., additional
Published: 2023
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13. CRIRES+ on sky at the ESO Very Large Telescope : Observing the Universe at infrared wavelengths and high spectral resolution

Author: Dorn, R. J., Bristow, P., Smoker, J. V., Rodler, F., Lavail, Alexis, Accardo, M., van den Ancker, M., Baade, D., Baruffolo, A., Courtney-Barrer, B., Blanco, L., Brucalassi, A., Cumani, C., Follert, R., Haimerl, A., Hatzes, A., Haug, M., Heiter, Ulrike, Hinterschuster, R., Hubin, N., Ives, D. J., Jung, Y., Jones, M., Kaeufl, H. -u., Kirchbauer, J. -p., Klein, B., Kochukhov, Oleg, Korhonen, H. H., Koehler, J., Lizon, J-l., Moins, C., Molina-Conde, I., Marquart, Thomas, Neeser, M., Oliva, E., Pallanca, L., Pasquini, L., Paufique, J., Piskunov, Nikolai, Reiners, A., Schneller, D., Schmutzer, R., Seemann, U., Slumstrup, D., Smette, A., Stegmeier, J., Stempels, Eric, Tordo, S., Valenti, E., Valenzuela, J. J., Vernet, J., Vinther, J., Wehrhahn, Ansgar, Dorn, R. J., Bristow, P., Smoker, J. V., Rodler, F., Lavail, Alexis, Accardo, M., van den Ancker, M., Baade, D., Baruffolo, A., Courtney-Barrer, B., Blanco, L., Brucalassi, A., Cumani, C., Follert, R., Haimerl, A., Hatzes, A., Haug, M., Heiter, Ulrike, Hinterschuster, R., Hubin, N., Ives, D. J., Jung, Y., Jones, M., Kaeufl, H. -u., Kirchbauer, J. -p., Klein, B., Kochukhov, Oleg, Korhonen, H. H., Koehler, J., Lizon, J-l., Moins, C., Molina-Conde, I., Marquart, Thomas, Neeser, M., Oliva, E., Pallanca, L., Pasquini, L., Paufique, J., Piskunov, Nikolai, Reiners, A., Schneller, D., Schmutzer, R., Seemann, U., Slumstrup, D., Smette, A., Stegmeier, J., Stempels, Eric, Tordo, S., Valenti, E., Valenzuela, J. J., Vernet, J., Vinther, J., and Wehrhahn, Ansgar
Abstract: The CRyogenic InfraRed Echelle Spectrograph (CRIRES) Upgrade project CRIRES+ extended the capabilities of CRIRES. It transformed this VLT instrument into a cross-dispersed spectrograph to increase the wavelength range that is covered simultaneously by up to a factor of ten. In addition, a new detector focal plane array of three Hawaii 2RG detectors with a 5.3 mu m cutoff wavelength replaced the existing detectors. Amongst many other improvements, a new spectropolarimetric unit was added and the calibration system has been enhanced. The instrument was installed at the VLT on Unit Telescope 3 at the beginning of 2020 and successfully commissioned and verified for science operations during 2021, partly remotely from Europe due to the COVID-19 pandemic. The instrument was subsequently offered to the community from October 2021 onwards. This article describes the performance and capabilities of the upgraded instrument and presents on sky results.
Published: 2023
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14. Cohort description:measures of early-life behaviour and later psychopathology in the LifeCycle Project — EU Child Cohort Network

Author: Nader, J. L. (Johanna L.), López-Vicente, M. (Mònica), Julvez, J. (Jordi), Guxens, M. (Monica), Cadman, T. (Tim), Elhakeem, A. (Ahmed), Järvelin, M.-R. (Marjo-Riitta), Rautio, N. (Nina), Miettunen, J. (Jouko), El Marroun, H. (Hanan), Melchior, M. (Maria), Heude, B. (Barbara), Charles, M.-A. (Marie-Aline), Yang, T. C. (Tiffany C.), McEachan, R. R. (Rosemary R. C.), Wright, J. (John), Polanska, K. (Kinga), Carson, J. (Jennie), Lin, A. (Ashleigh), Rauschert, S. (Sebastian), Huang, R.-C. (Rae-Chi), Popovic, M. (Maja), Richiardi, L. (Lorenzo), Corpeleijn, E. (Eva), Cardol, M. (Marloes), Mikkola, T. M. (Tuija M.), Eriksson, J. G. (Johan G.), Salika, T. (Theodosia), Inskip, H. (Hazel), Vinther, J. L. (Johan Lerbech), Strandberg-Larsen, K. (Katrine), Gürlich, K. (Kathrin), Grote, V. (Veit), Koletzko, B. (Berthold), Vafeiadi, M. (Marina), Sunyer, J. (Jordi), Jaddoe, V. W. (Vincent W. V.), Harris, J. R. (Jennifer R.), Nader, J. L. (Johanna L.), López-Vicente, M. (Mònica), Julvez, J. (Jordi), Guxens, M. (Monica), Cadman, T. (Tim), Elhakeem, A. (Ahmed), Järvelin, M.-R. (Marjo-Riitta), Rautio, N. (Nina), Miettunen, J. (Jouko), El Marroun, H. (Hanan), Melchior, M. (Maria), Heude, B. (Barbara), Charles, M.-A. (Marie-Aline), Yang, T. C. (Tiffany C.), McEachan, R. R. (Rosemary R. C.), Wright, J. (John), Polanska, K. (Kinga), Carson, J. (Jennie), Lin, A. (Ashleigh), Rauschert, S. (Sebastian), Huang, R.-C. (Rae-Chi), Popovic, M. (Maja), Richiardi, L. (Lorenzo), Corpeleijn, E. (Eva), Cardol, M. (Marloes), Mikkola, T. M. (Tuija M.), Eriksson, J. G. (Johan G.), Salika, T. (Theodosia), Inskip, H. (Hazel), Vinther, J. L. (Johan Lerbech), Strandberg-Larsen, K. (Katrine), Gürlich, K. (Kathrin), Grote, V. (Veit), Koletzko, B. (Berthold), Vafeiadi, M. (Marina), Sunyer, J. (Jordi), Jaddoe, V. W. (Vincent W. V.), and Harris, J. R. (Jennifer R.)
Abstract: Background: The EU LifeCycle Project was launched in 2017 to combine, harmonise, and analyse data from more than 250,000 participants across Europe and Australia, involving cohorts participating in the EU-funded LifeCycle Project. The purpose of this cohort description is to provide a detailed overview over the major measures within mental health domains that are available in 17 European and Australian cohorts participating in the LifeCycle Project. Methods: Data on cognitive, behavioural and psychological development has been collected on participants from birth until adulthood through questionnaire and medical data. We developed an inventory of the available data by mapping individual instruments, domain types, and age groups, providing the basis for statistical harmonization across mental health measures. Results: The mental health data in LifeCycle contain longitudinal and cross-sectional data for ages 0–18+ years, covering domains across a wide range of behavioural and psychopathology indicators and outcomes (including executive function, depression, ADHD and cognition). These data span a unique combination of qualitative data collected through behavioural/cognitive/mental health questionnaires and examination, as well as data from biological samples and indices in the form of brain imaging (MRI, foetal ultrasound) and DNA methylation data. Harmonized variables on a subset of mental health domains have been developed, providing statistical equivalence of measures required for longitudinal meta-analyses across instruments and cohorts. Conclusions: Mental health data harmonized through the LifeCycle project can be used to study life course trajectories and exposure-outcome models that examine early life risk factors for mental illness and develop predictive markers for later-life disease.
Published: 2023

15. Preliminary Ams 14C Measurements from Holocene-Age Carbonate Concretions

Author: Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Mojarro, A, Uveges, B, Roberts, M, Vinther, J, Summons, R, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Mojarro, A, Uveges, B, Roberts, M, Vinther, J, and Summons, R
Published: 2023

