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Project 1640 Design and Operations Documentation

1. Br i M Ls el e gt e KaR AS 2 Project 1640 Design and Operations 2 M c E us Ss Sk ae BE BEVEL 500 MAX FW sol D w A gt 4 i H i PA RBS 497920 087 Mo 52 2 64 25520 010 E amp 93 74620 094 WET A lt a per CT 14 90020 050 A Nar SECTION A A 1 OS os PIERO wx O X90 M t 7 MA M QuA TY nap me por 3 5 AND 3g AR N ea tr a a MAGA tem vG QN TO qM Hor C 1 a aama Mir ON AND Acres tat PER vu CABIETA g NOL 3477 34 2 AD34 23 ft Pads sme conma AAA CES OA aL fum Du DAMNA TEMO MA 0 Se COLUMATOR LENS 45 A nnl A 41362 505 A a E y IAL Mv Poy pet 2 224 Project 1640 Design and Operations 4 4 Camera Lens Mount Drawings dee i A 3 Veras a Dire e Leo rad b audi aro upps t unnn E GE lt N AN Project 1640 Design and Operations 225 y O P gt NATE O heme of Asuorcmy iara cot tt lal 226 Project 1640 Design and Operations unnn a al Borie P oe M AL CEL S e cara TT Project 1640 Design and Operations ELLE AX 4 Lm Poo ee a ee A ae Le NI esae cineres me manm ST Lal 220 Project 1640 Design and Operations 4 5 Detector Circuit Diagrams ee htt on XR a C Rf i i AA ce ADAADA TEA ttm A Hi i KA a d EE TITT oe o r a e Figure 194 Wiring diagram for SDSU four channel control
2. sees 184 3 3 60 De installation and stowage procedure is 185 Dod MARINO TOCE CURE ed n edd 185 0 9 0 daafnsportand MP coi sts e NERIS SS OO S RN US URSI NERIS nU SE RAI uS tut 185 Ds DOWWE Contra 186 obl AC a DE e a ROO 186 4 Project 1640 Design and Operations Dopo User A att air e eot Lent 191 9 0 JElectronics Coni urio cereri te 192 ole Decir I O a a ode dut N 192 3 9 2 Instrument Pressure and Temperature Sensors 192 0 929 Casera Cage aca 192 Sx Control Room uiuunt 194 o op EE Corio ED 194 94D ii A RO 195 E O cda 195 245 25 LA tio 196 A A o os 197 JOA Acg nino Cia ND Pat Oi Data 200 DOs COPE EXPO We redu m LL ILLI 200 3 6 6 Procedure Summary for Observing One Star 202 9 4 Data Proc io ttn ot tuos ated tac nee np eia etu E cud 202 ou Data Pipeline E CA A EEUd E uetU SR d bote UU tede 203 A a lr tae O A eO ER dte ih sete enne o dtess 203 3 7 3 Using the Data Pipeline Provisional for March 2010 run 204 3 7 4 Procedure Summary for Running Pipeline Provisional for December 2009 run 206 3 8 Observatory Testplan Commissioning Run ooooooocccccncccncccccnonnnnnnnnnanananancnnnnnnnos 208 9 9 JDatadxeducton Martial eto be ON T EE 211 d APPEAR 217 Wels Data ide San le su o UOCE t te EL i De NE 212 4 2 Coronagraph Optical mount Diagrams eee 215 do Colimatns Optics Drawing a 221 Ld Camera Lens Mour IIS iii 224 do
3. l DOS aaa tT 300 1 50 10 qu Cd too jal Z Ir A DG 2212 10 AMMR B This piece is Figure 51 The outer warm portion of the dewar snout screwed directly into the outer wall of the dewar 54 Project 1640 Design and Operations ARE A SO MAX IW SE VEL lt FO MAX FW e ica mb UNLESS OTWMERWSE SPLCT XO VLON APPLES A NOS ATINA AJ weit QUAL TY l A a m y Eon MAL as T TOM NI gt L Cb Y x z temae es osx DEWAR ENTRANCE WINDOW 41360 504 A Figure 52 The CaF2 dewar window 2 2 3 Optical Design and Optics The optical design for our integral field spectrograph is shown in the Figure below The overall design can be categorized into four components a lenslet array a dioptric collimator with a 200 mm focal length consisting of five lenses made up of three different glasses SK8 SF2 Bal which re images the telescope pupil on the prism a prism disperser element and a camera component All our transmissive optics except for the lenslet array were manufactured by Janos Technology while the reflective optics were manufactured by Axsys technologies We discuss each of these components in more detail below The optical design has been fully modeled using the Zemax design software including the effects of thermal contraction as the system 1s cooled The system does not perform at room temperature All optics with the e
4. Figure 107 Detail on the input plug to the Lakeshore 331 Temperature controller The input to the controller is a six pin connector with a pattern shown above The wires in the cable corresponding to these pins are colored as shown above in the table Table 7 The pins in the Detoronics plugs are wired to the temperature sensor wires as shown below Temp Poe Sensor A Cold Plate Vig E RAY V V lead gold E lead green o bo lead gold Resistor wiring Two resistors connected in series C lower case not capital Project 1640 Design and Operations Gerd cot aman st gd DOR ee ed LT aima Them rota 115 0 240 im 0 015 amp WI PO wt mnl nm J CELA 19 304 me 6 096 mm 6 219 SM el 3 958 me 6 096 ma 10 108 Generasi tolerance of 10 00 in 90 127 men unies otherwise noted Figure 108 The Silicone diode temperature sensor upper left This diodes 1s housed in a M3 screw housing as shown in the upper right and lower image 116 Project 1640 Design and Operations Figure 109 The back of the detector mount showing the resistors connected to the back plate and the temperature sensor screwed into the copper block in the PCB The four 1 4 20 screws fix the plate to the detector frame the smaller screws to the copper block Project 1640 Design and Operations 117 2 3 Wave Front Calibration System Pupil Alignment LI Mirror Phas
5. 3 9 9 5 AMNH Lab Configuration We created a subnetwork at AMNH using Palomar IP addresses Our fiber switch in the rack is connected to another fiber switch in the 5 floor closet via an ST SC MM fiber in Fiber port MM2 in the electronics room That switch 1s connected to the AMNH Internet via a firewall router PIX from old Lyot Project This firewall allows incoming and outgoing traffic to from the Palomar AO system and the Palomar TCS since it is on their subnet and gateway but on the museum s DNS servers 172 16 5 15 and 16 Our firewall has the AMNH internal IP address of 172 16 32 28 Exterior to the museum it has a dynamic IP address can be found at whatismyip com from any computer behind the firewall This IP address will change each time the firewall PIX is rebooted This may be an issue for Palomar If so we request from Kurt or Shadi that our firewall be given a static IP that Palomar allows incoming and outgoing traffic from to Doug s computer Jack in his office R94 384 1s on this internal network as well behind the PIX firewall so that his computer 1s also configured to be on the Palomar IP addresses but with the AMNH DNS server In this way our rack components and the main control computer all have Palomar IP addresses 198 202 125 164 170 the Palomar subnet mask 255 255 255 128 the Palomar gateway 198 202 125 129 but the AMNH DNS 172 16 5 15 16 When we move to Palomar we need only change the DNS on al
6. After about 7 minutes of filling the gushing noise should stop and the flow of LN2 is a bit quieter as some liquid begins to gather in the large tank After about 15 20 minutes the large tank will be full The temperature on the sensors will go down to 283 285K at the end of the large tank fill and reach about 260 265K after one hour past the fill start time The rate of temperature change as determined by the sensors may be as high as 1 0 deg 100s The pressure will fall significantly to between le 03 or le 04 mbar depending on whether or not the vacuum pump has been left attached e A Y m i Figure 163 The temperature when only the large tank has been filled Some data between 16 and 24 hours was missing and has been extrapolated 5 When the dewar has reached about 95K it 1s safe to put very small amounts of LN2 into the small tank This can be done using the stinger or simply pouring some liquid in via a thermos or cup If pouring in only pour about 4 cup at a time The temperature on the detector can change rapidly even at these low temperatures The plot below shows the detector temperature after adding some LN2 into the small tank starting at about 105K probably a bit high Note that even at these low temperatures the dI dt value can still approach 1 degree K minute After about 2 5 hours the detector has reached operating temperature The holding period for the system 1s shown in the last plot below The system seems to c
7. 514 Figure 95 This drawing identifies the corner at which the marked portion of the detector pins must be mounted see text 104 Project 1640 Design and Operations Figure 96 The PCB front left and back right showing the copper block heat sink The four M5 screws secure the entire PCB to the plate in the back of the detector mount see drawing of copper block holder below 2 2 5 5 Detector mount and detector cabling The printed circuit board PCB assembly is mounted onto the upper portion of the detector frame via the PCB s copper block and the aluminum plate shown below called Copper block holder This copper block holder is bolted via four 4 20 screws in slots which allow the aluminum plate and hence the detector to slide vertically up and down Figure 97 Left The PCB with test chip carrier The detector cabling travels down through a trough in the detector mount plate through the optics baseplate to the vacuum feed through socket Right the field lens with cell retainer mounted in front of the PCB In addition this upper detector frame piece is capable of x y movement in the plane parallel to the optics baseplate This 1s accomplished via an intermediate plate shown in the photo below This intermediate plate has screws 1n slots to allow the side movement as well as a rail to guide the upper detector frame for the forward movement These movements can happen independent of each other as large
8. Figure 37 The positions of the four pucks on the underside of the bench are marked on the work side of the bench 2 2 IFU The second major component of Project 1640 1s a lenslet based integral field spectrograph IFU hereafter operating in the J and H bands 1 05 1 75um The spectrograph is entirely encased in a cryogenic dewar that is cooled by liquid nitrogen operating at roughly 10 Torr 104 mbar when cold Starting from the outsided in this section gives an overview of the primary components of the IFU The cyrogenic dewar the optics and their mounts and the detector system 2 2 1 Dewar Our cryogenic dewar is very similar to that used for the PHARO infrared camera at Palomar Our dewar was built in 2006 by Precision Cryogenics in Indianapolis Indiana The dewar is made almost entirely of 6061 T 6 Aluminum with an outer shell divided into an upper and lower part The upper half ranges from to 4 inches in thickness and provides strong support for the overall assembly while the lower part is lighter weight These two halves wrap around the workplate the inner heat shields and the two Liquid Nitrogen LN2 tanks and each half has a Y inch flange or lip where the two are joined The optics workplate is comprised of a 1 inch thick light weight piece of Aluminum and is mounted to the outside of the dewar at the lower flange by four G 10 fiberglass mounting tabs These tabs help the workplate to be thermally insulated
9. hold the red button down until it goes solid This should turn on the Lakeshore controller and if you then go to the front of the electronics rack you will see 1ts blue LED screen on at the bottom left of the rack It should be reading out two temperatures generally within a degree of each other 3 2 4 2 Filling procedure The inner small tank can only be filled when the internal dewar temperature has dropped below about 95K At no time prior to this should any Nitrogen be put into the small tank Doing so could destroy the detector system in the instrument Note also that the placement of the two cans are different between PHARO and P1640 In the optics down configuration on the telescope or on the AO spit two LN2 vent tubes one for each tank are screwed into the two tanks to both allow the Nitrogen exhaust gas to vent as well as prevent the liquid from pouring out These two tubes are screwed via their brass threaded midsections and are nearly 1dentical to those for PHARO see photo Figure 167 Detail of one of the fill tubes left and showing how these are inserted into each tank Steps 1 Verify that the pressure gauge 1s plugged in and 1s near 0 1 0 2 mbar 172 Project 1640 Design and Operations Figure 168 The inner and outer tank fill ports Each 1s identical to PHARO but are in different places Also unlike PHARO insulating foam has been placed on the fittings 2 To fill the oute
10. 3 3 7 Crating procedure Figure 184 The AO spit 3 3 8 Transport and Shipping Shipping from AMNH to New York was handled by Dietl International contact 1s Deirdre O Connell 212 400 9555 doconnell dietl com via aircraft Airport supervision was in place at both JFK and LAX airports The delivery to the Observatory was handled by a covered alr ride truck The crates were unpacked in the ground floor of the 200 dome before moving the contents into the AO lab The empty crates will be stored at Palomar When shipping the instruments in the future the same procedures need to be followed Table 10 Weights for all project components Project Component Weight Ibs Handline cart instrument Handling cart alone IFU Coronagraph with Nitrogen Electronics rack with all cabling 186 Project 1640 Design and Operations 3 4 Software Configuration 3 4 1 Structure and Design Ben s notes Need lots of detail on AO Central FSM Computer DAC Regarding DAC server stuff launch script commands by xml SSH stuff from Doug The software interface to the instrument is a LabVIEW front panel designed to give the user control of taking 1mages powering parts of the instrument There are five main tabs on the front panel System Init Tab The system init tab contains several controls for powering on and initializing subsystems of the instrument Power Control box Allows the user to power on and off the Temperature
11. 60 declining to lt 50 and significant persistence effects due to lattice mismatch between the HgCdTe detector and its sapphire substrate Problems with amplifier glow in HAWAII 1 devices are expected to be solved in the HAWAII 2 devices but this is yet to be verified Integration time gt 36 hours 16 data samples T amp 3 cumulative distribut on s 04 electrons per second EF o xes ari bon Figure 85 Dark current distribution for Hawaii 1 array Quantum Efficiency Project 1640 Design and Operations Tz78K Areaz3 423e 6 9 34R SWIR1024 Peakz1 970 um Cutoffz2 579 um 1 2 2 4 1 6 2 0 Wavelength um Figure 86 Quantum efficiency function for HAWAII 1 dectector HAWAI Array Noise Performonce 65 K Operating Temperoture Ta LS nb ns L see I miy Jee Of O c ne d vt 500 Sec exposure e te DIR ROG Rd e IIS Sec exposure Figure 87 Read noise for a HAWAII 1 array measured at 65K with 250 mV bias as a function of number of correlated double samples The rate of ionizing events per pixel for the HAWAII 2 array with 18 um pixels will be more than a factor of two lower than for the 27 um pixel ALLADIN 1024x1024 InSb arrays Project 1640 Design and Operations 95 used in NIRI and GNIRS Mackay et al 1998 quote cosmic ray detection rates with their HAWAII I arrays of 1 event per square centimeter per minute corresponding to 815 events detected by a HAWAII 2 array in a 3
12. 75 20 HD AD C 20 PD over Y TUBE ANA VENT PIPE Figure 203 Design drawing for Liquid Nitrogen vent tubes Both vent tubes have a nylon washer to seal the Nitrogen in the cans and preventing draining 236 Project 1640 Design and Operations 4 7 Parts Inventory Project 1640 Part Inventory updated 7 7 08 Item Qty Primary IFU Coronagraph Handling cart Electronics rack IFU Coronagraph handling cart crate Electronics rack crate Miscellaneous crate eo vacuum amp cryo accessories KF40 to KF25 adapter KF40 clamp KF40 caps blanks Lesker series 900 gauge controller Custom KF25 dry Nitrogen adapter LN2 vent tubes N mB HL NN H mp Electronics 1640 Control Computer Control Computer keyboard mouse 1 each Tip tilt Etronix computer monitor 3 button Mice bag of fiber caps Leach to detector plug cable IR fiber yellow IR fiber orange Fibers for rack to cass patch panel Pupil cam monitor serial CIW16294 black Dell Keyboard power cables Detector resistors pi m QJ NJ HA H H5 H HE H Hd N N Tools hex key set non metric 1 hex key set metric 2 metric wrenches 10mm 15mm set 1 non metric wrenches 3 8 5 8 set 1 phil Scwdrvr box cutter wire cutter 1 each magnum marker 1 exacto knife set 1 adjustable spacing optics ring remover 1 fixed spacing optics ring remover 1 mini mag lite 1 1 4 20 screw kit 1 Dewar rad shield screws 1 bag each 8 32 nylon tipped steel s
13. CO O 2 2 t we a MB i MA os aran uc ww Ww Y ao lt TA l 5597 Ar JE 750 AX PW BR 500 MAX Pw i p 4 P d 2 i I 6 PO CER b L Hr SECTION A A Qd 4 gr E JANOS 51 I LEIOA 4 44910 023 2 j 875 192 0 075 20 254 SAG B4A0 0 025 o Ciz 40020 00 L7 010 8 m A ooo Ih 2 00 UB e EAA sns dnd at e s a CO i gt AA vm w uem 4 9o E M a 0 m we c A 4132 02 A OAC mrs qn tvm Dual COLUMATOR LENS 2 Te Wow Mow peu Sv 221 222 Project 1640 Design and Operations 2 mon e he b war 8 I NM m um cm wm es 1 usa e e a A y ya 5 vw sm men o we LESE A 2 A ww wow jw eI KA ESS COLUMATOR LENS a I A QC amp ise Ipasa wee o LEE ra F 9 4 ad i gt Fr 4 Ww Dew wo n YA MICA 8 Se 0 9 C re AAA LA PRA A 41362 503 A ZI t as CA uv mou peut 2v 2 2 V e T ana Li a gt UM ium om opt ov 0 LR Lun a a ur w w sw tase wr LT a a u QE s s e rd RA COLUMATOR LENS 44 o wien Lope wee A aal ca m 1 UJ oem to m 15 De te Jen 8 amp oe eee FL we Ape gt ee l T
14. Crowded Field Barnard s star Doradus Deep Field Coronagraphic performance as function of V magnitude Young stars Altair Rasalhague type A additional binary position HIP98767 other high priority targets from Lyot Project Continue with science observations Verify and Implement data backup procedure July 11 Departure noon Project 1640 Design and Operations 211 3 9 Data Reduction Manual Figure 192 Initial data from the instrument Top left the IFU has been illuminated with a 1330nm laser showing the exptected pattern of dots Top right A uniform light source Lower A broadband APLC image on an IFU obtained in the lab 212 Project 1640 Design and Operations Start with N sequential observations data cubes h Create minimum Image cube Y 2D Collapsed image y L imet spectrum Latched filter gt gt Compare y Defne annulus spectra JS Figure 193 Preliminary data reduction strategy 4 Appendices 4 1 Data File Sample Header SIMPLE T file does conform to FITS standard BITPIX 16 number of bits per data pixel NAXIS number of data axes NAXISI 0 length of data axis EXTEND T FITS dataset may contain extensions COMMENT FITS Flexible Image Transport System format 1s defined in Astronomy COMMENT and Astrophysics volume 376 page 359 bibcode 2001A amp A 376 359H BZERO 32768 offset data range to that of unsign
15. DTBbBE Disk Bright Faint Binary Exoplant Other DISTANCE 144 Distance pc SPC_TYPE AOe Spectral Type AGE 650000 Age Gyr IMG TYPE O i Core Occulted etc TOT_EXP Total number of exposures EXP NUM 1 l This exposure number EXP TIME 6 707000 Exposure time for each image ST_TIME 6 4 08 7 43 46 PM Exposure start time UT POINTING RA 04 55 31 60 RA in hours J2000 current ep amp eq DEC 30 34 36 38 Dec in degrees J2000 current ep amp eq INTT_ALT 33 094813 Initial altitude 1n degrees INIT AZI 353 392362 Initial azimuth in degrees INIT PAR 82 562940 Inital parangle in degrees INIT HR 4 550858 Initial hour angle in degrees INIT AM 1 831414 Initial air mass FINL_ALT 33 033597 Final alatude 213 214 Project 1640 Design and Operations FINL AZI 353 390383 Final azimuth FINL PAR 82 546847 Final parangle FINL HR 4 555977 Final hour angle FINL AM 1 834422 Final air mass RA OFF RA offset in arc secs DEC_OFF i DEC offset in arc secs RA T RAT i RA track rate in arc secs hr DEC RATE DEC track rate 1n arc secs hr CASS ANG i cass ring angle AO_DATA WES X offset for WS field stop center to WES Y i detector center arc secs FSM_INT FSM gains FSM_PROP i DM INT DM gains DM PROP z FSM RATE i FSM update rate WFS RATE WFS camera readout rate CON
16. gt 71 i i i r F LI i Uu i Figure 72 Internal bracket for spherical mirror mount Transmissive Optics Project 1640 Design and Operations 75 There are two transmissive optics in the camera portion of the spectrograph the meniscus and field lens Both are made of fused silica The meniscus corrector lens has two surfaces with radu of curvature 216 82 and 227 90 mm and was cored out of a larger 240mm diameter parent lens Itis 14 4 mm thick 70 mm in diameter and 80 mm off axis The field lens creates a flat focal plane for the final detector This lens is incorporated into the mount holding the detector and has adjustment capabilities in three dimensions This lens serves the double purpose of additional protection for the detector The field lens has a rear flat surface and a front surface with radius of curvature of 105 55 mm This lens is 57 mm square and 12mm thick Figure 73 The meniscus lens left and the field lens right Project 1640 Design and Operations 2 j 140 26 735 BEVEL 1 000 MAX FW i 2 rt R216 82020 217 i 2240 000t0 050 Fi i y 1 y l 2227 900 0 228 y a C7 14 40020 050 fecta UNLESS OMITA SPOOF ED V1 O APPLES 2 VATEREAL PUSO SCA H8 ORADE NH QUALTY am ten JANO 3 ANO 32 ARE PAOLO a 4 SECOND WEDGE SAGA CT Nu OS O2 wa one CAMERA LENS PARENT SE IEEE m A 413600 A KALE 349 EM PAN yu Ve i 2 Figure 74 D
17. i o e f I Az i k sal LL oi u Jj La j e u e 21 pa 3 t 7 t e Jia i S j aT Un f ys LJ B ci ret Y har zz LL ll Y r3 n ml 9 be O tite J qu j e m l I a re E A LIA n CJ i amp pa bh 3 o p am d n 2l e i 44 44 Ea Uu e J Fi ge gt CO I rt Ss 1 s I E de d _ _ 1 A P ee ow 6 a 5 b 4 c j go RACAR n gt 1A On LL me ore mn gt E NM 5J CJ L4 LL y c O e my gt pau m j I rz u LI LLJ A 7 y E rm 11 TL e TA Y nh a wg t CT i m J de md 4 mr S f T nm c had s i y i 3 Hi a te i uf 4 A ai gt i i A A is L j J I t Q pa m A A a 7 o L LIJ y A 1 a y 2 p C29 T CX het Pul J O rs ix u y y ii I OY fr Y J OL 0 Vul wt C Lu occo am 92 Project 1640 Design and Operations na e a m c G A mm m SO 22 22 225 _ a e A 2 2 2 5 Detector System The heart of the detector system is a Rockwell Hawan 11 2048x2048 pixel HgCdTe infrared array operating at cryogenic temperatures The detector control uses a Generation III infrared array controller designed and built by Astronomical Research Cameras Inc ARG and configured to our Hawai 2 chip We also have a dedicated ARC power supply to go with this 2 2 5 1 Hawaii
