Phoenix 4-m User`s Manual v2.04
Contents
1. Oa Se AX KN E EEE Figure 4 Mayall 2 monitor after opening the Saver and Status blue windows The windows have been resized and shifted to fit onto a single screen for clarity 4 m Phoenix User Guide V2 04 15 April 2015 8 66 99 If the answer to the question is y the program will go through an internal initialization then download five voltages It will then return a final question e Do you want to activate the array Normally you will answer y if planning to observe Do not answer y unless the instrument and detector are cold The program will then query the location of the mechanisms open up a second Phoenix Daemon window and end with the message Initialization complete and the WildFire prompt The end result is shown in Figure 5 NOTE Error messages shown in Fig 5 referring to the xterm are normal vestiges of the earlier use of xterm windows for running WildFire The final error message about expecting a Boolean value but getting refers to a dark slide mechanism which was used on the Gemini South telescope but is not used at Kitt Peak At this point you may wish to redistribute the windows among the two monitors to reduce clutter You should now be ready to set up the mechanisms and parameters for observing as described in the step by step operations section of this manual Section 5 One may also iconify the phxDaemon windows as they are used only for diagnostic2. if planning to observe Do not answer y unless the instrument and detector are cold The program will then query the location of the mechanisms open up a second Phoenix Daemon window and end with the message Initialization complete and the WildFire prompt The end result is shown in Figure 5 4 m Phoenix User Guide V2 04 15 April 2015 12 5 The Step by Step Phoenix Operation Guide 5 1 New Feature countdown clock Throughout the history of IR array operation with WildFire an annoying aspect of the operating system was that the software architecture did not permit any estimate of the time remaining in an exposure The microcode would send out an initial read command and wait for the data to come back when the exposure was completed Although this is still the case it has been possible to program a countdown clock on mayall 2 which is initiated by the start of an integration and gives the approximate time until the end of the exposure While not precise it should be a very useful guide to the observer 5 2 Setting up the detector and the mechanisms In Wildfire window Note that the Wildfire window is the same as the yellow Phoenix window activate Turns on the array Use the default 0 320 bias The echoed back bias should be 0 300 If it is not then use setbias value Normally value should be 0 320 in order to get an echoed back bias of 0 300 Adjust up and down to get to a read back of 0 300 In a te
3. c Was the computer rebooted with the DSP power on and the instrument power off y You should then see a short flurry of activity ending with a message about configuring the C004 being complete d Is the instrument power on now n e Turn on the instrument power and enter lt cr gt when it is on Now go out the Instrument Power box and switch on the power or have the Instrument Scientist do this if logged in remotely then lt cr gt This should initiate another flurry of activity after which the startup should proceed as during the normal startup At this point the system will bootstrap the network You should see a series of ten nodes being bootstrapped these are the fiber optic transceivers and network connections from 4 m Phoenix User Guide V2 04 15 April 2015 11 the DSP to khaki The system will then download four WildFire programs specific to running Phoenix and open up two more windows labeled Phoenix Status and Phoenix Saver which will display the instrument mechanism temperature status and the file saver updates as images are taken The program will then ask if these windows have been initialized Figure 4 f Do you see engineering saver and status windows If the answer to the question is y the program will go through an internal initialization then download five voltages It will then return a final question g Do you want to activate the array Normally you will answer y
4. 2 166 4221 26 4655 3 4678 7 K4748 11 1 4704 4803 2 082 2 126 13618 27 4737 2 4758 7 H6073 1 10 6017 6129 1 632 1 662 6514 34 6058 1 6087 9 H6420 12 1 6377 6464 1 547 1 568 7198 36 6404 4 6435 6 J7799 10 1 7750 7865 1 271 1 290 9878 44 7780 6 7817 4 J8265 8243 8360 1 196 1 213 13620 47 8246 2 8283 7 J9232 3 1 9183 9286 1 077 1 089 9151 52 9210 0 9254 0 J9440 13 1 9397 9497 1 053 1 064 53 9424 2 9470 1 J9671 9652 9709 1 030 1 036 13662 55 9649 1 9692 9 NOTE Filters K4132 J8265 and J9671 are not currently installed in Phoenix Name Filter name Photometric band and approximate center frequency Filt CVF The filt and cvf settings for the filter cm The approximate FWHM of the filter in cm um The approximate FWHM of the filter in microns Encoder The approximate grat encoder setting of the center frequency with no offset Order The grating order at the center frequency Range The frequency coverage on the detector in cm at the center frequency setting 4 m Phoenix User Guide V2 04 15 April 2015 28