16. MATISSE, the VLTI mid-infrared imaging spectro-interferometer

Author: Lopez, B., Lagarde, S., Petrov, R. G., Jaffe, W., Antonelli, P., Allouche, F., Berio, P., Matter, A., Meilland, A., Millour, F., Robbe-Dubois, S., Henning, Th, Weigelt, G., Glindemann, A., Agocs, T., Bailet, Ch, Beckmann, U., Bettonvil, F., van Boekel, R., Bourget, P., Bresson, Y., Bristow, P., Cruzalebes, P., Eldswijk, E., Caujolle, Y. Fantei, Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Heininger, M., Hofmann, K-H, Kroes, G., Laun, W., Lehmitz, M., Leinert, C., Meisenheimer, K., Morel, S., Neumann, U., Paladini, C., Percheron, I, Riquelme, M., Schoeller, M., Stee, Ph, Venema, L., Woillez, J., Zins, G., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Alonso, J., Augereau, J-C, Boehm, A., Bazin, G., Beltran, J., Bensberg, A., Boland, W., Brast, R., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., Danchi, W-C, Delbo, M., Drevon, J., Dominik, C., van Duin, A., Ebert, M., Eisenhauer, F., Flament, S., Frahm, R., Rosas, V. Gamez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Glazenborg, A., Gonte, F. Y. J., Guitton, F., de Haan, M., Hanenburg, H., Haubois, X., Hocde, V, Hogerheijde, M., ter Horst, R., Hron, J., Hummel, C. A., Hubin, N., Huerta, R., Idserda, J., Isbell, J. W., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klarmann, L., Klein, R., Kragt, J., Kuindersma, S., Kokoulina, E., Labadie, L., Lacour, S., Leftley, J., Le Poole, R., Lizon, J-L, Lopez, M., Lykou, F., Merand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Menut, J. L., Mohr, L., Mosoni, L., Navarro, R., Nussbaum, E., Pallanca, L., Pantin, E., Pasquini, L., Duc, T. Phan, Pott, J-U, Pozna, E., Richichi, A., Ridinger, A., Rigal, F., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Salabert, D., Schertl, D., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., Toledo, P., Tristram, K., Tromp, N., Vakili, F., Varga, J., Vinther, J., Waters, L. B. F. M., Wittkowski, M., Wolf, S., Wrhel, F., Yoffe, G., Lopez, B., Lagarde, S., Petrov, R. G., Jaffe, W., Antonelli, P., Allouche, F., Berio, P., Matter, A., Meilland, A., Millour, F., Robbe-Dubois, S., Henning, Th, Weigelt, G., Glindemann, A., Agocs, T., Bailet, Ch, Beckmann, U., Bettonvil, F., van Boekel, R., Bourget, P., Bresson, Y., Bristow, P., Cruzalebes, P., Eldswijk, E., Caujolle, Y. Fantei, Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Heininger, M., Hofmann, K-H, Kroes, G., Laun, W., Lehmitz, M., Leinert, C., Meisenheimer, K., Morel, S., Neumann, U., Paladini, C., Percheron, I, Riquelme, M., Schoeller, M., Stee, Ph, Venema, L., Woillez, J., Zins, G., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Alonso, J., Augereau, J-C, Boehm, A., Bazin, G., Beltran, J., Bensberg, A., Boland, W., Brast, R., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., Danchi, W-C, Delbo, M., Drevon, J., Dominik, C., van Duin, A., Ebert, M., Eisenhauer, F., Flament, S., Frahm, R., Rosas, V. Gamez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Glazenborg, A., Gonte, F. Y. J., Guitton, F., de Haan, M., Hanenburg, H., Haubois, X., Hocde, V, Hogerheijde, M., ter Horst, R., Hron, J., Hummel, C. A., Hubin, N., Huerta, R., Idserda, J., Isbell, J. W., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klarmann, L., Klein, R., Kragt, J., Kuindersma, S., Kokoulina, E., Labadie, L., Lacour, S., Leftley, J., Le Poole, R., Lizon, J-L, Lopez, M., Lykou, F., Merand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Menut, J. L., Mohr, L., Mosoni, L., Navarro, R., Nussbaum, E., Pallanca, L., Pantin, E., Pasquini, L., Duc, T. Phan, Pott, J-U, Pozna, E., Richichi, A., Ridinger, A., Rigal, F., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Salabert, D., Schertl, D., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., Toledo, P., Tristram, K., Tromp, N., Vakili, F., Varga, J., Vinther, J., Waters, L. B. F. M., Wittkowski, M., Wolf, S., Wrhel, F., and Yoffe, G.
Abstract: Context. Optical interferometry is at a key development stage. The Very Large Telescope Interferometer (VLTI) has established a stable, robust infrastructure for long-baseline interferometry that is usable by general astronomical observers. The present second-generation instruments offer a wide wavelength coverage and improved performance. Their sensitivity and measurement accuracy lead to data and images of high reliability. Aims. We have developed the Multi AperTure mid-Infrared SpectroScopic Experiment (MATISSE) to access, for the first time, high resolution imaging in a wide spectral domain. Many front-line topics are explored with this new equipment, including: stellar activity and mass loss; planet formation and evolution in the gas and dust disks around young stars; and environment interaction and accretion processes around super massive black holes in active galactic nuclei. Methods. The instrument is a spectro-interferometric imager in the transmission windows called L, M, and N, from 2.8 to 13.0 microns, combining four optical beams from the VLTI's unit or auxiliary telescopes. Its concept, related observing procedure, data reduction, and calibration approach, is the product of 30 years of instrumental research and has benefitted from the expertise developed in the frame of the VLTI's first generation instruments. The instrument utilises a multi-axial beam combination that delivers spectrally dispersed fringes. The signal provides the following quantities at several spectral resolutions: photometric flux, coherent fluxes, visibilities, closure phases, wavelength differential visibilities and phases, and aperture-synthesis imaging. Results. This article provides an overview of the physical principle of the instrument and its functionalities. The motivation of the choice of the instrumental concept and the characteristics of the delivered signal are detailed with a description of the observing modes and of their performance limit. MATISSE offers four spectra
Published: 2022

17. COSMOS2020:A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author: Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J.R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P.U., Gould, K. M.L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fevre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolcić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W. H., Zamorani, G., Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J.R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P.U., Gould, K. M.L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fevre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolcić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W. H., and Zamorani, G.
Abstract: The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data have been collected in the COSMOS field. This paper describes the collection, processing, and analysis of these new imaging data to produce a new reference photometric redshift catalog. Source detection and multiwavelength photometry are performed for 1.7 million sources across the 2 deg2 of the COSMOS field, ∼966,000 of which are measured with all available broadband data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i < 21 sources have subpercent photometric redshift accuracy and even the faintest sources at 25 < i < 27 reach a precision of 5%. Finally, these results are discussed in the context of previous, current, and future surveys in the COSMOS field. Compared to COSMOS2015, it reaches the same photometric redshift precision at almost one magnitude deeper. Both photometric catalogs and their photometric redshift solutions and physical parameters will be made available through the usual astronomical archive systems (ESO Phase 3, IPAC-IRSA, and CDS).
Published: 2022

18. COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author: Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J. R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P. U., Gould, K. M. L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fèvre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolc̆ić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W.-H., Zamorani, G., Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J. R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P. U., Gould, K. M. L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fèvre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolc̆ić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W.-H., and Zamorani, G.
Abstract: The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data have been collected in the COSMOS field. This paper describes the collection, processing, and analysis of these new imaging data to produce a new reference photometric redshift catalog. Source detection and multiwavelength photometry are performed for 1.7 million sources across the 2 deg2 of the COSMOS field, ∼966,000 of which are measured with all available broadband data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i < 21 sources have subpercent photometric redshift accuracy and even the faintest sources at 25 < i < 27 reach a precision of 5%. Finally, these results are discussed in the context of previous, current, and future surveys in the COSMOS field. Compared to COSMOS2015, it reaches the same photometric redshift precision at almost one magnitude deeper. Both photometric catalogs and their photometric redshift solutions and physical parameters will be made available through the usual astronomical archive systems (ESO Phase 3, IPAC-IRSA, and CDS).
Published: 2022

