diff --git a/docs/source/users-manual/about.md b/docs/source/users-manual/about.md new file mode 100644 index 00000000..b1205345 --- /dev/null +++ b/docs/source/users-manual/about.md @@ -0,0 +1,47 @@ +# About This Manual + +## Purpose + +This document is intended to serve the needs of all users of NGPS including astronomers and observatory support staff. + +## Scope + +This document contains practical information related to the operation, maintenance, and troubleshooting of NGPS. + +## Reference Documents + +1. [NGPS Technical Specifications](https://caltech.sharepoint.com/:w:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Systems%20Engineering%20%5BL2%5D/NGPS%20-%20User%27s%20Manual%20and%20Spec%20Sheet/NGPS%20Technical%20Specifications.docx?d=wf25246f6f4fe44ffb063d15639b0c222&csf=1&web=1&e=UcVdNO) (NGPS.SYS.TEC.005) +2. [NGPS Spare Parts List.xlsx](https://caltech.sharepoint.com/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Systems%20Engineering%20%5BL2%5D/NGPS%20Spare%20Parts%20List.xlsx?web=1) (NGPS.SYS.TEC.003) + +## Change Record + +| Revision | Date | Section | Modifications | +| --- | --- | --- | --- | +| Ver 01 | 5/7/2026 | All | NGPS Development Team, initial draft shared at Operations Handover Review | +| Ver 02, SP Ver (300.0) | 7/31/2026 | All | Released in response to OHR reviewers report actions | + +## Abbreviations, Definitions and Nomenclature + +### Acronyms + +| Acronym | Meaning | +| --- | --- | +| AO | Adaptive Optics | +| COO | Caltech Optical Observatories | +| DRP | Data Reduction Pipeline | +| ETC | Exposure Time Calculator | +| FITS | Flexible Image Transport System | +| FOV | Field of View | +| GUI | Graphical User Interface | +| ICS | Instrument Control Software | +| NGPS | Next Generation Palomar Spectrograph | +| OTM | Observation Timeline Modeler | +| POMO | Palomar Observatory Mountain Operation | +| RD | Reference Document of any kind, typically cited outside of requirements text | +| SNR | Signal to Noise Ratio | +| TCS | Telescope Control System | +| TLE | Target List Editor | + +## NGPS Overview + +Next Generation Palomar Spectrograph (NGPS) is conceived to be a radically more efficient workhorse spectrograph, replacing the 1970s-era Double Spectrograph (DBSP). NGPS achieves these gains via 1) increased optical efficiency from superior design and grating components, 2) a novel focal plane slicer unit that captures most traditional slit losses, 3) increased operational efficiency due to broad spectral coverage with fixed grating format and a minimal set of user-selectable settings, and 4) improved scheduling and observing tools, and feedback. diff --git a/docs/source/users-manual/acquisition-and-guiding.md b/docs/source/users-manual/acquisition-and-guiding.md index 55b8a7e7..e39e1697 100644 --- a/docs/source/users-manual/acquisition-and-guiding.md +++ b/docs/source/users-manual/acquisition-and-guiding.md @@ -1,151 +1,147 @@ -# Acquisition and Guiding GUIs +# Acquisition and Guiding ## ACAM and Slice Viewer GUIs -The Acquisition & Guide Camera (ACAM) and the Slice Viewing Cameras (SCAM) have similar GUIs that allow us to monitor what these systems are seeing in real time. A few camera settings can also be adjusted here. The ACAM and SCAM do not require these GUIs to function, so closing or resetting the GUIs will not interrupt the operation of either system. Icons to start or kill the GUIs are found on the desktop: +The Acquisition & Guide Camera (ACAM) and the Slice Viewing Cameras (SCAM) have similar GUIs that allow us to monitor what these systems are seeing in real time. A few camera settings can also be adjusted here. The ACAM and SCAM do not require these GUIs to function, so closing or resetting the GUIs will **not** interrupt the operation of either system. Icons to start or kill the GUIs are found on the desktop: -A kill ds9 GUIs icon is provided in case you lose track of the window locations across multiple VNC desktops or in case a window freezes. - -Seasoned astronomers will notice that the GUIs are based on SAOImage ds9, a popular FITS image visualization tool. Most of the familiar ds9 menu bar functions and tools are available, and additional buttons specific to ACAM and SCAM are found on the bottom 2 rows of the button panel. For help using built-in ds9 functionality, please see the ds9 manual. Both GUIs also have a gui help button on the button panel for brief descriptions of the new buttons. - -```{figure} assets/page_020_image_01.png +```{figure} assets/acquisition-and-guiding-01.png :alt: NGPS manual figure :width: 90% ``` -### Viewing and working with images - -Users are free to change the zoom, scale, and color settings in either GUI to get a better look at objects. However, we do not recommend “working” with images in these GUIs, e.g. adding extra frames, drawing regions, or attempting analysis. This can lead to unpredictable results as the GUIs continuously update with new images. If you find either GUI in a strange display state, try correcting it with sync gui on the button panel. Otherwise, try restarting the GUI (does not affect camera operation). - -To work with FITS images, use the grab fits button on either GUI. The SCAM will prompt you to first specify one of the 2 slice cameras. An independent ds9 window will pop up with a copy of the current FITS image, which is also saved to the current data directory under acam/ or slicecam/. Repeated clicks of grab fits will add frames to the new display. You can play with FITS images in this window and use all ds9 functionality without interruption. - -To continuously save FITS images from ACAM, use the save series button. From the pop-up menu, choose an integer N for how often to save (every Nth frame), then select START from the drop-down menu, then click OK. To stop saving images, return to this menu, select STOP from the drop-down, then click OK. Images are saved to /data/YYYYMMDD/acam/. +A **kill ds9 GUIs** icon is provided in case you lose track of the window locations across multiple VNC desktops or in case a window freezes. -The grab header button displays the FITS header data for the current image (does not update in real time). To view headers in grabbed images, use File > Header as usual for ds9. +Seasoned astronomers will notice that the GUIs are based on SAOImage ds9, a popular FITS image visualization tool. Most of the familiar ds9 menu bar functions and tools are available, and additional buttons specific to ACAM and SCAM are found on the bottom 2 rows of the button panel. For help using built-in ds9 functionality, please see the [ds9 manual](https://ds9.si.edu/doc/ref/index.html). Both GUIs also have a **gui help** button on the button panel for brief descriptions of the new buttons. -```{figure} assets/page_021_image_01.png +```{figure} assets/acquisition-and-guiding-02.png :alt: NGPS manual figure :width: 90% ``` -```{figure} assets/page_021_image_02.png +```{figure} assets/acquisition-and-guiding-03.png :alt: NGPS manual figure :width: 90% ``` -```{figure} assets/page_021_image_03.png +### Viewing and working with images + +Users are free to change the zoom, scale, and color settings in either GUI to get a better look at objects. **However, we do not recommend "working" with images in these GUIs, e.g. adding extra frames, drawing regions, or attempting analysis.** This can lead to unpredictable results as the GUIs continuously update with new images. If you find either GUI in a strange display state, try correcting it with **sync gui** on the button panel. Otherwise, try restarting the GUI (does not affect camera operation). + +To work with FITS images, use the **grab fits** button on either GUI. The SCAM will prompt you to first specify one of the 2 slice cameras. An independent ds9 window will pop up with a copy of the current FITS image, which is also saved to the current data directory under acam/ or slicecam/. Repeated clicks of **grab fits** will add frames to the new display. You can play with FITS images in this window and use all ds9 functionality without interruption. + +To continuously save FITS images from ACAM, use the **save series** button. From the pop-up menu, choose an integer N for how often to save (every Nth frame), then select START from the drop-down menu, then click OK. To stop saving images, return to this menu, select STOP from the drop-down, then click OK. Images are saved to /data/YYYYMMDD/acam/. + +```{figure} assets/acquisition-and-guiding-04.png :alt: NGPS manual figure :width: 90% ``` +The **grab header** button displays the FITS header data for the current image (does not update in real time). To view headers in grabbed images, use File > Header as usual for ds9. + ### Getting oriented The upper display sections of the ACAM and SCAM GUIs show the approximate celestial coordinates of the green crosshairs. These are guesses that have not yet been refined by the astrometric solver, thus there may be absolute errors of up to several arcsec. Relative distances and orientations between 2 points in the image are more reliable. -The ACAM field of view (FOV) is offset from the slit by about 8 arcmin, so we do not expect to see our target in the ACAM GUI during typical acquisition and guiding. The 30” scale marker at the image center shows the orientation of the slit but not its true location. The show slit button will zoom out to reveal a marker at the TCS pointing coordinates, which is close to the slit’s true location, well outside the ACAM FOV. To recover the default display, click sync gui. - -The SCAM GUI displays a FOV to either side of the slicer. Of course, the physical locations of the slit and slices are somewhere between the 2 images; however, the width and position of the gap between the images is not displayed accurately in this window. Do not trust the displayed gap as a reference for where sources are relative to the slit, e.g. to judge target centering. - -A “virtual slit” graphic is displayed to aid manual target acquisition. A scale marker is also displayed on the left. +The ACAM field of view (FOV) is offset from the slit by about 8 arcmin, so we do not expect to see our target in the ACAM GUI during typical acquisition and guiding. The 30" scale marker at the image center shows the orientation of the slit but not its true location. The **show slit** button will zoom out to reveal a marker at the TCS pointing coordinates, which is close to the slit's true location, well outside the ACAM FOV. To recover the default display, click **sync gui**. -```{figure} assets/page_022_image_01.png +```{figure} assets/acquisition-and-guiding-05.png :alt: NGPS manual figure :width: 90% ``` -### Changing camera settings - -Both GUIs have a camera settings button for changing image acquisition settings on the cameras themselves. Keep in mind that the acquisition and guide functions of NGPS are affected by these settings. For instance, if you increase the ACAM exposure time to get a better look at a faint galaxy, all the stars in the FOV may saturate, making guiding impossible. In other words, the acquisition and guide system is seeing what you’re seeing. You may want to experiment with camera settings if the system is struggling to provide stable guiding. Changing settings while guiding may disrupt guiding. - -The camera settings button on either GUI opens a window with options to set the exposure time and the electron multiplying (EM) gain. Rather than displaying each exposure, you can view a Rolling Average of the latest N frames by setting N>1, which can be useful for stabilizing the image in unstable seeing conditions. To reset the averaged image stack, make sure the checkbox is checked before clicking OK. +The SCAM GUI displays a FOV to either side of the slicer. Of course, the physical locations of the slit and slices are somewhere between the 2 images; however, the width and position of the gap between the images is not displayed accurately in this window. **Do not trust the displayed gap** as a reference for where sources