18. 0 0752 0 0758 0 0763 0 0768 0 0773 0 0778 0 0784 0 0789 0 0794 0 0799 0 0804 0 0810 0 0815 0 0820 0 0825 0 0830 0 0835 0 0841 0 0846 0 0851 0 0856 0 0861 0 0867 0 0872 Project 1640 Design and Operations 0 0261 0 0246 0 0230 0 0214 0 0197 0 0181 0 0164 0 0146 0 0129 0 0111 0 0093 0 0075 0 0057 0 0038 0 0019 0 0000 0 0020 0 0040 0 0060 0 0080 0 0100 0 0121 0 0142 0 0163 0 0185 0 0206 0 0228 0 0250 0 0273 0 0295 0 0318 0 0341 0 0364 0 0388 0 0411 0 0435 0 0459 0 0483 0 0508 0 0533 0 0558 0 0583 0 0608 0 0634 0 0659 0 0685 Project 1640 Design and Operations 27 1 7969 55 681 0 138 0 0285 0 0877 0 0711 1 8075 55 679 0 142 0 0312 0 0882 0 0738 1 8181 55 678 0 145 0 0339 0 0887 0 0764 1 8288 55 677 0 149 0 0367 0 0893 0 0791 1 8394 55 676 0 153 0 0395 0 0898 0 0818 1 8500 55 675 0 157 0 0424 0 0903 0 0845 2 1 3 1 ADC Calibration steps from Nick Law I d be happy to share my ADC control code It has all the calculations you d need to get the ADC working calculating rotation angles as a function of time and target coordinate and so forth but it has no TCS interoperability We just typed the sky coordinates into it when we went to a new target This was hardly ideal but worked well enough for a few nights is it those calculations that you re after For calibration we tweaked two things the total ADC rotation angle and the strength of th
19. 226 mm and a diameter of 130 mm We also utilize two fold mirrors to accommodate packaging All mirrors are made of diamond turned aluminum coated with nickel polished to 4 20 RMS surface error Figure 69 The Spherical mirror which forms an image on the focal plane array left and the fold meniscus lens assembly All mirrors are diamond turned aluminum coated with nickel followed by gold 72 Project 1640 Design and Operations o E ds gt U z ta ZO a a e ml ai wt gol i gau 2s i 5 3 Y Zi m1 AS o i P w j PF 0 PA N C o Of A n o g i o 3 Q a 4 Figure 70 The layout of the Axsys optical mounts Spherical mirror and fold meniscus assembly relative to the optics baseplate Project 1640 Design and Operations u I sif z i I if i o gu HP Y Lv ime est wn ewe a o oo i 8 g BN v A aM Er 1l 8 oe TE gt a E a L Fd st E amp Figure 71 Spherical mirror mount Project 1640 Design and Operations z o ate 2 7 za 29 3 ali uw i eo Li eee i AL i F Qi y Zi 7 j 5 F 9 has hm 2 Y _ F I gt a i E i i j J i i i gt i 5 ki 1 gt P a i LJ j f i 9 pi
20. 8 32 screw and held to table with clamp parts PS B 1 SS 1 A PS 0 125 PSF height 2 375 inches 2 1 1 11 Lyot Stop Beam splitter for Cal System Optic l inch flat with gold coating A 20 superpolished supplied by Opticology initially when Cal System 1s integrated this must be replaced with an 80 20 mirror Lyot Stop Wire EDM machined 50 um thick pupil pattern with spiders aligned with the telescope s up down left right placed on the optical surface Spiders are black anodized Mount Newport VGM 1BD custom baseplate to match VGM base holes and flange for clamping to baseboard part AMNH1640 2 with angle Height 2 400 angle is 7 and 9 Figure 15 Design drawing for Lyot mask Current as of Fall 2009 Lyot Mask design description for CTM Palomar Order 4 Sep 15 2009 dea Al Lego eur ia edge Source Repeat Palomar 3 order Clossic Lyot and unobscured pupil Add APLC from older Soummer CTM orders ID and vanes remain some Al part OOs 1 Vendor Joho J Piseck john ctm corp com 1 866 CTM CORP 1 866 286 2677 315 894 4377 Ent 227 CONSTANT PARAMETERS PART OD 25 4mm 0 0 0 1mm 1 PART THICKNESS 0 003 inch VANES Symmetric 90 degrees PER ITEM DESIGN PARAMETERS Cross Section before 0 00290 fine electrode drilling Q Part OD 254 5 0 0 0 1 mm 1 inch Anand Sivoramaknshnon Office 212 313 7653 Cell 410852 2201 andrea Project 1640 Design and Operations 1
21. AAA AA NNNM SC ENTCECOROSCCRCRSCONCCONC CROCO nd NOD AA E 40s Qd 800 Wan Ow A i Figure 40 Production drawings showing internals of the P1640 Dewar Project 1640 Design and Operations 45 Figure 41 Lower wells in the P1640 dewar left and the small tank fill tube right showing its o ring crucial for vacuum integrity Figure 42 The heatshield retaining rim being removed left and the two LN2 tanks after the optics plate has been removed right The small tank 1s evident on the right side with its fourteen 10 32 tapped holes The large tank 1s soldered to the heat shield Project 1640 Design and Operations ea 4 PELA mmm mp y j y US i m a usin i ur PPS mum f t 0 4 ee rrr m CE eee lee ILI LIS MA Y P pr 45 Figure 43 Some of the dewar internals showing details of the filling 1f a vent pipe is being used bottom and the mechanics of the outer LN fill port boss Project 1640 Design and Operations 47 T i Project 1640 Dewar Baseplate Figure 44 Production drawings of the P1640 baseplate Project 1640 Design and Operations Baseplate 4 j Project 1640 Dewar Figure 45 Production drawings of the P1640 baseplate Project 1640 Design and Operations 49 MA d A 2 i Ln Project 1540 Dewar Basepiate ow o 5 9 f 7 f F
22. Apodizer AO input beam Fast steering mirror OAP1 Figure 10 Same as the above figure but excluding the final spherical mirror Figure 11 Side view of the P1640 coronagraph Project 1640 Design and Operations 15 Figure 12 Isometric rendering of P1640 coronagraph with IFU purple dewar 2 1 1 1 Infrasil Window Optic 2 inch flat made of infrasil 302 10mm thickness AR coated for 0 6 2 0 um Lambda 20 rms irregularity at 632 8nm Less than 0 05 waves surface power at 632 8 nm Scratch dig is better than 60 40 and less than arc minute wedge Mount Newport U200 G2K NL thumb actuated gimbal mount and custom base riser with 45 degree cut out to fit base of the U200 Also included are flanges to allow clamping to baseboard Drawings list this part as AMNH1640 I height 2 400 2 1 1 2 Fold Mirror 1 FM1 Optic inch flat with gold coating 4 20 superpolished supplied by Opticology in New York City Mount Newport VGM 1BD custom baseplate to match VGM base holes and flange for clamping to baseboard Some drawings may list this part as AMNH 1640 2 Height 2 400 See appendix for detailed drawings of this mount 2 1 1 3 Off Axis Parabola 1 OAP1 Optic Lyot Project OAP2 removed from mounting bracket 16 Project 1640 Design and Operations Mount New Custom L bracket with interface to OAP2 s 3 tiered holes Shims to adjust position for alignment Drawing will list this part as AMNH1640 3 Thi
23. ICL LILLIE LLL LLL lle III 12 1 12 Imm TnT TETTIE III IITTITIITITITTITISITETTITIM 12777171717 T 1712713107171 1 te ete 2 set Figure 59 Machine drawing of the microlens array The lines going off at 18 43 degrees from vertical define our degree of rotation ptit n ceUeg e n z EC LI 20 10 10 20 Su qe sm am g m ge e a n l c hd MM E IM ECTOR DEPULUS i um THEOLICZI FOCUS SPOT DIAGRAM M i bete M I I Le 2 D NI T pal i H i I 4 Ds iH OUMLE BER LMibh MM CONFIG OF 2 Figure 60 Zemax spot diagrams showing lenslet array defocus Project 1640 Design and Operations 63 Lenslet Array 20 x 20 mm at 19 47 1 3 or 18 66 Alignment Marks to indicate lensiet ond angle Angle and grid not drawn to scale here 30 x J0 x 1 mas IR Grade Pused Silica Subotrate w MgF AR coat optimized for 1 3 um Figure 61 The IFU field of view superimposed onto the rotated lenslet array schematic 2 2 3 2 Collimating Optics The collimator assembly consists of five lenses mounted in a single housing The lens materials are BaF2 SF2 and SK8 detailed drawings of each lens are given in the appendix The collimator forms 40 mm pupil images at the prism s incident surface The collimator assembly is secured to its mount via four 8 32 screws from the underside The mount is a single piece of aluminum which serves also as the mount for the prism Using a single mount ensures al
24. NI 135 YM3Q 4314v Q311v15NI Sav ID Q3ONwYH2 38 OL SNid CONI INIOTIOW M Y 30 So 8C T DNI ADO TO DUO M3 A83A0 A19W3SSY gos 3i AW38 LANNOJ for mounting the dewar into its handling t iption Descr Figure 116 mechanism Project 1640 Design and Operations Figure 117 Design drawings of the dewar support and focus mechanism 123 124 Project 1640 Design and Operations Figure 118 Design drawings for the carriage portion of the dewar focus assembly Project 1640 Design and Operations 125 Figure 119 The customized rear dewar mounting pin which is bolted to the rear of the dewar and connected to the screw jack mechanism 126 Project 1640 Design and Operations Figure 120 The two front dewar mounting pins are identical and shown in this design drawing These are mounted directly on the dewar Project 1640 Design and Operations 127 Figure 121 This baseplate for the rear rail is bolted directly to the Thorlabs baseplate for the instrument The longer rail is bolted to this baseplate via three M6 screws The focussing screw is not shown in this drawing 128 Project 1640 Design and Operations Figure 122 This mounting plate for the rear runner block is bolted to the block via the four M6 tapped holes This plate in turn is bolted to the upper carriage portion of the handling mechanism via the 4 20 holes towards the front Note that only three of these 4 20 holes are used Project 1640 Design
25. P peeves HP171 m HIP107354 Slice 20 1 69 um pixel scale d 19 21 mas pix os11102 P mpesa ae HIP171 Slice 23 1 78 uum pixel scale d 19 33 mas pix os11102 O pestes apra y HIP107354 500 Physical sep mas 1000 1500 Figure 191 Project 1640 pixel scale measured using four different binaries and 12 channels 208 Project 1640 Design and Operations 3 8 Observatory Testplan Commissioning Run June 10 13 Final software version Lab Data for validation tests Hg Lamp ordered Schedule movers for 6 23 June 16 Neil Sasha test for several hours in mock observing run June 17 Last software Bugs Removed Begin dewar warm up maintain vaccuum Swivel casters installed on handling cart Optics covered check for loose parts Uncabling of instrument Cables rebundled for observatory ops Seal optics and secure instrument internals June 18 Instrument mounted on handling cart Rotation and balance tests Install 0 15 shims beneath pucks Rubber for beam entry hole June 19 Pack loose parts E rack computers KVM etc Write inventory Remind Rick Mark C about WFS accelerometers June 20 Safe Art Transport personnel to finish packing June 23 Dietl to pickup 3 30 pm June 24th Sasha Ben Doug Arrive 12 09pm SAN 3 30pm Palomar June 25 Brief visit from JPL people early afternoon to see instrument for CAL system issues Marty to send list of people
26. block soldered to the back of the printed circuit board In addition we have two 2 5 Q resistors to provide heating to the system Dewar mounted vacuum Feed Thru D TIH 16 26PN Connectors D TIH 16 26PN MS3116F 16 268 10m cabling 2 Anthony Custom Industries Project 1640 Design and Operations 113 Temperature sensors The sensors are two Lakeshore D T 670 SD Silicon Diodes mounted in a M3 screw see drawings below This particular series of sensors work from 1 4K 500K and have 12mK calibrated accuracy at cryogenic temperatures In addition we use a custom Lakeshore SMOD 4 D I32 4 wiring lead configuration going to the four wires on the diodes This corresponds to two Voltage inputs V V and two Current inputs I I We have four feet of wiring on each sensor These wire leads are soldered to a single Detoronics P N DTIH 16 26 vacuum feed thru connector mounted on the dewar wall The other 1s spare These connectors have been mounted via epoxy onto an aluminum plate This plate 1s o ring sealed on the dewar wall via 14 10 32 screws Figure 106 The temperature sensor cabling Left The key pattern on the connector Right The cabled connected We currently don t use one plug 114 Project 1640 Design and Operations Pin Symbol Description 1 Current Green 2 V Voltage Red __ DENN 8 Shield Model 340 Configuration 8 Curm Back 6 None Shield
27. brass plug is all the way down into its dewar socket Also make sure that a vacuum gauge 1s connected to the vacuum pump via a 1 junction Begin pumping down the pump hose leaving the dewar closed Don t ever pull up the black handle unless you are sure there 15 a suitable vacuum in the pump hose It 1s still possible for a person to pull up the black handle even if the dewar is at a high vacuum and the hose has room pressure Once the hose pressure has reached that of the dewar it is okay to open the dewar by pulling up on the black handle After you have done this stop the pump and let the turbine slow down to less than 500 Hz If you are certain the temperature of the dewar is suitable for venting allow a little gas to leak into the pump hose The AMNH pump has a small black knob near the base of the hose on the pump which allows some gas to leak into the hose and dewar If gas 1s 162 Project 1640 Design and Operations being transferred into the dewar you will hear a hissing noise When the hissing has stopped both the dewar and hose are at room pressure D i r i w a ow P j T a i Jew poor vS room temp tor vorying reiotive numigity y tw E p A A A AAA SA AA A y pan 979 gt a ou E 4 m s J i Figure 155 Dewpoint plot Given a room temperature and humidity the vertical axis represents the temperature at which dew will form on the optics or detector
28. carefully controlled to ensure that the rate of cooling is not too fast A good rule of thumb is that the detector should never experience a rate of cooling greater than about 1 degree K minute Substantially exceeding a rate in this area can cause the multiplexer portion of the the Hawai II array to crack see photo below 166 Project 1640 Design and Operations Figure 160 Detail of a cracked Hawaii 11 array This has likely occured because of heating or cooling of the detector too rapidly Cooling Procedure 1 Attach the Y shaped detector cable to the single connector on the dewar Make sure you are well grounded before doing this Place one hand on a well grounded surface to ensure that no static electricity jumps to the detector plug Even a small spark can fry the detector PLEASE DO NOT FRY THE DETECTOR The two Leech box connectors on the other end can be left danghng Making this connection ensures that the detector 1s cooled with the power off and that the connector on the dewar won t ice up 2 The dewar should be pumped down sufficiently over several hours 24 hours so that pressures of roughly 2x10 mbar are reached It may be the case that the turbo pump being used does not exceed 1100 1200Hz even after pumping for nearly 24 hours This 1s probably due to continual and significant outgassing of water vapor from the mylar thermal shielding The numerous layers of this shielding has a huge effective surface area and can outgas
29. continually even when being pumped down It 1s a good 1dea to leave the pump running while doing the cool down 3 Hook up the custom LN2 stinger to the fill hose on the LN2 dewar Pictures of the stinger and the desired configuration are shown below Note that the picture shows a 22 PSI safety valve on the liquid port of the dewar It 1s a good 1dea to use this for safety reasons but this valve has a tendency to freeze and become ineffective causing liquid to leak out of it A plug can replace this safety valve Project 1640 Design and Operations 167 Figure 161 The stinger used to fill both of the nitrogen cans left The configuration needed to begin the LN2 fill right 4 Place the stinger into the large tank fill port and open the stream wide open Since the large tank 1s fairly well decoupled from the detector the risk of harming the detector 1s very minimal here and the large tank can be filled rapidly without any worry However DO NOT PUT ANY LN2IN THE SMALL TANK AT THIS STAGE The small tank should only be filled once the detector temp gets to about 93K Note that it may take around 12 hours of keeping the large tank full to get to around 93K Very soon less than a minute after starting to fill the large tank the vacuum pressure starts to fall quickly The temperature sensors will not change very much however Figure 162 Cryo gloves need to be worn at the very least 168 Project 1640 Design and Operations
30. into the mount containing the two flat mirrors made by Axsys Technology The lens 1s pressed into the mount via three flexible fingers which make contact with the face of the lens outside the clear aperture In addition a single flexible finger on the top portion of the mount provides pressure on the lens to keep it centered in the mount The mount for this meniscus lens can be removed from the rest of the assembly containing the two flats Field Lens Mount The mount for the field lens is somewhat more complicated The lens 1s housed in an aluminum lens cell The inner square region for the lens 1s 61mm allowing a 2mm gap on either side of the 57mm field lens The lens 1s held in the center of the cell by a set of four phosphor bronze springs see photo below Uhe lens 1s held in place by a retainer piece that screws via six 6 32 screws into the lens cell The inside edge of this retaining face 1s beveled to accommodate the curved front face of the lens The ensure there is no contact between the retaining face and the lens two gaskets were cut from 0 015 inch thick nylon sheets These gaskets act as a compliant material between the retaining face and the lens and does not change 1s properties at cryogenic temperatures Also a similar shaped gasket of 50 um thick nylon sits between the back plano face of the lens and the back register of the lens cell outside the clear aperture of the lens 78 Project 1640 Design and Operations This le
31. laser spanning the operating band of the instrument 1100 nm to 1760 nm Each laser image contains the response of the Integral Field Spectrograph IFS to laser emission at a specific wavelength a matrix of point spread functions where the rows and columns correspond to the individual lenslets of the IFS These laser images were reproduced in 10 nanometer increments across the band Each laser image is effectively a key showing what regions of the 40 000 spectra landing on the detector correspond to a given central wavelength The matrix of laser point spread functions are used as filters to extract the science data and map them onto a cube forming images of the observed target at the series of wavelength channels represented in the laser point spread function PSF library The Data Pipeline carries out the following steps l Bad pixel and cosmic ray cleaning of detector images 2 Subtracts the bias from the detector images 3 Performs a cross correlation to align the detector plane data with the laser reference library the projection of the lenslet array onto the detector vary with telescope pointing due to mechanical flexure 4 Extracts a data cube from the detector image Flat fields the cube based on a library of Moon observations 6 Calibrates the flux in the spectral channels of the data cube to account for the transmission of the atmosphere and the response of the instrument 7 Produces collapsed images by summing th
32. not always be sufficient The lenslet array is kept in its housing by means of a retaining ring and a wave spring See figure below Procedure for inserting lenslet array into collimator housing 1 Use an adjustable spanning wrench to remove the outer spring retainer Size 2 56 screws may be used to remove the retaining ring if a spanner wrench is not available 2 Remove axial spring 1 and array retainer 3 Insert lenslet array into assembly V groove Project 1640 Design and Operations 59 4 Compress provided radial spring 1 and place above lenslet array Verify that the spring holds the array into the groove Use caution when installing the spring as deflection beyond nominal may affect the integrity of the spring 5 Insert array retainer and axial spring 1 into the assembly 6 Insert spring retainer 1 and turn the retainer until the engraved surface 1s flush with the assembly face to achieve the proper spring compression y amar FAA iw ww Xx Figure 57 Top row the lenslet array left and SEM detail of the structure Bottom row the lenslet in its housing in the collimating assembly left and an exploded view of the lenslet assembly right Table 4 Original manufacturing specs for MEMS Optical microlens array Lona pinch Clear Aperture Side 73 5 um square Radius of Curvature Side 2 158 5 um Clear Aperture Side 2 60 um square 60 Project 1640 Design and Operations 30 0
33. of oversizing the central obstruction in the Lyot Stop 10 Project 1640 Design and Operations 4 5 a m ed he Bp 6 g eJ 4 O 4 r 1 as B D 2 LO 15 20 Position D Figure 6 H band PSF with the optimal solution and a 25 oversize of the central obstruction Table 1 Table of coronagraph design parameters 2 1 1 Coronagraph Optical Train The layout of the coronagraph is shown in the figure below and is based on the concept of Sivaramakrishnan et al 2001 The f 15 4 beam from the Palomar AO system enters our coronagraph via an infrasil window which counteracts dispersion caused by the PALAO dichroic The beam 2 391 inches above the optics baseplate comes to a focus strikes an OAP and is formed into a collimated beam Next in the optical train is the apodizer The beam then strikes the fast steering mirror and continues onto the pair of atmospheric dispersion prisms more detail on these is given below The beam is brought back into a focus by an OAP in order to apply the primary coronagraphic correction at the Focal plane mask The hole in the reflective mask serves as the occultor and the light travelling through the hole meets our infrared tip tilt sensors The unocculted portion of the image is reflected off the Project 1640 Design and Operations 11 focal plane mask and travels to another OAP which brings the beam back out of focus where it meets the Lyot stop Similar to the focal plane m
34. proj1640pipe 2010march At the command line execute pipeline DATA goodstuff After the pipeline indicates the processing is complete open the result in a ds9 window Project 1640 Design and Operations Separation pix Separation pix Separation pix Separation pix Slice 5 1 24 um go Pixel scale F 19 17 mas pix osiriee 60 E P Wipsaras 40 a HIP171 20 l 7 gj HIP107354 9 Slice 15 1 54 um BO Pixel scale O 19 24 mas pix wositiez 60 e A WiPss745 40 Uo MIP171 20 m gj HIP107354 0 Slice 18 1 83 um BO Pixel scale O 19 24 mas pix wosiriez 60 P A wWipesras 40 Uo HIPI 20 za Ej HIP107354 0 Slice 21 1 72 um BO L Pixel scale O 19 24 mas pix wos11182 60 d A wWipseTas 40 at HIPIN 20 e Ef HIP107354 Physical sep mas O 500 1000 1500 0 Slice 9 1 36 um pixel scale 0 19 15 mas pix W0S11182 P peers HPM o HIP107354 Slice 18 1 57 um pixel scale eo 19 23 mas pix OS11102 A wees HIP171 E HIP107354 Slice 19 1 66 um pixel scale O 19 22 mas pix wbsiniaz A wpanz4s P wert po HIP107354 Slice 22 1 75 um pixel scale o 19 27 mas pix W0Ss1182 O Hipag Pig HIP17 p HIP107354 500 Physical sep mas 1000 1500 0 207 Slice 13 1 48 um pixel scale 0 19 20 mas pix 0S11102 mpesrs gt HP171 p HIP107354 Slice 17 1 60 um pixel scale Y 19 26 mas pix oS11108