19. MATISSE, the VLTI mid-infrared imaging spectro-interferometer

Author: Lopez, B., primary, Lagarde, S., additional, Petrov, R. G., additional, Jaffe, W., additional, Antonelli, P., additional, Allouche, F., additional, Berio, P., additional, Matter, A., additional, Meilland, A., additional, Millour, F., additional, Robbe-Dubois, S., additional, Henning, Th., additional, Weigelt, G., additional, Glindemann, A., additional, Agocs, T., additional, Bailet, Ch., additional, Beckmann, U., additional, Bettonvil, F., additional, van Boekel, R., additional, Bourget, P., additional, Bresson, Y., additional, Bristow, P., additional, Cruzalèbes, P., additional, Eldswijk, E., additional, Fanteï Caujolle, Y., additional, González Herrera, J. C., additional, Graser, U., additional, Guajardo, P., additional, Heininger, M., additional, Hofmann, K.-H., additional, Kroes, G., additional, Laun, W., additional, Lehmitz, M., additional, Leinert, C., additional, Meisenheimer, K., additional, Morel, S., additional, Neumann, U., additional, Paladini, C., additional, Percheron, I., additional, Riquelme, M., additional, Schoeller, M., additional, Stee, Ph., additional, Venema, L., additional, Woillez, J., additional, Zins, G., additional, Ábrahám, P., additional, Abadie, S., additional, Abuter, R., additional, Accardo, M., additional, Adler, T., additional, Alonso, J., additional, Augereau, J.-C., additional, Böhm, A., additional, Bazin, G., additional, Beltran, J., additional, Bensberg, A., additional, Boland, W., additional, Brast, R., additional, Burtscher, L., additional, Castillo, R., additional, Chelli, A., additional, Cid, C., additional, Clausse, J.-M., additional, Connot, C., additional, Conzelmann, R. D., additional, Danchi, W.-C., additional, Delbo, M., additional, Drevon, J., additional, Dominik, C., additional, van Duin, A., additional, Ebert, M., additional, Eisenhauer, F., additional, Flament, S., additional, Frahm, R., additional, Gámez Rosas, V., additional, Gabasch, A., additional, Gallenne, A., additional, Garces, E., additional, Girard, P., additional, Glazenborg, A., additional, Gonté, F. Y. J., additional, Guitton, F., additional, de Haan, M., additional, Hanenburg, H., additional, Haubois, X., additional, Hocdé, V., additional, Hogerheijde, M., additional, ter Horst, R., additional, Hron, J., additional, Hummel, C. A., additional, Hubin, N., additional, Huerta, R., additional, Idserda, J., additional, Isbell, J. W., additional, Ives, D., additional, Jakob, G., additional, Jaskó, A., additional, Jochum, L., additional, Klarmann, L., additional, Klein, R., additional, Kragt, J., additional, Kuindersma, S., additional, Kokoulina, E., additional, Labadie, L., additional, Lacour, S., additional, Leftley, J., additional, Le Poole, R., additional, Lizon, J.-L., additional, Lopez, M., additional, Lykou, F., additional, Mérand, A., additional, Marcotto, A., additional, Mauclert, N., additional, Maurer, T., additional, Mehrgan, L. H., additional, Meisner, J., additional, Meixner, K., additional, Mellein, M., additional, Menut, J. L., additional, Mohr, L., additional, Mosoni, L., additional, Navarro, R., additional, Nußbaum, E., additional, Pallanca, L., additional, Pantin, E., additional, Pasquini, L., additional, Phan Duc, T., additional, Pott, J.-U., additional, Pozna, E., additional, Richichi, A., additional, Ridinger, A., additional, Rigal, F., additional, Rivinius, Th., additional, Roelfsema, R., additional, Rohloff, R.-R., additional, Rousseau, S., additional, Salabert, D., additional, Schertl, D., additional, Schuhler, N., additional, Schuil, M., additional, Shabun, K., additional, Soulain, A., additional, Stephan, C., additional, Toledo, P., additional, Tristram, K., additional, Tromp, N., additional, Vakili, F., additional, Varga, J., additional, Vinther, J., additional, Waters, L. B. F. M., additional, Wittkowski, M., additional, Wolf, S., additional, Wrhel, F., additional, and Yoffe, G., additional
Published: 2022
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20. COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author: Weaver, J. R., primary, Kauffmann, O. B., additional, Ilbert, O., additional, McCracken, H. J., additional, Moneti, A., additional, Toft, S., additional, Brammer, G., additional, Shuntov, M., additional, Davidzon, I., additional, Hsieh, B. C., additional, Laigle, C., additional, Anastasiou, A., additional, Jespersen, C. K., additional, Vinther, J., additional, Capak, P., additional, Casey, C. M., additional, McPartland, C. J. R., additional, Milvang-Jensen, B., additional, Mobasher, B., additional, Sanders, D. B., additional, Zalesky, L., additional, Arnouts, S., additional, Aussel, H., additional, Dunlop, J. S., additional, Faisst, A., additional, Franx, M., additional, Furtak, L. J., additional, Fynbo, J. P. U., additional, Gould, K. M. L., additional, Greve, T. R., additional, Gwyn, S., additional, Kartaltepe, J. S., additional, Kashino, D., additional, Koekemoer, A. M., additional, Kokorev, V., additional, Le Fèvre, O., additional, Lilly, S., additional, Masters, D., additional, Magdis, G., additional, Mehta, V., additional, Peng, Y., additional, Riechers, D. A., additional, Salvato, M., additional, Sawicki, M., additional, Scarlata, C., additional, Scoville, N., additional, Shirley, R., additional, Silverman, J. D., additional, Sneppen, A., additional, Smolc̆ić, V., additional, Steinhardt, C., additional, Stern, D., additional, Tanaka, M., additional, Taniguchi, Y., additional, Teplitz, H. I., additional, Vaccari, M., additional, Wang, W.-H., additional, and Zamorani, G., additional
Published: 2022
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21. Mid-infrared circumstellar emission of the long-period Cepheid ℓ Carinae resolved with VLTI/MATISSE

Author: Hocdé, V., primary, Nardetto, N., additional, Matter, A., additional, Lagadec, E., additional, Mérand, A., additional, Cruzalèbes, P., additional, Meilland, A., additional, Millour, F., additional, Lopez, B., additional, Berio, P., additional, Weigelt, G., additional, Petrov, R., additional, Isbell, J. W., additional, Jaffe, W., additional, Kervella, P., additional, Glindemann, A., additional, Schöller, M., additional, Allouche, F., additional, Gallenne, A., additional, Domiciano de Souza, A., additional, Niccolini, G., additional, Kokoulina, E., additional, Varga, J., additional, Lagarde, S., additional, Augereau, J.-C., additional, van Boekel, R., additional, Bristow, P., additional, Henning, Th., additional, Hofmann, K.-H., additional, Zins, G., additional, Danchi, W.-C., additional, Delbo, M., additional, Dominik, C., additional, Gámez Rosas, V., additional, Klarmann, L., additional, Hron, J., additional, Hogerheijde, M. R., additional, Meisenheimer, K., additional, Pantin, E., additional, Paladini, C., additional, Robbe-Dubois, S., additional, Schertl, D., additional, Stee, P., additional, Waters, R., additional, Lehmitz, M., additional, Bettonvil, F., additional, Heininger, M., additional, Woillez, J., additional, Wolf, S., additional, Yoffe, G., additional, Szabados, L., additional, Chiavassa, A., additional, Borgniet, S., additional, Breuval, L., additional, Javanmardi, B., additional, Ábrahám, P., additional, Abadie, S., additional, Abuter, R., additional, Accardo, M., additional, Adler, T., additional, Agócs, T., additional, Alonso, J., additional, Antonelli, P., additional, Böhm, A., additional, Bailet, C., additional, Bazin, G., additional, Beckmann, U., additional, Beltran, J., additional, Boland, W., additional, Bourget, P., additional, Brast, R., additional, Bresson, Y., additional, Burtscher, L., additional, Buter, R., additional, Castillo, R., additional, Chelli, A., additional, Cid, C., additional, Clausse, J.-M., additional, Connot, C., additional, Conzelmann, R. D., additional, De Haan, M., additional, Ebert, M., additional, Elswijk, E., additional, Fantei, Y., additional, Frahm, R., additional, Gabasch, A., additional, Garces, E., additional, Girard, P., additional, Glazenborg, A., additional, Gonté, F. Y. J., additional, González Herrera, J. C., additional, Graser, U., additional, Guajardo, P., additional, Guitton, F., additional, Hanenburg, H., additional, Haubois, X., additional, Hubin, N., additional, Huerta, R., additional, Idserda, J., additional, Ives, D., additional, Jakob, G., additional, Jaskó, A., additional, Jochum, L., additional, Klein, R., additional, Kragt, J., additional, Kroes, G., additional, Kuindersma, S., additional, Labadie, L., additional, Laun, W., additional, Le Poole, R., additional, Leinert, C., additional, Lizon, J.-L., additional, Lopez, M., additional, Marcotto, A., additional, Mauclert, N., additional, Maurer, T., additional, Mehrgan, L. H., additional, Meisner, J., additional, Meixner, K., additional, Mellein, M., additional, Mohr, L., additional, Morel, S., additional, Mosoni, L., additional, Navarro, R., additional, Neumann, U., additional, Nußbaum, E., additional, Pallanca, L., additional, Pasquini, L., additional, Percheron, I., additional, Phan Duc, T., additional, Pott, J.-U., additional, Pozna, E., additional, Ridinger, A., additional, Rigal, F., additional, Riquelme, M., additional, Rivinius, Th., additional, Roelfsema, R., additional, Rohloff, R.-R., additional, Rousseau, S., additional, Schuhler, N., additional, Schuil, M., additional, Shabun, K., additional, Soulain, A., additional, Stephan, C., additional, ter Horst, R., additional, Tromp, N., additional, Vakili, F., additional, van Duin, A., additional, Venema, L. B., additional, Vinther, J., additional, Wittkowski, M., additional, and Wrhel, F., additional
Published: 2021
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22. The asymmetric inner disk of the Herbig Ae star HD 163296 in the eyes of VLTI/MATISSE: evidence for a vortex?

