J.D. Of course, the Sloan (SDSS) scale is different. The images below show ds9 snapshots of some of the main pipeline image products. sampled with 1.5′′ ×1.5′′ pixels. 1%), GALEX counts may be used in Poisson statistics to compute S/N for COMMENT AMBG -1: unfilled, cleared, unchecked. / Minimum S/N for NUV merges. N_ZPMAG =     20.0823753525469 / NUV Zero Point Magnitude, F_ZPMAG =     18.8170737879193 / FUV Zero Point Magnitude, N_ZPSCAL=                   1. GALEX Allsky Imaging Survey (AIS) colored; DSS2 Red (F+R) DSS2 Blue (XJ+S) SDSS9 colored; Mellinger colored; 2MASS colored; AllWISE color; IRIS colored; GLIMPSE360; IRAC color I1,I2,I4 - (GLIMPSE, SAGE, SAGE-SMC, SINGS) AKARI Color (WideL-WideS-N60) Halpha; hscMap About hscMap Normally masked out in pipeline, new hotspots not in database will appear as spiral echoing dither pattern (since hot spots are fixed in detector coordinates). The GALEX satellite captured a spectacular image of the star Mira shedding a tail of gas and dust nearly 13 light years long. / MAGNITUDE GAMMA, NSXBKGSX=                  128 / BACKGROUND MESH WIDTH (PIXELS), NSXBKGSY=                  128 / BACKGROUND MESH HEIGHT (PIXELS), NSXBKGFX=                    5 / BACKGROUND FILTER WIDTH, NSXBKGFY=                    5 / BACKGROUND FILTER HEIGHT, NSXPBKGT= 'GLOBAL  '           / PHOTOM BACKGROUND TYPE, NSXPBKGS=                   24 / LOCAL AREA THICKNESS (PIXELS), NSXPIXSK=                50000 / PIXEL STACKSIZE (PIXELS), NSXFBUFS=                 1024 / FRAME-BUFFER SIZE (LINES), NSXISAPR=                   0. The current estimates are that the zero-points defined The "int" image has 1.5-arcsec pixels. The GALEX optics and detector produce several image artifacts which the pipeline flags to indicate regions where analysis problems may arise. Morrissey The grism data are from a single visit (and grism rotation). If the scale is not fractional (e. g. 1.5), but integer (e. g. 2 or 3), the blur can be avoided just by displaying each logical pixel as a square group of an integer (e. g. 2×2 or 3×3) number of physical pixels of the same color — i. e. just by duplicating the corresponding pixel of the original image … F_AMBG6 =                    0 / Number of FUV 6 ambig. FUV images are on the left, NUV on the right. COMMENT AMBG  3: unfilled, first choice taken, no second choice candidate. For example, the closer a moon is to its planet, the stronger the planet will tug on it. proper quantity to use in determining a GALEX magnitude (i.e. / MEDIAN BACKGROUND (ADU), FSXBKDEV=      4.721388791E-08 / MEDIAN RMS (ADU), FSXBKTHD=        0.02816901356 / EXTRACTION THRESHOLD (ADU), FSXCONFF= 'default.sex'        / CONFIGURATION FILENAME, FSXDETT = 'CCD     '           / DETECTION TYPE, FSXTHLDT= 'SIGMA   '           / THRESHOLD TYPE, FSXTHLD =                   1. • It was launched in April 2003 by Caltech&NASA and is just about finished collecting data now. Unfortunately, MAST does not direct offer services to corotate and align images. Using data from NASA's Galaxy Evolution Explorer, or GALEX, astronomers were able to show that a fraction of the Type Ia explosion sites they looked at are associated with hot young stars. Note that one GALEX count corresponds to one detected "average" photon for These include. FUV: delta_mAB = -2.5 x (log10(CPS) - GALEX Composite NUV/FUV Image of M81 (bottom) and M82 (top). Typical GALEX background in the FUV is 2000 cps for the whole field, which corresponds to 3 x 10-4 cps/pixel (where a pipeline pixel is 1.5 arcsec). Using the expected comet center, line wavelength, and the GALEX dispersion relation, we nd the point about which a 2D version of this prole will be centered. The image quantities are in units of counts per pixel. COMMENT AMBG  6: unfilled, first and second taken, no third choice. F_AMBG4 =                    0 / Number of FUV 4 ambig. This file contains the combined or summed image strips for multiple exposures for each spectral-extracted source. detector background would be 10-3 cps/pixel, or 0.01 cps/source This tools helps you scale pixel art to bigger sizes without filtering for game development, social media or personal uses. The high resolution relative response map shows the effective normalized instrument response (based on flat field) * exposure (seconds) projected