985 research outputs found
Photospheric properties and fundamental parameters of M dwarfs
M dwarfs are an important source of information when studying and probing the
lower end of the Hertzsprung-Russell (HR) diagram, down to the hydrogen-burning
limit. Being the most numerous and oldest stars in the galaxy, they carry
fundamental information on its chemical history. The presence of molecules in
their atmospheres, along with various condensed species, complicates our
understanding of their physical properties and thus makes the determination of
their fundamental stellar parameters more challenging and difficult. The aim of
this study is to perform a detailed spectroscopic analysis of the
high-resolution H-band spectra of M dwarfs in order to determine their
fundamental stellar parameters and to validate atmospheric models. The present
study will also help us to understand various processes, including dust
formation and depletion of metals onto dust grains in M dwarf atmospheres. The
high spectral resolution also provides a unique opportunity to constrain other
chemical and physical processes that occur in a cool atmosphere The
high-resolution APOGEE spectra of M dwarfs, covering the entire H-band, provide
a unique opportunity to measure their fundamental parameters. We have performed
a detailed spectral synthesis by comparing these high-resolution H-band spectra
to that of the most recent BT-settl model and have obtained fundamental
parameters such as effective temperature, surface gravity, and metallicity
(Teff, log g and [Fe/H]) respectively.Comment: 15 pages, 10 figures, accepted for publication in A&
The Effective temperature scale of M dwarfs from spectral synthesis
We present a comparison of low-resolution spectra of 60 stars covering the
whole M-dwarf sequence. Using the most recent PHOENIX BT-Settl stellar model
atmospheres (see paper by F. Allard, in this book) we do a first quantitative
compari- son to our observed spectra in the wavelength range 550-950 nm. We
perform a first confrontation between models and observations and we assign an
effective tempera- tures to the observed M-dwarfs. Teff-spectral type relations
are then compared with the published ones. This comparison also aims at
improving the models' opacities.Comment: To be published in the on-line version of the Proceedings of Cool
Stars 16 (ASP Conference Series) New version with bibliography correcte
Progress in Modeling Very Low Mass Stars, Brown Dwarfs, and Planetary Mass Objects
We review recent advancements in modeling the stellar to substellar
transition. The revised molecular opacities, solar oxygen abundances and cloud
models allow to reproduce the photometric and spectroscopic properties of this
transition to a degree never achieved before, but problems remain in the
important M-L transition characteristic of the effective temperature range of
characterizable exoplanets. We discuss of the validity of these classical
models. We also present new preliminary global Radiation HydroDynamical M
dwarfs simulations.Comment: Submitted to Mem. S. A. It. Supp
Detection and characterisation of two VLM binaries: LP 1033-31 and LP 877-72
Using the high-resolution near-infrared adaptive optics imaging from the NaCo
instrument at the Very Large Telescope, we report the discovery of a new binary
companion to the M-dwarf LP 1033-31 and also confirm the binarity of LP 877-72.
We have characterised both the stellar systems and estimated the properties of
their individual components. We have found that LP 1033-31 AB with the spectral
type of M4.5+M4.5 has a projected separation of 6.71.3 AU. Whereas with
the spectral type of M1+M4, the projected separation of LP 877-72 AB is
estimated to be 45.80.3 AU. The binary companions of LP 1033-31 AB are
found to have similar masses, radii, effective temperatures, and log with
the estimated values of 0.200.04 , 0.220.03
, 3200 K, 5.060.04. However, the primary of LP 877-72 AB
is found to be twice as massive as the secondary with the derived mass of
0.5200.006 . The radius and log for the primary of LP
877-72 AB are found to be 1.8 and 0.95 times that of the secondary component
with the estimated values of 0.4920.011 and
4.7680.005, respectively. With an effective temperature of 375015 K,
the primary of LP 877-72 AB is also estimated to be 400 K hotter than the
secondary component. We have also estimated the orbital period of LP 1033-31
and LP 877-72 to be 28 and 349 yr, respectively. The binding
energies for both systems are found to be 10 erg, which signifies
both systems are stable.Comment: 14 pages, 6 figures, accepted for publication in MNRA
A high resolution spectroscopic atlas of M subdwarfs - Effective temperature and metallicity
Context. M subdwarfs are metal poor and cool stars. They are important probes
of the old galactic populations. However, they remain elusive due to their low
luminosity. Observational and modeling efforts are required to fully understand
their physics and to investigate the effects of metallicity in their cool
atmospheres.
Aims. We perform a detailed study of a sample of subdwarfs to determine their
stellar parameters and constrain the stat-of-the art atmospheric models.
Methods. We present UVES/VLT high resolution spectra of three late-K
subdwarfs and 18 M subdwarfs. Our atlas covers the optical region from 6400 AA
up to the near infrared at 8900 AA. We show spectral details of cool
atmospheres at very high resolution (R= 40 000) and compare with synthetic
spectra computed from the recent BT-Settl atmosphere models.
Results. Our comparison shows that molecular features (TiO, VO, CaH), and
atomic features (Fe I, Ti I, Na I, K I) are well fitted by current models. We
produce an effective temperature versus spectral type relation all over the
subdwarf spectral sequence. Thanks to the high resolution of our spectra, we
perform a detailed comparison of line profiles of individual elements such as
Fe I, Ca II, Ti I, and are able to determine accurate metallicities of these
stars. These determinations contribute to calibrate the relation between
metallicity and molecular band strength indices from low-resolution spectra.