Author: Varga, J., Hogerheijde, M., van Boekel, R., Klarmann, L., Petrov, R., Waters, L. B. F. M., Lagarde, S., Pantin, E., Berio, Ph, Weigelt, G., Robbe-Dubois, S., Lopez, B., Millour, F., Augereau, J-C, Meheut, H., Meilland, A., Henning, Th, Jaffe, W., Bettonvil, F., Bristow, P., Hofmann, K-H, Matter, A., Zins, G., Wolf, S., Allouche, F., Donnan, F., Schertl, D., Dominik, C., Heininger, M., Lehmitz, M., Cruzalebes, P., Glindemann, A., Meisenheimer, K., Paladini, C., Schoeller, M., Woillez, J., Venema, L., Kokoulina, E., Yoffe, G., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Agocs, T., Antonelli, P., Bohm, A., Bailet, C., Bazin, G., Beckmann, U., Beltran, J., Boland, W., Bourget, P., Brast, R., Bresson, Y., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., Danchi, W-C, De Haan, M., Delbo, M., Ebert, M., Elswijk, E., Fantei, Y., Frahm, R., Rosas, V. Gamez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Gonte, F. Y. J., Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Guitton, F., Haubois, X., Hron, J., Hubin, N., Huerta, R., Isbell, J. W., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klein, R., Kragt, J., Kroes, G., Kuindersma, S., Labadie, L., Laun, W., Le Poole, R., Leinert, C., Lizon, J-L, Lopez, M., Merand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Mohr, L., Morel, S., Mosoni, L., Navarro, R., Neumann, U., Nussbaum, E., Pallanca, L., Pasquini, L., Percheron, I, Pott, J-U, Pozna, E., Ridinger, A., Rigal, F., Riquelme, M., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Schuhler, N., Schuil, M., Soulain, A., Stee, P., Stephan, C., ter Horst, R., Tromp, N., Vakili, F., van Duin, A., Vinther, J., Wittkowski, M., Wrhel, F., Varga, J., Hogerheijde, M., van Boekel, R., Klarmann, L., Petrov, R., Waters, L. B. F. M., Lagarde, S., Pantin, E., Berio, Ph, Weigelt, G., Robbe-Dubois, S., Lopez, B., Millour, F., Augereau, J-C, Meheut, H., Meilland, A., Henning, Th, Jaffe, W., Bettonvil, F., Bristow, P., Hofmann, K-H, Matter, A., Zins, G., Wolf, S., Allouche, F., Donnan, F., Schertl, D., Dominik, C., Heininger, M., Lehmitz, M., Cruzalebes, P., Glindemann, A., Meisenheimer, K., Paladini, C., Schoeller, M., Woillez, J., Venema, L., Kokoulina, E., Yoffe, G., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Agocs, T., Antonelli, P., Bohm, A., Bailet, C., Bazin, G., Beckmann, U., Beltran, J., Boland, W., Bourget, P., Brast, R., Bresson, Y., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., Danchi, W-C, De Haan, M., Delbo, M., Ebert, M., Elswijk, E., Fantei, Y., Frahm, R., Rosas, V. Gamez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Gonte, F. Y. J., Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Guitton, F., Haubois, X., Hron, J., Hubin, N., Huerta, R., Isbell, J. W., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klein, R., Kragt, J., Kroes, G., Kuindersma, S., Labadie, L., Laun, W., Le Poole, R., Leinert, C., Lizon, J-L, Lopez, M., Merand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Mohr, L., Morel, S., Mosoni, L., Navarro, R., Neumann, U., Nussbaum, E., Pallanca, L., Pasquini, L., Percheron, I, Pott, J-U, Pozna, E., Ridinger, A., Rigal, F., Riquelme, M., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Schuhler, N., Schuil, M., Soulain, A., Stee, P., Stephan, C., ter Horst, R., Tromp, N., Vakili, F., van Duin, A., Vinther, J., Wittkowski, M., and Wrhel, F.
Abstract: Context. A complex environment exists in the inner few astronomical units of planet-forming disks. High-angular-resolution observations play a key role in our understanding of the disk structure and the dynamical processes at work.Aims. In this study we aim to characterize the mid-infrared brightness distribution of the inner disk of the young intermediate-mass star HD 163296 from early VLTI/MATISSE observations taken in the L- and N-bands. We put special emphasis on the detection of potential disk asymmetries.Methods. We use simple geometric models to fit the interferometric visibilities and closure phases. Our models include a smoothed ring, a flat disk with an inner cavity, and a 2D Gaussian. The models can account for disk inclination and for azimuthal asymmetries as well. We also perform numerical hydrodynamical simulations of the inner edge of the disk.Results. Our modeling reveals a significant brightness asymmetry in the L-band disk emission. The brightness maximum of the asymmetry is located at the NW part of the disk image, nearly at the position angle of the semimajor axis. The surface brightness ratio in the azimuthal variation is 3.5 +/- 0.2. Comparing our result on the location of the asymmetry with other interferometric measurements, we confirm that the morphology of the r < 0.3 au disk region is time-variable. We propose that this asymmetric structure, located in or near the inner rim of the dusty disk, orbits the star. To find the physical origin of the asymmetry, we tested a hypothesis where a vortex is created by Rossby wave instability, and we find that a unique large-scale vortex may be compatible with our data. The half-light radius of the L-band-emitting region is 0.33 +/- 0.01 au, the inclination is 52 degrees(+5 degrees)(-7 degrees) 52 degrees-7 degrees+5 degrees , and the position angle is 143 degrees +/- 3 degrees. Our models predict that a non-negligible fraction of the L-band disk emission originates inside the dust sublimation radius fo
Published: 2021

