rcoll <red_focus> (red_focus is provided by your SA)
bcoll <blue_focus> (blue_focus is provided by your SA)

The spectrograph focus in each arm will be defined by your SA. However, if you have multiple configurations such as different wavelength settings and/or different blocking filters in the beam, you may have to reposition the collimators in each configuration.

6. Configure the slit to view the sky:

agslit (move the acquisition/comparison mirror out of the beam)

This moves the acquisition/mirror mirror in the A&G box out of the light path, so that light from the sky falls on the slit. In this position the acquisition/comparison mirror directs light from the slit jaws to the acquisition TV, the configuration which is shown in the mimic example. This command also turns calibration lamps off.

7. Configure the slit to view the calibration unit:

agcomp (move the acquisition/comparison mirror into the light path)

This moves the acquisition/comparison mirror in the A&G box into the light path, so that light from the calibration unit falls on its reverse side and is directed to the slit. In this configuration the acquisition TV cannot view the slit.

8. Turn calibration lamps on:

complamps w (turn the tungsten flat-field lamp on)

The available arc lamps are CuAr, CuNe and both together, CuAr+CuNe. Selecting a different lamp turns the currently in-use lamp off, as does complamps off and agslit.

Note: If you turn the lamps on first and then move the comparison mirror into the light path, the lamps are turned off when the agcomp command is issued.

9. Deploy a neutral density filter in the calibration unit:

compnd 0.8 (insert neutral density with attenuation of 0.8 dex)

The tungsten flat field lamp saturates the detector with low resolution gratings, and neutral density filters amelioriate this. The calibration unit has two neutral density filter wheels, whose individual filter attenuations combine to reflect total demanded attenuation. The command compnd 0 removes the filters.

3.3  Controlling A&G box and ISIS mechanisms from the GUI

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1. Set detector readout speeds:
   
   rspeed <camera> <speed>
   
   Sets the camera readout speed to slow or fast.

   The operational characteristics for the two speeds are summarised for the EEV12 detector, and for the Red+ detector. Normally observations are carried out in slow mode because of the smaller read noise, but of course for bright targets, especially where higher cadence is needed, fast mode is preferred. As noted, the default readout speed is fast on resetting the CCD controllers.

2. Window the detectors:
   
   window red 1 "[555:1520,1:4200]" (Set the default window on Red+)
   
   window blue 1 "[585:1550,1:4200]" (Set the default window on EEV12)
   
   The default windows on the Red+ and EEV12 detectors are 966 pixels wide, corresponding to effective slit lengths of 3.54' and 3.22' respectively. The Y-axis window encompasses the full detector extent, including the overscan region. Smaller windows of course can be defined when high observing cadence is important.


3. Bin the detectors:
   
   bin <camera> <F_X F_Y>
   
   Sets the binning factors F_X and F_Y in the spatial and spectral directions respectively. For example, bin red 2 1 will bin Red+ x2 in the spatial direction, leaving the spectral direction unbinned.

   The spatial scales of the detectors are 0.20 arcsec/pixel (EEV12) and 0.22 arcsec/pixel (Red+). The grating dispersions and 1-arcsec resolution elements are listed here for the EEV12 detector in the blue arm, and here for the Red+ detector in the red arm.

   It's not recommended to use 4x1 or 4x2 binning with the detectors windowed, because the CCD controller times out and/or the observing system hangs for a short time (due to internal error in the controller), and one or other of these occurs at least 50% of the time. Also, high levels of binning are often accompanied by enhanced levels of clock-induced charge.

4. Save and recover detector configurations:
   
   saveccd <camera> <filename> (Save detector configuration)
   
   setccd <camera> <filename> (Recover detector configuration)
   
   Saves the detector window, readout speed and binning to a named file, and resets the detector configuration according to the named file description, respectively. If a filename isn't specified in the saveccd and setccd command line, the default filename udas_<camera>.cfg is used to store the configuration. The setccd command is especially useful when a dasreset (next paragraph) has been carried out, because the detector reverts to its default configuration following a reset.


5. Reset the detector hardware and software:
   
   dasreset <camera>
   
   This is the first step to recover from persistent problems with the camera and controller. It resets the detector hardware and software: (i) all processors in the SDSU CCD controller are reset to their power-on state, (2) all processors in the SDSU controller are reprogrammed, (3) the camera's configuration including operating temperature is reloaded, and the detector geometry is set to default values (no window and binning, fast readout speed). Unsaved exposures are lost. The procedure takes typically 30s to complete.


