Project Lyman

McCandliss, Stephan R.; Kruk, J. W.; Blair, William P.; Kaiser, M. E.; Feldman, P. D.; Meurer, G. R.; Dixon, W. V.; Sahnow, David J.; Neufeld, David A.; Lupu, Roxana; Fleming, Brian; Smee, Stephen A.; Andersson, B. G.; Moseley, S. H.; Kutyrev, A.; Li, Mary J.; Sonneborn, G.; Siegmund, Oswald H. W.; Vallerga, J. V.; Welsh, Barry Y.; Stiavelli, M.; Windhorst, Rogier A.; Shapley, Alice E.

doi:10.1117/12.789574

Cited by 8 publications

(9 citation statements)

References 60 publications

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“…The green dashes in the figure mark flux levels in units of a fraction of a FEFU ≡ 10 −15 ergs cm −2 s −1Å−1 . Overplotted in blue is our estimate of the background limit for FORTIS, 31 which is dominated by the contributions from geocoronal Lyα and Lyβ. We see that far-UV telescope with a 0.5 m aperture is perfectly capable of measuring escape fractions down to the levels expected for LyC escape from galaxies in the early universe.…”

Section: Science Enabledmentioning

confidence: 99%

“…It is designed to meet the challenges of far-UV imaging spectroscopy below Lyα where the targets are weak and mirrors that can reach the Lyman limit have a reflectivity of ∼ 30 -40%. The expected instrument performance and design rational have been detailed previously 1,31 and Table 2 summarizes the optical parameters. Here we provide an overview of the four major subsystems: optics, detector, microshutter assembly, and targeting system.…”

Section: Technical: Fortis Instrument Description and Fabrication Promentioning

confidence: 99%

“…24,30 Efforts to search for LyC escape are thus UV and optical problems. 31 undertook a study to quantify the requirements for detecting f esc at optical and UV wavelengths based on the galaxy luminosity functions (LF) in the literature. 32 They show that at z = 0.1 there are ∼ 100 galaxies deg −2 mag −1 with characteristic apparent magnitude at 1500Å, m * f uv = 20.…”

Section: Science Enabledmentioning

confidence: 99%

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Fabrication of FORTIS

McCandliss

Fleming

Kaiser

et al. 2010

Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray

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The Johns Hopkins University sounding rocket group is building the Far-ultraviolet Off Rowland-circle Telescope for Imaging and Spectroscopy (FORTIS), which is a Gregorian telescope with rulings on the secondary mirror. FORTIS will be launched on a sounding rocket from White Sand Missile Range to study the relationship between Lyman alpha escape and the local gas-to-dust ratio in star forming galaxies with non-zero redshifts. It is designed to acquire images of a 30 x 30 field and provide fully redundant "on-the-fly" spectral acquisition of 43 separate targets in the field with a bandpass of 900 -1800 Angstroms. FORTIS is an enabling scientific and technical activity for future cutting edge far-and nearuv survey missions seeking to: search for Lyman continuum radiation leaking from star forming galaxies, determine the epoch of He II reionization and characterize baryon acoustic oscillations using the Lyman forest. In addition to the high efficiency "two bounce" dual-order spectro-telescope design, FORTIS incorporates a number of innovative technologies including: an image dissecting microshutter array developed by GSFC; a large area (∼ 45 mm x 170 mm) microchannel plate detector with central imaging and "outrigger" spectral channels provided by Sensor Sciences; and an autonomous targeting microprocessor incorporating commercially available field programable gate arrays. We discuss progress to date in developing our pathfinder instrument.

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Section: Science Enabledmentioning

confidence: 99%

Section: Technical: Fortis Instrument Description and Fabrication Promentioning

confidence: 99%

Section: Science Enabledmentioning

confidence: 99%

See 1 more Smart Citation

Fabrication of FORTIS

McCandliss

Fleming

Kaiser

et al. 2010

Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray

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“…This is challenging, as evidenced by the left panel of Figure 1 from McCandliss et al [36], which shows estimated sensitivity requirements for detecting LyC leak in L * uv galaxies down to f e ≥ 0.01 as a function of redshift 0.02 < z 3, computed from rest frame UV LFs [37]. To reach f e ≈ 0.01 will require apertures well in excess of 2 m. Observations beyond z > 1.3 will be especially challenging, because of zodiacal light.…”

Section: Lyc Detection Requirements and Open Questionsmentioning

confidence: 99%

Essential Observations of the Lyman Continuum

McCandliss¹,

Steenberg²,

Sonneborn³

et al. 2009

AIP Conference Proceedings

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Abstract. Concurrent observations of Lyman continuum (LyC) and Lyman α (Lyα) emission escaping from star-forming systems at low redshift are essential to understanding the physics of reionization at high redshift (z 6). Some have suggested reionization is dominated by numerous small galaxies with LyC escape fractions f e ∼ 10%, while others suggest mini-quasars with higher f e might also play a role. At z > 3, direct observation of LyC leakage becomes progressively more improbable due to the increase of intervening Ly limit systems, leaving Lyα as the primary diagnostic available to the James Webb Space Telescope for exploring the epoch of reionization. If a quantitative relationship between escaping LyC and Lyα emission can be established at low z, then the diagnostic power of Lyα as a LyC proxy at high z can be fully realized. Past efforts to detect f e near z ≈ 3 have been fruitful but observations at low redshift have been less so. We discuss the sensitivity requirements for detecting LyC leak in the far-and near-UV as a function of redshift 0.02 < z 3 and f e ≥ 0.01 as estimated from UV luminosity functions. UV observations are essential to understanding of the physics of LyC escape and the ultimate goal of identifying the source(s) responsible for reionization.

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“…An understanding of the mechanisms that govern Lyα escape, and ultimately how it relates to LyC escape, is critical to the understanding of measurements from the first galaxies at the epoch of reionization by the James Webb Space Telescope (JWST). 2 A detailed description of the instrument design and early fabrication results was presented at the SPIE 2011 Optics and Photonics conference. 3 The first flight of the instrument occurred at 11:00pm on May 10, 2013 from the White Sands Missile Range (WSMR) in New Mexico.…”

Section: Introductionmentioning

confidence: 99%

Calibration and flight qualification of FORTIS

et al. 2013

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The Johns Hopkins University sounding rocket group has completed the assembly and calibration of the Farultraviolet Off Rowland-circle Telescope for Imaging and Spectroscopy (FORTIS); a sounding rocket borne multi-object spectro-telescope designed to provide spectral coverage of up to 43 separate targets in the 900 -1800 Angstrom bandpass over a 30 × 30 field-of-view. FORTIS is capable of selecting the far-UV brightest regions of the target area by utilizing an autonomous targeting system. Medium resolution (R ∼ 400) spectra are recorded in redundant dual-order spectroscopic channels with ∼40 cm 2 of effective area at 1216Å. The maiden launch of FORTIS occurred on May 10, 2013 out of the White Sands Missile Range, targeting the extended spiral galaxy M61 and nearby companion NGC 4301. We report on the final flight calibrations of the instrument, as well as the flight results.

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Project Lyman

Cited by 8 publications

References 60 publications

Fabrication of FORTIS

Fabrication of FORTIS

Essential Observations of the Lyman Continuum

Calibration and flight qualification of FORTIS

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