23. Mid-infrared circumstellar emission of the long-period Cepheid l Carinae resolved with VLTI/MATISSE

Author: Hocde, V, Nardetto, N., Matter, A., Lagadec, E., Merand, A., Cruzalebes, P., Meilland, A., Millour, F., Lopez, B., Berio, P., Weigelt, G., Petrov, R., Isbell, J. W., Jaffe, W., Kervella, P., Glindemann, A., Scholler, M., Allouche, F., Gallenne, A., de Souza, A. Domiciano, Niccolini, G., Kokoulina, E., Varga, J., Lagarde, S., Augereau, J-C, van Boekel, R., Bristow, P., Henning, Th, Hofmann, K-H, Zins, G., Danchi, W-C, Delbo, M., Dominik, C., Rosas, V. Gamez, Klarmann, L., Hron, J., Hogerheijde, M. R., Meisenheimer, K., Pantin, E., Paladini, C., Robbe-Dubois, S., Schertl, D., Stee, P., Waters, R., Lehmitz, M., Bettonvil, F., Heininger, M., Woillez, J., Wolf, S., Yoffe, G., Szabados, L., Chiavassa, A., Borgniet, S., Breuval, L., Javanmardi, B., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Agocs, T., Alonso, J., Antonelli, P., Bohm, A., Bailet, C., Bazin, G., Beckmann, U., Beltran, J., Boland, W., Bourget, P., Brast, R., Bresson, Y., Burtscher, L., Buter, R., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., De Haan, M., Ebert, M., Elswijk, E., Fantei, Y., Frahm, R., Gabasch, A., Garces, E., Girard, P., Glazenborg, A., Gonte, F. Y. J., Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Guitton, F., Hanenburg, H., Haubois, X., Hubin, N., Huerta, R., Idserda, J., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klein, R., Kragt, J., Kroes, G., Kuindersma, S., Labadie, L., Laun, W., Le Poole, R., Leinert, C., Lizon, J-L, Lopez, M., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Mohr, L., Morel, S., Mosoni, L., Navarro, R., Neumann, U., Nussbaum, E., Pallanca, L., Pasquini, L., Percheron, I, Duc, T. Phan, Pott, J-U, Pozna, E., Ridinger, A., Rigal, F., Riquelme, M., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., ter Horst, R., Tromp, N., Vakili, F., van Duin, A., Venema, L. B., Vinther, J., Wittkowski, M., Wrhel, F., Hocde, V, Nardetto, N., Matter, A., Lagadec, E., Merand, A., Cruzalebes, P., Meilland, A., Millour, F., Lopez, B., Berio, P., Weigelt, G., Petrov, R., Isbell, J. W., Jaffe, W., Kervella, P., Glindemann, A., Scholler, M., Allouche, F., Gallenne, A., de Souza, A. Domiciano, Niccolini, G., Kokoulina, E., Varga, J., Lagarde, S., Augereau, J-C, van Boekel, R., Bristow, P., Henning, Th, Hofmann, K-H, Zins, G., Danchi, W-C, Delbo, M., Dominik, C., Rosas, V. Gamez, Klarmann, L., Hron, J., Hogerheijde, M. R., Meisenheimer, K., Pantin, E., Paladini, C., Robbe-Dubois, S., Schertl, D., Stee, P., Waters, R., Lehmitz, M., Bettonvil, F., Heininger, M., Woillez, J., Wolf, S., Yoffe, G., Szabados, L., Chiavassa, A., Borgniet, S., Breuval, L., Javanmardi, B., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Agocs, T., Alonso, J., Antonelli, P., Bohm, A., Bailet, C., Bazin, G., Beckmann, U., Beltran, J., Boland, W., Bourget, P., Brast, R., Bresson, Y., Burtscher, L., Buter, R., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., De Haan, M., Ebert, M., Elswijk, E., Fantei, Y., Frahm, R., Gabasch, A., Garces, E., Girard, P., Glazenborg, A., Gonte, F. Y. J., Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Guitton, F., Hanenburg, H., Haubois, X., Hubin, N., Huerta, R., Idserda, J., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klein, R., Kragt, J., Kroes, G., Kuindersma, S., Labadie, L., Laun, W., Le Poole, R., Leinert, C., Lizon, J-L, Lopez, M., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Mohr, L., Morel, S., Mosoni, L., Navarro, R., Neumann, U., Nussbaum, E., Pallanca, L., Pasquini, L., Percheron, I, Duc, T. Phan, Pott, J-U, Pozna, E., Ridinger, A., Rigal, F., Riquelme, M., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., ter Horst, R., Tromp, N., Vakili, F., van Duin, A., Venema, L. B., Vinther, J., Wittkowski, M., and Wrhel, F.
Abstract: Context. The nature of circumstellar envelopes (CSEs) around Cepheids is a matter of ongoing debate. The physical origin of their infrared (IR) excess could be shown to either be made up of a shell of ionized gas, a dust envelope, or a combination of both.Aims. This study is aimed at constraining the geometry and the IR excess of the environment of the bright long-period Cepheid l Car (P = 35.5 days) at mid-IR wavelengths in order to understand its physical nature.Methods. We first used photometric observations in various bands (from the visible domain to the infrared) and Spitzer Space Telescope spectroscopy to constrain the IR excess of l Car. Then we analyzed the VLTI/MATISSE measurements at a specific phase of observation in order to determine the flux contribution as well as the size and shape of the environment of the star in the L band. Finally, we tested the hypothesis of a shell of ionized gas in order to model the IR excess.Results. We report the first detection in the L band of a centro-symmetric extended emission around l Car, of about 1.7 R-star in full width at half maximum, producing an excess of about 7.0% in this band.This latter value is used to calibrate the IR excess found when comparing the photometric observations in various bands and quasi-static atmosphere models. In the N band, there is no clear evidence for dust emission from VLTI/MATISSE correlated flux and Spitzer data. On the other side, the modeled shell of ionized gas implies a more compact CSE (1.13 0.02 R-star) that is also fainter (IR excess of 1% in the L band).Conclusions. We provide new evidence supporting a compact CSE for l Car and we demonstrate the capabilities of VLTI/MATISSE for determining common properties of CSEs. While the compact CSE of l Car is likely to be of a gaseous nature, the tested model of a shell of ionized gas is not able to simultaneously reproduce the IR excess and the interferometric observations. Further Galactic Cepheid observations with VLTI/MATISSE ar
Published: 2021

24. The EU Child Cohort Network’s core data:establishing a set of findable, accessible, interoperable and re-usable (FAIR) variables

Author: Pinot de Moira, A. (Angela), Haakma, S. (Sido), Strandberg-Larsen, K. (Katrine), van Enckevort, E. (Esther), Kooijman, M. (Marjolein), Cadman, T. (Tim), Cardol, M. (Marloes), Corpeleijn, E. (Eva), Crozier, S. (Sarah), Duijts, L. (Liesbeth), Elhakeem, A. (Ahmed), Eriksson, J. G. (Johan G.), Felix, J. F. (Janine F.), Fernandez-Barres, S. (Silvia), Foong, R. E. (Rachel E.), Forhan, A. (Anne), Grote, V. (Veit), Guerlich, K. (Kathrin), Heude, B. (Barbara), Huang, R.-C. (Rae-Chi), Järvelin, M.-R. (Marjo-Riitta), Jorgensen, A. C. (Anne Cathrine), Mikkola, T. M. (Tuija M.), Nader, J. L. (Johanna L. T.), Pedersen, M. (Marie), Popovic, M. (Maja), Rautio, N. (Nina), Richiardi, L. (Lorenzo), Ronkainen, J. (Justiina), Roumeliotaki, T. (Theano), Salika, T. (Theodosia), Sebert, S. (Sylvain), Vinther, J. L. (Johan L.), Voerman, E. (Ellis), Vrijheid, M. (Martine), Wright, J. (John), Yang, T. C. (Tiffany C.), Zariouh, F. (Faryal), Charles, M.-A. (Marie-Aline), Inskip, H. (Hazel), Jaddoe, V. W. (Vincent W. V.), Swertz, M. A. (Morris A.), Nybo Andersen, A.-M. (Anne-Marie), Pinot de Moira, A. (Angela), Haakma, S. (Sido), Strandberg-Larsen, K. (Katrine), van Enckevort, E. (Esther), Kooijman, M. (Marjolein), Cadman, T. (Tim), Cardol, M. (Marloes), Corpeleijn, E. (Eva), Crozier, S. (Sarah), Duijts, L. (Liesbeth), Elhakeem, A. (Ahmed), Eriksson, J. G. (Johan G.), Felix, J. F. (Janine F.), Fernandez-Barres, S. (Silvia), Foong, R. E. (Rachel E.), Forhan, A. (Anne), Grote, V. (Veit), Guerlich, K. (Kathrin), Heude, B. (Barbara), Huang, R.-C. (Rae-Chi), Järvelin, M.-R. (Marjo-Riitta), Jorgensen, A. C. (Anne Cathrine), Mikkola, T. M. (Tuija M.), Nader, J. L. (Johanna L. T.), Pedersen, M. (Marie), Popovic, M. (Maja), Rautio, N. (Nina), Richiardi, L. (Lorenzo), Ronkainen, J. (Justiina), Roumeliotaki, T. (Theano), Salika, T. (Theodosia), Sebert, S. (Sylvain), Vinther, J. L. (Johan L.), Voerman, E. (Ellis), Vrijheid, M. (Martine), Wright, J. (John), Yang, T. C. (Tiffany C.), Zariouh, F. (Faryal), Charles, M.-A. (Marie-Aline), Inskip, H. (Hazel), Jaddoe, V. W. (Vincent W. V.), Swertz, M. A. (Morris A.), and Nybo Andersen, A.-M. (Anne-Marie)
Abstract: The Horizon2020 LifeCycle Project is a cross-cohort collaboration which brings together data from multiple birth cohorts from across Europe and Australia to facilitate studies on the influence of early-life exposures on later health outcomes. A major product of this collaboration has been the establishment of a FAIR (findable, accessible, interoperable and reusable) data resource known as the EU Child Cohort Network. Here we focus on the EU Child Cohort Network’s core variables. These are a set of basic variables, derivable by the majority of participating cohorts and frequently used as covariates or exposures in lifecourse research. First, we describe the process by which the list of core variables was established. Second, we explain the protocol according to which these variables were harmonised in order to make them interoperable. Third, we describe the catalogue developed to ensure that the network’s data are findable and reusable. Finally, we describe the core data, including the proportion of variables harmonised by each cohort and the number of children for whom harmonised core data are available. EU Child Cohort Network data will be analysed using a federated analysis platform, removing the need to physically transfer data and thus making the data more accessible to researchers. The network will add value to participating cohorts by increasing statistical power and exposure heterogeneity, as well as facilitating cross-cohort comparisons, cross-validation and replication. Our aim is to motivate other cohorts to join the network and encourage the use of the EU Child Cohort Network by the wider research community.
Published: 2021

25. The asymmetric inner disk of the Herbig Ae star HD 163296 in the eyes of VLTI/MATISSE: evidence for a vortex?

Author: Varga, J., primary, Hogerheijde, M., additional, van Boekel, R., additional, Klarmann, L., additional, Petrov, R., additional, Waters, L. B. F. M., additional, Lagarde, S., additional, Pantin, E., additional, Berio, Ph., additional, Weigelt, G., additional, Robbe-Dubois, S., additional, Lopez, B., additional, Millour, F., additional, Augereau, J.-C., additional, Meheut, H., additional, Meilland, A., additional, Henning, Th., additional, Jaffe, W., additional, Bettonvil, F., additional, Bristow, P., additional, Hofmann, K.-H., additional, Matter, A., additional, Zins, G., additional, Wolf, S., additional, Allouche, F., additional, Donnan, F., additional, Schertl, D., additional, Dominik, C., additional, Heininger, M., additional, Lehmitz, M., additional, Cruzalèbes, P., additional, Glindemann, A., additional, Meisenheimer, K., additional, Paladini, C., additional, Schöller, M., additional, Woillez, J., additional, Venema, L., additional, Kokoulina, E., additional, Yoffe, G., additional, Ábrahám, P., additional, Abadie, S., additional, Abuter, R., additional, Accardo, M., additional, Adler, T., additional, Agócs, T., additional, Antonelli, P., additional, Böhm, A., additional, Bailet, C., additional, Bazin, G., additional, Beckmann, U., additional, Beltran, J., additional, Boland, W., additional, Bourget, P., additional, Brast, R., additional, Bresson, Y., additional, Burtscher, L., additional, Castillo, R., additional, Chelli, A., additional, Cid, C., additional, Clausse, J.-M., additional, Connot, C., additional, Conzelmann, R. D., additional, Danchi, W.-C., additional, De Haan, M., additional, Delbo, M., additional, Ebert, M., additional, Elswijk, E., additional, Fantei, Y., additional, Frahm, R., additional, Gámez Rosas, V., additional, Gabasch, A., additional, Gallenne, A., additional, Garces, E., additional, Girard, P., additional, Gonté, F. Y. J., additional, González Herrera, J. C., additional, Graser, U., additional, Guajardo, P., additional, Guitton, F., additional, Haubois, X., additional, Hron, J., additional, Hubin, N., additional, Huerta, R., additional, Isbell, J. W., additional, Ives, D., additional, Jakob, G., additional, Jaskó, A., additional, Jochum, L., additional, Klein, R., additional, Kragt, J., additional, Kroes, G., additional, Kuindersma, S., additional, Labadie, L., additional, Laun, W., additional, Le Poole, R., additional, Leinert, C., additional, Lizon, J.-L., additional, Lopez, M., additional, Mérand, A., additional, Marcotto, A., additional, Mauclert, N., additional, Maurer, T., additional, Mehrgan, L. H., additional, Meisner, J., additional, Meixner, K., additional, Mellein, M., additional, Mohr, L., additional, Morel, S., additional, Mosoni, L., additional, Navarro, R., additional, Neumann, U., additional, Nußbaum, E., additional, Pallanca, L., additional, Pasquini, L., additional, Percheron, I., additional, Pott, J.-U., additional, Pozna, E., additional, Ridinger, A., additional, Rigal, F., additional, Riquelme, M., additional, Rivinius, Th., additional, Roelfsema, R., additional, Rohloff, R.-R., additional, Rousseau, S., additional, Schuhler, N., additional, Schuil, M., additional, Soulain, A., additional, Stee, P., additional, Stephan, C., additional, ter Horst, R., additional, Tromp, N., additional, Vakili, F., additional, van Duin, A., additional, Vinther, J., additional, Wittkowski, M., additional, and Wrhel, F., additional
Published: 2021
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26. A molecular palaeobiological exploration of arthropod terrestrialization

Author: Lozano-Fernandez, J, Carton, R, Tanner, AR, Puttick, MN, Blaxter, M, Vinther, J, Olesen, J, Giribet, G, Edgecombe, GD, Pisani, D, Lozano-Fernandez, J, Carton, R, Tanner, AR, Puttick, MN, Blaxter, M, Vinther, J, Olesen, J, Giribet, G, Edgecombe, GD, and Pisani, D
Abstract: Understanding animal terrestrialization, the process through which animals colonized the land, is crucial to clarify extant biodiversity and biological adaptation. Arthropoda (insects, spiders, centipedes and their allies) represent the largest majority of terrestrial biodiversity. Here we implemented a molecular palaeobiological approach, merging molecular and fossil evidence, to elucidate the deepest history of the terrestrial arthropods. We focused on the three independent, Palaeozoic arthropod terrestrialization events (those of Myriapoda, Hexapoda and Arachnida) and showed that a marine route to the colonization of land is the most likely scenario. Molecular clock analyses confirmed an origin for the three terrestrial lineages bracketed between the Cambrian and the Silurian. While molecular divergence times for Arachnida are consistent with the fossil record, Myriapoda are inferred to have colonized land earlier, substantially predating trace or body fossil evidence. An estimated origin of myriapods by the Early Cambrian precedes the appearance of embryophytes and perhaps even terrestrial fungi, raising the possibility that terrestrialization had independent origins in crown-group myriapod lineages, consistent with morphological arguments for convergence in tracheal systems. This article is part of the themed issue ‘Dating species divergences using rocks and clocks’., © 2016 The Authors. Published by the Royal Society under the terms of the Creative Commons Attribution License http://creativecommons.org/licenses/by/4.0/, which permits unrestricted use, provided the original author and source are credited., NHM Repository
Published: 2020

27. Novel intermediate method of impedance calculation for connection requirements to high voltage grids

Author: Hansen, H., primary, Vinther, J. R., additional, Dalsgaard, M. T., additional, Christiansen, A. V., additional, Hansen, C. S., additional, and Kanstrup, K. R., additional
Published: 2021
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28. Preliminary Ams 14C Measurements from Holocene-Age Carbonate Concretions

Author: Mojarro, A., primary, Uveges, B., additional, Roberts, M., additional, Vinther, J., additional, and Summons, R., additional
Published: 2021
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29. Molecular Characterization and Effect of Diagenesis and Maduration of Melanin in the Fossil Record

Author: Herrera, J., primary, Sistiaga, A., additional, Vinther, J., additional, Brown, C. M., additional, Henderson, D. M., additional, and Summons, R. E., additional
Published: 2019
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30. Biomarker Taphonomy in Holocene-Age Concretions

Author: Mojarro, A., primary, Cui, X., additional, Vinther, J., additional, and Summons, R. E., additional
Published: 2019
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31. Dietary supplement rich in fiber fed to late gestating sows during transition reduces rate of stillborn piglets