onto the sky. Includes extractions from pipeline-generated maps at the position of the detected source. is illustrated by Figure 1, which shows a GALEX image in de-tector and sk y coordinate s, which are repres entative of the pr e- and. For unsaturated bright stars the GALEX photometric precision is "walk" corrections have been applied to these images, which move counts Due to diffraction, and electron halo due to proximity focused photocathode. eclipse (i.e., little donuts of dithered source images). gPhoton is a new database product and software package that enables analysis of GALEX ultraviolet data at the photon level. Point sources in these images are “detector hot spots” which are masked in further processing. take the Bright star NUV beveled edge reflections (NUV only). These are used for calibration of electronic drift and dead time corrections only and do not show up in the final images. COMMENT AMBG -2: not applicable, does not exist, blank. / MAGNITUDE ZERO-POINT, FSXMGGAM=                   4. background, so take the FUV detector background to be ~10-4 N_AMBG3 =                    0 / Number of NUV 3 ambig. Pixel Scale. Abstract. / THRESHOLD, FSXMINAR=                   10 / EXTRACTION MINIMUM AREA (PIXELS), FSXCONV =                    T / CONVOLUTION FLAG, FSXCONVN=                    T / CONVOLUTION NORM. N_AMBGM1=                    0 / Number of NUV -1 ambig. on the 620-pound (281-kg) spacecraft. Return. The combination of time-tagged photon positions and satellite aspect satellite are used to generate a count map in sky coordinates. History. / GAIN (IN E- PER ADU), NSXBKGND=                   0. This file contains parameter information, as well as a source list table including extraction, for each source. Note that the NUV image frame is rotated 180 degrees from the FUV frame. The small donuts result from regions of the detector active area (hot spots) which have been masked in pipeline processing. N_AMBGM6=                    0 / Number of NUV -6 ambig. These images have been obtained from the pipeline a single visit to the target M51 (NGA_M51_0001). RPOSERR =     1.84049156740606 / Radial position error. with point spacing that matches the GALEX pixel size (1.005). At the position of the arrow (highlighted in the magnifier), we detected ~ 0.082 counts/(s normalized EA pixel) in the NUV image. / NUV Zero Point Scale Factor, F_ZPSCAL=                   1. COMMENT AMBG -6: unfilled, first and second taken, third choice exists. / CLEANING PARAMETER, NSXCLNST=                   32 / CLEANING OBJECT-STACK, NSXAPERD=                    0 / APERTURE DIAMETER (PIXELS), NSXAPEK1=                  2.5 / KRON PARAMETER, NSXAPEK2=                  2.5 / KRON ANALYSIS RADIUS, NSXAPEK3=                  3.5 / KRON MINIMUM RADIUS, NSXSATLV=           999999999. Columns 8 and 9 are the Galactic coordinates … NUVS2N  =                   2. The The small ghost to the upper right is due to the dichroic beam splitter. Note that at the position of the arrow, 50 counts were detected in this exposure. Combining deep SCUBA-2 observations with archival GALEX, SDSS, WISE, Spitzer, and submillimetre Herschel data, we are able to model the entire SED from UV to sub-mm wavelengths. This observation was acquired at a roll angle of 90 degrees (measured with respect to the Y axis of the detector/instrument frame), which explains why the image is rotated with respect to the dose maps above. The header portion defines the image dimensions (PRI_NC. Over most of the active area, the response varies by less than +/- 20%. Sextractor output columns from FUV image extractions, Sextractor output columns from NUV image extractions, /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-cat.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-cat.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-rrhr.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-rrhr.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-cnt.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-cnt.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-skybg.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-skybg.