- ID:
- ivo://CDS.VizieR/J/A+A/656/A160
- Title:
- Comet C/2020 F3 (NEOWISE) emission lines
- Short Name:
- J/A+A/656/A160
- Date:
- 21 Mar 2022 09:16:33
- Publisher:
- CDS
- Description:
- Comet C/2020 F3 (NEOWISE) is considered to be the brightest comet observed in the northern hemisphere since the passage of comet C/1995 O1 (Hale-Bopp) in 1997. Since the study of comets offers a unique opportunity to investigate the early stages of the formation and evolution of our Sun and the Solar System, we obtained high-resolution optical spectra (R={lambda}/{Delta}{lambda}=115000) of comet NEOWISE. The unique passage and its brightness yielded spectra with a large number of emission lines, providing information on the coma composition and the physical and chemical processes occurring in the nucleus. The spectra have been used to generate a catalog of emission lines to be used for future studies of comets since there are no catalogs in the literature with such a high spectral resolution. Two high-resolution spectra of comet NEOWISE were obtained, on 26 July 2020 (geocentric distance of 0.7au) and 5 August 2020 (geocentric distance of 0.89au), with the High Accuracy Radial velocity Planet Searcher for the Northern hemisphere (HARPS-N) echelle spectrograph installed on the 360cm Telescopio Nazionale Galileo (TNG). The spectra cover the range between 383 and 693nm, and have been extracted using the HARPS-N Data Reduction Pipeline. To analyze the spectra and compile the high-resolution catalog, we collected several laboratory molecular line lists that cover the same wavelength range as that of our spectra. To validate the final identification, we compared our catalog with other atlases that resulted from the spectral analysis of other comets. We generate a high-spectral-resolution catalog of emission lines observed in comet NEOWISE, providing the identification for 4488 lines. We found cometary lines due to CN, CH, C_2_, C_3_, and NH_2_ and atomic lines due to NaI and [OI].
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/367/1049
- Title:
- Comet C/1995 O1 (Hale-Bopp) emission lines
- Short Name:
- J/A+A/367/1049
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- High-resolution and high signal-to-noise ratio spectra of Comet C/1995 O1 (Hale-Bopp), which provided continuous wavelength coverage from 5500{AA} to 8500{AA} and partial coverage from 4000{AA} to 5500{AA}, were obtained with the Coude Echelle Spectrograph at Beijing Astronomical Observatory on March 26, 28 and April 22, 1997. In the spectra we found 532 emission features, among which 459 lines from H, O, Na, C_2_, C_3_, CN, CH, NH_2_ and H_2_O^+^ were identified. The intensity of sodium emission lines at 5890 {AA} and 5896 {AA} on April 22 increased about 5 fold compared to that recorded on March 26 and 28. The intensity ratio I_{lambda}5577_/(I_{lambda}6300_+I_{lambda}6364_) of [O I] is consistent with the formation of excited O atoms from the photodissociation of H_2_O.
- ID:
- ivo://CDS.VizieR/J/A+A/619/A127
- Title:
- Comet C/2016 R2 (PanSTARRS) IRAM spectra
- Short Name:
- J/A+A/619/A127
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a multi-wavelength study of comet C/2016 R2 (PanSTARRS). This comet was observed on 23-24 January 2018 with the IRAM 30m telescope, and in January to March 2018 with the Nancay radio telescope. Visible spectroscopy was performed in December 2017 and February 2018 with small amateur telescopes. We report on measurements of CO, CH_3_OH, H_2_CO and HCN production rates, and on the determination of the N2/CO abundance ratio. Several other species, especially OH, were searched for but not detected. The inferred relative abundances, including upper limits for sulfur species, are compared to those measured in other comets at about the same heliocentric distance of ~2.8AU. The coma composition of comet C/2016 R2 is very different from all other comets observed so far, being rich in N2 and CO and dust poor. This suggests that this comet might belong to a very rare group of comets formed beyond the N_2_ ice line. Alternatively, comet C/2016 R2 (PanSTARRS) could be the fragment of a large and differentiated transneptunian object, with properties characteristic of volatile-enriched layers.
