112 research outputs found
Evidence for deuterium astration in the planetary nebula Sh2-216?
We present FUSE observations of the line of sight to WD0439+466 (LS V +46
21), the central star of the old planetary nebula Sh2-216. The FUSE data shows
absorption by many interstellar and stellar lines, in particular D I, H2 (J = 0
- 9), HD (J = 0 - 1), and CO. Many other stellar and ISM lines are detected in
the STIS E140M HST spectra of this sightline, which we use to determine N(HI).
We derive, for the neutral gas, D/H=(0.76 +0.12 -0.11)E-5, O/H = (0.89 +0.15
-0.11)E-4 and N/H = (3.24 +0.61-0.55)E-5. We argue that most of the gas along
this sightline is associated with the planetary nebula. The low D/H ratio is
likely the result of this gas being processed through the star (astrated) but
not mixed with the ISM. This would be the first time that the D/H ratio has
been measured in predominantly astrated gas. The O/H and N/H ratios derived
here are lower than typical values measured in other planetary nebulae likely
due to unaccounted for ionization corrections.Comment: Accepted for publication is ApJ
Efectividad del cipionato de estradiol inyectado al final de un tratamiento con progesterona sobre la eficiencia reproductiva
El cipionato de estradiol (CPE) ha sido utilizado para reemplazar al benzoato de estradiol (BE) administrado vía IM 24 h después de retirado el dispositivo intravaginal con progesterona (DISP), sin afectar los porcentajes de preñez. El objetivo del trabajo fue evaluar el efecto de dos dosis de CPE inyectado al retirar un DISP, sobre el porcentaje de preñez post inseminación artificial a tiempo fijo (IATF). Como objetivo secundario, se planteó comparar la eficiencia reproductiva de los tratamientos utilizados. Se emplearon 79 vaquillonas de 15 meses de edad. El día 0, se les colocó un DISP más BE. El día 7 se retiró el DISP, se administró D(+) cloprostenol y en forma aleatoria se inyectó 0,5 mg de CPE, 1 mg de CPE o BE 24 h después. Para la IATF (52–56 h) se utilizó semen proveniente de un toro de probada fertilidad. El día 22 se colocó a todas las vaquillonas un DISP de segundo uso, retirándolo 7 días después. Se continuó con detección de celo e IA. El diagnóstico de gestación se realizó por ultrasonografía en dos oportunidades para evaluar preñez de IATF y retorno, así como para verificar mortalidad embrionaria. Se evaluó el efecto de los tratamientos sobre la preñez a la IATF, del retorno y final. No se observaron efectos del tratamiento (p>0,05) sobre los porcentajes de preñez a la IATF (51,9%), del retorno (61,1%) y final (65,8%). Se observó un 7,3% de pérdidas embrionarias (p>0,05). Se concluye que la administración de 0,5 o 1 mg de CPE al retirar un DISP con progesterona en lugar de BE a las 24 h posteriores es igualmente efectiva para implementar una IATF. Además, no resulta afectada la eficiencia reproductiva del rodeo.
Orbital Parameters and Chemical Composition of Four White Dwarfs in Post-Common Envelope Binaries
We present FUSE observations of the hot white dwarfs in the post-common
envelope binaries Feige 24, EUVE J0720-317, BPM 6502, and EUVE J2013+400. The
spectra show numerous photospheric absorption lines which trace the white dwarf
orbital motion. We report the detection of C III, O VI, P V, and Si IV in the
spectra of Feige 24, EUVE J0720-317 and EUVE J2013+400, and the detection of C
III, N II, Si III, Si IV, and Fe III in the spectra of BPM 6502. Abundance
measurements support the possibility that white dwarfs in post-common envelope
binaries accrete material from the secondary star wind. The FUSE observations
of BPM 6502 and EUVE J2013+400 cover a complete binary orbit. We used the FUSE
spectra to measure the radial velocities traced by the white dwarf in the four
binaries, where the zero-point velocity were fixed using the ISM velocities in
the line of sight of the stellar systems. For BPM 6502 we determined a white
dwarf velocity semi-amplitude of K_WD = 18.6+/-0.5km/s, and with the velocity
semi-amplitude of the red dwarf companion (K_RD = 75.2+/-3.1 km/s), we estimate
the mass ratio to be q = 0.25+/-0.01. Adopting a spectroscopic mass
determination for the white dwarf, we infer a low secondary mass of M_RD =
0.14+/-0.01 M_solar. For EUVE J2013+400 we determine a white dwarf velocity
semi-amplitude of K_WD = 36.7+/-0.7 km/s. The FUSE observations of EUVE
J0720-317 cover approximately 30% of the binary period and combined with the
HST GHRS measurements (Vennes et al. 1999, ApJ 523, 386), we update the binary
properties. FUSE observations of Feige 24 cover approximately 60% of the orbit
and we combine this data set with HST STIS (Vennes et al. 2000, ApJ, 544, 423)
data to update the binary properties.Comment: Accepted for publication in Ap
Photospheric phosphorus in the FUSE spectra of GD71 and two similar DA white dwarfs
We report the detection, from FUSE data, of phosphorus in the atmospheres of
GD71 and two similar DA white dwarfs. This is the first detection of a trace
metal in the photosphere of the spectrophotometric standard star GD71.