35. server HTTP command http 195 194 120 66 5417 config hawanunlrg dummy app xml Run dummy application 3 Execute application command to camera server HTTP command http 195 194 120 66 7063 exec GO Execute Non Destructive Readout NDR application Load NDR application 98 Project 1640 Design and Operations 1 Load NDR application on camera server HTTP command http 195 194 120 66 7063 config hawanlrg ndr app xml 2 Load NDR application on filesave server HTTP command http 195 194 120 66 5417 config hawanulrg ndr app xml Run NDR application 3 Execute application command to camera server HTTP command http 195 194 120 66 7063 exec GO General Commands Read timing board at X memory at address 0x200 command to camera server HTTP command http 195 194 120 66 7063 exec RDM X 0x200 Write value 0x1234 to timing board X memory at address 0x200 command to camera server HTTP command http 195 194 120 66 7063 exec WR M X 0x200 0x1234 Execute application command to camera server HTTP command http 195 194 120 66 7063 exec GO Stop application command to camera server HTTP command http 195 194 120 66 7063 exec ST Status command to camera server HTTP command http 195 194 120 66 7063 status Status command to filesave server HTTP command http 195 194 120 66 5417 status File status command to filesave server HTTP command http 195 194 120 66 5417 fstatus Get application file name list command t
36. to make FSM work July 7 July 8 observing Present Doug Sasha Ben Antonin Rick Lynne Ian On Telescope Verify AO Alignment with stimulus source 210 Project 1640 Design and Operations Align Pupils using bright sky pre sunset tweak cass ring angle to align spiders Obtain on telescope Hg lamp data to check for flexure lambda changes Check pupil cam sensitivity with dome lights Verify and Calibrate ADC performance ADC calibration motor rotation algorithms need to be verified and scale factor determined 5 bright stars at airmasses of 1 0 to 1 56 lest for pupil wander 5 airmasses 5 HAs also tests for instrument flexure Verify star acquisition occulted images Acquire multiple sky flats July 9 10 observing Morning Acquire suite of on telescope darks and additional dome flats Astrometric and photometric data quality verification HIP 101769 RA 20h38m sep 0 44 V primary 3 64 delta V 0 91 HIP 102531 RA 20h47m sep 0 22 V primary 4 27 delta V 0 88 Spatially Resolved Spectroscopy Data verification Uranus and Neptune e g methane chemsitry across FOV Disks HD 141569A 7 mag DoAr 25 9 in J 12 65 in R Vega 0 Acquire non AO corrected G star flats do we need to implement G star flat mode on FSM to raster the star Magnitude Limits and FSM tracking limits Vega short and long exposures occulted 5 stars at 2 5 8 10 and 13 mag V FOV Distortion and initial coronagraphic performance
37. to the non dewar end of the LN2 fill hose Hook up the other end of the LN2 fill hose to the VENT port on the 50L LN2 dewar To do this you will need the threading adapter to fit on the VENT port Once this step 1s done clamp the special KF 16 fitting to the free end of the turbo pump T junction A KF 25 to KF 16 adapter is needed With the dewar closed and the pump hose connected to the dewar fully pump down the hose With the dry nitrogen fitang hooked up to the turbo pump there currently 1s no way to measure the pressure in the pump hose However the pressure in the pump hose will be very low once the turbine has reached 1500Hz When this has happened it 1s safe to open the dewar by pulling up on the black handle If the pressures between the dewar and the pump hose are comparable 1t should be easy to pull this handle up If it 1s a struggle stop something 1s probably wrong Once the dewar is open SLOWLY lift the VENT handle on the 50L dewar This doesn t need to be turned much perhaps only 5 degrees An extremely faint hissing sound should be heard and the pressure in the dewar should rise Do not open the VENT handle any more than it is already open It is important to not over pressurize the dewar with dry nitrogen When the pressure on the dewar has reached 400 500mbar remove the KF 15 clamp securing the dry nitrogen fitting to the IT on the pump while keeping the 50L hose and its fitting in place with your hand This is most easi
38. uk atc xml 4 Configure filesave server telescope settings HTTP command http 195 194 120 66 5417 config uk atc xml Load instrument configuration 3 Configure camera server instrument settings HTTP command http 195 194 120 66 7063 config ultracam xml 6 Configure filesave server instrument settings HTTP command http 195 194 120 66 5417 config ultracam xml Power on camera controller Project 1640 Design and Operations 97 Load power on application 1 Load power on application on camera server HTTP command http 195 194 120 66 7063 config hawanlrg pon app xml 2 Load power on application on filesave server HTTP command http 195 194 120 66 5417 config hawanlrg pon app xml Power on camera controller 3 Execute application command to camera server HTTP command http 195 194 120 66 7063 exec GO Power off camera controller Load power off application 1 Load power off application on camera server HTTP command http 195 194 120 66 7063 config hawanlrg pof app xml 2 Load power off application on filesave server HTTP command http 195 194 120 66 5417 config hawanlrg pof app xml Power off camera controller 3 Execute application command to camera server HTTP command http 195 194 120 66 7063 exec GO Execute dummy application Load dummy application 1 Load dummy application on camera server HTTP command http 195 194 120 66 7063 config hawanlrg dummy app xml 2 Load dummy application on filesave
39. uneven elevator floor often causes one portion of the instrument to reach the optical bench first Compression in this region will allow the instrument to become parallel with the AO bench as the instrument is raised up 2 Our cart has fine x y adjustment to match our mounting pucks with the AO bench pucks The instrument is mounted to the cart via two rotateable plates which share an axis This allows the instrument to be rotated on this cart in a spit manner essential for switching between the optics down configuration for mounting and the optics up configuration for instrument maintenance The instrument is mounted to these plates via eight M6 screws which screw into 8 tapped holes on each side of our instrument baseplate A locking pin on each end of the cart allows the instrument to be locked in the optics up or optics down The cart has a pump action hydraulic scissor jack mechanism for raising it The rolling cart portion blue yellow and green steel handle parts in the picture below 1s a standard McMaster Carr Light Duty Foot Operated Mobile Lift Table It has a 770lb weight capacity and is listed P N 2779145 The swivel casters are McMaster Carr P N 27791994 Project 1640 Design and Operations 153 Figure 146 The handling cart partially extended and detail on the rotating mounting plates 154 Project 1640 Design and Operations Figure 147 Detail on the ball bearing track rails that al
40. you can run a test cube extraction by simply calling the executable with no arguments S pipeline o This wil produce one example data cube from a detector image in the library subdirectory along with a sequence of comments directed to the terminal describing the various stages of processing To run the pipeline on a directory called e g DATA goodstutP containing a set of Project 1640 detector images run pipeline DATA goodstuff The extracted cubes will be organized under the directory DATA PROCESSED by target name and date Within the date subdirectory normal data cubes are stored in the subdirectory FITScubes standing for least squares fit to the read sequence As an example the full filename of one processed data cube could be DATA PROCESSED POLLUX 2008 10 25 FITScubes POLLUX C 2008 10 25 529 fits There are a few command line options to modify how the pipeline operates Ihe optional switches placed after the input directory are o for overwrite mode which will overwrite data cubes that have already been made for the given raw focal planes d for dat file mode which requires the dat files corresponding to a given fits file be in the given directory In this mode the pipeline forms a cube using slope fits to the individual bias subtracted dat file reads rather than the FITS file from the camera to form a cube If the dat files are handy along with up to date dark frames this gives significantly cleane
41. 0 9 to 1 7 um Following correcting for flat field errors and dark subtraction a simple centroiding algorithm is used to determine the stellar position We estimate we can track stars of at least 7 magnitude with a S N of 4 under median conditions These IR sensors are placed on a x y translation stage for fine adjustments of the star under the mask Table 3 Table of specs for the Hamamatsu G6849 01 series InGaAs PIN photodiode quad cell array used with the P1640 tip tilt system Parameter 0 9 1 7 um Project 1640 Design and Operations 33 991202 281102 Typ Tau 25 C WINDOW ACTNEAREA 59202 DETAILS OF eee PHOTODIODE SURFACE 25203 41 02 PHOTO SENSITIVITY A W 130220 WAVELENGTH um Figure 30 Left photosensitivity of the Hamamatsu InGaAs PIN photodiodes Right The dimensional specifications of the quad cell array units are mmy 34 Project 1640 Design and Operations Quad cell IR sensors Figure 31 The Hamamatsu infrared photodiode quad cell housing inside the coronagraph Project 1640 Design and Operations 35 Figure 32 New picture of the location of the tip tilt sensor relative to the cal system workplate 2 1 4 1 Electronics The electronics are comprised of an A D converter board in the FSM computer We have a LABview interface as well as an amplifier and PZT stage 36 Project 1640 Design and Operations Figure 33 P1640 electronics rack conta
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43. 0mm Substrate Material IR grade fused silica Substrate Thickness Table 5 Fitted radii of curvature for lenslets 3 5 E E E EY Average 0 45 O 94450 15720 94450 16060 Table 6 Wave front errors for the 10 lenslet wafers The first value in each cell is the RMS the second is peak to valley Both the RMS and the peak to valley values are listed as their fraction of a wavelength at 1 65um 6 A 600 50 4 72 22 0 163 184 1 19 6 A 600 47 A 76 22 4 163 498 QJ 6 4 600 42 1 85 20 A 180 467 1 7 7 A 514 60 4 60 23 4 156 174 4 20 6 A 600 43 1 83 20 A 180 161 4 22 7 A 514 45 4 80 19 X 189 167 QJ21 6 A 600 51 4 70 23 A 156 168 1 21 5 A 720 46 4 78 20 0 180 311 A 11 7 514 56 4 64 23 A 156 182 4 19 7 A 514 52 4 69 21 QJ171 347 4 10 6 2 600 44 4 81 6 4 600 50 4 72 19 A 189 149 4 24 6 2 600 46 1 78 6 4 600 44 1 81 23 0 156 243 0 14 6 A 600 43 1 83 21 QJ171 169 4 21 6 A 600 50 4 72 19 1 189 189 4 19 10 6 A 600 43 1 83 23 0 156 194 1 18 5 A 720 44 QJ81 19 0 189 187 4 19 6 60 600 416 1 78 21 M 171 428 4 8 6 0 600 47 QJ76 23 0 156 288 1 12 EN EAN BONN 61 Project 1640 Design and Operations ER n 6S NADA A AD LA A eeu DN 949322 au parda D Leu uw pha Ww me oe sar ance etm TOJA 2 06 C www v CH Aem o une ee os V
44. 16 67 pm 158 608 Pt 64QSPEC_TH_THERM ZMx PEFERENCE CHIEF PAY CONFIGURATION 2 OF 2 HAWEL PNG TH gt FIELD J E a 2 0020 QG DOQO MM 9 9 vli Sjel e i COCR edel D gt gt e 5 ws e ew e i rabo e SURFACE IM DETECTOR MATRIX SPOT DIAGRAM DIOP COLL CAT CAM PRISM FOLDS J H COMBINED FRI TUN 24 2006 UNITS APE pa PL64OSPEC_TH_THERM ZMx BOX WIDTH REFERENCE CENTROID CONFIGURATION 2 OF 2 90 Project 1640 Design and Operations u Se G EL a ul ho Es Ww du o n gt a 2 1 O gt o H Et G Q u 4 95 FIELO IN MILLIMETERS VIGNETTING OIACRAM DIOP COLL CAT CAM PRISM FOLDS J H COMBINEO FRI JUN 38 2006 PL64OSPEC_TH_THERM ZMX CONFIGURATION 2 OF 2 gt 4 7 4 7 j i a E e GRIO DISTORTION DIOP COLL CAT CAM PRISM FOLDS J H COMSINEO FRI JUN 38 2006 FIELD 14 00 W 14 00 H MILLIMETERS IMAGE 35 06 W 35 21 H MILLIMETERS MAXIMUM DISTORTION 1 3694 SCALE 4 980X WAVELENGTH 1 3500 44 PI64O0SPEC JH THERM ZMX CONFIGURATION Z OF 2 l I LE d be LE ls y LL b bl T hd IS I q icy 4 4 LU 1 4 L Ww M Li gt ot J gt 4 a LL 4 s A E e 2 Ch ja E e 1 E T LI 7 gt po Les j gt e k t1 gt 7 E I d c 1 j ET T 5 Ls L T pd
45. 600 s integration 2 2 5 2 Detector System Control In order to maintain the greatest amount of flexibility and portability our collaborators at the Astronomical Technology Centre in Edinburgh have configured our detector system to communicate with the outside world using XML files that are transferred using http Beard et al 2002 The http protocol was chosen to allow greater flexibility and stability when such a system 1s moved from a particular institution or telescope Ihe XML files include all of the necessary parameters for a particular observation exposure time number of reads etc The system can perform Non destructive reads NDR as well as Correlated Double Sampling CDS The flow of the user commands is shown schematically in the figure below The user sends the appropriate configuration XML files via http to a set of three separate but connected servers setup on our Data Acquisition Computer that organize the camera operations the filesaving and the detector de multiplexing The user can directly communicate with the Camera and Filesave servers but the Filesave server 1s the only module that will communicate with the de multiplexing server Figure 88 Schematic of the detector data handling XML command files are moved between three independent servers green boxes in the data acquisition computer and the SDSU controller 96 Project 1640 Design and Operations We communicate directly to our Camera and Filesave servers
46. 631 1 5737 1 5844 1 5950 1 6056 1 6162 1 6269 1 6375 1 6481 1 6588 1 6694 1 6800 1 6906 1 7013 1 7119 114225 1 7331 1 7438 1 7544 1 7650 1 7756 1 7863 99 704 99 704 99 761 2901 09 55 750 55 753 55 750 55 748 55 745 55 743 55 741 55 738 55 730 55 734 55 731 93 729 99 27 IRI 93 729 090 21 90 49 09 7 17 25 715 55 714 52 712 99 710 99 708 55 707 55 705 55 704 55 702 55 700 55 099 55 097 99 096 99 095 55 093 99 092 25 690 99 089 55 088 55 087 55 085 55 084 55 083 55 082 0 003 0 001 0 001 0 004 0 006 0 008 0 011 0 013 0 016 0 019 0 021 0 024 0 026 0 029 0 032 0 035 0 038 0 040 0 043 0 046 0 049 0 052 0 055 0 058 0 06 1 0 065 0 068 0 071 0 074 0 077 0 08 1 0 084 0 087 0 091 0 094 0 098 0 101 0 105 0 108 0 112 0 115 0 119 0 123 0 126 0 130 0 134 0 0256 0 0264 0 0270 0 0275 0 0279 0 0281 0 0283 0 0284 0 0284 0 0283 0 0281 0 0278 0 0274 0 0269 0 0264 0 0257 0 0250 0 0242 0 0233 0 0223 0 0213 0 0202 0 0190 0 0177 0 0164 0 0150 0 0136 0 0120 0 0104 0 0088 0 0070 0 0052 0 0034 0 0015 0 0005 0 0025 0 0046 0 0068 0 0090 0 0112 0 0135 0 0159 0 0183 0 0208 0 0233 0 0259 0 0638 0 0644 0 0649 0 0654 0 0659 0 0664 0 0670 0 0675 0 0680 0 0685 0 0690 0 0695 0 0701 0 0706 0 0711 0 0716 0 0721 0 0727 0 0732 0 0737 0 0742 0 0747
47. 9 Lyot Mask design description for CTM Palomar Order 4 Sep 15 2009 Palomar 4 1 this order same as Palomar 3 1 design Mop A rm aee a Palomar 4 2 this order same as Palomar 3 2 design ovre m A reel ti Palomar 4 3 this order a repeat of an older ID OD design but part OD 1 25 4mm 3514 5 Qty DD mm ID mm Vane thick Tota micron Count Figure 16 More specs on the P1640 Lyot stop Current as of Fall 2009 W o APSO LYOT 2 Pess Now APebDi26b APERTURE APODEIED APertoag JCS Cil APERTURE No APO 4 761 lU HEEL NY 3 3 5 f e CLEAR gt CLERA APERTURE 17 23 37 Figure 17 Configuration of the Lyot wheel as of March 2010 20 Project 1640 Design and Operations 2 1 1 12 Final Sphere Optic 600 00 mm FL Sphere from Opticology 38 1 mm in diameter Mount Part AMNH 1640 6 three tiered adaptor for 35 39 mm optics for inch optics mounts Interfaced to Newport SS100 F3H lockable kinematic mount attached to 1 4 inches of post by 8 32 screw and held to ramped AMNH1640 2 with clamp parts PS B 1 SS 1 A PS 0 125 PSF height 2 375 inches above raised platform supported by Newport 45s and the platform hardware from Lyot Project 2 1 2 Coronagraphic Mask Optical Specs Our three masks are shown below Our apodizing mask is a 12 7mm transparent optic made by Jenoptik It has a 3 9mm pupil and is shown in the photo below The transmission profile on this mask follows th
48. AAA a AS de As M Vu AN 4 ANAS E va Vy A A PR Ix V E F e eri y Ty Y NE S e A NL A Figure 178 The handling cart should be raised up via its pump mechanism until the yellow portion of the cart platform 1s higher than the narrowest part of the cass cage door Then the cart can then be wheeled towards the middle of the cage 8 As the instrument is lifted via the foot pump up to the four AO bench pucks the six screw mechanisms on the handling cart which reposition the handling cart A frame in an x y manner are used to position the four P1640 pucks directly under the four AO bench pucks Project 1640 Design and Operations 18 Figure 179 One of the six x y adjustment screws These are used to carefully align the four P1640 mounting pucks with the AO bench pucks 9 As the instrument continues to rise up one of the instrument pucks will invariably reach its corresponding puck on the PALAO bench first Assuming that the pucks are well aligned the instrument can continue to be raised upward The six springs on the handling cart will allow the side that has reached the top first to compress and all four pucks will eventually meet as the instrument 1s being pumped upwards 10 Once all four pucks are well aligned and flush with each other each puck pair can be clamped The current clamp configuration is tricky and it may help to have two people working on a single clamp Long ball drivers should be used as we
49. ADON 904 A rom ira 44 Ln A 26 19e fw gum ADN Gr Wee Ui PQULCO s Bang FO pa ELA AR PIDIO OFF wu Le Y m wee 7 MBA SQ fae Volo o9 LEDO OF PATA 2 4 440 Gere lox Y em Ope PADLA 3 C 9 85V Que Y C FIDA Y Cf ARA Aat abd cmn i AOON D wo DA owe wu O AAA v 5 WA CL P ap ouo nam JO 30 XU Doed CTs UM UO KM JO AAA AAA i MA DES 8 wv ow fu s F t VIDAD Ger m tere OA 0 mOUR PA MM ucc mus r JA 0 O UOuT4Qu Wu HA 4 4 TRJIT un Ghee OQ AIDA 9 ad Xn Peu 24 OQ Dua TOO Aun 6 IIA cm 4 09 we Sher s pact ss C S843 uod Tel QE Om sn uw Eu POL j AW Did Gis 494498 34 Ore a9 cipum HAGA A ja PALO A OR 497 WAN 1 OL WO DOW Fut A WIND Y MARA 31 74 wol m VEB 3 0 AA an E A ard the SS a Figure 58 As built specs for microlens array Project 1640 Design and Operations AMNH Lenslet Array Geometry gus S p am am N Alignment marks 3 sets of perpendicular Laes 7 aegoed wih otit gd 2 rotates 0 8 43 Gagrees 2171212 31 ilisdinisAdi itte mt RETETA fth 1712717717 I AFI ninos 27 1913 ITITITIT NILDILIILI nn ISLILITII aiciinios TITITITIT etereeter PIDLISIZIII nr erererter etabaetas ebabeesas 171712011 aisiipial no TII ttp ttm 112711 217171 e en 4 1 rspisrrisuia IILISISIT 222224 TM s e L c 217 T7IT7ITTT on m mu ITI sre
50. AR LST m o N nm PI640 LST 25 23 39 0 39 0 155 07 11 2008 03 55 7 11 08 UTC 11 Figure 186 Software panel showing details of the paths tab Project 1640 Design and Operations 189 Motor Control This panel allows full control over all the instrument s motors This tab primarily consists of two boxes The Move Pupil on Lyot Stop control box allows the user to tilt the FPM which effects movement of the pupil image at the Lyot stop The user can choose the amplitude of tilt to be imparted to the FPM The Move Star Behind FPM Hole box imparts movements to the tip tilt sensor housing This effectively allows the user to move the position of the star under the mask The current and nominal positions for the FPM and Tip tilt motors are listed there too Also two buttons allow the user to save the current motor positions to the nominal positions or to go to the nominal positions Then FPM and TT x and y current and nominal Three buttons Set ADCs to Offsets Go to Nominals Save Nominals Project 1640 Design and Operations 190 L90 t 0 151 IWWO TWd rA TAA 13185210 80 I11 4Z O GE SS EO 8002 11 40 1121290 Figure 187 Software panel showing details of the motor control tab 4 Take Darks 5 More Pointing Project 1640 Design and Operations 3 4 2 O Hour Angle 10 80 Alrmass 247 Altitude 23 86 Azimuth 349 55 Paralak Aaga 16 34 Star Catalog
51. AUD Rate 57600 Bits 8 Parity None Stop Bits 1 Flow None 3 4 0 onopPomogpnocese 4 4095 Power Strip a Mode Raw Server b BAUD 9600 Bits 8 Panty None Stop Bits 1 Flow None ES 525 Data Acquisition Computer DAC MAC address 00 E0 81 54 5D 58 IP 198 202 125 165 194 Project 1640 Design and Operations Operating System Linux version xx xx User root Password pl640dac Note The dazle software uses two users The second is optics the password for optics 1s DAZLE Gioal To run dazle software outside of labview from the main computer send the following from an xterm gt ssh root 198 202 125 165 XY where 172 is DAC s IP address gt xterm e root dazle startup IP Power Strip MAC Address IP 198 202 125 169 Name Password admin Ports Empty 2 KVM Drawer unit 3 DAC 4 FSM Amplifier 5 FSM Computer 6 Lakeshore Temperature Controller 7 MM4006 Motion Controller 8 SMC100CC Motion Controller Main Power Strip RS232 TCP converter IP addressable power strip 2 Unicom Smart Switch Pupil Camera 3 5 4 Control Room Electronics Main Control Computer 198 202 125 164 Data Reduction computer 198 202 125 170 3 5 5 Cabling 3 9 9 1 Observing Configuration Palomar IP Addresses 198 202 125 164 170 is open and now reserved for you The netmask 1s 255 255 255 128 the gateway 1s 198 202 125 129 Project 1640 Design and Operations 195 3 5 5 2 Palomar Lab Configuration
52. Detector rout Das ran alist 220 AD Miscellaneous Drawno ii s os Sagas aut bet fuum Seidel iu centes 234 dols Pare OVE MON arnee e etel sn ate aa e et Ee oc etai NEES 236 1 Introduction Project 1640 1s a complex astronomical instrument designed to produce images of the environments in close proximity to nearby stars with unprecedented contrast This document describes the design of the system from the point of view scientific reproducibility The driving requirements on the performance led to the following table summarizing the instrument s operational capabilities and modes of operation in conjunction with the Palomar Adaptive Optics System 1 1 System Operating Capabilities Project 1640 is the first ever Infrared diffraction limited Integral Field Spectrograph fed by an Apodized Pupil Lyot Coronagraph APLC and coupled to a high order Adaptive Optics System The lenslet based spectrograph covers both J and H bands 1 05 1 75 um and samples the 4 2 arcsec field of view with a 21mas lenslet platescale Our diffraction limited APLC can achieve suppression of 10 at arcsec as demonstrated by our results from the Lyot Project Coronagraph and the Gemini Planet Imager GPI testbed Project 1640 Design and Operations Property Wavelength coverage Central wavelength IFU FOV Platescale Total spectra Pixels per spectrum AX per 2 pixels R A AX Lenslet Pitch Input f ratio from coronagraph for A 2D Spaxels at 1 0