are relative to the slit, e.g. to judge target centering. -The Binning option on SCAM sets the cameras’ on-chip binning feature, which can reduce noise and improve clarity. A good default is 4x4 pixel binning since the PSF is large relative to SCAM pixels. After changing binning, click sync gui on the main button panel to reset the zoom for the new pixel scale. +A "virtual slit" graphic is displayed to aid manual target acquisition. A scale marker is also displayed on the left. -The ACAM Filter drop down menu on ACAM will move the ACAM filter wheel to the selected filter. After clicking OK, it will take several seconds for the wheel to change positions, and you may notice shadows on the images while the wheel is moving. Again, be aware that filter selection will affect the acquisition and guide performance. It also affects measurements of sky conditions (seeing, sky background, extinction) available in telemetry logging since these come from ACAM images. - -### Focus - -The focus button on the ACAM GUI allows for manually changing the focus of the P200 telescope, which affects the focus in ACAM, SCAM, and spectrograph images. Enter a new focus position in the pop-up menu and click OK. An audible “ding” should be heard in the P200 control room when the new focus position is reached. - -### Manual offsetting +### Changing camera settings -On the SCAM GUI, a set of jog buttons (left, right, up, down) are provided for fast manual adjustment (offsets) of the TCS pointing. If these buttons are used while stably guiding, the system will continue guiding at the resulting position as long as the offsets are kept small (<10”).. By default (unless someone has messed with the ds9 display options), a source on SCAM will appear to move in the direction of the button name, i.e. left will move the source to the left in the image. Sources on ACAM will move slightly differently since the camera orientations are not aligned. Use the scale marker in the ACAM center as a reference for the slit orientation. +Both GUIs have a **camera settings** button for changing image acquisition settings on the cameras themselves. Keep in mind that **the acquisition and guide functions of NGPS are affected by these settings**. For instance, if you increase the ACAM exposure time to get a better look at a faint galaxy, all the stars in the FOV may saturate, making guiding impossible. In other words, the acquisition and guide system is seeing what you're seeing. You may want to experiment with camera settings if the system is struggling to provide stable guiding. Changing settings while guiding may disrupt guiding. -```{figure} assets/page_023_image_01.png +```{figure} assets/acquisition-and-guiding-06.png :alt: NGPS manual figure :width: 90% ``` -```{figure} assets/page_023_image_02.png +```{figure} assets/acquisition-and-guiding-07.png :alt: NGPS manual figure :width: 90% ``` -Use the jog settings button to adjust the offset size of a single jog button click. The value in arcsec refers to a great circle distance, not a coordinate change, so images should appear to move by the same amount regardless of the original TCS pointing. +The **camera settings** button on either GUI opens a window with options to set the exposure time and the electron multiplying (EM) gain. Rather than displaying each exposure, you can view a Rolling Average of the latest N frames by setting N>1, which can be useful for stabilizing the image in unstable seeing conditions. To reset the averaged image stack, make sure the checkbox is checked before clicking OK. -We can also use the green crosshairs to move objects to and from the slit. On the SCAM GUI, click the center of your target so that it aligns with the green crosshairs. You may want to zoom in or change other display settings to get more precision. Clicking the put on slit button will offset the TCS to align the target with the SCAM virtual slit marker, which is the correct position before exposing a spectrum. Click the target again and repeat the process as needed to improve alignment with the virtual slit. +The **Binning** option on SCAM sets the cameras' on-chip binning feature, which can reduce noise and improve clarity. A good default is 4x4 pixel binning since the PSF is large relative to SCAM pixels. After changing binning, click **sync gui** on the main button panel to reset the zoom for the new pixel scale. -There is a similar put on slit button on the ACAM GUI that will offset a target from the ACAM crosshairs to the virtual slit on the SCAM, which will take a few seconds. Once it is visible on SCAM, use SCAM controls to adjust the position further. There is also a put on guider button on SCAM which will offset a target from the SCAM crosshairs to the ACAM (target will appear near the center scale marker). This can be useful for inspecting the local environment of the target using the larger ACAM FOV. +The **ACAM Filter** drop down menu on ACAM will move the ACAM filter wheel to the selected filter. After clicking OK, it will take several seconds for the wheel to change positions, and you may notice shadows on the images while the wheel is moving. Again, be aware that filter selection will affect the acquisition and guide performance. It also affects measurements of sky conditions (seeing, sky background, extinction) available in telemetry logging since these come from ACAM images. -Note that the jog buttons and “put on slit” buttons use open loop TCS offsets, which are not precise. Do not expect perfect, repeatable motions, and do not use these buttons for quantitative analysis. +### Focus -### Manual guiding and acquisition +The **focus** button on the ACAM GUI allows for manually changing the focus of the P200 telescope, which affects the focus in ACAM, SCAM, and spectrograph images. Enter a new focus position in the pop-up menu and click OK. An audible "ding" should be heard in the P200 control room when the new focus position is reached. -The user can manually initiate guiding using the guide button on ACAM. This will pop up a menu: +### Manual offsetting -The simplest option is to check the Guide Here box. After clicking OK, the ACAM system will enter guide mode, attempting to stabilize the current pointing using the ACAM FOV as a reference. The RA and DEC fields will be ignored. +On the SCAM GUI, a set of jog buttons (**left, right, up, down**) are provided for fast manual adjustment (offsets) of the TCS pointing. If these buttons are used while stably guiding, the system will continue guiding at the resulting position as long as the offsets are kept small (<10"). By default (unless someone has messed with the ds9 display options), a source on SCAM will appear to move in the direction of the button name, i.e. **left** will move the source to the left in the image. Sources on ACAM will move slightly differently since the camera orientations are not aligned. Use the scale marker in the ACAM center as a reference for the slit orientation. -With the box unchecked, the system will attempt to acquire the target (put it on the slit) specified by RA and DEC. Coordinates may be specified in decimal degrees, or HH:MM:SS.s format. The TCS pointing will be changed via offsetting, not slewing, so it does not require operator approval. The target must be within the offsetting range of the current TCS pointing (<6000”). After successful acquisition, the ACAM will switch to guiding mode. +Use the **jog settings** button to adjust the offset size of a single jog button click. The value in arcsec refers to a great circle distance, not a coordinate change, so images should appear to move by the same amount regardless of the original TCS pointing. -Remember that the TCS slew coordinates are not the same as the coordinates of the target to be acquired. There is an offset between the slit and the TCS that is already accounted for when sending coordinates to the operator via the main NGPS GUI. When a target is properly centered on the slit, it would be incorrect to record the RA and DEC of the TCS and enter them in the ACAM guide menu, expecting to re-acquire the target. +We can also use the green crosshairs to move objects to and from the slit. On the SCAM GUI, click the center of your target so that it aligns with the green crosshairs. You may want to zoom in or change other display settings to get more precision. Clicking the **put on slit** button will offset the TCS to align the target with the SCAM virtual slit marker, which is the correct position before exposing a spectrum. Click the target again and repeat the process as needed to improve alignment with the virtual slit. -A convenient feature is the acquire last slew button on SCAM. This will first reset the TCS pointing to the last coordinates that the operator used to slew (does nothing if the slew has just completed). Then guiding will begin in that position. This mode assumes the last slew intended to put a target on the slit. It tries to match the slit to the intended target coordinates rather than match the TCS pointing to the slew coordinates. +There is a similar **put on slit** button on the ACAM GUI that will offset a target from the ACAM crosshairs to the virtual slit on the SCAM, which will take a few seconds. Once it is visible on SCAM, use SCAM controls to adjust the position further. There is also a **put on guider** button on SCAM which will offset a target from the SCAM crosshairs to the ACAM (target will appear near the center scale marker). This can be useful for inspecting the local environment of the target using the larger ACAM FOV. -Stop guiding at any time by clicking stop guiding on the ACAM button panel. Remember that the SCAM jog buttons can be used to adjust pointing without interrupting guiding. +```{note} +The jog buttons and "put on slit" buttons use open loop TCS offsets, which are not precise. Do not expect perfect, repeatable motions, and do not use these buttons for quantitative analysis. +``` -### Troubleshooting +### Manual guiding and acquisition -The status of the Acquisition and Guide system is displayed at the top of the ACAM image as either “STANDBY”, “ACQUIRING”, or “GUIDING”. In poor observing conditions, the system may consistently or intermittently drop into the “STANDBY” state, meaning it is failing to obtain decent images for guiding. Acquisition and guiding is performed by continuously finding an astrometric solution to the ACAM FOV, not by tracking individual stars. ACAM requires a minimum of 4 stars (good signal to noise, unsaturated) in its FOV. More is typically better, unless there happens to be a large, bright stellar cluster in the FOV. +The user can manually initiate guiding using the **guide** button on ACAM. This will pop up a menu: -Steps you can take to improve A&G performance: +```{figure} assets/acquisition-and-guiding-08.png +:alt: NGPS manual figure +:width: 90% -1. Increase the ACAM exposure time to boost the number of detectable stars. This also slows +``` -down the guiding feedback loop. +The simplest option is to check the **Guide Here** box. After clicking OK, the ACAM system will enter guide mode, attempting to stabilize the current pointing using the ACAM FOV as a reference. The RA and DEC fields will be ignored. -2. Increase the ACAM Rolling Average to an integer > 1. This is useful when unstable seeing +With the box unchecked, the system will attempt to acquire the target (put it on the slit) specified by RA and DEC. Coordinates may be specified in decimal degrees, or HH:MM:SS.s format. The TCS pointing will be changed via offsetting, not slewing, so it does not require operator approval. The target must be within the offsetting range of the current TCS pointing (<6000"). After successful acquisition, the ACAM will switch to guiding mode. -causes sources to appear to bounce around. +**Remember that the TCS slew coordinates are not the same as the coordinates of the target to be acquired**. There is an offset between the slit and the TCS that is already accounted for