8 research outputs found
The CARMENES search for exoplanets around M dwarfs: rubidium abundances in nearby cool stars
Due to their ubiquity and very long main-sequence lifetimes, abundance determinations in M dwarfs provide a powerful and alternative tool to GK dwarfs to study the formation and chemical enrichment history of our Galaxy. In this study, abundances of the neutroncapture elements Rb, Sr, and Zr are derived, for the first time, in a sample of nearby M dwarfs. We focus on stars in the metallicity range â0.5 Ë· 0.0 is attained at metallicities higher than solar. These are surprising results, never seen for any other heavy element, and are difficult to understand within the formulation of the s- and r-processes, both contributing sources to the Galactic Rb abundance. We discuss the reliability of these findings for Rb in terms of non-LTE (local thermodynamic equilibrium) effects, stellar activity, or an anomalous Rb abundance in the Solar System, but no explanation is found. We then interpret the full observed [Rb/Fe] versus [Fe/H] trend within the framework of theoretical predictions from state-of-the-art chemical evolution models for heavy elements, but a simple interpretation is not found either. In particular, the possible secondary behaviour of the [Rb/Fe] ratio at super-solar metallicities would require a much larger production of Rb than currently predicted in AGB stars through the s-process without overproducing Sr and Zr. Python libraries Matplotlib, NumPy, SciPy and collection of software packages AstroPy
Discovery of the elusive carbonic acid (HOCOOH) in space
After a quarter century since the detection of the last interstellar
carboxylic acid, acetic acid (CHCOOH), we report the discovery of a new
one, the cis-trans form of carbonic acid (HOCOOH), toward the Galactic Center
molecular cloud G+0.693-0.027. HOCOOH stands as the first interstellar molecule
containing three oxygen atoms and also the third carboxylic acid detected so
far in the interstellar medium. Albeit the limited available laboratory
measurements (up to 65 GHz), we have also identified several pairs of unblended
lines directly in the astronomical data (between 75-120 GHz), which allowed us
to slightly improve the set of spectroscopic constants. We derive a column
density for cis-trans HOCOOH of = (6.4 0.4) 10
cm, which yields an abundance with respect to molecular H of 4.7
10. Meanwhile, the extremely low dipole moment (about fifteen
times lower) of the lower-energy conformer, cis-cis HOCOOH, precludes its
detection. We obtain an upper limit to its abundance with respect to H of
1.2 10, which suggests that cis-cis HOCOOH might be
fairly abundant in interstellar space, although it is nearly undetectable by
radio astronomical observations. We derive a cis-cis/cis-trans ratio 25,
consistent with the smaller energy difference between both conformers compared
with the relative stability of trans- and cis-formic acid (HCOOH). Finally, we
compare the abundance of these acids in different astronomical environments,
further suggesting a relationship between the chemical content found in the
interstellar medium and the chemical composition of the minor bodies of the
Solar System, which could be inherited during the star formation process.Comment: Accepted for publication in The Astrophysical Journa
First glycine isomer detected in the interstellar medium: glycolamide (NHC(O)CHOH)
We report the first detection in the interstellar medium of a
CHON isomer: -glycolamide (NHC(O)CHOH). The exquisite
sensitivity at sub-mK levels of an ultra-deep spectral survey carried out with
the Yebes 40m and IRAM 30m telescopes towards the G+0.693-0.027 molecular cloud
have allowed us to unambiguously identify multiple transitions of this species.