6. Take an exposure of a science target:
   
   run <camera> <int time> <"title">
   
   Takes an exposure of a science target and saves it as a FITS extension in rxxxxxxx.fit, with the target identified in the FITS header keywords. For example, run blue 600 "N157 B" take a 600s exposure with the blue arm and write it to disk as e.g., r1826342.fit.


7. Take multiple exposures of a science target:
   
   multrun <camera> <n> <int time> <"title">
   
   Take n exposures of a science target and generates n distinct output FITS files (not n extensions to a single FITS file).


8. Take an exposure of the flat-field calibration lamp:
   
   flat <camera> <int time> <"title">
   
   Takes an exposure of the flat-field lamp and identifies it as FLAT in the FITS header keywords.


9. Take multiple exposures of the flat-field calibration lamp:
   
   multflat <camera> <n> <int time> <"title">
   
   Takes n exposures of the flat-field lamp and generates n output FITS files.


10. Take a twilight sky flat-field exposure:
    
    sky <camera> <int time> <"title">
    
    Takes an exposure of the twilight sky and identifies it as SKY in the FITS header keywords.


11. Take multiple twilight sky flat-field exposures:
    
    multsky <camera> <n> <int time> <"title">
    
    Takes n exposures of the twilight sky and generates n output FITS files.


12. Take an exposure of the selected arc calibration lamp:
    
    arc <camera> <int time> <"title">
    
    Takes an exposure of the selected arc lamp and identifies it as ARC in the FITS header keywords (the specific arc lamp selected is also identified in keyword CAGLAMPS).


13. Take multiple exposures of the selected arc calibration lamp:
    
    multarc <camera> <n> <int time> <"title">
    
    Takes n exposures of the selected arc calibration lamp and generates n output FITS files.


14. Take a bias frame:
    
    bias <camera> <"title">
    
    Takes a zero-length dark frame and identifies it as BIAS in the FITS header keywords.


15. Take multiple bias frames:
    
    multbias <camera> <m>  <"title">
    
    Takes n zero-length dark frames and generates n output FITS files.


16. Take a test exposure (of any type):
    
    glance <camera> <int time>
    
    Takes a test exposure in the current A&G box and ISIS configuration, and saves it to s1.fit. This file is overwritten when the command is reissued. To convert a glance image to a permanent copy type:
    
    promote 1.fit (not promote s1.fit)
    
    and it will be renamed to rxxxxxxx.fit by the observing system, where xxxxxxx is the next available run number in sequence. Do not simply rename s1.fit from the shell; the observing system would have no knowledge of this action, and the renamed file would be overwritten in the next invocation of an observing command.


17. Take a scratch exposure (of any type):
    
    scratch <camera> <k> < int time> <"title">
    
    Takes a scratch exposure in the current A&G box and ISIS configuration, and writes it to sk.fit, where k is an integer in the range 1-99. In this way up to 99 test exposures can coexist. Of course subsequent glance images would overwrite scratch file s1.fit, so it's wise to start scratch file numbering at k=2.
    
    promote k (rename scratch file k to the next available, permanent run number)
    


18. Abort an exposure:
    
    abort <camera>
    
    Aborts an exposure which is running in the background without saving the data in the accumulated integration to disk.


19. Stop an exposure early, saving the accumulated data:
    
    finish <camera>
    
    Terminates an exposure which is running in the background, and saves the accumulated data to disk. This is a useful command when e.g., bad weather stops observing abruptly.


20. Change the integration time of an exposure:
    
    newtime <camera> <int time>
    
    Changes the integration time of an exposure which is running in the background. For example, newtime red 900 would change the integration time of the current red-arm exposure to 900s. This is a useful command when e.g., cloud cover thickens.

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In the afternoon before taking calibration images it's wise to check the general configuration of the instrument and the detector readout speeds, windowing and binning. These will have been set by your SA at the start of your run, but there's a small chance they may have been changed in the morning e.g., to troubleshoot a fault report, and not corrected. Also, if the DAS has been reset to fix a problem, the detector windows will have been lost, the readout speed will have been reset to fast and the detector will be unbinned. In this case windows, readout speeds and binning must be redefined as needed.