when sending coordinates to the operator via the main NGPS GUI. When a target is properly centered on the slit, it would be *incorrect* to record the RA and DEC of the TCS and enter them in the ACAM **guide** menu, expecting to re-acquire the target. -3. Change the ACAM filter. Although the “clear” filter will have the largest PSF, it may have the +A convenient feature is the **acquire last slew** button on SCAM. This will first reset the TCS pointing to the last coordinates that the operator used to slew (does nothing if the slew has just completed). Then guiding will begin in that position. This mode assumes the last slew intended to put a target on the slit. It tries to match the slit to the intended target coordinates rather than match the TCS pointing to the slew coordinates. -best SNR in poor observing conditions. The “r” filter is the recommended default. +Stop guiding at any time by clicking **stop guiding** on the ACAM button panel. Remember that the SCAM jog buttons can be used to adjust pointing without interrupting guiding. -```{figure} assets/page_025_image_01.png -:alt: NGPS manual figure -:width: 90% +### Troubleshooting -``` +The status of the Acquisition and Guide system is displayed at the top of the ACAM image as either "STANDBY", "ACQUIRING", or "GUIDING". In poor observing conditions, the system may consistently or intermittently drop into the "STANDBY" state, meaning it is failing to obtain decent images for guiding. Acquisition and guiding is performed by continuously finding an astrometric solution to the ACAM FOV, not by tracking individual stars. ACAM requires a minimum of 4 stars (good signal to noise, unsaturated) in its FOV. More is typically better, unless there happens to be a large, bright stellar cluster in the FOV. -4. Change the slit angle (a.k.a. change the P200 CASS angle), which will change what stars are +Steps you can take to improve A&G performance: -visible in the ACAM field. If this is done via the Target List’s slit angle value, the pointing coordinates transmitted to the P200 will be adjusted to keep the target on the slit. A 180º rotation is a natural first choice given the symmetry of the slit, but any angle may help. +1. Increase the ACAM exposure time to boost the number of detectable stars. This also slows down the guiding feedback loop. +2. Increase the ACAM Rolling Average to an integer > 1. This is useful when unstable seeing causes sources to appear to bounce around. +3. Change the ACAM filter. Although the "clear" filter will have the largest PSF, it may have the best SNR in poor observing conditions. The "r" filter is the recommended default. +4. Change the slit angle (a.k.a. change the P200 CASS angle), which will change what stars are visible in the ACAM field. If this is done via the Target List's slit angle value, the pointing coordinates transmitted to the P200 will be adjusted to keep the target on the slit. A 180º rotation is a natural first choice given the symmetry of the slit, but any angle may help. +5. If guiding is severely unstable, it may be preferable to skip guiding completely and rely on the P200 tracking stability (do nothing). Try using the crosshairs or **grab fits** features on the ACAM or SCAM GUI to monitor long term drift. If you notice a drift, use the SCAM jog buttons to manually correct the pointing. -5. If guiding is severely unstable, it may be preferable to skip guiding completely and rely on the +```{note} +Remember that any changes made to camera settings may need to be reset once conditions improve. +``` -P200 tracking stability (do nothing). Try using the crosshairs or grab fits features on the ACAM or SCAM GUI to monitor long term drift. If you notice a drift, use the SCAM jog buttons to manually correct the pointing. +## On-Target GUI -Remember that any changes made to camera setting may need to be reset once conditions improve, +```{figure} assets/acquisition-and-guiding-09.png +:alt: NGPS manual figure +:width: 90% -## On-Target GUI +``` -A small, one-button indicator GUI runs on a separate VNC desktop that is intended solely for use by the TCS operator. Policy decisions require a human to point the telescope and inform NGPS when the telescope is on target. “On target” does not simply indicate that the telescope is pointed at the requested coordinates; rather, on target specifically means “ready to observe” and includes factors which currently have no source of remote telemetry including dome shutter in correct position, etc. +A small, one-button indicator GUI runs on a separate VNC desktop that is intended solely for use by the TCS operator. Policy decisions require a human to point the telescope and inform NGPS when the telescope is on target. "On target" does not simply indicate that the telescope is pointed at the requested coordinates; rather, on target specifically means "ready to observe" and includes factors which currently have no source of remote telemetry including dome shutter in correct position, etc. Although NGPS automatically sends the target coordinates to the TCS, the TCS Operator must perform the actual move; the instrument control software merely provides the coordinates. The expected policy for NGPS to achieve the best possible throughput is that whenever the TCS operator receives coordinates, they are to immediately initiate the slew. After NGPS requests a telescope slew, it signals the On Target GUI to activate its button, and the observing sequence is in a holding pattern until the TCS operator makes the determination that the telescope is on target and ready to observe. Once the TCS Operator clicks on the on-target button, a signal is sent to NGPS allowing it to continue; the on-target button deactivates until the next slew request. diff --git a/docs/source/users-manual/acquisition-calibration-hardware.md b/docs/source/users-manual/acquisition-calibration-hardware.md index 47ecf8be..b770a2e1 100644 --- a/docs/source/users-manual/acquisition-calibration-hardware.md +++ b/docs/source/users-manual/acquisition-calibration-hardware.md @@ -1,12 +1,12 @@ -# Acquisition, Calibration, and Slice Viewing Hardware +# Acquisition and Calibration Hardware ## Acquisition and Guidance System -The acquisition and guidance system is an imager (offset approximately 8’) from the spectrograph optical axis. It has its own enclosure with a dedicated hatch (currently broken). A fold mirror redirects the light horizontally through a field lens and, subsequently, a fixed focusing lens. In the backfocal space between the lens and camera is a filter wheel with 6 positions. These are populated with 50 mm diameter filters: (g’, r’, I, blocking, clear, and empty). The clear filter is an AR coated piece of glass that maintains the same focus as the color filters. +The acquisition and guidance system is an imager (offset approximately 8') from the spectrograph optical axis. It has its own enclosure with a dedicated hatch (currently broken). A fold mirror redirects the light horizontally through a field lens and, subsequently, a fixed focusing lens. In the backfocal space between the lens and camera is a filter wheel with 6 positions. These are populated with 50 mm diameter filters: (g', r', I, blocking, clear, and empty). The clear filter is an AR coated piece of glass that maintains the same focus as the color filters. The camera was shimmed in lab to be confocal with the image slicer. There is no focus adjustment on this camera. -Both the filter wheel and the hatch are custom mechanisms, but both are driven by PI C-663.12 controllers. The hatch has an ST2818M0704-G2 stepper motor and JK8002C hall effect limit switches. The filter wheel also uses an ST2818M0704-G2 stepper motor and a JK8002C hall effect home switch. The A&G electronics are further detailed in the Electronic control instructions for NGPS A&G system document. +Both the filter wheel and the hatch are custom mechanisms, but both are driven by PI C-663.12 controllers. The hatch has an ST2818M0704-G2 stepper motor and JK8002C hall effect limit switches. The filter wheel also uses an ST2818M0704-G2 stepper motor and a JK8002C hall effect home switch. The A&G electronics are further detailed in the [Electronic control instructions for NGPS A&G system document](https://caltech.sharepoint.com/:w:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/A%26G%20System%20%5BAGS%5D/A%26G%20System%20-%20TECs/Electronic%20control%20instructions%20for%20NGPS%20A%26G%20system.docx?d=we90f09516f6d4099871aebd1cc87ab70&csf=1&web=1&e=iP5UMi). There are two cover panels on top of the A&G system. One of the panels has the hatch attached to it and there are wires installed on the underside. While this panel can be unbolted and lifted, care needs to be exercised when doing so to avoid accidentally stretching the conductors. There is no internal disconnect to completely free this panel. The other panel, that immediately above the camera and filter wheel, can be easily removed. @@ -18,57 +18,42 @@ The A&G system is served by the acam daemon and the ACAM GUI. The calibration unit provides the light sources and means to illuminate the NGPS slicer with light needed for spectral and flat-field calibration. The optics are designed to mimic the Hale Telescope f/16 focal ratio. -```{figure} assets/page_052_image_01.png -:alt: NGPS manual figure -:width: 90% - -``` - The calibration system is composed of two sections. -The first is a reimaging unit that is mounted on the NGPS slicer assembly. That contains an entrance aperture equipped with a light-blocking door, reimaging optics and diffuser. This section also includes the actuated instrument cover. The terms ‘door’ and ‘cover’ here are deliberate, and explicitly identify the actuator in the instrument control software. We recommend the instrument cover be closed whenever the instrument is not in use. Both axes are driven by PI L-220.50DG high-resolution linear actuators commanded by PI C-863.12 controllers. - -Figure 14: Alos Blort. +The first is a reimaging unit that is mounted on the NGPS slicer assembly. That contains an entrance aperture equipped with a light-blocking **door**, reimaging optics and diffuser. This section also includes the actuated instrument **cover**. The terms "**door**" and "**cover**" here are deliberate, and explicitly identify the actuator in the instrument control software. We recommend the instrument cover be closed whenever the instrument is not in use. Both axes are driven by PI L-220.50DG high-resolution linear actuators commanded by PI C-863.12 controllers. -The second is the calibration shelf in the electronics cabinet. This contains the light sources, their power supplies, and shutters. - -INCLUDE (ROUGHLY) LABELED PHOTO OF CALIBRATION UNIT SHELF Figure XX - -The two components are connected by an optical fiber harness (an octopus). Each lamp has a single multimode fiber attached to it. The continuum lamp paths then travel through adjustable fiber attenuators. The parallel paths then continue to a MIXING DEVICE, and terminate at the calibration box near the focal plane. - -INCLUDE DIAGRAM OF CAL LIGHT PATH Figure XX - -```{figure} assets/page_053_image_01.png +```{figure} assets/acquisition-calibration-hardware-01.jpg :alt: NGPS manual figure :width: 90% - ``` +The second is the calibration shelf in the electronics cabinet. This contains the light sources, their power supplies, and shutters. + +The two components are connected by an optical fiber harness (an octopus). Each lamp has a single multimode fiber attached to it. The continuum lamp paths then travel through adjustable fiber attenuators. The parallel paths then continue to a homogenizing rod and terminate at the calibration box near the focal plane. + Note that the instrument hatch is actually part of the calibration enclosure and is controlled by the calibd software daemon. -The calibration system is served by the calibd daemon +The calibration system is served by the calibd daemon. ### Spectral Calibration Sources -NGPS uses