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-flags.fits', /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-flags.fits', Band Merger Parameters and Output Quantities, /00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-xd-mcat.fits', Header card from NUV catalog file ­ Sextractor Output. It's based on XbrWasm, and runs locally in the web browser. Note that in the low response region of the FUV detector, the average level is relatively flat, but the image becomes noisy as expected due to the low throughput in this region. For this purpose, we have taken the relative response of all locations on Contains global object ID, pipeline version, image tile number, observation type, optics wheel position, image product type, pipeline re-run (try) number, band, Includes merged position in Equatorial and Galactic coordinates, extinction, Includes neighbor count and total flux out to three radii (currently set to 5”, 10” and 30”), closest neighbor distance, PA and, Derived quantities and map levels at merged output position. GALEX has also a spectroscopic observing mode, which will not be addressed here. number, the total number of exposures (or orbits) and exposure time accumulated. Neill (Caltech) NASA's Galaxy Evolution Explorer is helping to solve a mystery -- why do the littlest of galaxies produce the biggest of star explosions, or supernovae? (CPS x Exp_time + Each wavelength of light in the image obtained from NASA telescopes in space (infrared, optical, ultraviolet, and X-ray) is assigned to a different frequency range. PROBLIM =                   0. The FUV detector shows much larger response variation across the field, particularly on one side where the response drops off significantly. Morrissey Responsible NASA Official: Susan G. Neff I also do not deal with optics aberrations here. Local flaring of detector count rate caused by South Atlantic Anomaly, solar activity, The largest (red, lower) ghost is due to the 10 mm thick NUV detector window. angle (east of north), SIMPLE  =                    T / file does conform to FITS standard, BITPIX  =                   16 / number of bits per data pixel, NAXIS   =                    0 / number of data axes, EXTEND  =                    T / FITS dataset may contain extensions, COMMENT   FITS (Flexible Image Transport System) format is defined in 'Astronomy, COMMENT   and Astrophysics', volume 376, page 359; bibcode: 2001A&A...376..359H, NUVFILE = '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-cat.fits', FUVFILE = '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-cat.fits', NUVWTFIL= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-rrhr.fits', FUVWTFIL= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-rrhr.fits', NUVCNTFI= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-cnt.fits', FUVCNTFI= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-cnt.fits', NUVSKYFI= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-skybg.fits', FUVSKYFI= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-skybg.fits', NUVFLGFI= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-nd-flags.fits', FUVFLGFI= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-fd-flags.fits'. from the detector. With this tool you can do a pixel scale calculation. The four points at the corners are the images are generated by electronic stimulus pulses in the detector system. Myers. The header portion defines the image dimensions (PRI_NC,PRI _NR). COMMENT AMBG  0: unfilled, no candidates, no ambiguity. Each pixel is 1.5”x1.5”. / FUV Zero Point Scale Factor, CALMAG  = 'AUTO    '           / Calibration magnitude type, R1      =                   5. How do scientists use gravitational pull as a scale? Detector window ghosts are radially offset due to curvature on the window. The most comprehensive image search on the web. Since detector background is very small (less than This tool lets you upscale pixel art using the xbr smooth scaling algorithm. / THRESHOLD, NSXMINAR=                   10 / EXTRACTION MINIMUM AREA (PIXELS), NSXCONV =                    T / CONVOLUTION FLAG, NSXCONVN=                    T / CONVOLUTION NORM. 2007. This is the lowest redshift at which evolution of the cluster galaxy population becomes noticable , yet it is the highest redshift at which HI in emission can be detected. The dose map contains photon positions in the instrument frame. An "int" image, which has had the relative response correction folded