adsabs/AstroCLIMB huggingface dataset:
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: Early commissioning flexure measurements. The blue points are the measured entrance flexures and the black points are the measured spectrograph flexures. Each measurement is the magnitude of the drift calculated by summing the flexure along the spectral direction and the flexure along the cross-spectral direction in quadrature. The shaded regions represent the expected drift due to flexure over a range of exposure times, spanning from 300 s (the dotted line) to 600 s (the solid line). These are calculated using the commissioning flexure goals outlined in the text.
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: Zemax ray traces showing the optical performance of the spectrograph (telescope and relay not included). The top panels show the unconvolved PSF (without the microlens array) in each of the three wavelength configurations. The bottom panels are the convolved pupil images (with the microlens array) for each lenslet pitch at a central wavelength of 658 nm.
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: We have designed custom mounts for the entrance optics, grating, and camera optics. Many of these optics are retained using spring-loaded or clamped mounting systems, so that they can be removed from their mounts without having to break any epoxy bonds. Here, we show an overview of the custom mount designs in SolidWorks. The zoomed-in regions present exploded views of the retention mechanisms.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: The coverage in the COSMOS-XS survey of the luminosity–redshift plane. The gray solid lines depict the redshift and luminosity bins used in the LF analysis. The red line indicates the detection limit of 5σ, where σ = 0.53 μ Jy beam−1 at 3 GHz, and a fixed spectral index of α = −0.7 is assumed. Sources that fall below the detection limit exist within a region with a low local r.m.s. or have a shallower spectral index.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Local radio LF of SF galaxies from several surveys with different observed areas and sensitivities. Our modified-Schechter function fit to the combined data is shown with the solid line. The dashed line indicates the depth of the COSMOS-XS survey at 0.1 < z < 0.4.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: G182.5 and surrounding area for the GALFACTS Stokes I (main image), DRAO-ST Stokes I (top left inset), DRAO-ST polarized intensity (bottom left inset), Urumqi polarized intensity data (bottom center inset), and GALFACTS peak polarized intensity data (bottom-right inset). The black square in the main image indicates the region shown in the inset images. Prominent features in the surrounding area are labeled.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Density maps as a function of redshift in the COSMOS-XS field of view constructed by Scoville et al. (2013) with the Voronoi technique. The images were made by summing the derived densities measured from the individual redshift slices. The colorbar corresponds to the density unit per Mpc2 divided by the median density over the whole COSMOS field. The redshift range is given in each panel, and the COSMOS-XS area is shown with the dashed circle.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: Planck 545 GHz dust image showing a portion of the Orion-Eridanus superbubble. The approximate edge of the bubble is shown by the shaded white band (based on Ochsendorf et al. 2015 and Tahani et al. 2022). The white contours near the top right are the DRAO Stokes I data showing the position and orientation of the G182.5–4.0 filaments.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Corner plots showing the two-dimensional posterior probability distributions of α L and α D for the density+luminosity evolution fitted to the COSMOS-XS + VLA-COSMOS 3 GHz samples. The marginalized distributions for each parameter is shown independently in the histograms. For all redshift bins, the parameters have well-defined peaks.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: The late-time spectra of SN 2019muj, as compared to other SNe Iax (Jha et al. 2006; Sahu et al. 2008; Stritzinger et al. 2014; Yamanaka et al. 2015; Kawabata et al. 2018), on day ∼+120 days (top), ∼+250 days (middle), and ∼+400 days (bottom) since the maximum light. At a given phase, the spectra of different objects are shown roughly following an order of decreasing peak luminosity from top (bright) to bottom (faint). For spectra at ∼+120 and ∼+400 days, the corresponding spectra of SN 2019muj with an arbitrary flux scale are overplotted with each SN spectrum for comparison (gray). Note that the apparent H α  feature seen in a few SNe, especially strong in SN 2010ae, is likely a background host galaxy contamination. The spectra for comparison SNe are obtained from WISeREP (https://www.wiserep.org) (Yaron & Gal-Yam 2012).
