Fluences of solar energetic particles (SEPs) are not easy to evaluate, especially for high-energy events (i.e. ground-level enhancements, GLEs). Earlier estimates of event-integrated SEP fluences for GLEs were based on partly outdated assumptions and data, and they required revisions. Here, we present the results of a full revision of the spectral fluences for most major SEP events (GLEs) for the period from 1956-2017 using updated low-energy flux estimates along with greatly revisited high-energy flux data and applying the newly invented reconstruction method including an improved neutron-monitor yield function. Low- and high-energy parts of the SEP fluence were estimated using a revised space-borne/ionospheric data and ground-based neutron monitors, respectively. The measured data were fitted by the modified Band function spectral shape. The best-fit parameters and their uncertainties were assessed using a direct Monte Carlo method. A full reconstruction of the event-integrated spectral fluences was performed in the energy range above 30MeV, parametrised and tabulated for easy use, along with estimates of the 68% confidence intervals. This forms a solid basis for more precise studies of the physics of solar eruptive events and the transport of energetic particles in the interplanetary medium, as well as the related applications.
The CNS3 catalog contains all known stars as of 1991 that are within 25 parsecs of the Sun. It depends mainly on a preliminary version (Spring 1989) of the new General Catalogue of Trigonometric Parallaxes (YPC) prepared by Dr. William F. van Altena (Yale University). The catalog contains every then-known star with a trigonometric parallax greater than or equal to 0.0390 arcsec, even though it may be evident from photometry or for other reasons that the star has a larger distance. For red dwarf stars, new color-magnitude calibrations for broad-band colors were carried out and applied. For white dwarfs, the recipes of McCook and Sion in ApJS, 65, 603 (1987) were applied. Stroemgren photometry was used (not yet systematically) for early-type stars and for late dwarfs, the latter supplied by E. H. Olsen from Copenhagen Observatory (private communication). In contrast to the CNS2 (Gliese 1969) catalog, trigonometric parallaxes and photometric or spectroscopic parallaxes were not combined in this version. The resulting parallax in the present version is the trigonometric parallax if the relative error of the trigonometric parallax is smaller than 14 percent. The parallax may be the photometric or spectroscopic parallax only if no trigonometric parallax is available or if the standard error of the trigonometric parallax is considerably larger. The original catalog and the notes describing it were prepared by Wilhelm Gliese and Hartmut Jahreiss, Astronomisches Rechen-Institut, Moenchhofstrasse 12-14, D-6900 Heidelberg 1, Germany, in 1991. The CDS has made a number of formatting and documentation changes in the period 1994-1997, e.g., in December 1997 it added a running number to the name for 1388 stars which had all been given the same name of "NN" in the original version, starting with "NN 3001" (for the first "NN" star in order of 1950 RA), and ending with "NN 4388" (for the last "NN" star in order of 1950 RA). This revised version of the catalog (CDS/ADC Catalog V/70A) was used by the HEASARC to create this database in February 2001. This is a service provided by NASA HEASARC .
We provide precise J2000/epoch 2000 coordinates and cross-identifications to sources in the 2MASS Point Source Catalog for nearly all stars in the Gliese, Gliese-Jahreiss, and Woolley catalogs of nearby stars. The only Gliese objects where we were not successful are two Gliese sources that are actually QSOs; two proposed companions to brighter stars, which we believe do not exist; four stars included in one of the catalogs but identified there as only optical companions; one probable plate flaw; and two stars that simply remain unrecovered. For the 4251 recovered stars, 2693 have coordinates based on Hipparcos positions, 1549 have coordinates based on 2MASS data, and 9 have positions from other astrometric sources. All positions have been calculated at epoch 2000 using proper motions from the literature, which are also given here.
Gliese Catalog Stars with Accurate Coordinates and 2MASS Cross-Identifications
Short Name:
GLIESE2MAS
Date:
27 Sep 2024
Publisher:
NASA/GSFC HEASARC
Description:
This table contains precise epoch 2000 coordinates and cross-identifications to sources in the 2MASS Point Source Catalog for nearly all stars in the Gliese, Gliese-Jahreiss, and Woolley catalogs of nearby stars. The only Gliese objects where the authors were not successful are two Gliese sources that are actually QSOs; two proposed companions to brighter stars, which they believe do not exist; four stars included in one of the catalogs but identified there as only optical companions; one probable plate flaw; and two stars that simply remain unrecovered. For the 4251 recovered stars, 2693 have coordinates based on Hipparcos positions, 1549 have coordinates based on 2MASS data, and 9 have positions from other astrometric sources. All positions have been calculated at epoch 2000 using proper motions from the literature, which are also given here. This table was created by the HEASARC in May 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/PASP/122/885">CDS Catalog J/PASP/122/885</a> file table1.dat. This is a service provided by NASA HEASARC .
