entrepreneurial space astrophysics enabled by new
TRANSCRIPT
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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
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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
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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)
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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
29
? 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
JHU Sounding Rocket Program Highlights
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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°
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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
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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
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VAB sandbox movie
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Grating Recovery
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UV-Vis PI Program Review 2017 5327-September-2017
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ISON Flight DataPrimarily Cometary Lyα (625 krayleighs peak) in dispersed channels
Primarily Cometary CI λ1657 in imaging channel
UV-Vis PI Program Review 2017 54
Recently verified by spectra acquired concurrently by Mercury Messenger
27-September-2017
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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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