53. II HgCdTe Array Specifications The information in this section was taken from the Gemini NIFS System Design Note 8 00 dated April 5 2000 entitled NIFS Science Detector Trade offs by Peter J McGregor Although many of the passages in here refer to the earlier generation HAWAII 1 arrays the characteristics of the HAWAII 2 are very similar The HAWAII 2 HgCdTe array is an evolution of the successful 1024x1024 HAWAII 1 array It uses PACE technology in which the HgCdTe detector material is deposited on a sapphire substrate The 2048 x 2048 HAWAII 2 18 um pixel arrays use similar technology to the 1024 x 1024 HAWAII 1 arrays Both devices have a 2 5 um wavelength cutoff They are expected to have similar performance with a single double correlated sample read noise of 9 Project 1640 Design and Operations 93 e Read noises of 4 e are likely using eight double correlated 1 e Fowler samples The dark current performance of the HAWAII 1 array is not well documented due partly to the dithculty of measuring extremely low dark currents Finger et al 1998 report a mean dark current of lt 30 e hr lt 0 0083 e s for a HAWAII 1 array operated at 78 K This very low measurement 1s limited by electrical drifts in the data system Ihe Rockwell Science Center WWW pages show a dark current distribution with a mode of 0 01 e s pixel for a HAWAII 1I array at an operating temperature of 78 K Kozlowski et al 1998 plot a different da
54. Ludi PA RA 12000 4 55 45 93 User s Manual 04 38 59 UTC 06 04 2008 20 38 59 EFA LST 13 45 29 9 Dec 2000 30 33 46 1 Current Target of Observation Survey s OTSE At Curreet Epoch RA ard tu Dec mas yr p Dec 24 mas yr Sp Type d pc 144 No of Exposure A Time s d Coo 191 KOS DETECTOR f a Camera Matus p RA 2 mas yr p De 24 mas RAE v J H Sp Type dipti 5 06 ADe 144 Notes for Log Figure 188 Front Panel of Operating software 3 4 2 1 VPN settings Cisco VPN settings for main computer Create new profile Connection Entry AMNH Description AMNH Host vpn gw amnh org Group Authentication Name amnh Password r0tund 192 Project 1640 Design and Operations 3 9 Electronics Configuration The electronics rack consumes 350W of power without the motors powered up With the tip tilt system on the system consumes 10W of power 3 9 1 Detector System Detector Leach box Data acquisition computer DAC Set to boot up when powered on Local login requires the password pl640dac A second user optics used by the dazle software has the password DAZLE ioa1 3 5 2 Instrument Pressure and Temperature Sensors Lakeshore Temperature Controller Model 331 Precision Calibration for sensor B D6003010 on detector 1s in channel 21 sensor A D6007636 on base plate in channel 22 Connected via RS232 crossover cable to Lava T CP R5232 box Heaters 4 1 ohm re
55. NAME i reconstructor name STATUS i AO_TCS i number of seconds of disconnect TSTABLE i number of seconds of instability CIFU MOT 7 CIFU motors FSM i on off INI ADCI i Initial ADC motorl position INI ADC2 Initial ADC motor2 position FIN_ADCI Final ADC motorl position FIN_ADC2 i Final ADC motor position WEATHER i TEMP Centigrade HUMID 9 o CLOUD 9 o WIND mph SEEING END Project 1640 Design and Operations 4 2 Coronagraph Optical mount Diagrams 215 Project 1640 Design and Operations 216 Pi Project 1640 Design and Operations 219 220 Project 1640 Design and Operations Project 1640 Design and Operations 4 3 Collimating Optics Drawings 2 SEIR Mr e WS vim k us ous we Ww Y BEVEL A TS MAX PW o EEES mum i pr WS 51 Je Y i Y CRANE x Y J eol 28051 0000 kr d SETI I f 52 813773 0014 f t ES 224 000 i E a A i e NE 4 p E t He Um A CT 5 20040 100 x pe SAG 701310025 Pos SECTION A A 1 APRES Maier Wa Ne ts n APR hes Ad te gt On TO M FOR JD fp nu ADS AT OR D AMO Ache at CM FA PN MIL ABBIA GE UM JANOS FARADRAPIS 24 34 12 4ND34 19 CHNO po BRALA A AS eT mew COLUMATOR LENS 1 gt i B Dw wa es mo TE pta A 41362 501 A n z mmen ARII
56. Project 1640 Design and Operations Documentation Version 0 1 12 5 10 6 32 59 PM 2 Project 1640 Design and Operations Project 1640 Participants AMNH AMNH AMNH IoA AMNH AMNH AMNH AMNH JPL 2010 by Sasha Hinkley Ben R Oppenheimer amp Neil Zimmerman This document 1s based on work funded by the American Museum of Natural History the National Science Foundation The National Aeronautics and Space Administration Hillary and Ethel Lipsitz the Vincent Astor Fund Anthony Marshall Judy Vale Ihe Cordelia Corporation Ann Mallinckrodt and two anonymous donors Items to add More info on apodizer and Remi s design document Tip t lt system rack pictures Software inventory subsection Procedure for on telescope fill ADC equations and algorithm SAN4 data structure De installation procedure Software guide Calibrations needed Pictures needed pictures of all cabling Specs on Tip tlt mirror Ian s calculations Fix image orientation image Project 1640 Design and Operations 3 Table of Contents MCL sri mma l Desienand Operations Documentatii dad l ke Junto HOT its 4 Lie Sten Operaune Capabilities suisse a a a ise Res edens 4 I A DISCO a T ae det I uiae 5 ER Ug ia in 6 2 MOTO TTA rer a E E E Ere Ie Pt UIA ete 6 Dale C oronaorapi Coe al TO o dente fais Dag Ena ci nea heu ecd 10 24 2 Coronasraphic Mask Opucal Specs destin ig ate n UE ete ans 20 2 1 3 Atmospheric Dispersi
57. Reassemble instrument Recable instrument to E rack verify detector functionality motors etc Check instrument pressure pump down MO Project 1640 Design and Operations 209 June 26t Rick Arrives for 26 27 possibly available over weekend Rick to bring Accellerometers for vibration tests from Mark Colavita AO system replaced to spit by mountain crew Install instrument on AO bench Verify LN2 filing procedure in optics down configuration on bench June 27 July 6 lan arrive July 5 Begin Alignment to AO system budget 4 days Imagine Optic WFS Alignment will be in lab on arrival Need to verify AO system communication is working Verify correct keywords are being written to headers Additional software testing and debugging FSM Lightsource readouts changed from what we would expect FSM Make sure x y gain and PID gains are giving the expected results Apodizer Test grid with AO WLS Apodizer Test pupil alignment to telescope AO pupil to p200 pupil Infrasil window angle needs to be calibrated Wavelength Calibrations Hg lamp Lambda scale reference 1mages Realign Pupil Cam Determine 0 point offsets for each ADC prism Vibration measurements on AO Bench Flexure Verify alignment 1s same after rotation back to optics up position White Light stimulus lab performance coronagraphic contrast estimate Pupil alignment Check alignment and look for signs of wander at different spit angles Attempt
58. Residual Difflimit mm 1 0000 55 899 0 046 0 0650 0 0488 0 0560 1 0106 55 893 0 046 0 0570 0 0493 0 0556 1 0212 55 886 0 045 0 0512 0 0498 0 0551 1 0319 55 880 0 044 0 0458 0 0504 0 0546 1 0425 955 874 0 043 0 0406 0 0509 0 0540 1 0531 55 868 0 043 0 0356 0 0514 0 0533 1 0637 55 962 0 042 0 0309 0 0519 0 0526 1 0744 55 857 0 041 0 0264 0 0524 0 0519 1 0850 553 891 0 039 0 0222 0 0530 0 0511 1 0956 55 840 0 038 0 0182 0 0535 0 0503 1 1062 55 841 0 037 0 0143 0 0540 0 0495 1 1169 955 836 0 036 0 0107 0 0545 0 0485 1 1275 55 831 0 034 0 0073 0 0550 0 0476 1 1381 95 827 0 033 0 0041 0 0555 0 0466 1 1487 55 822 0 031 O 0011 0 0561 0 0456 1 1594 955 818 0 030 0 0018 0 0566 0 0445 1 1700 955 814 0 028 0 0045 0 0571 0 0434 1 1806 55 809 0 027 0 0070 0 0576 0 0423 1 1912 55 805 0 025 0 0093 0 0581 0 0411 1 2019 55 801 0 023 0 0115 0 0587 0 0399 1 2125 55 798 0 021 0 0135 0 0592 0 0387 1 2231 55 794 0 020 0 0154 0 0597 0 0374 1 2538 55 790 0 018 0 0172 0 0602 0 0561 1 2444 55 787 0 016 0 0188 0 0607 0 0348 1 2550 55 783 0 014 0 0202 0 0612 0 0334 1 2656 55 780 0 012 0 0216 0 0618 0 0520 1 2763 55 777 0 010 0 0228 0 0623 0 0306 1 2869 55 773 0 008 0 0239 0 0628 0 0291 1 2975 55 770 0 005 0 0248 0 0633 0 0276 26 1 3081 1 3188 1 3294 1 3400 1 3506 1 3613 1 3719 1 3825 1 3931 1 4038 1 4144 1 4250 1 4356 1 4463 1 4569 1 4675 1 4781 1 4888 1 4994 1 5100 1 5206 1 5313 1 5419 1 5525 1 5
59. SR50CC from Newport custom mounting and spacing bracket Part AMNH1640 5a and b Height 2 400 shown in drawing below Four 8 32 screws secure the SR50CC motors to these mounts 2 1 1 7 Fold Mirror 2 FM2 Optic 1 inch flat with gold coating 4 20 superpolished supplied by Opticology Mount Newport VGM 1BD custom baseplate to match VGM base holes and flange for clamping to baseboard part AMNH 1640 2 Height 2 400 2 1 1 8 Off Axis Parabola 2 OAP2 Optic 640 00 mm OAP from Precision Asphere 35 mm in diameter Mount Drawings will list this part as AMNH 1640 6 three tiered adaptor for 35 39 mm optics for inch optics mounts Interfaced to Newport SS100 F3H lockable kinematic mount attached to 1 4 inches of post by 8 32 screw and held to table with clamp parts PS B 1 SS 1 A PS 0 125 PSF height 2 375 inches 2 1 1 9 Focal Plane Mask FPM l inch diameter Silicon FPM from MEMS Optical with U100 G gimbal mount with CMAI2CCCL actuators on Newport Model M B 2C base x2 on MRP3 1 base clamped to table Height 2 400 Figure 14 The P1640 Focal plane mask 2 1 1 10 Off Axis Parabola OAP3 Optic 640 00 mm OAP from Precision Asphere 35 mm in diameter Mount Drawings will list this part as AMNH 1640 6 three tiered adaptor for 35 39 mm optics for 1 inch optics mounts Interfaced to Newport SS100 F3H lockable kinematic mount 18 Project 1640 Design and Operations attached to 1 4 inches of post by
60. Sensor Data Acquisition Computer DAC the Tip Tilt sensor the SMC motor Electronics rack KVM unit FSM computer FSM amplifier and MM4006 motors Detector System Control and Configuration box This box contains three initialization buttons for the DAC Launch Camera Servers RST RCO Init and Detector Power On When powering up the systems these buttons must be executed in that same sequence A final button Kill All Camera Processes allows the user to terminate camera processes This tab also contains several other buttons Start TOS Communications which allows the software to communicate with the Palomar TCS Start FSM Communications which initializes communications between the software and the FSM computer Record Observations in Catalog is currently not used and finally Synchronize with NTP Time Server is also not currently being used 197 wes amen vv qu AILILI ped IM IN I NECI p mas 9 SLON OOV HON t X s e EID NN matj aq srasle P VW P On C 6 TT RS CFA A in3 21 ZTLUSTEZ Dn Step e iS 11 LIP 151 049 1d 0 6 SS 0 154 800Z T1 Z0 1121299 Project 1640 Design and Operations Control software with details of the System Init tab shown Figure 185 Paths Tab 188 Project 1640 Design and Operations This tab shows the locations where that current night s data are being stored as well as IP addresses of the DAC TCS computer and TCP to RS232 converter 43 06 7 PALOM
61. aks to the angle of OAP2 and 3 may be necessary to minimize aberrations lip ilt optical path alignment The lens should be well focused but with the detector in the midrange nominal positions the fold mirror may need to be adjusted 3 2 Instrument Preparation and IFU Dewar Procedures AMNH 3 2 1 Pump down procedure AMNH The Project 1640 dewar has a KF 25 vacuum seal off valve connected to the underside ports next to the large tank fill hole This fitang which 1s angled off at a 45 degrees can be connected to a KF 25 sized vacuum hose via a KF 25 o ring and clamp To secure this valve fitting on the dewar place the fitting onto the dewar port and tighten the fitting via the 1 Y brass nut Gaution When tightening this nut make sure not to apply too much torque as the fitting could be damaged Typically the wrench for a 1 3 4 brass nut will be nearly three feet long It 1s extremely easy with a wrench this large to apply too much torque and damage the seal off valve fitting or the dewar port or both 160 Project 1640 Design and Operations Figure 153 The vacuum pump valve on the P1640 dewar This valve can be opened and closed via a brass plug that fits into a socket in the dewar port see drawing below This plug can be taken in and E out of its socket via a shaft with a black plastic knob on the end This shaft can be disconnected from the plug by unscrewing it when the plug 1s in place Note however tha
62. and Operations 129 Figure 123 This mount for the left hand runner block is bolted to the Thorlabs baseplate via the four 4 20 clear holes The runner blocks are bolted to this piece via the four M6 holes 130 Project 1640 Design and Operations Figure 124 Similar to the above drawing This mount is bolted to the right hand runner block Project 1640 Design and Operations 131 2 4 2 System Enclosure The enclosure for the system IFU coronagraph is comprised of 1 8 thick painted Aluminum panels secured by standard optical table rails The enclosure 1s comprised of two segments see drawing below The first is a rectangular cube shape enclosed on three sides back left and right forming a skirt around the IFU dewar The second is a rectangular cube shape enclosed on four sides front left right and top housing primarily the coronagraph The enclosure rails will be constructed from Thorlabs components XE25 rails and RM1G construction cubes Drawings of the panels are included below Table 9 Parts list for system enclosure Component Oty Description XE25L 12 12 inch rail XE25L20 8 20 inch rail XE25L30 4 30 inch rail XE25L16 custom 7 16 inch custom rail RMIG 16 corner constructon cubes XE2514 2 T nuts for attachment of braces to rails gt pa tee Figure 125 Side views of the P1640 enclosure rail structure 152 Project 1640 Design and Operations ul Figure 126 Top view of the rail structure A
63. ar s point spread function to a favorable region of the detector Once the observer verifies that the desired target is in the field of view and that the AO correction 1s optimal he should align the pupil of the coronagraph This step is necessary before acquiring data on each target because the ADC prisms introduce a sky position dependent shift in the pupil position After switching to PUPIL mode take a single exposure and inspect the detector image Ideally the illuminated ring is round and symmetric in thickness To adjust the pupil accordingly change the pupil motor positions in Motor Control tab at the lower left corner of the front panel Once the pupil is aligned the observer can switch back to image mode to begin acquiring science data 200 Project 1640 Design and Operations Figure 190 Initial data from the instrument Top left the IFU has been illuminated with a 1330nm laser showing the expected pattern of dots Top right A uniform light source Lower A broadband APLC image on an IFU obtained in the lab 3 6 4 Acquiring Calibration Data In order to enable useful measurements from the science data it 1s necessary to acquire several pieces of calibration data during each observing run By setting aside time for these tasks the observer allows whoever is analyzing the data in the future to constrain the wavelength dependent transmission of the atmosphere and the instrument the spatially varying sensitivit
64. ask the Lyot stop is reflective passing the unocculted portion of the image on to the rest of the system Finally this 1s brought to an image on our lenslet array of the spectrograph using a 600mm Spherical mirror not shown in the figure below The entrance beam into the spectrograph 1s a 1 143 beam We discuss each of these components and their mounts in detail here Estimated throughput Tip tilt pick off 0 50 Spatial filter 0 50 Beamsplitter 0 50 0 50 Anamorphs 0 92 0 92 Re imaging lens doublet 0 92 0 92 Camera losses 0 55 0 55 Science CAL split 0 2 Other 0 89 0 96 TOTAL THRUPUT 5 2 4 5 96 Throughput to CAL 5 total estimated throughput 0 25 96 Figure 7 Initial estimated throughput from February 2010 through cal system courtesy of GV 12 Project 1640 Design and Operations DY T b bl A 0 r wu OSST 3e 058 19q14 5 Figure 8 Coronagraph throughput measurements as determined by Dr Vasisht with help from Mr Robert Ligon in March 2010 Project 1640 Design and Operations 13 Fast steering mirror AO input beam H Figure 9 Layout of the Project 1640 coronagraph All of the optics are 2 4 inches above the optics baseplate except for the the Final Sphere the last optic which 1s 10 3 inches above the table 14 Project 1640 Design and Operations Focal Plane mask o ON OAP3 ye Atmospheric Dispersion Lyot Stop Prisms Fold 4 De
65. at the same time and find a new solution with the Lyot mask slightly larger The parameters of the optimized H band solution are not affected by the Lyot stop oversizing so that the J band performance can be improved by a factor of a few by oversizing the Lyot stop The following figure shows the expected contrast as a function of central wavelength and mask size GRAY Contrast Dark Zone J H band mask size la D Figure 1 Parameter space for the two main parameters mask size at band center lambda 1 65 microns The vertical axis corresponds to the wavelength at which the prolate apodizer is applied 8 Project 1640 Design and Operations Fall 1 4 10 tone INTA sim Contrast ae nn i Y I riterion 1 5 1 7 1 0 1 65 An 4 Seed 1 8 Wavelength m Figure 2 Sensitivity of the contrast criteriion as a function of wavelength in the H band t j Lm B pr e af Contra l e q U a g Position D Figure 3 H band contrast without aberrations The dotted line is the focal plane mask radius and the dashed line is a conservative inner working angle radius of the mask two resolution elements Project 1640 Design and Operations 9 Figure 4 Full images of the Lyot plane at J left and H band right Most of the leakage for this optimum solution at H comes from the light around the central obstruction at J GCORLI8BST Cfravetion Figure 5 Effect
66. bservational data of the requested star should appear In order to observe targets in a new version of the catalog the AO operator needs to load his own version of the new catalog into the main telescope control system The perl script makePal pl takes the csv target catalog file and produces a text file catalog in the Palomar specific format This is accomplished with the following command makePal pl MS format catalog csv This will immediately produce the text file Pall640 current date txt in the current directory Transfer this text file to the Palomar machine vulcan This can be accomplished through a UNIX shell with an scp operation to vulcan palomar caltech edu using the username password user b34mmEU9 Be sure to tell the telescope operator the name and location of the new catalog file on vulcan and have him check that the file 1s formatted correctly before observing begins 3 6 3 Data Acquisition Once the target catalog has been loaded entering the HIP number or other identifying name in the object box will bring up a history of observations for that target The history will come up automatically when you set the image type the number of observations the integration time and the number of reads To prepare the instrument for the new target hit the Set as Target Star button Executing the Set as Target Star command loads the relevant target information into the appropriate xml files that make
67. ce socket while holding the array in place only touching at the corners of the ceramic portion of the chip carrier see photo below lake great care that one of your fingers does not make any contact with the extremely fine gold wires going between the gold pads on the ceramic chip carrier and to the chip itself Any contact could sever a wire compromising the entire detector Once the lever 1s horizontal the chip 1s free and can fall out of place 2 Remove the detector holding it at the corners as in the picture below 3 The detector can be stored in its trasport box as shown in the figure below This is simply a ZIF socket installed on a spring mounted copper plate Place the detector in place in the ZIF socket making sure that all the pins on the back of the array fit squarely into the holes in the ZIF socket The correct orientation 1s noted by a missing corner of pins on the back of the array see photo below This corner should be placed at the corner that 1s closest to were the lever hinges the upper left corner if viewed face on 112 Project 1640 Design and Operations Figure 105 Several steps showing the removal of the Hawaii 2K detector from its ZIF socket 2 2 5 7 Temperture Control The temperature sensing and control in the IFU 1s controlled via two Silicon diode temperature sensors and a rack mounted Lakeshore 3315 temperature controlling unit One sensor 1s located in the center of the copper
68. crews 1 bag 6 32 screws set and normal Palomar mounting hardware mounting pucks mounting half clamp stationary mounting half clamp moving AAO Calibration Hardware Mercury vapor bulb Mercury Lamp 1310nm Laser source 1550nm Laser source hhh Miscellaneous 5 and 6 5 wide rubber sheets 2 Dewar window aluminum blank 1 Phosphor Br sheets 22 36mm thick 1 each 25 thick spacer plates 1 4 20 holes 2 0 5 thick spacer plate 1 4 20 holes 1 Velcro strips 1 pack Dewar handling mech rail dummies 3 standard optical table clamps several 1 enclosure corner blocks 6 1 4 20 enclosure block screws many Newport XE25T4 rail nuts 4 1 2 20 enclosure bolts 3 boxes M6 screws 16 25 30 50mm 1 bag each Adhesive black felt material 1 sheet Corona Beer sign 1 Extra locking pin 1 shims thickness 2
69. d orbits so that the angular separation and orientation of the stars can be computed to adequate precision for the observation epoch The Project 1640 team has assembled a list of binary stars printed out on a table titled P1640 Calibration Binary Stars that meet the criteria of 1 fitting in the field of view 2 a brightness differences large enough so that the AO system can lock on one of the stars and 3 an orbit well determined and listed in the U S Naval Observatory Sixth Orbit Catalog There are only a handful of binary systems meeting 202 Project 1640 Design and Operations these criteria for a given time of the year so the observer should acquire unocculted data of as many of these as possible on each run Acquire 5 read sequences for each calibration binary 3 6 5 4 Dark Frames At some point during the run at either the beginning or end of a night the observer should record dark frames Before doing this make sure that the coronagraph window is covered We recommend repeating 11 dark read sequences for each read length used during the run For example 1f the observer acquired science data in 10 and 20 read sequences then they would take 11 x 10 reads and 11 x 20 reads in the dark 3 6 6 Procedure Summary for Observing One Star The following list summarizes the steps needed for a typical target star observation Immediately after the last exposure switch on Maintenance Mode Set the target i
