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published time ↑
Dark Energy Survey Data Release 2
Publish Time: 2024-11-30
Dark Energy Survey Data Release 2 (DES DR2) is a dataset captured by the Dark Energy Camera (DECam), which is mounted on the Blanco Telescope at the Cerro Tololo Inter-American Observatory in Chile. The data from DES DR2 originates from observations conducted between August 15, 2013, and January 9, 2019, spanning 681 distinct observation nights. The data primarily consists of wide-field imaging and time-domain project data, with the wide-field footprint designed to significantly overlap with the South Pole Telescope (SPT) survey and SDSS Stripe 82 to enhance overall calibration. DES DR2 includes 96,263 DECam exposures, of which 83,706 are part of the wide-field survey and 12,557 are part of supernova surveys and other projects. Characteristically, each location in DES DR2 is typically observed by 7-10 overlapping DECam exposures in the griz bands. The median point spread function (PSF) full width at half maximum (FWHM) across different bands are: g=1.11", r=0.95", i=0.88", z=0.83", and Y=0.90". The processing methods involve image processing, astrometric calibration, and photometric calibration. The data is processed through the DESDM pipeline, which includes image correction, astrometric calibration, and photometric calibration to ensure the consistency and accuracy of the data. In terms of quality, the exposures in DES DR2 have a median airmass of 1.2, with over 99% of the exposures having a airmass less than 1.4. All magnitudes in all bands are expressed in the AB system (Oke 1974), and all astrometric coordinates are provided in the Gaia-CRF2 reference frame (Gaia Collaboration 2018). The DES DR2 dataset has a wide range of applications, including the study of dark energy, mapping of the large-scale structure of the universe, research on galaxy evolution, and the distance estimation of Type Ia supernovae. Here we have both the image and catalog data. And these data are downloaded from https://desdr-server.ncsa.illinois.edu/despublic/dr2_tiles/. You can get the more detailed information through https://des.ncsa.illinois.edu/releases/dr2.
Zwicky Transient Facility Data Release 21
Publish Time: 2024-10-21
The Zwicky Transient Facility (ZTF) conducts a wide-field time-domain survey using the Samuel Oschin 48-inch Schmidt Telescope at Palomar Observatory. The initial observations began in March 2018, and since the first data release, new versions of the data have been published regularly, approximately every two to six months. ZTF Data Release 21 (DR21) includes observational data from March 17, 2018, to February 29, 2024, spanning about 71 months. This encompasses both public and private survey projects, with private survey observations concluding on October 31, 2022. The camera used for observations consists of 16 CCDs, each divided into 4 readout quadrants, resulting in 64 CCD-quadrant images. Each quadrant covers an area of approximately 0.854° by 0.854° on the sky. Observations are primarily conducted in the g, r, and i bands, with i-band data originating from private survey time. The main exposure time is 30 seconds, although private surveys also include exposures of 60, 90, 120, 240, and 300 seconds. Data products include raw CCD images, calibrated science images, reference images, difference images, catalogs, and light curves. The processing pipeline is managed by the ZTF Science Data System (ZSDS) at IPAC/Caltech and includes astrometric and photometric calibration, image co-addition, and difference imaging. ZTF DR21 contains approximately 56.3 million single-exposure images, 176 thousand co-added images, 860 billion detected sources, and about 4.89 billion light curves. Data quality has undergone basic automated checks but may still contain low-quality data affected by factors such as clouds, atmospheric transparency variations, and moonlight contamination. Users can filter data using quality flags. Calibrated ZTF photometry may exhibit systematic biases of up to 0.025 magnitudes for bright sources (brighter than 15.5 magnitude), and these biases are corrected in the light curve data. ZTF DR21 is a valuable resource for time-domain astronomy research, covering a large portion of the northern sky, with a long time span and moderate depth across multiple bands. The mirrored data in this release includes only light curve data. Files are organized in subdirectories by observational field ID, with each field covering an area of approximately 7° by 7°. The DR21 light curve data spans 1,181 fields, with a total of 176,218 parquet files. These files can be read using libraries such as Pandas, pyarrow, or Dask. For more detailed instructions on using the light curve files, refer to section 12.c of the ZTF DR21 documentation. The documentation can be accessed at the following link: https://irsa.ipac.caltech.edu/data/ZTF/docs/releases/dr21/ztf_release_notes_dr21.pdf.
