The FUSE Archival Data Handbook - MAST - STScI

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Figure 4.7: Examples of coadded detector spectra for two channels of observation C1600101. These plots are for both segments of the SiC1 (left) and LiF1 (right) channels. Note the difference in flux level over the wavelength range common to both channels. Such discrepancies usually indicate that the target was either partly or completely out of the aperture of one channel during part of the observation. Preview Spectra (*spec*.gif) These spectral plots are generated from the ALL files for the channels exhibiting the highest S/N in the 900–1000, 1000–1100 and 1100–1200 ˚A regions and thus offer a quick look at the entire FUSE wavelength range for a given observation. These are the preview files presented by MAST when FUSE data are queried. Figure 4.8 displays the preview file D064030100000specttagf.gif for observation D0640301. 38
Figure 4.8: Example of a combined, observation-level preview file for observation D0640301. The image presents spectra from three segments that span the FUSE wavelength range. It also contains the number of exposures that were combined and the total observation time of the combined exposures. Note that the total exposure time as well as the number of exposures can be different for each segment since CalFUSE processing may eliminate portions of the data affected by various effects or anomalies (see Chapter 7). Summed Exposures (*nvo*.fit) One National Virtual Observatory (NVO) file is generated for each observation. This file contains one single spectrum spanning the entire FUSE wavelength range (905 ≤ λ ≤ 1187˚A). The spectrum is assembled by cutting and pasting segments from the ALL file using the channel with the highest signal-to-noise (S/N) ratio at each wavelength. Segments are shifted to match the guide channel (either LiF1 or LiF2) between 1045 and 1070˚A. Warning: While these NVO spectra form a convenient overview of each data set, their direct use for scientific analysis is not encouraged without detailed checking. Because of possible channel drifts, the target may have been outside of one or more apertures for some fraction of the observation. Not only might the resulting spectrum be non-photometric, but the photometric error may be wavelength-dependent, because of the way that the NVO files 39
Page 1 and 2: The FUSE Archival Data Handbook Jun
Page 3 and 4: 5 Ancillary Files 42 5.1 FES Image
Page 5 and 6: List of Tables 1.1 FUSE Data Inform
Page 7 and 8: List of Figures 2.1 Optical layout
Page 9 and 10: Chapter 1 Introduction The Far Ultr
Page 11 and 12: Chapter 2 The Instrument 2.1 Introd
Page 13 and 14: Y Coordinate (arcsec) -150 -100 -50
Page 15 and 16: 2.2.3 Detectors Table 2.2: Waveleng
Page 17 and 18: apertures simultaneously for best r
Page 19 and 20: sent to the spacecraft Attitude Con
Page 21 and 22: NOTES to table: (1) Data taken prio
Page 23 and 24: 3.3 Overview of CalFUSE The CalFUSE
Page 25 and 26: Figure 4.1: A geometrically correct
Page 27 and 28: 19 Table 4.1: FUSE Data File Types
Page 29 and 30: Table 4.2: Science Programs Code Ca
Page 31 and 32: also be placed at the reference poi
Page 33 and 34: 4.2.1.2 Extracted Spectral Files (*
Page 35 and 36: Table 4.9: Format of Intermediate D
Page 37 and 38: Table 4.10: IDF Channel Array Apert
Page 39 and 40: *ext.gif: These files show a calibr
Page 41 and 42: 4.2.1.5 Trailer Files (*.trl) The t
Page 43 and 44: Note that verbose level N includes
Page 45: 4.2.2.2 Preview Files (*00000*.gif,
Page 49 and 50: Table 4.15: Format of NVO Spectral
Page 51 and 52: images have observation IDs and exp
Page 53 and 54: Earth’s magnetic field, which was
Page 55 and 56: engineering data used by CalFUSE to
Page 57 and 58: 5.5 Mission Planning Schedule (MPS)
Page 59 and 60: 1 - FUV (Far UltraViolet) Peak-up 2
Page 61 and 62: the positions of the apertures. The
Page 63 and 64: The example in Fig. 5.7 shows the s
Page 65 and 66: 7-Nov-2008 14:42 Seconds since Thur
Page 67 and 68: Chapter 6 FITS File Headers 6.1 Sci
Page 69 and 70: SUMMARY EXPOSURE INFORMATION DATEOB
Page 71 and 72: DET2HVBL= 101 / Det2 MCP B HV bias
Page 73 and 74: CHID_CAL= ’chid1b014.fit ’ / Wi
Page 75 and 76: BKG_MAX3= 0 / [pixels] bkgd sample
Page 77 and 78: ASSOCIATION KEYWORDS ASN_ID = ’A1
Page 79 and 80: NOGDEINF is the fraction of EXP DUR
Page 81 and 82: Figure 7.1: The difference in the d
Page 83 and 84: 7.2 Additional Contributions to the
Page 85 and 86: Table 7.3: Ratio of Grating-Scatter
Page 87 and 88: 7.3.2 Grid Wires and the Worm Two g
Page 89 and 90: 7.3.4 Gain Sag and Detector Walk Th
Page 91 and 92: Figure 7.7: The effect of gain sag
Page 93 and 94: 7.4 Instrumental Effects 7.4.1 Spec
Page 95 and 96: Table 7.5: FUSE Calibration Star Pa
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Figure 7.11: Same as Figure 7.10 ab
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Figure 7.13: A zoomed-view of the s
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Figure 7.16: A zoomed view of a sma
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Because the worm in LiF1B LWRS is b
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Figure 7.21: Same as Fig. 7.19 abov
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Figure 7.24: Same as Figure 7.10 ab
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Figure 7.26: Residual wavelength er
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(for possible solutions see Dixon e
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8.2.1 IDL Analysis Packages Conside
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[H2ools] is a package of IDL routin
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of synthetic interstellar spectra.
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Chapter 9 Special Cases and Frequen
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TTAG exposures of moderately-bright
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Bibliography Abgrall, H., Roueff, E
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Shchigolev, B.M. 1965, Mathematical
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Name Definition SiC1A The A segment
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The photon events with pulse height
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Appendix C Trailer File Warning Mes
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LIF CNT RATE out of bounds. Setting
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Table D.1: Formats of Housekeeping
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Appendix E Format of Engineering Sn
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Table E.3: Table E.1 (continued) a
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Figure F.1: Residual wavelength err
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Page 145 and 146:
Page 147 and 148:
Page 149 and 150:
Page 151:
Figure F.11: Residual wavelength er
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