AndreaBozzo/ceres-open-data-index huggingface dataset:
M 31 Chandra HRC X-Ray Source Catalog

The authors have obtained 17 epochs of Chandra High Resolution Camera (HRC) snapshot images, each covering most of the M31 disk. The data cover a total baseline of ~2.5 yr and contain a mean effective exposure of 17 ks. The authors measured the mean fluxes and long-term light curves for 166 objects detected in these data. At least 25% of the sources show significant variability. The cumulative luminosity function (CLF) of the disk sources is well fitted by a power law with a slope comparable to those observed in typical elliptical galaxies. The CLF of the bulge is a broken power law similar to measurements made by previous surveys. The authors note several sources in the southwestern disk with L&lt;sub&gt;X&lt;/sub&gt; &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. They cross-correlate all of their sources with published optical and radio catalogs, as well as new optical data, finding counterpart candidates for 55 sources. In addition, 17 sources are likely X-ray transients. Finally, the frequency of bright X-ray transients in the M31 bulge suggests that the ratio of neutron star to black hole primaries in low-mass X-ray binaries (NS/BH) is 1. The data for this project were originally part of a survey program to look for X-ray transients in M31. Nearly every month from 1999 November to 2001 February, Chandra took HRC-I images of five fields covering most of M31. Observations were then made every few months until 2002 June. The details of the 81 Chandra observations are summarized in Table 1 of the reference paper, which is available in a machine-readable form at &lt;a href="http://cdsarc.u-strasbg.fr/ftp/cats/J_ApJ/609/735/"&gt;http://cdsarc.u-strasbg.fr/ftp/cats/J_ApJ/609/735/&lt;/a&gt;. The authors combined all the data into three data sets using the task merge_all. One set contained the data for the northern half of the galaxy, another contained the southern half, and the last contained the center. The authors searched for sources in the three data sets using the CIAO task wavdetect. They ran this task searching for sources on four size scales: 1, 2, 4, and 8 pixels. The pixels in the merged images were 1 arcsecond in the central 18 arcmin by 18 arcmin and 2 arcsec outside of this region. By searching on several scales, wavdetect is able to overcome the large changes in the size of the Chandra PSF from about 0.5 arcsec near the center of the field to over 10 arcsec in the outer regions of the field. A total of 166 sources were detected above their 3.5-sigma detection threshold. This table was created by the HEASARC in September 2015 based on the &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/609"&gt;CDS Catalog J/ApJ/609&lt;/a&gt;, 735 file table2.dat . This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSINAC 4 ESC1-MTP013 RDR-STRLIGHT V1.0

This CODMAC level 4 data set contains solar stray light corrected, radiometric calibrated and geometric distortion corrected (resampled) image data in W/m^2/sr/nm, acquired by the OSIRIS Narrow Angle Camera on the Rosetta spacecraft during the COMET ESCORT 1 mission phase, covering the period from 2015-02-10T23:25:00.000 to 2015-03-10T23:24:59.000. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V1.0 is the first version of this dataset: Lien corrected dataset after October 2018 PSA/PDS external peer review.

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Organization: National Aeronautics and Space Administration
Hipparcos Main Catalog