We derived a column density of (7.4 0.7)10 cm,
which implies a molecular abundance with respect to H of
5.510. The other CHON isomers, including the
higher-energy conformer of glycolamide, and two conformers of glycine,
were not detected. The upper limit derived for the abundance of glycine
indicates that this amino acid is surely less abundant than its isomer
glycolamide in the ISM. The abundances of the CHON isomers cannot
be explained in terms of thermodynamic equilibrium, and thus chemical kinetics
need to be invoked. While the low abundance of glycine might not be surprising,
based on the relative low abundances of acids in the ISM compared to other
compounds (e.g. alcohols, aldehydes or amines), several chemical pathways can
favour the formation of its isomer glycolamide. It can be formed through
radical-radical reactions on the surface of dust grains. The abundances of
these radicals can be significantly boosted in an environment affected by a
strong ultraviolet field induced by cosmic rays, such as that expected in
G+0.693-0.027. Therefore, as shown by several recent molecular detections
towards this molecular cloud, it stands out as the best target to discover new
species with carbon, oxygen and nitrogen with increasing chemical complexity.Comment: Accepted in The Astrophysical Journal Letter
HORuS transmission spectroscopy and revised planetary parameters of KELT-7 b
We report on the high-resolution spectroscopic observations of two planetary transits of the hot Jupiter KELT-7b (Mp = 1.28 +/- 0.17Mjup, Teq=2028 K) observed with the High Optical Resolution Spectrograph (HORuS) mounted on the 10.4-m Gran Telescopio Canarias (GTC). A new set of stellar parameters are obtained for the rapidly rotating parent star from the analysis of the spectra. Using the newly derived stellar mass and radius, and the planetary transit data of the Transiting Exoplanet Survey Satellite (TESS) together with the HORuS velocities and the photometric and spectroscopic data available in the literature, we update and improve the ephemeris of KELT-7b. Our results indicate that KELT-7 has an angle Lamda = -10.55 +/- 0.27 deg between the sky projections of the starâs spin axis and the planetâs orbital axis. By combining this angle and our newly derived stellar rotation period of 1.38 +/- 0.05 d, we obtained a 3D obliquity Psi = 12.4 +/- 11.7 deg (or 167.6 deg), thus reinforcing that KELT-7 is a well-aligned planetary system. We search for the presence of Halfa, Li i, Na i, Mg i, and Ca ii features in the transmission spectrum of KELT-7b but we are only able to determine upper limits of 0.08â1.4 % on their presence after accounting for the contribution of the stellar variability to the extracted planetary spectrum. We also discuss the impact of stellar variability in the planetary data. Our results reinforce the importance of monitoring the parent star when performing high-resolution transmission spectroscopy of the planetary atmosphere in the presence of stellar activity
Precursors of the RNA-world in space: Detection of ()-1,2-ethenediol in the interstellar medium, a key intermediate in sugar formation
We present the first detection of ()-1,2-ethenediol, (CHOH), the enol
form of glycolaldehyde, in the interstellar medium towards the G+0.693-0.027
molecular cloud located in the Galactic Center. We have derived a column
density of (1.80.1)10 cm, which translates into a
molecular abundance with respect to molecular hydrogen of
1.310. The abundance ratio between glycolaldehyde and
()-1,2-ethenediol is 5.2. We discuss several viable formation routes
through chemical reactions from precursors such as HCO, HCO, CHOH or
CHCHOH. We also propose that this species might be an important precursor
in the formation of glyceraldehyde (HOCHCHOHCHO) in the interstellar medium
through combination with the hydroxymethylene (CHOH) radical.Comment: Accepted for publication in The Astrophysical Journal Letter
The CARMENES search for exoplanets around M dwarfs Diagnostic capabilities of strong K I lines for photosphere and chromosphere