Digitized Data of China Astronomical Plates: Image and Astrometric Catalog
Publish Time: 2024-03-08
DOI: 10.12149/100742
CSTR: 11379.11.100742
Astronomical plates are the precious heritage of astronomical observation research. With the support of the Special Key Project for Fundamental Work in Science and Technology of the Ministry of Science and Technology, the Shanghai plate digitization laboratory completed the scanning and archiving of 29,314 plates in 2017. On this basis, the research team of Shanghai Astronomical Observatory conducted further astrometric calibration work on the digitized astronomical plates based on the Gaia DR2 catalog, converting the initial version of the digital plates into astronomical digital images in the standard fits format to satisfy the research work of relevant professional astronomers. The current data release contains 15,696 high quality digital plates and corresponding astrometric results, with the observation targets mainly being extrasolar objects. This batch of data contains observations from nine telescopes at five Chinese astronomical stations, namely, the National Astronomical Observatory, the Shanghai Astronomical Observatory, the Purple Mountain Observatory, the Yunnan Astronomical Observatory, and the Qingdao Observatory, and spans the period from 1901 to 1998. The astrometric precision is mainly related to the focal length of the telescopes. For the plates of long focal length telescopes, such as the 40cm binoculars refractor telescope and the 1.56-meter reflector telescope of the Shanghai Astronomical Observatory, and the 1-meter reflector telescope of the Yunnan Astronomical Observatory, the astrometric precison can be as high as 0.1-0.3″. The differences between this release and the "Digitized Data of China Astronomical Plates: Early Data Release" are as follows: (1) The fits header information of all 6,615 astronomical plates in the early batch has been updated, and the astrometric results of these plates have been added. (2) 9081 astronomical plates and the corresponding astrometric results have been added.
Map of the surface of the Moon(the Third Edition)
Publish Time: 2024-02-22
DOI: 10.12149/100891
CSTR: 11379.21.100891
The third edition of ultra-high definition lunar surface map, with 450 million pixels, has 1294 lunar surface land place names marked, including 15 different types of landmarks, covering almost all lunar surface landmarks with observational value that can be seen by amateur telescopes, including 655 Crater, 348 Satellite Feature, 19 Oceanus, 17 Mare, 10 Sinus, 3 Palus, 9 Promontorium, 103 Rima, 8 Vallis, 43 Mons, and 37 Dorsums, 8 Rupes, 9 Catena, 1 Albedo Feature point and 24 Landing Site Names. Compared to the second version, the third board has made improvements in the following aspects: (1) adding new landmarks for four crater and eleven rimaes--Armstrong crater, Collins ,Aldrin crater, Bobillier, Rimae Pitatus, Rimae Aristarchus, Rimae Apollonius, RimaeVladimir, Rima Flammarion, Rimae Gassendi, Rima Rudolf, Rima Mairan, Rimae Palmieri, Rimae Parry, Rimae Chacornac; (2) correcting three incorrect markings--Rima Revise the Rimae Aristarchus to the Rimae Alzimovich, correct the position of the Vallis Snellius , and move the position of the Yangel' crater to the correct position; and (3) providing more precise markings for terrain with unclear markings-- add boxes, circles, or arrows to accurately identify landmarks such as Rima, Rupes, Mons, Dorsums, Promontorium etc that are not clearly labeled yet. If you have more suggestions on the revision of land place names, please contact Liu Jing of Dongguan Science Museum or the National Astronomical Data Center.
FASHI Data Release 1
Publish Time: 2023-12-13
DOI: 10.12149/100875
CSTR: 11379.11.100875
The FAST All Sky HI survey (FASHI) was designed to cover the entire sky observable by the Five-hundred-meter Aperture Spherical radio Telescope (FAST), spanning approximately 22000 square degrees of declination between -14 deg and +66 deg, and in the frequency range of 1050-1450 MHz, with the expectation of eventually detecting more than 100000 HI sources. Between August 2020 and June 2023, FASHI had covered more than 7600 square degrees, which is approximately 35% of the total sky observable by FAST. It has a median detection sensitivity of around 0.76 mJy/beam and a spectral line velocity resolution of ~6.4 km/s at a frequency of ~1.4 GHz. As of now, a total of 41741 extragalactic HI sources have been detected in the frequency range 1305.5-1419.5 MHz, corresponding to a redshift limit of z<0.09. By cross-matching FASHI sources with the Siena Galaxy Atlas (SGA) and the Sloan Digital Sky Survey (SDSS) catalogs, we found that 16972 (40.7%) sources have spectroscopic redshifts and 10975 (26.3%) sources have only photometric redshifts. Most of the remaining 13794 (33.0%) HI sources are located in the direction of the Galactic plane, making their optical counterparts difficult to identify due to high extinction or high contamination of Galactic stellar sources. Based on current survey results, the FASHI survey is an unprecedented blind extragalactic HI survey. It has higher spectral and spatial resolution and broader coverage than the Arecibo Legacy Fast ALFA Survey (ALFALFA). When completed, FASHI will provide the largest extragalactic HI catalog and an objective view of HI content and large-scale structure in the local universe.