thorium argon (ThAr) and iron argon (FeAr) hollow cathode arc lamps. Each is in its own enclosure and is powered a dedicated Photron P209-USB power supply. +NGPS uses thorium argon (ThAr) and iron argon (FeAr) hollow cathode arc lamps. Each is in its own enclosure and is powered by a dedicated Photron P209-USB power supply. -The current (Apr 2026) ThAr lamp is a: Green Scientific G858A hollow cathode lamp The current (Apr 2026) FeAr lamp is a: Photron P826A hollow cathode lamp +The current (Apr 2026) ThAr lamp is a Green Scientific G858A hollow cathode lamp. The current (Apr 2026) FeAr lamp is a Photron P826A hollow cathode lamp. Notes: -It is enough to turn the power on to the two lamps for them to turn on. There are rocker switches on the photron supplies if power needs to be cut locally. +It is enough to turn the power on to the two lamps for them to turn on. There are rocker switches on the Photron supplies if power needs to be cut locally. -Lifetime of the lamps varies a bit and depends on the implementation, usage details, etc. We anticipate a lifetime of about 2 years. The lamp enclosures are designed to be serviceable with the removal of just one of the four electronics cabinet covers (cover X-X) +Lifetime of the lamps varies a bit and depends on the implementation, usage details, etc. We anticipate a lifetime of about 2 years. The lamp enclosures are designed to be serviceable with the removal of just one of the four electronics cabinet covers. ThAr lamps (as of this writing, Apr 2026) are somewhat difficult to source. -INCLUDE A ZOOM ON THE TWO LAMP BOXES INCLUDE PHOTO OF A BULB Figure XX - ### Flatfield Calibration Sources -NGPS has two continuum sources. A tungsten-halogen lamp (Red lamp) from Thorlabs (model #SLS301) and Enegetiq Laser Line Source (Blue lamp, model #EQ-99X LDLS). Each lamp has beam splitter optics at the front that separate the light path to a direct and sent part of the light through an etalon. The etalon produces a periodic spectrum, whereas the direct path is a clean continuum. The two paths each have an independent shutter. +NGPS has two continuum sources. A tungsten-halogen lamp (Red lamp) from Thorlabs (model #SLS301) and Energetiq Laser Line Source (Blue lamp, model #EQ-99X LDLS). Each lamp has beam splitter optics at the front that separate the light path, sending part of the light directly and part through an etalon. The etalon produces a periodic spectrum, whereas the direct path is a clean continuum. The two paths each have an independent shutter. -The lamps also have dDichroic beam splitters for their spectra to interleave. +The lamps also have dichroic beam splitters for their spectra to interleave. We have also implemented, but do not currently use, optical paths for the continuum lamp light to pass through etalons generating periodic spectra. The intent was to use these spectra for concurrent calibration (light injected via optics-coupled fibers at the edges of the slit and slices). The functionality is available, and we may implement this in the future. @@ -76,47 +61,44 @@ Notes: The Red continuum lamp turns on when the appropriate outlet in the NPS is powered. There is a rocker switch on its enclosure to cut power locally. -The blue continuum lamp needs an interlock to turn on. There is a control box with NGPS equipment in the instrument bay. We have implemented, but not yet deployed computer control of this lamp. More information can be found here. +The blue continuum lamp needs an interlock to turn on. There is a control box with NGPS equipment in the instrument bay. We have implemented, but not yet deployed, computer control of this lamp. More information can be found [here](https://caltech.sharepoint.com/:w:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/Electronics%20Rack%20%5BEL%5D/Electronics%20Rack%20-%20TECs/Calibration%20Lamps/Blue%20Continuum%20Remote%20Control.docx?d=w422074f72fd14c4a98ba98440f8a990f&csf=1&web=1&e=Nf5Odd). -Unfortunately, the calibration system optical throughput is very low at wavelengths shorter than about 350 nm (due to mirror coatings and multiple reflections, most likely), so the utility of the Blue lamp is limited. As of Apr 2026, we have procured some bright UV LEDs and will attempt to construct a pseudo- continuum source to overcome the reduced throughput. This work is ongoing. +Unfortunately, the calibration system optical throughput is very low at wavelengths shorter than about 350 nm (due to mirror coatings and multiple reflections, most likely), so the utility of the Blue lamp is limited. As of Apr 2026, we have procured some bright UV LEDs and will attempt to construct a pseudo-continuum source to overcome the reduced throughput. This work is ongoing. The short-pass filter installed in the Blue lamp has some leak that can be seen in the R and I channel data. -Blue Lamp images To Be Added Figure XX - -Red Lamp images To Be Added Figure XX - -Blue Lamp leak images To Be Added Figure XX - ### Calibration Shutters (AKA Modulators) -There are 6 modulators installed in the calibration system, one per lamp. The assignment is shown in the table below. These can function as bona-fide shutters, or to limit the lamp duty cycle mechanically. These modulators are Takano BOS10-15 bi-stable rotary optical shutters and are controlled by an Arduino Teensy 4.1. The arduino embedded code (NGPS_Mods_V006_quiet.ino) can be found here (in SharePoint > NGPS - Subsystems [L3] > Electronics Rack [EL] > Electronics Rack -TECs > Calibration Lamps > Modulators ). +There are 6 modulators installed in the calibration system, one per lamp. The assignment is shown in the table below. These can function as bona-fide shutters, or to limit the lamp duty cycle mechanically. These modulators are Takano BOS10-15 bi-stable rotary optical shutters and are controlled by an Arduino Teensy 4.1. The arduino embedded code (NGPS_Mods_V006_quiet.ino) can be found [here](https://caltech.sharepoint.com/:f:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/Electronics%20Rack%20%5BEL%5D/Electronics%20Rack%20-%20TECs/Calibration%20Lamps/Modulators?csf=1&web=1&e=27YsZC) (in SharePoint > NGPS - Subsystems [L3] > Electronics Rack [EL] > Electronics Rack -TECs > Calibration Lamps > Modulators). Notes: The modulators are very sensitive to the mounting torque of the screws that hold them in place. Best to have these operating as you install, if possible. -One of the modulators (#2, for blue continuum etalon). is sticky; it is rarely, if ever, used. +One of the modulators (#2, for blue continuum etalon) is sticky; it is rarely, if ever, used. -Modulator # Lamp +| Modulator # | Lamp | +|---|---| +| 1 | FeAr | +| 2 | Blue Continuum Etalon (flaky) | +| 3 | Red Continuum Etalon | +| 4 | Red Continuum Direct | +| 5 | Blue Continuum | +| 6 | ThAr | -### Taking a calibration image +### Taking a Calibration Image by Hand Users should not need to do this, but it is included here for engineering purposes: -1) Ensure shutter is enabled in camerad and appropriate exposure time is set - -2) Close the instrument cover - -3) Open the calibration door - -4) Open the modulator for the appropriate lamp - -5) Turn on the appropriate lamp +1. Ensure shutter is enabled in camerad and appropriate exposure time is set +2. Close the instrument cover +3. Open the calibration door +4. Open the modulator for the appropriate lamp +5. Turn on the appropriate lamp ## Slice Viewing System -There are two Andor iXon Ultra 888 EMCCD cameras that pick off the telescope field. The cameras have FOVs of approximately 60” x 30” and plate scale of XX. The fields are adjacent to the outer two slices and, as such, shift as the slit width is adjusted. +There are two Andor iXon Ultra 888 EMCCD cameras that pick off the telescope field. The cameras each have FOVs of approximately 21" x 50" and plate scale of 0.060"/pixel. The fields are adjacent to the outer two slices and, as such, shift as the slit width is adjusted. The cameras are controlled via the SLICEVIEW GUI. 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taken - -NGPS calibrations are tied to the detector binning and slit-width configurations used for science observations. The basic rule is: take arcs and biases for every binning mode used, and take dome flats for every slit-width plus binning combination used. It is generally acceptable to use the same slit widths - -```{figure} assets/page_008_image_01.png +```{figure} assets/calibrations-01.png :alt: NGPS manual figure :width: 90% - ``` -on internal cals as what will later be used for science if the slit width is picked to track typical seeing conditions (2” or narrower). If very wide slits will be used for science, use a narrower slit to take internal cals (so that arc lines can be fit for the wavelength solutions). Configurations that are not used for science or standards do not need to be calibrated. +NGPS calibrations are tied to the detector binning and slit-width configurations used for science observations. The basic rule is: take arcs and biases for every binning mode used, and take dome flats for every slit-width plus binning combination used. It is generally acceptable to use the same slit widths on internal cals as what will later be used for science if the slit width is picked to track typical seeing conditions (2" or narrower). If very wide slits will be used for science, use a narrower slit to take internal cals (so that arc lines can be fit for the wavelength solutions). Configurations that are not used for science or standards do not need to be calibrated. -Calibration observations are executed through the normal NGPS sequencer. Observers should use the GUI to generate calibration target lists for the desired internal calibrations or dome-flat sequences, then run those target lists with Go. Internal calibration target lists are generated for a selected binning mode. Dome-flat target lists are generated for a selected binning mode and slit width. This replaces the older Calibration GUI workflow and the separate getcalib_cf scripts used for long U and G calibrations. +Calibration observations are executed through the normal NGPS sequencer. Observers should use the GUI to generate calibration target lists for the desired internal calibrations or dome-flat sequences, then run those target lists with **Go**. Internal calibration target lists are generated for a selected binning mode. Dome-flat target lists are generated for a selected binning mode and slit width. This replaces the older Calibration GUI workflow and the separate getcalib_cf scripts used for long U and G calibrations. A complete internal calibration set for a binning mode consists of the required arc and bias frames for each active spectrograph channel. The standard requirements are 3 ThAr arcs, 3 FeAr arcs, and 7 bias frames per channel and binning mode. Arc frames should show clear, unsaturated lines. Bias frames should have normal low count levels and no obvious detector problems. Internal flats may be acquired as part of some calibration sequences, but the key required products tracked for wavelength calibration and bias subtraction are the arcs and biases. Dome flats are required for each slit width and binning combination used for science or standards. A complete dome-flat set consists of at least 5 dome flats per channel for each setup (7-10 are preferred for U and G channels). Before taking dome flats, confirm with the Support Astronomer or Telescope Operator that the dome is dark, the telescope and mirror-cover configuration are appropriate, and the high lamp can be turned on. Set the ACAM and SCAM exposure times to zero before using the high lamp. Dome flats should have useful high counts without saturation. -Calibration completeness can be checked from a terminal with the terminal command ngps_cals (this is normally started by SAs and should be already running when observers start taking cals. +Calibration completeness can be checked from a terminal with the terminal command ngps_cals (this is