VAM Enhanced Sensor Pallet - Revision history

Cyclops: changed caption formatting

2023-12-23T02:02:41Z

changed caption formatting

← Older revision		Revision as of 02:02, 23 December 2023
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	== Range ==		== Range ==
	{\| class="wikitable"		{\| class="wikitable"
	\|+ style="caption-side:bottom;" \| ~~'''''~~1 AU~~'''~~ (Astronomical Unit) = ~~'''~~1.5 Million km~~'''~~<br>~~'''~~1 ly~~'''~~ (light year) = ~~'''~~63241.1 AU~~'''''~~		\|+ style="text-align:center;font-size:x-small;caption-side:bottom;" \| 1 AU (Astronomical Unit) = 1.5 Million km<br>1 ly (light year) = 63241.1 AU
	! Type !! Range !! Description		! Type !! Range !! Description
	\|-		\|-

Cyclops: Added caption for distance scale of AU and ly

2023-12-23T01:53:56Z

Added caption for distance scale of AU and ly

← Older revision		Revision as of 01:53, 23 December 2023
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	== Range ==		== Range ==
	{\| class="wikitable"		{\| class="wikitable"
			\|+ style="caption-side:bottom;" \| '''''1 AU''' (Astronomical Unit) = '''1.5 Million km'''<br>'''1 ly''' (light year) = '''63241.1 AU'''''
	! Type !! Range !! Description		! Type !! Range !! Description
	\|-		\|-

Cyclops: /* Range */ fixed a typo

2023-12-23T01:50:16Z

Range: fixed a typo

← Older revision		Revision as of 01:50, 23 December 2023
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	\| style="white-space:nowrap;" \| High Resolution Temporal Scanners \|\| style="white-space:nowrap;text-align:right;" \| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.		\| style="white-space:nowrap;" \| High Resolution Temporal Scanners \|\| style="white-space:nowrap;text-align:right;" \| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.
	\|-		\|-
	\| style="white-space:nowrap;" \| Short Range Sensors \|\| style="white-space:nowrap;text-align:right;" \| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.		\| style="white-space:nowrap;" \| Short Range Sensors \|\| style="white-space:nowrap;text-align:right;" \| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with a general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.
	\|-		\|-
	\| style="white-space:nowrap;" \| Subspace Distortion Sensors \|\| style="white-space:nowrap;text-align:right;" \| 9.5 ly \|\| Geared towards detecting major subspace distortions.		\| style="white-space:nowrap;" \| Subspace Distortion Sensors \|\| style="white-space:nowrap;text-align:right;" \| 9.5 ly \|\| Geared towards detecting major subspace distortions.

Cyclops: still trying to change the table formatting to my liking.

2023-12-23T01:49:46Z

still trying to change the table formatting to my liking.

← Older revision		Revision as of 01:49, 23 December 2023
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	! Type !! Range !! Description		! Type !! Range !! Description
	\|-		\|-
	\| Planetary Sensor Array \|\| style="white-space:nowrap;text-align:right;" \| 87 AU \|\| Specifically designed for detailed surface scans of planets and stellar bodies within a range of 87 astronomical units.		\| style="white-space:nowrap;" \| Planetary Sensor Array \|\| style="white-space:nowrap;text-align:right;" \| 87 AU \|\| Specifically designed for detailed surface scans of planets and stellar bodies within a range of 87 astronomical units.
	\|-		\|-
	\| VAM Topographical Imaging Array \|\| style="white-space:nowrap;text-align:right;" \| 1,897.23 AU \|\| Specialized for studying various subspace energy flows not otherwise scanned for, ties in with all other sensors to assist in data processing.		\| style="white-space:nowrap;" \| VAM Topographical Imaging Array \|\| style="white-space:nowrap;text-align:right;" \| 1,897.23 AU \|\| Specialized for studying various subspace energy flows not otherwise scanned for, ties in with all other sensors to assist in data processing.
	\|-		\|-
	\| Neutrino Emission Scanner \|\| style="white-space:nowrap;text-align:right;" \| 15,810 AU \|\| Focused neutrino detection and imaging scanner specialized for short-range detection.		\| style="white-space:nowrap;" \| Neutrino Emission Scanner \|\| style="white-space:nowrap;text-align:right;" \| 15,810 AU \|\| Focused neutrino detection and imaging scanner specialized for short-range detection.
	\|-		\|-
	\| High Resolution Temporal Scanners \|\| style="white-space:nowrap;text-align:right;" \| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.		\| style="white-space:nowrap;" \| High Resolution Temporal Scanners \|\| style="white-space:nowrap;text-align:right;" \| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.
	\|-		\|-
	\| Short Range Sensors \|\| style="white-space:nowrap;text-align:right;" \| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.		\| style="white-space:nowrap;" \| Short Range Sensors \|\| style="white-space:nowrap;text-align:right;" \| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.
	\|-		\|-
	\| Subspace Distortion Sensors \|\| style="white-space:nowrap;text-align:right;" \| 9.5 ly \|\| Geared towards detecting major subspace distortions.		\| style="white-space:nowrap;" \| Subspace Distortion Sensors \|\| style="white-space:nowrap;text-align:right;" \| 9.5 ly \|\| Geared towards detecting major subspace distortions.
	\|-		\|-
	\| Advanced Spectral Analyzers \|\| style="white-space:nowrap;text-align:right;" \| 12.8 ly \|\| Specialized sensors capable of analyzing detailed spectral data.		\| style="white-space:nowrap;" \| Advanced Spectral Analyzers \|\| style="white-space:nowrap;text-align:right;" \| 12.8 ly \|\| Specialized sensors capable of analyzing detailed spectral data.
	\|-		\|-
	\| Low Resolution Temporal Anomaly Sensors \|\| style="white-space:nowrap;text-align:right;" \| 17 ly \|\| Designed to detect temporal anomalies at a lower resolution.		\| style="white-space:nowrap;" \| Low Resolution Temporal Anomaly Sensors \|\| style="white-space:nowrap;text-align:right;" \| 17 ly \|\| Designed to detect temporal anomalies at a lower resolution.
	\|-		\|-
	\| Gravitational Displacement Scanners \|\| style="text-align:right;" \| 18.2 ly \|\| Focused on detecting fluctuations in gravitational fields.		\| style="white-space:nowrap;" \| Gravitational Displacement Scanners \|\| style="text-align:right;" \| 18.2 ly \|\| Focused on detecting fluctuations in gravitational fields.
	\|-		\|-
	\| Long Range Sensors \|\| style="text-align:right;" \| 22 ly \|\| Optimized for detecting major mass bodies and energy readings.		\| style="white-space:nowrap;" \| Long Range Sensors \|\| style="text-align:right;" \| 22 ly \|\| Optimized for detecting major mass bodies and energy readings.
	\|}		\|}

Cyclops: /* Range */ changed table formatting again

2023-12-23T01:48:28Z

Range: changed table formatting again

← Older revision		Revision as of 01:48, 23 December 2023
Line 5:		Line 5:
	! Type !! Range !! Description		! Type !! Range !! Description
	\|-		\|-
	\| Planetary Sensor Array \|\| style="text-align:right;" \| 87 AU \|\| Specifically designed for detailed surface scans of planets and stellar bodies within a range of 87 astronomical units.		\| Planetary Sensor Array \|\| style="white-space:nowrap;text-align:right;" \| 87 AU \|\| Specifically designed for detailed surface scans of planets and stellar bodies within a range of 87 astronomical units.
	\|-		\|-
	\| VAM Topographical Imaging Array \|\| style="text-align:right;" \| 1,897.23 AU \|\| Specialized for studying various subspace energy flows not otherwise scanned for, ties in with all other sensors to assist in data processing.		\| VAM Topographical Imaging Array \|\| style="white-space:nowrap;text-align:right;" \| 1,897.23 AU \|\| Specialized for studying various subspace energy flows not otherwise scanned for, ties in with all other sensors to assist in data processing.
	\|-		\|-
	\| Neutrino Emission Scanner \|\| style="text-align:right;" \| 15,810 AU \|\| Focused neutrino detection and imaging scanner specialized for short-range detection.		\| Neutrino Emission Scanner \|\| style="white-space:nowrap;text-align:right;" \| 15,810 AU \|\| Focused neutrino detection and imaging scanner specialized for short-range detection.
	\|-		\|-
	\| High Resolution Temporal Scanners \|\| style="text-align:right;" \| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.		\| High Resolution Temporal Scanners \|\| style="white-space:nowrap;text-align:right;" \| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.
	\|-		\|-
	\| Short Range Sensors \|\| style="text-align:right;" \| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.		\| Short Range Sensors \|\| style="white-space:nowrap;text-align:right;" \| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.
	\|-		\|-
	\| Subspace Distortion Sensors \|\| style="text-align:right;" \| 9.5 ly \|\| Geared towards detecting major subspace distortions.		\| Subspace Distortion Sensors \|\| style="white-space:nowrap;text-align:right;" \| 9.5 ly \|\| Geared towards detecting major subspace distortions.
	\|-		\|-
	\| Advanced Spectral Analyzers \|\| style="text-align:right;" \| 12.8 ly \|\| Specialized sensors capable of analyzing detailed spectral data.		\| Advanced Spectral Analyzers \|\| style="white-space:nowrap;text-align:right;" \| 12.8 ly \|\| Specialized sensors capable of analyzing detailed spectral data.
	\|-		\|-
	\| Low Resolution Temporal Anomaly Sensors \|\| style="text-align:right;" \| 17 ly \|\| Designed to detect temporal anomalies at a lower resolution.		\| Low Resolution Temporal Anomaly Sensors \|\| style="white-space:nowrap;text-align:right;" \| 17 ly \|\| Designed to detect temporal anomalies at a lower resolution.
	\|-		\|-
	\| Gravitational Displacement Scanners \|\| style="text-align:right;" \| 18.2 ly \|\| Focused on detecting fluctuations in gravitational fields.		\| Gravitational Displacement Scanners \|\| style="text-align:right;" \| 18.2 ly \|\| Focused on detecting fluctuations in gravitational fields.

Cyclops: Changed table formatting

2023-12-23T01:43:57Z

Changed table formatting

← Older revision		Revision as of 01:43, 23 December 2023
Line 5:		Line 5:
	! Type !! Range !! Description		! Type !! Range !! Description
	\|-		\|-
	\| Planetary Sensor Array \|\| 87 AU \|\| Specifically designed for detailed surface scans of planets and stellar bodies within a range of 87 astronomical units.		\| Planetary Sensor Array \|\| style="text-align:right;" \| 87 AU \|\| Specifically designed for detailed surface scans of planets and stellar bodies within a range of 87 astronomical units.
	\|-		\|-
	\| VAM Topographical Imaging Array \|\| 1,897.23 AU \|\| Specialized for studying various subspace energy flows not otherwise scanned for, ties in with all other sensors to assist in data processing.		\| VAM Topographical Imaging Array \|\| style="text-align:right;" \| 1,897.23 AU \|\| Specialized for studying various subspace energy flows not otherwise scanned for, ties in with all other sensors to assist in data processing.
	\|-		\|-
	\| Neutrino Emission Scanner \|\| 15,810 AU \|\| Focused neutrino detection and imaging scanner specialized for short-range detection.		\| Neutrino Emission Scanner \|\| style="text-align:right;" \| 15,810 AU \|\| Focused neutrino detection and imaging scanner specialized for short-range detection.
	\|-		\|-
	\| High Resolution Temporal Scanners \|\| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.		\| High Resolution Temporal Scanners \|\| style="text-align:right;" \| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.
	\|-		\|-
	\| Short Range Sensors \|\| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.		\| Short Range Sensors \|\| style="text-align:right;" \| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.
	\|-		\|-
	\| Subspace Distortion Sensors \|\| 9.5 ly \|\| Geared towards detecting major subspace distortions.		\| Subspace Distortion Sensors \|\| style="text-align:right;" \| 9.5 ly \|\| Geared towards detecting major subspace distortions.
	\|-		\|-
	\| Advanced Spectral Analyzers \|\| 12.8 ly \|\| Specialized sensors capable of analyzing detailed spectral data.		\| Advanced Spectral Analyzers \|\| style="text-align:right;" \| 12.8 ly \|\| Specialized sensors capable of analyzing detailed spectral data.
	\|-		\|-
	\| Low Resolution Temporal Anomaly Sensors \|\| 17 ly \|\| Designed to detect temporal anomalies at a lower resolution.		\| Low Resolution Temporal Anomaly Sensors \|\| style="text-align:right;" \| 17 ly \|\| Designed to detect temporal anomalies at a lower resolution.
	\|-		\|-
	\| Gravitational Displacement Scanners \|\| 18.2 ly \|\| Focused on detecting fluctuations in gravitational fields.		\| Gravitational Displacement Scanners \|\| style="text-align:right;" \| 18.2 ly \|\| Focused on detecting fluctuations in gravitational fields.
	\|-		\|-
	\| Long Range Sensors \|\| 22 ly \|\| Optimized for detecting major mass bodies and energy readings.		\| Long Range Sensors \|\| style="text-align:right;" \| 22 ly \|\| Optimized for detecting major mass bodies and energy readings.
	\|}		\|}