Collectively, these objects represent the coolest DA white dwarfs in which
photospheric phosphorus has been observed. We use a grid of homogeneous non-LTE
synthetic spectra to measure abundances of[P/H]=-8.57 +0.09 -0.13, -8.70 +0.23
-0.37 and -8.36 +0.14 -0.19 in GD71, RE J1918+595 and RE J0605-482
respectively. At the observed level we find phosphorus has no significant
impact on the overall energy distribution of GD71. We explore possible
mechanisms responsible for the presence of this element in these stars,
concluding that the most likely is an interplay between radiative levitation
and gravitational settling but possibly modified by weak mass loss.Comment: Accepted for publication in MNRAS Letter
The Deuterium, Oxygen, and Nitrogen Abundance Toward LSE 44
We present measurements of the column densities of interstellar DI, OI, NI,
and H2 made with FUSE, and of HI made with IUE toward the sdO star LSE 44, at a
distance of 554+/-66 pc. This target is among the seven most distant Galactic
sight lines for which these abundance ratios have been measured. The column
densities were estimated by profile fitting and curve of growth analyses. We
find D/H = (2.24 +1.39 -1.32)E-5, D/O = (1.99 +1.30 -0.67)E-2, D/N = (2.75
+1.19 -0.89)E-1, and O/H = (1.13 +0.96 -0.71)E-3 (2 sigma). Of the most distant
Galactic sight lines for which the deuterium abundance has been measured LSE 44
is one of the few with D/H higher than the Local Bubble value, but D/O toward
all these targets is below the Local Bubble value and more uniform than the D/H
distribution. (Abstract abridged.)Comment: 20 pages, including 9 figures. Accepted for publication in Ap
Deuterium toward the WD0621-376 sight line: Results from the Far Ultraviolet Spectroscopic Explorer (FUSE) Mission
Far Ultraviolet Spectroscopic Explorer observations are presented for
WD0621-376, a DA white dwarf star in the local interstellar medium (LISM) at a
distance of about 78 pc. The data have a signal-to-noise ratio of about 20-40
per 20 km/s resolution element and cover the wavelength range 905-1187 \AA.
LISM absorption is detected in the lines of D I, C II, C II*, C III, N I, N II,
N III, O I, Ar I, and Fe II. This sight line is partially ionized, with an
ionized nitrogen fraction of > 0.23. We determine the ratio (2). Assuming a standard interstellar
oxygen abundance, we derive . Using the
value of N(H I) derived from EUVE data gives a similar D/H ratio. The D I/N I
ratio is (2).Comment: accepted for publication in the ApJ
JWST Fine Guidance Sensor Calibration
Abstract. The primary function of the Fine Guidance Sensor (FGS) is to provide continuous pointing information to the Observatory. The FGS will image two separate regions of the JWST field of view onto two independent 2k x 2k infrared focal planes arrays, which will cover a wavelength range of 0.6 to 5 µm. Once in fine guiding, the FGS will provide continuous pointing information to a precision of ≤ 5 milli-arc seconds at an update rate of 16 Hz for J 18.5 magnitude stars. In order to fulfill its functions, i.e., Identification, Acquisition, Track, and Fine Guide, the FGS will require calibration. In this paper, we present a brief overview of the FGS design, its operations, and its calibration
High-resolution FUSE and HST ultraviolet spectroscopy of the white dwarf central star of Sh 2-216
LS V +4621 is the DAO-type central star of the planetary nebula Sh 2-216. We
perform a comprehensive spectral analysis of high-resolution, high-S/N
ultraviolet observations obtained with FUSE and STIS aboard the HST as well as
the optical spectrum of LS V +4621 by means of state-of-the-art NLTE
model-atmosphere techniques in order to compare its photospheric properties to
theoretical predictions from stellar evolution theory as well as from diffusion
calculations.
From the N IV - NV, O IV - O VI, Si IV - Si V, and Fe V - Fe VII ionization
equilibria, we determined an effective temperature of 95 +/- 2 kK with high
precision. The surface gravity is log g = 6.9 +/- 0.2. An unexplained
discrepancy appears between the spectroscopic distance d = 224 +46/-58 pc and
the parallax distance d = 129 +6/-5 pc of LS V +4621. For the first time, we
have identified Mg IV and Ar VI absorption lines in the spectrum of a
hydrogen-rich central star and determined the Mg and Ar abundances as well as
the individual abundances of iron-group elements (Cr, Mn, Fe, Co, and Ni). With
the realistic treatment of metal opacities up to the iron group in the
model-atmosphere calculations, the so-called Balmer-line problem (found in
models that neglect metal-line blanketing) vanishes.
Spectral analysis by means of NLTE model atmospheres has presently arrived at
a high level of sophistication, which is now hampered largely by the lack of
reliable atomic data and accurate line-broadening tables. Strong efforts should
be made to improve upon this situation.Comment: 13 pages, 20 figure
O/H in the Local Bubble
We present new measurements of the oxygen gas-phase abundance along four
sightlines probing gas inside the Local Bubble, using data obtained with the
Far Ultraviolet Spectroscopic Explorer (FUSE) and the Hubble Space Telecope
(HST). Combining these with seven previously published N(O I) and N(H I)
measurements we determine a mean O/H ratio for the Local Bubble, (O/H) = (3.45
+/- 0.19)x10^(-4) (1 sigma in the mean). Our result is virtually identical to
O/H = (3.43 +/- 0.15)x10^(-4) derived from data for sightlines probing gas well
outside the Local Bubble. In contrast to the D/O and D/H ratios, which seem to
have different values beyond the Local Bubble, our results show that the O/H
ratio is constant and single-valued both inside and outside the Local Bubble,
for low density sightlines, with column densities up to log N (H) ~ 21. In
addition, the similarity of the two values above suggests that the net effect
of the uncertain O I f-values in the FUSE bandpass is not significant. Taking
into account the latest determinations of the Solar abundance of oxygen, our
result implies that ~25% of the oxygen in the Local Bubble is depleted onto
dust grains. The similarity of the value for O/H along low average density
sightlines in the Local Bubble with that of denser sightlines beyond may permit
a limit on the diluting effects of infalling low metallicity gas.Comment: Accepted for publication in the Astrophysical Journa
- …