The ESBO DS project Towards a balloon-based observatory. Duffard.pdf · Instituto de Astrofísica de Andalucía Max Planck Gesellschaft (MPG), Institute for extraterrestrial Physics

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


European Stratospheric Balloon Observatory

Content 1.  Balloon-based telescopes 2.  The ESBO DS Project 3.  Planetary Science Applications


Balloon-based telescopes



THISBE, 1969 STO-2, 2016

PILOT, 2015

BLAST, 2006



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

]



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


Motivation

•  Some technical challenges…

Sunrise (2009) PoGOLite (2011)

Sunrise (2013) PoGOLite (2013)


Motivation

Ground Balloons Space

?


Motivation

Ground Balloons Space

European Stratospheric Balloon Observatory



ESBO


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


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:


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


ESBO DS Approach

0.5 m UV/vis telescope

5 m FIR telescope

Operating structure / concept /…

Prototype Feasibility/First Design

Draft/Roadmap


ESBO DS Approach

UV/visible Prototype (0.5 m)


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


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


UV/vis Prototype (0.5 m)

•  Expected Performance V-band sensitivity at SNR = 5

Angular resolution (diffraction limit)


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


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


Potential Timeframe


•  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

Documents

The ESBO DS project Towards a balloon-based observatory. Duffard.pdf · Instituto de Astrofísica de Andalucía Max Planck Gesellschaft (MPG), Institute for extraterrestrial Physics