417 research outputs found
On the accuracy of GAIA radial velocities
We have obtained 782 real spectra and used them as inputs for 6700 automatic
cross-correlation runs to the aim of investigating the radial velocity accuracy
that GAIA could potentially achieve as function of spectral resolution and
signal-to-noise ratio. We have explored the dispersions 0.25, 0.5, 1 and 2
Ang/pix (bracketing the 0.75 Ang/pix currently baselined for the 8490--8740 Ang
GAIA range centered on the near-infrared CaII triplet) over S/N ranging from 10
to 110. We have carefully maintained the condition FWHM (PSF) = 2 pixels during
the acquisition of the 782 input spectra, and therefore the resolutions that we
have explored are 0.5, 1, 2 and 4 Ang corresponding to resolving powers
R=17200, 8600, 4300 and 2150. We have investigated late-F to early-M stars
(constituting the vast majority of GAIA targets), slowly rotating (V_{rot} sin
i = 4 km/sec, as for field stars at these spectral types), of solar metallicity
( = -0.07) and not binary. The results are accurately described by the
simple law: lg sigma = 0.6(lg S/N)^2 - 2.4(lg S/N) + 1.75(lg D) + 3, where
sigma is the cross-correlation standard error (in km/sec) and D is the spectral
dispersion (in Ang/pix). The spectral dispersion has turned out to be the
dominant factor governing the accuracy of radial velocities, with S/N being
less important and the spectral mis-match being a weak player. These results
are relevant not only within the GAIA context but also to ground-based
observers because the absence of telluric absorptions and proximity to the
wavelengths of peak emission make the explored 8490--8740 Ang interval an
interesting option for studies of cool stars with conventional telescopes.Comment: 12 pages, 2 figures, 5 tables, in press in Baltic Astronom
Spectroscopy and BVI photometry of the young open cluster NGC 6604
BVI photometry (from South Africa Astron. Obs.), Echelle high resolution
spectroscopy and AFOSC integral field spectroscopy (from Asiago, Italy) of the
young open cluster NGC 6604 are presented. Age, distance, reddening,
membership, radial and rotational velocities are derived and discussed. An age
of 5 million years, a distance of 1.7 kpc and a reddening E(B-V)=1.02 are
found. The cluster radial velocity is in agreement with the Hron (1987) model
for the Galaxy disk rotation. Pre-ZAMS objects are not present down to M_V =
+1.5 mag.Comment: accepted in Astron.Astrophys.Suppl. Figure 2 is degraded in
resolutio
Asiago eclipsing binaries program. III. V570 Per
The orbit and physical parameters of the previously unsolved SB2 EB V570 Per
are derived using high resolution Asiago Echelle spectroscopy and B, V
photo-electric photometry. The metallicity from chi^2 analysis is [M/H]=+0.02
+/- 0.03, and reddening from interstellar NaI and KI absorption lines is E(B-V)
=0.023 +/- 0.007. The two components have masses of 1.449 +/- 0.006 and 1.350
+/- 0.006 Msun and spectral types F3 and F5, respectively. They are both still
within the Main Sequence band (T_1 =6842 +/- 25 K, T_2 =6562 +/- 25 K from
chi^2 analysis, R_1 =1.523 +/- 0.030, R_2 =1.388 +/- 0.019 Rsun) and are
dynamically relaxed to co-rotation with the orbital motion (Vrot sin i_{1,2}
=40 and 36 (+/-1) km/sec). The distance to V570 Per obtained from the orbital
solution is 123 +/- 2 pc, in excellent agreement with the revised Hipparcos
distance of 123 +/- 11 pc. The observed properties of V570 Per components are
compared to BaSTI models computed on purpose for exactly the observed masses
and varied chemical compositions. This system is interesting since both
components have their masses in the range where the efficiency of convective
core overshooting has to decrease with the total mass as a consequence of the
decreasing size of the convective core during the central H-burning stage. Our
numerical simulations show that, a small but not null overshooting is required,
with efficiencies lambda_{OV} =0.14 and 0.11 for the 1.449 and 1.350 Msun
components, respectively. This confirms the finding of Paper II on the similar
system V505 Per. At the approx 0.8 Gyr age of the system, the element diffusion
has reduced the surface metallicity of the models from the initial [M/H]=+0.17
to [M/H]=+0.02, in perfect agreement with the spectroscopically derived
[M/H]=+0.02 +/- 0.03 value.Comment: accepted by A&A. This revised upload to astro-ph correct a formatting
error generated by uncorrect A&A style fil
Correlated radial velocity and X-ray variations in HD 154791/4U 1700+24
We present evidence for approximately 400-d variations in the radial velocity
of HD 154791 (V934 Her), the suggested optical counterpart of 4U 1700+24. The
variations are correlated with the previously reported approximately 400 d
variations in the X-ray flux of 4U 1700+24, which supports the association of
these two objects, as well as the identification of this system as the second
known X-ray binary in which a neutron star accretes from the wind of a red
giant. The HD 154791 radial velocity variations can be fit with an eccentric
orbit with period 404 +/- 3 d, amplitude K=0.75 +/- 0.12 km/s and eccentricity
e=0.26 +/- 0.15. There are also indications of variations on longer time scales
>~ 2000 d. We have re-examined all available ASM data following an unusually
large X-ray outburst in 1997-98, and confirm that the 1-d averaged 2-10 keV
X-ray flux from 4U 1700+24 is modulated with a period of 400 +/- 20 d. The mean
profile of the persistent X-ray variations was approximately sinusoidal, with
an amplitude of 0.108 +/- 0.012 ASM count/s (corresponding to 31% rms). The
epoch of X-ray maximum was approximately 40 d after the time of periastron
according to the eccentric orbital fit. If the 400 d oscillations from HD
154791/4U 1700+24 are due to orbital motion, then the system parameters are
probably close to those of the only other neutron-star symbiotic-like binary,
GX 1+4. We discuss the similarities and differences between these two systems.Comment: 6 pages, 2 figures; accepted by Ap
SN 2013df, a double-peaked IIb supernova from a compact progenitor and an extended H envelope
Optical observations of the type IIb SN 2013df from a few days to about 250
days after explosion are presented. These observations are complemented with UV
photometry taken by \textit{SWIFT} up to 60 days post-explosion. The
double-peak optical light curve is similar to those of SNe 1993J and 2011fu
although with different decline and rise rates. From the modelling of the
bolometric light curve, we have estimated that the total mass of synthesised
Ni in the explosion is M, while the ejecta mass is
M and the explosion energy erg. In
addition, we have estimated a lower limit to the progenitor radius ranging from
. The spectral evolution indicates that SN 2013df had a
hydrogen envelope similar to SN 1993J ( M). The line
profiles in nebular spectra suggest that the explosion was asymmetric with the
presence of clumps in the ejecta, while the [O\,{\sc i}]
, luminosities, may indicate that the progenitor
of SN 2013df was a relatively low mass star ( M).Comment: 18 pages, 11 figures, 9 tables, accepted for publication in MNRA
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