adsabs/AstroCLIMB huggingface dataset:
Paper: JWST's TEMPLATES for Star Formation: The First Resolved Gas-phase Metallicity Maps of Dust-obscured Star-forming Galaxies at z ∼ 4
Authors: Jack E. Birkin, Taylor A. Hutchison, Brian Welch, Justin S. Spilker, Manuel Aravena, Matthew B. Bayliss, Jared Cathey, Scott C. Chapman, Anthony H. Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Gourav Khullar, Keunho J. Kim, Guillaume Mahler, Matthew A. Malkan, Desika Narayanan, Grace M. Olivier, Kedar A. Phadke, Cassie Reuter, Jane R. Rigby, J. D. T. Smith, Manuel Solimano, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiss
Figure caption: Top row: resolved Hα, [N II], and [N II]/Hα maps of SPT0418-47 from JWST/NIRSpec (left to right). The [N II]/Hα map is used as a proxy for metallicity. Bottom row: ALMA rest-frame 380 μm continuum and [C I] line maps, along with the resultant [C I]/380 μm map (left to right). The [C I]/380 μm map is used as a proxy for the gas-to-dust ratio. The gray circles show the approximate PSF of the data in each panel, and the horizontal bars in the top right of each panel indicate the scale of 1″ (∼0.7 kpc at z = 4).
Paper: JWST's TEMPLATES for Star Formation: The First Resolved Gas-phase Metallicity Maps of Dust-obscured Star-forming Galaxies at z ∼ 4
Authors: Jack E. Birkin, Taylor A. Hutchison, Brian Welch, Justin S. Spilker, Manuel Aravena, Matthew B. Bayliss, Jared Cathey, Scott C. Chapman, Anthony H. Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Gourav Khullar, Keunho J. Kim, Guillaume Mahler, Matthew A. Malkan, Desika Narayanan, Grace M. Olivier, Kedar A. Phadke, Cassie Reuter, Jane R. Rigby, J. D. T. Smith, Manuel Solimano, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiss
Figure caption: Zoom-in 1D spectra of SPT0418-47 (top) and SPT2147-50 (bottom). All flux densities are in units of erg cm−2 s−1 μm−1. The left panels show the integrated spectra, and the right panels show a sample typical 3 × 3 binned spaxel, as used in the spatially resolved fitting. The emission lines are well modeled by Gaussians. We note that the integrated spectra are fit here with [S II] as shown in the plot, but for the binned spaxels we only fit Hα and the [N II] doublet, as [S II] is typically too faint to be significantly detected in individual binned spaxels.
Paper: JWST's TEMPLATES for Star Formation: The First Resolved Gas-phase Metallicity Maps of Dust-obscured Star-forming Galaxies at z ∼ 4
Authors: Jack E. Birkin, Taylor A. Hutchison, Brian Welch, Justin S. Spilker, Manuel Aravena, Matthew B. Bayliss, Jared Cathey, Scott C. Chapman, Anthony H. Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Gourav Khullar, Keunho J. Kim, Guillaume Mahler, Matthew A. Malkan, Desika Narayanan, Grace M. Olivier, Kedar A. Phadke, Cassie Reuter, Jane R. Rigby, J. D. T. Smith, Manuel Solimano, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiss
Figure caption: Same maps as presented in Figure 3, but this time for SPT2147-50. This source displays two regions of very intense [N II] emission which clearly match with regions of strong rest-frame 380 μm and [C I] emission. Given that [N II]/Hα > 1 in these regions, we are likely detecting emission from an active galactic nucleus (AGN).
Paper: JWST's TEMPLATES for Star Formation: The First Resolved Gas-phase Metallicity Maps of Dust-obscured Star-forming Galaxies at z ∼ 4
Authors: Jack E. Birkin, Taylor A. Hutchison, Brian Welch, Justin S. Spilker, Manuel Aravena, Matthew B. Bayliss, Jared Cathey, Scott C. Chapman, Anthony H. Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Gourav Khullar, Keunho J. Kim, Guillaume Mahler, Matthew A. Malkan, Desika Narayanan, Grace M. Olivier, Kedar A. Phadke, Cassie Reuter, Jane R. Rigby, J. D. T. Smith, Manuel Solimano, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiss
Figure caption: One-dimensional JWST/NIRSpec rest-frame spectra of SPT0418-47 and SPT2147-50, displaying strong detections of the Hα and [N II] emission lines, in addition to the [S III] doublet. Both spectra are extracted only from spaxels where Hα+[N II] is detected with S/N > 8. SPT2147-50 displays detections of the He I line and Paγ lines, and marginal evidence for Paδ emission. Neither of the sources are detected in [O I].
