Submillimeter, millimeter, and microwave spectral line catalog

Poynter, R. L.; Pickett, Herbert M.

doi:10.1364/ao.24.002235

Cited by 195 publications

(107 citation statements)

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“…The appropriate parameters are taken from the JPL spectral line catalog [Poynter and Pickett, 1985]. The inversion calculations are performed using Rodgers optimal estimation method (OEM) [Rodgers, 1976].…”

Section: Methodsmentioning

confidence: 99%

Water vapor of the polar middle atmosphere: Annual variation and summer mesosphere Conditions as observed by ground‐based microwave spectroscopy

Seele

Hartogh

1999

Geophysical Research Letters

111

100

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Abstract. We have been operating a ground-based microwave radiometer for the 22.235GHz water vapor line at the ALOMAR observatory, Norway, in 1995/96 and continuously since July 1997. Its high latitude location (69øN, 16øE) provides a new and unique dataset of stratospheric and mesospheric water vapor observations. We briefly describe our instrument and measuring technique and present the data of our ongoing measurements. The water vapor mixing ratio shows a pronounced annual cycle that is stronger than what has been reported for mid-latitudes. We also present an analysis of our data for the upper mesosphere for the relationships between mesospheric water vapor, temperature, polar mesosphere summer echoes (PMSE), and noctilucent clouds (NLC) during summer months. This investigation indicates that water vapor is already present near mesopause heights when the PMSE/NLC season starts and is still present long after it has declined.

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Section: Methodsmentioning

confidence: 99%

Water vapor of the polar middle atmosphere: Annual variation and summer mesosphere Conditions as observed by ground‐based microwave spectroscopy

Seele

Hartogh

1999

Geophysical Research Letters

111

100

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“…We modeled this spectrum in the local thermodynamic equilibrium using the XCLASS software developed by Peter Schilke (private communication). This software package uses the line catalogs from JPL and CDMS (Poynter & Pickett 1985;Müller et al 2001). The model spectrum with a temperature of 150 K is shown in Fig.…”

Section: Temperature From Chmentioning

confidence: 99%

Different evolutionary stages in the massive star-forming region S255 complex

Wang

Beuther

Bik

et al. 2011

A&A

108

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Aims. Massive stars form in clusters, and they are often found in different evolutionary stages located close to each other. To understand evolutionary and environmental effects during the formation of high-mass stars, we observed three regions of massive star formation at different evolutionary stages, and all are found that in the same natal molecular cloud. Methods. The three regions, S255IR, S255N, and S255S, were observed at 1.3 mm with the submillimeter array (SMA), and followup short spacing information was obtained with the IRAM 30 m telescope. Near infrared (NIR) H + K-band spectra and continuum observations were taken for S255IR with VLT-SINFONI to study the different stellar populations in this region.Results. This combination of millimeter (mm) and near infrared data allow us to characterize different stellar populations within the young forming cluster in detail. While we find multiple mm continuum sources toward all regions, their outflow, disk, and chemical properties vary considerably. The most evolved source S255IR exhibits a collimated bipolar outflow visible in CO and H 2 emission, and the outflows from the youngest region S255S are still small and fairly confined in the regions of the mm continuum peaks. Also the chemistry toward S255IR is the most evolved, exhibiting strong emission from complex molecules, while much fewer molecular lines are detected in S255N, and in S255S we detect only CO isotopologues and SO lines. Also, rotational structures are found toward S255N and S255IR. Furthermore, a comparison of the NIR SINFONI and mm data from S255IR clearly reveal two different (proto) stellar populations with an estimated age difference of approximately 1 Myr. Conclusions. A multiwavelength spectroscopy and mapping study reveals different evolutionary phases of the star formation regions. We propose the triggered outside-in collapse star formation scenario for the bigger picture and the fragmentation scenario for S255IR.

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“…[112] BEAM uses an internal spectroscopic database that was originally produced in 1995 from earlier versions of the JPL catalog [Poynter and Pickett, 1985] and HITRAN [Rothman et al, 1992]. Today, the BEAMCAT database [Feist, 2004[Feist, , 1999b can be used to produce merged database files from the most recent versions of these catalogs [Pickett et al, 1998;Rothman et al, 1998].…”

Section: A2 Bernese Atmospheric Model (Beam)mentioning

confidence: 99%

Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range

et al. 2005

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[1] We compare a number of radiative transfer models for atmospheric sounding in the millimeter and submillimeter wavelength range, check their consistency, and investigate their deviations from each other. This intercomparison deals with three different aspects of radiative transfer models: (1) the inherent physics of gaseous absorption lines and how they are modeled, (2) the calculation of absorption coefficients, and (3) the full calculation of radiative transfer for different geometries, i.e., up-looking, down-looking, and limblooking. The correctness and consistency of the implementations are tested by comparing calculations with predefined input such as spectroscopic data, line shape, continuum absorption model, and frequency grid. The absorption coefficients and brightness temperatures calculated by the different models are generally within about 1% of each other. Furthermore, the variability or uncertainty of the model results is estimated if (except for the atmospheric scenario) the input such as spectroscopic data, line shape, and continuum absorption model could be chosen freely. Here the models deviate from each other by about 10% around the center of major absorption lines. The main cause of such discrepancies is the variability of reported spectroscopic data for line absorption and of the continuum absorption model. Further possible causes of discrepancies are different frequency and pressure grids and differences in the corresponding interpolation routines, as well as differences in the line shape functions used, namely a prefactor of (n/n 0 ) or (n/n 0 ) 2 of the Van-Vleck-Weisskopf line shape function. Whether or not the discrepancies affect retrieval results remains to be investigated for each application individually.Citation: Melsheimer, C., et al. (2005), Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range, Radio Sci., 40, RS1007,

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Submillimeter, millimeter, and microwave spectral line catalog

Cited by 195 publications

References 0 publications

Water vapor of the polar middle atmosphere: Annual variation and summer mesosphere Conditions as observed by ground‐based microwave spectroscopy

Water vapor of the polar middle atmosphere: Annual variation and summer mesosphere Conditions as observed by ground‐based microwave spectroscopy

Different evolutionary stages in the massive star-forming region S255 complex

Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range

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