Cyclops: Changed wiki table

2023-12-23T01:35:45Z

Changed wiki table

← Older revision		Revision as of 01:35, 23 December 2023
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	== Range ==		== Range ==
	{\| class="wikitable ~~sortable~~"		{\| class="wikitable"
	! Type !! Range !! Description		! Type !! Range !! Description
	\|-		\|-

Cyclops: Added ranges for various types of sensors.

2023-12-23T01:35:02Z

Added ranges for various types of sensors.

← Older revision		Revision as of 01:35, 23 December 2023
Line 1:		Line 1:
	The VAM Enhanced Sensor Pallet is the successor to the previously used ''TD Enhanced Sensor Pallet'' widely used through [[Solas Tempus]] vessels and facilities. It is coupled with a intelligent ECC array processing unit which controls an entire array of the enhanced sensor pallets processing raw information before sending it on to a primary computer system.		The VAM Enhanced Sensor Pallet is the successor to the previously used ''TD Enhanced Sensor Pallet'' widely used through [[Solas Tempus]] vessels and facilities. It is coupled with a intelligent ECC array processing unit which controls an entire array of the enhanced sensor pallets processing raw information before sending it on to a primary computer system.

			== Range ==
			{\| class="wikitable sortable"
			! Type !! Range !! Description
			\|-
			\| Planetary Sensor Array \|\| 87 AU \|\| Specifically designed for detailed surface scans of planets and stellar bodies within a range of 87 astronomical units.
			\|-
			\| VAM Topographical Imaging Array \|\| 1,897.23 AU \|\| Specialized for studying various subspace energy flows not otherwise scanned for, ties in with all other sensors to assist in data processing.
			\|-
			\| Neutrino Emission Scanner \|\| 15,810 AU \|\| Focused neutrino detection and imaging scanner specialized for short-range detection.
			\|-
			\| High Resolution Temporal Scanners \|\| 1.7 ly \|\| Specialized sensors offering high-resolution detection of temporal anomalies. These scanners can be tied to the Planetary Sensor Array for higher resolution scans of smaller anomalies.
			\|-
			\| Short Range Sensors \|\| 3.23 ly \|\| General purpose high resolution sensors with both active and passive elements. These sensors are also equipped with general purpose imaging systems which assist other sensor clusters in generating higher resolution data within the short range sensor range.
			\|-
			\| Subspace Distortion Sensors \|\| 9.5 ly \|\| Geared towards detecting major subspace distortions.
			\|-
			\| Advanced Spectral Analyzers \|\| 12.8 ly \|\| Specialized sensors capable of analyzing detailed spectral data.
			\|-
			\| Low Resolution Temporal Anomaly Sensors \|\| 17 ly \|\| Designed to detect temporal anomalies at a lower resolution.
			\|-
			\| Gravitational Displacement Scanners \|\| 18.2 ly \|\| Focused on detecting fluctuations in gravitational fields.
			\|-
			\| Long Range Sensors \|\| 22 ly \|\| Optimized for detecting major mass bodies and energy readings.
			\|}