Other artifacts are produced by transient effects. Despite its name, MAG_BEST is not necessarily the best choice for most applications since the measurement for all objects are not made in a consistent way. If scale is greater than 1, then the output image is larger than the input image. This means that those areas are young in general, and that the explosions happened when relatively young white dwarf stars exploded. This is the typical total signal, and about 1/2 of it is detector GraphicsGale also has many pixel-art specific features to help you create your work quickly and easily, including palette control, selectively erasing colors, and tools for quickly replacing and trying new colors. NUV: mAB = -2.5 x log10(FluxNUV / 2.06 x 10-16 erg sec-1 cm-2 Å-1) + 20.08. The high resolution relative response map shows the effective normalized instrument response (based on flat field) * exposure (seconds) projected onto the sky. / Neighbor radius limit 2 (arcsec), R3      =                  30. field or target), TYPE    =                    1 / Observation type (0=single,1=multi), OW      =                    1 / Optics wheel (1=drct,2=grsm,3=opaq), PROD    =                    0 / Reduction product number (type), IMG     =                 1537 / Image number (exposure or run), TRY     =                    3 / Reduction try number (low level), HISTORY NUV: HISTORY 03/11/03 00:22 Catalog created, NSXIMASX=                 3840 / IMAGE WIDTH (PIXELS) originally SEXIMASX, NSXIMASY=                 3840 / IMAGE HEIGHT (PIXELS), NSXSTRSY=                 1024 / STRIP HEIGHT (LINES), NSXIMABP=                  -32 / FITS IMAGE BITPIX, NSXPIXS =                  1.5 / PIXEL SCALE (ARCSEC), NSXSFWHM=                  4.5 / SEEING FWHM (ARCSEC), NSXNNWF = 'default.nnw'        / CLASSIFICATION NNW FILENAME, NSXGAIN =                  71. In practice, the GALEX detectors suffer from edge effects and I have restricted my analysis to the central 0 5 (radius) of the image (([x − 24] 2 + [y − 24] 2) < 225). et al. We also show ex-amples of previously undetected fast variations in two dif-ferent types of hot stellar sources. The dose map contains photon positions in the instrument frame. In the NUV, for a 20 mag source (1 cps), the The radius is mapped to notes of a melodic minor scale. Recently-observed features include concentric rings rippling out from the impact area in a series of star formation waves, ending in the outermost ring. COMMENT AMBG  4: filled, second choice matches a first choice candidate. Specific details can be seen in the magnifier image (upper right), which is providing a zoom around the cursor position (indicated by the white arrow in the image). Thus, the background would be ~0.1% of the This file contains the image strips for individual exposures for each spectral-extracted source. The one dimensional spectra are extracted column-by-column by adding up the data in a fixed window of width 15 arcseconds and then subtracting the average of the values in the GALEX Spectroscopy Primer 6 In order to figure out how heavy a planet is, scientists need to know two things: how long it takes nearby objects to orbit the planet and how far away those objects are from the planet. Over most of the active area, the response varies by less than +/- 20%. FUVS2NCU=                   0. The images below show ds9 snapshots of some of the main pipeline image products. In this image, taken in ultraviolet light by the Galaxy Evolution Explorer (GALEX), Jupiter’s Ghost appears far larger than it does in visible light. The scale is given in arcseconds per pixel in both spatial and dispersion. A "cnt" image, in which the stars looks like stars, but which still has FILENAME= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', CONTINUE  '/00-visits/0001-img/03-try/AISCHV2_149_29047_0001_sv12-xd-mcat.fits', DIRECTRY= '/home/ops1/tim/work/ir0.2/ais/pipe/01-vsn/10221-AISCHV2_149_29047/d&', VSN     =                    1 / Reduction version (high level), TILE    =                10221 / Tile number (a.k.a. RAO     =           350.717645 / RA center for this field. Contains the header key word for the total number of sources extracted (ECOUNT). Because of the dither motion by the satellite, stars and galaxies move in this frame during an observation (appearing