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: Left panel: Mass–metallicity relation of the AGN-RPS galaxies (edge-colored squares), AGN-FS galaxies (edge-colored circles), SF-RPS galaxies (edge-black squares), and SF-FS galaxies (edge-black circles) with stellar masses ﹩\mathrm{log}({M}_{* }/{M}_{\odot })\geqslant 10.4﹩, where the metallicities are the median values of 12 + log (O/H) within 1 kpc from the galaxy centers. The filled-colored circles are the median metallicity (12 + log (O/H)AGN,1 kpc) of the AGN inside the mass bin (i.e., strips of different colors) with the errors given by the 16th/84th percentile of the distribution. The filled-colored stars are the median metallicities (12 + log (O/H)SF,1 kpc) of the SF galaxies inside the mass bin. Right panel: Difference between (12 + log (O/H)AGN,1kpc) and (12 + log (O/H)SF,1kpc) as a function of stellar mass. Within the same physical region, galaxies hosting AGN are more enriched in metals than those without AGN activity.
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: Residuals of the AGN-RPS (squares) and AGN-FS (circles) metallicity from the SF MZR, as a function of the galaxy stellar mass, color-coded according to L[O III] as in Figure 5. To compute the error bars on Δ (O/H), we consider the errors on the AGN metallicity and the errors on the SF MZR, computed as described in Section 5.3. The horizontal black solid line remarks the level of Δ(O/H) = 0. AGN hosts show Δ(O/H)>0 on average, except for 2/11 galaxies in the AGN-RPS sample that have lower metallicity than SF galaxies.
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: NII- and SII- BPT diagrams with overlaid the H II models (black lines) provided with the code NEBULABAYES. The model’s gas pressure is log P/k (cm−3/K) = 5. The red line is the empirical Kauffmann et al. (2003) relation, while the black lines are the theoretical Kewley et al. (2001) relationships. The distribution of the observed star-forming line ratios (from GASP and MANGA galaxies) is shown by density curves filled with shades of purples, where darker colors indicate higher densities.
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: [N II]-diagrams of the nuclear regions r < 0.5 R e (left panels) and r < 1  kpc (right panels) centered on the SF and AGN host galaxies in the MaNGA sample. The points are color-coded according to the metallicity in the bottom panels, and according to the ionization parameter in the top panels. The red line is the Kauffmann et al. (2003) relation, and the black line is the Kewley et al. (2001) relation.
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: [N II]-diagrams of the nuclear regions r < 0.5 R e (left panels) and r < 1  kpc (right panels) centered on the SF and AGN host galaxies in the GASP sample. The points are color-coded according to the metallicity in the bottom panels, and according to the ionization parameter in the top panels. The red line is the Kauffmann et al. (2003) relation, and the black line is the Kewley et al. (2001) relation.
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: Median metallicity estimated inside the aperture of r ∼ 0.5 R e as a function of the SFR (H ﹩\alpha {)}_{1.5{R}_{{\rm{e}}}}﹩ for the SF galaxies. We divide the galaxies into stellar mass bins of width 0.25 dex. The errors are the 25th and 68th percentile of the metallicity distribution inside each bin of mass. At ﹩\mathrm{log}{M}_{* }/{M}_{\odot }\leqslant 9.5﹩, we observe an anticorrelation between the SFR(H ﹩\alpha {)}_{1.5{R}_{{\rm{e}}}}﹩ and 12 + log (O/H), with higher metallicities corresponding to lower SFR (in agreement with Mannucci et al. 2010).
