NSSDCA ID: PSPG-00848
Availability: Archived at NSSDC, accessible from elsewhere
Time span: 2009-06-20 to 2009-10-09
This description was generated automatically using input from the Planetary Data System.
Data Set Overview ================= This data set contains calibrated imagery from mid-infrared camera #1 (MIR1) on the LCROSS spacecraft. MIR1 is a filtered camera sensitive from 6.0 to 10.0 microns. The images in this dataset have targets named Moon, Earth, Centaur, Calibration (i.e., not targeted) and TestImage. Test images include ramps and settling-time images that contain no science content. Each calibrated image file is a 160 x 120, 32-bit PC_REAL greyscale image. The effective field-of-view [FOV] is 16.0 [H] x 11.0 [V] degrees. The time each image was captured is encoded in the image's filename as follows: LCROSS_MIR1_CAL_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= MIR1_RAW (described in MIR1_RAW_DS.CAT) contains the raw versions of the images contained in this dataset of calibrated images. The MIR2_RAW and MIR2_CAL datasets contain images from the other mid-infrared camera. MIR2 had almost exactly the same field of view and was slightly more sensitive due to having no added filter. However, MIR2 experienced a shift of focus during launch and produced out-of-focus images. Parameters ========== Science ------Gain is either High Gain for best sensitivity with low scene temperatures (T < +150 C) or Low Gain for best sensitivity with high scene temperatures (+150 C < T < +500 C). The majority of the mid-infrared images are taken at High Gain. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each mid-infrared image was transmitted digitally from the camera to the spacecraft, split into 20 separate packets, compressed losslessly and downlinked in telemetry. The LCROSS ground system extracted the packets from telemetry, combined them into images, and converted them to PNG format. These files were further processed with the LCROSS Archive program to generate the PDS-format image (.IMG) and ASCII label (.lbl) files, timestamping each pair with the UTC time the data was received by the spacecraft. This data path from camera to PDS is lossless except for missing packets, which occurred occasionally because LCROSS transmitted all science telemetry in realtime. Missing packets resulted either in missing images or in images with horizontal bands of missing data. Each mid-infrared image packet contained 160 x 6 pixel band corresponding to 1/20th of an image. Missing images are not contained in the dataset at all. Missing bands are filled with zeros and their presence in an image is indicated by a value of 'Y' for the MISSING_PACKET_FLAG attribute in each label file. This dataset contains radiometrically calibrated images in which data numbers (DNs) were mapped to scene temperature in degrees Centigrade. The mapping is described in the Instrument Response and Calibration Report in the CALIB directory of this archive. Data ==== These files are stored as 32-bit PC_REAL image files. Each pixel's value is reported in degrees Centigrade. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images utilize the camera's coordinate system. To convert the coordinates to the LCROSS Payload Common Camera Coordinate System, the images must be flipped along the X axis (horizontally flipped). A description of mapping the images with respect to each other and the spacecraft coordinate system is contained within the LCROSS Instrument Response and Calibration Report. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The LCROSS MIR calibration pipeline (contained within the Make Archive program) used to generate the calibrated images is Version 5. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw imagery from mid-infrared camera #1 (MIR1) on the LCROSS spacecraft. MIR1 is a filtered camera sensitive from 6.0 to 10.0 microns. The images in this dataset have targets named Moon, Earth, Centaur, Calibration (i.e., not targeted) and TestImage. Test images include ramps and settling-time images that contain no science content. Each raw image file is a 160 x 120, 16-bit integer greyscale image. Each pixel has 14 bits of dynamic range encoded in the low 14 bits of each 16 bit pixel. The effective field-of-view [FOV] is 16.0 [H] x 11.0 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_MIR1_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= MIR1_CAL (described in MIR1_CAL_DS.CAT) contains the calibrated versions of the images contained in this dataset of raw images. The MIR2_RAW and MIR2_CAL datasets contain images from the other mid-infrared camera. MIR2 had almost exactly the same field of view and was slightly more sensitive due to having no added filter. However, MIR2 experienced a shift of focus during launch and produced out-of-focus images. Parameters ========== Science ------Gain is either High Gain for best sensitivity with low scene temperatures (T < +150 C) or Low Gain for best sensitivity with high scene temperatures (+150 C < T < +500 C). The majority of the mid-infrared images are taken at high gain. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each mid-infrared image was transmitted digitally from the camera to the spacecraft, split into 20 separate packets, compressed losslessly and downlinked in telemetry. The LCROSS ground system extracted the packets from telemetry, combined them into images, and converted them to PNG format. These files were further processed with the LCROSS Archive program to generate the PDS-format image (.IMG) and ASCII label (.lbl) files, timestamping each pair with the UTC time the data was received by the spacecraft. This data path from camera to PDS is lossless except for missing packets, which occurred occasionally because LCROSS transmitted all science telemetry in realtime. Missing packets resulted either in missing images or in images with horizontal bands of missing data. Each mid-infrared image packet contained 160 x 6 pixel band corresponding to 1/20th of an image. Missing images are not contained in the dataset at all. Missing bands are filled with zeros and their presence in an image is indicated by a value of 'Y' for the MISSING_PACKET_FLAG attribute in each label file. Data ==== These files are stored as PDS-formatted, 16 bit MSB_UNSIGNED_INTEGER files. Each pixel contains a 14 bit count in the low bits of a 16 bit unsigned integer. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images have been left in the camera's coordinate system. To convert them to the LCROSS Payload Common Camera Coordinate System, they must be flipped along the X axis (horizontally flipped). A description of mapping the images with respect to each other and the spacecraft coordinate system is contained within the LCROSS Instrument Response and Calibration Report. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated imagery from mid-infrared camera #2 (MIR2) on the LCROSS spacecraft. MIR2 is a camera sensitive from 7.5 to 13.5 microns. These images are out-of-focus due to a shift during launch (described below). The images in this dataset have targets named Moon, Earth, Calibration (i.e., not targeted) and TestImage. Test images include ramps and settling-time images that contain no science content. Each calibrated image file is a 160 x 120, 32-bit PC_REAL greyscale image. The effective field-of-view [FOV] is 16.0 [H] x 11.0 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_MIR2_CAL_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= MIR2_RAW (described in MIR2_RAW_DS.CAT) contains the raw versions of the images contained in this dataset of calibrated images. The MIR1_RAW and MIR1_CAL datasets contain images from the other mid-infrared camera. MIR1 had almost exactly the same field of view and was slightly less sensitive due to having an added filter. However, MIR1 experienced no shift of focus during launch and produced in-focus images. Parameters ========== Science ------Gain is either High Gain for best sensitivity with low scene temperatures (T < +150 C) or Low Gain for best sensitivity with high scene temperatures (+150 C < T < +500 C). The majority of the mid-infrared images are taken at high gain. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each mid-infrared image was transmitted digitally from the camera to the spacecraft, split into 20 separate packets, compressed losslessly and downlinked in telemetry. The LCROSS ground system extracted the packets from telemetry, combined them into images, and converted them to PNG format. These files were further processed with the LCROSS Archive program to generate the PDS-format image (.IMG) and ASCII label (.lbl) files, timestamping each pair with the UTC time the data was received by the spacecraft. This data path from camera to PDS is lossless except for missing packets, which occurred occasionally because LCROSS transmitted all science telemetry in realtime. Missing packets resulted either in missing images or in images with horizontal bands of missing data. Each mid-infrared image packet contained 160 x 6 pixel band corresponding to 1/20th of an image. Missing images are not contained in the dataset at all. Missing bands are filled with zeros and their presence in an image is indicated by a value of 'Y' for the MISSING_PACKET_FLAG attribute in each label file. This dataset contains radiometrically calibrated images in which data numbers (DNs) were mapped to scene temperature in degrees Centigrade. The mapping is described in the Instrument Response and Calibration Report in the CALIB directory of this archive. Data ==== These files are stored as 32-bit PC_REAL image files. Each pixel's value is given in degrees Centigrade. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images have been left in the camera's coordinate system. To convert them to the LCROSS Payload Common Camera Coordinate System, they must be flipped along the X axis (horizontally flipped). A description of mapping the images with respect to each other and the spacecraft coordinate system is contained within the LCROSS Instrument Response and Calibration Report. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The LCROSS MIR calibration pipeline (contained within the Make Archive program) used to generate these calibrated images is Version 5. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw imagery from mid-infrared camera #2 (MIR2) on the LCROSS spacecraft. MIR1 is a filtered camera sensitive from 7.5 to 13.5 microns. These images are out-of-focus due to a shift during launch (described below). The images in this dataset have targets named Moon, Earth, Calibration (i.e., not targeted) and TestImage. Test images include ramps and settling-time images that contain no science content. Each raw image file is a 160 x 120, 16-bit integer greyscale image. Each pixel has 14 bits of dynamic range encoded in the low 14 bits of each 16 bit pixel. The effective field-of-view [FOV] is 16.0 [H] x 11.0 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_MIR2_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= MIR2_CAL (described in MIR2_CAL_DS.CAT) contains the calibrated versions of the images contained in this dataset of raw images. The MIR1_RAW and MIR1_CAL datasets contain images from the other mid-infrared camera. MIR1 had almost exactly the same field of view and was slightly less sensitive due to having an added filter. However, MIR1 experienced no shift of focus during launch and produced in-focus images. Parameters ========== Science ------Gain is either High Gain for best sensitivity with low scene temperatures (T < +150 C) or Low Gain for best sensitivity with high scene temperatures (+150 C < T < +500 C). The majority of the mid-infrared images are taken at high gain. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each mid-infrared image was transmitted digitally from the camera to the spacecraft, split into 20 separate packets, compressed losslessly and downlinked in telemetry. The LCROSS ground system extracted the packets from telemetry, combined them into images, and converted them to PNG format. These files were further processed with the LCROSS Archive program to generate the PDS-format image (.IMG) and ASCII label (.lbl) files, timestamping each pair with the UTC time the data was received by the spacecraft. This data path from camera to PDS is lossless except for missing packets, which occurred occasionally because LCROSS transmitted all science telemetry in realtime. Missing packets resulted either in missing images or in images with horizontal bands of missing data. Each mid-infrared image packet contained 160 x 6 pixel band corresponding to 1/20th of an image. Missing images are not contained in the dataset at all. Missing bands are filled with zeros and their presence in an image is indicated by a value of 'Y' for the MISSING_PACKET_FLAG attribute in each label file. Data ==== These files are stored as PDS-formatted, 16 bit MSB_UNSIGNED_INTEGER files. Each pixel contains a 14 bit count in the low bits of a 16 bit unsigned integer. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images have been left in the camera's coordinate system. To convert them to the LCROSS Payload Common Camera Coordinate System, they must be flipped along the X axis (horizontally flipped). A description of mapping the images with respect to each other and the spacecraft coordinate system is contained within the LCROSS Instrument Response and Calibration Report. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains imagery from the near-infrared camera #1 (NIR1) on the LCROSS spacecraft (S/C). NIR1 is a filtered camera sensitive from 1.4 to 1.7 microns. The images in this dataset have targets named Moon, Earth, Calibration (i.e., not targeted) and TestImage. Test images include ramps and camera initialization images that contain no science content. Each calibrated image file is a 32-bit PC_REAL greyscale image, with a 720 x 486 pixel format. The image aspect ratio [H:V] is 1.33. The effective field-of-view [FOV] is 28.3 [H] x 21.4 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_NIR1_CAL_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= NIR1_RAW (described in NIR1_RAW_DS.CAT) contains the raw versions of the images contained in this dataset of calibrated images. The NIR2_RAW and NIR2_CAL datasets contain images from the other near-infrared camera. NIR2 had almost exactly the same field of view and was slightly more sensitive due to having no added filter. Parameters ========== Science ------After initialization, the near-infrared cameras were operated by setting two independent parameters: 1. LCROSS:NIR_OPR (an integer [0, 15] inclusive) One of 16 operational configurations stored in non-volatile memory. The factory default settings for these configurations were used. This setting determines the camera's integration time (in the labels as LCROSS:NIR_INTEGRATION_TIME in microseconds) and gain setting (LCROSS:NIR_GAIN in electrons per DN). 2. LCROSS:ENHANCEMENT_MODE [OFF,ON] Image stretching. Enabled only during the STARFIELD data collection period. These cameras have additional configuration settings that were redundant or kept constant and so are not noted in the labels. The digital gain setting was always 1. The effect of automatic gain control is to vary the OPR number, which is reported in the labels, so the automatic gain configuration is redundant. In any case, this setting was off except for during the lunar swingby. The Global Offset Value was always 100 except during initialization where it was briefly set to 4095. This parameter isn't noted in the labels, but all images where it was not 100 have a TARGET_NAME of TEST_IMAGE. Test images include ramps, all states high (white image), and all-states-low (flat dark image) and contain no science content. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== The detector produces 320 x 240, 12-bit grayscale images. Each image was converted inside the camera to an analog, NTSC image and transmitted to the spacecraft. The spacecraft multiplexed the two near-infrared cameras with the visible light 'context' camera, receiving images from only one of these three cameras at a time. When received, the spacecraft converted each NTSC image back to a 720 x 486, 24-bit RGB digital image and compressed it using a lossy, proprietary, wavelet-based compression algorithm for downlink. On the ground, the images are decompressed and recompressed losslessly as RGB PNG files by GSEOS (Ground Support Equipment Operating System). The LCROSS Make Archive program read these files, selected the Red channel, and wrote that as a single-channel, PDS-formatted image (.IMG) file and a FITS file. Data ==== These files are stored as 32-bit PC_REAL image files. Each pixel's value is given as radiance units [W/m^2 sr]. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images have been left in the camera's coordinate system. To convert them to the LCROSS Payload Common Camera Coordinate System, these images must be rotated +180 degrees. A description of mapping the images with respect to each other and the S/C coordinate system is contained within the LCROSS Instrument Response and Calibration Report in the CALIB directory of this archive. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains imagery from the near-infrared camera #1 (NIR1) on the LCROSS spacecraft (S/C). NIR1 is a filtered camera sensitive from 1.4 to 1.7 microns. The images in this dataset have targets named Moon, Earth, Calibration (i.e., not targeted) and TestImage. Test images include ramps and camera initialization images that contain no science content. Each raw image file is an 8-bit integer greyscale image, with a 720 x 486 pixel format. The image aspect ratio [H:V] is 1.33. The effective field-of-view [FOV] is 28.3 [H] x 21.4 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_NIR1_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= NIR1_CAL (described in NIR1_CAL_DS.CAT) contains the calibrated versions of the images contained in this dataset of raw images. The NIR2_RAW and NIR2_CAL datasets contain images from the other near-infrared camera. NIR2 had almost exactly the same field of view and was slightly more sensitive due to having no added filter. Parameters ========== Science ------After initialization, the near-infrared cameras were operated by setting two independent parameters: 1. LCROSS:NIR_OPR (an integer [0, 15] inclusive) One of 16 operational configurations stored in non-volatile memory. The factory default settings for these configurations were used. This setting determines the camera's integration time (in the labels as LCROSS:NIR_INTEGRATION_TIME in microseconds) and gain setting (LCROSS:NIR_GAIN in electrons per DN). 2. LCROSS:ENHANCEMENT_MODE [OFF,ON] Image stretching. Enabled only during the STARFIELD data collection period. These cameras have additional configuration settings that were redundant or kept constant and so are not noted in the labels. The digital gain setting was always 1. The effect of automatic gain control is to vary the OPR number, which is reported in the labels, so the automatic gain configuration is redundant. In any case, this setting was off except for during the lunar swingby. The Global Offset Value was always 100 except during initialization where it was briefly set to 4095. This parameter isn't noted in the labels, but all images where it was not 100 have a TARGET_NAME of TEST_IMAGE. Test images include ramps, all states high (white image), and all-states-low (flat dark image) and contain no science content. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== The detector produces 320 x 240, 12-bit grayscale images. Each image was converted inside the camera to an analog, NTSC image and transmitted to the spacecraft. The spacecraft multiplexed the two near-infrared cameras with the visible light 'context' camera, receiving images from only one of these three cameras at a time. When received, the spacecraft converted each NTSC image back to a 720 x 486, 24-bit RGB digital image and compressed it using a lossy, proprietary, wavelet-based compression algorithm for downlink. On the ground, the images were decompressed and recompressed losslessly as RGB PNG files by GSEOS (Ground Support Equipment Operating System). The LCROSS Make Archive program read these files, selected the Red channel, and wrote that as a single-channel, PDS-formatted image (.IMG) file and a FITS file. Data ==== These files are stored as PDS-formatted, 8 bit UNSIGNED_INTEGER files. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images have been left in the camera's coordinate system. To convert them to the LCROSS Payload Common Camera Coordinate System, these images must be rotated +180 degrees. A description of mapping the images with respect to each other and the S/C coordinate system is contained within the LCROSS Instrument Response and Calibration Report. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated imagery from the near infrared camera #2 (NIR2) on the LCROSS spacecraft (S/C). NIR2 is a camera sensitive from 0.9 to 1.7 microns. The images in this dataset have targets named Moon, Earth, Calibration (i.e., not targeted) and TestImage. Test images include ramps and camera initialization images that contain no science content. Each calibrated image file is a 32-bit PC_REAL greyscale image, with a 720 x 486 pixel format. The image aspect ratio [H:V] is 1.33. The effective field-of-view [FOV] is 28.3 [H] x 21.4 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_NIR2_CAL_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= NIR2_RAW (described in NIR2_RAW_DS.CAT) contains the raw versions of the images contained in this dataset of calibrated images. The NIR1_RAW and NIR1_CAL datasets contain images from the other near-infrared camera. NIR1 had almost exactly the same field of view and was slightly less sensitive due to having an added filter. Parameters ========== Science ------After initialization, the near-infrared cameras were operated by setting two independent parameters: 1. LCROSS:NIR_OPR (an integer [0, 15] inclusive) One of 16 operational configurations stored in non-volatile memory. The factory default settings for these configurations were used. This setting determines the camera's integration time (in the labels as LCROSS:NIR_INTEGRATION_TIME in microseconds) and gain setting (LCROSS:NIR_GAIN in electrons per DN). 2. LCROSS:ENHANCEMENT_MODE [OFF,ON] Image stretching. Enabled only during the STARFIELD data collection period. These cameras have additional configuration settings that were redundant or kept constant and so are not noted in the labels. The digital gain setting was always 1. The effect of automatic gain control is to vary the OPR number, which is reported in the labels, so the automatic gain configuration is redundant. In any case, this setting was off except for during the lunar swingby. The Global Offset Value was always 100 except during initialization where it was briefly set to 4095. This parameter isn't noted in the labels, but all images where it was not 100 have a TARGET_NAME of TEST_IMAGE. Test images include ramps, all states high (white image), and all-states-low (flat dark image) and contain no science content. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== The detector produces 320 x 240, 12-bit grayscale images. Each image was converted inside the camera to an analog, NTSC image and transmitted to the spacecraft. The spacecraft multiplexed the two near-infrared cameras with the visible light 'context' camera, receiving images from only one of these three cameras at a time. When received, the spacecraft converted each NTSC image back to a 720 x 486, 24-bit RGB digital image and compressed it using a lossy, proprietary, wavelet-based compression algorithm for downlink. On the ground, the images were decompressed and recompressed losslessly as RGB PNG files by GSEOS (Ground Support Equipment Operating System). The LCROSS Make Archive program read these files, selected the Red channel, and wrote that as a single-channel, PDS-formatted image (.IMG) file and a FITS file. Data ==== These files are stored as 32-bit PC_REAL image files. Each pixel's value is given as radiance units [W/m^2 sr]. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images have been left in the camera's coordinate system. To convert them to the LCROSS Payload Common Camera Coordinate System, these images must be rotated +180 degrees. A description of mapping the images with respect to each other and the S/C coordinate system is contained within the LCROSS Instrument Response and Calibration Report in the CALIB directory of this archive. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains imagery from the near-infrared camera #2 (NIR2) on the LCROSS spacecraft (S/C). NIR2 is a camera sensitive from 0.9 to 1.7 microns. The images in this dataset have targets named Moon, Earth, Calibration (i.e., not targeted) and TestImage. Test images include ramps and camera initialization images that contain no science content. Each raw image file is an 8-bit integer greyscale image, with a 720 x 486 pixel format. The image aspect ratio [H:V] is 1.33. The effective field-of-view [FOV] is 28.3 [H] x 21.4 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_NIR2_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. Related Data Sets ================= NIR2_CAL (described in NIR2_CAL_DS.CAT) contains the calibrated versions of the images contained in this dataset of raw images. The NIR1_RAW and NIR1_CAL datasets contain images from the other near-infrared camera. NIR1 had almost exactly the same field of view and was slightly less sensitive due to having an added filter. Parameters ========== Science ------After initialization, the near-infrared cameras were operated by setting two independent parameters: 1. LCROSS:NIR_OPR (an integer [0, 15] inclusive) One of 16 operational configurations stored in non-volatile memory. The factory default settings for these configurations were used. This setting determines the camera's integration time (in the labels as LCROSS:NIR_INTEGRATION_TIME in microseconds) and gain setting (LCROSS:NIR_GAIN in electrons per DN). 2. LCROSS:ENHANCEMENT_MODE [OFF,ON] Image stretching. Enabled only during the STARFIELD data collection period. These cameras have additional configuration settings that were redundant or kept constant and so are not noted in the labels. The digital gain setting was always 1. The effect of automatic gain control is to vary the OPR number, which is reported in the labels, so the automatic gain configuration is redundant. In any case, this setting was off except for during the lunar swingby. The Global Offset Value was always 100 except during initialization where it was briefly set to 4095. This parameter isn't noted in the labels, but all images where it was not 100 have a TARGET_NAME of TEST_IMAGE. Test images include ramps, all states high (white image), and all-states-low (flat dark image) and contain no science content. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== The detector produces 320 x 240, 12-bit grayscale images. Each image was converted inside the camera to an analog, NTSC image and transmitted to the spacecraft. The spacecraft multiplexed the two near-infrared cameras with the visible light 'context' camera, receiving images from only one of these three cameras at a time. When received, the spacecraft converted each NTSC image back to a 720 x 486, 24-bit RGB digital image and compressed it using a lossy, proprietary, wavelet-based compression algorithm for downlink. On the ground, the images were decompressed and recompressed losslessly as RGB PNG files by GSEOS (Ground Support Equipment Operating System). The LCROSS Make Archive program read these files, selected the Red channel, and wrote that as a single-channel, PDS-formatted image (.IMG) file and a FITS file. Data ==== These files are stored as PDS-formatted, 8 bit MSB_UNSIGNED_INTEGER files. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images need to be rotated +180 degrees to place them in the LCROSS Payload Common Camera Coordinate System. A description of mapping the images with respect to each other and the S/C coordinate system is contained within the LCROSS Instrument Response and Calibration Report in the CALIB directory of this archive. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated spectra from Near Infrared Spectrometer #1 on the LCROSS spacecraft. NSP1 was the primary instrument on LCROSS, and its boresight was the reference for all nadir-looking instruments. After the centaur impact, the LCROSS spacecraft kept the impact site within the field of view of this instrument until shortly before its own impact. Each file in this dataset contains a 100 pixel spectra in an ascii, single-column, tabular format. All spectra in this dataset used an integration time of 0.5 sec. The spectrometer's field of view was circular and 1 deg in diameter. The spectra in this dataset have targets named Moon, Earth and Calibration (i.e., not targeted). The time each spectra was captured is encoded in the spectra's filename like this: LCROSS_NSP1_CAL_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. This dataset encompasses all calibrated spectra collected by NSP1 during the mission, however, the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= This dataset is closely related to the NSP1_PREHAD and NSP1_RAW datasets. This spectrometer transmits data through the spacecraft to the ground in a format that is processed to create these raw spectra. The processing algorithm is a kind of Fourier transform called a Hadamard transform. The pre-Hadamard data for this spectrometer is contained in a dataset described in NSP1_PREHAD_DS.CAT in this directory. This algorithm is deterministic and has no inputs other than the pre-hadamard data, so reprocessing that data to generate updated raw spectra is unlikely. However, the pre-hadamard data is used to determine whether spectra contain saturated pixels. This dataset is not as closely related to NSP2_RAW and NSP2_CAL. Unlike the camera pairs which had overlapping fields of view, NSP1 and NSP2 were pointed in different directions. NSP1 was pointed downward, toward the centaur impact, while NSP2 was pointed toward the sun to measure absorption spectra. Parameters ========== Science ------No instrument parameters vary within this dataset. The integration time is uniformly 0.5 seconds. Housekeeping -----------Instrument temperature at the data capture time is reported in the label file under INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its pre-hadamard transformed format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, the hadamard transform was applied, and they were converted to CSV format. The LCROSS Make Archive program read these files, applied the per-pixel calibration function and wrote them as PDS-formatted table (.TAB) and label (.LBL) files. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Coordinate System ================= The label files for these spectra contain the spectrometer's boresight vector in J2000 Geocentric Inertial frame. Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated flash-mode spectra from Near Infrared Spectrometer #1 on the LCROSS spacecraft. NSP1 was the primary instrument on LCROSS, and its boresight was the reference for all nadir-looking instruments. NSP1 was in its high-speed, low spectral resolution 'flash' mode from 1 minute before Centaur impact until 5 seconds afterwards. This dataset contains those observations. Unlike the other spectra and images, flash mode data is in table files containing multiple spectra taken at 72 Hz (in this dataset). There is one of these table files per payload data collection period where NSP1 flash mode was used. This dataset also contains table files holding housekeeping data. Related Data Sets ================= This dataset contains calibrated spectra. The NSP1_FL_RAW dataset contains the corresponding uncalibrated spectra. That dataset is described in NSP1_FL_RAW_DS.CAT in this directory. NSP1_RAW_DS.CAT and NSP1_CAL_DS.CAT describe data taken from this spectrometer in its high-resolution 'hadamard' mode. Parameters ========== Science ------The data collection period is 72 Hz. Housekeeping -----------Instrument temperature at the data capture time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its raw format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, and they were converted to CSV format. For each data collection period, the LCROSS Make Archive program read these files, applied a per-mask calibration function and wrote them as a PDS-formatted table (.TAB) and label (.LBL) file. Data ==== The files in this dataset are PDS-formatted, ascii, tables with detached label files. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw flash-mode spectra from Near Infrared Spectrometer #1 on the LCROSS spacecraft. NSP1 was the primary instrument on LCROSS, and its boresight was the reference for all nadir-looking instruments. NSP1 was in its high-speed, low spectral resolution 'flash' mode from 1 minute before Centaur impact until 5 seconds afterwards. This dataset contains those observations. Unlike the other spectra and images, flash mode data is in table files containing multiple spectra taken at 72 Hz (in this dataset). There is one of these table files per payload data collection period where NSP1 flash mode was used. This dataset also contains table files holding housekeeping data. Related Data Sets ================= This dataset contains uncalibrated spectra. The NSP1_FL_CAL dataset contains the corresponding calibrated spectra. That dataset is described in NSP1_FL_CAL_DS.CAT in this directory. NSP1_RAW_DS.CAT and NSP1_CAL_DS.CAT describe data taken from this spectrometer in its high-resolution 'hadamard' mode. Parameters ========== Science ------The data collection period is 72 Hz. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its raw format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, and they were converted to CSV format. For each data collection period, the LCROSS Make Archive program read these files and wrote them as a PDS-formatted table (.TAB) and label (.LBL) file. Data ==== The files in this dataset are PDS-formatted, ascii, tables with detached label files. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw mask data from Near Infrared Spectrometer #1 on the LCROSS spacecraft from which full-resolution, hadamard-mode spectra can be assembled. The dataset contains one table per data collection period. Each table contains one row per full-resolution, Hadamard spectrum captured during that collection period. Each row contains a timestamp and 256 values corresponding to 256 distinct configurations of the MEMS mask within the spectrometer. Conversion of raw mask data into raw spectra is deterministic and involves no calibration inputs. However, this form of the data makes some attributes more apparent. In particular, the check for saturation is done on this form. The timestamp used in each row of these tables is the uncorrected spacecraft time which appears in the labels for the raw and calibrated spectra as the SPACECRAFT_CLOCK_STOP_COUNT attribute. This dataset encompasses all pre-hadamard mask data collected by NSP1 during the mission. Note that the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= This dataset is closely related to the NSP1_RAW and NSP1_CAL datasets. Parameters ========== Science ------No instrument parameters vary within this dataset. The integration time is uniformly 0.5 seconds. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its raw format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, and they were converted to CSV format. For each data collection period, the LCROSS Make Archive program read these files and wrote them as a PDS-formatted table (.TAB) and label (.LBL) file. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Coordinate System ================= The label files for these spectra contain the spectrometer's boresight vector in J2000 Geocentric Inertial frame. Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw spectra from Near Infrared Spectrometer #1 on the LCROSS spacecraft. NSP1 was the primary instrument on LCROSS, and its boresight was the reference for all nadir-looking instruments. After the centaur impact, the LCROSS spacecraft kept the impact site within the field of view of this instrument until shortly before its own impact. Each file in this dataset contains a 100 pixel spectra in an ascii, single-column, tabular format. All spectra in this dataset used an integration time of 0.5 sec. The spectrometer's field of view was circular and 1 deg in diameter. The spectra in this dataset have targets named Moon, Earth and Calibration (i.e., not targeted). The time each spectra was captured is encoded in the spectra's filename like this: LCROSS_NSP1_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. This dataset encompasses all raw spectra collected by NSP1 during the mission. Note that the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= This dataset is closely related to the NSP1_PREHAD and NSP1_CAL datasets. This spectrometer transmits data through the spacecraft to the ground in a format that is processed to create these raw spectra. The processing algorithm is a kind of Fourier transform called a Hadamard transform. The pre-Hadamard data for this spectrometer is contained in a dataset described in NSP1_PREHAD_DS.CAT in this directory. This algorithm is deterministic and has no inputs other than the pre-hadamard data, so reprocessing that data to generate updated raw spectra is unlikely. However, the pre-hadamard data is used to determine whether spectra contain saturated pixels. This dataset is not as closely related to NSP2_RAW and NSP2_CAL. Unlike the camera pairs which had overlapping fields of view, NSP1 and NSP2 were pointed in different directions. NSP1 was pointed downward, toward the centaur impact, while NSP2 was pointed toward the sun to measure absorption spectra. Parameters ========== Science ------No instrument parameters vary within this dataset. The integration time is uniformly 0.5 seconds. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its pre-hadamard transformed format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, the hadamard transform was applied, and they were converted to CSV format. The LCROSS Make Archive program read these files and wrote them as PDS-formatted table (.TAB) and label (.LBL) files. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Coordinate System ================= The label files for these spectra contain the spectrometer's boresight vector in J2000 Geocentric Inertial frame. Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated spectra from Near Infrared Spectrometer #2 on the LCROSS spacecraft. During the final moments of the LCROSS mission, NSP2 looked toward the sun to capture absorption spectra as the spacecraft passed through the ejecta and vapor cloud left by the centaur impact. Each file in this dataset contains a 100 pixel spectra in an ascii, single-column, tabular format. All spectra in this dataset used an integration time of 0.5 sec. The spectrometer's field of view was circular and 1 deg in diameter. All spectra in this dataset have the sun as their target, although it is outside the instrument's field of view during some calibration data collection periods. The time each spectra was captured is encoded in the spectra's filename like this: LCROSS_NSP2_CAL_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. This dataset encompasses all calibrated spectra collected by NSP2 during the mission, however, the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= This dataset is closely related to the NSP2_PREHAD and NSP2_RAW datasets. This spectrometer transmits data through the spacecraft to the ground in a format that is processed to create these raw spectra. The processing algorithm is a kind of Fourier transform called a Hadamard transform. The pre-Hadamard data for this spectrometer is contained in a dataset described in NSP2_PREHAD_DS.CAT in this directory. This algorithm is deterministic and has no inputs other than the pre-hadamard data, so reprocessing that data to generate updated raw spectra is unlikely. However, the pre-hadamard data is used to determine whether spectra contain saturated pixels. This dataset is not as closely related to NSP1_RAW and NSP1_CAL. Unlike the camera pairs which had overlapping fields of view, NSP1 and NSP2 were pointed in different directions. NSP1 was pointed downward, toward the centaur impact, while NSP2 was pointed toward the sun to measure absorption spectra. Parameters ========== Science ------No instrument parameters vary within this dataset. The integration time is uniformly 0.5 seconds. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its pre-hadamard transformed format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, the hadamard transform was applied, and they were converted to CSV format. The LCROSS Make Archive program read these files, applied the per-pixel calibration function and wrote them as PDS-formatted table (.TAB) and label (.LBL) files. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated flash-mode spectra from Near Infrared Spectrometer #2 on the LCROSS spacecraft. During the final moments of the LCROSS mission, NSP2 looked toward the sun to capture absorption spectra as the spacecraft passed through the ejecta and vapor cloud left by the centaur impact. Unlike the other spectra and images, flash mode data is in table files containing multiple spectra taken at 72 Hz (in this dataset). There is one of these table files per payload data collection period where NSP2 flash mode was used. This dataset also contains table files holding housekeeping data. Related Data Sets ================= This dataset contains calibrated spectra. The NSP2_FL_RAW dataset contains the corresponding uncalibrated spectra. That dataset is described in NSP2_FL_RAW_DS.CAT in this directory. NSP2_RAW_DS.CAT and NSP2_CAL_DS.CAT describe data taken from this spectrometer in its high-resolution 'hadamard' mode. Parameters ========== Science ------The data collection period is 72 Hz. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its raw format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, and they were converted to CSV format. For each data collection period, the LCROSS Make Archive program read these files, applied a per-mask calibration function and wrote them as a PDS-formatted table (.TAB) and label (.LBL) file. Data ==== The files in this dataset are PDS-formatted, ascii, tables with detached label files. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw flash-mode spectra from Near Infrared Spectrometer #1 on the LCROSS spacecraft. During the final moments of the LCROSS mission, NSP2 looked toward the sun to capture absorption spectra as the spacecraft passed through the ejecta and vapor cloud left by the centaur impact. Unlike the other spectra and images, flash mode data is in table files containing multiple spectra taken at 72 Hz (in this dataset). There is one of these table files per payload data collection period where NSP2 flash mode was used. This dataset also contains table files holding housekeeping data. Related Data Sets ================= This dataset contains uncalibrated spectra. The NSP2_FL_CAL dataset contains the corresponding calibrated spectra. It's described in NSP2_FL_CAL_DS.CAT in this directory. NSP2_RAW_DS.CAT and NSP2_CAL_DS.CAT describe data taken from this spectrometer in its high-resolution 'hadamard' mode. Parameters ========== Science ------The data collection period is 72 Hz. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its raw format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, and they were converted to CSV format. For each data collection period, the LCROSS Make Archive program read these files and wrote them as a PDS-formatted table (.TAB) and label (.LBL) file. Data ==== The files in this dataset are PDS-formatted, ascii, tables with detached label files. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw mask data from Near Infrared Spectrometer #2 on the LCROSS spacecraft from which full-resolution, hadamard-mode spectra can be assembled. The dataset contains one table per data collection period. Each table contains one row per full-resolution, Hadamard spectrum captured during that collection period. Each row contains a timestamp and 256 values corresponding to 256 distinct configurations of the MEMS mask within the spectrometer. Conversion of raw mask data into raw spectra is deterministic and involves no calibration inputs. However, this form of the data makes some attributes more apparent. In particular, the check for saturation is done on this form. The timestamp used in each row of these tables is the uncorrected spacecraft time which appears in the labels for the raw and calibrated spectra as the SPACECRAFT_CLOCK_STOP_COUNT attribute. This dataset encompasses all pre-hadamard mask data collected by NSP2 during the mission. Note that the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= This dataset is closely related to the NSP2_RAW and NSP2_CAL datasets. Parameters ========== Science ------No instrument parameters vary within this dataset. The integration time is uniformly 0.5 seconds. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its raw format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, and they were converted to CSV format. For each data collection period, the LCROSS Make Archive program read these files and wrote them as a PDS-formatted table (.TAB) and label (.LBL) file. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Coordinate System ================= The label files for these spectra contain the spectrometer's boresight vector in J2000 Geocentric Inertial frame. Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw spectra from Near Infrared Spectrometer #2 on the LCROSS spacecraft. During the final moments of the LCROSS mission, NSP2 looked toward the sun to capture absorption spectra as the spacecraft passed through the ejecta and vapor cloud left by the centaur impact. Each file in this dataset contains a 100 pixel spectra in an ascii, single-column, tabular format. All spectra in this dataset used an integration time of 0.5 sec. The spectrometer's field of view was circular and approximately 80 degrees in radius. All spectra in this dataset have the sun as their target, although it is outside the instrument's field of view during some calibration data collection periods. The time each spectra was captured is encoded in the spectra's filename like this: LCROSS_NSP2_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. This dataset encompasses all raw spectra collected by NSP2 during the mission, however, the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= This dataset is closely related to the NSP2_PREHAD and NSP2_CAL datasets. This spectrometer transmits data through the spacecraft to the ground in a format that is processed to create these raw spectra. The processing algorithm is a kind of Fourier transform called a Hadamard transform. The pre-Hadamard data for this spectrometer is contained in a dataset described in NSP1_PREHAD_DS.CAT in this directory. This algorithm is deterministic and has no inputs other than the pre-hadamard data, so reprocessing that data to generate updated raw spectra is unlikely. However, the pre-hadamard data is used to determine whether spectra contain saturated pixels. This dataset is not as closely related to NSP1_RAW and NSP1_CAL. Unlike the camera pairs which had overlapping fields of view, NSP1 and NSP2 were pointed in different directions. NSP1 was pointed downward, toward the centaur impact, while NSP2 was pointed toward the sun to measure absorption spectra. Parameters ========== Science ------No instrument parameters vary within this dataset. The integration time is uniformly 0.5 seconds. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. Processing ========== Each near-infrared spectra was digitally transmitted from the spectrometer to the spacecraft in its pre-hadamard transformed format, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry, the hadamard transform was applied, and they were converted to CSV format. The LCROSS Make Archive program read these files and wrote them as a PDS-formatted table (.TAB) and label (.LBL) files. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated spectra from Total Luminance Photometer on the LCROSS spacecraft. The TLP was active only during the final 25 minutes of the mission, including the time of the centaur impact. It sampled an ~10 deg full angle, circular field of view at 1000 Hz. This dataset consists of a single ascii table holding temperature-normalized voltages from the instrument and a second table holding housekeeping data. The only target was Cabeus crater on the moon. Note that this dataset is not contain a measurement of power. The Instrument Response and Calibration Report describes the detector response as a function of wavelength, which, together with an assumption about the spectrum observed, is needed to map the measured voltage to power. Related Data Sets ================= TLP_RAW_DS holds the raw TLP measurements, in DNs. This dataset is described in TLP_RAW_DS.CAT in this directory. Parameters ========== Science ------No instrument parameters vary within this dataset. The sample rate is uniformly 1000 Hz. Housekeeping -----------Instrument temperature is reported in the metadata tables in the SEM_TEMPERATURE and DEM_TEMPERATURE columns in degrees Centigrade. These are the two spacecraft telemetry points closest to the TLP Sensor Electronics Module (SEM) and (Digital Electronics Module (DEM) respectively. TLP_CAL_DS also contains the temperature of the detector in degrees Centigrade. The voltage reported in the table has been used to correct the reported voltage to a detector temperature of 0 degC. Processing ========== TLP sensor readings were transmitted to the spacecraft in 0.1 second groups (100 values). Each group was inserted into telemetry uncompressed and downlinked. The ground system extracted these groups in oder and appended them to a single .CSV file. The LCROSS Make Archive program read this file, applied temperature normalization function, and wrote two PDS-formatted table (.TAB) files, one each for the PREIMPACT and IMPACT data collection periods. Corresponding to each of these two files is a table (.TAB) file containing metadata. Data ==== The data files in this dataset are PDS-formatted, ascii, two-column tables with detached label files. The first column contains the time in UTC, and the second column contains temperature-normalized voltages. The rows are in time order and generally 1 msec apart. Metadata is contained in PDS-formatted, ascii, multi-column tables, also with detached labels. Coordinate System ================= The metadata tables contain the NSP1 boresight vector in J2000 Geocentric Inertial frame. This is the reference boresight vector for the LCROSS payload and is approximately at the center of the TLP field of view. Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw spectra from Total Luminance Photometer on the LCROSS spacecraft. The TLP was active only during the final 25 minutes of the mission, including the time of the centaur impact. It sampled an ~10 deg full angle, circular field of view at 1000 Hz. This dataset consists of a single ascii table holding raw values from the instrument and a second table holding housekeeping data. The only target was Cabeus crater on the moon. Related Data Sets ================= TLP_CAL_DS holds an intermediate calibration product, described in TLP_CAL_DS.CAT in this directory. Parameters ========== Science ------No instrument parameters vary within this dataset. The sample rate is uniformly 1000 Hz. Housekeeping -----------Instrument temperature is reported in the metadata tables in the SEM_TEMPERATURE and DEM_TEMPERATURE columns in degrees Centigrade. These are the two spacecraft telemetry points closest to the TLP Sensor Electronics Module (SEM) and (Digital Electronics Module (DEM) respectively. TLP_CAL_DS also contains the temperature of the detector. That temperature is not listed in this dataset. Processing ========== TLP sensor readings were transmitted to the spacecraft in 0.1 second groups (100 values). Each group was inserted into telemetry uncompressed and downlinked. The ground system extracted these groups in oder and appended them to a single .CSV file. The LCROSS Make Archive program read this file and wrote two PDS-formatted table (.TAB) files, one each for the PREIMPACT and IMPACT data collection periods. Corresponding to each of these two files is a table (.TAB) file containing metadata. Data ==== The files in this dataset are PDS-formatted, ascii, two-column tables with detached label files. The first column contains the time in UTC, and the second column contains the raw data value from the TLP. The rows are in time order and generally 1 msec apart. Metadata is contained in PDS-formatted, ascii, multi-column tables, also with detached labels. Coordinate System ================= The metadata tables contain the NSP1 boresight vector in J2000 Geocentric Inertial frame. This is the reference boresight vector for the LCROSS payload and is approximately at the center of the TLP field of view. Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains context imagery from the visible light camera (VIS) on the LCROSS spacecraft. The images in this dataset have targets named Moon, Earth and Calibration (i.e., not targeted). Each raw image file is a 24-bit RGB image, with a 720 x 486 pixel format. The image aspect ratio [H:V] is 1.33. The effective field-of-view [FOV] is 30.5 [H] x 22.8 [V] degrees. The time each image was captured is encoded in the image's filename like this: LCROSS_VIS_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. Detached labels for each image have the same filename as the image but with the 'LBL' extension. Related Data Sets ================= There is no dataset containing radiometrically calibrated images from this camera. The field of view of this camera overlaps with the fields of view of all other instruments except Near Infrared Spectrometer #2 (NSP2). Parameters ========== Science ------There are no configurable parameters for the visible camera. Housekeeping -----------Instrument temperature at the image generation time is reported in the label file under: INSTRUMENT_TEMPERATURE, INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the camera chassis temperature for the image. Processing ========== The detector produces 768 x 494, RGB images. Each image was converted inside the camera to an analog, NTSC image and transmitted to the spacecraft. The spacecraft multiplexed this camera with the two near-infrared cameras, receiving images from only one of these three cameras at a time. When received, the spacecraft converted each NTSC image to a 720 x 486, 24-bit RGB digital image and compressed it using a lossy, proprietary, wavelet-based compression algorithm for downlink. On the ground, the images are decompressed and recompressed losslessly as RGB PNG files by GSEOS (Ground Support Equipment Operating System). The LCROSS Make Archive program read these files, selected the Red channel, and wrote that as a three-channel, PDS-formatted (.IMG) file and a FITS file. Data ==== These files are stored as PDS-formatted, three channel, 8-bit MSB_UNSIGNED_INTEGER files. Each image file has a corresponding detached PDS label file sharing the same filename and an 'LBL' filetype. The EXTRAS directory contains these images in FITS format as well. Coordinate System ================= These images have been left in the camera's coordinate system. These images need to be rotated +233 degrees to place them in the LCROSS Payload Common Camera Coordinate System. A description of mapping the images with respect to each other and the S/C coordinate system is contained within the LCROSS Instrument Response and Calibration Report. Software ======== The GSEOS Version used to generate these images is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The LCROSS Make Archive program used to combine the output from GSEOS, LCROSS.py and LCROSS Report Generator to generate the PDS image and ASCII label files is dated 03/14/2010.
