Search

Based on high-resolution 3D data cubes from a magnetohydrodynamic (MHD) turbulence simulation, we study how to reveal the direction of the magnetic field within the optically thick interstellar medium by using the velocity gradient technique (VGT), correlation function anisotropy (CFA), and principal component analysis of anisotropies (PCAA). Considering the CO molecular tracers as a tracing method for radiative transfer processes, we find that the VGT and CFA can successfully trace the orientation of mean magnetic fields, which is in good agreement with the low-resolution numerical results obtained in the case of an optically thin medium. Similar to the simulation of an optically thin ISM, our simulations show that PCCA is still unusable in optically thick media. The synergetic application of the VGT and CFA to high-resolution spectroscopic observations is expected to yield valuable information on the interstellar magnetic field.

NIRPS is a near-infrared (YJH bands), fiber-fed, high-resolution precision radial velocity (pRV) spectrograph currently under construction for deployment at the ESO 3.6-m telescope in La Silla, Chile. Through the use of a dichroic, NIRPS will be operated simultaneously with the optical HARPS pRV spectrograph and will be used to conduct ambitious planet-search and characterization surveys through a 720-night of guaranteed time allocation. NIRPS aims at detecting and characterizing Earth-like planets in the habitable zone of low-mass dwarfs and obtain high-accuracy transit spectroscopy of exoplanets. Here we present a summary of the full performances obtained in laboratory tests conducted at Universite Laval (Canada), and the first results of the on-going on-sky commissioning of the front-end. Science operations of NIRPS is expected to start in late-2020, enabling significant synergies with major space and ground instruments such as the JWST, TESS, ALMA, PLATO and the ELT.

We present the confirmation of two new planets transiting the nearby mid-M dwarf LTT 3780 (TIC 36724087, TOI-732, $V=13.07$, $K_s=8.204$, $R_s$=0.374 R$_{\odot}$, $M_s$=0.401 M$_{\odot}$, d=22 pc). The two planet candidates are identified in a single TESS sector and are validated with reconnaissance spectroscopy, ground-based photometric follow-up, and high-resolution imaging. With measured orbital periods of $P_b=0.77$ days, $P_c=12.25$ days and sizes $r_{p,b}=1.33\pm 0.07$ R$_{\oplus}$, $r_{p,c}=2.30\pm 0.16$ R$_{\oplus}$, the two planets span the radius valley in period-radius space around low mass stars thus making the system a laboratory to test competing theories of the emergence of the radius valley in that stellar mass regime. By combining 63 precise radial-velocity measurements from HARPS and HARPS-N, we measure planet masses of $m_{p,b}=2.62^{+0.48}_{-0.46}$ M$_{\oplus}$ and $m_{p,c}=8.6^{+1.6}_{-1.3}$ M$_{\oplus}$, which indicates that LTT 3780b has a bulk composition consistent with being Earth-like, while LTT 3780c likely hosts an extended H/He envelope. We show that the recovered planetary masses are consistent with predictions from both photoevaporation and from core-powered mass loss models. The brightness and small size of LTT 3780, along with the measured planetary parameters, render LTT 3780b and c as accessible targets for atmospheric characterization of planets within the same planetary system and spanning the radius valley., Comment: Accepted to AJ. 8 figures, 6 tables. CSV file of the RV measurements (i.e. Table 2) are included in the source code

Laser frequency combs (LFCs) are well on their way to becoming the next-generation calibration sources for precision astronomical spectroscopy. This development is considered key in the hunt for low-mass rocky exoplanets around solar-type stars whose discovery with the radial-velocity method requires cm/s Doppler precision. In order to prove such precise calibration with an LFC, it must be compared to another calibrator of at least the same precision. Being the best available spectrograph calibrator, this means comparing it to a second - fully independent - LFC. This test had long been pending, but our installation of two LFCs at the ultra-stable spectrograph HARPS presented the so far unique opportunity for simultaneous calibrations with two separate LFCs. Although limited in time, the test results confirm the 1 cm/s stability that has long been anticipated by the astronomical community., 22 pages, 14 figures. View the Nature Astronomy publication under https://rdcu.be/b1tMB . Nature Astronomy article available under https://www.nature.com/articles/s41550-020-1010-x

NIRPS (Near Infra Red Planet Searcher) is a new ultra-stable infrared ( YJH) fiber-fed spectrograph that will be installed on ESO’s 3.6-m telescope in La Silla, Chile. Aiming at achieving a precision of 1 m/s, NIRPS is designed to find rocky planets orbiting M dwarfs, and will operate together with HARPS (High Accuracy Radial velocity Planet Searcher). In this paper we describe NIRPS science cases, present its main technical characteristics and its development status.