It's useful to take photographs of the instrument and detector mimics as a record of the configuration set up by your SA, so that you can refer to these on subsequent afternoons to check that the configuration remains as expected. If you fnd that an A&G box or ISIS mechanism, or a detector parameter, isn't configured as needed, use the appropriate command in Section 3 or Section 4 respectively to reconfigure it correctly.

Note that when the telescope is parked in "engineering mode", processed FITS headers such as RA, Dec, parallactic angle and slit sky position angle in calibration images are incorrect. If the actual slit sky position angle is needed, e.g., for zenith spectropolarimetry sky flats, it can be calculated from raw FITS header entries as described here.

5.1 Taking calibration images

Before taking calibration images turn off all dome lights (first check that nobody is working in the dome) and close the curtains in the control room.

Flat-field exposures should not be brighter than approximately 40000 ADU to avoid issues with non-linearity of the detectors. When using the low-dispersion gratings in the red arm the detector will saturate in short exposures of the tungsten lamp, so that neutral density should be deployed. In the blue arm arc exposure times in excess of 60s are needed to have well-exposed lines, and it can be useful to take a much longer exposure (which will saturate these lines) to have some reasonably-well exposed lines in the bluest spectral region.

1. View the calibration unit:
   
   agcomp (moves the acquisition/comparison mirror into the light path)
   

   This moves the acquisition/comparison mirror in the A&G box into the light path, so that light from the calibration unit falls on its reverse side and is directed to the slit. In this configuration the acquisition TV cannot view the slit, but can view the sky (with the X-direction opposite to that in slit-view mode).

2. Turn calibration lamps on:
   
   complamps <lamp> (turn the selected lamp on)
   

   The available arc lamps are CuAr, CuNe and both together, CuAr+CuNe, and a tungsten lamp, w. Selecting a different lamp turns the currently used lamp off, as does complamps off and agslit.

3. Take a test exposure:
   
   glance <camera> <int time>
   
   This exposure will allow you to compute a suitable exposure time to obtain well-exposed arcs or flat fields.


4. If needed, deploy a neutral density filter in the calibration unit:
   
   compnd <attenuation> (insert neutral density with attenuation in dex)
   

   To remove the neutral density use compnd 0.

5. Take lamp flat field exposures:
   
   flat <camera> <int time> <title> (take a single flat-field exposure)
   
   multflat <camera> <n> <int time> <title> (take n flat-field exposures


6. Take arc lamp exposures:
   
   arc <camera> <int time> <title> (take a single arc lamp exposure)
   
   multarc <camera> <n> <int time> <title> (take n arc lamp exposures)


7. Take bias frames:
   
   bias <camera> <title> (take a single bias frame)
   
   multflat <camera> <n> <title> (take n bias frames)

Before taking bias frames ensure that all the dome lights and calibration lamps are off, and the blinds in the control room are closed. It's also good practice to configure the comparison mirror in the beam (agcomp).

In principle, one can also take biases on ACAM simultaneously with those in the ISIS red and blue arms. However, it's been noted that taking biases simultaneously for ACAM and the ISIS red arm causes additional noise in the form of horizontal lines on ACAM and the ISIS red arm, which are not present if biases are taken separately. Taking biases on ACAM and ISIS simultaneously is therefore strongly discouraged.


8. Take sky flats:
   
   agslit (view the sky)
   
   sky <camera> <int time> <title> (take a single sky flat-field exposure)
   
   multsky <camera> <n> <int time> <title> (take n sky flat-field exposures
   

   The internal-lamp flats, being free of lines, are of course used for determining the CCD's pixel-to-pixel response. However, we suggest that observers take twilight sky flat fields to determine the slit illumination function; knowledge of this is important when observing extended targets or two (or more) point targets simultaneously in the slit, and is useful for accurate sky subtraction.

   To take sky flats with ISIS leave the telescope parked at zenith in engineering mode (i.e., not tracking). In this way dithering between individual exposures isn't needed.

   For the higher resolution gratings (R1200R, R1200B, H2400B), you should start ~10-15 minutes before a sunset, and for the lower resolution gratings start around sunset.