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: Line profiles of [Ca II]λλ7292, 7324 and the Ca II NIR triplet, on day 131 and day 480 (black). The convolution of Gaussian profiles is shown (red). The Gaussian FWHM is taken to be the same for the λ7292 and 7324 components at a given epoch; 900 km s−1 (day 131) and 760 km s−1 (day 480), after being corrected for the instrumental spectral resolution. The same is the case for the 8498, 8542, and 8662 components of the Ca II NIR triplet; 1300 km s−1 on day 131 and 760 km s−1 on day 480.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: The same as Figure 2 but expanded around 7300 Å. The rest wavelengths of [Fe II]λ7155, [Ca II]λλ7292, 7324 and [Ni II]λ7378 are shown by the vertical gray lines. The spectra of SN 2019muj are overplotted by gray lines to the spectra of SN 2014dt (+125 and +412 days) and SN 2005hk (+377 days), with an additional blueshift by 300 km s−1.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: Line widths (FWHM) of [Ca II]λ7324, [Fe II]λ7155, the 8542 component of Ca II NIR, and the flux ratio of [Ca II]λ7324/[Fe II]λ7155 (from left to right) for late-time spectra of the SN Iax sample shown in Figures 2 and 3 at ∼+120 days (red; squares), +250 days (blue; triangles), and +400 days (black; circles). The dependence is shown as a function of the V-band peak magnitude, which is taken from the compilation by Kawabata et al. (2021).
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: The V and R-band images of SN Iax 2019muj at 131 and 480 days after the explosion.
Paper: Modeling the Extragalactic Background Light and the Cosmic Star Formation History
Authors: Justin D. Finke, Marco Ajello, Alberto Domínguez, Abhishek Desai, Dieter H. Hartmann, Vaidehi S. Paliya, Alberto Saldana-Lopez
Figure caption: Left: 68% confidence interval (orange contour) on the stellar mass density as a function of z from Model A, along with data (black circles) from Madau & Dickinson (2014). Right: 68% confidence interval (orange contour) on the gas-phase metallicity as a function of z from Model A, along with the fit from (Madau & Fragos 2017, blue curve). Mean metallicity measurements from damped Lyα systems corrected for dust depletion (Péroux & Howk 2020) are shown as black circles.
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption: A schematic overview of the procedure we follow to generate artificial images of stellar systems fully populated with individual stars. In (a), we sample stellar masses from an IMF (weights indicated by the color bar) and interpolate the associated stellar fluxes from an isochrone of the indicated age and metallicity. In (b), we assign spatial positions to each star using random draws from a two-dimensional Plummer distribution. In (c), the stars are injected into an image array, which is then convolved with the PSF. Finally, noise from the sources, sky, and detector are added to the image. In (d), we show a grI-composite image of an ArtPop simulation of a metal-poor globular cluster at 5 kpc. In this example, the mock observations used the filter set, PSFs, and pixel scale of HST ACS/WFC. </>
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption:  ArtPop simulations of an old dwarf spheroidal of stellar mass 3 × 106  M ⊙, placed at a distance of 5 Mpc. The galaxy is composed of an SSP of age 12.6 Gyr and metallicity [Fe/H] = −1.8. We show gri-composite images of mock observations of varying image resolution (FWHM values indicated at the top of each column) and exposure times (indicated on the left of each row). The image resolutions were chosen to be similar to HST/ACS (left column), HSC (middle column), and SDSS (right column). All images assume a mirror diameter of 8 m and sky brightnesses of 22, 21, and 20 mag arcsec−2 in g, r, and i, respectively. In each panel, the green line indicates the scale of 20″.</>
Paper: Modeling the Extragalactic Background Light and the Cosmic Star Formation History
Authors: Justin D. Finke, Marco Ajello, Alberto Domínguez, Abhishek Desai, Dieter H. Hartmann, Vaidehi S. Paliya, Alberto Saldana-Lopez
Figure caption: 68% contour FUV dust extinction, A(z), as a function of redshift for Model A (orange shaded region) and Model E (violet shaded region). Observational data are shown as black circles.