normally started by SAs and should already be running when observers start taking cals). + +ngps_cals opens the NGPS calibration-status display. The top table, "Arcs/Bias by binning," groups internal calibrations by detector binning, listed as BINSPAT x BINSPEC. For each channel, the THAR, FEAR, and BIAS columns show the number of valid frames found compared with the number required. For example, 3/3 means that all required frames of that type are present. The SLITW<=2 columns indicate how many of the arc frames satisfy the slit-width criterion used for wavelength calibration. The SCI column shows how many science frames were found for that channel and binning setup. + +The lower table, "Dome flats by setup," groups dome flats by detector binning and slit width. For each setup and channel, the DOMEFLAT column shows the number of valid dome flats found compared with the required number. Green entries indicate complete calibration sets; red entries indicate missing or incomplete sets. The summary lines give the number of complete setups compared with the number of required setups for each channel. -ngps_cals opens the NGPS calibration-status display shown in Figure 3-1. The top table, “Arcs/Bias by binning,” groups internal calibrations by detector binning, listed as BINSPAT x BINSPEC. For each channel, the THAR, FEAR, and BIAS columns show the number of valid frames found compared with the number required. For example, 3/3 means that all required frames of that type are present. The SLITW<=2 columns indicate how many of the arc frames satisfy the slit-width criterion used for wavelength calibration. The SCI column shows how many science frames were found for that channel and binning setup. +The status display can be left open while calibrations are being taken. If a science setup appears in red, generate and run the missing calibration target list before relying on that configuration for science-quality reductions. If only partial data is missing, the calibration target list can be modified by setting NEXP to 0 for frames that are not needed, and then re-running the calibration list with the **Go** button. If a new binning or slit width is introduced during the night, rerun ngps_cals and obtain the missing calibrations for that setup. -The lower table, “Dome flats by setup,” groups dome flats by detector binning and slit width. For each setup and channel, the DOMEFLAT column shows the number of valid dome flats found compared with the required number. Green entries indicate complete calibration sets; red entries indicate missing or incomplete sets. The summary lines give the number of complete setups compared with the number of required setups for each channel. +## Wavelength Calibration -The status display can be left open while calibrations are being taken. If a science setup appears in red, generate and run the missing calibration target list before relying on that configuration for science-quality reductions. If only partial data is missing, the calibration target list can be modified by setting NEXP to 0 for frames that are not needed, and then re-running the calibration list with the Go button. If a new binning or slit width is introduced during the night, rerun ngps_cals and obtain the missing calibrations for that setup. +The internal NGPS arc lamps provide usable calibration lines only at wavelengths longer than approximately 3500 Å. Consequently, the extrapolated wavelength solution near the blue edge of the U-channel detector, around 3200 Å, may drift by a few Å. -Add example ThAr exposure figure. Discuss. +He dome-lamp exposures can be obtained to anchor the wavelength solution to approximately 3200 Å using the He I 3187 Å line. This line is detected near the blue edge of the **central U-channel slice**. The exposures can be included in the regular dome-flat calibration target list by setting NEXP > 0 for the CAL_DOMEHE entries in the automatically generated calibration target list. Both the automatic quicklook reduction and PypeIt will use these calibration data when they are available. If He dome arcs are obtained, an RMS of < 0.1 Å can be expected at 3200 Å. -Add example FeAr exposure figure. Discuss. +For an accurate wavelength solution to 3200 Å on the **U-channel side slices**, we recommend observing a bright planetary nebula during twilight. The planetary-nebula spectrum provides the same He I 3187 Å line on all slices, allowing the wavelength solution to be anchored independently across the full image slicer. The table below lists suitable planetary nebulae visible from Palomar near the start of the night at different times of year. If the side slices will not be used for science, this data is of course not necessary. -Add example dome flat exposure(s) figure. Discuss. +| Target | RA (J2000) | Dec (J2000) | Approx. evening twilight window | Published He I 3187 detection | +| --- | --- | --- | --- | --- | +| NGC 2392 | 07:29:10.77 | +20:54:42.5 | February-May | He I λ3187 detected; log observed flux = -11.96 (quality c). Aller & Keyes (1980/1981). | +| NGC 6210 | 16:44:29.52 | +23:47:59.4 | June-October | He I λ3187.74 measured directly; reddening-corrected flux ratio I(3187.7)/I(3444.1) = 2.189. O'Dell & Miller (1992). | +| NGC 6818 | 19:43:57.77 | -14:09:13.4 | August-November | Observed at 3187.11 Å and identified as He I λ3187.74; dereddened intensity = 2.20 for Hβ = 100. Tsamis et al. (2003). | +| NGC 7009 | 21:04:10.82 | -11:21:48.6 | September-December | He I λ3187.74 measured directly; observed intensity = 0.742 relative to He I λ4471 = 1. Fang & Liu (2013). | +| NGC 7027 | 21:07:01.57 | +42:14:10.5 | August-January | He I λ3187.74 measured directly; reddening-corrected flux ratio I(3187.7)/I(3444.1) = 0.086. O'Dell & Miller (1992). | +| NGC 7662 | 23:25:53.83 | +42:32:05.8 | September-February | He I λ3187.74 measured directly; reddening-corrected flux ratio I(3187.7)/I(3444.1) = 0.094. O'Dell & Miller (1992). | ## Inter-Target Calibration -Calibration measurements can be automatically performed during the night, between science targets. To do this, you can include any one or more of the calibration targets along with your science targets when you prepare your target list, using one of the reserved calibration target names listed in the table below. Along with the special target name, set your desired binning, slit width, and exposure time. When the sequencer loads this target, it will configure all subsystems (lamps, calibration covers, etc.) as needed for that type of calibration. No telescope moves will take place. When the system loads your next science target, the instrument will be automatically reconfigured, and science observations will continue. +Calibration measurements can be automatically performed during the night, between science targets. To do this, you can include any one or more of the calibration targets along with your science targets when you prepare your target list, using one of the reserved calibration target names listed below. Along with the special target name, set your desired binning, slit width, and exposure time. When the sequencer loads this target, it will configure all subsystems (lamps, calibration covers, etc.) as needed for that type of calibration. No telescope moves will take place. When the system loads your next science target, the instrument will be automatically reconfigured, and science observations will continue. -Calibration Targets: +**Calibration Targets:** -CAL_THAR CAL_THAR_UG CAL_FEAR CAL_FEAR_UG CAL_CONTR CAL_CONTB CAL_DOME CAL_DOME_UG CAL_BIAS CAL_DARK +- CAL_THAR +- CAL_THAR_UG +- CAL_FEAR +- CAL_FEAR_UG +- CAL_CONTR +- CAL_CONTB +- CAL_DOME +- CAL_DOME_UG +- CAL_DOMEHE +- CAL_DOMEHE_UG +- CAL_BIAS +- CAL_DARK -Calibration targets with the “_UG” suffix will use only those channels -- channels I,R are disabled. +Calibration targets with the "_UG" suffix will use only those channels -- channels I,R are disabled. diff --git a/docs/source/users-manual/camera-systems.md b/docs/source/users-manual/camera-systems.md index 59fc7407..349e3067 100644 --- a/docs/source/users-manual/camera-systems.md +++ b/docs/source/users-manual/camera-systems.md @@ -4,23 +4,15 @@ The G, R, and I spectrograph cameras use Petzval-type designs. This design family has a positive group in the front, a positive group in the middle, and a negative group near the image. The Petzval is a common design family for spectrograph cameras because it can accommodate an external aperture stop and can achieve relatively high performance and loose tolerances for fields of a few degrees and apertures of F/2-3. Designs are constrained to have no vignetting. -```{figure} assets/page_048_image_01.png -:alt: NGPS manual figure -:width: 90% - -``` - ## Focus -Internal spectrograph focus for the G, R, and I channels (reimaging of the instrument entrance slit onto the detector) is accomplished by actuating the second to last element in the camera (element before the field flattener=dewar window). The mechanisms are PI M-D01.11S actuators with PI C-663.12 controllers. The stages need to be homed and that is done by the instrument software when the system is initialized. The nominal stage range is 0 mm to 10 mm. The 0 mm position is closest to the center of the NGPS instrument, 10 mm position would be furthest out, however, the mechanical design does not allow motion out to the full 10 mm. The stage encounters a hard stop prior to that reading and, as it is a stepper stage and there is no limit switch, running into that hard stop will cause skipped steps and the stage reading to not be accurate. A component shutdown and daemon restart/rehome will resolve this. The focusd daemon does not permit commanding of the stage outside of its real physical range. The table below lists the nominal focus and max value for each of the G, R, and I focus axes. - -Focus Axis Typical Max - -G 3.3 7.8 +Internal spectrograph focus for the G, R, and I channels (reimaging of the instrument entrance slit onto the detector) is accomplished by actuating the second-to-last element in the camera (the element before the field flattener/dewar window). The mechanisms are PI M-D01.11S actuators with PI C-663.12 controllers. The stages need to be homed and that is done by the instrument software when the system is initialized. The nominal stage range is 0 mm to 10 mm. The 0 mm position is closest to the center of the NGPS instrument, the 10 mm position would be furthest out, however, the mechanical design does not allow motion out to the full 10 mm. The stage encounters a hard stop prior to that reading and, as it is a stepper stage and there is no limit switch, running into that hard stop will cause skipped steps and the stage reading to not be accurate. A component shutdown and daemon restart/rehome will resolve this. The focusd daemon does not permit commanding of the stage outside of its real physical range. The table below lists the nominal focus and max value for each of the G, R, and I focus axes. -R 2.7 6.7 - -I 5.1 7.6 +| Focus Axis | Typical | Max | +|---|---|---| +| G | 3.3 | 7.8 | +| R | 2.7 | 6.7 | +| I | 5.1 | 7.6 | As implemented, the mechanical focus change reading corresponds almost exactly to a shift in focus position at the detector. @@ -30,35 +22,31 @@ Note that for the U channel, the focus axis is at the collimator and that functi The U channel is a Schmidt design, including a transmissive aspherical corrector plane. This was chosen to minimize UV losses and improve imaging performance. -Documentation on the U channel design can be found in NGP.SPC.TEC.020. +Documentation on the U channel design can be found in [NGP.SPC.TEC.020](https://caltech.sharepoint.com/:b:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/Spectrograph%20%5BSPC%5D/Spectrograph%20-%20TECs/NGPS.SPC.TEC.020.pdf?csf=1&web=1&e=oeRTZv). ## Detector Systems -NGPS has four detector systems, they are referred to as U, G, R, and I channels. To reduce risk and cost, the instrument has repurposed the two Oxford