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6. Observing with ISIS

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6.1 Focusing the telescope

The focus applied to the telescope is

F_applied = F_measured + dF(temperature) + dF(elevation) + dF(filter) mm

where the dF terms are corrections for telescope truss temperature, telescope elevation and filter focus offset. The temperature and elevation corrections are applied automatically by the TCS throughout the night to ensure the telescope remains focused on the slit as its environment changes. Example values (in mm, taken from the FITS headers of image r2345903 on 20160412) are

F_measured = 97.85
dF(temperature) = 0.099
dF(elevation) = 0.055
dF(filter) = 0.00

Focusing the telescope in twilight therefore involves determining F_measured in the above expression. To do this, point to a bright star (r~9-11), e.g., one of your standards, at low airmass. It's usually fine to perform the focus run in the default 1 arcsec slit, but if you prefer, you can open the slit to e.g., 8 arcsecs, for the focus run:


slitarc 8.0

Since seeing is better at longer wavelengths it's preferable to focus using the red arm, but it's wise at the start of your run to also check focus in the blue arm, to ensure the best telescope focus is common to both arms. Use fast readout speed to save on overheads, check that the detector isn't binned, and take a test image of ~10s to check the level of the counts:

agslit (to view the sky)

rspeed <camera> fast

glance <camera> 10


The exposure time of the focus run needs to be ~7-10s to adequately sample the seeing. Inspect the test image to check that the spectrum isn't saturated and has SNR of at least ∼50 per pixel, and then execute the focusrun script:

focusrun <camera> <number exp> <int time> <focus start> <focus increment>

Typical parameters in an ISIS focus run are:

focusrun red 9 10 97.7 0.05

This will take nine images of 10s each, changing the focus of the telescope from 97.70 mm in increments of 0.05 mm between the images. All nine images are saved to path /obsdata/whta/"yyyymmdd", and you can determine the best focus by analysing "manually" the spatial profile in each image using IRAF/imexamine. However, it's preferable to run the bespoke focus script isis_focus directly on the nine images in the IRAF window at the ecl prompt:

!isis_focus

Note that the preceding exclamation mark is necessary to escape the command (isis_focus is a Python script, executed at the Linux shell level). The script prompts for the run number of the first image (without the ".fit" extension, e.g., r1234567) and the number of images taken in the focus sequence. The first image will then open in ds9 and you can position the cursor on the spectrum and press any key (e.g., spacebar) to measure the spatial profile at that position. All subsequent images are displayed one-by-one, and a spatial profile fit is shown for each image in the sequence. Finally, a graphical window opens showing the measured FWHM versus the telescope focus, with a parabolic fit over-plotted. The best empirical and fitted telescope focus values are printed in the IRAF terminal. Close this graphical window to regain the ecl prompt in the IRAF session.

When the the best focus value has been determined (e.g., 97.85) set the telescope to this focus and reset the detector readout speed to slow (if this is the preferred read speed):

focus <best focus>

rspeed <camera> slow

Warning: For runs involving both ISIS and ACAM, be aware that reconfiguring ACAM when ISIS is the selected instrument in use on-sky, will apply the configured ACAM optic focus offset, dF(filter), immediately, defocusing ISIS immediately. If such a change were made to ACAM in the afternoon of an ISIS run, and an ISIS focus run performed in twilight with such a focus offset applied, the focus run will compensate for the focus offset. However, if the telescope focus is set to the ISIS nominal focus with such a focus offset applied, but an explicit focus run isn't performed (e.g. due to time constraints in twilight), the telescope will be defocused by an amount commensurate with the offset. In this case, if you notice that the dF parameter in the TCS window is non-zero, ask the OSA to remove it. Check at the start of the night that a focus offset isn't applied, and never change the configuration of ACAM while observing with ISIS.

Note also that the optimum telescope focus, F_measured, is different for ACAM and ISIS, distinct from any ACAM optic focus offsets applied, so care is needed to ensure that the telescope focus remains optimal if switching back-and-forth between these instruments. Reselecting ISIS after using ACAM removes any ACAM optic focus offset applied, but otherwise does not change the telescope focus to its ISIS value.

6.2 Target acquisition

Acquisition of targets in the slit will be carried out by the OSA. Briefly, the slit jaws are polished and aluminised, and are inclined to the optical axis of the telescope at an angle of 7.5 degrees to allow the reflected image of the sky off the jaws to be viewed by the A&G box TV camera, currently ag4. To configure the A&G box for acquisition and observing, issue the command

agslit


The TV camera images suffer from coma, and for "fainter" targets, conservatively, V>18-18.5 dark-of-moon and V>16-16.5 bright-of-moon (and of course depending on seeing and extinction), blind-offset acquisitions are recommended (see Section 6.2.1 below).

