79 research outputs found
Time-resolved Ultraviolet Spectroscopy of the M-dwarf GJ 876 Exoplanetary System
Extrasolar planets orbiting M-stars may represent our best chance to discover
habitable worlds in the coming decade. The ultraviolet spectrum incident upon
both Earth-like and Jovian planets is critically important for proper modeling
of their atmospheric heating and chemistry. In order to provide more realistic
inputs for atmospheric models of planets orbiting low-mass stars, we present
new near- and far-ultraviolet (NUV and FUV) spectroscopy of the M-dwarf
exoplanet host GJ 876 (M4V). Using the COS and STIS spectrographs aboard the
Hubble Space Telescope, we have measured the 1150-3140A spectrum of GJ 876. We
have reconstructed the stellar HI LyA emission line profile, and find that the
integrated LyA flux is roughly equal to the rest of the integrated flux
(1150-1210A + 1220-3140A) in the entire ultraviolet bandpass (F(LyA)/F(FUV+NUV)
~0.7). This ratio is ~ 2500x greater than the solar value. We describe the
ultraviolet line spectrum and report surprisingly strong fluorescent emission
from hot H2 (T(H2) > 2000 K). We show the light-curve of a chromospheric +
transition region flare observed in several far-UV emission lines, with
flare/quiescent flux ratios >= 10. The strong FUV radiation field of an M-star
(and specifically LyA) is important for determining the abundance of O2 -- and
the formation of biomarkers -- in the lower atmospheres of Earth-like planets
in the habitable zones of low-mass stars.Comment: 6 pages, 4 figures. ApJL accepte
The Mass of the Black Hole in XTE J1118+480
We present contemporaneous, broadband, near-infrared spectroscopy (0.9-2.45 μm) and H-band photometry of the black hole X-ray binary, XTE J1118+480. We determined the fractional dilution of the NIR ellipsoidal light curves of the donor star from other emission sources in the system by comparing the absorption features in the spectrum with field stars of known spectral type. We constrained the donor star spectral type to K7 V-M1 V and determined that the donor star contributed 54% ± 27% of the H-band flux at the epoch of our observations. This result underscores the conclusion that the donor star cannot be assumed to be the only NIR emission source in quiescent X-ray binaries. The H-band light curve shows a double-humped asymmetric modulation with extra flux at orbital phase 0.75. The light curve was fitted with a donor star model light curve, taking into account a constant second flux component based on the dilution analysis. We also fitted models that included emission from the donor star, a constant component from the accretion disk, and a phase-variable component from the bright spot where the mass accretion stream impacts the disk. These simple models with reasonable estimates for the component physical parameters can fully account for the observed light curve, including the extra emission at phase 0.75. From our fits, we constrained the binary inclination to 68° ≤ i ≤ 79°. This leads to a black hole mass of 6.9 M_☉ ≤ M_(BH) ≤ 8.2 M_☉. Long-term variations in the NIR light curve shape in XTE J1118+480 are similar to those seen in other X-ray binaries and demonstrate the presence of continued activity and variability in these systems even when in full quiescence
Near-Infrared Spectroscopy of Low Mass X-ray Binaries : Accretion Disk Contamination and Compact Object Mass Determination in V404 Cyg and Cen X-4
We present near-infrared (NIR) broadband (0.80--2.42 m) spectroscopy of
two low mass X-ray binaries: V404 Cyg and Cen X-4. One important parameter
required in the determination of the mass of the compact objects in these
systems is the binary inclination. We can determine the inclination by modeling
the ellipsoidal modulations of the Roche-lobe filling donor star, but the
contamination of the donor star light from other components of the binary,
particularly the accretion disk, must be taken into account. To this end, we
determined the donor star contribution to the infrared flux by comparing the
spectra of V404 Cyg and Cen X-4 to those of various field K-stars of known
spectral type. For V404 Cyg, we determined that the donor star has a spectral
type of K3 III. We determined the fractional donor contribution to the NIR flux
in the H- and K-bands as and , respectively. We
remodeled the H-band light curve from \citet{sanwal1996} after correcting for
the donor star contribution to obtain a new value for the binary inclination.
