The Berkeley Infrared Spatial Interferometer: A Heterodyne Stellar Interferometer for the Mid‐Infrared

Hale, David; Bester, M.; Danchi, W. C.; Fitelson, W.; Hoss, S.; Lipman, Everett A.; Monnier, John D.; Tuthill, P. G.; Townes, C. H.

doi:10.1086/309049

Cited by 102 publications

(56 citation statements)

References 25 publications

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“…The spectra were obtained using an infrared heterodyne system (Betz et al 1977) on one of the 1.65-m telescopes of the Infrared Spatial Interferometer (ISI; Hale et al 2000) at Mount Wilson, California. The infrared heterodyne technique and its application to planetary atmospheres are described by Kostiuk (1994) and Kostiuk et al (1997) in application to planetary atmospheres.…”

Section: Data Acquisition and Reductionmentioning

confidence: 99%

Temporal Behavior of Stratospheric Ammonia Abundance and Temperature Following the SL9 Impacts

Fast

Kostiuk

Romani

et al. 2002

Icarus

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Infrared emission lines of stratospheric ammonia (NHwith cold jovian air. During the first 4 days after impact, NH 3 was present primarily at altitudes above 1 mbar with a column density of (7.7 ± 1.6) × 10 17 cm −2 after 1 day and (3.7 ± 0.8) × 10 17 cm −2 after 4 days. (Errors represent precision.) We obtained >2.5 times more NH 3 than can be supplied by nitrogen from a large cometary fragment, suggesting a primarily jovian source for the NH 3 . By 18 days postimpact, a return to quiescent upper stratospheric temperature is retrieved for the G region, with an NH 3 column density of 7.3 × 10 17 cm −2 or more in the lower stratosphere, possibly supplied by NH 3 upwelling across an impact-heated and turbulent tropopause, which may have been masked by initial dust and haze. Above the 1-mbar level, the maximum retrieved column density decreased to 6.5 × 10 16 cm −2 . Comparison to photochemical models indicates that photolysis alone is not sufficient to account for the loss of NH 3 above 1 mbar by that time, even when chemical reformation of NH 3 is ignored. We speculate that the dispersion of plume material at high altitudes (above 1 mbar) is responsible for the change in the spectra observed a few days postimpact. Data on the K impact region provide qualitatively consistent results. c 2002 Elsevier Science (USA)

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Section: Data Acquisition and Reductionmentioning

confidence: 99%

Temporal Behavior of Stratospheric Ammonia Abundance and Temperature Following the SL9 Impacts

Fast

Kostiuk

Romani

et al. 2002

Icarus

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“…Earth rotation foreshortened the baseline and allowed a range of spatial frequencies to be used. Details concerning data reduction and calibration can be found in Hale et al (2000) and references therein. Table 1 and Figure 1 show the visibility data for IRC ]10216 calibrated using a Tau, approximately a point source at the resolution of this experiment.…”

Section: Data From Fall 1998mentioning

confidence: 99%

Mid‐Infrared Interferometry on Spectral Lines. II. Continuum (Dust) Emission around IRC +10216 and VY Canis Majoris

Monnier

Danchi

Hale

et al. 2000

ApJ

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The University of California Berkeley Infrared Spatial Interferometer has measured the mid-infrared visibilities of the carbon star IRC ]10216 and the red supergiant VY CMa. The dust shells around these sources have been previously shown to be time variable, and these new data are used to probe the evolution of the dust shells on a decade timescale, complementing contemporaneous studies at other wavelengths. Self-consistent, spherically symmetric models at maximum and minimum light both show the inner radius of the IRC ]10216 dust shell to be much larger (150 mas) than expected from the dust-condensation temperature, implying that dust production has slowed or stopped in recent years. Apparently, dust does not form every pulsational cycle (638 days), and these mid-infrared results are consistent with recent near-infrared imaging, which indicates little or no new dust production in the last 3 yr. Spherically symmetric models failed to Ðt recent VY CMa data, implying that emission from the inner dust shell is highly asymmetric and/or time variable.

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“…This program was initiated by Charles H. Townes and his colleagues from the University of California at Berkeley (40). The key idea of this program is to use a star as PM and a very high angular resolution telescope Infrared Spatial Interferometer (ISI) as a meter to detect the changes (distortions) of the star itself.…”

Section: Discussionmentioning

confidence: 99%

Experiments with probe masses

Braginsky

2007

Proc. Natl. Acad. Sci. U.S.A.

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This contribution is part of the special series of Inaugural Articles by members of the National Academy of Sciences elected on April 25, 2006. Contributed by V. B. Braginsky, November 29, 2006 (sent for review October 30, 2006) It is reasonable to regard the experiments performed by C. Coulomb and H. Cavendish in the end of the 18th century as the beginning of laboratory experimental physics. These outstanding scientists have measured forces (accelerations) produced by electric charges and by gravitational ''charges'' on probe masses that were attached to torque balance. Among the variety of different research programs and projects existing today, experiments with probe masses are still playing an important role. In this short review, the achieved and planned sensitivities of very challenging LIGO (Laser Interferometer Gravitational wave Observatory) and LISA (Laser Interferometer Space Antennae) projects are described, and a list of nonsolved problems is discussed as well. The role of quantum fluctuations in high precision measurements is also outlined. Apart from these main topics, the limitations of sensitivity caused by cosmic rays and the prospects of clock frequency stability are presented.gravitational waves ͉ measurement I. Classical and Quantum Limitations of Sensitivity in the Experiments with Probe MassesI n the simplest classical ''case,'' when a probe mass (PM) m p is coupled with a heat-bath by means of friction H, the FluctuationDissipation Theorem (FDT) gives the limit for detectable value of AC accelerationwhere T is the heat-bath temperature, k B is the Boltzmann constant, and ⌬f is the bandwidth of force acting on the PM F ϭ m p ⅐a PM . Equation 1 is valid when the parameter H does not depend on frequency and if the time interval (averaging time) is equal to Ӎ (⌬f ) Ϫ1 . If PM is in the absolute vacuum (no mechanical contact with the entourage-envelope), then the remaining fluctuating force acting on PM is the AC component of thermal radiation pressure F THERM from the entourage if T Ͼ 0. This effect is a classical one (i.e., it exists due to fluctuations of envelope temperature in thermal equilibrium). This small effect will be discussed in Section III.Simple calculations [almost 40 years old (1)] give another limit for the detectable force F ϭ m p ⅐a PM , which acts on PM. This limit is of quantum origin; it depends on the chosen observable of the measuring device (meter). If PM is a part of the mechanical oscillator whose eigenfrequency is m , and if F ϭ F 0 sin m t during time interval , then using an optical Fabry-Perot resonator pumped by a laser as a continuous monitor of the coordinate, it is possible to measure the amplitude (1) [2]The term ''Standard Quantum Limit'' (SQL) was coined by K. S. Thorne. This limit can be obtained only provided that laser pumping power in the meter is equal to the optimal value:where R is the mirrors reflectivity, c is the speed of light, and optic is the laser frequency. If W is smaller or higher than W optim , then the variance of output signal w...

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The Berkeley Infrared Spatial Interferometer: A Heterodyne Stellar Interferometer for the Mid‐Infrared

Cited by 102 publications

References 25 publications

Temporal Behavior of Stratospheric Ammonia Abundance and Temperature Following the SL9 Impacts

Temporal Behavior of Stratospheric Ammonia Abundance and Temperature Following the SL9 Impacts

Mid‐Infrared Interferometry on Spectral Lines. II. Continuum (Dust) Emission around IRC +10216 and VY Canis Majoris

Experiments with probe masses

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