Solar Physics Historical Data
Publish Time: 2023-09-01
DOI: 10.12149/100777
CSTR: 11379.11.100777
This project primarily involves the processing of historical solar observation data in China, sourced from multiple domestic solar observation stations. The data exists in various formats such as paper, film, and glass plates, and is primarily scanned and digitized for electronic presentation. The electronic data generated includes: hand-drawn sunspot maps for China from 1925 to 2015, solar eclipse spectroscopic plates from Papua New Guinea in 1983, historical data from the National Astronomical Observatory of China's solar radio flux meter from 1958 to 1994, historical observation data from the National Astronomical Observatory of China's solar radio spectrometer from 1994 to 2014, solar spectrum magnetic field data from Yunnan Observatory from 1976 to 1985, fine structure plates of the sun from Yunnan Observatory from 1984 to 1993, full-disk chromosphere plates from Yunnan Observatory from 1981 to 1994, solar-terrestrial physics data for China from 1971 to 2001, and important solar eruption event data from 2000 to 2014. Some of the data in the project is electronically preserved and has undergone scientific-level data processing to provide data suitable for scientific applications. The standardization of data into scientific-grade data includes: solar magnetic field observation data from Huairou, Beijing from 1987 to 2011, solar velocity field observation data from Huairou, Beijing from 1987 to 2011, and two-dimensional spectroscopic observation data from the solar tower from 1999 to 2015. Throughout the data processing process of the entire project, various data processing software has been developed, and a standardization report for solar physics data has been established. The data processing software includes digitization of solar radio paper tape observation data, software for extracting information from scanned images, software capable of handling multiple data levels, and standardized data processing software. The standardization report for solar physics data is primarily based on international standards combined with specific data processing procedures.
The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)
Publish Time: 2017-10-23
The fourth United States Naval Observatory (USNO) CCD Astrograph Catalog, UCAC4, was released in 2012 August (double-sided DVD and CDS data center Vizier catalog I/322). It is the final release in this series and contains over 113 million objects; over 105 million of them with proper motions (PMs). UCAC4 is an updated version of UCAC3 with about the same number of stars also covering all-sky. Bugs were fixed, Schmidt plate survey data were avoided, and precise five-band photometry was added for about half the stars. Astrograph observations have been supplemented for bright stars by FK6, Hipparcos, and Tycho-2 data to compile a UCAC4 star catalog complete from the brightest stars to about magnitude R=16. Epoch 1998–2004 positions are obtained from observations with the 20 cm aperture USNO Astrograph’s “red lens,” equipped with a 4k by 4k CCD. Mean positions and PMs are derived by combining these observations with over 140 ground- and space-based catalogs, including Hipparcos/Tycho and the AC2000.2, as well as unpublished measures of over 5000 plates from other astrographs. For most of the faint stars in the southern hemisphere, the first epoch plates from the Southern Proper Motion program form the basis for PMs, while the Northern Proper Motion first epoch plates serve the same purpose for the rest of the sky. These data are supplemented by 2MASS near-IR photometry for about 110 million stars and five-band (B,V,g,r,i) APASS data for over 51 million stars. Thus the published UCAC4, as were UCAC3 and UCAC2, is a compiled catalog with the UCAC observational program being a major component. The positional accuracy of stars in UCAC4 at mean epoch is about 15–100 mas per coordinate, depending on magnitude, while the formal errors in PMs range from about 1 to 10 mas/yr depending on magnitude and observing history. Systematic errors in PMs are estimated to be about 1–4 mas/yr