APEX - The Atacama Pathfinder Experiment Telescope & Instrument development plan Rolf Güsten for the APEX Consortium R.Güsten
APEX re-investments plan Pending approval of the extended operation of the project (2018-22), the Consortium prepares for necessary re-investments to secure APEX’ position as leading submm facility: Re-investments into • Sequitor & Chajnantor general infrastructure • telescope upgrades – critical spares/replacements to secure basic performance for extended lifetime – wobbler/secondary/hexapod (with enhanced performance) • suite of new instruments to remain at the forefront of innovation Ringberg APEX 2016 R.Güsten
Telescope enhancements The ensemble of [ hexapod, wobbler, secondary mirror ] is the most likely single-point failure of aging telescope hardware, failure will result in long downtimes (6-12 months) We suggest timely preventive replacements to ensure continued smooth operation of the facility beyond 2017: – hexapod: replace against ALMA production line unit (fully compatible with new APEX control hard-/software, spares at site) – buy in on advanced design for new wobbler, or refurbish existing unit as necessary (trade-off between engineering and schedule risks) – integrate with light-weighted Alu vs. higher precision CF subreflector (partly dependent on decision about wobbler) The new ensemble shall offer enhanced performance (requirement) wobbler throw: +/-150" on sky (as is), but with >90% duty cycle o the surface accuracy of the antenna could improve by 2-3 µm rms o Timeline is important: goal must be an installation during the early 2018 shutdown R.Güsten
Incoherent detectors at APEX Bolometer Arrays at APEX (as of 2015) in operation number of FoV NEFD instrument λ c [µm] Instrument notes [mJy √ s] pixels [arcmin] status since until LABOCA * 870 295 11.4 100 05/07 facility 210 pixels as of 2014 SABOCA 350 37 1.5 750 05/09 facility effectively de-commissioned ASZCa 2000 280 22 50 12/05 08/10 PI (MPIfR) UC Berkeley with MPIfR P-ArTeMiS b 450 256 1.6×1.6 2000 03/07 07/09 PI (ESO) ESO with CEA/Saclay Incoherent Arrays for APEX in development 865 3520 50 06/16 A-MKID 15×15 PI (MPIfR) MPIfR with SRON 353 21600 160 /17 450 2048 4.4×2.4 400 ArTeMiS 350 2048 4.4×2.4 700 07/13 a PI (ESO) ESO with Saclay 200 1024 1.0×0.9 1000 R.Güsten
Coherent detectors at APEX Development goals – cover all atmospheric windows accessible from Chajnantor with state-of-the-art receivers – for all bands: dual-polarization (co-aligned on sky) and 2SB if possible – if technologically feasible: 4-12 GHz IF response – dual-color operating bands: (7 & 9), 8 &10 – wideband IF-processors and digital back-ends (handling 64-112 GHz of signal) R.Güsten
Coherent detectors at APEX Heterodyne and Grating Spectrometers at APEX (as of 2015) RF range IF band in operation instrument T Rx [K] a Instrument mixer notes [GHz] [GHz] status since until Z-Spec (h) R: 2-400 d -- c 185 – 305 09/10 12/12 PI (ESO) grating spectrometer SEPIA-B5 158 – 211 4 – 8 ~40 2SB 02/15 PI(OSO/ESO) dual-polarization 85 − 160 4 – 8 f APEX-1 213 – 268 SSB 02/08 facility(OSO) 45 − 55 195 g – 270 PI230 4 – 12 2SB 12/15 PI (MPIfR) VLBI, dual pol. 85 − 190 APEX-2 267 – 378 4 – 8 f