There are several strong K I lines found in the spectra of M dwarfs, among them the doublet near 7700 angstrom and another doublet near 12 500 angstrom. We study these optical and near-infrared doublets in a sample of 324 M dwarfs, observed with CARMENES, the high-resolution optical and near-infrared spectrograph at Calar Alto, and investigate how well the lines can be used as photospheric and chromospheric diagnostics. Both doublets have a dominant photospheric component in inactive stars and can be used as tracers of effective temperature and gravity. For variability studies using the optical doublet, we concentrate on the red line component because this is less prone to artefacts from telluric correction in individual spectra. The optical doublet lines are sensitive to activity, especially for M dwarfs later than M5.0 V where the lines develop an emission core. For earlier type M dwarfs, the red component of the optical doublet lines is also correlated with Ha activity. We usually find positive correlation for stars with Ha in emission, while early-type M stars with Ha in absorption show anti-correlation. During flares, the optical doublet lines can exhibit strong fill-in or emission cores for our latest spectral types. On the other hand, the near-infrared doublet lines very rarely show correlation or anti-correlation to Ha and do not change line shape significantly even during the strongest observed flares. Nevertheless, the near-infrared doublet lines show notable resolved Zeeman splitting for about 20 active stars which allows to estimate the magnetic fields B
The CARMENES search for exoplanets around M dwarfs Stellar atmospheric parameters of target stars with STEPARSYN
We determined effective temperatures, surface gravities, and metallicities for a sample of 343 M dwarfs observed with CARMENES, the double-channel, high-resolution spectrograph installed at the 3.5 m telescope at Calar Alto Observatory. We employed STEPARSYN, a Bayesian spectral synthesis implementation particularly designed to infer the stellar atmospheric parameters of late-type stars following a Markov chain Monte Carlo approach. We made use of the BT-Settl model atmospheres and the radiative transfer code turbospectrum to compute a grid of synthetic spectra around 75 magnetically insensitive Fel and Til lines plus the TiO gamma and epsilon bands. To avoid any potential degeneracy in the parameter space, we imposed Bayesian priors on T-eff and log g based on the comprehensive, multi-band photometric data available for the sample. We find that this methodology is suitable down to M7.0 V, where refractory metals such as Ti are expected to condense in the stellar photospheres. The derived Teff, log g, and [Fe/H] range from 3000 to 4200 K, 4.5 to 5.3 dex, and -0.7 to 0.2 dex, respectively. Although our T (eff) scale is in good agreement with the literature, we report large discrepancies in the [Fe/H] scales, which might arise from the different methodologies and sets of lines considered. However, our [Fe/H] is in agreement with the metallicity distribution of FGK-type stars in the solar neighbourhood and correlates well with the kinematic membership of the targets in the Galactic populations. Lastly, excellent agreement in T (eff) is found for M dwarfs with interferometric angular diameter measurements, as well as in the [Fe/H] between the components in the wide physical FGK+M and M+M systems included in our sample
First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
We report the first detection in the interstellar medium (ISM) of a C _2 H _5 O _2 N isomer: syn -glycolamide (NH _2 C(O)CH _2 OH). The exquisite sensitivity at sub-mK levels of an ultradeep spectral survey carried out with the Yebes 40 m and IRAM 30 m telescopes toward the G+0.693â0.027 molecular cloud has allowed us to unambiguously identify multiple transitions of this species. We derived a column density of (7.4 ± 0.7) Ă 10 ^12 cm ^â2 , which implies a molecular abundance with respect to H _2 of 5.5 Ă 10 ^â11 . The other C _2 H _5 O _2 N isomers, including the higher-energy anti conformer of glycolamide and two conformers of glycine, were not detected. The upper limit derived for the abundance of glycine indicates that this amino acid is surely less abundant than its isomer glycolamide in the ISM. The abundances of the C _2 H _5 O _2 N isomers cannot be explained in terms of thermodynamic equilibrium; thus, chemical kinetics need to be invoked. While the low abundance of glycine might not be surprising, based on the relative low abundances of acids in the ISM compared to other compounds (e.g., alcohols, aldehydes, or amines), several chemical pathways can favor the formation of its isomer glycolamide. It can be formed through radicalâradical reactions on the surface of dust grains. The abundances of these radicals can be significantly boosted in an environment affected by a strong ultraviolet field induced by cosmic rays, such as that expected in G+0.693â0.027. Therefore, as shown by several recent molecular detections toward this molecular cloud, it stands out as the best target to discover new species with carbon, oxygen, and nitrogen with increasing chemical complexity