61 research outputs found
Seeing, Wind and Outer Scale Effects on Image Quality at the Magellan Telescopes
We present an analysis of the science image quality obtained on the twin 6.5
metre Magellan telescopes over a 1.5 year period, using images of ~10^5 stars.
We find that the telescopes generally obtain significantly better image quality
than the DIMM-measured seeing. This is qualitatively consistent with
expectations for large telescopes, where the wavefront outer scale of the
turbulence spectrum plays a significant role. However, the dominant effect is
found to be wind speed with Magellan outperforming the DIMMs most markedly when
the wind is strongest. Excluding data taken during strong wind conditions (>10
m/s), we find that the Magellan telescopes still significantly outperform the
DIMM seeing, and we estimate the site to have L_0 ~ 25 m on average. We also
report on the first detection of a negative bias in DIMM data. This is found to
occur, as predicted, when the DIMM is affected by certain optical aberrations
and the turbulence profile is dominated by the upper layers of the atmosphere.Comment: Accepted for publication in PASP. 10 pages, 12 figures
The 15 years of comet photometry: A comparative analysis of 80 comets
In 1976, a program of narrowband photometry of comets was initiated that has encompassed well over 400 nights of observations. To date, the program has provided detailed information on 80 comets, 11 of which were observed during multiple apparitions. The filters (initially isolating CN, C2, and continuum and later including C3, OH, and NH) as well as the detectors used for the observations were changed over time, and the parameters adopted in the reduction and modeling of the data have likewise evolved. Accordingly, we have re-reduced the entire database and have derived production rates using current values for scalelengths and fluorescence efficiencies. Having completed this task, the results for different comets can now be meaningfully compared. The general characteristics that are discussed include ranges in composition (molecular production rate ratios) and dustiness (gas production compared with Af(rho)). Additionally an analysis of trends on how the production rates vary with heliocentric distance and on pre- and post-perihelion asymmetries in the production rates of individual comets. Possible taxonomic groupings are also described
Signatures of Cloud, Temperature, and Gravity From Spectra of the Closest Brown Dwarfs
We present medium resolution optical and NIR spectral data for components of
the newly discovered WISE J104915.57-531906.1AB (Luhman 16AB) brown dwarf
binary. The optical spectra reveal strong 6708 A Li I absorption in both Luhman
16A (8.0+/-0.4 A) and Luhman 16B (3.8+/-0.4 A). Interestingly, this is the
first detection of Li I absorption in a T dwarf. Combined with the lack of
surface gravity features, the Li I detection constrains the system age to 0.1 -
3 Gyr. In the NIR data, we find strong KI absorption at 1.168, 1.177, 1.243,
and 1.254 {\mu}m in both components. Compared to the strength of KI line
absorption in equivalent spectral subtype brown dwarfs, Luhman 16A is weaker
while Luhman 16B is stronger. Analyzing the spectral region around each doublet
in distance scaled flux units and comparing the two sources, we confirm the J
band flux reversal and find that Luhman 16B has a brighter continuum in the
1.17 {\mu}m and 1.25 {\mu}m regions than Luhman 16A. Converting flux units to a
brightness temperature we interpret this to mean that the secondary is ~ 50 K
warmer than the primary in regions dominated by condensate grain scattering.
One plausible explanation for this difference is that Luhman 16B has thinner
clouds or patchy holes in its atmosphere allowing us to see to deeper, hotter
regions. We also detect comparably strong FeH in the 0.9896 {\mu}m Wing-Ford
band for both components. Traditionally, a signpost of changing atmosphere
conditions from late-type L to early T dwarfs, the persistence and similarity
of FeH at 0.9896 {\mu}m in both Luhman 16A and Luhman 16B is an indication of
homogenous atmosphere conditions. We calculate bolometric luminosities from
observed data supplemented with best fit models for longer wavelengths and find
the components are consistent within 1{\sigma} with resultant Teffs of
1310+/-30 K and 1280+/-75 K for Luhman 16AB respectively.Comment: 17 pages, 11 figures, 4 tables. Submitted to ApJ and revised after
referee repor
Transit Timing Variation Analysis of Ogle-Tr-132b with Seven New Transits
December 15, 2010We report the results of the first transit timing variation analysis of the very hot Jupiter OGLE-TR-132b, using 10 transits collected over a seven-year period. Our analysis combines three previously published transit light curves with seven new transits, which were observed between 2008 February and 2009 May with the new MagIC-e2V instrument on the Magellan Telescopes in Chile. We provide a revised planetary radius of R[subscript p] = 1.23 ± 0.07R[subscript J] , which is slightly larger, but consistent within the errors, than that given by previously published results. Analysis of the planet-to-star radius ratio, orbital separation, inclination, and transit duration reveals no apparent variation in any of those parameters during the time span observed. We also find no sign of transit timing variations larger than –108 ± 49 s, with most residuals very close to zero. This allows us to place an upper limit of 5-10 M [subscript ⊕] for a coplanar, low-eccentricity perturber in either the 2:1 or 3:2 mean-motion resonance with OGLE-TR-132b. We similarly find that the data are entirely consistent with a constant orbital period and there is no evidence for orbital decay within the limits of precision of our data.United States. National Aeronautics and Space Administration (Origins Grant NNX07AN63G
Six High-Precision Transits of Ogle-Tr-113b
We present six new transits of the hot Jupiter OGLE-TR-113b observed with MagIC on the Magellan