5. Phoenix commands Phoenix Engineering Daemon this red window can be used for executing low level commands in the event that the system requires extensive diagnostics This window is not for use by general observers 3 Follow the directions on the startup menu in the Phoenix window You will be asked a number of questions which must be read carefully Simply hitting a lt cr gt will return the default answer which may not be appropriate This example assumes that the DSP and Instrument Power have not been interrupted or communications through the fibers have been lost These more dramatic cases will be covered in the next section a Enter lt cr gt to continue from the initial startup window b Has the DSP been turned off since the last time you ran startwf n c Has the instrument power been off since the last time you ran startwf n At this point the system will bootstrap the network You should see a series of ten nodes being bootstrapped these are the fiber optic transceivers and network connections from the DSP to khaki The system will then download four WildFire programs specific to running Phoenix and open up two more windows labeled Phoenix Status and Phoenix Saver which will display the instrument mechanism temperature status and the file saver updates as images are taken The program will then ask if these windows have been initialized Figure 4 d Do you see engineering saver and status windows y
6. WildFire architecture which runs on a Sun SparcStation 20 named khaki located in the computer room There is a local monitor and keyboard in that room but the observer runs Phoenix from the control room through a VNC session to royal running on the MacMini named mayall 2 a second MacMini mayall 3 may also be used An Ethernet cable from the second port on khaki provides the private network connection to the Phoenix motor controller In the computer rack to the left of khaki is the black Heurikon Digital Signal Processor DSP electronics The DSP is connected through four fibers to the Instrument Power box on Phoenix During the initial installation and setup of Phoenix it is important to ensure that there is two way communication through all fibers This can be verified by checking the red receiver status error LEDs on both the DSP and the Phoenix Instrument Power box If all four lights are out the communications should be good If one or more error lights are lit this condition must be rectified before the instrument can be run 4 m Phoenix User Guide V2 04 15 April 2015 4 During a normal nightly startup when the instrument has been running the observer should not have to interact with any of the electronics on the instrument or in the computer room When the instrument is first installed or if it suffered a software crash while observing a more comprehensive startup procedure will be required This manual will cover these two situati
7. can be moved continuously Filter This wheel has 13 positions including an open The filter names are the photometric band and the central frequency in cm e g K4220 is at 4220 cm CVF This originally housed a continuously variable filter CVF but is now a second filter wheel The naming convention is the same as for the filter wheel Note that one of the Filter or CVF position must be open Slit There are three slit widths 2 3 and 4 pixels The 2 and 3 pixel slits have different lenses for three wavelength regions to focus the pupil on the cold Lyot stop The open position is used for imaging the field Lyot This wheel contains pupil stops for the 2 1 m and 4 m telescopes Because the Phoenix foreoptics are transmissive the pupil will be imaged at slightly different axial locations in the different wavelength regions so there is a different Lyot stop for a particular photometric band The masks are used for setup only Viewer This can be used to image the slit or object directly on the detector image for darks dark or for normal spectroscopy open The Lyot position is used during setup Table 1 Phoenix Mechanism Positions No Filter CVF Slit Lyot Viewer 1 open open pinhole_n1 dark image 2 M2150 ND 54um 0 9 2 0 4m 1 1 dark 3 J9232 M1930 54um 1 9 2 8 4m 1 5 open 4 L2734 L3010 54um 3 0 5 0 4m 2 5 lyot 5 K4220 L2462 84um 0 9 2 0 4m 3 6 6 K4308 K4578 84
8. is roughly linear with a slope of about 3 mv K Below 40 K 30K for the Lakeshore diode the behavior becomes highly nonlinear Diode Calibration 100 ua 1N914 Lakeshore Voltage 0 10 20 30 40 50 60 70 80 90 100 Temperature K Figure 6 Calibration curves for the 1N914 and Lakeshore temperature diodes 4 m Phoenix User Guide V2 04 15 April 2015 23 6 2 Operating Temperatures In normal operation one will see a status screen shown in the top panel of Figure 7 showing the detector temperatures detector activation status observation parameters and mechanism status The lamps and sliders are not encoded at Kitt Peak as they were at Gemini so they will normally return The detector temperature should be approximately 1 11 v 28 K and the detector heater power should read a nonzero value indicating that the temperature control is active This screen updates automatically so it will record changes in temperatures mechanisms etc One may update manually by entering status s A more detailed temperature status screen bottom of Figure 7 can be displayed by entering status t 000 Phoenix Status Phoenix Status Display 18 23 09 Detector Temp 1 104 Mount Temp 1 115 Det Htr Pur m 132 552 Mnt Htr Pur mv 24 926 Vlet e LA Vdd UC 25 49 The array IS activated Observation Settings File name test203d Index 36 Space Available Header Dir datal Zmeter 2013test 8136664kb Pixel Dir datal