70. dotted is prior to the coating 04 Project 1640 Design and Operations 100 no AR coating 10 w AR coating e 0 01 Filter transmission 0 001 1 12 14 16 18 2 22 24 2 6 Wavelength um Figure 84 Same as above but now in log scale 2 2 4 Optical performance Here we include some zemax optical perfomance metrics Project 1640 Design and Operations 05 IE 2 POLYCHROMATIC LOG FET PSF DIOP COLL CAT CAM PRISM FOLDS I H COMBINED FRI JUN 30 2026 1 4500 TO 1 8288 pm AT 0 2084 0 0090 HM SIDE IS 51 92 pa SURFACE IMAGE DETECTOR 3 PI S4QSPEC_TH_THERM ZM PEFEPENCE COORDINATES 0 200 4 53208E 302 CONFIGURATION 2 OF e 06 Project 1640 Design and Operations IE 0 m Ul E T DL bh L HROMA i L Lt E Fr po S e CAT CAM PRISM FOLDS J H COMBINED N 30 20606 1 9988 po AT 9 0030 4 3000 HM SIDE IS 663 55 pa IMAGE DETECTOR COORDINATES lE E 1 IE 2 E 3 IE E gt PI6 40SPEC TH THERM ZM ZHBULE BOO 3995E CONFIGURATION 2 OF e _ a PEFERENCE ul POLYCHROMATIC LOG FET PSF CAT CRM PRISM FOLDS J H COMBINED N Ju Ae b 1 9888 po AT 0 0080 6 1000 HM 664 52 pa IMAGE DETECTOR gt COORDINATES ODOULE 000 1 54645E ae PI6HOSPEC JH THERM ZM CONFIGURATION 2 OF Project 1640 Des
71. ds Then inspect the new image in the ds9 window Measure the counts sec values of the brightest pixels Calculate how many 7 7 second reads can be accumulated without saturating 65 000 counts sec In practice the P1640 team has found most occulted stars can be recorded with satisfactory count values using 5 10 or 20 read exposures Sticking to those exposure lengths also simplifies the data processing After setting the number of reads 198 Project 1640 Design and Operations set the No of Images field to however many exposure loops are needed to reach the desired cumulative exposure time For example with 20 read exposures setting the No of Images to 15 will result in a total of 7 721 15 20 2316 seconds 38 6 minutes of exposure Hitting Expose starts image acquisition Two indicator bars display the progress in the current exposure sequence Once the desired number of images has been taken the history window changes to a note window where comments may be entered During the acquisition of each exposure an assortment of observational information 1s collected from the Palomar AO system All relevant data such as time telescope position and air mass are written to the header of the corresponding FITS file After each image acquisition the DAZLE software executes a script called 1640 export data in home optics ucam bin This script uses FTP to move FTIS files to the Data Acquisition workstation The DAC inform
72. e tae at ET LALA AA de T bh nn 2712127797122 1712 141 nr o iarbarrbinipnisSnici id lal sree TII ere ere tee te tot ee te tet ee te tet te tet te tet SELES ES LARISA HEELS EE OCECE PEEL Ete HE ete hertetas SS SS 0S SST So shertererteter IIIIISITIIEISITIIIIIIIIIEIIIIIIIEISIIMIIMEIUIII TIT 171271717 177101 ITI I ILIRISRARARRARARAS e 9 TMPMTTTMCPE TP P E Ah tty roS OTTON tere PTO ere Tere rt ee PCP ETO PT ete Pe Pt rmrm 121 22 2170127277217 7971271777712 1771297227712 1712171212 71712 77277 ICRA FIFA FICS FISICAS FICA LARISA FIFA FIFA FICA TII TALULA LALA 444 errr sates tetee 2122 Im TETTETETT etm 22 7297929279 SS HESS PSST SES SS SES PSSST STS SE SOS Pe Se She 971 SHCHCS HCHO FE ICI TOULL LOLLO mor o o s TANTINO SE Ee OS MH TTTttt nr M2 2 1221121220012 2721221272212 3192221922222 Te Pe eT Serre rer rs SHES HTHCSPSHTECS HT HCE TEPC IIIJ IJI IJ re Hehehe et 2122121217777 17 949499 9 P M 9 OF 9 mme EERE EE EEO E HMM 9 III III III SE Oe EE Oe 8 Oe EES Ee EOS E rr et eters IIIS ert TTT te tot eT Te tote terete Let Te LLL LLL eee TTT Te Te ToT Te TOL Te TOL LOLOL TOLLE ett ttm ttp tma tatem 4949499999999 9 99 94929 7 9 9 29 9 Eee Eee ete T TOTOLO Rerec rrna rra am ipinidriniaidicicinri nididricici nicidricinid4cinid IIT TULIP ial 12 22222 222222
73. e Shift Mirror Tip Titt Beam Splitter Tip Tilt Sensor Figure 110 Detail for the P1640 Wave front calibration system 118 Project 1640 Design and Operations Image of Pupi Image of Target OPD RT MI gigement mirror and LOWF 5 Besesph tier Figure 111 Cal optics in detail with mounts removed Image courtesy of GY Figure 112 Another image of the Cal System courtesy of LCR Project 1640 Design and Operations Cryolines AE A Major Components 1 New cryostat Ucryo with Polycold Joule Thompson cold head remote compressor 2 E grade Teledyne Picnic Array 3 Leach controller for TPF BIBs extensively modified 4 Detector commanding and data acquisition based on PCI interface DSP assembly code based clock generation Wavefront Sensing H band 1 64 um interferometric wave front sensing 64x64 resolution Speed 250 kHz pixel reads Y 40 Hz 64x64 frame rates Current max possible is 128x128 pixels at 10 Hz PACE HgCdTe at lt 90 K Can support J or Ks band operation with filter swap Det Performance Quantum efficiency 0 7 Dark current 10 e pix sec 82 K read noise is 18 e cds read amp 10 e rms with 4 non destructive reads Backgrounds baffling within camera snout to restrict A N Figure 113 Cal system camera specs courtesy of GV 119 120 Project 1640 Design and Operations 1 nm 10 nm t nm LAB Exposure Time 5 e 3 E gt 6 Stellar Magn
74. e code directory The following variables should be changed SIRAF PATH is the file name of your IRAF interpreter cl e PIPELINE_PATH is the full path to the directory where the pipeline source code and executable will reside DATA_PATH is the directory where the processed data will be stored SLIBRARY PATH is the directory of the pipeline library files Initially these are located inside the pipeline directory SIRAFSCRIPTS PATH is the directory of the IRAF scripts Initially these are located inside the pipeline directory After those are set run the Perl script on the command line S configure pl This will produce a customized Makefile By default the Makefile links to an Intel Mac version of the CFITSIO library included in the pipeline tarball If you re not using an Intel Mac you ll need to modify this location to your own machine s installed version of CFTTISIO Next to compile the pipeline run Smake The program should compile with no errors or warnings Last to allow the IRAF scripts called by the pipeline executable to run do Smkiraf to initialize a login cl file in the pipeline directory 3 7 3 Using the Data Pipeline Provisional for March 2010 run Project 1640 Design and Operations 205 The newest version of the pipeline on the Data Analysis workstation 1s in the directory proj1640pipe 2010march Open an xterm and change to this directory To test that the pipeline 1s installed correctly
75. e correction as a function of relative rotation angle between the prisms We first worked out the theoretical values which turned out to be fairly close 10 off in strength 10 degrees or so in rotation We then used the short exposure speckle pattern to get the fine corrections As you of course know in the short exposure PSF in a reasonably broad band the speckles all streak towards the PSF core A mis calibrated ADC makes the speckles streak towards some other point The radial position of that point is set by how wrong the strength of the ADC correction 1s and the azimuthal position is set by errors in the total rotation of the ADC Using that it s fairly simple to adjust the correction parameters to put the speckle streak point in the center of the PSF at which point your ADC 1s calibrated I think this is quite a sensitive procedure at least very fine adjustments were required to get it right We repeated this procedure for all our filters Telescope time is of course needed for this but it s quite quick After our first few trys we got 1t down to about a couple of minutes per calibration ESI MIO a DOO eO O ee 6 Hu D x lime vt Pg em inb m P4 vw E SY MS WITUDNNOUCURTUTT LES Sey onu weg TN O 1 DITA IED LIDO Gee UND 1 Au v Project 1640 Design and Operations e mOB IICA Wile ON NS 3 Um VIX e SFO WAY 5E NONI Sore The two wedges of CaF2 and BaF2 are Isms Figure 24 Design for ADC pr cemented tog
76. e mask and let the unocculted portion of the image around the hole be reflected on to the rest of the optical train The hght that has passed through the hole 1s used to drive our tip tilt system using a set of four infrared Hamamatsu photodiode sensors The center of the stellar image is maintained on the sensors using a centroiding algorithm in conjunction with a control loop working with our fast steering mirror FSM Our fast steering mirror is updated at a 1 kHz frequency to maintain the position of the star on the center of the spot To determine the best combination of mask parameters for the APLC we have optimized our mask characteristics by calculating the expected contrast and PSFs for the system Considering just the H band along ignoring the J band we identified a very good solution for the H band which is also acceptable at J We have found however that optimum solutions for the combination of J and H bands exist but they require masks that are much larger impacting the inner working angle IWA too much In addition the AO system will not Project 1640 Design and Operations deliver the same performance at J band so 1t is not necessary to have the same theoretical contrast at J band However we find that we can improve the performance at J band by oversizing the Lyot stop central obstruction to elimanate most of the J band leakage in the Lyot plane Putting these two issues together we re optimize the H band solution
77. e prolate spheroid apodization prescription as described in Soummer et al 2003 The transmission profile is defined by a microdot pattern lithographically placed onto the suprasil substrate The dots are placed on a 2 mm grid initially via electron beam lithography followed by a deposition of black chrome Figure 18 The apodizing mask left and Lyot mask right Project 1640 Design and Operations 21 mous 19 ygo wave front measurements of the Focal plane mask ei Ex T AAA GN oio gm m 3 4nm rms focus subtracted Figure 20 Zygo wave front measurements of the P1640 apodizer 22 Project 1640 Design and Operations Figure 21 A scanning electron microscope image of the focal plane mask edge Position arcsec 0 ac Uu Bea E Gu 0 8 Gar Ge MN 3 9 di N 11 y zl j E 3 QE 13 I G 6 me RA 15 3 o p o 9 7 17 e 19 8 21 I La 2 L 0 5 10 15 20 Position 4p D Figure 22 Achieved contrast on the GPI APLC testbed at the AMNH Astrophysics Lab We expect to achieve a similar level of coronagraphic suppression with P1640 2 1 3 Atmospheric Dispersion Correcting Prisms Refraction in the earth s atmosphere will cause the position of a star at one wavelength to differ from the position at another wavelength From the blue edge of the J band 1 05 mm to the red edge of the H band 1 75 mm this displacement can be 100
78. e slices of the extracted cube facilitating the detection and photometry of faint objects 3 7 2 Installing the Data Pipeline In order for the cube extraction pipeline to compile two C libraries need to be installed CFITSIO and GNU Science Library CFITSIO is currently available from http heasarc nasa gov docs software fitsio fitsio html Get the latest version of the UNIX tarball and after unpacking it somewhere home directory works fine follow the standard UNIX installation described in the README configure make make install Be sure to preface the make install command with sudo The GNU Science Library 1s currently available from http www gnu org software gsl After unpacking this configure the installation with the disabled shared option as in configure disable shared followed by sudo make and sudo make install 204 Project 1640 Design and Operations After obtaining the pipeline program tarball unpack it in an appropriate location where it can reside permanently Copy the Lib subdirectory of the CFITSIO source code directory into the pipeline directory overwriting the existing lib subdirectory There is a subdirectory in the pipeline directory called include Into include copy the fitsio h fitsio2 h and longnam h header files from the CFTTIO source code directory Next you will need to edit a few file system paths in configure pl a Perl script located at the root of the pipeline sourc
79. ed short BSCALE default scaling factor HIERARCH START PAR VALUES UNKNOWN Application parameter value VERSION UNKNOWN Application parameter value Project 1640 Design and Operations NUM EXPsS I Application parameter value DWELL 7 Application parameter value LED_FLSH UNKNOWN Application parameter value NUM READ 2 Application parameter value X SIART I i Application parameter value Y_START l Application parameter value X SIZE 2048 Application parameter value Y SIZE 2048 Application parameter value RD TIME 6000 Application parameter value RS TIME IO Application parameter value HIERARCH END PAR VALUES UNKNOWN Application parameter value HIERARCH COM TAB SIARTI UNKNOWN Application parameter value UT DATE 6 4 08 UT date at start of night ISCOPE 200 HALE 200 Hale Telescope at Mt Palomar INSTRMNT P1640_CIFU AMNH Coronagraphic IFU FOC PLNE HAWAII 2 Dazle Hawa112 detector WAV_BAND JH Wave Band SPEC RES 30 Spectral Resolution FILE NAM ABAur O 72 fhit Object Date Type Number fits OLD NAME 00001330 As assigned by DAC run fits OBJECT AB Aur Object RA 4 55 45 93 Target R A in hours J2000 epoch 2000 DEC 30 33 46 1 Target DEC in degrees J2000 epoch 2000 RAPM 2 RA proper motion mas yr DEC PM 24 DEC proper motion mas yr VMAG 7 06 JMAG 5 94 HMAG 5 06 KMAG 2 423 OBJ CLSS
80. esign drawing for the meniscus lens parent BEVEL BEVEL TA E 500 MAX FW i 7777 f EZA e D70 00020 050 H 025A f yA tf ho Olos 4 Fr 74 8227 900 l j VIA SEE NOTE 5 6 EA E d H R214820 TE E LA SEE NOTE 5 4 C 80 000 0 050 A SEE NOTE 4 que 14 43 SECTION C C PARENT AXIS A t Notes 7 1 UNLESS OTHERWISE SPEOFIED MIL O 13830 APPLIES TIT 2 MATERIAL 41360501 BLANK o TEMA OFF AXE SECTION CUT FROM PARENT AS SHONN rras E 5 AR 1 05 2 AVG TRANSMISSION gt OR TO 88 OVER eno Ga MB w AM AN ADI OF PER MC CAMUTA PARAGRAPHS 411 LAMP PY PPP ee CA VERA LENS in 6 CLEAR APERTURE BEST EFFORT FOR FULL SURFACE mo manus een se ues NO TS A 41360 501 A ON 81 AND 52 MR LG e no SA SCALE PEC 8N558 SHEET 2 OF 2 Figure 75 Design drawing for the meniscus lens Project 1640 Design and Operations 77 254 565 4X BEVEL Trk 0 500 MAX FW A 4x BEVEL 0 500 MAX FW i 3 UN 7 a f gt PLAND m n Sud a 3 ban i i i on p gt MIOS SAS 12 a S i A AX BEVEL EDO MAX FW eT Map CT 12 0000 100 CA 54 XI ECUON AA ole erst PL D ur ex Art MATERA FUSTO SUCA vtt QUAL TY AND SI ARE PX EL RECOMD WEDGE 4 EE EA JANOS 14 ar p 4 e VILA ADIVA PARADAN ITCHMNDOILOGY e at 1 4 of Dro CAMERA LENS 2 A 41360 502 A Figure 76 Design drawing for the field lens Meniscus Lens Mount The mount for the meniscus lens 1s incorporated
81. ether and cored out Project 1640 Design and Operations 29 CELL ASSEMBL Y IE 2 E FP app TA ATV DEO o4 AROUND Cer TE Ge LN SET PRIOR TO SOONG INTO HOUSIMC ws P Figure 25 Final Assembly of the ADC prisms Note that the profile drawing shows a 31 8mm diameter plastic cap which arrived with each prism assembly This plastic cap was removed prior to installation in the motors 30 Project 1640 Design and Operations Thin part SECTION A A Figure 26 The arrow on each assembly indicates the correct orientation It points in the direction of the exit beam The placement of the arrow around the ring coincides with the thickest part of the CaF2 wedge and the thinnest part of the BaF2 wedge Project 1640 Design and Operations 3l Trammision 9 IAT TA nA LL AI WAT ETE TAS Ree tf LTT TT 101 10 678910 Wavelength microns Figure 27 Prism glue transmission curve Figure 28 Inserting the ADC prism assembly into the SR50 Newport motor 32 Project 1640 Design and Operations Figure 29 Zemax drawing from Chris Shelton of the prism pairs 1n the beam 2 1 4 Tip Tilt System We are using a Physik Intrumente S 330 30 Piezo tip tilt platform in conjunction with an infrared position sensor comprised of four individual PIN photodiode detectors built by Hamamatsu G6849 series The sensor detector area is mm in diameter and sensitive from
82. for both crates in and out of them The ramp is stored in the larger crate To load the largest crate the IFU and coronagraph combination are be mounted on the handling cart and the cart rolled into place in the crate Iud PT Poem inches handling cart 35 x 37 x 61 Safe Art Transport 26 x 29 x 22 158 Project 1640 Design and Operations Figure 152 The two large shipping crates for the Project lavender containing the instrument plus its cart and the electronics rack respectively We use the larger of the unpainted crates for miscellaneous items 3 Operations 3 1 Alignment 3 1 1 Coronagraph Alignment After the instrument is placed on the AO Bench 1 Rotate bench so 1640 optics are vertical on the table table underneath 2 Turn on stimulus with brightest source available laser Turn on the entire 1640 system and put the tip tilt mirror at the midrange done by software automatically on running Move all motors to nominal positions Project 1640 Design and Operations 159 3 Before moving anything try to tilt FM1 only to see whether the beam can be directed to form a good image at the FPM This is probably not possible However if the beam follows the path indicated in the Zemax and Inventor models but is out of focus at the FPM change the AO focus to see whether it can be brought into a good focus 4 If this works adjust FPM x and Y to direct the beam onto the lyot stop Use Pupil Cam for fine al
83. from the outside of the dewar The assembly has a mounting bracket see Section below to provide focus movement and prevent Project 1640 Design and Operations 4 any flexure while the telescope 1s rotated While at Palomar the whole assembly hangs down from the AO bench The bottom half of the Project 1640 dewar 1s the same as that for PHARO but mirrored internally so that the detector is on the opposite end of the dewar from the window We maintain our temperature near 77K with 0 01 K rms stability The LN2 fill holes are in the same place as on PHARO but unlike PHARO s five ports this dewar has four ports two for the LN2 inputs into each can one for the vacuum pump and another for attachment of a vacuum guage Radiation shielding and Liquid Nitrogen tanks Inside the outer surface of the dewar are the upper and lower radiation shields The shields are wrapped in multiple layers of mylar insulation Like the PHARO dewar the Project 1640 dewar has two separate LN2 tanks The smaller 3 3L inner can is directly bolted into the optics base plate via fourteen 10 32 screws The underside of the baseplate has a region scalloped out for the small can for even more effective coupling between the two The primary role of the small can is to provide a local heat sink for the detector and optics The larger 11L can maintains close contact with the radiation shield and serves as the more global dewar cooler This large can is bolted to the wo
84. he dewar vacuum feed through port has a single military type connector while the detector controller box has two military connectors Project 1640 Design and Operations tas as A tw ee A EUA AA AA Ne ee tk ewe mms c e om o e Figure 101 Design drawing for the detector mount baseplate 107 108 Project 1640 Design and Operations DRAWING DATE 01 74 07 i j i i i i or ererar a o we Figure 102 Design drawing for the detector frame The copper block slides into the square region in the frame Project 1640 Design and Operations 109 li n jl Figure 103 More design drawing views of the detector frame Se al A e m tm Project 1640 Design and Operations ass mmp B 4 Ae 4 9 sARATIF am FO As oZ 33 47b Hem UA om thue amp m pem oar m al ng ommo o9 s dm ooo o 1 pun M M 9 need T terap Ate ML oe we we ame e na PTs 9v 110 104 Design for the rear detector mount plate which is connected to the PCB copper block and the detector frame Figure Project 1640 Design and Operations 111 2 2 5 6 Detector Removal and Insertion To remove the detector chip from its mount on the PCB extreme care must be taken not to impart any electrical shocks to the array but also to ensure the chip does not fall since its mounted vertically 1 First lift the aluminum lever on the left side of the ZIF Zero Insertion For
85. holes provide access to these screws Project 1640 Design and Operations 105 Figure 98 Left the middle mount plate moves left to right Note the fin on the right which guides the upper detector frame Right The detector frame piece moves parallel to the beam path and can be moved to adjust the detector focus The detector cabling which comes out of the plug at the bottom of the PCB travels straight down through a groove cut into the detector mount base see photo below This cabling travels down through the main optics baseplate via a semi circular hole see drawings of dewar baseplate and out through a hole in the radiation shield These cables are soldered to a 41 pin Amphenol vacuum feed through socket P N 602GB 07H20 41 PN Mil C 26482 specification which is o ring mounted to a round Aluminum plate bolted to the dewar The cabling for the detector has a single Military type connector on one end and two military type connectors that are plugged into the detector electronics box see photo below The detector electronics box 1s connected to 1ts power supply via a single multi pin military type connector Figure 99 The Amphenol vacuum feed through socket The aluminum portion shown on the right is the surface making contact with the o ring on the 106 Project 1640 Design and Operations aluminum dewar plate The black housing clamps this aluminum piece to the dewar ensuring a good seal Figure 100 Detector Cabling T
