entrepreneurial space astrophysics enabled by new
TRANSCRIPT
Nurturing the space-
adept in a sounding
rocket crucible
Entrepreneurial
space astrophysics
enabled by new
technologies
Stephan R. McCandliss - JHU
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Why Sounding Rockets?• Unique Science
– Can only be done from space!
– Precursor science (400 seconds)
– Space only bandpasses
• Xray, UV, IR
• Enabling Technology
– First Fight Tests
• Geiger Counters, Cyrogenic Telescope, MCP, X-ray CCD, Holographic gratings, Rowland Circle Spectrographs, SiC Mirrors, Reflective Dielectric Multilayers, InSb Hybrid Detectors, X-ray Quantum Calorimeters, Far-UV sensitive delta-doped CCDs…
• Training Next Generation of Space Leadership
– Missions in Microcosm - Crucible of Experience - Space Guild
• New Science Thrust
• Synthesis of Mission Concept
• Development of Requirements
• Preparation of Instrument for Space
• Lessons Captured from Success and Failure
• Targets of Opportunity3
Atmospheric Attenuation
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X-ray BackgroundNobel for Giacconi – 40 years later
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Nobel citation:
“For pioneering
contributions to
astrophysics, which
have led to the
discovery of cosmic
X-ray sources.”
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Saw galactic center (Harwit private communication)
Pathfinder for:
ISO,
SWAS,
Spitzer,
Hershel,
JWST
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Fastie: Before 3C273 we were just
astronomers, afterwards we were
“ASTROPHYSICISTS”
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Reported in NYTimes
Enabling Technologies
Examples of significant new technology developed and proven on sounding rockets that has enabled major NASA
missions.
Technology NASA Sounding Rocket NASA Mission UV Geiger Counter 1955 - NRL - Kupperian - NRL25 OAO - 2, Copernicus (OAO-3), TD-1, ANS
X-ray Geiger Counter 1962 - ASE - Giacconi - AB3.352 HEAO-1
Collimated X-ray Proportional Counter 1963 - NRL - Bowyer - NB3.130 Uhuru (SAS-1), SAS-3, OAO-8
Chopped IR Cyrogenic Telescope 1965 - Cornell - Harwit - NF3.162R IRAS, Spitzer
Objective Grating Far-UV Spectrograph - Film 1965 - Prin - Morton - 4.133UG IMAPS
InSb, InAs, Au:Ge IR photodiodes 1965 - Cornell - Harwit - NF3.162R NICMOS on HST, Spitzer
X-Ray Modulation Collimator 1966 - ASE/MIT - Giacconi/Oda - 4.148CG Uhuru (SAS-1), SAS-3, OAO-8
Multi-anode X-ray detectors 1967 - UWI - Code/Bless/ Kraushaar - 4.172 HEAO-I
Pulse Shape Discriminator 1967 - ASE - Giacconi/Gursky - 4.228CG Uhuru (SAS-1), SAS-3, OAO-8
X-ray Polarimeter 1968 - Columbia - Novick - 4.236UG OSO 8
LiF - Al, FUV Electronographic Grating Spectrograph 1970 - NRL Carruthers - 4.328DG Apollo -16 Far-UV Camera/Spectrograph
Grazing incidence mirrors 1972 - ASE - Kellogg - 13.30 CG Skylab, Enistein, BBXRT, EUVE, Chandra
MCP with wire grid anode - HRI 1972 - ASE - Kellogg - 13.30CG Enistein, Chandra
Image Intensified MCP - Film, Folded Concave Grating 1975 - GSFC - Stecher - 26.26GG UIT
Fixed Rowland Circle Spectrograph 1977 - JHU - Fastie - 21.54UG HUT, ORFEUS, FUSE, HST/COS
Multi-Anode Micro-channel Array (MAMA) 1984 - CU - Snow - 27.84UG STIS, ACS and COS on HST
Image Intensified Reticon 1-D 1985 - JHU - Feldman - 4.342UG HUT on Astro-1, -2
X-ray CCD (including cosmic ray veto) 1987 - PSU - Garmire - 36.030UH ACIS/Chandra, SIS/ACSA, XRT/SWIFT
Electron Bombarded CCD 1987 - PU - Jenkins - 27.82UG ORFEUS/IMAPS
Delay Line Readout Systems for UV MCP Detectors 1994 - CU - Green - 36.102UG - HIRES SOHO, FUSE, GALEX, COS on HST
Aberration Corrected Holographic Gratings 1994 - CU - Green - 36.102UG - HIRES FUSE, HST/COS
Reflective dielectric multilayer coatings 1996 - Columbia - Martin - 36.113UG - NUVIEWS GALEX