- ID:
- ivo://CDS.VizieR/J/A+A/647/A119
- Title:
- Comet 67P/Churyumov-Gerasimenko FUV aurora
- Short Name:
- J/A+A/647/A119
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We aim to determine whether dissociative excitation of cometary neutralsby electron impact is the major source of far-ultraviolet (FUV) emissions at comet 67P/Churyumov-Gerasimenkoin the southern hemisphere at large heliocentric distances, both during quiet conditions and impacts of corotating interaction regions observed in the summer of 2016. We combined multiple datasets from the Rosetta mission through a multi-instrument analysis to complete the first forward modelling of FUV emissions in the southern hemisphere of comet 67P and compared modelled brightnesses to observations with the Alice FUV imaging spectrograph. We modelled the brightness of OI1356, OI1304, Lyman-beta, CI1657, and CII1335 emissions, which are associated with the dissociation products of the four major neutral species in the coma: CO2, H2O, CO, and O2. The suprathermal electron population was probed by the Ion and Electron Sensor of theRosetta Plasma Consortium (RPC/IES) and the neutral column density was constrained by several instruments: the RosettaOrbiter Spectrometer for Ion and Neutral Analysis (ROSINA), the Microwave Instrument for the Rosetta Orbiter (MIRO)and the Visual InfraRed Thermal Imaging Spectrometer (VIRTIS). The modelled and observed brightnesses of the FUV emission lines agree closely when viewing nadir and dissociative excitation by electron impact is shown to be the dominant source of emissions away from perihelion. The CII1335 emissions are shown to be consistent with the volume mixing ratio of CO derived from ROSINA. When viewing the limb during the impacts of corotating interaction regions, the model reproduces brightnesses of OI1356 and CI1657 well, but resonance scattering in the extended coma may contribute significantly to the observed Lyman-beta and OI1304 emissions. The correlation between variations in the suprathermal electron flux and the observed FUV line brightnesses when viewing the comet's limb suggests electrons are accelerated on large scales and that they originate in the solar wind. This means that the FUV emissions are auroral in nature.
- ID:
- ivo://CDS.VizieR/J/A+A/461/789
- Title:
- Comet 153P/Ikeya-Zhang emission lines catalog
- Short Name:
- J/A+A/461/789
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A program of high resolution spectroscopy of comets is being conducted at TNG (Canary Islands) using the echelle spectrograph SARG. The aim of the program is to catalogue emission lines in the visible range of various comets, compare them and possibly identify the many existing unknown lines. As a first step, we catalogued the lines in the spectrum of the comet 153P/Ikeya-Zhang and compared them with the lines already listed in existing catalogues. The comet was observed with SARG on the night 19-20 of April, 2002, with a short slit covering the spectral range of 4620-7920{AA} and with a resolving power R=57000, finding 8468 emission lines.
- ID:
- ivo://CDS.VizieR/J/A+A/648/A49
- Title:
- Comet 46P/Wirtanen millimetre-wave spectra
- Short Name:
- J/A+A/648/A49
- Date:
- 08 Feb 2022
- Publisher:
- CDS
- Description:
- We present the results of a molecular survey of comet 46P/Wirtanen undertaken with the IRAM 30-m and NOEMA radio telescopes in December 2018. Observations at IRAM 30-m during the 12-18 Dec. period comprise a 2mm spectral survey, which covers 25GHz, and a 1mm survey which covers 62GHz. The gas outflow velocity and kinetic temperature have been accurately constrained by the observations. We derive abundances of 11 molecules, some being identified remotely for the first time in a Jupiter-family comet, including complex organic molecules such as formamide, ethylene glycol, acetaldehyde or ethanol. Sensitive upper limits on the abundances of 24 other molecules are obtained. The comet is found to be relatively rich in methanol (3.4% relative to water) but relatively depleted in CO, CS, HNC, HNCO or HCOOH.
