adsabs/AstroCLIMB huggingface dataset:
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: O-C values phased with a frequency of 1.288 c days−1.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: O-C diagram for ATLAS 4 from 229 times of maximum light.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Period–luminosity relations from Poro et al. (2021). Lines represent period–luminosity relations for fundamental pulators (blue), first overtone (green), second overtone (red), and third overtone (purple).
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: O–C diagram for ATLAS 59 from 979 times of maximum light.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Phased data for ATLAS 75 from BYU, ATLAS, ASAS-SN, and TESS using optimal periods found by Period04 for each survey.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: O–C diagram for ATLAS 75 from 13 times of maximum light.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Phased data for ATLAS 63 from BYU, ATLAS, ASAS-SN, and TESS.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: O–C diagram for ATLAS 63 from 20 times of maximum light.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Phased data for ATLAS 59 from BYU, ATLAS, ASAS-SN, and TESS.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption: Li abundance patterns among MSTO stars. As before, red and blue symbols show stars with detected Li or upper limits. Black symbols show the CMD location for stars with no successful synthesis measurement of Li. Numbers to the right of the CMD in the left panel show the stellar masses in solar units at the corresponding magnitude levels, based on isochrones of Figure 4.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption: Li abundance patterns among the giants. The location of WOCS4009 is shown with a cyan dot. Blue triangles indicate upper limits to A(Li) while red squares illustrate detections.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption: Estimates for [Fe/H] for individual RG/SG stars as a function of T eff. Error bars show the MAD statistic.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption: Abundance estimates for individual Fe lines. Results are shown for RG/SG members only. Error bars show MAD statistics
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: The average radial surface density profile (gray points with error bars) fit with a smoothly broken two-component power law (the dashed blue line). The hatched region on the left marks the limits from the FPM as in other figures, and the dotted–dashed light purple curve represents the radial profile determined by scattered-light modeling. The values derived from this average surface density profile for r  c , α in, and α out are substantially different from those determined via scattered-light modeling, perhaps due to a difference in the SPF or bias due to the low SNR detection of the backscattering portion of the disk; alternatively, these differences may simply be an artifact of the different modeling approaches.
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: (Left) Measured brightness curves along the radial direction of HD 156623's deprojected disk for various angles. The region covered by the FPM is blocked out (hatched in light purple, labeled FPM), and it is clear that in most cases, the inner hole is unresolved, with the exception of possibly PA 45°–90° and PA 90°–235°. Each profile is arbitrarily offset for clarity, and the dashed lines correspond to zero for each profile depicted. (Right) Surface density (brightness corrected by a factor of 1/r 2) profiles along the radial direction of HD 156623's deprojected disk for various angles. The region covered by the FPM is blocked out (hatched in light purple, labeled FPM). Each profile is arbitrarily offset for clarity, and the dashed lines correspond to zero for each profile depicted.
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: PSF-subtracted total-intensity GPI H-band image of HD 156623 using five KL modes (top) and polarized intensity GPI H-band image of HD 156623 smoothed with a 2 pixel wide Gaussian kernel for visualization (bottom). The debris disk is only detected in polarized light, with a signal-to-noise ratio of ∼2–3 per resolution element. The point sources visible in the total intensity image were determined to be unbound background stars in Esposito et al. (2020).
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: Corner plot of posteriors from MCFOST modeling of scattered-light imaging.
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption:  MCFOST maximum-likelihood scattered-light model of HD 156623 with data and residuals for Stokes ﹩{{ \mathcal Q }}_{\phi }﹩, ﹩{{ \mathcal U }}_{\phi }﹩, ﹩{ \mathcal Q }﹩, and ﹩{ \mathcal U }﹩, drawn from only the last 600 iterations (i.e., excluding burn-in).
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: Diagram with the scattering angle across the disk of HD 156623, assuming the geometric parameters defined in Section 4. The most forward scattering occurs in the southwest, and the most backscattering occurs in the northeast.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: PSF subtraction results for the Vega system. Left: the scattered-light image of Vega using α Cyg as a PSF template presented in millijanskys per square arcsecond. Right: the signal-to-noise ratio (S/N) of the scattered-light disk detection using the uncertainty map described in Section 4 and presented in the Appendix. Both images are presented north up, east left. While the signal interior to 10.″5 (cross-hatched region) is indistinguishable from PSF residuals due to a color mismatch, the signal from 10.″5 to 27″ has an S/N > 1 per pixel and is consistent with a face-on disk. The scattered-light surface brightness drops off quickly between 27″ (red dashed line) and 30″ (yellow dashed line).