9. off This turns off the lamp ask Type in a comment saying these are dark The exposure time must be unchanged from those taken with the lamp on go When done remember to remove the mirror in the Interface Unit from the beam For the thermal IR 3 5 microns In the thermal IR the ambient background is brighter than the flat field lamp so the flat exposures can be taken without turning on the lamp Take a test exposure to set the exposure time Then as above ask Set the number of pictures to 10 go 4 m Phoenix User Guide V2 04 15 April 2015 21 There are two schools of thoughts about darks at 4 6 microns they are worthless or you should take them If you want darks it is necessary to move a mechanism within Phoenix to the dark position Then take 10 exposures with the same integration time as for the flat When done remember to remove the mirror in the Interface Unit from the beam 5 7 Hollow cathode lamp The hollow cathode lamp works only in the 1 3 micron region Using the bottom slider on the Interface Unit move the hollow cathode lamp into the beam slider in In Wildfire hlamp on ask Generally it will take a minute or more to see hollow cathode lines go hlamp off IMPORTANT you must turn the lamp off after taking data It has a limited lifetime and is impossibly difficult to change When done remove the hollow cathode lamp from the beam slider to middle position 5 8 End of night At the Interface Uni
10. xpos ypos This will move the telescope so that the star is at the xcenter ycenter coordinates of the center of the slit If you encounter any trouble with these routines you can always do the recentering yourself Compare your measured position to that of the slit center multiply by 0 123 arcsec per pixel at the 4 m and move the telescope by the right amount to center the star at the slit center using the commands below In Wildfire north arcsec or south arcsec east arcsec or west arcsec go go takes another image Make sure star is at the slit center location or iterate the adjustments until the star is there On TV guider monitor mark position of center with wax pencil NOTE Each filter will have a different position On the first night of an observing block the instrument scientist will focus the star on the array and then adjust the focus of the TV so the image is in focus Afterwards it should only be necessary to adjust the secondary focus to maintain a sharply focused image on the TV If you wish to check the focus use imexam and the r key to generate a radial plot of the star image Iterate using small focus motions until the best image is obtained 2 Acquire a relatively bright K giant or A star move to marked spot on TV In Wildfire slit number of your science slit viewer open ask 4 m Phoenix User Guide V2 04 15 April 2015 16 Enter name of source set time to some small amount appropria
11. JS BO OP MIQUE ko 22 ON Saving your CALA REE EE NN anegidastwea seat 22 6 Operation Guide nininini nar a R E R E RE EEA 23 GALT Temperate Gali Pratl OM SG 23 6 2 Operating Temperat te Sanit e ere e a e te A a ores 24 6 3 Typical IMA ge Sinnsir ae ea a EEE EEE EE A ERER EA 25 7 Mechanism TOPE ALLOW aiis e ects Ne 27 4 m Phoenix User Guide V2 04 15 April 2015 2 Phoenix User Guide for the Kitt Peak 4 m Telescope 1 General Description Phoenix is installed at the 4 m on the rotator guider used with other Cassegrain instruments with the exception of NEWFIRM The instrument itself is mounted to the Interface Unit which is bolted directly to the back of the guider The Interface Unit provides the proper back spacing for the f 15 telescope focus to the instrument and also contains the calibration sources With the rotator at the nominal position angle of 90 the Instrument Power box is located on the east side of the instrument to the left as one enters the Cassegrain Cage and the motor controller box on the NW side of the instrument There are two AC power lines which connect to the UPS power outlets in the cage a set of four optical fibers from the Instrument Power to a fiber interface box on the telescope and an Ethernet cable running from the motor controller box to a media converter box in the Cage and then through the fiber interface box to the computer room this provides motor control through a private network e T
12. Phoenix High Resolution Infrared Spectrograph User s Guide KPNO 4 m Telescope Ken Hinkle Dick Joyce Colette Salyk Version 2 04 2015 April 15 4 m Phoenix User Guide V2 04 15 April 2015 1 Contents l General Description tsan dod cntialods vides it aati auabi be GS 3 2 Come RON ses 4 S NOa Sarp ssse SE 5 31 WildFire St artupuamipeusadetangsakredemkerhuihahetannhreiv ddbn 5 ME ele eas ods cas cena sot ce vcs oa ee aac odode wa E 5 3 2 Nightly Startup and Shutdown Summary eeorooooorovorrrrvnrrrrnrerrrnsenrrnssnrrnernrrvennnne 10 4 Startup in Special Circumstances c 2 4ssscess wccareanvssaasoundeceds svcsanee lassad casnsede tune seastasoteaats 10 5 The Step by Step Phoenix Operation Guide arrrnrnnnnnrerrnnrrrrnnrrrrnnenrrnsnnrreernrrsernrssennn 13 SI New Beature cbunidovrdotkva4v44rm E E 13 5 2 Setting up the detector and the mechanisms srrnrnvrnrenvvnrennnnererrnerrrrnserrreserrresennn 13 5 3 Locating and marking the position of the slit esnrrororrnorrrrnrrrrrnrrnrrverrrrvernrrvennnne 15 5 4 Fine Tuning the Grating Positlon uusesisrnasrmssanerssiisssimrstsivaassedikeisenre 17 JD ODSEV fuss 18 5 5 1 Observing infrared bright visually very faint Objects rrrernrrrornrrvornrrvrrnrree 19 5 5 2 Integration time and data quality cc lt sciesssccassecceds saccassacseacdesedccusteccstesevenies 20 5 60 FR and dass eek 21 57 Hollow cathode Va gcse whee ne tite seas sole ae an Re ekke 22