GLIMPSE360 is a Warm Mission Spitzer Cycle 6 Exploration Science Program (PIDs 60020, 61070, 61071, 61072, 61073, 70072) that mapped 187 degrees of longitude of the Galactic plane that have not been mapped by previous Spitzer Galactic Plane surveys (GLIMPSE, GLIMPSEII, GALCEN, GLIMPSE3D, Vela Carina, SMOG and Cygnus-X). The specific Galactic longitudes covered by GLIMPSE360 are l=65◦-76◦, 82◦-102◦, and 109◦-265◦. The latitude range is about 2.8◦. The latitude center follows the Galactic warp. GLIMPSE360 completes the full circle of the Galactic plane.
The GLIMPSE360 Archive (GLM360A or the “Archive”) consists of point sources with less stringent selection critera than the Catalog. The information provided is in the same format as the Catalog. The Catalog is a subset of the Archive, but the entries for a particular source might not be the same due to additional nulling of magnitudes in the Catalog because of the more stringent requirements.
We present the results of a 6.7GHz methanol maser survey from the Effelsberg 100m radio telescope. A sample of 404 sources from the Bolocam Galactic Plane Survey (BGPS) 1.1mm dust clump survey that met specific Galactic Legacy Infrared Mid-Plane Survey Extraodinaire (GLIMPSE) point-source color criteria was selected and 318 of these were observed. The new observations resulted in the detection of 29 methanol masers, including 12 new ones. Together with the additional 74 detections from the literature, this means that a total of 103 methanol masers are coincident with 1.1mm dust clumps, yielding an overall detection rate of 26%. A comparison of the properties of a 1.1mm dust clump and a 6.7GHz methanol maser indicates that methanol masers with a higher flux density and/or luminosity are generally associated with more massive but less dense 1.1mm dust clumps. The overall detection rate of 26% appears to vary as a function of the derived H_2_ column density of the associated 1.1mm dust clump. The methanol masers were primarily detected toward the brighter and more massive 1.1mm dust clumps. A subsample of 194 sources that overlapped sources with observations of the 95GHz methanol line was investigated in more detail for the properties of 1.1mm dust clumps. The statistical analysis reveals that 1.1mm dust clumps with both class I and II counterparts have much higher mean and median values of mass, column density, and flux density than those with only class I or II counterparts. Based on our much larger sample, we slightly revise the boundary defined previously for selecting BGPS sources associated with a class II methanol maser, wherein ~80% of expected class II methanol masers will be detected with a detection rate in the range of 40-50%.
GLIMPSE360 is a Warm Mission Spitzer Cycle 6 Exploration Science Program (PIDs 60020, 61070, 61071, 61072, 61073, 70072) that mapped 187 degrees of longitude of the Galactic plane that have not been mapped by previous Spitzer Galactic Plane surveys (GLIMPSE, GLIMPSEII, GALCEN, GLIMPSE3D, Vela Carina, SMOG and Cygnus-X). The specific Galactic longitudes covered by GLIMPSE360 are l=65◦-76◦, 82◦-102◦, and 109◦-265◦. The latitude range is about 2.8◦. The latitude center follows the Galactic warp. GLIMPSE360 completes the full circle of the Galactic plane.
The GLIMPSE360 Catalog (GLM360C, or the “Catalog”) consists of the highest reliability point sources. For each IRAC band the Catalog provides fluxes (with uncertainties), positions (with uncertainties), the areal density of local point sources, the local sky brightness, and a flag that provides information on source quality and known anomalies present in the data.
The Cygnus-X Catalog and Archive contain sources from longitudes l=76-82d extracted from data processed using the GLIMPSE pipeline. There are two types of source lists: a high reliability point source Catalog and a more complete point source Archive.
The Cygnus-X Catalog and Archive contain sources from longitudes l=76-82d extracted from data processed using the GLIMPSE pipeline. There are two types of source lists: a high reliability point source Catalog and a more complete point source Archive.
GLIMPSE3D is the third in a series of large area projects to map selected regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). GLIMPSEI1 covered the Galactic plane from |l| = 10◦ to 65◦ and |b| < 1◦; GLIMPSEII filled in the inner 20 degrees of the Galactic plane, |l| < 10◦, with vertical extensions up to ±1.5◦ for |l| =5◦to 2◦, and up to ±2◦ from |l| =2◦to 0◦. GLIMPSE3D adds vertical extensions, generally up to |b| < 3◦, but up to |b| < 4.2◦ in the center of the Galaxy. The goal of this coverage is to provide data to study the vertical stellar and interstellar
The GLIMPSE3D Archive (GLM3DA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSE3D Catalog is a subset of the Archive, but note that the entries for a particular source might not be the same due to additional nulling of magnitudes in the Catalog because of the more stringent requirements.