X-ray Quantum Calorimeter 1996 - UWI - McCammon - 27.140UH Suzaku (Astro-E2), NEXT, Con-X/IXO
InSb 256 x 256 1997 - CIT - Lange - 36.163 UR Spitzer-IRAC
Tomographic Inversion Spectrograph 1998 - BU - Chakrabarti - 36.177UG -- SPINR SPIDER
Off-Rowland Circle Imaging Spectrograph 2004 - CU - Wilkinson –36.197UG - ISIS COS
Off Plane X-ray Grating Array 2006 - CU - CASH - 36.224UH -- CyXESS Con-X/IXO
Lost in Space Star Tracker - ST5000 2007 - UWI - Nordsieck/Percival/Costello –12.059 Sounding Rockets, Balloons, Small Satellites
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The Space Guild Training the Next Generation of Space Experimentalists
• ‘The space workforce is fundamentally a craft-based "guild", where
knowledge is passed from generation to generation. However ... process-
profit focus has profoundly affected the aerospace workforce ... science and
engineering is treated as a commodity ...[which]... has broken ... the
generation-to-generation training thread within the entire aerospace
enterprise.’
– Steve Battel, 2008
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Process
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NASA HQ Science Divisions
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NASA Sounding Rocket Vehicle StableMaintained by NASA Sounding Rocket Operations Contractor – (NROC)
Typical Astrophysics Payload –they all look the same from the outside; standardized support systems
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Celestial Acquisition and Control
System
0.5” pointing stability
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Performance Curves
BBIX is most common vehicle for
astrophysics and solar payloads.
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Acceleration
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Sequence of Events
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Success Criteria - Minimum
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Success Criteria - Comprehensive
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Practice
Mission Milestones
Write Winning
Proposal
Mission Initiation
Conference (MIC)
Requirements Definition
Meeting (RDM)
Preliminary Design
Review (PDR)
Critical Design
Review (CDR)
Pre-Integration
Review (PIR)
Mission Readiness
Review (MRR)
Launch Preparations
45 days
3 weeks
3 weeks
3 weeks
Build Phase
Put it all together
I&T
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? years
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Student Drivers (Beware)
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Rouge Elephant
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Recent Past
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Strongest Ever Carbon Monoxide Emission
Discovered in Coma of Comet Hale-Bopp
•Remaining emissions are bands of the carbon
monoxide Fourth Positive system.
Image of Comet Hale-Bopp, courtesy W. Johnasson.
Comet Hale-Bopp 6 April 1997
JHU-NASA Sounding Rocket 36.156 UG
SO C+ CCS
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Constant Scattering Efficiency in far-UV06/10/2019 Space@Hopkins: Small Mission
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JHU Sounding Rocket Finds Blue DustStephan R. McCandliss, Paul D. Feldman -- JHU and Kevin France, Eric Burgh -- CU
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Evacuated Rowland Circle
Spectrograph β = 0°
Far UV - LIDOS - McCandliss (PI)
Science:•Goals
- Determine the far-UV
scattering and extinction
properties of the dust within
the Orion Nebula. Account for
the total far-UV luminous
output from stars, dust and
gas.
•Mission Objective- Acquire longslit spectra of the
nebula with a holographic
grating, symmetrically feeding
integrating and photon
counting detectors to achieve
high dynamic range.