13. WildFire is a command line control system based on transputer technology which was thought in the late 1980s to be the Next Great Design in computing This technology combines integrated memory and serial communications and can run at Kitt Peak only on the Sun Workstations which have been superseded by newer generations of instrumentation control Fortunately it has been possible to incorporate some technology advances into the Observer Interface such as running WildFire through a VNC session on the MacMinis with their dual monitors and incorporating GUIs to hide some of the startup details from the user Figure 2 shows the left hand monitor of mayall 2 from which one initiates the WildFire startup Any of the windows can be moved seamlessly from one monitor to the other In addition there are four spaces on which one may run ancillary processes Web interfaces etc and keep clutter under control These may be selected by the spaces icon on the task line at the bottom of the monitor screen 4 m Phoenix User Guide V2 04 15 April 2015 5 O O X Pho Phoenix Menu Ready Start Phoenix Restart IRAF Restart Phoenix pe Kill Phoenix Figure 2 View of the left hand monitor of mayall 2 Double clicking on the Phoenix icon has brought up the Phoenix Menu GUI 1 Starting with mayall 2 logged in as 4meter locate the Phoenix icon on the right side of the screen and double click to open T
14. Zmeter 2013test 8136664kb Integration time 5 000 seconds coadds 1 Inrs 1 The Filter Wheel filt is at wn_4748 11 Hollow cathode OFF The Lyot Stop Wheel lyot is at 4m 2 5 4 Flat lamp OFF The CYF Wheel cvf is at open 1 The Slit Wheel slit is at 54u_1 9 2 8 3 Slides The Viewer Wheel viewer is at open 153000 NORMAL out in center The Grating grat is at encoder 11202 hollow cathodes in in flat lamp in out center dark in with lamps off ga lamptgas tube in out out gas tube only out in out th ane N Phoenix Status Phoenix Temperature Status Display 18 27 06 Detector Temp 1 105 Mount Temp 1 114 Det Htr Pur mu 433 897 Mnt Htr Pwr mv 23 230 Top Outer Shield 0 566 Top Inner Shield 1 032 Head 1 Stage 1 1 094 Head 1 Stage 2 1 605 Head 23 Stage 1 1 100 Head 23 Stage 2 1 858 CVF SLIT Cover 1 1 060 Mirror Mount 1 061 CVF SLIT Cover 2 1 055 Lyot Cover 1 060 Fixed Filter Cover 1 048 Grating 1 059 Grating Frame 1 067 Grating Tipper 1 064 Fixed Filter Right Angle Drive 5 Lyot Stop Right Angle Drive 1 066 Visible Dichroic Mirror Mount 1 056 Secondary Mirror Focus Frame 0 378 Secondary Mirror Focus Mount 0 394 Collimator Box Bottom Cover 1 064 Bottom Inner Heat Shield 1 041 Bottom Outer Heat Shield 0 556 Figure 7 Screens for status s top and status t bottom with the instrument cold 4 m Phoenix User Guide V2 04 15 April 2015 24 6 3 Ty
15. be appended to the end of this filename Typically the exposure time should be about 10 sec go This takes an image of the sky through the slit NOTE Initially images may not display automatically on the ds9 If this is the case change to the current data directory in the IRAF window and display an image using the IRAF display command display lt imagename gt 1 If the image displays properly on the ds9 succeeding images should autodisplay as they are taken In IRAF Measure position of the middle of the slit and write down the coordinates If all is well this should be close to x 128 and y 510 This position will be different for each filter Mark down this position xcenter ycenter and then In Wildfire zcenter xcenter ycenter pa 0 123 This will orient the software for the slit geometry lt xcenter gt and lt ycenter gt are the slit center coordinates measured above lt pa gt is the position angle of the 4 m instrument rotator and 0 123 is the scale in arcsec per pixel at the 4 m 4 m Phoenix User Guide V2 04 15 April 2015 15 NOTE You must run zcenter prior to running either recenter abba or ab for the first time or after any change in the rotator angle since these routines require the coordinate and scale information In Wildfire slit open ask Set the time for an image of the star typically about I sec go In IRAF Measure position xpos ypos of the center of the star In Wildfire recenter
16. gration times from the ITC can then be scaled A more detailed assessment of the data quality can be made by extracting a spectrum using the following commands In IRAF imar aperture a spectrum aperture b spectrum some name for difference spectrum twodspec apextract apall onedspec splot name for difference spectrum ms 4 m Phoenix User Guide V2 04 15 April 2015 20 The spectrum can be smoothed if required and S N measured on specific regions using the tools in splot The s key will smooth the spectrum to a desired pixel resolution a will redefine the display window c will reset to the full display and m will calculate the S N between two cursor positions on the spectrum 5 6 Flats and darks Every time the grating is moved a new set of flats must be observed To do this the sliders on the interface unit are used The sliders must be moved by hand Pull the mirror middle mechanism into the beam The dark slide top can be open or closed The reference slide bottom should be at the middle open position For the near IR 1 2 5 microns In Wildfire flamp on This turns on the flat lamp Lamp flats require roughly 4 second exposures in the K band We recommend using ask to set up a test image Execute this with go Then measure the signal with the T command in IRAF imexam The maximum signal level should be between 1000 and 2000 ask Set the number of pictures to 10 go flamp
17. haki the DSP box and the Instrument Power are all turned on Visually check the red fiber LEDs on both the Instrument Power and DSP If any of them is red WildFire will not run and the fiber hardware situation must be repaired 2 If the fibers are OK turn the Instrument Power OFF 3 Go down to the computer room and turn the power on the Heurikon DSP box OFF for about 30 seconds then ON Alternatively the operator can do this remotely through 4m power 4 where the IR DSP power is outlet 7 4 Reboot khaki This requires superuser permission and must be carried out by the OA Electronic Maintenance or the Instrument Scientist NOTE Since WildFire is run as an ssh session on khaki the Start Phoenix button on the mayall 2 monitor will automatically log in so it is not necessary to specifically log into khaki after the reboot Periodically ping khaki from a window on mayall 2 until you get a response indicating that khaki is alive 5 Once the reboot is completed click the Start Phoenix button on the Phoenix GUI NOTE the Instrument Power should still be OFF This will bring up the normal startup configuration displayed in Figure 3 6 Go through the startup sequence as in Section 3 However the answers to the questions will be different and there will be more of them a Enter lt cr gt to continue from the initial startup window b Has the DSP been turned off since the last time you ran startwf y