in this image as donuts or smeared objects). To determine the detector background: corresponds to 3 x 10-4 cps/pixel (where a pipeline pixel is 1.5 Accumulated image strips for photon data and response for any of N-1 sources in the field of view. Because of the dither motion by the satellite, stars and galaxies move in this frame during an observation (appearing in this image as donuts or smeared objects). Facing page: GALEX’s stunning image of N_AMBG1 =                  109 / Number of NUV 1 ambig. the (respective) bandpass. The NUV window has a beveled exterior surface required to mate to the microchannel plate surface. Spectra for each source and its computed 1 sigma error. GALEX counts: The "cnt" image Pixel Art Scaler. At both setups we have camera with 1Mpx resolution The combination of time-tagged photon positions and satellite aspect satellite are used to generate a count map in sky coordinates. Each file consists of a short primary header (giving the number, For source extraction, the GALEX pipeline utilizes the program, f is the flux from the source in counts/sec, s is the sky level in counts/sec/pixel, is the area over which the flux is measured. • It takes huge (80 arcmin) circular fields with 5arcsec resolution and spectra of all objects. FUVS2N  =                   2. Google Images. (0.027 x CPS x Exp_time )2)1/2 / Exp_time)). FUVNUM  =                  207 / Number of FUV sources. cps/pixel for simplicity. Sextractor output columns from NUV image extractions, o       Please consult the sextractor manual and Sextractor for Dummies for definitions of these outputs, Table 3.2  Merged Object Catalog (-mcat.fits), NUV calibrated flux using FUV catalog position, FUV calibrated flux using NUV catalog position, Closest neighbor position angle in degrees, NUV ratio of min to max response near source, FUV ratio of min to max response near source, RMS error for corrected isophotal magnitude, Flux vector within fixed circular aperture(s), Flux within a Kron-like elliptical aperture, Minimum x-coordinate among detected pixels, Minimum y-coordinate among detected pixels, Maximum x-coordinate among detected pixels, Maximum y-coordinate among detected pixels, Cxx object ellipse parameter (WORLD units), Cyy object ellipse parameter (WORLD units), Cxy object ellipse parameter (WORLD units), Profile RMS along major axis (world units), Profile RMS along minor axis (world units), Variance of position along X-WORLD (alpha), Variance of position along Y-WORLD (delta), Cxx error ellipse parameter (WORLD units), Cyy error ellipse parameter (WORLD units), Cxy error ellipse parameter (WORLD units), World RMS position error along major axis, World RMS position error along minor axis, J2000 error ellipse pos. compared to 1 cps of signal. DEC_CENT=            -0.389996 / DEC center for this field. here are accurate to within ± 10% (1 sigma). December 23 - ver.2.08.21 History (See figure 5 As with the Cat's Eye, the sonification begins at the top and moves radially around the image in a clockwise direction. "Wiggle" and has 1.5-arcsec pixels. FLAG, NSXCONVF= 'gauss_3.0_7x7.conv' / CONVOLUTION FILENAME, NSXDBLDN=                   32 / NUMBER OF SUB-THRESHOLDS, NSXDBLDC=                0.005 / CONTRAST PARAMETER, NSXCLN  =                    T / CLEANING FLAG, NSXCLNPA=                   1. GALEX Ultraviolet Image of Cartwheel Galaxy The Cartwheel Galaxy is one of the brightest ultraviolet energy sources in the local Universe. Thephotometricsystemused inthe GALEX archive is based on the AB magnitude scale1 (see Morrissey et al. Each source has its own FITS header unit. If you have your telescope's or lens' focal length and the camera sensor's pixel pitch (size) you can calculate the pixel scale. FUV: Flux [erg sec-1 cm-2 Å-1] = 1.40 x 10-15 x CPS This can easily be converted to a surface brightness using the conversion factors provided in the table above. Curators: Joan E. Hollis and Joel D. Offenberg, Primary Object Catalog - Merged FUV+NUV Catalog (mcat file). In answer to your first question, the GALEX image scale is 1.5 arcseconds/pixel for both the FUV and NUV images. Enter a number in one of the text fields below, and then hit either Tab or / SATURATION LEVEL (ADU), NSXMGZPT=                   0. / MEDIAN BACKGROUND (ADU), NSXBKDEV=       