We report on the installation of a laser frequency comb (LFC) at the HARPS spectrograph, which we characterize relative to a second LFC that we had brought to HARPS for testing. This allowed us for the first time to probe the relative stability of two independent astronomical LFCs over an extended wavelength range. Both LFCs covered the spectral range of HARPS at least from 460 to 690 nm. After optimization of the fiber coupling to HARPS to suppress modal noise, a relative stability of the two LFCs in the low cm/s range was obtained. In combination with the results of our four earlier LFC test campaigns on HARPS, the available data now cover a time span of more than six years.

We present a re-engineered version of the laser frequency comb that has proven a few-cm/s calibration repeatability on the HARPS spectrograph during past campaigns. The new design features even better performance characteristics. The newly arranged oscillator, filter cavities and fiber injection for spectral broadening allow robust long term operation, controlled from a remote site. Its automation features enable easy operation for non-experts. The system is being prepared for installation on the HARPS spectrograph in fall of 2014, and will subsequently become available to the astronomical community.

New spectroscopic observations of the double-lined chromospherically active binary 54 Camelopardalis (=AE Lyncis) have been obtained, resulting in improved orbital elements and the determination of the fundamental properties of the system. 54 Cam has a period of 11.06794 days, an eccentricity of 0.125, and a mass ratio of 0.9945. The spectral types are F8 IV–V and G5 IV, positioning the components on opposite sides of the Hertzsprung gap. From a comparison with theoretical evolutionary tracks, the masses are estimated to be 1.60 and 1.59 M⊙ for the G and F stars, respectively, while the radii are 3.7 and 3.2 R⊙. Only the G star is chromospherically active. 54 Cam is particularly interesting since the F star is the brighter star at blue and red wavelengths, but the G star is slightly more massive and evolved. Both stars appear to be pseudosynchronously rotating, and the orbital and rotational inclinations are aligned. The lithium abundances of the two components are significantly different but consistent with standard theory, supporting the conclusion that both stars are more massive than the lithium-dip stars.

Esse trabalho pretende, através de uma abordagem didática, apresentar a íntima ligação entre o magnetismo estelar e o geomagnetismo, ressaltando a importância da teoria de dínamo na compreensão do magnetismo no universo. This work aims to show, through a didactic approach, the intimate connection between stellar magnetism and geomagnetism, revealing the importance of the dynamo theory to understanding of magnetism in the universe.

The laser frequency comb, with its extreme precision, opens a new window for high precision spectroscopy for current facilities, as well as for the ELT's. We report on the latest performance of the laser frequency comb obtained in combination with the HARPS spectrograph, which allowed calibration with cm/sec repeatability. The laser frequency comb system developed is described. Details of its laboratory set-up, characterization and integration with HARPS are shown. The results of the recent test campaigns are presented, showing excellent performance in terms of repeatability as well as wavelength coverage. Preliminary on sky data and next activities to integrate such a system in HARPS are presented.

G and K giants are a class of radial velocity (RV) variables. One reason for this variability are planetary companions which are indicated in time series of stellar spectra. Since 2004 these spectra in the visual range were obtained with the high resolution coude echelle spectrograph mounted on the 2 m telescope of the Thuringer Landessternwarte Tautenburg (TLS) for a northern sample of 62 very bright K giants. In the South around 300 G and K giants were observed with HARPS mounted on the 3.6 m telescope on La Silla. The TLS sample contains at least 11 stars (18%) which show low‐amplitude, long‐period RV variations most likely due to planets. This percentage of planet frequency is confirmed by preliminary results of the HARPS study. Moreover the TLS survey seems to indicate that giant planets do not favour metal‐rich stars, are more massive, and have longer periods than those found around solar‐type host stars.

4 pages, 3 figures.-- Supporting Online Material: Text, Fig. S1, Table S1 and References, available at: http://www.sciencemag.org/cgi/content/full/322/5901/558/DC1, Oscillations of the Sun have been used to understand its interior structure. The extension of similar studies to more distant stars has raised many difficulties despite the strong efforts of the international community over the past decades. The CoRoT (Convection Rotation and Planetary Transits) satellite, launched in December 2006, has now measured oscillations and the stellar granulation signature in three main sequence stars that are noticeably hotter than the sun. The oscillation amplitudes are about 1.5 times as large as those in the Sun; the stellar granulation is up to three times as high. The stellar amplitudes are about 25% below the theoretic values, providing a measurement of the nonadiabaticity of the process ruling the oscillations in the outer layers of the stars.