86. id Nitrogen stinger used for PHARO placed into the large tank on P1640 During the initial cool down only the large tank should be filled No nitrogen should be put into the small tank if the internal temperature is above 95K Note also that the insulating foam is not shown in this picture 5 After several fills of the large tank and roughly 24 hours the small tank can be sately filled Should we let the AMNH folks do that when we get here 3 2 4 3 Expedited Warm Up using Dry Nitrogen gas Warning when the dewar 15 cold and filled with dry nitrogen the Nitrogen gas acts as a coupling between the cold dewar internals and the warm outer shell of the dewar This will cause the outer shell of the dewar to become cold and water condensation to form on the outside of the dewar including the dewar window and puddles of water may form under the dewar This water can drain down into the optics base plate causing rust If the dewar 1s in a cold state and needs to warmed quickly the dewar can be flooded with Nitrogen gas dry nitrogen Such gas has no water vapor in it and will not affect either the optics or the detector However this 1s a sensitive operation on many different levels and care should be taken Project 1640 Design and Operations 175 Amm 905 os gt a e 3 ud y T ving lie 4 4 a Ld M a Y Hook up the special KF 16 dry nitrogen fitting
87. idest part of the door in the North direction Project 1640 Design and Operations 177 Figure 174 The Cass cage has been rotated into the position needed for mounting 4 The green handle on the handling cart must be removed via the two large nuts at its base before the instrument can be raised through the Cass cage door 178 Project 1640 Design and Operations rs Figure 175 The AO bench showing the four mounting pucks Figure 176 The orientation of the instrument on the Palomar ram must be aligned with its mounting place on the AO system Project 1640 Design and Operations 179 5 The handling cart is placed onto the hydraulic ram in the same orientation as that which the instrument will be mounted on the AO bench see photo below which is the gold electronics box facing out At this point the instrument 1s ready to be raised up on the ram 6 Raise the instrument on the Ram so that the A frame passes through the widest part of the cage door see photo below 7 Pump the handling cart pedal until the instrument lower platform the yellow portion 1s higher than the narrowest part of the Cass cage door see photo below When this has been achieved the cart can be moved towards the center of the cage Figure 177 The instrument being raised on the ram through the widest part of the Cass cage door 180 Project 1640 Design and Operations I A PIN a l ANANAS A WALK M y X y AA a See i CONO C o A
88. ign and Operations DIOP COLL CAT CAM PRISM FOLOS J H COMBINED FRI JUN 30 2086 t BSGO TO 1 92988 po AT 9 0080 7 5000 HM SIDE IS 665 55 pa SURFACE IMAGE DETECTOR 3 REFERENCE COORDINATES 08 8E 8OO 1 98495E 801 DIOP COLL CAT CAM PRISM FOLDS T H COMBINED FRI JUN 30 2026 1 0500 TO 1 8088 pm AT 4 2094 7 0003 MM SIDE IS 641 21 pu SURFACE IMAGE DETECTOR 3 PEFEPENCE COORDINATES G 2NABLE 200 76823E 001 POLYCHROMATIC LOG FFT POLYCHROMATIC LOG FFT PIS4YOSPEC_JIH_THERM ZM CONFIGURATION 2 OF PL64OSPEC_TH_THERM ZM gt CONFIGURATION OF 88 Project 1640 Design and Operations lE E 1 IE 2 IE Z IE 4 E POLYLCHROMA TIC LOG FFT PS DIOP COLL CAT CAM PRISM FOLDS J H COMBINED FRI JUN 20 2086 1 4580 TO 1 9288 pm AT 7 9880 7 0000 MM SIDE IS 676 23 pa CJ Li ul SURFACE IMAGE DETECTOR 3 P1S4OSPEC_TH_THERM ZM PEFEPENCE COORDINATES 1 77847E 001 1 79435E4081 CONFIGURATION 2 OF POLYCHROMATIC LOG FFT gt S DIDP COLL CAT CRM PRISM FOLDS I H COMBINED FRI JUN 30 2006 1 8588 TO 1 9888 pm RT 7 B8800 7 0020 MM SIDE IS 649 149 pa SURFACE IMAGE DETECTOR 3 PLS4 SPEC_TH_THERM 2ZM PREFERENCE COORDINATES 1 77366E 001 1 74594E 001 CONFIGURATION 2 OF Project 1640 Design and Operations coo DEFOCUS IN um gt THROUGH FOCUS SPOT DIRGRRM DIOP COLL CAT CAM PRISM FOLDS J H COMBINEO EE Mem 30 2006 em ARE pm AIRY RADIUS
89. ignment Fine tune Lyot stop tip tilt to center the beam on the final Sphere and the rejected light onto Pupil Cam lens Tilt final sphere to center the beam on the dewar window beam cover center of milled aluminum pattern Take images to center up the focal plane mask on the detector s field of view by only tilting the final sphere Adjust focus of dewar until satisfied If OAP2 needs to be moved 1 Most likely the above will not work and both FM1 tip tilt and the OAPI need to be moved to get the beam going down OAP2 s axis The focus position after FM1 is as per the inventor drawing close to hole 10 5 check and the beam should be incident on OAP at hole x x with a width of 4 mm To proceed remove the Apodizer FMI s tilt is determined by placing the beam in the right location Now the only free parameter is OAPI tip tilt and xy position on table A slight misalignment of the OAPI axis to the beam results in significant astigmatism It must be positioned so that a good image is produced at the FPM To do this do not move the FSM FM2 or OAP2 Simply move OAPI to get a good image on FPM well centered on the mask hole This may take 3 weeks It may be helpful to remove the ADC prisms during this process If the stimulus phase diversity software works 1t may provide superior metrics in placing OAP2 To achieve this retroreflect the beam after the ADC prism assemblies to get a return beam back to the stimulus camera Final twe
90. ignment and stability between the collimator assembly and the prism This mount drawing below 1s attached to the optics baseplate via six 1 4 20 screws The baseplate has six tapped holes for the mount The position of this mount relative to the baseplate is shown in a drawing below The position of this mount is critical for the overall performance of the instrument The collimator assembly housing and the prism are mounted at different heights so the portion of the mount containing the prism 1s raised slightly to achieve the proper height for the prism Project 1640 Design and Operations X X us O It 5 E Y e T LJ E r Na Lo iz lt m x o o 2 2 2 hs m _ 3 M F Y gt e e I y pl pa Li s Doa 4 EI e si m G lt G a Figure 62 Machine drawings for the collimating assembly holder 65 c ac pa o ad es abso So Ium o Res oa ol ntl MA o ooa oo oom ee te 0 1 8 YHSYS HNWY bam 9p KU e cw m t e ae o ee Project 1640 Design and Operations a3sSvu WSTHd ONY YOLVHITIOS d emp an a pjm a y am pe nw LLL su Cae UA 3m 9 A v 1 1 tane py o e m o ee ho y g eae oc bd b m ge pe LI t i Ag 4 mo s Ys 5 E b t Jiva i i Figure 63 Machine drawings for the mount holding the collimator as
91. igure 46 Isometric views of the P1640 baseplate showing the region carved out for the small LN2 tank as well as the scallopped regions to reduce load Figure 47 The P1640 charcoal getter placement on the baseplate Project 1640 Design and Operations odes Cit LO meme o ay ps tud LIA ore n mem A Figure 48 Dewar internals showing the placement of the optics Project 1640 Design and Operations 51l Dewar window The beam from the coronagraph enters the dewar through a single 2 inch piece of CaF 1 2 inch thick that has been anti reflection coated for the region 0 5 2 0 um This is sealed against the dewar via an o ring a trough for which has been milled into the outside of the dewar see photo The window is kept firm in place via a brass outer housing which is bolted directly to the outer shell of the dewar Figure 49 The dewar window o ring left and the window with its blanking plate right Project 1640 Design and Operations 52 Dewar Snout 2 2 2 Ae TK SPIT G 10 y ETA RING P ml E ponve ADAP SPF 38 1 24 wns Alumindiae TUBE DWG OLI 10 ANNH A C Figure 50 Internal blackened tube for the dewar snout This piece is cryogenic 93 Project 1640 Design and Operations Heic ISON OFYOGENIC S TPH PHARO IDo M JEX VACUUM D y Ru T 2 130 T 0Q 4285 p2 00 2 5 Ciia Snes SyS 2 US INC D if
92. in 4 Tir a E a i a LE gt 2 e o X x gt i o f 1 x x 1 c _ Ad m e o dAl E d D A c is a z I Figure 136 Custom optical breadboard from Thorlabs showing five locations for mounting pucks Project 1640 Design and Operations 143 9o UNC B INC 18 Figure 137 Placement of mounting pucks on underside of mounting plate 144 Project 1640 Design and Operations AA 11 1 P d e Figure 138 Design drawings for the puck mounting mechanisms One puck is attached to the PALAO bench and the other to the P1640 bench When these are adequately lined up they may be clamped Project 1640 Design and Operations 145 Detail B TI SEE i t pro tS 918 trem i D a n 05 THU LJft20950 2x Ott GOD THPU TAP Wide 7 BO Figure 139 Machine drawings for the mountng pucks All four pucks are identical 146 Project 1640 Design and Operations LAA 3 ore CAME LOL A LOR A3 rr ANH 2 Figure 140 Machine drawing of the locator pad for each clamp This pad serves as a pilot for each pad to ensure each clamp pair is aligned the same way each time the instrument is removed and replaced on the telescope Project 1640 Design and Operations 147 z E nf i ji a2 Figure 141 One half of each clamp mechanism this half of the clamp remains fixed on each cla
93. in the dewar The temperature sensors list in degrees Kelvin 3 2 2 Pump down procedure Palomar Mountain Crew First hook up P1640 Lesker pressure gauge to the pressure sensor on the dewar both shown in the photo below and check the pressure This gauge should be set to read in mbar but scrolling through the electronic menus will allow you to adjust the settings need more info here Project 1640 Design and Operations 163 Figure 156 The P1640 pressure sensor and the corresponding pressure guage The guage can be read in either Torr or mbar 2 Make sure the black handled plunger is sealing the dewar closed by ensuring the plunger 1s pushed all the way in Remove the KF25 cap on the vacuum fitting and attach the vacuum pump Figure 157 The P1640 vacuum valve The left picture shows the black handled plunger out dewar open while the right shows the plunger down dewar closed Also theKF40 to KF25 adapter is shown on the right 164 Project 1640 Design and Operations Operator in place prior to Seal off valve in place aher evacuator evacestion Figure 158 A diagram showing the inner workings of the brass plug which seals the dewar Note that the black handle need not be unscrewed in any way It only needs to be pushed or pulled in and out Unscrewing will detach the shaft from the brass plug 3 If the dewar internal pressure 1s room pressure pull out the plunger dewar open Start the vacuum pump and ve
94. ing data We recommend switching on the Maintenance Mode before beginning a night of observations at least one hour before taking any science or calibration data Make sure that Maintenance Mode is switched on whenever data 1s not being taken In addition to the LabView control panel a separate application called the AO Paddle needs to be launched in order to permit small changes to the instrument pointing To start this open an xterm on the Data Acquisition workstation Run the following commands ssh X aousr harbor palomar caltech edu enter password ao usr Sidl IDL gt aopaddle Now select P1640 from the instrument menu and the AO paddle will be ready to step the instrument pointing by an adjustable angular increment in any cardinal direction The beginning of every Project 1640 observing run requires especially close coordination with the Palomar Adaptive Optics AO System operator There 1s a fair chance that both the beam alignment and the Zernike polynomial coefficients of the AO system will need to be tweaked requiring the Project 1640 user to take a series of test images of a white light source built into the AO system The user should plan to dedicate roughly one hour of the start of every observing run to optimizing the optical interface with the AO system Before astronomical observations begin power on the Data Analysis workstation and log in as DataAnalysis abaur This machine is useful fo
95. ining all of the electronics associated with the Tip tilt system as well as the temperature control and Data Acquisition Computer 2 1 4 2 Pre photodiode Optics The pre optics are composed of a flat mirror directly after the FPM a 150mm focal length achromat l inch Thorlabs lens part number AC254 150 C This is mounted in a standard 1 inch mount on a post 2 1 4 3 Circuit diagrams The circuit diagram for the Hamamatsu IR sensor power supply is shown in the following diagram he base power for the quad cell system is 120V with an upper range of 13 132V and a lower range of 10 104V In the Cass cage the voltage has dropped as low as 105V during the night approaching the lower limit Project 1640 Design and Operations 37 Figure 34 Circuit Diagram for Hamamatsu infrared PIN photodiode quad cell assembly 30 Project 1640 Design and Operations 3 BOOS ITV Figure 35 Quad cell detector board layout The individual quad cells are labelled J2 5 1n the diagram 2 1 5 Coronagraph Optical Bench The coronagraph is a T horlabs custom breadboard measuring 18 x 54 x 2 36 One side has a standard 4 20 grid of 1 inch holes while the other side has tapped holes for five custom mounting pucks see below Project 1640 Design and Operations 39 Figure 36 The Thorlabs 18 x 54 coronagraph optical bench with several pieces of the coronagraph in place 40 Project 1640 Design and Operations
96. ire coronagraph IFU package is mounted on a single Thorlabs custom breadboard 18 x 54 x 2 4 in size One side of our breadboard has 4 20 tapped holes on a one inch grid suitable for mounting the coronagraphic optics and the dewar mounting bracket The other side of this breadboard contains four custom aluminum pucks for mounting the entire assembly to the Palomar AO system The AO bench has an identical set of pucks attached in the same configuration When the instrument is raised up to the bench the four opposing sets of pucks are aligned and clamped together with the dewar and coronagraphic optics hanging down This procedure allows complete repeatability in each mounting 140 Project 1640 Design and Operations E E i t gt gt gt gt 8 Figure 134 The AO bench layout with the placement of the four mounting pucks shown Project 1640 Design and Operations 141 Figure 135 Side view of the AO bench showing the AO beam height as well as the placement of the pucks 142 Project 1640 Design and Operations r9 ri a Dow s gt 9 wt B OM I DS LA b f i a Y j wr m 4 y o wT nul e i i 734 4 B a 4 L 433 s I mia n gt bw y es a E i a i 2r Y A gt E J ow us aS E s T zs T Y ak oa oe I gt p2 1 wx F 13 X YA x sw l2 d
97. itude H Figure 114 Initial exposure time estimates for the CAL system courtesy of GV 2 4 Ancillary Components 2 4 1 Dewar Support Focus Mechanism To maintain dewar stability while minimizing flexure during telescope slewing have have developed a custom dewar handling bracket and manufactured by Opticology in New York City Our dewar has three mounting pins two towards the front and one on the rear face which are used to attach to our mounting bracket I he entire bracket assembly 1s mounted on flexure resistant rails which allows 20 30mm of focus movement using a fine thread screw This mounting bracket also allows a 10 degree tilt using a screw jack mechanism at the rear of the dewar allowing the entire dewar to pivot on its front two mounting pins by applying a vertical movement at the rear pin Project 1640 Design and Operations 121 Figure 115 The detector focus and support mechanism The entire assembly can provide a 10 degree tilt via the screw jack mechanism in the rear pivoting on the front two pins The entire mechanism is mounted on low flexure rails mounted in runner blocks Table 8 Parts list for the dewar handling mechanism rail systems Ball rail 176mm long Rexroth Bosch R160520231 Ball rail 116mm long Rexroth Bosch R160520231 25 8 preload H accuracy Project 1640 Design and Operations 122 Ixe NYI OL O31INDOW 38 Ol 31 v 143S v 8 OS3I8W3SSV CISIANIO 38 TIM XOS JV id
98. l components 3 6 Observing Procedures Here we describe the procedure for observing with Project 1640 once the instrument has been cooled mounted and all cables and communication links for the Cassegrain cage are in place 3 6 1 System Initialization After the Data Acquisition workstation has been powered on log in with the user password pl640 p1640 Load the LabVIEW control panel LOCATION FILENAME If configured properly the Lab View front panel will indicate the dewar temperature which at this point should be near 78 Kelvin for both the detector and the plate Find the System Init menu tab at the lower left corner of the panel Turn on the DAC machine with the power button After 1t finishes booting hit the Launch Camera Servers button This will open three terminal windows and a ds9 window for displaying the most recent detector image Unfortunately the DAC machine may have to be rebooted many times before it initializes properly Once it 1s working the user should leave it on for the duration of the observing run Next hit the RST RCO Init button to initialize the camera Next power on the detector 196 Project 1640 Design and Operations In order to minimize the amount of charge that builds up on the detector when it is left idle there 1s a mode of operation implemented in the control panel called Maintenance Mode Switching this on will cause the detector to be continuously read when not tak
99. ler Project 1640 Design and Operations Figure 195 SDSU controller to Hawaii 2K wiring 229 230 Project 1640 Design and Operations ee 7 e te oe Res is La E zi FCR sd Cnt ta 5 thas 2 5 Figure 196 Printed Circuit board wiring diagram Project 1640 Design and Operations Figure 197 Accelerometer measurements taken on the P1640 bench in longitudinal direction of the instrument with no telescope tracking Figure 198 Longitudinal measurement with telescope tracking on Project 1640 Design and Operations Figure 199 Longitudinal measurement with tracking on and dome spin Figure 200 Measurement along the telescope axis with tracking on Project 1640 Design and Operations 233 Channel 1 Figure 201 Measurement along the telescope axis with tracking on and spining dome 234 Project 1640 Design and Operations 4 6 Miscellaneous Drawings LN2 FILL TUBE v a A gt E we NEED Iu bee OF STRAIGHT PIPE Y ae A E im THREADS ED TD RE Abov T 3x4 IDE AND jb THREADS Y ade N THese VME ERS NEED TD BE ChELLED PRECISEL Figure 202 Liquid Nitrogen stinger used to fill the dewar Project 1640 Design and Operations 235 M AR 011 10p PRECTRION CROUOGENTIC SYSTER 717 P732 FAN p c a uii i al WASHER gt Any BE Ayo LE Lor
100. ll 182 Project 1640 Design and Operations Figure 180 The mounting clamps Note that these clamps have had some posts installed which raise the clamps making the installation easier 11 When the clamps are tightened the eight M6 bolts on each of the instrument mountng plates can be removed At this point the instrument is fully mounted to the telescope and the handling cart can be lowered down and stored Project 1640 Design and Operations 183 Figure 181 The eight M6 screws used to secure the instrument to each mounting pad on the handling cart 3 3 2 Mounting Electronics Rack The electronics rack will be placed in position 5 shown in the figure below Figure 182 The P1640 electronics rack will be placed in position 5 184 Project 1640 Design and Operations 3 3 39 On PalAO spit in the AO lab Mounting the instrument on the AO bench on its spit is nearly identical to the mounting process on the telescope The brake on the AO spit may need to be removed for clearance Other than this there are no serious clearance issues 3 3 4 Cabling procedure Connecting the electronics control box is a sensitive job and needs to be done carefully Make sure vou are fully grounded before making any connections Es ld Figure 183 Cable Bundle 1 connected to the rack 3 3 5 Control Room Setup and Power up Procedure Project 1640 Design and Operations 185 3 3 6 De installation and stowage procedure
101. low the upper A frame portion of the handling cart to move in the plane parallel to the floor bottom The x y adjustments that facilitate this movement top Project 1640 Design and Operations 155 Figure 148 The A frame portion of the handling cart 156 Project 1640 Design and Operations Figure 149 Design for either of the two rotating mounting plates onthe handling cart The instrument is mounted via the 8 M6 sized holes on each place The 8 screws screw directly into the optics baseplate shown below v Figure 150 Eight M6 holes in the workplate used for mounting the instrument on the handling cart Project 1640 Design and Operations 157 Figure 151 The instrument on its handling cart Note the placement of the shims between the cart mounting plae and the instrument itself 2 4 6 Transport Crating The Project 1640 Transport is handled by three crates with the dimensions given in the table below The two largest crates for transporting the instrument and the electronics rack were built by SafeArt Transport in New York city All crates are wooden and the two largest crates have an outer wooden structure For weatherproofing the insides are lined with Tyvek and the dewar joints are lined with a rubber gasket Also the paint adds a level of waterproofing Each door on the larger crates are secured with bolts and the floor is lined with masonite There is a small ramp which can facilitate moving the instrumentation
102. ly done with two people As the pressure in the dewar begins to rise and finally passes room pressure you will be able to feel dry nitrogen leaking out of the seal between the dry nitrogen fitting and the I adapter When you feel this excess Figure 172 Necessary setup for dry nitrogen warmup 176 Project 1640 Design and Operations has rushing out the dewar 1s at room pressure and the VENT handle can be fully closed Next quickly lift the dry nitrogen fitting off the I and replace it with a KF 16 cap Do not clamp this cap to the I junction Instead place a small weight on the cap light enough to keep the cap in place but light enough so that the nitrogen gas can escape as the dewar warms The dewar will warm at a rate given by the plot below and probably not exceed 1 degree K per minute Figure 173 Temperature plot for the dry nitrogen warmup 3 3 Installation 3 3 1 On telescope installation procedure If the instrument and rack are being stored in the AO lab both can be transported on their casters to the freight elevator and raised up to the observatory floor l Prior to installation the IFU should be evacuated and cooled as per the procedure in Section 3 2 2 and 3 2 4 2 The instrument should already be mounted on its handling cart in the optics down pucks up configuration 3 After the cage door has been removed the Cassegrain ring needs to be rotated by 180 shown in the figure below with the w