The Hipparcos and Tycho Catalogues are the primary products of the European Space Agency&#39;s astrometric mission, Hipparcos. The satellite, which operated for four years, returned high quality scientific data from November 1989 to March 1993. Each of the catalogues contains a large quantity of very high quality astrometric and photometric data. In addition there are associated annexes featuring variability and double/multiple star data, and solar system astrometric and photometric measurements. In the case of the Hipparcos Catalogue, the principal parts are provided in both printed and machine-readable form (on CDROM). In the case of the Tycho Catalogue, results are provided in machine-readable form only (on CDROM). Although in general only the final reduced and calibrated astrometric and photometric data are provided, some auxiliary files containing results from intermediate stages of the data processing, of relevance for the more-specialised user, have also been retained for publication. (Some, but not all, data files are available from the Centre de Donnees astronomiques de Strasbourg.) The global data analysis tasks, proceeding from nearly 1000 Gbit of raw satellite data to the final catalogues, was a lengthy and complex process, and was undertaken by the NDAC and FAST Consortia, together responsible for the production of the Hipparcos Catalogue, and the Tycho Consortium, responsible for the production of the Tycho Catalogue. A fourth scientific consortium, the INCA Consortium, was responsible for the construction of the Hipparcos observing programme, compiling the best-available data for the selected stars before launch into the Hipparcos Input Catalogue. The production of the Hipparcos and Tycho Catalogues marks the formal end of the involvement in the mission by the European Space Agency and the four scientific consortia. For much more information about this catalog, such as fuller descriptions of the parameters, the user is urged to check the Hipparcos and Tycho Catalogs website at &lt;a href="https://www.cosmos.esa.int/web/hipparcos/catalogues"&gt;https://www.cosmos.esa.int/web/hipparcos/catalogues&lt;/a&gt;. This database table was created by the HEASARC in April 2000 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/239"&gt;CDS Catalog I/239&lt;/a&gt; file hip_main.dat.gz, the Hipparcos Main Catalog. It was updated in October 2002 to fix some entries which were missing coordinates. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Herbig&BellCatalogofOrionPop.Emission-LineStars

This database table contains the Third Catalog of Emission-Line Stars of the Orion Population (Herbig and Bell (1988)) which lists 735 pre-main sequence stars, members of the Orion Population, that have been observed with slit spectrographs or at equivalent resolution. It is intended to replace the Second Catalog of Herbig and Rao (1972). It gives accurate coordinates (many determined especially for this Catalog); light ranges for known variables; UBVRI data near maximum light; references to ultraviolet, X-ray, and radio observations, and to light curves; value of v sin i and the radial velocity when known; spectral type; equivalent width of the H-alpha emission line; references to spectral reproductions or scans and spectroscopic studies and to identification charts; and a classification (as a T Tau star, FU Ori object, etc.). This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
M 31 Bulge Chandra X-Ray Point Source Catalog

The authors explore the population of X-ray point sources in the bulge of M 31 so as to contrast properties of various subpopulations, such as persistent and transient sources and primordial LMXBs and dynamically formed ones. Based on the data from 26 archival Chandra ACIS observations with aim-points within 10 arcminutes of the center of M 31 (J2000 coordinates of 00:42:44.31, +41:16:09.4), the authors study the source content and properties of various subpopulations of X-ray sources to a maximum distance of 12 arcminutes from the center of M 31. To a limiting luminosity of ~10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the authors find 263 X-ray point sources, with ~1/3 of these being background galaxies. A study of the spatial distribution and the luminosity function of the X-ray sources shows that the distribution of primordial LMXBs is consistent with the distribution of the K-band light and that their luminosity function flattens below ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the dN/dL ~ L&lt;sup&gt;-1&lt;/sup&gt; law in agreement with the behavior found earlier for LMXBs in the Milky Way and in Cen A. Within a radius of 12 arcminutes, the luminosity function is independent of distance to the center of M 31, in contrast to earlier Chandra studies. The LMXBs located in globular clusters and within ~1 arcminute from the center of M 31 are presumably created via dynamical interactions. The dynamical origin of the r &lt; 1 arcminute sources is strongly suggested by their radial distribution which follows the rho&lt;sub&gt;*&lt;/sub&gt;&lt;sup&gt;2&lt;/sup&gt; profile rather than the K-band light distribution. Their luminosity function shows a prominent fall-off below log(L&lt;sub&gt;X&lt;/sub&gt;) &lt;~ 36.5. Although the statistics are insufficient to claim a genuine low-luminosity cut-off in the luminosity function, the best fit power-law with a slope of -0.6 +/- 0.2 is significantly flatter than the dN/dL ~ L&lt;sup&gt;-1&lt;/sup&gt; law. The authors also searched for transients and found 28 sources that varied by a factor larger than 20. Their spatial distribution follows the distribution of the persistent LMXBs within the accuracy allowed by the limited number of transients. This HEASARC table was created in March 2010 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/468/49"&gt;CDS catalog J/A+A/468/49&lt;/a&gt; file table2.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RPCMAG 2 ESC4 RAW V9.0

This dataset contains EDITED RAW DATA (CODMAC LEVEL 2) of theCOMET ESCORT 4 Phase from October 21, 2015 until January 12, 2016of the ROSETTA orbiter magnetometer RPCMAG. Observations are done inthe vicinity of comet 67P/CHURYUMOV-GERASIMENKO 1 (1969 R1).The current version of the dataset is V9.0.The difference to the datasets of earlier versions is mainly a significantlyimproved sensor temperature model, more detailed documentation about magneticdisturbance sources, more data handling information for the user andalso an improved quality flagging system.This applies mainly to CALIBRATED and RESAMPLED datasets. The RAW dataset,however, has been updated as well in order provide all datasets at thesame stage, although RAW data proper did not change.