The default orientation of the slit is set to the parallactic angle at the mid-point of your integration by the OSA, but inform the telescope operator if you prefer a different angle, for example, to place two targets in the slit, or to orientate the slit along features in an extended source.

Precession of the equinoxes causes a rotation of the equatorial coordinate system (the direction of North changes), so if you plan to place two targets in the slit and therefore need to orientate the slit along their common sky position angle, the calculation of this position angle should be carried out in precessed coordinates, and of course where necessary, with coordinates corrected for proper motions. This is especially true of very faint targets for which visual confirmation of the acquisition may not be possible; for bright targets the slit orientation can be easily adjusted to ensure both targets are well centred. The impact of precession on sky position angle grows with declination.

To save an acquisition image, ask the telescope operator to stop ag4 running in TV framing mode and execute the command

run ag4 <int time> <title>


This doesn't interfere with ongoing ISIS integrations, but remember to ask the telecope operator to switch ag4 back to TV framing mode, so that target centring in the slit can be monitored.

6.2.1 Blind offset acquisition

As noted above, the TV acquisition camera images suffer from coma, and for "fainter" targets, conservatively, V>18-18.5 dark-of-moon and V>16-16.5 bright-of-moon (and of course depending on seeing and extinction) it's expedient to first acquire a brighter object (brighter than the limiting magnitude) close to the target (less than 20 arcminutes, but preferably less than 10 arcminutes from the target), and do a blind offset to your target. In such cases prepare blind offset stars in advance to save time. For accurate blind offsets, coordinates should be quoted to at least two decimal places in seconds of RA and one decimal place in arcseconds of Dec. Always check if the offset star has an appreciable proper motion.

Blind offset acquisition requires the coordinates of both the reference star and the target, i.e., not coordinates of the reference star and the offset distance to the target.

In the blind offset procedure, the accumulated handset corrections applied to locate the reference object in the slit from its initial "gocat" location are converted to tangent-plane coordinates, and these are added to the pointing model's collimation terms in elevation and azimuth. This creates a localised, incremental correction to the pointing model, and this localised pointing model is adopted in the blind offset procedure to position the faint target in the slit once the reference target has been acquired accurately. However, closing the loop on the reference star discards this localised pointing model, and if the loop is subsquently opened and a blind_offset applied, the rms offset accuracy will be degraded to at least 0.5-arcsec. A blind offset should not be executed if the loop has been closed on the reference object. For example, if a bright target in a galaxy or cluster is observed closed-loop, then followed immediately by a blind offset to a faint target in the same galaxy or cluster, the acquisition of the faint target will be compromised.

The procedure for making a blind offset acquisition is:

(i) gocat "target" and identify a suitable guide star
(ii) gocat "reference"
(iii) centre the reference object
(iv) quickly apply blind_offset "target"
(v) quickly close the loop

The rms accuracy of this procedure is <~0.2-arcsec. Open-loop tracking error (~0.1-arcsec/minute) in the acquisition is minimised by identifying a guide star in advance of the blind offset, allowing the loop to be closed quickly after the blind offset to the target completes, and of course by quickly applying the blind offset once the reference target has been centred in the slit.

It's good practice to take a deep exposure of at least 100s on the slit-view camera following a blind offset acquisition to check centring of the target, e.g., accrued proper motion error could restrict acquisition accuracy.

Occasionally, blind offsets are needed to acquire a faint moving target. In this case follow the above procedures and apply the blind offset to the moving target less than one minute before the precise epoch adopted for the target coordinates, to limit open-loop tracking error. Apply the target's differential rates at exactly the epoch of its coordinates; the target will ''drift'' into the slit until the rates are applied, and the telescope will track it once the rates are applied. Close the loop immediately on applying the differential rates, and take a deep exposure on the TV to confirm acquisition.

6.3 Taking spectra of a target

First select the slit mode and slit width 

agslit (view the sky)

slitarc 1.0 (set the slit width to e.g., 1-arcsec)

Ask the OSA to point to your target (it's useful to provide a catalogue of the targets and their coordinates, and proper motions if relevant). Also state the position angle you want for the slit.