	== Upgraded Capabilities ==		== Upgraded Capabilities ==

Cyclops: Created page with "The VAM Enhanced Sensor Pallet is the successor to the previously used ''TD Enhanced Sensor Pallet'' widely used through Solas Tempus vessels and facilities. It is couple..."

2020-06-20T18:57:44Z

Created page with "The VAM Enhanced Sensor Pallet is the successor to the previously used ''TD Enhanced Sensor Pallet'' widely used through Solas Tempus vessels and facilities. It is couple..."

New page

The VAM Enhanced Sensor Pallet is the successor to the previously used ''TD Enhanced Sensor Pallet'' widely used through [[Solas Tempus]] vessels and facilities. It is coupled with a intelligent ECC array processing unit which controls an entire array of the enhanced sensor pallets processing raw information before sending it on to a primary computer system.

== Upgraded Capabilities ==
Each pallet unit has a number of advancements over previous models:
* Enhanced Temporal Displacement Tracking
: Capable of a 37.9% increased displacement recognition, tracking, and pattern matching.
* Sequenced Transphasic Signature Recognition
: Sensor elements within an array can be cross-linked and sequenced to provide recognition of transphasic signatures with variable subspace depth and orientation.
* Projected Subspace Active Depth Scanning
: Can scan through the local subspace field through a multi-element active scan phase from one pallet element to another with increase subspace arc. Allows sensors to determine the depth of the local subspace field and how subspace layers are oriented at different levels.
* Passive Subspace Topographical Scanning
: Examines passive readings from the interaction between subspace layers to determine local subspace topography passively.
* VAM Passive Scan Elements
: Receive and process signals from VAM sensor elements in real time.
* Passive Enhanced Anomaly Tracking and Identification
: Using multimodal algorithms sensor elements can be sequenced to detect and track subspace anomalies with a 97.89% increase in tracking, pattern matching, and identification.

== Enhanced Detection and Tracking ==
One of the primary upgrades of this sensor system is that it has an increased vessel detection and tracking capability, particularly of candidates for potential cloaked vessels. While it still cannot detect a cloaked vessel, it is an upgrade which potentially can flag locations of possible conventionally cloaked vessels. Testing is ongoing, this upgraded has the potential to eventually allow for accurate detection of cloaked vessels -- though this has not yet been achieved.

In addition the system is designed to provide accurate tracking of temporal and subspace anomalies even those which are otherwise beyond conventional detection. Testing of a pallet element within the [[Schatten Star System]] showed faster detection, tracking, and tracking range of subspace anomalies.

== Enhanced Processing ==
Each pallet element is equipped with an isolinear and bioneural processing core. These cores are the first stage signal processing which the network of pallet elements feed into the array ECC core for coordination. The ECC core provides intelligent signal processing to feed directly into a facilities main computer. The sensors provide too much data for a computer core to process in real time, so the first stage processing does initial pattern matching and organization of data while the second stage ECC further processes the data to provide a central core with meaningful and actionable information.

The ECC in the 2nd stage coordinates the first stage processing based on the needs determined by the central core and operations officer or MASI. This multi-stage processing allows the sensors to have a 123.89% total processing efficiency during normal operations. Raw sensor data is still available from the each stage should it be required.

== Calibration ==
The system automatically recalibrates itself on a per-array basis at the 2nd stage ECC processors. The processors will use active emitters and known stellar phenomena to automatically calibrate themselves over time, flagging potential problems for the operations officer.

[[Category:Advanced Technology]]