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption:  ArtPop calculations of the time evolution of SSPs. The top row shows the V- and I-band mass-to-light ratios (left) and integrated V − I color (right). The bottom row shows the V- and I-band absolute SBF magnitudes (left) and ﹩\overline{V}-\overline{I}﹩ SBF color (right). The SSPs were generated using the Kroupa (2001) IMF. Solar metallicity SSPs are shown as dashed lines, and metal-poor SSPs with [Fe/H] = −1.5 are shown as solid lines.</>
Paper: Modeling the Extragalactic Background Light and the Cosmic Star Formation History
Authors: Justin D. Finke, Marco Ajello, Alberto Domínguez, Abhishek Desai, Dieter H. Hartmann, Vaidehi S. Paliya, Alberto Saldana-Lopez
Figure caption: 68% contours for the contribution to the local (z = 0) EBL that originates at redshift < z for various wavelengths from Model A, as shown in the legends. The symbols represent the resolved contribution from galaxies, which are essentially lower limits on the contribution to the local EBL. Square symbols are from BLAST (Marsden et al. 2009) and circle symbols are from Herschel-SPIRE (Béthermin et al. 2012).
Paper: Modeling the Extragalactic Background Light and the Cosmic Star Formation History
Authors: Justin D. Finke, Marco Ajello, Alberto Domínguez, Abhishek Desai, Dieter H. Hartmann, Vaidehi S. Paliya, Alberto Saldana-Lopez
Figure caption: 68% contour of the dust escape fraction, f esc,d  (λ, z) for Model A.
Paper: Modeling the Extragalactic Background Light and the Cosmic Star Formation History
Authors: Justin D. Finke, Marco Ajello, Alberto Domínguez, Abhishek Desai, Dieter H. Hartmann, Vaidehi S. Paliya, Alberto Saldana-Lopez
Figure caption: Same as Figure 3 but the shaded regions are the 68% confidence intervals are for model B, the fit to γ-ray data only.
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption: Simulated gri-composite images of dwarf galaxies of stellar mass 106 M ⊙ at a distance of 5 Mpc. The galaxies are SSPs with [Fe/H] = −1.5, assuming the MIST model isochrones. Each row shows a single galaxy of fixed age, which is indicated on the left. For each galaxy, the leftmost panel shows the full SSP, and the remaining five panels show stars that are on the MS, RGB, CHeB stars, and the early and thermally pulsating asymptotic branches (E-AGB and TP-AGB, respectively). The simulations were tuned to resemble an LSST-like observatory and observing conditions with exposure times of 90 minutes in i and 45 minutes in g and r. Each panel is 2 kpc on a side. As noted in the main text, the phases are defined according to the MIST primary equivalent evolutionary phases.</>
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption:  ArtPop model of an ultrafaint dwarf galaxy with a stellar mass of M ⋆ = 5 × 105 M ⊙, placed at a distance of 1 Mpc. The left panel shows the gri-composite color image and the middle panel shows the same model injected into a Dark Energy Survey image. In the right panel we show the gr color–magnitude diagram, where stars are color coded according to their stellar phase. The dashed horizontal line marks the g-band limiting magnitude reported by DES DR1 of ﹩{m}_{g,\mathrm{lim}}=24.33\,\mathrm{mag}﹩. Ignoring star–galaxy separation issues, stars that are brighter than this limit should, in theory, be detected in the image.</>
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption: Visual comparison of artificial dwarf galaxies generated using stellar fluxes from the MIST (left panel) and PARSEC (right panel) isochrones. The isochrones were generated consistently using the Flexible Stellar Population Synthesis software package. Other than the choice of isochrone, the model parameters are identical, including the individual stellar positions and masses. The images are HST ACS/WFC grI composites, with the integrated g 475 − I 814 galaxy color indicated below each image. The middle panel shows the color–magnitude diagram of the constituent MIST (red) and PARSEC (blue) stars. The galaxies are SSPs composed of 5 × 106 stars with the population parameters indicated in the middle panel.</>
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption: DECam g − i color distribution of 1000 realizations of an ArtPop dwarf galaxy with fixed model parameters. The galaxy is composed of an ancient, metal-poor SSP with an age of 12.6 Gyr and metallicity of [Fe/H] = −2. Given its low stellar mass of 105 M ⊙, stochasticity in the numbers of luminous evolved stars leads to a wide range of integrated and visual properties. The gri-composite images on the top show the bluest (left), median (middle), and reddest (right) dwarf galaxy in the sample. A DECam-like observatory and observing conditions were assumed, with ∼ 1″ seeing and 2 hr (1 hr) exposures in i (g and r). The galaxy is placed at a distance of 2.5 Mpc, and the images are 800 pc on a side.</>