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Organization: National Aeronautics and Space Administration
MARS EXPRESS SUN MRS 1/2/3 EXTENDED MISSION 5 3728 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2015-01-01 to 2016-12-31. It is a Solar Conjunction measurement and covers the time 2015-04-27T04:24:45.000 to 2015-04-27T09:26:52.500.

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Organization: National Aeronautics and Space Administration
LOFAR Bootes Field 62-MHz Source Catalog

This table contains the source list from Low Frequency Array (LOFAR) Low Band observations of the Bootes field at 62 MHz. The images of this field and the 3C 295 field made at 62 MHz reach a noise level of 5 mJy beam&lt;sup&gt;-1&lt;/sup&gt;, making them the deepest images ever obtained at this frequency. In total, the authors detect 329 sources in the Bootes 62-MHz field image, covering an area of 19.4 square degrees out to a primary-beam attenuation factor of 0.4. From the observations, the authors derive Euclidean-normalized differential source counts. The 62-MHz source counts agree with previous GMRT 153 MHz and Very Large Array 74 MHz differential source counts, scaling with a spectral index of -0.7. The authors find that a spectral index scaling of -0.5 is required to match up the LOFAR 34 MHz source counts. This result is also in agreement with source counts from the 38 MHz 8C survey, indicating that the average spectral index of radio sources flattens toward lower frequencies. The authors also find evidence for spectral flattening using the individual flux measurements of sources between 34 and 1400 MHz and by calculating the spectral index averaged over the source population. To select ultra-steep spectrum (alpha &lt; -1.1) radio sources that could be associated with massive high-redshift radio galaxies, the authors compute spectral indices between 62 MHz, 153 MHz, and 1.4 GHz for sources in the Bootes field. They cross-correlate these radio sources with optical and infrared catalogs and fit the spectral energy distribution to obtain photometric redshifts. They find that most of these ultra-steep spectrum sources are located in the 0.7 &lt;~ z &lt;~ 2.5 range. The Bootes and 3C 295 fields were simultaneously observed on 2012 April 12 as part of a multi-beam observation with the LOFAR LBA stations. The idea behind the multi-beam setup was to use the 3C 295 observations as a calibrator field to transfer the gain amplitudes to the (target) Bootes field (pointing center of J2000.0 RA and Dec of 14&lt;sup&gt;h&lt;/sup&gt; 32&lt;sup&gt;m&lt;/sup&gt; 03.0&lt;sup&gt;s&lt;/sup&gt;, +34&lt;sup&gt;o&lt;/sup&gt; 16&#39; 33&quot;). The total integration time on both fields was 10.25 hr. The observing band for the Bootes field observations was centered at 62 MHz, with a bandwidth of 16 MHz. The synthesized beam for this observation had dimensions of 31 arcseconds x 19 arcseconds. An overview of the observations is given in Table 1 of the reference paper, and an overview of the image characteristics in Table 2 of the reference paper. This table was created by the HEASARC in January 2015 based on some of the contents of the machine-readable version of Table 3 from the reference paper, namely the 329 entries listing sources in the Bootes field detected at 62 MHz. The remaining entries in this table listing the sources detected in the 3C295 field at frequencies of 34, 46 and 62 MHz are available as the HEASARC tables LOF3C29534, LOF3C29546 and LOF3C29562, respectively. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
AIDJEX Beaufort Sea Upward Looking Sonar April 1976, Version 1