18. he power switch for the Instrument Power is a toggle switch on the top of the electronics box This should be the only control other than the mechanical slides on the Interface Unit which the observer may have to operate The Interface Unit has three mechanisms which must be manually operated by the observer e The top slider controls an environmental cover which should be moved in during the daytime to protect the instrument window and out while observing at night Calibrations may be done with the cover in e The middle slider moves a mirror directing the light from the tungsten flat field lamp into the instrument The mirror should be out of the way when observing e The bottom slider has three positions o In moves a ThAr emission line source into the beam o Middle open used while observing o Out moves a CO gas absorption cell into the beam Figure 1 shows Phoenix installed on the 2 1 m telescope where the various mechanisms are easier to see than in the 4 m Cassegrain cage 4 m Phoenix User Guide V2 04 15 April 2015 3 NN MN MOTOR CONTROLLER i H Ae PRIVATE ETHERNET Figure 1 View of Phoenix installed on the 2 1 m telescope showing the main components The three manual slides on the Interface Unit are not easily visible in this image The power switch to the Instrument Power Analog Electronics is on top next to the power cord 2 Computer Room Phoenix is the last instrument running on the
19. his will bring up the Phoenix Menu which consists of four selections 4 m Phoenix User Guide V2 04 15 April 2015 6 Start Phoenix this opens a VNC session to royal and brings up the initial startup screens which allow for a full startup of WildFire Restart IRAF this will restart the IRAF session which normally comes up with the Start Wildfire without exiting from WildFire in case the xgterm or ds9 has been inadvertently closed Restart Phoenix this will restart the Phoenix WildFire session if it has been terminated gracefully and not as a result of a power or communications failure Kill Phoenix this will exit WildFire in a graceful manner and shutdown any background processes In theory this should allow an efficient restart using the Restart Phoenix button 2 Click on the Start Phoenix button This will bring up four windows as shown in Fig 3 Note these windows have been resized and arranged to fit onto a single screen on the Mayall 2 monitor for clarity Figure 3 Mayall 2 monitor after commanding Start Phoenix from the Menu GUI 4 m Phoenix User Guide V2 04 15 April 2015 Phoenix IRAF this is an IRAF xgterm running on khaki and can be used for accessing and quick look examination of the data SAOimage ds9 this is actually running on mayall 2 but will display images from khaki over a network once initialized Phoenix this distinctive yellow window is the command line interface for all of the
20. iewer positions are open dark or image Typically we will want image to start The choice for spectroscopy is open Note that for the viewer unlike for the other mechanisms you cannot type viewer 1 or viewer 2 etc You must use viewer image viewer open or viewer dark 4 m Phoenix User Guide V2 04 15 April 2015 14 grat pos in cm K offset The grat K command moves the grating toa given frequency The offset parameter is necessary to account for the encoder zero point An offset of 800 works well as of May 2013 grat encoder position moves the grating to a given encoder position If a mechanism fails to move then try kick mech Name pos value this commands applies extra torque When the telescope is running tepon This starts communication between the telescope and the Phoenix computer Itis sometimes needed at the start of the night It should not be necessary after that 5 3 Locating and marking the position of the slit 1 Acquire a V 9 SAO star that is close to overhead If you are observing in the 4 5 micron region use a bright star In Wildfire Check that the viewer is set to image ask Enter the title target name filename and the exposure time Filename is just the start of the filename for example image or setup for imaging the slit or data if you want all files to have the same file start A 3 digit extension will
21. n the peak of the positive feature If the centering is good enter q and yes to the questions about tracing and fitting the apertures The display will show a plot of the fit to the spectral aperture sampled at intervals typically 10 pixels along the spectrum If the fit looks good enter q again and answer yes to the questions about storing the apertures and extracting the spectra You will finally get a spectral plot answer y to the question about saving the spectrum The result will be a spectrum named diff image 0001 fits or diffimage ms fits in the data directory The command help apall will bring up a more comprehensive explanation for the task 4 m Phoenix User Guide V2 04 15 April 2015 17 Display the spectrum using splot diffimage 0001 Compare the spectrum to the Arcturus Atlas and figure out the central wavenumber Frequency increases with pixel number so the orientation of the spectrum should be the same on the display as in the Arcturus Atlas Note how many wavenumbers off the desired center the spectrum is Add the opposite of this difference to your original wavenumber and rerun grat with the corrected value Re observe the spectrum and repeat the above analysis to converge on the desired central wavenumber During the November 2012 observing run we found it necessary to adjust the wavenumber setting in grat by 2 cm in the K band 5 5 Observing It would be best to s
