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H2020 project ESBO DS Ph. Maier 13.11.2017
The ESBO DS projectTowards a balloon-based observatoryRené Duffard & José Luis OrtizInstituto de Astrofísica de Andalucía - CSIC
P. Maier1, J. Wolf1, T. Keilig1, A. Krabbe1, R. Duffard4, J. L. Ortiz4, S. Klinkner1, M. Lengowski1, T. Müller5, C. Lockowandt2, C. Krockstedt2, N. Kappelmann3, B. Stelzer3, K. Werner3, S. Geier3,6, C. Kalkuhl3, T. Rauch3, T. Schanz3, J. Barnstedt3, L. Conti3, L. Hanke3, D. Angerhausen71Institute of Space Systems, University of Stu[gart, Germany, 2Swedish Space Corporation, Sweden, 3Institut für Astronomie und Astrophysik, Universität Tübingen, Germany, 4Instituto de Astrofísica de Andalucía (CSIC), Spain, 5Max-Planck-Institut für extraterrestrische Physik, Germany, 6Institut für Physik und Astronomie, Universität Potsdam, Germany, 7Center for Space and Habitability, Universität Bern, Swiaerland
H2020 project ESBO DS Ph. Maier 13.11.2017
European Stratospheric Balloon Observatory
Content 1. Balloon-based telescopes 2. The ESBO DS Project 3. Planetary Science Applications
H2020 project ESBO DS Ph. Maier 13.11.2017
Balloon-based telescopes
H2020 project ESBO DS Ph. Maier 13.11.2017
Balloon-based telescopes
THISBE, 1969 STO-2, 2016
PILOT, 2015
BLAST, 2006
H2020 project ESBO DS Ph. Maier 13.11.2017
Balloon-based telescopes
Typical flight parameters • Gondola mass:
o 500 – 2000 kg • Flight altitude:
o 30 to 40 km • Flight duration:
o 10 hours - ~ 40 days
• Launch sites: o Continental U.S. (short duration) o Kiruna, Sweden (mid- & long duration) o Antarctica (long duration)
Mid-duration flight (20-40 h)
Long-duration flights (5 days / 55 days)
Exemplary altitude profile (SUNRISE)
35
30
20
10
0
Alit
utde
[km
]
H2020 project ESBO DS Ph. Maier 13.11.2017
Balloon-based telescopes
Why balloons? Observation conditions „between ground & space“, particularly: • Access to additional spectral regions
o UV o Near- and Mid-IR o Far-IR
• Practically no seeing o Enables diffraction limited spatial resolution
• Drastically reduced scintillation noise o Enables high photometric accuracy
• Practical implications: o Exchange of instruments o Update & repair of instruments o Refill of cryogens
UV atmospheric transmission
FIR atmospheric transmission
Scintillation noise
H2020 project ESBO DS Ph. Maier 13.11.2017
Motivation
• Some technical challenges…
Sunrise (2009) PoGOLite (2011)
Sunrise (2013) PoGOLite (2013)
H2020 project ESBO DS Ph. Maier 13.11.2017
Motivation
Ground Balloons Space
?
H2020 project ESBO DS Ph. Maier 13.11.2017
Motivation
Ground Balloons Space
European Stratospheric Balloon Observatory
H2020 project ESBO DS Ph. Maier 13.11.2017
H2020 project ESBO DS Ph. Maier 13.11.2017
ESBO
H2020 project ESBO DS Ph. Maier 13.11.2017
The ESBO DS Project
European Stratospheric Balloon Observatory Design Study
European Stratospheric Balloon Observatory Design Study:
Design study under H2020 call INFRADEV-01-2017 (RIA)
Duration: 36 months (Mar 2018- Mar 2021)
Total budget: 3.009.575 EUR
Follow-on to the H2020 Project ORISON
Conceptualisation of a European research infrastructure
2-tier approach:
A) development and construction of a prototype UV/vis flight system
B) conceptual design of a FIR balloon observatory, including supportive infrastructure
IAA-CSIC
H2020 project ESBO DS Ph. Maier 13.11.2017
ESBO DS Partners
Swedish Space Corporation (SSC)
Universität Stuttgart (USTUTT), Institute of Space Systems
Universität Tübingen (EKUT), Institute for Astronomy and Astrophysics
Consejo Superior de Investigaciones Científicas (CSIC), Instituto de Astrofísica de Andalucía
Max Planck Gesellschaft (MPG), Institute for extraterrestrial Physics
3 ORISON consortium partners:
2 new partners:
H2020 project ESBO DS Ph. Maier 13.11.2017
ESBO DS Approach European Stratospheric Balloon Observatory
o Regular flights with payload recovery and reflight o Proposal-based time allocation