- ID:
- ivo://CDS.VizieR/I/121
- Title:
- Common proper motions stars in AGK3
- Short Name:
- I/121
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The 326 common proper motion systems that have a ratio angular separation to proper motion smaller than 1000 years are in table1. The number of optical systems is expected to be around 4. Each system fills a 256 byte-length record that may also be considered as two 128 byte-length records for print-out edition. The 113 common proper motion systems that have a ratio angular separation to proper motion between 1000 and 3500 years are in table2. The number of physical systems is expected to be around 68. The presentation is the same as for table1. This table differs from the original printed version, since the the magnitude and the spectral type of the secondary component of the 47th system were corrected. The system 47 was also added to the notes.
- ID:
- ivo://CDS.VizieR/J/ApJ/835/75
- Title:
- Common proper motion stars in the Kepler field
- Short Name:
- J/ApJ/835/75
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In a search of proper motion catalogs for common proper motion stars in the field of the Kepler spacecraft I identified 93 likely binary systems. A comparison of their rotation periods is a test of the gyrochronology concept. To find their periods I calculated the autocorrelation function (ACF) of the Kepler mission photometry for each star. In most systems for which good periods can be found, the cooler star has a longer period than the hotter component, in general agreement with models. However, there is a wide range in the gradients of lines connecting binary pairs in a period-color diagram. Furthermore, near the solar color, only a few stars have longer periods than the Sun, suggesting that they, and their cooler companions, are not much older than the Sun. In addition, there is an apparent gap at intermediate periods in the period distribution of the late K and early M stars. Either star formation in this direction has been variable, or stars evolve in period at a non-uniform rate, or some stars evolve more rapidly than others at the same mass. Finally, using the ACF as a measure of the activity level, I found that while the F, G, and early K stars become less active as their periods increase, there is no correlation between period and activity for the mid K to early M stars.
- ID:
- ivo://CDS.VizieR/J/PASJ/60/1297
- Title:
- CO molecular clouds in Carina flare supershell
- Short Name:
- J/PASJ/60/1297
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a catalogue of ^12^CO(J=1-0) and ^13^CO(J=1-0) molecular clouds in the spatio-velocity range of the Carina Flare supershell, GSH287+04-17. The data cover a region of ~66 square degrees and were taken with the NANTEN 4m telescope, at spatial and velocity resolutions of ~2.6' and 0.1km/s. Decomposition of the emission results in the identification of 156 ^12^CO clouds and 60 ^13^CO clouds, for which we provide observational and physical parameters.
- ID:
- ivo://CDS.VizieR/J/PASJ/53/1081
- Title:
- CO molecular clouds in Lupus
- Short Name:
- J/PASJ/53/1081
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Lupus star-forming region has been surveyed for molecular clouds in ^12^CO with the NANTEN radio telescope, and a cloud mass of 1.7x10^4^M_{sun}_ has been revealed. We were able to detect 105 molecular clouds, most of which are relatively small and of low mass. The members of the Sco OB 2 association and the X-ray detected pre-main-sequence stars (PMSs) are distributed all around this region. The OB stars and the molecular clouds show exclusive distributions. Large fractions of the PMSs are located away from the molecular clouds, and are thus isolated. The origin of the isolated PMSs is discussed. About 40% of the PMSs have candidates of their parent clouds less massive than 20M_{sun}_ within 4pc, which suggests in-situ star formation in the small clouds and their rapid dissipation. The separations from the PMSs to the clouds are typically larger than those in the Chamaeleon region, probably because of coexisting OB stars. From the cloud structures and the distributions of the OB stars, PMSs, and H I expanding shell, it is suggested that the molecular clouds have been effectively dissipated by the OB stars and a shock wave, which may also have triggered star formation in Lupus and the {rho} Oph clouds.