SWIFT detector systems [REFERENCE] and the two detector systems from Double Spectrograph [REFERENCE]. - -Our documentation for the OSWIFT systems can be found here. +NGPS has four detector systems, they are referred to as U, G, R, and I channels. To reduce risk and cost, the instrument has repurposed the two Oxford SWIFT detector systems and the two detector systems from Double Spectrograph. -Our documentation for the DoubleSpec systems can be found here. +Documentation for the OSWIFT systems and DoubleSpec systems exists on the Caltech Sharepoint and can be made available upon request. We have retained the original readout electronics and associated harnessing. All front ends (instrument mounting interface, entrance windows) were rebuilt. Dewars were modified to include ½ tank depth stinger tubes to effectively eliminate liquid nitrogen spillage as the telescope slews on sky. -G, R, and I detector mounts include independent in-plane adjustments and tip tilt adjustments. - -G, R, and I channels are now equipped with frame transfer masks that cover ½ of the physical detector. The other ½ is where light from the spectrograph is collected. In principle, these devices could now be +G, R, and I detector mounts include independent in-plane adjustments and tip/tilt adjustments. -used in frame transfer mode. Unfortunately, the U device has the vertical and horizontal clocks running in directions that do not permit this, so a full 4 channel frame transfer mode is not possible. +G, R, and I channels are now equipped with frame transfer masks that cover ½ of the physical detector. The other ½ is where light from the spectrograph is collected. In principle, these devices could now be used in frame transfer mode. Unfortunately, the U device has the vertical and horizontal clocks running in directions that do not permit this, so a full 4-channel frame transfer mode is not possible. ### U Channel -The U channel cryostat is the former Double Spectrograph Blue detector system. Not many changes to this system. We refabricated the thermal sensing and control harness. Drawing can be found at NGPS_Temperature_Sensor_Cables.pdf with pinout. +The U channel cryostat is the former Double Spectrograph Blue detector system. Not many changes to this system. We refabricated the thermal sensing and control harness. Drawing can be found at [NGPS_Temperature_Sensor_Cables.pdf](https://caltech.sharepoint.com/:b:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/Electronics%20Rack%20%5BEL%5D/Electronics%20Rack%20-%20TECs/NGPS_Temperature_Sensor_Cables.pdf?csf=1&web=1&e=A1wRVl) with [pinout](https://caltech.sharepoint.com/:x:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/Electronics%20Rack%20%5BEL%5D/Electronics%20Rack%20-%20TECs/NGPS.EL.TEC.001.xlsx?d=w16bcd7f4b6c142bca8ae316b65bf12b5&csf=1&web=1&e=6Wb1r0&nav=MTJfQTcyMl97MDAwMDAwMDAtMDAwMS0wMDAwLTAxMDAtMDAwMDAwMDAwMDAwfQ). The cold link on the U channel is slightly undersized. The operating temperature is safe, but slightly elevated compared to what we would ideally want. ### G Channel -The G channel cryostat is the former Double Spectrograph Red detector system. We have replaced the dewar with a very similar (but longer) design to improve hold time. We have retained the same electrical interface to the tank thermal sensors and heater. We refabricated the thermal sensing and control harness. Drawing can be found at NGPS_Temperature_Sensor_Cables.pdf with pinout. We replaced the detector, as the original DBSP R detector was damaged by excessive illumination. +The G channel cryostat is the former Double Spectrograph Red detector system. We have replaced the dewar with a very similar (but longer) design to improve hold time. We have retained the same electrical interface to the tank thermal sensors and heater. We refabricated the thermal sensing and control harness. Drawing can be found at [NGPS_Temperature_Sensor_Cables.pdf](https://caltech.sharepoint.com/:b:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/Electronics%20Rack%20%5BEL%5D/Electronics%20Rack%20-%20TECs/NGPS_Temperature_Sensor_Cables.pdf?csf=1&web=1&e=A1wRVl) with [pinout](https://caltech.sharepoint.com/:x:/r/sites/coo/ngps/Shared%20Documents/NGPS%20-%20Subsystems%20%5BL3%5D/Electronics%20Rack%20%5BEL%5D/Electronics%20Rack%20-%20TECs/NGPS.EL.TEC.001.xlsx?d=w16bcd7f4b6c142bca8ae316b65bf12b5&csf=1&web=1&e=6Wb1r0&nav=MTJfQTcyMl97MDAwMDAwMDAtMDAwMS0wMDAwLTAxMDAtMDAwMDAwMDAwMDAwfQ). We replaced the detector, as the original DBSP R detector was damaged by excessive illumination. ### R Channel @@ -70,62 +58,59 @@ We have seen an intermittent connection issue on the clocks for this system. Thi This is one of the OSWIFT detectors. -Chan Device Physical Used Gain (e/DN) RN (e rms) DC (e/px/h) - -U E2V CCD44-82 BI 2048x4096 1028x4096 0.755 2.8 TBC - -G LBNL SNAP CCD 2040x4114 1020x4114 2.8 7.8 TBC - -R LBNL SNAP CCD 2040x4114 1020x4114 0.9 3.7 TBC - -I LBNL SNAP CCD 2040x4114 1020x4114 0.86 4.6 TBC - -Table of read-out times? +| Chan | Device | Physical | Used | Gain (e/DN) | RN (e rms) | DC (e/px/h) | +|---|---|---|---|---|---|---| +| U | E2V CCD44-82 BI | 2048x4096 | 1028x4096 | 0.755 | 2.8 | < 5.6 (TBC) | +| G | LBNL SNAP CCD | 2040x4114 | 1020x4114 | 2.8 | 7.8 | < 1.7 | +| R | LBNL SNAP CCD | 2040x4114 | 1020x4114 | 0.9 | 3.7 | < 1.2 | +| I | LBNL SNAP CCD | 2040x4114 | 1020x4114 | 0.86 | 4.6 | < 1.0 | ### Lakeshores NGPS has two Lakeshore 336 temperature controllers. Channel assignments are as follows: -Lakeshore U-R Description Typical value (setpoint) [K] - -A U CCD 168* (163) - -B U Dewar 75.3 - -C R CCD 128 (128) - -D R Dewar 76.5 - -Lakeshore G-I Description Typical value (setpoint) [K] +**Lakeshore U-R** -A G CCD 128 (128) +| Lakeshore | Description | Typical value (setpoint) [K] | +|---|---|---| +| A | U CCD | 168* (163) | +| B | U Dewar | 75.3 | +| C | R CCD | 128 (128) | +| D | R Dewar | 76.5 | -B G Dewar 82.6 +**Lakeshore G-I** -C I CCD 130 (130) - -D I Dewar 76.5 +| Lakeshore | Description | Typical value (setpoint) [K] | +|---|---|---| +| A | G CCD | 128 (128) | +| B | G Dewar | 82.6 | +| C | I CCD | 130 (130) | +| D | I Dewar | 76.5 | ### Pressure gauges Each cryostat has an Edwards D147010000 wide range gauge and they are read out in pairs by two Edwards ADC dual channel standard controllers. -Typical operating values when cold, are between few x 10-7 to few x 10-6 Torr. Generally, during a cooldown, it takes a cryostat several days to reach 10-7 Torr levels. +Typical operating values when cold, are between few × 10⁻⁷ to few × 10⁻⁶ Torr. Generally, during a cooldown, it takes a cryostat several days to reach 10⁻⁷ Torr levels. ### Cooling guidance -All four dewars are equipped with active charcoal getters. When preparing to cool, we generally like to pump till we get down to 10-4 to 10-3 Torr range then close the pump valve as we start filling. When possible allow for an extended warm pump down to clear out any accumulated moisture, etc. +All four dewars are equipped with active charcoal getters. When preparing to cool, we generally like to pump till we get down to 10⁻⁴ to 10⁻³ Torr range then close the pump valve as we start filling. When possible allow for an extended warm pump down to clear out any accumulated moisture, etc. -The cooldown time for all dewars is several hours. It’s generally OK to take images with G, R, and I once the temperature comes down to below 160K. U can be exposed a bit warmer. +The cooldown time for all dewars is several hours. It's generally OK to take images with G, R, and I once the temperature comes down to below 160K. U can be exposed a bit warmer. The hold times for the dewars are approximately: -U: 24h - -G: 18h - -R: 17h +| Channel | Hold time | +|---|---| +| U | 24h | +| G | 18h | +| R | 17h | +| I | 17h | -I: 17h +```{figure} assets/camera-systems-01.jpg +:alt: NGPS manual figure +:width: 90% +``` Figure 13: NGPS G Channel cooldown curve. Other cooldown curves are similar. The spike in the blue and red traces at 15:25 corresponds to a fill. diff --git a/docs/source/users-manual/command-line-interface.md b/docs/source/users-manual/command-line-interface.md index 376128bf..216f09bc 100644 --- a/docs/source/users-manual/command-line-interface.md +++ b/docs/source/users-manual/command-line-interface.md @@ -1,19 +1,67 @@ # Command Line Interface -A command line interface gives users the ability to send interactive commands and to create scripts to control any aspect of the instrument. A single wrapper, - -`seq` +```{note} +This is a future feature. +``` -```{figure} assets/page_026_image_01.png -:alt: NGPS manual figure -:width: 90% +A command line interface gives users the ability to send interactive commands and to create scripts to control any aspect of the instrument. A single wrapper, `seq`, can be entered into any shell and provides the interface for both scripts and single interactive commands. The general syntax structure is: +```text +seq +seq = +seq = = ... ``` -can be entered into any shell and provides the interface for both scripts and single interactive commands. The general syntax structure is +Scripts can be made using any plain text editor and have no restrictions on the file name. Scripting syntax uses the following rules: -`seq seq = seq = = ...` +```text +# comments begin with '#' +# one command per line +command +command key=value +command key1=value1 key2=value2 -Scripts can be made using any plain text editor and have no restrictions on the file name. Scripting syntax uses the following rules: +# execution grouping keywords +parallel: +serial: +end +on_error stop|continue + +# rules +- commands require a group start and end +- 'serial:' group start is optional (default is serial) but when used, + requires a matching 'end' +- no nested groups +- 'end' must have a matching group start, serial: or parallel: +- 'on_error' sets the behavior when an error occurs in a group, + - stop means to stop execution of group when an error occurs + - continue means to continue to the next command if an error occurs +- all other first tokens must be valid commands +- unknown commands/keywords are errors +- malformed key=value pairs are errors +- empty groups are errors +- blank lines are ignored +- comments are ignored + +# example +parallel: +move_to_target ra=12:34:56.7 dec=+12:34:56.7 +set_slit width=0.5 +set_camera exptime=0 +end +expose +set_camera binspat=2 binspec=3 +expose +``` + +The command to run a script is `run`, for example: ```text +seq run myscript.seq +``` + +Note that the `.seq` extension is not a requirement, only an example. A complete list of commands is given in the {doc}`detector-and-command-reference`. + +```{note} +Not yet implemented. +``` diff --git a/docs/source/users-manual/data-reduction-and-telemetry.md b/docs/source/users-manual/data-reduction-and-telemetry.md index 85c42e4e..000dc9ca 100644 --- a/docs/source/users-manual/data-reduction-and-telemetry.md +++ b/docs/source/users-manual/data-reduction-and-telemetry.md @@ -1,54 +1,49 @@ # Data Reduction and Telemetry -## Observation Timeline Modeler +## Data Reduction Pipeline -Future Feature - -```{figure} assets/page_030_image_01.png +```{figure} assets/data-reduction-and-telemetry-01.png :alt: NGPS manual figure :width: 90% ``` -### Data Reduction Pipeline - -Figure 2: Quicklook DRP GUI - The Quicklook DRP is the observer-facing reduction system for NGPS. In normal operation it runs continuously on the Palomar Quicklook computer, watches the raw-data archive for new NGPS science frames, builds or selects the needed calibrations, and writes reduced products within a few tens of seconds after readout. The current production pipeline is MATLAB based and reduces all four spectrograph channels (U, G, R, I) and the three image-slicer slices independently, using calibrations matched to the observing date, slit width, and binning. For observers, the primary interface is the Quicklook DRP GUI shown in the figure in this section. The GUI is normally open on workspace 1 of the