The OSA will take an image of the slit on the TV camera, and when you've identified your target, will centre it in the slit and start autoguiding. When the OSA confirms your target is acquired and the telescope guide loop is closed, you can start your integration by typing:

run red <exp_time> "<comment>" & run blue <exp_time> "<comment>"; bell

An audio alarm will sound when the blue-arm exposure completes, in this example.

If you will observe with the slit at parallactic angle (i.e. oriented in the vertical direction to minimise differential slit losses due to differential chromatic refraction), it's advisable to adjust this at least every 1.5-2 hours because the slit of course doesn't actively track the parallactic angle. The change of parallactic angle with time can be determined using the Staralt software (select Option=Parallactic Angle).

Note that it's as important to adjust the slit orientation every ~1.5-2 hours near zenith as it is at higher air mass; although differential chromatic refraction is smaller near zenith, the rate of change of parallactic angle is higher. These two effects combine to make the relative movement of blue and red images across the slit only weakly dependent on air mass.

If you do change the slit position angle to better track the vertical, always check the acquisition, and re-centre as necessary. In the case of a target acquired in a blind offset, repeat the blind offset acquisition if you change the slit orientation.

6.4 On-sky calibrations

To take arc calibration spectra (or lamp flats) during the night, proceed exactly as described in section 5.2. for afternoon calibrations. Observers requiring accurate radial velocities should take frequent arc lamp calibration exposures, e.g. every 15-20 minutes or so, to limit the impact of instrument flexure on radial velocity.

6.5 Observing bright targets

If you need to observe bright targets you can deploy the main neutral density filters in the light path, so that light reaching each arm is attenuated. Take into account that these neutral density filters are not uniform spectrally in the peripheral regions of the detectors. The table below indicates the area of the chip in pixels where the filters were determined to be "grey". In addition to their spectral non-uniformity, all these filters have small-scale throughput structures, which are difficult to remove fully by flat-field correction. If there is a need to use these filters (you should first consider narrowing the slit and/or defocusing the telescope as a solution in suitable cases), flat-fields should be taken to mask out affected regions.

To insert a main neutral density filter, use the command:

mainfiltnd <filter_pos>

where filter_pos is the filter position, corresponding to the required attenuation in dex, as listed in the table below. As an example, filter_pos 3 would correspond to an attenuation of 0.9 dex. The options are:



Filter Position	ND (dex)	Useful Window
1	0	-
2	0.3	[500:1600,1400:2800]
3	0.9	[500:1600,1900:3000]
4	1.3	[600:1600,1400:3000]
5	1.8	[500:1600,1400:2800]
6	3.0	[1050:1550,1900:3000]




6.6 Quick-look spectrum extraction

A basic quick-look spectral-extraction tool is available. We suggest that you first copy data to be analysed to a scratch area, e.g., /scratch/whta/'yyyymmdd' on the whtdrpc1 data reduction computer. To run the tool first ensure the necessary IRAF local packages are initialised (Section 2.2):

ecl> ing

ecl> isis

then at the isis> prompt type

isis> isis_ql <image number> <trace_X_pos>

where the image number is given without the '.fit' extension, and trace_X_pos is the approximate X-position of the spectral trace on the detector. For example,

isis> isis_ql r1234567 450

The script carries out an optimal extraction (which takes about a second), and displays the spectrum in the IRAF graphics window using splot. No wavelength calibration is provided. The usual splot keystrokes are available; for example, to zoom in on a feature type w to enter window mode, position the cursor at the lower left corner of the window you want and type e, and repeat this at its upper right corner. Type w n to unset the zoom in flux, w m to unset the zoom in wavelength, w a to unset the zoom in both axes, and q to exit splot.

Note that if the detector is binned, e.g., x2, in the dispersion direction, isis_ql still plots the extracted spectrum in unbinned pixels. Therefore a line expected to fall e.g., 300 binned pixels redward of the central pixel will fall 600 plotted pixels redward of the central pixel.

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7. Copying your data 

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You can copy your data to location laptop_path on your laptop when it's connected to the ingext-WiFi or wired networks (ask your SA or OSA for the relevant passwords):


• rsync -avuz whtguest@whtdrpc1.ing.iac.es:/obsdata/whta/yyyymmdd/ <laptop_path>
  
  
Or, you can copy the data to the FTP area, and subsequently retrieve it over the Internet:


• follow these instructions:
  
  
Or, you can write your data to a DVD (capacity ~4GB):


• ask your SA or OSA for blank DVDs
• follow these instructions