An Infrared Stellar Spectrometer.

Kuiper, G. P.; Wilson, William J.; Cashman, R. J.

doi:10.1086/144955

Cited by 34 publications

(12 citation statements)

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“…Including preamplifier the total gain comes to 80120 db. This structure chiefly follows the Cashman type [4] and its formation is comparatively simple . Its adjustment was done by one capacity in a simple way, and its character has brought about a rather good results as shown in Fi., 2.…”

Section: Methods Of Measurementmentioning

confidence: 94%

The Way to Measure the Surface Temperature through PbS-Photoconductive Cell

Kamiyama¹,

Moriguchi²,

Eguchi

1953

Pap.Met.Geophy

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Section: Methods Of Measurementmentioning

confidence: 94%

The Way to Measure the Surface Temperature through PbS-Photoconductive Cell

Kamiyama¹,

Moriguchi²,

Eguchi

1953

Pap.Met.Geophy

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“…Naturally, observations at multiple infrared wavelengths are also desirable to observe spectral features of different molecular species and/or surface compositions (e.g., Kuiper et al 1947;Hu et al 2012). Table 1 shows that the number of planets accessible to highcontrast characterization drops steadily as the observing wavelength increases from 1.0 µm to 3.5 µm.…”

Section: Observing Wavelength: Scattered Starlight and Thermal Emissionmentioning

confidence: 99%

On high-contrast characterization of nearby, short-period exoplanets with giant segmented-mirror telescopes

Crossfield

2013

A&A

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Measurements of the frequency with which short-period planets occur around main sequence stars allows a direct prediction of the number and types of such planets that will be amenable to characterization by high-contrast instruments on future giant segmentedmirror telescopes (GSMTs). Adopting conservative assumptions, I predict of order 10 planets with radii R P = 1−8 R ⊕ and equilibrium temperatures 400 K should be accessible around stars within 8 pc of the Sun. These numbers are roughly the same for both nearinfrared observations of scattered starlight and mid-infrared observations of planetary thermal emission, with the latter observations demonstrating greater relative sensitivity to smaller and cooler planets. Adopting the conservative assumption that planets with R P = 1−2 R ⊕ and 2−4 R ⊕ occur with equal frequency, I predict a 40% chance that a planet with R P = 1−2 R ⊕ and equilibrium temperature 200-250 K will accessible to high-contrast thermal infrared characterization; this would be a compelling object for further study. To validate these predictions, more detailed analyses are needed of the occurrence frequencies of low-mass planets around M dwarfs, both in the Kepler field and in the solar neighborhood. Several planets already discovered by radial velocity surveys will be accessible to near-infrared high-contrast GSMT observations, including the low-mass planets α Cen Bb and (depending on their albedos) GJ 139c and d, GJ 876b and c, and τ Cet b, c, and d; τ Cet f would be amenable to thermal infrared characterization. Further efforts to model the near-infrared reflectance and mid-infrared emission of these and other short-period planets are clearly warranted, and will pave the way for the interpretation of future high-contrast characterization of a variety of planets around the nearest stars.

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“…This work, although promising, was not extended beyond his specific interest in the form of the reddening curve. Kuiper et al [43] also used a lead sulphide photocell in an infrared spectrometer and published stellar spectra, but thereafter turned the instrument to planetary studies.…”

Section: Starting Over Againmentioning

confidence: 99%

History of infrared telescopes and astronomy

Rieke

2009

Exp Astron

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The first attempts to measure the infrared outputs of stars preceded by nearly a century the permanent establishment of infrared astronomy as an important aspect of the field. There were a number of false starts in that century, significant efforts that had little impact on the astronomical community at large. Why did these efforts fizzle out? What was different in the start that did not fizzle, in the 1960s? I suggest that the most important advances were the success of radio astronomy in demonstrating interesting phenomena outside of the optical regime, and the establishment virtually simultaneously in the United States of a number of research groups that could support each other and compete against one another in their approach to infrared astronomy.

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An Infrared Stellar Spectrometer.

Cited by 34 publications

References 0 publications

The Way to Measure the Surface Temperature through PbS-Photoconductive Cell

The Way to Measure the Surface Temperature through PbS-Photoconductive Cell

On high-contrast characterization of nearby, short-period exoplanets with giant segmented-mirror telescopes

History of infrared telescopes and astronomy

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