The Emission Spectrum of the CO2+ Ion: Band System

1975 ◽  
Vol 53 (19) ◽  
pp. 2040-2059 ◽  
Author(s):  
D. Gauyacq ◽  
M. Horani ◽  
S. Leach ◽  
J. Rostas
Keyword(s):  
Emission Spectrum ◽  
Spectral Resolution ◽  
Band System ◽  
High Spectral Resolution ◽  
Vibronic Transition ◽  
Electronic Band ◽  
Rotational Constants ◽  
Band Origin ◽  
Resolution Analysis ◽  
Vibronic Level

The [Formula: see text] and [Formula: see text] transitions of the CO2+ ion were photographed in emission under high spectral resolution. Analysis of the electronic band origin of the [Formula: see text] transition has provided rotational constants which are more refined and extensive than those previously known. The presence of a perturbation at J′ ~ 36.5 in the [Formula: see text] vibronic level was confirmed and a second stronger perturbation was shown to exist for values of J′ < 20.5.The four subbands 0110 2Πg–0100 μ2Σu, 0110 2Πg–0120 2Δu5/2, 0110 2Πg–0120 2Δu3/2, and 0110 2Πg–0100 κ2Σu of the Renner–Teller split [Formula: see text] vibronic transition 010–010 were identified and rotationally analyzed. The results lead to values of [Formula: see text], [Formula: see text], [Formula: see text], and [Formula: see text].

Searching for 3D effects in the optical, high spectral resolution emission spectrum of KELT-9b

2021 ◽  
Author(s):  
Lorenzo Pino ◽  
Matteo Brogi ◽  
Jean-Michel Désert ◽  
Emily Rauscher
Keyword(s):  
Emission Spectrum ◽  
Spectral Resolution ◽  
Planet Formation ◽  
Emission Spectra ◽  
Optical Emission ◽  
High Spectral Resolution ◽  
Optical Emission Spectrum ◽  
Hot Jupiters ◽  
Atmospheric Structure ◽  
3D Effects

&lt;p&gt;Ultra-hot Jupiters (UHJs; T&lt;sub&gt;eq&lt;/sub&gt; &amp;#8805; 2500 K) are the hottest gaseous giants known. They emerged as ideal laboratories to test theories of atmospheric structure and its link to planet formation. Indeed, because of their high temperatures, (1) they likely host atmospheres in chemical equilibrium and (2) clouds do not form in their day-side. Their continuum, which can be measured with space-facilities, can be mostly attributed to H- opacity, an indicator of metallicity. From the ground, the high spectral resolution emission spectra of UHJs contains thousands of lines of refractory (Fe, Ti, TiO, &amp;#8230;) and volatile species (OH, CO, &amp;#8230;), whose combined atmospheric abundances could track planet formation history in a unique way. In this talk, we take a deeper look to the optical emission spectrum of KELT-9b covering planetary phases 0.25 - 0.75 (i.e. between secondary eclipse and quadrature), and search for the effect of atmospheric dynamics and three-dimensionality of the planet atmosphere on the resolved line profiles, in the context of a consolidated statistical framework. We discuss the suitability of the traditionally adopted 1D models to interprete phase-resolved observations of ultra-hot Jupiters, and the potential of this kind of observations to probe their 3D atmospheric structure and dynamics. Ultimately, understanding which factors affect the line-shape in UHJs will also lead to more accurate and more precise abundance measurements, opening a new window on exoplanet formation and evolution.&lt;/p&gt;

The rotational analysis of the A1Π–X1Σ+ system of Si130Te

1992 ◽  
Vol 70 (5) ◽  
pp. 291-294 ◽  
Author(s):  
Sheila Gopal ◽  
M. Singh ◽  
G. Lakshminarayana
Keyword(s):  
High Resolution ◽  
Emission Spectrum ◽  
Microwave Discharge ◽  
Band System ◽  
Rotational Structure ◽  
Quartz Tube ◽  
Rotational Analysis ◽  
Rotational Constants

The emission spectrum of Si130Te was excited by microwave discharge (2450 MHz) in a sealed quartz tube. The A1Π–X1Σ+ band system (3100–3900 Å) (1 Å = 10−10 m) photographed under high resolution on a 10.6 m Ebert grating spectrograph. The rotational analysis of 32 bands was carried out, which led to the determination of the accurate vibrational and rotational constants. The rotational structure belonging to ν′ > 9 levels appear to be perturbed.

High spectral resolution analysis of tunable narrowband resonant grating waveguide structures

2007 ◽  
Vol 89 (2-3) ◽  
pp. 151-154 ◽  
Author(s):  
M.A. Bader ◽  
A. Selle ◽  
O. Stenzel ◽  
R. Delmdahl ◽  
G. Spiecker ◽  
...  
Keyword(s):  
Spectral Resolution ◽  
High Spectral Resolution ◽  
Resonant Grating ◽  
Resolution Analysis

scholarly journals IRC +10216 as a spectroscopic laboratory: improved rotational constants for SiC2, its isotopologues, and Si2C

2018 ◽  
Vol 618 ◽  
pp. A4 ◽  
Author(s):  
J. Cernicharo ◽  
M. Guélin ◽  
M. Agúndez ◽  
J. R. Pardo ◽  
S. Massalkhi ◽  
...  
Keyword(s):  
Spectral Resolution ◽  
Molecular Species ◽  
Signal To Noise Ratio ◽  
Laboratory Data ◽  
High Spectral Resolution ◽  
Circumstellar Envelope ◽  
Centrifugal Distortion ◽  
Rotational Constants ◽  
Good Signal ◽  
Centrifugal Distortion Constants

This work presents a detailed analysis of the laboratory and astrophysical spectral data available for 28SiC2, 29SiC2, 30SiC2, Si13CC, and Si2C. New data on the rotational lines of these species between 70 and 350 GHz have been obtained with high spectral resolution (195 kHz) with the IRAM 30 m telescope in the direction of the circumstellar envelope IRC +10216. Frequency measurements can reach an accuracy of 50 kHz for features observed with a good signal to noise ratio. From the observed astrophysical lines and the available laboratory data new rotational and centrifugal distortion constants have been derived for all the isotopologues of SiC2, allowing us to predict their spectrum with an estimated accuracy better than 50 kHz below 500 GHz and around 50–100 kHz for the strong lines above 500 GHz. Improved rotational and centrifugal distortion constants have also been obtained for disilicon carbide, Si2C. This work shows that observations of IRC +10216 taken with the IRAM 30 m telescope, with a spectral resolution of 195 kHz, can be used for any molecular species detected in this source to derive, or improve, its rotational constants. Hence, IRC +10216 in addition to be one the richest sources in molecular species in the sky, can also be used as a spectroscopy laboratory in the millimetre and submillimetre domains.

ROTATIONAL ANALYSIS OF THE β BANDS OF PHOSPHORUS MONOXIDE

1959 ◽  
Vol 37 (2) ◽  
pp. 136-143 ◽  
Author(s):  
Nand Lal Singh
Keyword(s):  
Ground State ◽  
Band System ◽  
Electronic States ◽  
Rotational Analysis ◽  
Rotational Constants ◽  
Fine Structures ◽  
Π State

The fine structures of three of the β bands of PO which occur near 3200 Å have been analyzed. The analysis shows that the upper state of this band system is a 2Σ and not a 2Π state as previously believed. The rotational constants of both electronic states have been determined and it is found that the ground state constants, previously determined from the γ bands, are incorrect.

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