Quicklook computer. Set the path in the upper-right field to /media/data_archive/YYYYMMDD_reduced/spec2d, click List files, and enable Listen for new files to have new reductions appear automatically. Selecting an object or a specific FITS file in the file list displays the reduced 2D frame and extracts a 1D spectrum. The Stack button sums repeated exposures of the same object until Clear plots is used. The 1D extraction settings are intended for rapid inspection, classification, and exposure-time decisions during the night. The Trace width field changes the extraction aperture; clicking on the 2D image changes the spatial extraction location for an individual channel; Place aperture moves all channels together from the spatial-profile panel. Lock zoom keeps the same 2D display region between frames, and Lock trace shape can be useful when a bright standard star defines the trace shape better than a faint science exposure. The DRP already applies a 2D sky subtraction; the Background sub control applies an additional local background subtraction in the GUI when that is useful for crowded or structured backgrounds. -The reduction sequence applies bias subtraction, flat-field correction, wavelength calibration, sky subtraction, and flux calibration. Master calibrations are generated per channel, per image-slicer slice, and per binning mode; science reductions are skipped until a matching bias, flat, mask, and wavelength solution are available. Wavelength solutions are based on FeAr/ThAr reference atlases. Flux calibration uses sensitivity functions derived from recognized HST CALSPEC spectrophotometric standards, and - -```{figure} assets/page_031_image_01.png -:alt: NGPS manual figure -:width: 90% - -``` - -the GUI automatically selects the standard observed closest in time to the science exposure. If no same- night standard is available, a previous sensitivity function may be used; observers should klick “Calibration info” and manually select a same-binning standard when multiple binnings were used. Flux standards should stay below saturation, roughly 40,000 counts, and should reach at least about 1,000 counts, preferably closer to 10,000 counts, in the spatial-profile display. These counts can be inspected on the fly quickly by looking at the spatial profiles panel as the flux standard is being observed. +The reduction sequence applies bias subtraction, flat-field correction, wavelength calibration, sky subtraction, and flux calibration. Master calibrations are generated per channel, per image-slicer slice, and per binning mode; science reductions are skipped until a matching bias, flat, mask, and wavelength solution are available. Wavelength solutions are based on FeAr/ThAr reference atlases. Flux calibration uses sensitivity functions derived from recognized HST CALSPEC spectrophotometric standards, and the GUI automatically selects the standard observed closest in time to the science exposure. If no same-night standard is available, a previous sensitivity function may be used; observers should click "Calibration info" and manually select a same-binning standard when multiple binnings were used. Flux standards should stay below saturation, roughly 40,000 counts, and should reach at least about 1,000 counts, preferably closer to 10,000 counts, in the spatial-profile display. These counts can be inspected on the fly quickly by looking at the spatial profiles panel as the flux standard is being observed. Cosmic-ray rejection is enabled by default in the GUI. The default parameters are tuned for common NGPS binning modes; for bright standards or twilight data, increase Nsig and/or reduce Grow if the 2D display looks blurred from excessive clipping. It can be helpful to disable the cosmic-ray rejection, clear the display, and re-extract the object for comparison and to assess the impact of the cosmic-ray removal. The Compute SNR checkbox provides a quick per-pixel SNR estimate for the extracted spectrum. Treat sharp jumps in the SNR curve as diagnostic rather than definitive, because narrow spectral features and residual cosmic rays can bias the moving-window estimate. Reduced products are written under /media/data_archive/YYYYMMDD_reduced/. The spec2d/ directory contains multi-extension reduced 2D FITS files; the spec1d/ directory contains 1D spectra saved from the GUI with Extract/Save; sensitivity-function FITS files are stored at the top level of the reduced-date directory. The reduced 2D files include the bias/flat corrected data, the 2D sky model, the 2D wavelength solution, a bad-pixel map, and an illumination-flat extension. -The full Quicklook manual, with step-by-step GUI instructions and troubleshooting detail, is maintained separately at https://sites.astro.caltech.edu/~cfremling/Quicklook_MANUAL.pdf. +The full Quicklook manual, with step-by-step GUI instructions and troubleshooting detail, is maintained separately at . -### PypeIt data reduction +## PypeIt data reduction PypeIt is an independent, community-developed Python reduction package for slit-based astronomical spectroscopy. It is useful as a second reduction path for NGPS data, especially for offline analysis, comparison against the Quicklook DRP, and reductions that need the standard PypeIt QA, calibration, extraction, and output products. The Quicklook DRP remains the real-time telescope reduction system; PypeIt should be treated as a complementary science-reduction option. For NGPS, use the PypeIt spectrograph identifiers p200_ngps_u, p200_ngps_g, p200_ngps_r, and p200_ngps_i for the four channels. The R and I channels are already represented in the public PypeIt documentation and code; U and G support is being added by Frank Verdi, and this manual assumes the completed four-channel support is available. If a local installation only lists p200_ngps_r and p200_ngps_i, update to the current NGPS-capable branch before reducing U or G data. -The recommended upstream branch for normal NGPS reductions is the PypeIt repository release branch: https://github.com/pypeit/PypeIt/tree/release. A typical source installation is: git clone https://github.com/pypeit/PypeIt.git; cd PypeIt; git checkout release; then follow the PypeIt installation instructions at https://pypeit.readthedocs.io/en/latest/installing.html. +The recommended upstream branch for normal NGPS reductions is the PypeIt repository develop branch: . The develop branch will hold the most up to date PypeIt branch for NGPS. A typical source installation is: `git clone https://github.com/pypeit/PypeIt.git; cd PypeIt; git checkout develop`; then follow the PypeIt installation instructions at . -The normal workflow is described in the PypeIt Read the Docs pages, especially Setup and Execution: https://pypeit.readthedocs.io/en/latest/ and https://pypeit.readthedocs.io/en/latest/running.html. In outline form, run pypeit_setup with the appropriate NGPS spectrograph name and the raw-data directory, inspect and edit the generated .pypeit reduction file, then run run_pypeit on that file. Run each NGPS channel as a separate PypeIt reduction, using the matching raw science frames, biases, flats, arcs, and standards for that channel and binning. +The normal workflow is described in the PypeIt Read the Docs pages, especially Setup and Execution: and . In outline form, run pypeit_setup with the appropriate NGPS spectrograph name and the raw-data directory, inspect and edit the generated .pypeit reduction file, then run run_pypeit on that file. Run each NGPS channel as a separate PypeIt reduction, using the matching raw science frames, biases, flats, arcs, and standards for that channel and binning. PypeIt builds its own calibration products, traces the slit/slicer apertures, solves the wavelength calibration, subtracts sky, finds and extracts objects, and writes PypeIt spec2d, spec1d, calibration, and QA outputs. -### Data Management +A wrapper script around PypeIt for NGPS is available at . This script can automatically process a night and extract merged, flux calibrated, telluric corrected 1D spectra across the full wavelength range from the central slice of NGPS. + +The main differences between PypeIt and Quicklook reductions are: + +1. Quicklook rectifies the images so the spectral trace is roughly straight, while PypeIt does not. +2. PypeIt measures spatial flexure from slit edge fits, while Quicklook uses residual signal between slits. +3. PypeIt does not use FeAr line lists and arcs. +4. PypeIt performs an optimal extraction following the "Horne" algorithm, while the MATLAB pipeline uses a box extraction. + +## Data Management All raw data is stored in a /data/YYYYMMDD/ directory for each UTC date. For convenience, a symbolic link is created each day from /data/latest/ which points to the current UTC. The instrument control computer performs no management of data. Palomar should appoint a person to manage data storage and removal. If an automatic data management policy were to be desired, something could be implemented at that time. As delivered, the disk can fill up, and the instrument will not function. @@ -56,26 +51,95 @@ All raw data is stored in a /data/YYYYMMDD/ directory for each UTC date. For con Telemetry is recorded in a telemetry database for each subsystem and is automatically copied to a computer which has public WWW access so that telemetry plots can be made available to anyone. Note that TCS coordinates are stored in a table not transferred so as not to be available publicly. -[Not fully implemented: Outside telemetry access was never implemented. TCS coordinates have not been separated. Only ACAM and Thermal telemetry has been implemented and only Thermal has a database tool.] +```{note} +Outside telemetry access was never implemented, and TCS coordinates have not been separated. Only ACAM and Thermal telemetry has been implemented, and only Thermal has a database tool. +``` ### ACAM -The ACAM writes the following telemetry to a database, one record for every frame while the ACAM is running. [Not fully implemented: Retrieval tools were never created for ACAM telemetry]. - -Table 3: ACAM +The ACAM writes the following telemetry to a database, one record for every frame while the ACAM is running. -NAME SOURCE DESCRIPTION CASANGLE TCS Cassegrain ring angle in degrees RAtel TCS telescope right ascension decimal hours DECLtel TCS telescope declination decimal degrees AZ TCS telescope azimuth focus TCS telescope focus AIRMASS TCS current airmass OBS_ID Target Database OBS ID of the current target read by the sequencer NAME Target Database NAME of the current target read by the sequencer POINTMODE acamd SLIT or ACAM coordinates RA Target Database RA of target read by the sequencer DECL Target Database DEC of target read by the sequencer result astrometry solver result of solution one of {NMATCH NFRACT NOISY GOOD} RAsolve astrometry solver DECsolve astrometry solver ANGsolve astrometry solver matches astrometry solver rms_arcsec astrometry solver RAoffset astrometry solver DECLoffset astrometry solver +```{note} +Retrieval tools were never created for ACAM telemetry. +``` -acquired astrometry solver boolean “is acquired” seeing astrometry solver seeing_std astrometry solver seeing_zen astrometry solver extinction astrometry solver extinction_std astrometry solver background astrometry solver background_std astrometry solver filter acamd current filter name datetime astrometry solver current UTC timestamp when record is inserted into database +Table: ACAM telemetry + +| NAME | SOURCE | DESCRIPTION | +| --- | --- | --- | +| CASANGLE | TCS | Cassegrain ring angle in degrees | +| RAtel | TCS | telescope right ascension decimal hours | +| DECLtel | TCS | telescope declination decimal degrees | +| AZ | TCS | telescope azimuth | +| focus | TCS | telescope focus | +| AIRMASS | TCS | current airmass | +| OBS_ID | Target Database | OBS ID of the current target read by the sequencer | +| NAME | Target Database | NAME of the current target read by the sequencer | +| POINTMODE | acamd | SLIT or ACAM coordinates | +| RA | Target Database | RA of target read by the sequencer | +| DECL | Target Database | DEC of target read by the sequencer | +| result | astrometry solver | result of solution, one of {NMATCH, NFRACT, NOISY, GOOD} | +| RAsolve | astrometry solver | | +| DECsolve | astrometry solver | | +| ANGsolve | astrometry solver | | +| matches | astrometry solver | | +| rms_arcsec | astrometry solver | | +| RAoffset | astrometry solver | | +| DECLoffset | astrometry solver | | +| acquired | astrometry solver | boolean "is acquired" | +| seeing | astrometry solver | | +| seeing_std | astrometry solver | | +| seeing_zen | astrometry solver | | +| extinction | astrometry solver | | +| extinction_std | astrometry solver | | +| background | astrometry solver | | +| background_std | astrometry solver | | +| filter | acamd | current filter name | +| datetime | astrometry solver | current UTC timestamp when record is inserted into database | ### Thermal Thermal telemetry is recorded to a database continuously, once per minute whenever the instrument control software is running. A Grafana interface is provided for retrieving the thermal telemetry from the database. The following table lists the telemetry recorded. -To access the Grafana page, open a browser to http://10.200.129.161:6502 and click on the “NGPS Thermal” dashboard. - -Table 4: Thermal - -NAME SOURCE DESCRIPTION datetime thermald / Lakeshore timestamp when record is inserted into database TCCD_U thermald / Lakeshore U channel CCD temperature TDEWAR_U thermald / Lakeshore U channel dewar temperature HEAT_U thermald / Lakeshore U channel heater TCCD_R thermald / Lakeshore R channel CCD temperature TDEWAR_R thermald / Lakeshore R channel dewar temperature HEAT_R thermald / Lakeshore R channel heater TCCD_I thermald / Lakeshore I channel CCD temperature TDEWAR_I thermald / Lakeshore I channel dewar temperature HEAT_I thermald / Lakeshore I channel heater TCCD_G thermald / Lakeshore G channel CCD temperature TDEWAR_G thermald / Lakeshore G channel dewar HEAT_G thermald / Lakeshore G channel heater TRACKSURF thermal / Campbell Electronics rack surface temperature TRACK_1 thermal / Campbell Electronics rack interior temperature near the computer and PI motor controllers TRACK_2 thermal / Campbell TRACK_3 thermal / Campbell - -TRHRACK_1 thermal / Campbell Temperature measured in the electronics rack interior near the U/R flexure controllers TRHRACK_2 thermal / Campbell Temperature measured in the electronics rack interior near the I/G flexure controllers RHRACK_1 thermal / Campbell Relative humidity measured in the electronics rack interior near the U/R flexure controllers RHRACK_2 thermal / Campbell Relative humidity in the electronics rack interior near the I/G flexure controllers TCOLL_U thermal / Campbell U channel collimator temperature TCOLL_G thermal / Campbell G channel collimator temperature TCOLL_R thermal / Campbell R channel collimator temperature TCOLL_I thermal / Campbell I channel collimator temperature TETA_B thermal / Campbell Temperature measured near the blue continuum calibration electronics in the electronics rack interior RHETA_B thermal / Campbell Relative humidity measured near the blue continuum calibration electronics in the electronics rack interior TETA_R thermal / Campbell Temperature measured near the red calibration electronics in the electronics rack interior RHETA_R thermal / Campbell Relative humidity measured near the red calibration electronics in the electronics rack interior TFOCUS_U thermal / Campbell U channel focus motor temperature TFOCUS_G thermal / Campbell G channel focus motor temperature TFOCUS_R thermal / Campbell R channel focus motor temperature TFOCUS_I thermal / Campbell I channel focus motor temperature TFLEXCON_IG thermal / Campbell Temperature measured above the I/G flexure controllers inside the electronics rack interior TFLEXCON_UR thermal / Campbell Temperature measured above the U/R flexure controllers inside the electronics rack interior TACAM thermal / Campbell Temperature measured inside the A&G interior near the partition next to the camera barrel assembly +To access the Grafana page, open a browser to and click on the "NGPS Thermal" dashboard. + +Table: Thermal telemetry + +| NAME | SOURCE | DESCRIPTION | +| --- | --- | --- | +| datetime | thermald / Lakeshore | timestamp when record is inserted into database | +| TCCD_U | thermald / Lakeshore | U channel CCD temperature | +| TDEWAR_U | thermald / Lakeshore | U channel dewar temperature | +| HEAT_U | thermald / Lakeshore | U channel heater | +| TCCD_R | thermald / Lakeshore | R channel CCD temperature | +| TDEWAR_R | thermald / Lakeshore | R channel dewar temperature | +| HEAT_R | thermald / Lakeshore | R channel heater | +| TCCD_I | thermald / Lakeshore | I channel CCD temperature | +| TDEWAR_I | thermald / Lakeshore | I channel dewar temperature | +| HEAT_I | thermald / Lakeshore | I channel heater | +| TCCD_G | thermald / Lakeshore | G channel CCD temperature | +| TDEWAR_G | thermald / Lakeshore | G channel dewar | +| HEAT_G | thermald / Lakeshore | G channel heater | +| TRACKSURF | thermal / Campbell | rack surface temperature | +| TRACK_1 | thermal / Campbell | rack interior temperature near the computer and PI motor controllers | +| TRACK_2 | thermal / Campbell | | +| TRACK_3 | thermal / Campbell | | +| TRHRACK_1 | thermal / Campbell | Temperature measured in the electronics rack interior near the U/R flexure controllers | +| TRHRACK_2 | thermal / Campbell | Temperature measured in the electronics rack interior near the I/G flexure controllers | +| RHRACK_1 | thermal / Campbell | Relative humidity measured in the electronics rack interior near the U/R flexure controllers | +| RHRACK_2 | thermal / Campbell | Relative humidity in the electronics rack interior near the I/G flexure controllers | +| TCOLL_U | thermal / Campbell | U channel collimator temperature | +| TCOLL_G | thermal / Campbell | G channel collimator temperature | +| TCOLL_R | thermal / Campbell | R channel collimator temperature | +| TCOLL_I | thermal / Campbell | I channel collimator temperature | +| TETA_B | thermal / Campbell | Temperature measured near the blue continuum calibration electronics in the electronics rack interior | +| RHETA_B | thermal / Campbell | Relative humidity measured near the blue continuum calibration electronics in the electronics rack interior | +| TETA_R | thermal / Campbell | Temperature measured near the red calibration electronics in the electronics rack interior | +| RHETA_R | thermal / Campbell | Relative humidity measured near the red calibration electronics in the electronics rack interior | +| TFOCUS_U | thermal / Campbell | U channel focus motor temperature | +| TFOCUS_G | thermal / Campbell | G channel focus motor temperature | +| TFOCUS_R | thermal / Campbell | R channel focus motor temperature | +| TFOCUS_I | thermal / Campbell | I channel focus motor temperature | +| TFLEXCON_IG | thermal / Campbell | Temperature measured above the I/G flexure controllers inside the electronics rack interior | +| TFLEXCON_UR | thermal / Campbell | Temperature measured above the U/R flexure controllers inside the electronics rack interior | +| TACAM | thermal / Campbell | Temperature measured inside the A&G interior near the partition next to the camera barrel assembly | diff --git a/docs/source/users-manual/daytime-setup.md b/docs/source/users-manual/daytime-setup.md index 9e654dc7..8b798303 100644 --- a/docs/source/users-manual/daytime-setup.md +++ b/docs/source/users-manual/daytime-setup.md @@ -1,14 +1,10 @@ -# Daytime Setup - -## Daytime Activities +# Daytime Activities Before observing, verify that the observing plan, target list, and calibration plan are ready. The observer should decide which slit widths and binning modes will be used during the night, including those needed for standard stars, and should take calibrations for those configurations. Internal spectrograph focus is normally performed during the day by the Support Astronomer or telescope/instrument operators. Observers should not normally need to run the internal focus procedure. Confirm with the Support Astronomer before starting calibrations that the internal focus has been checked and that the instrument is ready for afternoon calibrations. -Upload or create the target list before the start of the night. Target lists are CSV files and are loaded through the NGPS GUI into the target database. At minimum, each science target requires a name, RA, and DECL; additional columns may specify exposure time, slit width, number of exposures, binning, slit angle, acquisition mode, and comments. If target-list preparation and loading are described in detail in - -Choosing Slit Width and Detector Binning, this section should only state that the target list should be loaded and checked during the afternoon. +Upload or create the target list before the start of the night. Target lists are CSV files and are loaded through the NGPS GUI into the target database. At minimum, each science target requires a name, RA, and DECL; additional columns may specify exposure time, slit width, number of exposures, binning, slit angle, acquisition mode, and comments. Target-list preparation and loading are described in detail in the {doc}`target-lists` section; for the purposes of daytime setup, it is enough that the target list be loaded and checked during the afternoon. Afternoon calibrations should be taken once the dome is dark and the Support Astronomer or Telescope Operator confirms that it is safe to do so. Select the desired calibration type, binning, and, for dome flats, slit width; generate the calibration target list; then execute it with the normal sequencer by clicking Go. diff --git a/docs/source/users-manual/detector-and-command-reference.md b/docs/source/users-manual/detector-and-command-reference.md index a19587bc..24a945a7 100644 --- a/docs/source/users-manual/detector-and-command-reference.md +++ b/docs/source/users-manual/detector-and-command-reference.md @@ -6,20 +6,14 @@ This appendix describes the available CCD amplifiers, their naming conventions, ### G,R,I Channels -Figure 20: p-channel CCD layout - -Figure 21: p-channel CCD amplifier naming - -```{figure} assets/page_075_image_01.png +```{figure} assets/detector-and-command-reference-01.png :alt: NGPS manual figure :width: 90% - ``` -```{figure} assets/page_075_image_02.png +```{figure} assets/detector-and-command-reference-02.png :alt: NGPS manual figure :width: 90% - ``` ### U Channel @@ -28,80 +22,24 @@ Figure 21: p-channel CCD amplifier naming This section contains the recognized command line interface (CLI) commands. -[Not yet implemented. Incomplete list.] - -move_to_target [ ra= dec= ] - -Move to specified coordinates. Omit coordinates to move to the currently loaded database target. If coordinates are specified, then both are required. - -expose - -Triggers exposure and waits for completion - -trigger_exposure - -Triggers exposure and returns (no wait) - -repeat_exposure - -Repeat the last exposure - -stop_exposure - -Stops the exposure delay in progress (not the readout) - -abort - -Sends abort signal to all processes - -sequence_start - -Starts the sequencer list processing - -calib_set cal= - -configures the calibrator for the specified target where name is one of: - -THAR, FEAR, THAR_UG, FEAR_UG, CONTR, CONTB, DOME, DOME_UG, BIAS, DARK - -camera_init [ chan=,... ] - -initialize connection to science cameras. default is all cameras. optionally specify one or more channels with comma-separated list. where is one of: - -U, G, R, I - -Examples: - -camera_init chan=I - -camera_init chan=U,G - -camera_shutdown - -shut down camera system - -camera_set exptime= binspec= binspat= - -configure science camera settings - -slit_set width= offset= - -set slit width and offset. offset is optional - -focus_set = - - is one of U, G, R, I - -flexure_set - -acam_init - -acam_shutdown - -acam_set acquire=