This data contains Upward Looking Sonar (ULS) profiles of the underside of the Arctic pack ice along three transects whose total length is 777 nautical miles. The data were obtained by the USS Gurnard (SSN-662), a U.S. Navy submarine, on a traverse of the AIDJEX Main Experiment area in the Beaufort Sea from 07 April 1976 to 10 April 1976. The sea ice thickness derived from the ULS is given in feet. The data are in a single ASCII text file: Aidjex_04_1976_uls.txt. The data in this text file are not formatted into columns; all data are presented in one long row separated by spaces. Little is known about the format of the file, so caution should be used when working with the data. NSIDC is providing this data as part of our effort to preserve historical data. The data file begins with nine values that appear to be header information. These nine values include latitude and longitude values along with other unknown values. After the header, there are approximately 2100 measurements of what NSIDC believes is sea ice thickness in feet, however it is unclear how often these measurements were taken. After these 2100 values, another header of nine values occurs followed again by 2100 measurements. The file continues in this pattern through the remainder of the file. Users with information about the contents of the file are encouraged to contact <a href="mailto:nsidc.org">NSIDC User Services</a>. Two supporting documents that provide some background have been scanned and included as PDF files. These are AIDJEX_ULS_background.pdf and AIDJEX_ULS_format.pdf. These data are available via FTP. <strong>Note:</strong> These data are in a raw format with unknown fields and are being provided as is for preservation purposes. A processed version of the data are available in the <a href="/data/g01360.html">Submarine Upward Looking Sonar Ice Draft Profile Data and Statistics</a> data set.

Tags: earth-science-sea-ice-cryosphere-pack-ice-pack-ice, earth-science-sea-ice-oceans-pack-ice-pack-ice
Organization: National Aeronautics and Space Administration
SAGE-SMC MIPS 160 micron Combined Epoch Full List

The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. \n\nTo be included in each single epoch catalog, each 24 um source has to meet a number of criteria. The source had to be nearly point like with a correlation value >0.89. This removed approximately 2/3 of the entries in the single epoch source lists. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. This requirement removed a small number of sources (70). Finally, all sources had to have signal-to-noise (S/N) values >5. The S/N used was that estimated from the StarFinder code using the mosaic uncertainty image added in quadrature with an 0.6% error due to the background subtraction. This removed 700 sources. The final Epoch 1 catalog likely has a few remaining unreliable sources, estimated to be at less than the 1% level. The Full List contains ALL sources extracted from the MIPS 24 um mosaics, thus a user should be aware that it contains spurious sources. For more details, see Section 4.1 of the SAGE-SMC Data Delivery Document.

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Organization: National Aeronautics and Space Administration
AMSR-E/Aqua level 3 global monthly Surface Soil Moisture Standard Deviation V005 (AMSRE_STDMO) at GES DISC

The dataset contains global monthly soil moisture statistics (standard deviation ) for 1 by 1 degree grid cells. The source for the data is AMSR-E daily estimates of soil moisture (AE_Land3.002: AMSR-E/Aqua Daily L3 Surface Soil Moisture, Interpretive Parameters, QC EASE-Grids. Version 2 ). The dataset covers the time period from 2002-10-01 to 2011-09-30.

Tags: earth-science-soils-land-surface-soil-moisture-water-content
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER PRELANDING OSINAC 2 EDR MTP003 V2.0

This data set contains images acquired by the OSIRIS Narrow Angle Camera during the PRELANDING phase of the Rosetta mission at the comet 67P, covering the period from 2014-05-07T12:48:00.000 to 2014-06-04T10:49:59.000. This version V2.0 supersedes previous deliveries of the same dataset.

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Organization: National Aeronautics and Space Administration
NGC 253 XMM-Newton X-Ray Point Source Catalog

This table contains the NGC 253 XMM-Newton X-Ray Point Source Catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma). This table was created by the HEASARC in April 2009 based on the electronic version of Tables A1 and A2 from the paper which were obtained from the CDS (their catalog J/MNRAS/388/849 files tablea1.dat and tablea2.dat). This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 PRELANDING 0221 V1.0

This is a Rosetta Radio Science data set, collected during the PRELANDING phase 2014-01-21 to 2014-11-18. It is a Global Gravity measurement at the comet 67P and covers the time 2014-08-19T07:11:45.000 to 2014-08-19T13:09:58.000.

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Organization: National Aeronautics and Space Administration