From this, we determined the mass of the black hole in V404 Cyg to be . We performed the same spectral analysis for Cen X-4
and found the spectral type of the donor star to be in the range K5 -- M1V. The
donor star contribution in Cen X-4 is in the H-band while in the
K-band, the accretion disk can contribute up to 10% of the infrared flux. We
remodeled the H-band light curve from \citet{shahbaz1993}, again correcting for
the fractional contribution of the donor star to obtain the inclination. From
this, we determined the mass of the neutron star as . However, the masses obtained for both systems should
be viewed with some caution since contemporaneous light curve and spectral data
are required to obtain definitive masses
Near-Infrared Light Curves of the Black Hole Binary A0620-00
We measured the near-infrared orbital light curve of the black hole binary
A0620-00 in 1995 and 1996. The light curves show an asymmetric, double-humped
modulation with extra emission in the peak at orbital phase 0.75. There were no
significant changes in the shape of the light curve over the one-year
observation period. There were no sharp dips in the light curves nor reversals
of the asymmetry between the two peaks as seen in earlier observations. The
light curves are well fit by models incorporating ellipsoidal variations from
the mass-losing K-type star plus a beamed bright spot on the accretion disk
around the compact star. The long-term stability of the light curve shape rules
out superhumps and star spots as sources of asymmetry when we observed
A0620-00. The ellipsoidal variations yield a lower limit i >= 38 deg on the
orbital inclination. The light curves show no eclipse features, which places an
upper limit i <= 75 deg. This range of inclinations constrains the mass of the
compact object to 3.3 < M_1 < 13.6 Msun. The light curves do not further
constrain the orbital inclination because the contribution of the accretion
disk to the observed flux is unknown. We argue that a previous attempt to
measure the near-infrared flux from the accretion disk using the dilution of
the 12CO(2,0) bandhead in the spectrum of the K star is not reliable because
the band strength depends strongly on surface gravity.Comment: Accepted for publication in the Astronomical Journal. 17 pages, 4
figures. Prepared using AASTEX V. 5.
A Survey of Far Ultraviolet Spectroscopic Explorer Observations of Cataclysmic Variables
During its lifetime, the Far Ultraviolet Spectroscopic Explorer (FUSE) was
used to observe 99 cataclysmic variables in 211 separate observations. Here, we
present a survey of the moderate resolution (R\simeq10,000), far-ultraviolet
(905 - 1188 {\deg}A), time-averaged FUSE spectra of cataclysmic variables
(CVs). The FUSE spectra are morphologically diverse. They show contributions
from the accretion disk, the disk chromosphere, disk outflows, and the white
dwarf, but the relative contribution of each component varies widely as a
function of CV subtype, orbital period and evolutionary state, inclination,
mass accretion rate, and magnetic field strength of the white dwarf. The data
reveal information about the structure, temperature, density and mass flow
rates of the disk and disk winds, the temperature of the white dwarf and the
effects of ongoing accretion on its structure, and the long-term response of
the systems to disk outbursts. The complete atlas of time-averaged FUSE spectra
of CVs are available at the Multimission Archive at Space Telescope Science
Institute as a High Level Science Product.Comment: ApJS, in press. The extra panels in the figure sets for Figures 1 and
2 are included at the end of the manuscrip
The Ultraviolet Radiation Environment Around M dwarf Exoplanet Host Stars
The spectral and temporal behavior of exoplanet host stars is a critical
input to models of the chemistry and evolution of planetary atmospheres. At
present, little observational or theoretical basis exists for understanding the
ultraviolet spectra of M dwarfs, despite their critical importance to
predicting and interpreting the spectra of potentially habitable planets as
they are obtained in the coming decades. Using observations from the Hubble
Space Telescope, we present a study of the UV radiation fields around nearby M
dwarf planet hosts that covers both FUV and NUV wavelengths. The combined
FUV+NUV spectra are publically available in machine-readable format. We find
that all six exoplanet host stars in our sample (GJ 581, GJ 876, GJ 436, GJ
832, GJ 667C, and GJ 1214) exhibit some level of chromospheric and transition
region UV emission. No "UV quiet" M dwarfs are observed. The bright stellar
Ly-alpha emission lines are reconstructed, and we find that the Ly-alpha line
fluxes comprise ~37-75% of the total 1150-3100A flux from most M dwarfs; >
10^{3} times the solar value. The F(FUV)/F(NUV) flux ratio, a driver for
abiotic production of the suggested biomarkers O2 and O3, is shown to be ~0.5-3
for all M dwarfs in our sample, > 10^{3} times the solar ratio. For the four
stars with moderate signal-to-noise COS time-resolved spectra, we find UV
emission line variability with amplitudes of 50-500% on 10^{2} - 10^{3} s
timescales. Finally, we observe relatively bright H2 fluorescent emission from
four of the M dwarf exoplanetary systems (GJ 581, GJ 876, GJ 436, and GJ 832).
Additional modeling work is needed to differentiate between a stellar
photospheric or possible exoplanetary origin for the hot (T(H2) \approx
2000-4000 K) molecular gas observed in these objects.Comment: ApJ, accepted. 16 pages, 10 figures. On-line data at:
http://cos.colorado.edu/~kevinf/muscles.htm
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