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: NII-BPT diagram and maps of the galaxy 8993-12705 (part of the AGN-FS, on the left) and JO201 (part of the AGN-RPS, on the right). Top panel: NII-BPT diagram for all the spaxels in the galaxies, where in the case of JO201 we also include the spaxels of the stripped tail. SF spaxels are in red, composite spaxels are in orange, LINER spaxels are in light blue, and Seyfert spaxels are in green. Darker color shades indicate more intense line ratios, and vice versa. The black line is the Kauffmann et al. (2003) relation, and the dotted black line is the Kewley et al. (2001) relation. Middle panel: Galaxy map color-coded according to the NII-BPT classification on which we draw the r ∼ 1 kpc (bright green circle) and r ∼ 0.5R e (yellow circle) apertures. The r ∼ 1  kpc aperture is clearly dominated by AGN-only spaxels, while the r ∼ 0.5R e includes a small fraction of SF and/or composite spaxels. The typical PSF size is shown in the top left corner, with a gray circle. Bottom panels: Galaxy map color-coded to the values of 12 + log (O/H) and ﹩\mathrm{log}(U)﹩. The black contours, overlaid on the maps, divide regions classified as AGN, composite and SF by the NII-BPT. The oxygen abundance 12 + log (O/H) varies between 8.4 and 9.2; the ionization parameter ranges between −4.0 and −1.0.
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: MZR of the AGN-RPS (squares) and AGN-FS (circles) color-coded according to their L[O III]. We show as dashed white symbols those AGN for which we could not estimate L[O III] (see text for details). The 12 + log (O/H) is computed within the mass-scaled aperture (r ∼ 0.5 R e), and L[O III] is computed within the fixed aperture (r ∼ 1 kpc). The error bars are the average values of the 16th and 84th percentiles of the PDF among all the spaxels within 0.5R e. The white and gray histograms (in the top and left insets) show the mass and metallicity distributions of the AGN-FS and the AGN-RPS. The two samples have similar ranges of oxygen abundances and L[O III].
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: H II models (black lines) in the NII-BPT (top panel) and in the SII-BPT diagram (bottom panel). The H II models, generated with CLOUDY, have n H = 100 cm−3, and stellar ages t * = 4 Myr. Density curves, filled with different shades of purple, are drawn to show the distribution of the observed line ratios of the SF spaxels in the MaNGA and GASP samples together. Red lines are the Kauffmann et al. (2003), Kewley et al. (2001) relations defining the SF regions in the NII-BPT and in the SII-BPT respectively. The black line in the NII-BPT is the Kewley et al. (2001) relationship, which distinguishes composite and Seyfert/LINER. The H II grids fold, due to the degeneracy between the metallicity and the ionization parameter, around 12 + log (O/H) = 8.6–8.7.
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: [O III] /[S II] vs. [N II] /[S II] line ratios in the case of ionization from SF (top left), AGN+SF (top right), and AGN (bottom). The gray points are the observed line ratios inside the spaxels of the MaNGA and GASP samples together. The distribution of the observed points is outlined by density curves filled with different shades of purple and shown by the gray histograms in the top and right insets. Darker colors indicate regions where the density of data is higher. The black solid lines are the CLOUDY models. The H II models have stellar ages t * = 4 Myr; composite models have the ionization parameter of the stars ﹩\mathrm{log}{U}_{{\rm{H}}{\rm\small{}}\mathrm{ii}}﹩ fixed to −3.0, and f AGN is 0.2; AGN models have α = −2.0 (see text for details).
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: Histograms of the 12 + log (O/H) values inside all the spaxels classified as SF by the NII-BPT, in the MaNGA sample. The black histogram shows a uniform distribution in metallicity, obtained when using the [O III] and [N II] lines, normalized for [S II]. The blue histogram shows a strong bimodality, with a gap around 12 + log (O/H) ∼ 8.6, and is obtained when normalizing with Hβ the set of lines: Hβ, [N II], [O III], Hα, [S II]. The bimodality is caused by the ﹩\mathrm{log}(U)﹩ - ﹩\mathrm{log}Z﹩ degeneracy of the models observed in the NII-BPT shown in Figure 2 (see Section 4).
Paper: Gas-phase Metallicity of Local Active Galactic Nuclei in the GASP and MaNGA Surveys: The Role of Ram Pressure Stripping
Authors: Giorgia Peluso, Mario Radovich, Alessia Moretti, Matilde Mingozzi, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Marco Gullieuszik
Figure caption: Mass–metallicity relation of the SF (colored points) and AGN (gray points) galaxies, with different symbols for the RPS (squares) and non-RPS (circles) samples. Metallicity is computed as the median value in all the spaxels (AGN, SF and composite) within 0.5 R e. The blue dotted curve is the best fit for the SF galaxies. SF galaxies are color-coded according to their SFR within 1.5 R e, a proxy for the total SFR. