1 ASTE Report and Plans for 2018/2019 Seiichi Sakamoto (ASTE Manager) on behalf of ASTE Team
2 What is ASTE? ASTE Atacama Submillimeter Telescope Experiment • ↓ 10-m submm telescope located at • Pampla La Bola within Chajnantor area Specifications of telescope: • – Surface accuracy: 19 um → 50 um? – Pointing accuracy: 2” rms – Scientific Observing Time: ~1000h/yr ALMA Infrastructure: • – Gensets ×2 + fuel tanks (15 kL)×2 – Satellite Network (1 Mbps) – Weather Station, web cameras, etc. The prime objectives of ASTE operations: • – Strengthen EA ALMA proposals – Promote science with submm single dish – Promote astronomical instrumentation
3 Definition of Science Requirements 1. Galactic star formation Understand and quantify the physical environments associated with star-formation processes, from large-scale molecular filaments (~10 pc = 1.5° at Orion) down to small-scale cores (~0.1 pc = 50" at Orion) including their kinematics ( ΔV = 0.03 km/s over 60 km/s), through wide-field observations and deep (σ ~ 0.1 Msun for a 10σ detection) integration of nearby star forming regions in CO J=3-2, J=4-3, their isotopes, and the [CI] lines, as well as key carbon-chain molecules which are the proxy for the chemical evolution. 2. Molecular evolution in galaxies Probe the evolution of molecular clouds by mapping the distribution (~1 kpc = 21" at 10 Mpc) and kinematics ( ΔV < 0.5 km/s over 1000 km/s) of the key total mass and dense gas tracers such as CO J=3-2, J=4-3 and [CI] in nearby (D < 10 Mpc) galaxies, including the Magellanic Clouds. 3. Distribution and star-formation history of obscured galaxies in the early universe Probe the large scale distribution and the history of obscured massive star formation in the universe by observing the bright (S 850 > 10 mJy) submillimeter galaxies at z = 3-7 in the [CII] line and the underlying continuum and deriving their precise redshifts ( Δz = 0.01 at z = 4), at a rate of one galaxy per night. 4. Demonstration science in submillimeter wavelength and platform for ALMA2 development Use ASTE as a telescope to obtain pilot Band 9/10 data for future ALMA proposals (including ACA standalone) that request high resolution/sensitivity follow-up. ASTE shall be used for the platform for ALMA2 development.
4 ASTE Organization Structure ASTE Manager as of 2018 December Seiichi Sakamoto* A-Project application for FY2019: ASTE Deputy Manager 6.25 FTEs (incl 2 PD) Takeshi Kamazaki* + 1 FTE (EPO, safety, log, admin) Maintenance and Development Group Science Operation Group Lead: Shinichiro Asayama* Lead: Daisuke Iono* Telescope Operation Science Operation - Toshihiko Kobiki (Lead) - Natsuko Izumi - Yasuhiro Fujimoto* - Andrea Silva - Tetsuya Ito* - Tomofumi Umemoto* - Masumi Yamada* Computing RX Development - Yasunori Fujii* (Lead) - Kyoko Ashitagawa* - Takayuki Matsui* - Motoko Inata* - Tetsuya Ito
5 Current/Recent Issues • Az (+El) Drive Problem ⁻ During DESHIMA commissioning session, ASTE Az drive got stuck/locked on 2017 Nov 26 during DESHIMA commissioning campaign. ⁻ There is an issue on Az mechanism. Similar problem was found also for El mechanism. Spare parts are in preparation. ⁻ Because of this problem, we decided not to operate the telescope this year and focus on corrective maintenance. • Review as A (small size)-Project • Fuel Leakage from Genset After stopping 4 months, fuel overflow (several × 100 L) from ⁻ the service tank of a genset was detected on 2018 Nov 23. ⁻ Contaminated soil was removed. ⁻ Leaky valves were replaced.
6 ASTE Science Operation - Status Available time 2012 2013 2014 2015 2016 2017 2018 2019a Total time 360 630 2020 2152 900 800 0 959 [hours] 2500 2000 1500 1000 500 0 2012 2013 2014 2015 2016 2017 2018 2019
7 ASTE Science Operation - Status Available time 2012 2013 2014 2015 2016 2017 2018 2019a Total time 360 630 2020 2152 900 800 0 959 [hours] Available time for 2019a Call for proposals for 2019a Carryover from 2017 348 hours No. of Accepted proposals Carryover from 2018 216 hours Under EA: 203 hours East Asia 9 (228 h) 2019a evaluation CL: 96 hours (10%) Chile 2 Contingency 96 hours (10%) Total 959 hours
8 ASTE-related Publication Trends in the number of publications. • Publication of CATS345 is the highest. Publication of AzTEC sporadic. • The number of Band 8QM data is still not enough. → Demo science data released in 2017 November (Izumi's talk)
9 [CI] mapping of RCW38 Sample images of integrated intensity map (made by archived CASA fits data, 3 pixel gaussian smoothing)
10 Current Instrumentation Receivers Freq HPBW Receiver Type N pix N pol [GHz] [arcsec] DASH345 Heterodyne 324-372 22 1 2 Band 8 Heterodyne 385-500 17 1 2 Spectrometer BW Δf Spectrometer Type [MHz] [kHz] 4096 2000 1.7 over 3500 km/s FX 2048 1000 0.86 over 1755 km/s WHSF 3-bit 1024 500 0.43 over 878 km/s 2048 ch 64 31.25 0.027 over 55 km/s F-FX 32 15.625 0.013 over 27 km/s
11 ASTE Receiver Development 60 • DASH345 (345 GHz receiver) P0S1_old FEM60 P1S1_old FEM60 P0S1_new FEM37 P1S1_new FEM60 SIS bias current with LO [uA] 50 • Corrective maintenance 40 • Replacement of SIS mixer 30 • Replacement of cold IF cable 20 • Replacement of cold LNA 10 • Upgrade 0 320 330 340 350 360 370 380 • Pol 1 LO power could not satisfy LO freq. [GHz] all frequency range due to over-sized waveguide. • Design new fundamental waveguide and improvement of LO input power • ASTE Band 10 • PI: S. Asayama. JSPS Kiban (A) 18H03725 • Defined as ASTE project mission • Receiver is in preparation by using proto-type Band 10 receiver.
12 12 Plan for CY2018-2019 2018 • Nov-Dec: Site maintenance – Fuel leakage... 2019 • Jan-Mar: Antenna maintenance • Mar-May: New 345 / Band 8 / WHSF high- res commissioning • Jun-Sep: Common-use (ASTE 2019a) • Oct-: Installation of ASTE Band 10
13 Future Upgrades? Instrument Institute Status ASTE Band 10 RX NAOJ Initiative based on Kakenhi. To be installed in FY2019. Band 7/8 (multi-)RX KASI Needs JSAC approval for installation. 230 GHz RX UEC Initiative based on Kakenhi Needs JSAC approval for installation. ASTECAM NAOJ Original TES cam did not pass gate (2-color TES review after CSV. MKID camera under → 6-color MKID) development based on Kakenhi. →A -Pol Chinese Will be reviewed after installation of (polarimeter) U. HK ASTECAM. DESHIMA U. Leiden Test observations done in 2017. → DESHIMA2.0 U. Leiden Needs JSAC approval for installation. →MOSAIC U. Leiden Future plan GPU Spectrometer KASI Needs JSAC approval for installation.
14 Points of Discussion • Re-definition of ASTE's role in ALMA era (+ACA standalone mode) • Upgrades with PI instruments • Collaboration with universities • Large programs • Sinergy with NRO 45m • Other issues?
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