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Radial profiles of the Vega PSF-subtracted image (Figure 2) are presented. For comparison, we also present the radial profile from the ζ Aql − α Cyg subtraction (gray) to test the impacts of the color-dependent PSF. Uncertainties are generated using the radial profile of the respective uncertainty maps. The Vega reductions are binned to an 8 pixel radius, while the noisier ζ Aql − α Cyg reduction uses 12 pixel bins. The y-axis is shown on a logarithmic scale. The profile shapes differ significantly inside of ∼8″, and the data in this region are untrustworthy. Outside of this region, the Vega − α Cyg subtraction shows a halo of disk material extending out to at least ∼27″ (210 au). The difference in the S/N achieved for α Cyg and ζ Aql is evident in the uncertainties.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Comparison of the wavelength-dependent radial profiles for the Vega (top) and Fomalhaut (bottom) debris disks. The radial profiles for Vega are provided for HST/STIS (this work), JWST/MIRI (K. Su et al. 2024, in preparation), Herschel/PACS (Su et al. 2013), and ALMA (using the Gaussian model from Matrà et al. 2020). Radial profiles for Fomalhaut are adapted from HST/STIS (Gáspár et al. 2020), JWST/MIRI (Gáspár et al. 2023), Herschel/PACS (Su et al. 2013), and ALMA (MacGregor et al. 2017).
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Spectral comparison between Vega and the two PSF calibration sources: α Cyg and ζ Aql. The spectra have been convolved with the STIS 50CCD transmission function available through the pysynphot package (i.e., the unfiltered sensitivity or detector quantum efficiency). While all targets are close spectral types, the fainter ζ Aql is a much better color match to Vega than α Cyg. The spectra are based on the BOSZ theoretical library (Bohlin et al. 2017) and the extinction law from Gordon et al. (2021), plus the measured stellar parameters, e.g., T eff, log(g), and A  V .
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: The computed stellar positions for each frame of the 25 Vega orbits and six reference orbits obtained in this program. The center positions have been color-coded based on the orbit (see Table 1) and have corresponding orbit labels. Within an orbit the center positions are very stable and remain stable over the full 11 months of observations.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Here we compare radial profiles of the scattered light observed with HST/STIS and the thermal emission observed with JWST/MIRI to a simple dust model. The data are shown with solid lines and the models with dashed lines. The model includes a dust population comprised of water ice with a size distribution from 0.2 to 5 μm, a power-law slope of −3.65, a radial dust density distribution ∝r −1, and a radius from 10″ to 30″. The model is able to reproduce the observed scattered-light surface-brightness levels without overproducing the flux observed in thermal emission.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Wavelength ranges of the infrared spectrum of each of the four initial WISE bands. While W3 and W4 have the broadest ranges, they require onboard cryogen, which depleted in mid-2013.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Confusion matrices produced by a trained VARnet Classifier.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: How WISE surveys the sky, based on figures seen in E. L. Wright et al. (2010).
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: The anomaly extraction pipeline.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Example light curves of the four classes. Note that y scales differ so that the shapes are more apparent.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Example point cloud of a source: HD 165459.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: The Complete VARnet Model.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Light-curve sampling with MSX LMC 1689.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Random Dirac impulses, convolved with a Gaussian filter, produce a smooth but potentially highly unique waveform.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: The relationship between full-cone performance to collimated FRD performance was established by measuring a fiber with artificially varying FRD performance on both a collimated FRD setup (panel (a)) and a full-cone FRD setup (panel (b)). Since the focal plane is designed so that the fiber is aligned to the chief ray to within 0.°4 (or 26′) and we require that losses due to FRD do not exceed 90%, we determine that the full fiber system must perform with an FWHM ≤2.°3 for f/in = 3.9 in the collimated FRD test. Panel (a) shows the Collimated FRD test data for a fiber with varying amounts of FRD performance. Panel (b) shows the full-cone test data for this same fiber with FRD artificially induced. Panel (c) shows the result of combining the results in these panels to establish an FRD requirement for various injection angle offsets. The different lines show the allowable FRD performance for different injection angle offsets. For DESI, we allow for a 20′ offset at the focal plane, so the final spliced fiber system must have an FWHM ≤1.°5 at f/3.9 input.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Panel (a) shows the route of the fiber cables around the decl. axis. The cables route around this axis in the e-chain, and to test the load that this would place on the telescope bearing, we loaded 10 short lengths of cable into a section of the e-chain and measured the force required to roll and unroll the bundle. Panel (b) shows the lab setup. A force gauge was attached to the top tray and the force as the cable was rolled and unrolled was measured. The tests were performed at speeds much faster than the slew rate of the telescope. The results are shown in panel (c) and the results reassured us that the movement of the telescope would not be impeded with this routing design.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Drawing for the positioner fiber assembly. A ∼3.1 m length of optical fiber is cleaved and bonded into a glass ferrule with a UV-curing epoxy (Dymax 431). A polyimide tube is used to provide strain relief and is bonded to the back of the ferrule with a viscous UV-curing epoxy (Loctite 3751) to protect the fiber as it routes through the positioner. The strain relief is shown with an OD of 0.4 mm and fits within a pocket at the back of the ferrule. A hytrel sleeve is added to the fiber to further protect it at the back of the focal plane but is not bonded so that the fiber is free to rotate inside of it.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: The splicing process has four distinct steps. First, the polyimide buffer is removed from the fiber to expose the glass. Then each fiber is cleaved to obtain a high-quality optical surface. Next, the two prepared fibers are aligned, heated, and pushed together to form a splice. Finally, the fiber is recoated with acrylate to protect the splice. Panel (a) shows the “ring of fire” stripper removing polyimide buffer from the fiber. Panel (b) shows images of the fiber during the splicing process.