Conclusions. This work shows that the new generation of models are able to
reproduce various spectral features of M subdwarfs. Working with these high
resolution spectra allowed us to disentangle the atmospheric parameters
(effective temperature, gravity, metallicity), which is not possible when using
low resolution spectroscopy or photometry.Comment: 15 pages, 20 figures, 2 tables, accepted for publication in Astronomy
and Astrophysic
The effective temperature scale of M dwarfs
Context. Despite their large number in the Galaxy, M dwarfs remain elusive objects and the modeling of their photosphere has long remained a challenge (molecular opacities, dust cloud formation). Aims. Our objectives are to validate the BT-Settl model at
The Effective Temperature Scale of M dwarfs
Despite their large number in the Galaxy, M dwarfs remain elusive objects and
the modeling of their photospheres has long remained a challenge (molecular
opacities, dust cloud formation). Our objectives are to validate the BT-Settl
model atmospheres, update the M dwarf T eff -spectral type relation, and find
the atmospheric parameters of the stars in our sample. We compare two samples
of optical spectra covering the whole M dwarf sequence with the most recent
BT-Settl synthetic spectra and use a \c{hi}2 minimization technique to
determine Teff . The first sample consists of 97 low-resolution spectra
obtained with NTT at La Silla Observatory. The second sample contains 55
mid-resolution spectra obtained at the Siding Spring Observatory (SSO). The
spectral typing is realized by comparison with already classified M dwarfs. We
show that the BT-Settl synthetic spectra reproduce the slope of the spectral
energy distribution and most of its features. Only the CaOH band at 5570{\AA}
and AlH and NaH hydrides in the blue part of the spectra are still missing in
the models. The Teff-scale obtained with the higher resolved SSO 2.3 m spectra
is consistent with that obtained with the NTT spectra. We compare our Teff
scale with those of other authors and to published isochrones using the
BT-Settl colors. We also present relations between effective temperature,
spectral type and colors of the M dwarfs.Comment: 16 pages, 6 figures, accepted for publication in A&
First Results from MFOSC-P : Low Resolution Optical Spectroscopy of a Sample of M dwarfs within 100 parsecs
Mt. Abu Faint Object Spectrograph and Camera (MFOSC-P) is an in-house
developed instrument for Physical Research Laboratory (PRL) 1.2m telescope at
Mt. Abu India, commissioned in February 2019. Here we present the first science
results derived from the low resolution spectroscopy program of a sample of M
Dwarfs carried out during the commissioning run of MFOSC-P between
February-June 2019. M dwarfs carry great significance for exoplanets searches
in habitable zone and are among the promising candidates for the observatory's
several ongoing observational campaigns. Determination of their accurate
atmospheric properties and fundamental parameters is essential to constrain
both their atmospheric and evolutionary models. In this study, we provide a low
resolution (R500) spectroscopic catalogue of 80 bright M dwarfs (J10)
and classify them using their optical spectra. We have also performed the
spectral synthesis and minimisation techniques to determine their
fundamental parameters viz. effective temperature and surface gravity by
comparing the observed spectra with the most recent BT-Settl synthetic spectra.
Spectral type of M dwarfs in our sample ranges from M0 to M5. The derived
effective temperature and surface gravity are ranging from 4000 K to 3000 K and
4.5 to 5.5 dex, respectively. In most of the cases, the derived spectral types
are in good agreement with previously assigned photometric classification.Comment: Accepted for Publication in MNRA
Physical insights from the spectrum of the radio halo in MACS J0717.5+3745
We present new LOFAR observations of the massive merging galaxy cluster MACS
J0717.5+3745. The cluster hosts the most powerful radio halo known to date.
These new observations, in combination with published uGMRT (300850 MHz) and
VLA (16.5 GHz) data, reveal that the halo is more extended than previously
thought, with a largest linear size of . The halo shows a
steep spectrum () and a
steepening () above 1.5 GHz.
We find a strong scattering in spectral index maps on scales of 50100 kpc.
We suggest that such a strong scattering may be a consequence of the regime
where inverse Compton dominate the energy losses of electrons. The spectral
index becomes steeper and shows an increased curvature in the outermost regions
of the halo. We combined the radio data with \textit{Chandra} observations to
investigate the connection between the thermal and non-thermal components of
the intracluster medium (ICM). Despite a significant substructure in the halo
emission, the radio brightness correlates strongly with the X-ray brightness at
all observed frequencies. The radio-versus-X-ray brightness correlation slope
steepens at a higher radio frequency (from to
) and the spectral index shows a significant
anti correlation with the X-ray brightness. Both pieces of evidence further
support a spectral steepening in the external regions. The compelling evidence
for a steep spectral index, the existence of a spectral break above 1.5 GHz,
and the dependence of radio and X-ray surface brightness correlation on
frequency are interpreted in the context of turbulent reacceleration models.
Under this scenario, our results allowed us to constrain that the turbulent
kinetic pressure of the ICM is up to 10%.Comment: 16 pages, 12 figures, accepted for publication in A&
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