22. ons in separate sections 3 Normal Startup 3 1 WildFire Startup When all is well during an observing run the observer need only carry out a few tasks at the end and beginning of the night See Section 3 2 for a summary On the first night of a run the instrument support person will take the observer through a startup of the WildFire program since this may be necessary if the system crashes or needs to be restarted for other reasons The 4 m control room contains three MacMini computers with large flatscreen displays One of these mayall 1 is located at the Operator s station and is used by the OA only for controlling the telescope operation The other two located on the long Observer s station are mayall 2 and mayall 3 these are used for operating the various instruments used on the 4 m Mayall 2 is generally preferred for instrument operation since it has additional monitors displaying the telescope status information VDU and guider camera field while mayall 3 is generally used for off line data inspection analysis if there are multiple observers NOTE The instructions in this section assume that a previous session of WildFire has been shut down gracefully and not as a result of a serious software crash power interruption to the Instrument Power or Digital Processors or loss of communication over the fiber network These situations call for a more comprehensive recovery which will be described in Section 4 3 1 1 WildFire
23. or low level commands k Grab file Edit Capture Window Hein gen 09 Thea Mar 14 1142 AM ameter Q Figure 5 Mayall 2 monitor after a successful WildFire startup The various steps are annotated on the yellow WildFire command line window 4 m Phoenix User Guide V2 04 15 April 2015 9 3 2 Nightly Startup and Shutdown Summary Here we summarize the nightly startup and shutdown See section 5 for the detailed step by step version During the course of a normal observing run the instrument and all of the control screens may be left running during the day At the end of each night the observer should only need to e Deactivate the array by entering deactivate e Close the dark slide top slider on the Interface Unit Upon starting up the following evening the observer must Open the dark slide on the Interface Unit Activate the array by entering activate enter a bias value near 0 320 to give 0 300 Create a new data directory for the night on datal 4meter in terminal Execute ped to enter the new data directory into WildFire After the telescope has been started up enter tepon to establish communications with the telescope These instructions and the commands are described in more detail in the Step by step Operations section of the Manual Section 5 NOTE At the end of a Phoenix observing block before the instrument is powered off the viewer should be moved to the dark position and the filter CVF and slit wheels to
24. pical Images Figures 8 and 9 show some typical images under normal operation ae Figure 8 from left a Dark frame There are some noisy and or high dark current pixels in the image which is normal The crack in the lower left is an array defect b Flat field image the striped pattern in the upper half of the array is a normal property of the detector controller c A frame showing an unusual Phobos event These are believed to be electrical discharges within the array introduced by stresses and are more frequent during the first few days after the instrument has been cooled The dark current in the lower 75 of the array is evident in this 900 s exposure is at a level 350 e Some of this may result from very low level thermal background d Spectrum of the flat field lamp at 4275 cm with the CO cell in the beam Only six of the low J 2 0 lines are visible 4 m Phoenix User Guide V2 04 15 April 2015 25 Figure 9 from left a Image of ThAr hollow cathode lamp taken during the spectrograph focus procedure b Raw image of a star in the 6395 cm band note the OH emission lines from the atmosphere c Result of subtracting two images after dithering along the slit demonstrating the removal of the sky features 4 m Phoenix User Guide V2 04 15 April 2015 26 7 Mechanism Information Of the seven mechanisms five have discrete positions which can be commanded by number or name Section 5 The grating and focus mechanisms
25. rminal window ssh to khaki Check that you are in data directory should be datal 4meter df Check that there is sufficient disk space on datal to store your data Each image is 1 05 MB in size In IRAF window mkdir label For label use a directory name using the date for example 2012nov23 cd label pwd In Wildfire window ped Stands for Parameter EDitor You should leave most parameters as default However you will want to change the header and pixel directory to match the IRAF data directory If the IRAF directory was for instance datal 4meter 2012nov23 you should type in datal 4meter 2012nov23 in Wildfire eask 4 m Phoenix User Guide V2 04 15 April 2015 13 This sets the parameters that whose values will be requested before each observation Set with la the parameters to be shown requested by ask Other parameters get T and will not be shown or requested before an observation You can always rerun eask if you change your mind Note that while picture number is automatically incremented by the software you may want to set this to la so that you see the frame number before beginning an observation and can mark this on your observing log ask To get started make sure the integration time is set to a small value pictures to 1 Inrs to 1 coadds to 1 The following commands involve mechanisms status s displays the current position of all of the instrument mechanisms in the status window The