Data Set Overview ================= This data set contains calibrated spectra from the LCROSS Visible Spectrometer (VSP). This instrument's boresight was parallel to the payload reference boresight (Near Infrared Spectrometer #1). After the centaur impact, the spacecraft kept the impact site within the field of view of this instrument until shortly before its own impact. Each file in this dataset contains a 1024 pixel spectra in an ascii, single-column, tabular format. Integration time varied and is noted in the labels. The spectrometer's field of view was circular and 1 degree in diameter. The spectra in this dataset have targets named Moon, Earth and Calibration (i.e., not targeted). The time each spectra was captured is encoded in the spectra's filename like this: LCROSS_VSP_CAL_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. This dataset encompasses all calibrated spectra collected by the VSP during the mission. Note that the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= The VSP_RAW dataset contains the raw versions of the spectra in this dataset. Parameters ========== Science ------Integration time varies between spectra and is noted in milliseconds by the EXPOSURE_DURATION attribute in the label files. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. The thermoelectric cooler control setpoint and best-estimate detector temperature temperature are noted in degrees centigrade in the LCROSS:TEC_SETPOINT and LCROSS:TEC_TEMPERATURE attributes, respectively. The VSP implemented a 'bracket' exposure mode intended to vary the integration time to compensate for uncertainty about the expected scene. In this mode, the spectrometer captured three spectra in quick succession with short, medium and long integration times. Other than integration time, no other aspect of data collection was changed. This aspect of VSP data collection is visible in the LCROSS:VSP_BRACKET_NUMBER and LCROSS:PACKET_TIMESTAMP attributes, which allow PDS-formatted spectra to be tracked back to the slot in the telemetry packet they were created from. Processing ========== Each visible and ultraviolet light spectra was digitally transmitted from the spectrometer to the spacecraft with error detection, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry and converted to CSV format. The LCROSS Make Archive program read these files, applied a per-pixel calibration function and wrote them as PDS-formatted (.TAB) and label (.LBL) files. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Each table contains 1024 rows. The 20 non-spectral pixels have not been given calibrated values and their values are not present in these files. Their values are available in the raw spectra files. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
Data Set Overview ================= This data set contains raw spectra from the LCROSS Visible Spectrometer (VSP). This instrument's boresight was parallel to the payload reference boresight (Near Infrared Spectrometer #1). After the centaur impact, the spacecraft kept the impact site within the field of view of this instrument until shortly before its own impact. Each file in this dataset contains a 1024 pixel spectra plus 20 reference pixels in an ascii, single-column, tabular format. Integration time varied and is noted in the labels. The spectrometer's field of view was circular and 1 degree in diameter. The spectra in this dataset have targets named Moon, Earth and Calibration (i.e., not targeted). The time each spectra was captured is encoded in the spectra's filename like this: LCROSS_VSP_RAW_<timestamp>.IMG where <timestamp> = YYYYMMDDHHMMSSmmm and YYYY = the four digit year; MM = the two digit month, DD = the two digit day, and so on through hours, minutes, seconds and milliseconds. The detached label for each spectra has the same filename as the spectra but with the 'LBL' extension. This dataset encompasses all raw spectra collected by the VSP during the mission. Note that the archive's DATA directory is partitioned initially by payload data collection period. The data collection period called 20091009113022_IMPACT contains the data from one minute prior to the Centaur impact through the end of the mission. Other data collection periods periods contain data from various calibration targets. Related Data Sets ================= The VSP_CAL dataset contains the calibrated versions of the spectra in this dataset. Parameters ========== Science ------Integration time varies between spectra and is noted in milliseconds by the EXPOSURE_DURATION attribute in the label files. Housekeeping -----------Instrument temperature at the data collection time is reported in the label file under: INSTRUMENT_TEMPERATURE and INSTRUMENT_TEMPERATURE_COUNT in degrees Centigrade and raw counts, respectively. This is a single telemetry point most representative of the instrument chassis temperature. The thermoelectric cooler control setpoint and best-estimate detector temperature temperature are noted in degrees centigrade in the LCROSS:TEC_SETPOINT and LCROSS:TEC_TEMPERATURE attributes, respectively. The VSP implemented a 'bracket' exposure mode intended to vary the integration time to compensate for uncertainty about the expected scene. In this mode, the spectrometer captured three spectra in quick succession with short, medium and long integration times. Other than integration time, no other aspect of data collection was changed. This aspect of VSP data collection is visible in the LCROSS:VSP_BRACKET_NUMBER and LCROSS:PACKET_TIMESTAMP attributes, which allow PDS-formatted spectra to be tracked back to the slot in the telemetry packet they were created from. Processing ========== Each visible and ultraviolet light spectra was digitally transmitted from the spectrometer to the spacecraft with error detection, inserted into a packet uncompressed and downlinked in telemetry. On the ground, the spectra were extracted from telemetry and converted to CSV format. The LCROSS Make Archive program read these files and wrote them as PDS-formatted (.TAB) and label (.LBL) files. Data ==== The files in this dataset are PDS-formatted, ascii, single-column tables with detached label files. Each table contains one 1024 pixel spectra in its first 1024 rows, followed by 20 reference pixels. File rows [1031,1032] inclusive may be used as dark pixels. They are at the long wavelength end of the spectrometer. Rile rows [1036,1038] inclusive may also be used as dark pixels, and they are at the short wavelength end. All other, non-spectral rows are unused. These indices label the first row of the file as row #1. Coordinate System ================= TBD Software ======== The GSEOS Version used to generate these spectra is GSEOS 5.2.407 (Feb 25, 2008), Python 2.2.3 (#37, Nov 28, 2003, 04:20:20), Project Version 6.1.064. The LCROSS.py Python script used with GSEOS is Version Jun 11, 2008. The LCROSS Report Generator used on GSEOS created CCSDS.dat files is version 114. The version of Satellite Toolkit used to prepare geometric information for the labels is 8.1.3. The LCROSS Make Archive program used to assemble the PDS-formatted submission is dated 03/14/2010.
These data are available on-line from the Planetary Data System (PDS) at:
http://pds-geosciences.wustl.edu/lunar/lcross-e_l-mir1-2-raw-v1/lcro_0001/
Questions and comments about this data collection can be directed to: Dr. David R. Williams
Name | Role | Original Affiliation | |
---|---|---|---|
Dr. Anthony Colaprete | Data Provider | NASA Ames Research Center | Anthony.Colaprete-1@nasa.gov |
Dr. Anthony Colaprete | General Contact | NASA Ames Research Center | Anthony.Colaprete-1@nasa.gov |