UV-NIR 0.5 m telescope o High-accuracy pointing
(goal: 1 arcsec) o Suitable for UV
FIR 5 m telescope o less confusion noise than Herschel o Goal: 40 flight days per mission o Launch from Antarctica
Mid
term
Vis-NIR 1.5 m telescope o High photometric stability o Suitable for planetary science,
exoplanets
0.5 m telescope
1.5 m telescope
5 m telescope
Ground SystemsProp
osal
Too
ls
Dat
a Pi
pelin
es
ESBO Infrastructure Governance Structure
H2020 project ESBO DS Ph. Maier 13.11.2017
ESBO DS Approach
0.5 m UV/vis telescope
5 m FIR telescope
Operating structure / concept /…
Prototype Feasibility/First Design
Draft/Roadmap
H2020 project ESBO DS Ph. Maier 13.11.2017
ESBO DS Approach
UV/visible Prototype (0.5 m)
H2020 project ESBO DS Ph. Maier 13.11.2017
Goal - UV/vis (0.5 m)
Flight-ready Prototype
Telescope/Platform
• 0.5 m UV-NIR Telescope • 400-500 kg Gondola • Coarse telescope stabilization in
azimuth & elevation • Exchangeable instruments • Space for add-on instruments
Instruments
• Highly sensitive imaging UV-camera (Uni Tübingen)
• Andor-camera for the visible range
• Image stabilization within the optical path (goal: ~ 1 arcsec)
(1) - GPS Antenna (2) - Antenna boom (3) - Receiver (4) - Pivot (5) - Satellite antenna (6) - Elevation torque motor (8) - Gyro sensor
(9) - Star tracker (10) - Batteries (11) – Crush pad (13) - Add-on instrument (15) - Telescope (17) – Reaction wheel
H2020 project ESBO DS Ph. Maier 13.11.2017
Main Telescope Parameters
Scientific Application / Main Instrument
Instrument Custom MCP*
Main application UV Photometry
Main wavelength range 180 – 330 nm
Sensor size 40 mm ∅
Pixel size 20 µm x 20 µm
Preferred FOV Ca. 32 arcmin ∅
Secondary Instrument
Instrument Andor iXon
Main application Image stabilisation
Wavelength range Ca. 330 – 1000 nm
Sensor size 13.3 mm x 13.3 mm
Pixel size 13 µm x 13 µm
Current Telescope configuration
Configuration Cassegrain
Aperture 500 mm
Focal ratio f/8
UV MCP detector Andor iXon 888
*MCP = Micro Channel Plate
H2020 project ESBO DS Ph. Maier 13.11.2017
UV/vis Prototype (0.5 m)
• Expected Performance V-band sensitivity at SNR = 5
Angular resolution (diffraction limit)
H2020 project ESBO DS Ph. Maier 13.11.2017
Goal – FIR (5 m)
Extended interest in balloon-based FIR observations
o Current FIR state-of-the-art: SOFIA, 2.5 m mirror
o Several existing balloons (BLAST, PILOT, STO, up to 2.5 m mirrors)
o Next step: increase on confusion limit of Herschel (3.5 m, requires 5 m+ mirror dimension)
o 5x2.5 m elliptical would have similar area as Herschel mirror
o Uncooled telescope temperature: ca. 200 K, might be possible down to 180 K (vs. 230 K on SOFIA)
o Instruments, Sensitivity & spectral resolution TBD
0.001
0.01
0.1
1
10
100
1 10 100 1000An
gularresolution[arcsec]
Wavelength[µm]
ESBOangularresolution
E-ELT
ESBO5m
JWST
ISO
SPICA
Spitzer HerschelSOFIA
ALMA
H2020 project ESBO DS Ph. Maier 13.11.2017
Goal – FIR (5 m)
Potential scientific observations
ISM/Star Formation: o High spatial resolution line surveys (e.g.
CII, NII, OI, HD) o 100 µm continuum survey @ 5 arcsec
resolution (SOFIA: 10 as, Herschel: 7 as)
Planetary Science / Solar System o Atmospheric gas abundances & vertical
distribution o E.g. H2O, O2, HCl (Mars, Venus, satellites,
small bodies, comae)
(900 s exposure time, 4σ, ca. 44 kHz, i.e. 0.003 to 0.01 km/s resolution)
1.E-17
1.E-16
1.E-15
1.E-14
1.E-13
1.E-12
0 50 100 150 200 250
Min
. det
ecta
ble
line
flux
[W/m
^2]
Wavelength [µm]
Potential Sensitivities
SOFIA 1km/s ESBO 1km/s
SOFIA 100km/s ESBO 100km/s
H2020 project ESBO DS Ph. Maier 13.11.2017
Potential Timeframe
H2020 project ESBO DS Ph. Maier 13.11.2017
• Summary • Prototype (0.5m telescope) flying in 2020 • Recovery of the telescope and instruments
o Exchange of instruments o Update & repair of instruments o Refill of cryogens
• Five meter telescope planned for the near future