entrepreneurial space astrophysics enabled by new

Nurturing the space-

adept in a sounding

rocket crucible

Entrepreneurial

space astrophysics

enabled by new

technologies

Stephan R. McCandliss - JHU

06/10/2019 Space@Hopkins: Small Mission

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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

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°

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

UV-Vis PI Program Review 2017 54

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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entrepreneurial space astrophysics enabled by new

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