In preparation for the COROT space mission, we determined the fundamental parameters (spectral type, temperature, gravity, vsini) of the Be stars observable by COROT in its seismology fields (64 Be stars). We applied a careful and detailed modeling of the stellar spectra, taking into account the veiling caused by the envelope, as well as the gravitational darkening and stellar flattening due to rapid rotation. Evolutionary tracks for fast rotators were used to derive stellar masses and ages. The derived parameters will be used to select Be stars as secondary targets (i.e. observed for 5 consecutive months) and short-run targets of the COROT mission. Furthermore, we note that the main part of our stellar sample is falling in the second half of the main sequence life time, and that in most cases the luminosity class of Be stars is inaccurate in characterizing their evolutionary status., 25 pages, 9 figures, Accepted for publication in A&A

We present and discuss statistical relation between rotation and X-ray activity for giant and supergiant stars.”

No presente trabalho investigamos alguns efeitos físicos que acontecem na estrutura e evolução estelar. Focalizamos nossa atenção em estrelas de baixa massa na pré-sequência principal. Incluímos alguns efeitos físicos no código de estrutura e evolução estelar ATON2.3, escrito pelo Dr. Ítalo Mazzitelli (1989) e posteriormente modificado pelo Dr. Luiz Themystokliz Sanctos Mendes (1999b) para adicionar os efeitos de rotação e redistribuição interna de momento angular. Com o objetivo de economizar tempo computacional, introduzimos o mecanismo de parada de controle (checkpoint), que permite iniciar uma dada execução em um estágio de evolução intermideário, desde que os passos iniciais tenham sido devidamente registrados. Essas modificações foram feitas juntamente com um controle completo de variáveis não inicializadas, precisão e reestruturação do programa, visando futuramente paralelizar o código. Introduzimos efeitos combinados de rotação e forças de maré na configuração de equilíbrio das estrelas. Estes efeitos perturbadores, contidos na função potencial total, desviam a forma da estrela da aproximação esfericamente simétrica. Usamos o método de Kippenhahn & Thomas (1970), posteriormente aperfeiçoado por Enda & Sofia (1976). À função potencial obtida por estes autores, adicionamos termosrelacionados à forças de maré e àqueles relacionados à parte não simétrica do potencial gravitacional devido à distorção que tais forças causam na figura da estrela. Seguindo esta aproximação, corrigimos as equações constitutivas a fim de obter uma configuração estrutural de uma estrela distorcida. Cálculos de constantes de estrutura interna e raios de giração foram incluídos no código. Várias trilhas evolutivas foram geradas com os novos modelos, incluindo as quantidades mencionadas acima. Os novos modelos foram testados através de dados observacionais das dimensões absolutas, taxa de movimento apsidal e abundância de lítio das componentes do sistema binário eclipsante EK Cephei. No presente trabalho, também apresentamos estimativas teóricas do convective turnover time, Tc e Números de Rossby, Ro, para estrelas com massas semelhantes à massa solar, com rotação e na pré-sequência principal. Ro está relacionado com a força magnética na teoria do dínamo e, pelo menos para estrelas na seqüência principal, observa-se uma correlação entre rotação e atividade estelar. Incluímos também a possibilidade de utilizar modelos de atmosferas não cinza, com o objetivo de seguir a evolução estelar de estrelas de baixa massa desde estágiosbem iniciais, caracterizados por baixa gravidade. Adotamos os modelos NextGen e ATLAS9 de atmosferas estelares. Usando os nossos novos modelos não-cinza, geramos vários conjuntos de trilhas evolutivas, partindo da pré-sequência principal. Tais trilhas foram usadas para investigar algumas propriedades físicas e rotacionais de estrelas jovens na Nebulosa de Orion. Comparações entre resultados teóricos e dados observacionais, permitiram-nos obter informações sobre esta classe de objetos, principalmente no que diz respeito à distribuição inicial de momento angular. A interpretação dos dados depende fortemente das considerações físicas feitas no modelos, sendo a eficiência da convecção a mais importante. Nossa análise indica que um segundo parâmentro é necessário para descrever a convecção na pré-sequência principal. Tal parâmetro está possivelmente relacionado ao efeito estrutural de um campo magnético gerado por efeito dínamo.