Paper: ArtPop: A Stellar Population and Image Simulation Python Package
Authors: Johnny P. Greco, Shany Danieli
Figure caption: Simulated HST ACS/WFC grI-composite images of uniformly distributed SSPs with ﹩\mathrm{log}(\mathrm{age})=10\,\mathrm{Gyr}﹩ and [Fe/H] = −1.6. The mean I-band surface brightness of each column is indicated at the top, and the distance to the populations in each row is indicated on the left. The surface brightness increases from left to right, and the distance increases from bottom to top. Each panel shows a distinct realization of an SSP with the indicated parameters The images are 35″ ×  25″, with a pixel scale of 0.05″  pixel−1.</>
Paper: Relation of Observable Stellar Parameters to Mass-loss Rate of AGB Stars in the LMC
Authors: Henry A. Prager, Lee Anne Willson, Massimo Marengo, Michelle J. Creech-Eakman
Figure caption: The fit of ﹩\dot{M}﹩ to the K − [8.0] color, using the function ﹩{\rm{log}}\dot{M}=A/((K-[8.0])+B)+C-D(J-K)﹩ is shown. In the case of the oxygen-rich, fundamental-mode pulsators M0 (a), oxygen-rich, first-overtone pulsators M1 (b), and carbon-rich, fundamental-mode pulsators C0 (c), a second color (J − K) was used, and is accounted for by including this dependence on the y-axis with ﹩\mathrm{log}\dot{M}﹩ with the appropriate fitting exponent. For the carbon-rich, extreme, fundamental pulsators C0x (d) (see Figure 2 for details), and carbon-rich, first-overtone pulsators C1 (e), only a single color was used and thus only ﹩\mathrm{log}\dot{M}﹩ is found on the y-axis. The values of these fits and their accuracy can be found in Table 8.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: Completeness tests, recovered artificial point sources. Top left: NGC 3368; top right: NGC 4395; bottom left: NGC 4736; bottom right: NGC 4826. Colors indicate points from artificial images that were actually used in the fits, to ensure the samples of all regions were statistically equivalent.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: Completeness tests. Top left: NGC 3368; top right: NGC 4395; bottom left: NGC 4736; and bottom right: NGC 4826. Fits (solid lines) to recovered fractions (dots) vs. K  s  mag with Equation (2). Colors (red, blue, green, gold) refer to the centermost ellipse, and inner, middle, and external annuli, respectively. Blue dotted lines indicate the 90% and 50% completeness values.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: (u* – ﹩i^{\prime} ﹩) vs. (﹩i^{\prime} ﹩ – K  s ) colors and structural parameters of sources in and closely around the selection region of NGC 3368. Top: FWHM; bottom: 100 × SPREAD_MODEL. Left column: all sources; right column: final sample. The gray contour outlines the GCC selection region. GCCs appear in shades of blue and cyan in both compactness estimators.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: Morphology variations across the ﹩u* i^{\prime} {K}_{s}﹩ diagram. Top: NGC 3368; second row: NGC 4395; third row: NGC 4736; bottom: NGC 4826. Indicators of shape in the ﹩i^{\prime} ﹩ band are coded as shown by the color bars: FWHM (left) and 100 × SPREAD_MODEL (right).
Paper: Relation of Observable Stellar Parameters to Mass-loss Rate of AGB Stars in the LMC
Authors: Henry A. Prager, Lee Anne Willson, Massimo Marengo, Michelle J. Creech-Eakman
Figure caption: The derived distribution of the masses of the oxygen- and carbon-rich stars in our sample, showing that the parameter determining C/O composition is primarily the mass. Mass loss reducing M and shell flashes modulating L introduce scatter in M and may be responsible for most of the overlap in the distributions.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: (u* – ﹩i^{\prime} ﹩) vs. (﹩i^{\prime} ﹩ – K  s ) colors and structural parameters of sources in and closely around the selection region of NGC 4395. Top: FWHM; bottom: 100 × SPREAD_MODEL. Left column: all sources; right column: final sample. Symbols as in Figure 5.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: CFHT ﹩i^{\prime} ﹩-band images, asinh scale. Top left: NGC 3368; top right: NGC 4395; bottom left: NGC 4736; bottom right: NGC 4826.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: BCES fits to spiral galaxies. Top: log M • vs. log N GC; bottom: log N GC vs. log M •. Left: no additional scatter; center: additional ϵ  y ; right: ϵ  y  and ϵ  x . Lines and symbols as in Figure 15.