103. mas To correct for this we use two sets of Risley prisms via the prescription in Wynne 1996 Each prism set 1s constructed by coring out a cylinder from two cemented wedges of BaF and Car The Project 1640 Design and Operations 22 amplitude of correction is determined by the zenith angle of the target star and the positions of these prisms are update every second Atmospheric Dispersion from 1 05 wm to 1 75 um at Palomar 400 c O 200 Dispersion mas 100 0 20 40 60 80 Zenith Angle degrees Figure 23 The Differential Atmospheric Dispersion from the first channel in a cube to the final channel as a function of zenith angle Table 2 Summary of Design parameters for Atmospheric Dispersion Correcting prisms Thickness along mechanical axis Exiting beam Thick part of CaF thin part of Bak 24 Project 1640 Design and Operations Atmospheric Dispersion Calculations from Chris Shelton 10 18 2007 3 03 32 PM Telescope diameter m 5 16 Beam diameter mm 4 21 Optimization wavelength range um 1 00 to 1 85 Plot wavelength range um 1 00 to 1 85 Magnification 1225 9 Zenith angle degrees 50 00 Barometric pressure millibar 827 Effective temperature of air column C 10 0 Max allowed surface angle from axis deg 30 0 Range of surface thickness mm 6 00 to 10 00 Pupil distance mmy 112 00 Pupilrmsweight 1 000E 0002 Pupiloffsetweight 1 000E 0002 Pivot
104. minimal loss due to roll over between the lenslets The rear face lenslets have a 159 um radius of curvature to create the pupil images 280 um behind the lenslet array substrate The effective f number of each lenslet 1s f 4 measured using the diagonal of each square lenslet 106 1 um Each lenslet has a pitch of 75 um We have 270 x 270 lenslets on our array but only use 200 x 200 lenslets The array is mounted 4mm directly in front of the first lens of the collimator The table below lists many of the characteristics of the array Project 1640 Lenslet Design EX Square fused silica substrate 30 x 30 mm 267 x 267 square lenslets 75 ym pitch Aligned lens surfaces on both faces Maximize fill factor lt 2 um gap between lenses Radus of Curvature 950 um Radius of Curvature 158 5 um v ye 220 ym i t p LS 1 mm On this side Ihe lenalets should be blackoned exceot for a 60 x 60 micron square centered on each lensiet Figure 56 Lenslet Array Design Specs The exact clocking of the lenslet array can be changed with the turnable knob on the front of the collimator housing This adjustment knob has fine threaded screw 100 threads inch CHECK THIS so the rotation can be controlled easily The clocking assembly has a retaining spring against which this fine threaded screw works The assembly can occasionally become sticky and the rotation may need to be assisted manually i e just rotating the threaded knob may
105. mp set as the clamp screws are tightened 148 Project 1640 Design and Operations 99 3 de e a Y LI gt i v Ed Cc MJ 2 0 7 a x d D r i e C 4 e Ll t c X e Us a gt a i B o 4 rs 2 9 a a E s 2 A r a i t i T 1 i i Figure 142 One half of each of the mounting clamps This portion will move inward and secure the tow pads together as the clamp screws are tightened Project 1640 Design and Operations 149 C 4200 mee PP 4 4 p ll a ins 4958 M x 70 i gt E Ej PF de fs 2 AAA a E e Baneao gt e a l 4t Figure 143 Revised version of mounting pucks including the cone lock height pads 150 Project 1640 Design and Operations Sagra 12221 meu Figure 144 Machine drawings for the mounting puck alignment jig frame Project 1640 Design and Operations 124 Figure 145 Machine drawing of alignment jig mechanism 152 Project 1640 Design and Operations 2 4 5 Handling Cart We have developed a customized handling cart for smooth instrument transport The cart design aids in the installation on the AO bench primarily via two features 1 Six spring housings cushion the transport as well as provide differential compression As the instrument 1s raised up on the Cassegrain elevator the slightly
106. n the control panel Turn off the ADC Tell the operator the slew to the chosen target Switch coronagraph to Pupil configuration Turn on the ADC While the operator is locking the AO system align the Pupil Switch coronagraph configuration to Image mode 9 Switch exposure mode to Core and acquire Core images 10 Occult star using AO Paddle 11 Lock the tip tilt system 12 Switch exposure mode to Occulted and expose 3 7 Data Processing The Project 1640 Data Pipeline processes and calibrates the raw detector images to prepare the data for inspection and analysis Most importantly the pipeline extracts data cubes from the detector images two spatial dimensions the third in wavelength The pipeline can run on any computer with a GNU C Compiler IRAF version 2 14 or newer and a Perl interpreter for the initial configuration For maximum efficiency during an observing run we recommend a second observer oversee the operation of the Data Pipeline on incoming data at the Data Analysis workstation while the other observer leads the acquisition of new data with the main Project 1640 control panel The username password for the Data Analysis workstation 1s DataAnalysis abaur and the IP address is 198 202 125 17 Project 1640 Design and Operations 203 3 7 1 Data Pipeline Description In order to extract cubes from the raw detector image the Data Pipeline program has a library of 1mages made using a laboratory tunable
107. ns cell assembly lens cell retaining face 1s placed into a lens cell holder piece Six 6 32 set screws are used to keep this lens cell centered in the holder One side of the holder has two set screws while the opposing face has a single screw To keep the lens cell firmly against the back register of the lens cell holder a U shaped retaining piece 1s attached to the lens cell holder via six 6 32 screws Simply securing this retaining piece onto the lens cell holder 1s not sufficient to keep lens cell 1n place However the retaining face has three 6 32 set screws to press the lens cell back against the back register of the lens cell holder The blocking filter carriage assembly is screwed directly to this lens cell retaining piece This entire lens cell assembly 1s screwed into the bottom plate of the detector mount via two 10 32 screws Slots in the lens cell assembly base allow the whole assembly to move forward or backward 10mm stroke for focusing purposes Figure 77 The left shows a mock field lens in the lens cell with the phosphor bronze springs used to hold the lens in place The right panel shows the teflon gasket which serves as a compliant material between the lens and its retaining face Project 1640 Design and Operations i SS iw HAY Na 79 Project 164 E instituto ot Astronomy exploded c gt p pum EF Nm Force cone small A Figure 78 An exploded view of
108. o camera server HTTP command http 195 194 120 66 7063 list Get dummy application file command to camera server HTTP command http 195 194 120 66 7063 get fhilename hawailrg dummy app xml Get NDR application file command to camera server HTTP command http 195 194 120 66 7063 get hlename hawanlrg ndr app xml Project 1640 Design and Operations 99 Non Destructive Read Correlated Double NDR mode Sampling CDS mode xr Owell 6700ms r uo gt t 5 amp Dwel 3 8 6700ms 1 5 3 2 E E time Dwel 8700ms Num_read 8 Num read 4 Num_read 2 fixed Num exp 1 Num_exp 2 Num exp 3 Fits file is the average of the slopes counts sec Figure 89 Two schematic drawings showing the Non destructive Reads NDR and the Correlated Double Sampling CDS modes of detector readout This is the algorithm for the NDR slope used in the demux task EN Vii ey idum dl x 13 n 11 where V is the voltage of the sample i n is the total number of samples and dt is the time interval between the samples Ref SPIE Vol 1235 Instrumentation in Astronomy VII 1990 Figure 90 Formula used for NDR slope in the de multiplexing software This is not well understood 100 Project 1640 Design and Operations for P1640 Figure 92 The power off left and power on right lighting configurations on the SDSU controller 2 2 5 4 Printed Circuit Board The detector 1s housed in a black Zero Insertion Force ZIF socke
109. off valve in place alter evacestion Figure 154 Detail showing how the brass plug can be pulled in or out of the dewar Venting the dewar When you are pretty sure the dewar is not cold stop Check again It is a good idea to have 2 3 checks look at the temperatures sensor ask people if there 1s any chance it 1s cold look at the logbook etc to make sure that the dewar 1s warm enough to be vented Venting room air into the dewar when it 15 cold could form ices on the optics and detector ruining the entire spectrograph The plot below shows the dew point the combination of temperature and pressure at which condensation would form on the optics and detector for various humidities and room temperatures For example the dew point as read on the the temperature sensors for a 75 degree day with 20 humidity will be 272K i e the temperature sensors must read at least 272K before venting should begin However for a 75 degree day with 40 humidity the dew point is at about 283K Note however that these calculations should only be used as guides so play it safe and let the dewar warm a bit more than these tempertures before venting Currently the only way to vent the dewar with room air 1s to connect the vacuum pump vacuum the hose open the dewar and slowly leak air into the hose and dewar Connect the vacuum pump hose to the dewar valve fitting if it is not already connected The dewar will be closed now Verify this by making sure the
110. on Correcting Prisms s ee e qoi te eee ien n RE 22 22 P NER ler d i sane E 32 21 5 amp oronasraph Opt calBetieIi static rere bebe sies 30 2E MUST 40 2 A MOV i MU NENNEN 40 guae E tex ue UEM NE m Mc I Mop put 52 2 29 Optical D sien AiG CO PGS on 54 2 9 AN DN e wo oni UI NERA DOR ce REL UB REDIERE uU UNIS 04 22 97 Detector ySL E 92 2 95 Wave ront Calbrato nta iii 117 2425 mella COMpPoOnc aaa 120 ZA Dewar support Focus Mechanist dis 120 Dee y O E EO sabaten sees 131 ZE stem Gabino DESI rain 135 2 Intertice with Palomar AO syste ts 139 2219 O viuo ent eile ts ud Di edes ss ERR Rosada ds deno ou odis dios 152 2480 DranspOLD CTN 157 D ET 158 als ZAMTSTITHO HE onse vette lia 158 Dl WOOrODndsraprHr XI S DEDE DIE oce eto RA tbt us aatis Nee tei ie eque 158 3 2 Instrument Preparation and IFU Dewar Procedures AMNH 159 9 2 PP dovi procedure AVENEL osse enn ii eee eii 159 3 2 2 Pump down procedure Palomar Mountain Crew ococccccnnononcnononannncnnnnnnnns 162 0 2 9 Coolin procedure AMNH escis esset tinent eei D nen ssi e 165 3 2 4 Cool down procedure Palomar Mountain crew cccccccccnnnnnnnnnnanananannncnnnnns 170 2 9 InstallatiOll ap es ub t Gt td tct uS tU obe etaed 176 0 9 1 Ontelescope installation DFOCGQUEE a 176 9 9 2 Motuntno Hector 183 S008 On PabXC Pi tie 2X0 das isses I DEN RN RN RU e MU 184 9 04 AI DO i 184 3 3 5 Control Room Setup and Power up Procedure
111. onsistently have a hold time around 60 hours Project 1640 Design and Operations 169 Final coo down 7 6 08 om B I4 t sm o uE J mp a gt t e C A mum E Bau 4 gt on u 7 vw m 60 ME ee ee m 4 m J O 0 5 g A 24 2 5 elopsed time hrs E ET e o 00mU XP P i lt a D 7 b 220 4 e j b t D amp m P a 4 1 p B x Pi 4 D E A gt p j 1 m M 4 uor E gt a D e a E lol gt a gt lt gt a s gt m n sU ij m s Qn d U U gt T J bre hrs Figure 164 A plot showing the temperature drop after placing some LN2 in the small tank This should only be done when the large tanks have been full for an extended period and have reached 95K 105K 170 Project 1640 Design and Operations Holding period 2 6 08 3 18pm 2 11 08 9 010m HN O Small tank ce e empty i x Large tank empty o Temperture K Ww g O O 0 20 40 60 80 100 120 elopsed time hrs DETAIL of Holding period 2 6 08 3 18pm 2 11 08 9 010m 80 5 80 4 80 3 Temperture K 80 2 80 1 0 20 40 60 80 100 120 elopsed time hrs Figure 165 The points at which the two tanks are exhausted are shown in the top plot Bottom Detail showing the intrinsic temperature wander 3 2 4 Cool down p
112. picture of the secured railings are shown below The railings are secured to the table via standard Newport optical table clamps An XE2514 I nut and an 8 32 screw is required to secure the clamp to the rail while the clamp is secured to the table via a 4 20 screw Figure 127 Left the enclosure rails and corner blocks for the enclsure Right The rails are clamped to the workplate via standard optical bench clamps using a T nut in the rail Project 1640 Design and Operations Figure 128 Design drawings for the enclosure panels 133 134 Project 1640 Design and Operations Figure 129 Design drawings for the enclosure panels cont Project 1640 Design and Operations 135 2 4 3 System Cabling Design 1640 Wiring Schematic incomplete Figure 130 Internal wiring schematic Project 1640 Design and Operations 156 6 K o As MZ ra i e F a7 ua Si ANZI RAM Pi Fo h M n i ao a z A A 4 L 7 A Aae o s e ul qeo WOOY 01 U0N Or9L 12efoug Figure 131 Control Room Cabling Un c O p a Q a ce a q E op u Q a E lt 45 Q Q o am Figure 132 Cass Cage Cabling Internal Rack Cabling Figure 133 P1640 Internal Rack Cabling Project 1640 Design and Operations Project 1640 Design and Operations 139 2 4 4 Interface with Palomar AO system This section describes the design for mounting to the PALAO bench Our ent
113. r a second observer to process and inspect incoming data The disk drive of the Data Acquisition machine can be mounted from the Data Analysis machine over the ethernet network facilitating rapid transfer of data To take advantage of this capability open a Finder window on the Data Analysis workstation select SHARED select p1640 and connect with user password p1640 p 1640 3 6 2 Target Catalog The Project 1640 target catalog will inevitably grow over the lifetime of the instrument as new objects of interest are added Here we outline the procedure for loading a new version of the target catalog into the data acquisition interface and the Palomar Telescope Control System The LabVIEW control panel expects a catalog stored as a Microsoft format csv file Example files are stored on the Data Acquisition workstation The location of the current catalog file can be viewed in the LabVIEW control panel by opening the Paths tab in the lower left corner By placing the new catalog at the same location the user can replace the old catalog To load the new catalog into the interface restart the LabVIEW control panel The user can verify that the new catalog 1s in place by checking for the existence of one of the new entries To do this enter either the HIP number or another identifier in the box in the Star Project 1640 Design and Operations 197 Catalog area in the lower right corner of the front panel The coordinates and other o
114. r can one of two LN2 stingers can be used either the normal PHARO stinger or the custom P1640 stinger The stinger used for PHARO may stay in the tube better To insert the stinger the instrument must be rotated 30 40 degrees on its cart to allow access to the fill port Remove the locking pin on the handling cart and allow the instrument to rotate Caution The instrument will choose to rotate on its own so be prepared for a rotation when the locking pin 1s removed Once the tube has been inserted the instrument can be rotated back to its original position and the locking pin replaced Figure 169 The threaded locking pin on the handling cart Use care when removing this as the instrument will immediately rotate when this pin is removed see photo below Project 1640 Design and Operations 173 Figure 170 The locking pin is removed and instrument is rotated in order to insert the LN2 stinger This orientation is the instrument s natural orientation after the locking pin has been removed 3 Allow the Nitrogen to flow freely into the large tank It 1s a good 1dea to drive the 50L dewar with Dry nitrogen to keep the pressure up around 6 psi The pressure on the guage will fall significantly to between 1e 03 or 1e 04 mbar during the fill 4 The fill may take 20 30 minutes Several fills over a few hours may be required to get the large tank full Refill several times 174 Project 1640 Design and Operations Figure 171 The liqu
115. r results with better removal of bias tilt hot pixels and cosmic rays The finished cubes are placed in a subdirectory called DATcubes rather than FITScubes t causes the pipeline to use the dat file to make a series of cubes from the difference of every pair of consecutive reads in a given exposure sequence f to turn off the flat field by default it is on b to fit the bias in the detector image rather than subtracting one of a library of dark images This is necessary a to process all types of images in the given directory rather than Just Core and Occulted Images These switches can be combined so for example the user can run S pipeline DATA goodstuff do Or S pipeline DATA goodstuff odf 206 Project 1640 Design and Operations Lastly the s switch allows the user to override the focal plane alignment determined by cross correlation with a laser reference For example S pipeline DATA goodstuff so 0 3 0 6 instructs the program to shift the detector image by 0 3 pixels in x and 0 6 pixels in y before extracting as opposed to using values determined by the cross correlation algorithm QO 3 7 4 Procedure Summary for Running Pipeline Provisional for December 2009 run Transfer the fits focal plane files you want to process e g HD172648 O 127 fits to some directory on the Data Processing workstation e g DATA goodstuff In an xterm window change to the pipelne directory
116. rify that the pressure is going down on both the pump guage and dewar guage If only the pump gauge shows a pressure drop but not the dewar either a the black handle has not been lifted or b 1f the black handle has been lifted the brass plug is disconnected from the shaft but still sealing the dewar middle picture above If this is the case screw the handle back into the brass plug and pull up to dislodge the brass plug If the pressure 1s significantly less than room pressure leave the plunger pushed in dewar closed start pumping and only release the plunger when the vacuum hose pressure is similar to the internal dewar pressure Since the pressure in the vacuum hose is similar to the internal dewar pressure it should be pretty easy to release the plunger Cont nue to pump down until dewar the dewar reaches 0 2 0 1 mbar this may take 30 60 minutes Close the plunger on dewar The inner tank on the dewar is now ready for LN2 Project 1640 Design and Operations 165 Pumpdown of P1640 dewar no cryo cooling 12 7 2009 12 9 2009 1000 1000 100 100 _ 10 10 T L 2 E 1 y p z o 0 1 0 1 i o 0 01 0 01 0 001 dewar closed 3 0 001 0 0001 0 01 0 1 1 10 100 1000 104 Time elapsed minutes Figure 159 Measured pumpdown rate for the P1640 dewar Pressure in Torr 1s on the left mbar on the right Note the logarithmic scale 3 2 3 Cooling procedure AMNH The rate of cooling the dewar needs to be
117. rk current distribution for a HAWAII 1 array operated at 78 K This has a mode of 0 026 e s pixel and a high dark current tail extending to 0 15 e s pixel Bailey et al 1998 quote a mean dark current of 0 05 e s pixel with gt 99 66 of pixels having lt 1 e s dark current for a HAWAII 1 array operated at 77 K and 0 5 V reverse bias Mackay et al 1998 report a mean dark current at 90 110 K for three of their HAWAII 1 arrays of 0 1 e s pixel and 2 e s pixel for an earlier fourth array They note that for their devices 10 of all pixels have dark currents gt 5 times the mean 4 have dark currents gt 10 times the mean and 1 have dark currents gt 20 times the quoted mean value These hot pixels behave in a predictable and repeatable way The latter two high dark current measurements are partly due to the higher detector reverse bias voltage or higher operating temperature used We conclude that HAWAII 1 arrays are capable of achieving modal dark currents as low as 0 01 e s pixel when operated below 70 K and with reverse bias voltages lt 200 mV but that the dark current distribution has a tail extending to gt 0 1 e s pixel The node capacitance 1s 40 fF at this reverse bias Hodapp et al 1996 so the well depth is 50 000 e PACE technology devices have fast output amplifiers permitting sample times of 5 us pixel but they suffer from declining quantum efficiency at wavelengths shortward of 1 3 um QE
118. rkplate via three posts just behind the G 10 tabs The dewar s internal parts remain at 77K for 60 hours without refilling the nitrogen tanks see hold time plot below Optics base plate All of the optical mounts for the IFU are mounted onto a single baseplate inside the dewar This is a single rectangular piece of l inch thick 6061 T 6 Aluminum 23 3 8 x 11 38 1n size Several regions have been scalloped out of the underside of the baseplate to reduce the weight of the piece In addition a charcoal getter for absorbing volatiles wrapped in metal screen and aluminum foil has been installed on the underside of this plate Project 1640 Design and Operations 42 PR AAA Vidi AIN di NOR wet motus MPO AO Py ee www ober acc vae pn DS AA UA MA a ew desi UU tran fA e mA a ORA e RPR P Sern m sean p elm ery M n LIA uh pn mtm ons noni Jemog 091 129 04d Figure 38 Project 1640 Dewar 43 Project 1640 Design and Operations epo IN om ma Dom nat dhu Kn qaom Hurt Fm ma rim pem Um pem ARA qaom ew A oap mmm mg cua m mo pfi mi ihc ALLE t AR y edm A Fa CN EAT A LAA PA de UE aee ores pued pase qi Apa oi Pa A ote del mmi W IN mes shielding and outer Figure 39 Project 1640 Dewar showing radiation portions of Liquid Nitrogen tanks Project 1640 Design and Operations 44 Tae VANA LAA AAA AAA AMARME AA ERR ZE ALZA TT 00 A gt Se e 0000
119. rm special steps need to be taken Request that the AO control system loop be left open and that the sidereal tracking be switched off Lastly the number of reads should be set to at least 10 so that any surface features are averaged out in the resulting FITS file of each exposure To minimize flexure distortion in the images observe the Moon as close to transit as possible Repeat at least 5 read sequences 3 6 5 2 Spectroscopic Standard Stars In order to account for the wavelength dependent transmission of the atmosphere and the instrument during each observing run the observer should obtain a core exposure sequence of at least one star with a readily available reference spectrum A suggested list of F and G stars has been compiled for this purpose printed on a table titled IRTF Spectroscopic Standard Stars hey are all stars that have publicly available spectra in the Infrared Telescope Facility IR TF Spectral Library Also note these stars are dim enough V mag gt 5 9 that the PSF core won t saturate the detector in a single read Repeat 5 exposure loops for each spectroscopic standard star 3 6 5 3 Calibration Binary Stars lo enable high precision astrometry it 15 necessary for the data analyst to constrain the plate scale and orientation of the science images Observations of calibration binary star systems are the currently favored solution to this It is necessary to use binary stars with well determine