Technology Development: Workforce Training:
LIDOS Longslit Imaging Dual-
Order Spectrograph
• Top (Bright Target)
– First FUV spectrum of 1 Ori C, primary power source of the Orion Nebula. Acquired with CCD delta-doped by JPL.
• Bottom (Faint Targets)
– Longslit profiles of nebular dust scattered light. Acquired with photon counting MCP.
Flight Data from 36.243 UG, 10 Jan 2008.
Dual Order SpectrographFar-UV Sensitive
Delta Doped CCD
From One Generation to the Next
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David Sahnow - STScI
Mel Martinez - DISC
Kevin France - CUEric Burgh - SOFIAJason McPhate – UC Berkeley
Partick Morrissey - Caltech
Keith Redwine – JHU/APLBrian Fleming - CU
Paul Feldman -JHUStephan McCandliss - JHU Roxana Lupu - SETI
My JHU Rocket Genes
Brian Welch– JHUAnna Carter -
JHU
Russ Pelton – JHU
Current Project
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Next Generation FORTIS*
*Far-UV Off Rowland-circle Telescope for Imaging and Spectroscopy
PI: Stephan McCandliss/JHU
Description and Objectives:• Demonstrate the scientific utility and feasibility of multi-
object spectroscopy over wide angular fields in the far-UV. First Science Investigation:
- Spectroscopy of Blue Stragglers in Globular Cluster M10
- Why do they exist? How do they form?
Key Challenge/Innovation:• Pulsed Actuated Next Gen Microshutter Arrays(NGMSA)• New low scatter baffles to trap geo-Lyman alpha light• Longlife, High QE, Large Area Borosilicate MCP’s• Autonomous Target Acquisitions
Approach:• Collaborate with GSFC on NGMSA requirements and fabrication• Sensor Sciences retrofit detector with new borosilicate MCPs
with CsI photocathode• Develop Wide-Field Lyα Geocoronal Simulator (WFLaGS)• Design light traps suppress Lyα• Involve graduate and undergraduates all phases of mission
Key Collaborators:• Brian Welch, Anna Carter, Paul Feldman, William Blair, Luciana
Bianchi – JHU • Matt Greenhouse, S. Harvey Moseley, Alexander Kutyrev, Mary
Li – GSFC • Gerhardt Meurer – U. Western Australia
Development Period: Scheduled 1st launch Aug 2019 (1 January 2017 to 31 December 2021)
Accomplishments and Next Milestone:• Three flights of FORTIS have proven basic design • Science results on Comet ISON have been published• Baseline in-flight instrument performance established:- Scattered geo-Lyman alpha tall pole identified- Reproduced in-flight scatter signature
•Upcoming milestones inlcude:- Buildup for August Flight at JHU- Integration at WFF June- Begin field operations WSMR July
Application: Enabling Multi-object Spectroscopy for UVOIR future missions (Explorers, Probes, Flagships)
a)
f)
c)a) FORTIS exploded view
b) NGMSA Sizes,
c) Large Area MCP detector 170 x 43 mm2
d) Single Slit Spectrum of D2 Lamp d)
New Tech Readiness TRLin = TRLcurrent = TRLtarget =
Borosilicate MCPs 4 6 7
NGMSA 4 6 7
Low Scatter Baffles 4 6 7
b)
FORTIS
64x128
JWST
172x365
LUVOIR/HabE
x
420x840
(in Dev SAT)
Next Generation Microshutter
Arrays
VAB sandbox movie
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Grating Recovery
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UV-Vis PI Program Review 2017 5327-September-2017
ISON Flight DataPrimarily Cometary Lyα (625 krayleighs peak) in dispersed channels
Primarily Cometary CI λ1657 in imaging channel
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Recently verified by spectra acquired concurrently by Mercury Messenger
27-September-2017
Summary
• Troika of Science, Technology and Training
– SR base of the launch pyramid
– Essential to sustaining the space astrophysics
enterprise
• New delivery systems will provide an
enhanced Low Cost Assess to Space capability
– Avenue to cost effective science
• Standardization is the key
– Will enable routine LCAS in Low Earth Orbit
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