26. status display automatically updates when you move mechanisms help mechanism name tells about the command and the position options IMPORTANT make sure the mechanism command has finished i e that you get a prompt back before typing anything else This is the main cause of lost time with Phoenix If you type in a new command before the previous one finishes you can hang the computer IMPORTANT at the beginning of a run the instrument scientist will initialize the mechanisms except for the collimator focus which have home switches to define the zero position using the command init lt mechanism gt This command may be done by the user if for some reason one of the mechanisms seems to have become lost However the order of the words is important For some reason the software interprets the word init as a position so reversing the order of the two words will attempt to move the mechanism to a position which is impossible for some of the mechanisms Make sure the mechanism went where you wanted The new position is echoed back filt pos value selects the filter There is a second set of filters in the cvf wheel which is now effectively a second filter wheel To use these first do filt open and then evf pos value Otherwise set cvf to open lyot pos value sets the lyot stop for the telescope and wavelength slit pos value sets the slit The commonly used 4 pixel slit is number 8 viewer pos value The v
27. t executed zcenter you must do so before using recenter This must also be done whenever the rotator position angle is changed Recenter moves the star to the zcenter position It may be necessary to do this twice When the star is centered up a final image can be taken by putting the slit back in and imaging through the slit 5 5 2 Integration time and data quality The data quality will naturally depend on conditions Each observation should be checked It is the observer s responsibility to do this and to talk to the start up person about the data quality The starting point for setting the integration time is the Phoenix ITC Using the ITC tool compute integration times for the planned observations Most observations require four separate frames abba so the total integration time should be divided by four After taking an observation the spectral image will appear on the ds9 display In IRAF imexam This allows measurements of the spectral image j takes a horizontal cross cut of the image and carries out a Gaussian fit kK does the same in a vertical cut e provides a contour map Roughly integrate the number of ADU in the cross cut using the peak signal and FWHM provided on the graphics terminal Multiply this by 9 2 the gain in e ADU and take the square root This is the approximate S N in this observation ignoring the read noise of the detector Multiply by two to get the final S N for four frames The inte
28. t move the dark slide into place top slider in In Wildfire deactivate NOTE At the end of a Phoenix observing block before the instrument is powered off the viewer should be moved to the dark position to protect the detector from condensation with the command viewer dark Also move the filter CVF and slit wheels to the open position 5 9 Saving your data While at Kitt Peak sep can be used to copy your data to your laptop It is highly recommended that you copy your data to your laptop and take the data away with you From your laptop scp rp 4meter khaki data directory You can get the data directory using pwd in the IRAF window All data also goes into the Kitt Peak data archive 4 m Phoenix User Guide V2 04 15 April 2015 22 6 Operation Guide 6 1 Temperature Calibration The temperatures are measured as the forward bias voltage on a temperature sensitive diode operated at a current of 100 ua Most of the diodes in Phoenix are 1N914 diodes which are relatively inexpensive those on the detector and mount are factory calibrated Lakeshore diodes which have a slightly different dependence from the 1N914 The calibration curve for both diodes is presented in Figure 6 The status readbacks Figure 7 are in voltages so one may refer to this curve to convert to temperature In general the 1N914 diodes read approximately 0 400 volts at room temperature and 1 000 volts at 70K The behavior in between
29. tart with a bright star perhaps a hot star for removing the telluric lines Observing a bright star with a short integration time minimizes time lost if anything is not set up correctly NOTE The array will saturate at approximately 9000 ADU For the minimum integration time of 1 002 sec the saturation occurs at about 5000 ADU We recommend keeping the maximum signals to no more than half of these values to avoid nonlinearity effects In Wildfire At the start of the night after the telescope has gone to the first star it might be necessary to type tepon This starts communication between the telescope and the Phoenix computer tcpon should only be needed when the telescope is started For the first observation only the position angle and plate scale must be entered zcenter fxcenter ycenter pa 0 123 lt xcenter gt and lt ycenter gt are the X and Y values of the slit image center on the detector which were measured in the last section These numbers will be close to 128 and 510 but will differ slightly for each filter lt pa gt is the position angle of the 4 m instrument rotator 0 123 is the 4 m plate scale in imaging mode For all observations ask this command sets up the observing parameters for this observation eask determines which parameters are set by ask abba 10 number of repeats 10 is the nod A B separation in arcseconds This corresponds to the east 5 and west 5 that were used above This is a good value for