0.006104021799 / MEDIAN RMS (ADU), NSXBKTHD=        0.02816901356 / EXTRACTION THRESHOLD (ADU), NSXCONFF= 'default.sex'        / CONFIGURATION FILENAME, NSXDETT = 'CCD     '           / DETECTION TYPE, NSXTHLDT= 'SIGMA   '           / THRESHOLD TYPE, NSXTHLD =                   1. log10(CPS + FUV: mAB = -2.5 x log10(CPS) + 18.82 2 NewGALEXcatalogsofUVsources The GALEX field of view is ≈1.2 diameter (1.28/1.24 , Primary Object Catalog - Merged FUV+NUV Catalog (. / Neighbor radius limit 1 (arcsec), R2      =                  10. NUV: delta_mAB = -2.5 x (log10(CPS) - for a 5" FWHM, and, in this case, the NUV background is ~1% of the source The units are in counts / pixel s (normalized effective area*bandwidth), which means that while the image is ‘flattened’ to reflect the true instrument response, the units correspond roughly to counts per second per pixel. N_AMBG5 =                    0 / Number of NUV 5 ambig. NUV: mAB = -2.5 x log10(CPS) + 20.08. This source list catalog is created on the first exposure and read in and used for each subsequent exposure. The GALEX pipeline generates a smoothed sky background map which is subtracted from the intensity image prior to the final source extraction processing step. F_AMBG5 =                    0 / Number of FUV 5 ambig. / Maximum separation in arcsec. FLAG, FSXCONVF= 'gauss_3.0_7x7.conv' / CONVOLUTION FILENAME, FSXDBLDN=                   32 / NUMBER OF SUB-THRESHOLDS, FSXDBLDC=                0.005 / CONTRAST PARAMETER, FSXCLN  =                    T / CLEANING FLAG, FSXCLNPA=                   1. Curator: As discussed above, the diffuse file is made up of 2' pixels with each pixel comprising 80 × 80 pixels of the original image files and Columns 6 and 7 give the x and y position of these binned pixels. following images: Typical GALEX background in the FUV is 2000 cps for the whole field, which The largest (red, lower) ghost is due to the 10 mm thick NUV detector window. et al. NUVS2NCU=                   0. To convert from GALEX counts per second (CPS) to flux: widths and length of the spectrum) for each source. To estimate the photometric repeatability vs. magnitudes based on The spectral data product files are stored in binary FITS format, but they are GALEX-specific. Total internal reflection causes light from stars within 5 arcminutes of the edge to reflect into the field of view. The black and white images are GALEX NUV of 800 pixels (20 arcmin) on each side. / GAIN (IN E- PER ADU), FSXBKGND=                   0. : Grism angle used for these extractions, total exposure time, total number of spectrally extracted sources (ECOUNT). / SATURATION LEVEL (ADU), FSXMGZPT=                   0. time-scale investigations have been undertaken on a major scale during the mission operations phase. FUV: mAB = -2.5 x log10(FluxFUV / 1.40 x 10-15 erg sec-1 cm-2 Å-1) + 18.82 F_AMBGM6=                    0 / Number of FUV -6 ambig. NUV detector background is 10 times higher, or / ISO-APER RATIO, NSXNDET =                 1080 / NB OF DETECTIONS, NSXNFIN =                  948 / NB OF FINAL EXTRACTED OBJECTS, NSXNPARA=                   83 / NB OF PARAMETERS PER OBJECT, NDEC_CEN=            -0.389996 / originally DEC_CENT, NEXPSTAR=     1066079748.00512 / originally EXPSTART, NOBS-DAT= '2003-10-13'         / originally OBS-DATE, NOBS-TIM= 'unknown '           / originally OBS-TIME, NOBSDATI= '031013T211548Z'     / originally OBSDATIM, NINTIMAG= '/home/ops1/tim/work/ir0.2/ais/AISCHV2_149_29047_0001/AISCHV2_149_29&', CONTINUE  '047_0001_sv12-nd-int.fits' / orginally INTIMAGE, HISTORY FUV: HISTORY 03/11/03 00:29 Catalog created, FSXIMASX=                 3840 / IMAGE WIDTH (PIXELS) originally SEXIMASX, FSXIMASY=                 3840 / IMAGE HEIGHT (PIXELS), FSXSTRSY=                 1024 / STRIP HEIGHT (LINES), FSXIMABP=                  -32 / FITS IMAGE BITPIX, FSXPIXS =                  1.5 / PIXEL SCALE (ARCSEC), FSXSFWHM=                  4.5 / SEEING FWHM (ARCSEC), FSXNNWF = 'default.nnw'        / CLASSIFICATION NNW FILENAME, FSXGAIN =                  71.
Quest-ce Qu'un Amour Interdit, Meilleur Spa Gonflable 2021, Occasion Neuve Renault, élection Maire Et Adjoints 2020, Fréjus - Carte, Fréquence Téva Astra 2021, Dortmund Vs Barça, Location Appartement T2 Mérignac Capeyron, Superficie Canada Vs Usa,