Telescopes between 2007 January and 2009 May. We update the system parameters and revise the planetary radius to R[subscript p] = 1.084 ± 0.029R[subscript J] , where the error is dominated by stellar radius uncertainties. The new transit midtimes reveal no transit timing variations from a constant ephemeris of greater than 13 ± 28 s over two years, placing an upper limit of 1–2M[subscript ⊕] on the mass of any perturber in a 1:2 or 2:1 mean-motion resonance with OGLETR-
113b. Combining the new transit epochs with five epochs published between 2002 and 2006, we find hints that the orbital period of the planet may not be constant, with the best fit indicating a decrease of [dot over P] = −60±15 ms yr−1. If real, this change in period could result from either a long-period (more than eight years) timing variation due to a massive external perturber or more intriguingly from the orbital decay of the planet. The detection of a changing period is still tentative and requires additional observations, but if confirmed it would enable direct tests of tidal stability and dynamical models of close-in planets.United States. National Aeronautics and Space Administration (Origins Grant NNX07AN63G
A Spitzer Study of Comets 2P/Encke, 67P/Churyumov-Gerasimenko, and C/2001 HT50 (LINEAR-NEAT)
We present infrared images and spectra of comets 2P/Encke,
67P/Churyumov-Gerasimenko, and C/2001 HT50 (LINEAR-NEAT) as part of a larger
program to observe comets inside of 5 AU from the sun with the Spitzer Space
Telescope. The nucleus of comet 2P/Encke was observed at two vastly different
phase angles (20 degrees and 63 degrees). Model fits to the spectral energy
distributions of the nucleus suggest comet Encke's infrared beaming parameter
derived from the near-Earth asteroid thermal model may have a phase angle
dependence. The observed emission from comet Encke's dust coma is best-modeled
using predominately amorphous carbon grains with a grain size distribution that
peaks near 0.4 microns, and the silicate contribution by mass to the sub-micron
dust coma is constrained to 31%. Comet 67P/Churyumov-Gerasimenko was observed
with distinct coma emission in excess of a model nucleus at a heliocentric
distance of 5.0 AU. The coma detection suggests that sublimation processes are
still active or grains from recent activity remain near the nucleus. Comet
C/2001 HT50 (LINEAR-NEAT) showed evidence for crystalline silicates in the
spectrum obtained at 3.2 AU and we derive a silicate-to-carbon dust ratio of
0.6. The ratio is an order of magnitude lower than that derived for comets
9P/Tempel 1 during the Deep Impact encounter and C/1995 O1 (Hale-Bopp).Comment: Accepted for publication in the Astrophysical Journal 48 pages, 15
figures, 10 table
Optical Properties of (162173) 1999 JU3: In Preparation for the JAXA Hayabusa 2 Sample Return Mission
We investigated the magnitude-phase relation of (162173) 1999 JU3, a target
asteroid for the JAXA Hayabusa 2 sample return mission. We initially employed
the international Astronomical Union's H-G formalism but found that it fits
less well using a single set of parameters. To improve the inadequate fit, we
employed two photometric functions, the Shevchenko and Hapke functions. With
the Shevchenko function, we found that the magnitude-phase relation exhibits
linear behavior in a wide phase angle range (alpha = 5-75 deg) and shows weak
nonlinear opposition brightening at alpha< 5 deg, providing a more reliable
absolute magnitude of Hv = 19.25 +- 0.03. The phase slope (0.039 +- 0.001
mag/deg) and opposition effect amplitude (parameterized by the ratio of
intensity at alpha=0.3 deg to that at alpha=5 deg, I(0.3)/I(5)=1.31+-0.05) are
consistent with those of typical C-type asteroids. We also attempted to
determine the parameters for the Hapke model, which are applicable for
constructing the surface reflectance map with the Hayabusa 2 onboard cameras.
Although we could not constrain the full set of Hapke parameters, we obtained
possible values, w=0.041, g=-0.38, B0=1.43, and h=0.050, assuming a surface
roughness parameter theta=20 deg. By combining our photometric study with a
thermal model of the asteroid (Mueller et al. in preparation), we obtained a
geometric albedo of pv = 0.047 +- 0.003, phase integral q = 0.32 +- 0.03, and
Bond albedo AB = 0.014 +- 0.002, which are commensurate with the values for
common C-type asteroids.Comment: 27 pages, 4 figure, accepted for publication in the Astrophysical
Journa
ACCESS: An optical transmission spectrum of the high-gravity, hot Jupiter HAT-P-23b
We present a new ground-based visible transmission spectrum of the
high-gravity, hot Jupiter HAT-P-23b, obtained as part of the ACCESS project. We
derive the spectrum from five transits observed between 2016 and 2018, with
combined wavelength coverage between 5200 {\AA} - 9269 {\AA} in 200 {\AA} bins,
and with a median precision of 247 ppm per bin. HAT-P-23b's relatively high
surface gravity (g ~ 30 m/s^2), combined with updated stellar and planetary
parameters from Gaia DR2, gives a 5-scale-height signal of 384 ppm for a
hydrogen-dominated atmosphere. Bayesian models favor a clear atmosphere for the
planet with the tentative presence of TiO, after simultaneously modeling
stellar contamination, using spots parameter constraints from photometry. If
confirmed, HAT-P-23b would be the first example of a high-gravity gas giant
with a clear atmosphere observed in transmission at optical/NIR wavelengths;
therefore, we recommend expanding observations to the UV and IR to confirm our
results and further characterize this planet. This result demonstrates how
combining transmission spectroscopy of exoplanet atmospheres with long-term
photometric monitoring of the host stars can help disentangle the exoplanet and
stellar activity signals.Comment: 28 pages, 18 Figures, accepted for publication in AJ. arXiv admin
note: text overlap with arXiv:1911.0335
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