30. te for the spectrum of this bright star use ITC If star is very bright multiple coadds can be used to average several very short exposures east 5 This moves the star to the bottom of the slit go In IRAF Measure signal using imexam and the j key In Wildfire north 0 5 go Then measure signal repeat these steps moving the star small amounts north and south perpendicular to the slit and recording signal When you find the best signal move back to this position confirm reading and mark on TV screen Then move west 10 and repeat the process When done move east 5 and re mark point at the middle of the slit The middle point is just used for acquisition so there is no need to peak up the signal here NOTE Remember the slit position will be different for each filter 5 4 Fine Tuning the Grating Position Using the best pair of bright star spectra obtained during the above peaking procedure or by observing a new pair of spectra with the star at the east and west ends of the slit In IRAF imar east spectral image west spectral image diff image twodspec apextract apall diff image Apall is the IRAF spectral extraction task It will begin by asking a number of questions about finding apertures Answer yes to all 1 to number of apertures to extract You will then get a display of a row cut across the image showing the negative and positive spectral sections There should be an aperture marked o
31. the open position to protect the detector and filters from condensation see Section 5 4 Startup in Special Circumstances Because of the complex organization between the Sun computer khaki the DSP and the Instrument Power it is necessary to establish communications between these in the proper order Once this has been done restarting WildFire is fairly straightforward as described in Section 3 However there are situations in which the simple startup will not work such as e The computer software has crashed for some reason If this happens first try using the Kill Phoenix button on the Phoenix menu to close all of the processes then Start Phoenix as described above Depending on the cause and severity of the crash this might work e There has been a significant power failure which affected the Instrument Power DSP or khaki or any of them has been turned off for any reason e Communication through the fibers has been lost for some reason If this is suspected check the red Error LEDs on both the DSP and the Instrument Power If any of them is red there is a hardware communication problem which must be repaired before attempting to run WildFire e The instrument has just been installed on the telescope since the Instrument Power will have been powered off 4 m Phoenix User Guide V2 04 15 April 2015 10 1 Before starting the procedure particularly if the instrument has just been installed make sure that k
32. the 4 m abba will take four spectra The default number of repeats for the abba script is 1 4 m Phoenix User Guide V2 04 15 April 2015 18 The command ab nod number of repeats is similar to abba except that it just does one observation at each point 5 5 1 Observing infrared bright visually very faint objects If objects can not be seen on the guide TV they must be acquired in the IR using the imaging mode Tracking on the slit can be done using an offset star and the guide camera provided one is visible in the field In the near IR In Wildfire viewer image slit your science slit ask go This images the slit Record the mid point This needs to be done once slit open ask If the exposure time is very short coadds 10 will average over 10 exposures go east 5 go west 5 In IRAF imar fimagel image2 some name for the difference image displ name of difference image 1 This displays the difference in the ds9 window Measure the position of the positive star image In the thermal IR The sky will likely saturate the images Use the neutral density filter in the cvf wheel to reduce the flux This filter is not intended to be used in spectroscopy mode so make sure it is removed prior to science observing For both near IR and thermal IR In Wildfire 4 m Phoenix User Guide V2 04 15 April 2015 19 recenter x pos y pos Note that recenter requires a previous use of zcenter If you have not ye
33. um 1 9 2 8 4m 5 1 7 L3290 L2870 84um 3 0 5 0 2m_1 1 8 K4484 K4396_ 107m_1 0 5 0 2m 1 5 9 M2030 K4667 lyot_viewer 2m_2 5 10 J7799 H6073 open 2m 3 6 11 K4798 L3100 plus 2m 5 1 12 H6420 dark 4m mask 2 5mag 1 5 13 J9440 4m mask 2 5mag 3 0 14 2m mask 2 5mag 15 mask 5mag 16 secondary mask 4 m Phoenix User Guide V2 04 15 April 2015 27 Table 2 Phoenix Order Sorting Filters Name Filt CVF cm um Encoder Order Range cm M1930 1 3 1890 1970 5 076 5 291 14764 11 1926 7 1934 3 M2030 9 1 1980 2030 4 808 5 050 7897 11 2024 3 2035 7 M2150 2 1 2105 2190 4 566 4 751 5208 12 2144 7 2155 4 L2462 1 5 2410 2495 4 008 4 149 13603 14 2456 4 2467 6 L2734 4 1 2680 2770 3 610 3 731 2131 15 2726 7 2741 3 L2870 1 7 2820 2910 3 436 3 545 4716 16 2862 8 2877 2 L3010 1 4 2950 3050 3 279 3 390 10368 17 3002 9 3017 1 L3100 1 11 3030 3145 3 180 3 300 2340 17 3091 7 3108 3 L3290 7 1 3240 3355 2 980 3 085 22532 19 3283 2 3296 8 K4132 4077 4156 2 406 2 452 4064 23 4121 6 4142 4 K4220 5 1 4188 4263 2 348 2 392 13670 24 4210 4 4229 6 K4308 6 1 4258 4355 2 296 2 349 4421 24 4297 2 4318 8 K4396 1 8 4355 4446 2 249 2 296 13651 25 4386 0 4406 0 K4484 8 1 4429 4525 2 210 2 250 4751 25 4472 8 4495 2 K4578 1 6 4525 4630 2 160 2 210 12987 26 4567 5 4588 5 K4667 1 9 4617 4717 2 120
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