SSB 02/08 facility(OSO) APEX-2a 279 – 381 4 – 8 120 – 160 DSB 07/05 12/07 facility(OSO) de-commissioned 4 – 8 (k) 64 pixel het array (k) SuperCam 344 – 346 105 DSB 11/14 05/15 PI(OSO/ESO) 95 − 120 APEX-3 386 – 504 4 – 8 DSB 10/12 facility(OSO) SEPIA-B9 610 – 720 4 – 8 70 – 130 tbc DSB 2016 PI(OSO/ESO) ESO/OSO with SRON 420 – 500 2 – 4 110 – 180 DSB 12/11 FLASH 05/04 PI (MPIfR) dual-color 780 – 880 4 – 8 400 – 500 DSB 12/09 268 – 375 2 × 4 – 8 80 – 100 2SB 04/10 FLASH + PI (MPIfR) dual-color 385 – 510 2 × 4 – 8 100 – 160 2SB 06/12 (D)SB b 620 – 720 7 × 4 – 8 175 – 250 dual-color array CHAMP + 04/07 PI (MPIfR) 2 × 7 pix hexag. (D)SB b 780 – 950 7 × 4 – 8 500 – 600 990 – 1050 4 – 8 400 – 550 DSB 1.05 THz Rx 02/09 ../13 PI (MPIfR) under repair 460 2 – 4 130 DSB APEX-T2 1250-1385 2 – 4 1000-1600 DSB facility(OSO) de-commissioned CONDOR (i) 1250-1530 1.1 – 1.8 3200 DSB 10/05 11/05 PI (MPIfR) KOSMA Spectroscopy Receivers for APEX in development LAsMA 268 – 375 7 × 2 × 4 – 8+ 80 – 100 2SB 10/16 PI (MPIfR) 7 pixel het array SEPIA-B9 610 – 720 4 – 12 2SB 2017 PI(OSO/ESO) ESO/OSO with SRON R ∼ 1000 d ZEUS-2 490 …1500 -- c PI (MPIfR) Cornell with MPIfR R.Güsten
Timeline for instrument upgrades (subject to approval of funding requests/ resources) Nasmyth Cabin A Nasmyth Cabin B SHeFI SEPIA FLASH+ CHAMP+ PI230 Q1/2016 7x 660 – 7x 850 230/2 230 – 345 – 460 180/2 – open – 660/2 345/1 – 460/1 SHeFI SEPIA FLASH+ LAsMA PI230 Q4/2016 230 – 345 – 460 180/2 – open – 660/2 345/1 – 460/1 7x 345/1 230/2 LFA/HFA device upgrade CHAMP+ 7x 660 – 7x 850 decommission 345/1 no HFA devices SEPIA FLASH+ CHAMP+ LAsMA PI230 Q1/2018 180/2 – 345/2 – 660/2 850/2 – 460/2 2x 7x 660 7x 345/1 230/2 SHeFI decommissioned Note: temporary installations at visitor port are not considered (Zeus-2, MPIfR THz Rx) color coding DSB (4-8) DSB (4-12) SSB (4-8) 2SB (4-12) 2SB (4-8) PI instrument facility instrument
IF processing /back-ends The new heterodyne receivers come with enhanced IF processing bandwidth Front-end (examples) Mode of Operation Pix × BW [GHz] BW T PI230 (or SEPIA-B9) dual pol 2SB 2x2x 4-12 32 FLASH++(460 & 850) dual color, dual pol, 2SB 2x2x2x 4-12 64 LAsMA single pol 2SB 2x7x 4-8 56 CHAMP+ (upgraded) dual color DSB 2x7x 4-12 112 which does require a novel (integrated) approach on signal processing based on high- bandwidth FFT boards (4 GHz min) Delivery by early 2018 (in time for the new/upgraded front-ends) will be challenging. R.Güsten
The APEX Mission Philosophy This brief outlook on upcoming instrument/telescope enhancements carries forward into the 2018-22 extension the APEX mission philosophy: • operate a superb telescope at its design limits - safely, efficiently • provide the APEX communities with the best possible detectors • continuously upgraded with latest technological innovations • while exploring new technological frontiers Within very few years our balanced mix of facility and Pl instruments, supported by strong home-based/guest instrument teams, has put APEX on the front line of submm astronomy. To all expectations, our ambitious re-investment program will maintain APEX in its globally unrivaled position for years to come. R.Güsten
Recommend
More recommend