120. rocedure Palomar Mountain crew Once the dewar has been evacuated down to 0 1 0 2 mbar the outer large tank 1s safe to be filled First the temperature sensor should be connected 3 2 4 1 Connecting the Temperature Sensor To connect the temperature sensor and read it out while doing the P 1640 cooldown procedure 1 Connect the thick grey cable to the dewar with the milspec connector on the port on the short side of the dewar the back if you will Figure 166 Milspec temperature controller cable 2 Connect the other side of this cable to the Temp Sensor connector on the front panel of the electronics Project 1640 Design and Operations 171 rack 3 Plug in the electronics rack The power cable is coiled and stored in the bottom left corner of the front panel where this is an opening in the front panel Just pull this cable out and plug it into a standard wall socket 4 The only thing left to do is to power on the Lakeshore temperature controller The power in the rack is controlled by a single power strip controlled via TCP IP but it can be controlled from the back of the electronics rack Open the back of the rack The power strip is at the bottom and you should see to the left 6 unlit LEDs and a small circular red button Press this button and one of the LEDs should start blinking Press it again and the next LED over will start blinking You want to illuminate the LED labeled 6 Once that one 1s blinking
121. s is just a shortened copy of the Axsys part 2039 122 00 height 2 400 See detailed drawings in appendix 2 1 1 4 Apodizer Optic 12 7 mm transparent apodizer Pupil is 3 9 mm in diameter More detail is given in the following section Mount Newport SN050 F3 lockable kinematic mount with ADAP I SUP 0 5 to provide 0 32 mounting point from 2 56 screw through mount MS 500 XYZ MS AP 3 Adapter plate MS A T K screw kit x2 May need another 0 75 inch base plate MRP3 0 25 MRP3 0 5 3 x each Model 38 x2 Height adjustable Chromium alloy microdots on glass MEMS Optical denopt k Tum 2um microdots MEMS apodizer Figure 13 Detail of the Jenoptik microdot apodizing pupil mask The astrometric grid is evident in the upper left panel 2 1 1 5 Fast Steering Mirror FSM Tip Tilt Control Optic Lyot Project FSM on PI 5303 10 Stage Mount Interface plate from Lyot Project to new Custom L Bracket Part AMNH1640 4 Height 2 400 See detailed drawing of this mount in the appendix 2 1 1 6 Atmospheric Dispersion Correction ADC prisms Optics Two cemented wedges of BaF2 and CaF2 wedge angles of 26 467 and 29 159 respectively A single prism set 1s cored out of the cemented wedges Prisms are contained in a l inch cell for mounting in the Newport SR50CC mounts Central thickness is 12mm for the cemented set See section below for detailed drawings Project 1640 Design and Operations 17 Mount 2 x
122. s the LabVIEW control panel that the file has been sent using the scrpt file sent in home optics ucam data The Data Acquisition workstation listens over a designated port for the file sent signal Prior to sending the file the Data Acquisition workstation 1s told that image acquisition 1s complete so that the software can grab the latest position settings After the exposure completes and the FITS file is transferred to the Data Acquisition machine the new image appears in the ds9 window The orientation of the image with respect to celestial coordinates 1s diagrammed in Figure 1 along with the relationship to the orientation of the lenslet array Figure 2 shows an example of raw data as 1t appears in the ds9 window during observations Project 1640 Design and Operations 199 Looking at Front Looking at Lenslet Face of Detector Array B A C D Data as represented by DS9 To obtain NE orientation Flip about y axis Rotate by 90 Then view is like looking At the detector Figure 189 Schematic showing how the data are oriented on the detector upper left on the lenslet array upper right and as it first appears in the DS9 window Between exposures the observer can fine tune the pointing with the AO Paddle as described in section 1 1 1 1n order to move the image of the target on the detector This will be necessary for example to accurately occult a star with the focal plane mask or to move a st
123. sembly and the prism assembly 66 Project 1640 Design and Operations Figure 64 The placement of the collimator and prism mount relative to the optics plate The six 1 4 20 tapped holes for the mount were drilled according to their location relative to the Axsys mount holes as shown Project 1640 Design and Operations 67 2 2 3 3 Prism Dispersing Element Our prism is a single piece of BK7 glass with a wedge angle of 4 on each face 60mm in diamter and a central thickness of 15 135mm This prism 1s optimized for the wavelength range 1 05 1 75 um with a dispersion direction parallel with the plane of the workplate The prism is secured in it s housing via a wave spring and a retaining ring Three 10 32 screws secure the housing face and hence the prism to the rest of the housing in Figure 65 The JH prism This montage shows the prism being mounted into its mount Note that the wave spring needs to be mounted prior to the retaining ring bottom row 68 Project 1640 Design and Operations The prism assembly shares the same mount as the collimator assembly This assembly rests on a portion of the mount that has been raised slightly due to the varying heights between the collimator and the prism We have also developed a customized pupil mask to be placed onto the prism mount This prevents stray light from entering into the optical path This mask is secured onto the prism mount via the three 10 32 screws Howe
124. sistors Heater Control Set Point 81 K Heater Control Parameters set using Lake Shore auto tune P Gain I Gain D Gain 3 9 3 Cassegrain Cage Rack Motor Cables Number on cable to label on front Panel motor type 0 FPM x CMAI2CCCL l FPM y CMAI2CCCL 2 T T offset x CMAI2CCCL 3 T T offset y CMAI2CCCL 4 Unused Card for Goniometric 5 Unused Card for large Rot Stage 6 ADC I SR50CC 7 ADC 2 Connected to SMCI00CC SR50CC Internet Cables Unicom Fiber Switch l DAC 198 202 125 165 2 FSM 198 202 125 166 3 RS232 TCP IP box 198 202 125 167 4 5 6 7 8 Power Strip 198 202 125 169 9 Fiber Cable to Project 1640 Design and Operations Unicom Smart Switch IP router see above MAC Address 00 00 1C 01 57 CE IP 198 202 125 168 Use Safari or Internet Browser do not use Foxfire User Password root 193 Fiber Port connection port 9 uses I00Base FX technology to make it compatible with Palomar Lava Ether to Serial Link RS232 TCP IP converter MAC Address 00 04 3B 00 3D BF IP 198 202 125 167 Passwords admin and portl port2 etc T CP Ports 1 4098 Newport Motion Controller a Mode Raw Server b BAUD Rate 19200 c Bits 8 d Panty None e Stop Bits f Flow None 2 4097 Lake Shore Temperature Controller Use Crossover Null Modem Cable Mode Raw Server BAUD Rate 9600 Bits 7 Parity ODD Stop Bits 1 Flow None 96 SMC100CC Motion Controller Mode Raw Server B
125. t to pull the plug in or out the shaft does not need to be turned in any way To evacuate Make sure the pump hosed 1s clamped onto the KF 25 valve fitting with a suitable clamp and an O ring greased with some vacuum grease The stiffness of the vacuum pump r hose has a tendency to exert some significant torque on the entire valve fitting Make sure the pump An and hose 1 placed in such a way as to minimize the torque on the fitting Starting with the plug in its dewar socket make sure the shaft is screwed into this plug by giving the black handle several clockwise turns When you have convinced yourself that the shaft and plug are connected pull the shaft straight up do not unscrew The dewar is now fully open Start the pump and only the roughing pump will be working initially After several minutes the turbo pump will achieve a rotation of several hundred Hz The dewar should be left on the pump for several hours If a significant work has been done on the dewar it should be left on the pump for a longer period This is especially true 1f new volatile producing substances tape ink etc have been incorporated into the dewar or if you suspect there may be fingerprints inside After about 24 hours of pumping the dewar will achieve a pressure of around 2 mbar 1 2 Torr At these pressures 1t 1s safe to begin putting Liquid LR 5 _ T e E Project 1640 Design and Operations 161 Nitrogen into the tanks Seal
126. t which is mounted on a custom printed circuit board shown in the drawing below The rounded corner of the board was determined in order to prevent collision with the radiation shield In addition a copper block see drawing below has been soldered to the back of of the ZIF socket to act as a good thermal cooling pathway This block also serves as the primary mounting mechanism for the Project 1640 Design and Operations 101 detector A single aluminum plate Copper Block holder in the drawing below 1s used to mount this copper block to the detector mount via four M5 screws PROJECT 1640 Be Au asc a T Te L Le EO ov e A e e gt lt hoc j E ns b Figure 93 Design drawings for the P1640 Printed Circuit Board 102 Project 1640 Design and Operations Contact Steve Modan Tet 012232 228927 9 Fax 01223 330804 eed sra CAP ac us 000000000 166 HOLES SPACED 7 54 1 5 6 0 DEEP mI IT Fa y M PROJECT 1640 Heat Sink 7 E31 NE institute of Astronomy HeatSek c ds Figure 94 This copper block serves as the primary detector heat sink and is soldered to the back of the ZIF socket on the PCB Note the tapped hole for the temperature sensor mounted in an M3 screw 103 Project 1640 Design and Operations sU GIL t ME Pe z p SERN HOHE 1000 em y h P m gt 1 3 Br ML A iy E ac tam ed J s gt i4
127. the edges Right The actual blocking filter with the retaining face installed The filter mount 1s comprised of two pieces a filter carriage to hold the glass substrate and a retaining face to keep it fixed against the back register of the carriage As with the field lens a 50um teflon gasket 1s placed between the glass and the rear register Also phosphor bronze springs are used to hold the filter centered in its carriage Note that there is only a Imm gap between the carriage and the glass substrate 0 015 teflon gaskets are placed between the filter and the retaining face outside the clear aperture The screws for mounting the filter assembly sit in slotted holes to allow 8mm movement of the carriage when incorporated into the rest of the field lens mount The filter was specified to allow greater than 75 transmission from 1050 1750nm The actual transmission curve is shown in the plot below Note that the filter is slightly out of spec and turns on closer to 1100nm with some sharp peaks in the region 1100 1200nm The filter was also specified to have OD5 blocking from 400 1000nm and OD4 blocking from 1800 2700nm The filter comes close to these benchmarks The dotted line in the transmission spectrum was measured prior to the AR coating while the solid line 1s post coating Project 1640 Design and Operations 83 Figure 83 Transmission curve for the JH blocking filter used The solid line is the spectrum after the AR coating while the
128. the field lens mount assembly including the mount for the blocking filter The compliant teflon gaskets are not shown 80 Project 1640 Design and Operations Figure 79 The field lens holder mounted on the rest of the detector assembly Figure 80 The entire field lens mount and blocking filter mount installed into the rest of the detector mount Project 1640 Design and Operations 81 1 o m mou picor gt y be AMNH Sasha Drawing date 11 19 07 ee Ua cade foe Pelee oC Ere meee Fee Of he Bete te E ett Che aep of Ue bee e de Got eee fee Cty Faso cn ta P Figure 81 Machine drawings of the lens mount and detector mount Note the distance of 1 004 in between the face of the detector frame and the back of the field lens cell holder This distance is critical for instrument focus 02 Project 1640 Design and Operations 2 2 3 5 Blocking Filter We use a 60x60mm square blocking filter to achieve the passband for the instrument The filter has a 57x57mm clear aperture and is comprised of three cemented pieces of glass a 2mm thick piece of Schott RG850 and two pieces of Schott B270 with thickness 2mm and 3mm The filter has an 8mm thickness The edges of the filter have been sealed with a hermetic polymer Figure 82 Left A mock filter placed into the filter holder The 50 micron teflon gasket 1s visible on the back register as are the phosphor bronze springs at
129. um Focal Plane Mask size Optimal coronagraph wavelength Apodizer throughput Telescope Diameter Bio Niah 2D 1 1 8 m Date Available 1 2 Acronyms Used The following 1s a list of all acronyms or abbreviations used in this document Atmospheric Dispersion Project 1640 IFU Coronagraph 1 05 1 75 um AX 0 7 um 1 405 um 73 um chosen for manufacturing 1ssues f 143 21 5 6 A d 1 65 um Palomar 3000 Actuator AO System D 5 10m 1010 to 1818 mas March 2010 1 5 m subaperture with 90 Strehl usable in 5 Correction Correction for what is sometimes 6 Project 1640 Design and Operations called Differential Atmospheric Refraction FOV FPM FSM Tip Tilt system ZIF Zero Insertion Force 2 Design 2 1 Coronagraph lo suppress the starlight of our target stars we have built an apodized pupil Lyot coronagraph APLC based on the designs of Sivaramakrishnan 2001 and Soummer 2003 2005 We achieve our suppression with the combination of an apodzing mask a Focal Plane Mask and a pupil plane Lyot mask This section describes in detail the design and optimization of our APLC which can theoretically achive a suppression of 10 at 5A D Our design is further constrained by the f 15 4 Palomar Input beam space constraints on the PALAO bench and the 75 um lenslets pitch Our focal plane mask FPM is reflective with a 1322um diameter hole We use the hole as an opaqu
130. up DAZLE s instruction set and sets the values for the header of the FITS data files Tell the telescope operator the Palomar TCS number of the target so he can slew the telescope and lock the AO system Note that you should always switch off the atmospheric dispersion corrector ADC while the telescope 1s moving A button on the right side of the front panel switches the ADC on or off Before an exposure sequence begins the user can set the Image Type option to either CORE or OCCULTEDS based on whether or not the star is currently behind the focal plane mask The CORE and OCCULTED options are solely for the purpose of organizing the data the focal plane mask remains physically fixed in place regardless There is also a PUPIL option to form an image of the coronagraph pupil on the detector Switching to and from PUPIL mode requires a few moments to allow the motors to position the optics appropriately Monitor the indicator box underneath the Image Type switch to verify that the instrument 1s ready for the new exposure The user should carefully set the No of Images and READS controls for each target The camera reads occur in 7 7 second intervals The No of Images value dictates how many times the DAC will loop through the read sequence and produce an individual FITS file A simple way to optimize the number of reads 1s to first acquire an exposure of minimum duration two rea
131. using customized LabVIEW software These servers communicate with the SDSU detector controller which in turn organizes the reading of the infrared array through the timing and clock boards When an exposure is complete the data files are stored in a raw data format and the de multiplexing http server converts these into FITS files 2 2 5 3 Tutorial for Controlling the Camera The following is a single HTML page written by Stewart McLay sam roe ac uk to provide a simple tutorial on how to interface with the P1640 camera controller software system The camera controller software system has two HTTP server processes that run continously listening for commands on HTTP ports These processes are called camera and filesave The camera server process is the main thread of control that handles commands for downloading and running applications on the SDSU camera controller timing board The filesave server process handles the data acquisition from the SDSU camera controller and storing the data to disk camera p 7063 filesave p 7063 Initialise camera and filesave server Reset hardware 1 Reset PCI card software reset command to camera server HTTP command http 195 194 120 66 7063 exec RST 2 Reset Timing board hardware reset command to camera sever HTTP command http 195 194 120 66 7063 exec RCO Load telescope configuration 3 Configure camera server telescope settings HTTP command http 195 194 120 66 7063 config
132. ver washers are necessary on each of the screws to act as spacers and ensure that the mask does not make contact with the prism BA DC 2X BEVEL DD MAX PW i a T i Yor 04 44 000v 055 L 7 A Sdn a PLANO Le 24 PLANG 4 A lt mE I9 475 B8 0 0 2C n SE DN ALA a dida 1 PERA Cv STOOD wa ots AP T3 NOS 5 MATS Ma NX NHT QUALTTY 4 NE SURFACES 3 AND 32 AE POL OE TECHNOLOGY tee 88 owe wre 2 i 3 a e e JH PRISM A 41360 503 A Figure 66 Design drawings for the prism Project 1640 Design and Operations bey J AS gt 4 Tx e O m A YU QJ gt Y an P J Fi n 65 ws MONT AND REAP ES over Hw we d Figure 67 Machine drawings for the prism assembly Ojanos JH PRM ASSEMBLY B 41360 001 XA Project 1640 Design and Operations A S o 1L 110 115 581 DM Ps e 40 TE 8 tures HNMY NSYH SIA Figure 68 The mask for the prism This is mounted directly onto the prism assembly face Project 1640 Design and Operations 7l 2 2 3 4 Camera Optics The camera portion of the spectrograph consists of a meniscus corrector lens spherical mirror and a field flattening lens field lens in front of the detector Two fold mirrors accommodate the packaging of the instrument and a spherical mirror brings the beam to a focus on the detector Reflective Optics The sphere has a radius of curvature of 888
133. wavelength if any um 1 250 Pivotweight 1 000E 0003 Min allowed 25mm internal transmission at 400nm 0 980 Min allowed 25mm internal transmission at 1535nm 0 980 Min allowed 25mm internal transmission at 2325nm 0 980 The following are for one of the two ADC prism assemblies alpha theta th Z y 0 000000 0 0000 0 0000 100 0000 100 0000 0 000000 0 4762 1 4954 5 9738 6 0000 0 000000 0 3566 27 9622 6 0267 6 0000 0 049653 0 0025 1 1966 111 9997 112 0000 0 012144 0 0000 0 0000 0 017031 Raytrace prescription including chief ray surface thickness mm and glass type with index at 1 250 um and coord break tilt angles deg l 0 0 1 49539 2 0 0 BaP2 1 467190 3 25 9738 1 01916 4 0 0 27 48597 5 0 0 CaF2 1 427460 0 0267 20 319881 7 0 0 0 83997 0 0 9 111 9997 1 19907 11 PUPIL Project 1640 Design and Operations Mechanical prescription including glass type wedge angle of glass deg and thickness of glass along mechanical axis mm l BaF2 26 46681 6 0000 2 CaF2 29 15878 6 0000 3 Distance to pupil mm 112 0000 The following are for the complete ADC both prism assemblies Pupil decenter at 1 250 um mm 0 034 ADC deviation at 1 250 um arcsec on sky 0 015 Telescope pointing offset wrt vacuum arcsec on sky 55 790 Average pupil decenter mm 0 000 Merit function arcsec on sky 0 027 Wavelength Angular Displacement Pupil um in arcsec on the sky decenter Air ADC
134. xception of the lenslet array are oriented square with the optics baseplate The lenslet array is rotated 18 43 The prism is oriented to disperse the light parallel to the workplate This places the detector square with the mounting plate as well requiring only a rotation on the lenslet array Wavelength filtering 1s achieved with J and H band filter 1 05 1 75 um with OD3 OD4 blocking outside this range placed directly in front of the detector ROAD 4 a T a A mo i ATTAT DS Eo e TL DAVID KING INSTITUTE OF ASTRONOMY MADINGL EY un te ce aL al ha e d e u uN ht ac o ti u j a C ul z e un ca D u z C 2 e e 4 u 4 a H i be Project 1640 Design and Operations Figure 54 Optical Layout of the P1640 IFU Project 1640 Design and Operations mov 63 Ez Figure 55 Optical layout of the P1640 coronagraph in the dewar 20 Project 1640 Design and Operations 2 2 3 1 Microlens Array The square lenslet array manufactured by MEMS Optical Boston consists of two powered faces etched into a Imm thick wafer of fused silica The first face placed in the focal plane at the output of our coronagraph has lenslets with a radius of curvature of 950 um and is primarily used to separate the light from each segment of the image so that the higher powered exit surface retains as much of the light as possible with
135. y of the detector the bias dark current contribution to the detector signal and the angular scale and orientation of the camera 3 6 5 Core Exposures Either before or after acquiring occulted data of every target star the observer should record a sequence of unocculted core images Core images are useful for photometric Project 1640 Design and Operations 201 calibration Before initiating the core exposure sequence be sure that the star 1s well placed in the field of view For the best quality core images the star s image should be centered away from both the focal plane mask and the edge of the detector preferably centered on one of the quadrants so that a large area of the point spread function can be recorded Keep in mind that despite the appearance of the raw focal plane data the measurable extent of a bright star s diffraction pattern easily extends beyond a quarter of the detector diameter 3 6 5 1 Moon If the Moon 1s visible during the observing run the user should set aside time to acquire a sequence of exposures for future flat helding purposes The coordinates of the Moon can be determined from the JPL Horizons website http ssd jpl nasa gov horizons cgi The MOON option in the Image Type switch was designed to annotate this data In addition call up Moon from the target catalog to be sure the exposures are named correctly So that the beam entering the coronagraph is approximately unifo

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