Author: Feyera, Takele, Højgaard, Camilla Kaae, Vinther, J, Bruun, T S, and Theil, Peter Kappel
Subjects: animal diseases, stillbirth, piglets, preweaning, dietary fiber, transition period, late gestation
Abstract: The beneficial effects of dietary fiber (DF) from a behavioral and welfare perspective have been thoroughly studied. However, data on the effects of DF on reproductive performance are scarce. Therefore, the aim of this study was to investigate the impact of increased DF supply during the last 2 wk of gestation on stillbirth rate, preweaning mortality, and total piglet mortality. A total of 644 sows were selected for the experiment from a commercial farm, and the sows were inseminated in weekly batches. Sows in the control group (n = 310) were fed according to the normal feeding strategy of the farm with a gestation diet until 1 wk before expected farrowing, then a transition diet until d 5 of lactation, and then a lactation diet until weaning. Sows in the treatment group (n = 334) were fed as the control group except that 280 g/d of the gestation diet (from d 102 to 108 of gestation) and 570 g/d of the transition diet (from d 109 of gestation until farrowing) was daily replaced with 350 and 700 g/d, respectively, of a DF-rich supplement. Both groups received isocaloric diets on a NE basis. The numbers of live-born and stillborn piglets as well as mortality of live-born piglets with presumed causes of death were recorded. The supplemented DF reduced the proportion of stillborn piglets from 8.8 to 6.6% (P < 0.001) and mortality of total born piglets from 22.3 to 19.9% (P = 0.004) but had no impact on preweaning mortality of the piglets (P = 0.21). Moreover, supplemented DF reduced the proportion of death due to poor viability (P < 0.001; 2.8 vs. 1.5% in the control and treatment groups, respectively) and prevalence of piglet diarrhea (P = 0.004; 0.7 vs. 0.3% in the control and treatment groups, respectively). Crushing, low birth weight, and poor viability were the top 3 contributors to preweaning mortality of live-born piglets, in descending order. In conclusion, the supplemented DF reduced the proportion of stillborn piglets and total piglet mortality as well as mortality due to poor viability and piglet diarrhea in lactation.
Published: 2017

32. Molecfit

Author: Smette, Alain, Sana, H., Horst, H., Kausch, W., Noll, S., Kimenswenger, S., Barden, M., Szyszka, C., Jones, A.M., Gallenne, A., Vinther, J., Ballester, P., and Taylor, J.
Abstract: "Molecfit is a tool to correct for telluric absorption lines based on synthetic modelling of the Earth's atmospheric transmission. \nWe will present the tool, its applicability, its limitations, examples of applications at ESO and at other observatories, as well as recent and future developments."
Published: 2017
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33. Correction to ‘Multiple optimality criteria support Ornithoscelida’

Author: Parry, L. A., primary, Baron, M. G., additional, and Vinther, J., additional
Published: 2018
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34. Dietary supplement rich in fiber fed to late gestating sows during transition reduces rate of stillborn piglets1

Author: Feyera, T., primary, Højgaard, C. K., additional, Vinther, J., additional, Bruun, T. S., additional, and Theil, P. K., additional
Published: 2017
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35. Molecular clocks indicate turnover and diversification of modern coleoid cephalopods during the mesozoic marine revolution

Author: Tanner, A., Fuchs, D., Winkelmann, I., Gilbert, Thomas, Pankey, M., Ribeiro, A., Kocot, K., Halanych, K., Oakley, T., Da Fonseca, R., Pisani, D., Vinther, J., Tanner, A., Fuchs, D., Winkelmann, I., Gilbert, Thomas, Pankey, M., Ribeiro, A., Kocot, K., Halanych, K., Oakley, T., Da Fonseca, R., Pisani, D., and Vinther, J.
Abstract: Coleoid cephalopod molluscs comprise squid, cuttlefish and octopuses, and represent nearly the entire diversity of modern cephalopods. Sophisticated adaptations such as the use of colour for camouflage and communication, jet propulsion and the ink sac highlight the unique nature of the group. Despite these striking adaptations, there are clear parallels in ecology between coleoids and bony fishes. The coleoid fossil record is limited, however, hindering confident analysis of the tempo and pattern of their evolution. Here we use a molecular dataset (180 genes, approx. 36 000 amino acids) of 26 cephalopod species to explore the phylogeny and timing of cephalopod evolution. We show that crown cephalopods diverged in the Silurian–Devonian, while crown coleoids had origins in the latest Palaeozoic.While the deep-sea vampire squid and dumbo octopuses have ancient origins extending to the Early Mesozoic Era, 242+38 Ma, incirrate octopuses and the decabrachian coleoids (10-armed squid) diversified in the Jurassic Period. These divergence estimates highlight the modern diversity of coleoid cephalopods emerging in the Mesozoic Marine Revolution, a period that also witnessed the radiation of most ray-finned fish groups in addition to several other marine vertebrates. This suggests that that the origin of modern cephalopod biodiversity was contingent on ecological competition with marine vertebrates.
Published: 2017

36. Molecfit : A general tool for telluric absorption correction

Author: Smette A., Sana H., Noll S., Horst, H, Kausch W., Kimeswenger S., Barden, M, Szyszka, C, Jones, AM, Gallenne A., Vinther, J, Ballester, P, and Taylor J.
Published: 2015

37. Reproductive performance of 'nurse sows' in Danish piggeries

Author: Bruun, T. S., Williams, Charlotte Amdi, Vinther, J., Schop, M., Strathe, Anders Bjerring, Hansen, Christian Fink, Bruun, T. S., Williams, Charlotte Amdi, Vinther, J., Schop, M., Strathe, Anders Bjerring, and Hansen, Christian Fink
Abstract: The use of nurse sows in Danish piggeries is common practice because of large litter sizes; however, the effect of being selected as a nurse sow on subsequent reproductive performance is unknown. Therefore, the aim of this study was to quantify a nurse sow's reproductive performance in the subsequent litter. Nurse sows were defined as sows weaning their own litter at least 18 days postpartum and thereafter nursing another litter (nurse litter) before service. Data (2012–2013) from 20 piggeries with more than 14.5 live born piglets per litter and a stable distribution of sows among parities over time were selected. Records from 79,864 litters were obtained and analyzed using mixed linear and logistic regression models. The average lactation lengths were 40.3 days for nurse sows and 27.8 days for non-nurse (normal) sows. Nurse sows weaned on average 12.4 piglets and subsequently 11.5 nurse piglets, whereas non-nurse weaned 11.7 piglets in their single weaning. There was no difference in re-service rate between nurse and non-nurse sows in the subsequent reproductive cycle. Subsequent litter size in the next reproductive cycle was higher for nurse sows than that for non-nurse sows (18.69 vs. 18.11 total born piglets; P < 0.001). Nurse sows were of a slightly lower parity than non-nurse sows (3.12 vs. 3.27, P < 0.001), and nurse sows had an increased weaning to estrus interval compared to non-nurse sows (4.23 vs. 4.19 days, P < 0.001). The results indicate that nurse sows were selected among sows nursing large litters and could therefore suggest that these sows represent the best percentile of sows in a given piggery. In conclusion, this survey indicated no negative effects of being selected as a nurse sow on the subsequent reproductive performance. On the contrary, nurse sows gave birth to more piglets compared to non-nurse sows in their subsequent litter.
Published: 2016

38. A new fireworm (Amphinomidae) from the Cretaceous of Lebanon identified from three-dimensionally preserved myoanatomy

Author: Parry, LA, Wilson, P, Sykes, D, Edgecombe, GD, Vinther, J, Parry, LA, Wilson, P, Sykes, D, Edgecombe, GD, and Vinther, J
Abstract: © 2015 Parry et al. Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. The Creative Commons Public Domain Dedication waiver (http://creativecommons.org/publicdomain/zero/1.0/) applies to the data made available in this article, unless otherwise stated. The attached file is the published version of the article., NHM Repository
Published: 2016

39. Reproductive performance of “nurse sows” in Danish piggeries

Author: Bruun, T.S., primary, Amdi, C., additional, Vinther, J., additional, Schop, M., additional, Strathe, A.B., additional, and Hansen, C.F., additional
Published: 2016
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40. Vetulicolians from the Lower Cambrian Sirius Passet Lagerstatte, North Greenland, and the polarity of morphological characters in basal deuterostomes

Author: Vinther, J, Smith, M, and Harper, D
Abstract: Vetulicolians are problematic Cambrian fossils with a debated phylogenetic history. Here, we describe two vetulicolian specimens from the Lower Cambrian Sirius Passet locality in North Greenland. One of the specimens is assigned to Ooedigera peeli gen. et sp. nov, whereas the other is retained under open nomenclature. The mode of tail flexibility has been debated in the literature, and we argue here that the tail normally flexed laterally to generate power strokes rather than dorsoventrally. The phylogenetic relationships of vetulicolians are discussed in the light of current knowledge of deuterostome phylogeny and morphology, and it is concluded that the best hypothesis on currently available evidence is that vetulicolians are a clade or paraphyletic assemblage of stem-Deuterostomata. The presence of a voluminous, sediment-filled anterior chamber suggests that the atrium may be a synapomorphy of deuterostomes. © The Palaeontological Association.
Published: 2011

