이천에서 관측한 지구자기장 관측 및 계산된 자료 입니다. 해당 데이터가 보유한 컬럼은 다음과 같습니다. 컬럼명 : 관측일시, X성분 지구자기장(관측값), Y성분 지구자기장(관측값), Z성분 지구자기장(관측값), 지구자기장 크기(관측값)

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. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.

The Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSEI), using the Spitzer Space Telescope Infrared Array Camera (IRAC) surveyed approximately 220 square degrees of the Galactic plane, covering a latitude range of ±1◦, and a longitude range of |l| =10◦−65◦, plus the Observation Strategy Validation (OSV) region at l=284◦. The observations consisted of two 1.2 second integrations at each position, for a total of over 77,000 pointings and ∼310,000 IRAC frames in 400 hours total survey time. The survey consists of a point source Catalog, a point source Archive, and mosaicked images.The GLIMPSEI Archive (GLMIA 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 GLIMPSEI 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.

WARNING: On 2021/09/23 the EOS Aqua executed a Deep Space Maneuver (DSM). In the DSM, the spacecraft is turned such that the normal Earth field of regard is deep space.The thermal impact of the DSM caused a shift of the centroids of spectral response functions (SRF) of about 1% of the width of the SRF, equivalent to a frequency shift of 9 parts per million. This shift is reflected in the “spectral_freq” parameter (observed frequencies) in the L1b v5 files for each 6 minute granule. The magnitude of the effect on brightness temperatures (BT) depends on the spectral gradient of each channel. Maximum BT shifts are approximately +- 0.5 K, although many channels experience far smaller BT shifts. Approximately 1803 channels have BT shifts of less than 0.1 K and 575 channels are now shifted in BT by more than 0.1 K, while 231 of these channels have BT shifts greater than 0.2 K.Users of the L1b v5 product who are concerned that these shifts may impact their science investigations and applications are encouraged to switch to the AIRS L1c v6.7.4 product, which, among many other improvements, converts the spectra to a fixed frequency grid. END OF WARNING.The Atmospheric Infrared Sounder (AIRS) is a grating spectrometer (R = 1200) aboard the second Earth Observing System (EOS) polar-orbiting platform, EOS Aqua. In combination with the Advanced Microwave Sounding Unit (AMSU) and the Humidity Sounder for Brazil (HSB), AIRS constitutes an innovative atmospheric sounding group of visible, infrared, and microwave sensors. The AIRS Infrared (IR) level 1B data set contains AIRS calibrated and geolocated radiances in milliWatts/m^2/cm^-1/steradian for 2378 infrared channels in the 3.74 to 15.4 micron region of t he spectrum. The AIRS instrument is co-aligned with AMSU-A so that successive blocks of 3 x 3 AIRS footprints are contained within one AMSU-A footprint. The AIRIBRAD_005 products are stored in files (often referred to as "granules") that contain 6 minutes of data, 90 footprints across track by 135 lines along track.

'Spaceborne Imaging Radar-C (SIR-C) was part of an imaging radar system that was flown on board two Space Shuttle flights (9 - 20 April, 1994 and 30 September - 11 October, 1994). The U.S. Geological Survey (USGS) Earth Resources Observation and Science (EROS) Center distributes the C-band (5.8 cm) and L-band (23.5 cm) Survey Data. A total of about 50 hours of data, corresponding to roughly 50 million square kilometers of ground coverage, were collected during each mission. The ground swath width varies from 15 to 90 kilometers depending on the imaging mode and incidence angles of the radar beams. All science data were processed into Survey products. The Survey product is intended as a \"quick look\" browsing tool for viewing the areas imaged by SIR-C. This product is not designed to be used for quantitative scientific analysis. Survey Data consists of a frame image of a data segment, which represents a subset of the data swath. Resolution is approximately 100 meters, processed to a 50-meter pixel spacing. Additional information on SIR-C is available at: http://southport.jpl.nasa.gov.'

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. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.

Since May 1981, the National Aeronautics and Space Administration (NASA) has used aircraft to collect cosmic dust (CD) particles from Earth's stratosphere. Specially designed dust collectors are prepared for flight and processed after flight in an ultraclean (Class-100) laboratory constructed for this purpose at the Lyndon B. Johnson Space Center (JSC) in Houston, Texas. Particles are individually retrieved from the collectors, examined and cataloged, and then made available to the scientific community for research. Cosmic dust thereby joins lunar samples and meteorites as an additional source of extraterrestrial materials for scientific study.

Since May 1981, the National Aeronautics and Space Administration (NASA) has used aircraft to collect cosmic dust (CD) particles from Earth's stratosphere. Specially designed dust collectors are prepared for flight and processed after flight in an ultraclean (Class-100) laboratory constructed for this purpose at the Lyndon B. Johnson Space Center (JSC) in Houston, Texas. Particles are individually retrieved from the collectors, examined and cataloged, and then made available to the scientific community for research. Cosmic dust thereby joins lunar samples and meteorites as an additional source of extraterrestrial materials for scientific study.

Since May 1981, the National Aeronautics and Space Administration (NASA) has used aircraft to collect cosmic dust (CD) particles from Earth's stratosphere. Specially designed dust collectors are prepared for flight and processed after flight in an ultraclean (Class-100) laboratory constructed for this purpose at the Lyndon B. Johnson Space Center (JSC) in Houston, Texas. Particles are individually retrieved from the collectors, examined and cataloged, and then made available to the scientific community for research. Cosmic dust thereby joins lunar samples and meteorites as an additional source of extraterrestrial materials for scientific study.