Nineteen-port photonic lantern with multimode delivery fiber

Noordegraaf, Danny; Skovgaard, Peter M. W.; Sandberg, Rasmus Kousholt; Maack, Martin D.; Bland-Hawthorn, Joss; Lawrence, Jon; Lægsgaard, Jesper

doi:10.1364/ol.37.000452

Cited by 20 publications

(10 citation statements)

References 14 publications

(13 reference statements)

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“…Thus, the MM to SM conversion throughput will increase if we slow the beam feeding the OH suppression fiber from f /5 to f /7. For a back-to-back system with 1×19 photonic lanterns, the total throughput increases by ≈ 0.5 dB (11%) when slowing the input beam from f /5 to f /7 (Noordegraaf et al 2012). However, doing so will decrease the fiber's FOV.…”

Section: Discussionmentioning

confidence: 99%

“…The GNOSIS OH suppression fibers use two 1×19 photonic lanterns (one for input and one for output) to provide the fibers with the light collecting ability of an MMF. The photonic lanterns were manufactured by NKT Photonics (Noordegraaf et al 2012) and consist of a 50 µm core diameter MM port connected to an array of 19 SMFs by a taper transition with a taper ratio of 11 Note. -Symbols are defined as follows: λ 0 is the notch center, B 0 − B∞ is the notch depth, w is the notch width, n is the profile index, and σ is the standard deviation in each quantity.…”

Section: Photonic Lanternsmentioning

confidence: 99%

“…The solution to this problem is a device called a photonic lantern (Leon-Saval et al 2005Noordegraaf et al 2009Noordegraaf et al , 2012. The device consists of a multi-mode (MM) port connected to an array of SMFs by a taper transition.…”

Section: Introductionmentioning

confidence: 99%

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Gnosis: The First Instrument to Use Fiber Bragg Gratings for Oh Suppression

Trinh

Ellis

Bland-Hawthorn

et al. 2013

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The near-infrared is an important part of the spectrum in astronomy, especially in cosmology because the light from objects in the early universe is redshifted to these wavelengths. However, deep near-infrared observations are extremely difficult to make from ground-based telescopes due to the bright background from the atmosphere. Nearly all of this background comes from the bright and narrow emission lines of atmospheric hydroxyl (OH) molecules. The atmospheric background cannot be easily removed from data because the brightness fluctuates unpredictably on short timescales. The sensitivity of ground-based optical astronomy far exceeds that of near-infrared astronomy because of this long-standing problem. GNOSIS is a prototype astrophotonic instrument that utilizes "OH suppression fibers" consisting of fiber Bragg gratings and photonic lanterns to suppress the 103 brightest atmospheric emission doublets between 1.47 and 1.7 µm. GNOSIS was commissioned at the 3.9 m Anglo-Australian Telescope with the IRIS2 spectrograph to demonstrate the potential of OH suppression fibers, but may be potentially used with any telescope and spectrograph combination. Unlike previous atmospheric suppression techniques GNOSIS suppresses the lines before dispersion and in a manner that depends purely on wavelength. We present the instrument design and report the results of laboratory and on-sky tests from commissioning. While these tests demonstrated high throughput (≈ 60%) and excellent suppression of the skylines by the OH suppression fibers, surprisingly GNOSIS produced no significant reduction in the interline background and the sensitivity of GNOSIS+IRIS2 is about the same as IRIS2. It is unclear whether the lack of reduction in the interline background is due to physical sources or systematic errors as the observations are detector noise dominated. OH suppression fibers could potentially impact ground-based astronomy at the level of adaptive optics or greater. However, until a clear reduction in the interline background and the corresponding increasing in sensitivity is demonstrated optimized OH suppression fibers paired with a fiber-fed spectrograph will at least provide a real benefit at low resolving powers.

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Section: Discussionmentioning

confidence: 99%

Section: Photonic Lanternsmentioning

confidence: 99%

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Gnosis: The First Instrument to Use Fiber Bragg Gratings for Oh Suppression

Trinh

Ellis

Bland-Hawthorn

et al. 2013

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“…1). These early devices underwent further optimization to maximize throughput around the 1.55 µm region for a 7-port [18], 19-port [19] and even a 61-port device [20]. An average throughput of ∼ 97% was achieved across several 19-port devices, which were specifically designed and optimized for an instrument called GNOSIS [21] (described in the following section).…”

Section: A Single Element Photonic Lanternsmentioning

confidence: 99%

Astronomical Applications of Multi-Core Fiber Technology

Jovanović

Harris

Cvetojevic

2020

IEEE J. Select. Topics Quantum Electron.

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Optical fibers have altered astronomical instrument design by allowing for a complex, often large instrument to be mounted in a remote and stable location with respect to the telescope. The fibers also enable the possibility to rearrange the signal from a focal plane to form a psuedo-slit at the entrance to a spectrograph, optimizing the detector usage and enabling the study of hundreds of thousands of stars or galaxies simultaneously. Multi-core fibers in particular offer several favorable properties with respect to traditional fibers: 1) the separation between single-mode cores is greatly reduced and highly regular with respect to free standing fibers, 2) they offer a monolithic package with multi-fiber capabilities and 3) they operate at the diffraction limit. These properties have enabled the realization of single component photonic lanterns, highly simplified fiber Bragg gratings, and advanced fiber mode scramblers. In addition, the precise grid of cores has enabled the design of efficient singlemode fiber integral field units for spectroscopy. In this paper, we provide an overview of the broad range of applications enabled by multi-core fiber technology in astronomy and outline future areas of development.

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“…The proposal harnessed an emerging technology, known as the photonic lantern (PL), to allow efficient conversion of an essentially arbitrary input (e.g. a combination of arbitrarily excited modes) to the consistent and diffraction-limited format of single-mode fibers (SMFs) [2][3][4][5]. The PL remaps the entrance slit of the spectrograph, thus achieving throughput equivalent to a multimode fiber (MMF) design and the spectral resolution of a diffraction-limited slit width.…”

Section: Introductionmentioning

confidence: 99%

Beating the classical limit: A diffraction-limited spectrograph for an arbitrary input beam

Betters¹,

Leon-Saval²,

Robertson³

et al. 2013

Opt. Express

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Abstract:We demonstrate a new approach to classical fiber-fed spectroscopy. Our method is to use a photonic lantern that converts an arbitrary (e.g. incoherent) input beam into N diffraction-limited outputs. For the highest throughput, the number of outputs must be matched to the total number of unpolarized spatial modes on input. This approach has many advantages: (i) after the lantern, the instrument is constructed from 'commercial off the shelf' components; (ii) the instrument is the minimum size and mass configuration at a fixed resolving power and spectral order (~shoebox sized in this case); (iii) the throughput is better than 60% (slit to detector, including detector QE of ~80%); (iv) the scattered light at the detector can be less than 0.1% (total power). Our first implementation operates over 1545-1555 nm (limited by the detector, a 640×512 array with 20µm pitch) with a spectral resolution of 0.055nm (R~30,000) using a 1×7 (1 multi-mode input to 7 single-mode outputs) photonic lantern. This approach is a first step towards a fully integrated, multimode photonic microspectrograph.

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Nineteen-port photonic lantern with multimode delivery fiber

Cited by 20 publications

References 14 publications

Gnosis: The First Instrument to Use Fiber Bragg Gratings for Oh Suppression

Gnosis: The First Instrument to Use Fiber Bragg Gratings for Oh Suppression

Astronomical Applications of Multi-Core Fiber Technology

Beating the classical limit: A diffraction-limited spectrograph for an arbitrary input beam

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