41. Molecfit: A general tool for telluric absorption correction

Author: Smette, A., primary, Sana, H., additional, Noll, S., additional, Horst, H., additional, Kausch, W., additional, Kimeswenger, S., additional, Barden, M., additional, Szyszka, C., additional, Jones, A. M., additional, Gallenne, A., additional, Vinther, J., additional, Ballester, P., additional, and Taylor, J., additional
Published: 2015
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42. Large regional differences in incidence of arthroscopic meniscal procedures in the public and private sector in Denmark

Author: Hare, K. B., primary, Vinther, J. H., additional, Lohmander, L. S., additional, and Thorlund, J. B., additional
Published: 2015
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43. Constraints on the timescale of animal evolutionary history

Author: Benton, MJ, primary, Donoghue, PCJ, additional, Vinther, J, additional, Asher, RJ, additional, Friedman, M, additional, and Near, TJ, additional
Published: 2015
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44. Fossil evidence for evolution of the shape and color of penguin feathers

Author: Clarke, J.A., Ksepka, D.T., Salas-Gismondi, R., Altamirano, A. J., Shawkey, M.D., D'Alba, L., Vinther, J., De Vries, T.J., and Baby, Patrice
Abstract: Penguin feathers are highly modified in form and function, but there have been no fossils to inform their evolution. A giant penguin with feathers was recovered from the late Eocene (similar to 36 million years ago) of Peru. The fossil reveals that key feathering features, including undifferentiated primary wing feathers and broad body contour feather shafts, evolved early in the penguin lineage. Analyses of fossilized color-imparting melanosomes reveal that their dimensions were similar to those of non-penguin avian taxa and that the feathering may have been predominantly gray and reddish-brown. In contrast, the dark black-brown color of extant penguin feathers is generated by large, ellipsoidal melanosomes previously unknown for birds. The nanostructure of penguin feathers was thus modified after earlier macrostructural modifications of feather shape linked to aquatic flight.
Published: 2010

45. Machaeridians are Palaeozoic armoured annelids

Author: Vinther, J., Van Roy, P., and Briggs, D.E.G.
Abstract: The systematic affinities of several Palaeozoic skeletal taxa were only resolved when their soft-tissue morphology was revealed by the discovery of exceptionally preserved specimens. The conodonts provide a classic example, their tooth-like elements having been assigned to various invertebrate and vertebrate groups for more than 125 years until the discovery of their soft tissues revealed them to be crown-group vertebrates. Machaeridians, which are virtually ubiquitous as shell plates in benthic marine shelly assemblages ranging from Early Ordovician (Late Tremadoc) to Carboniferous, have proved no less enigmatic. The Machaeridia comprise three distinct families of worm-like animals, united by the possession of a dorsal skeleton of calcite plates that is rarely found articulated. Since they were first described 150 years ago machaeridians have been allied with barnacles, echinoderms, mollusks or annelids. Here we describe a new machaeridian with preserved soft parts, including parapodia and chaetae, from the Upper Tremadoc of Morocco, demonstrating the annelid affinity of the group. This discovery shows that a lineage of annelids evolved a dorsal skeleton of calcareous plates early in their history; it also resolves the affinities of a group of problematic Palaeozoic invertebrates previously known only from isolated elements and occasional skeletal assemblages.
Published: 2008

46. A preliminary study of iron isotope fractionation in marine invertebrates (chitons, Mollusca) in near-shore environments

Author: Emmanuel, S., primary, Schuessler, J. A., additional, Vinther, J., additional, Matthews, A., additional, and von Blanckenburg, F., additional
Published: 2014
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47. Flux calibration of medium-resolution spectra from 300 nm to 2500 nm: Model reference spectra and telluric correction

Author: Moehler, S., primary, Modigliani, A., additional, Freudling, W., additional, Giammichele, N., additional, Gianninas, A., additional, Gonneau, A., additional, Kausch, W., additional, Lançon, A., additional, Noll, S., additional, Rauch, T., additional, and Vinther, J., additional
Published: 2014
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48. Iron isotope fractionation in marine invertebrates in near shore environments

Author: Emmanuel, S., primary, Schuessler, J. A., additional, Vinther, J., additional, Matthews, A., additional, and von Blanckenburg, F., additional
Published: 2014
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49. Recalibrating Equus evolution using the genome sequence of an early Middle Pleistocene horse

Author: Orlando, L., Ginolhac, A., Zhang, G., Froese, D., Albrechtsen, A., Stiller, M., Schubert, M., Cappellini, E., Petersen, B., Moltke, I., Johnson, P., Fumagalli, M., Vilstrup, J., Raghavan, M., Korneliussen, T., Malaspinas, A., Vogt, J., Szklarczyk, D., Kelstrup, C., Vinther, J., Dolocan, A., Stenderup, J., Velazquez, A., Cahill, J., Rasmussen, M., Wang, X., Min, J., Zazula, G., Seguin-Orlando, A., Mortensen, C., Magnussen, K., Thompson, J., Weinstock, J., Gregersen, K., Roed, K., Eisenmann, V., Rubin, C., Miller, D., Antczak, D., Bertelsen, M., Brunak, S., Al-Rasheid, K., Ryder, O., Andersson, L., Mundy, J., Krogh, A., Gilbert, Thomas, Kjær, K., Sicheritz-Ponten, T., Jensen, L., Olsen, J., Hofreiter, M., Nielsen, R., Shapiro, B., Wang, Jun, Willerslev, E., Orlando, L., Ginolhac, A., Zhang, G., Froese, D., Albrechtsen, A., Stiller, M., Schubert, M., Cappellini, E., Petersen, B., Moltke, I., Johnson, P., Fumagalli, M., Vilstrup, J., Raghavan, M., Korneliussen, T., Malaspinas, A., Vogt, J., Szklarczyk, D., Kelstrup, C., Vinther, J., Dolocan, A., Stenderup, J., Velazquez, A., Cahill, J., Rasmussen, M., Wang, X., Min, J., Zazula, G., Seguin-Orlando, A., Mortensen, C., Magnussen, K., Thompson, J., Weinstock, J., Gregersen, K., Roed, K., Eisenmann, V., Rubin, C., Miller, D., Antczak, D., Bertelsen, M., Brunak, S., Al-Rasheid, K., Ryder, O., Andersson, L., Mundy, J., Krogh, A., Gilbert, Thomas, Kjær, K., Sicheritz-Ponten, T., Jensen, L., Olsen, J., Hofreiter, M., Nielsen, R., Shapiro, B., Wang, Jun, and Willerslev, E.
Abstract: The rich fossil record of equids has made them a model for evolutionary processes1. Here we present a 1.12-times coverage draft genome from a horse bone recovered from permafrost dated to approximately 560–780 thousand years before present (kyr bp)2, 3. Our data represent the oldest full genome sequence determined so far by almost an order of magnitude. For comparison, we sequenced the genome of a Late Pleistocene horse (43?kyr bp), and modern genomes of five domestic horse breeds (Equus ferus caballus), a Przewalski’s horse (E. f. przewalskii) and a donkey (E. asinus). Our analyses suggest that the Equus lineage giving rise to all contemporary horses, zebras and donkeys originated 4.0–4.5?million years before present (Myr bp), twice the conventionally accepted time to the most recent common ancestor of the genus Equus4, 5. We also find that horse population size fluctuated multiple times over the past 2?Myr, particularly during periods of severe climatic changes. We estimate that the Przewalski’s and domestic horse populations diverged 38–72?kyr bp, and find no evidence of recent admixture between the domestic horse breeds and the Przewalski’s horse investigated. This supports the contention that Przewalski’s horses represent the last surviving wild horse population6. We find similar levels of genetic variation among Przewalski’s and domestic populations, indicating that the former are genetically viable and worthy of conservation efforts. We also find evidence for continuous selection on the immune system and olfaction throughout horse evolution. Finally, we identify 29 genomic regions among horse breeds that deviate from neutrality and show low levels of genetic variation compared to the Przewalski’s horse. Such regions could correspond to loci selected early during domestication.
Published: 2013

50. MicroRNAs and Their Antagonists as Novel Therapeutics

Author: Erdmann, Volker A., Barciszewski, Jan, Vinther, J, Rukov, J, Shomron, N, Erdmann, Volker A., Barciszewski, Jan, Vinther, J, Rukov, J, and Shomron, N
Published: 2012

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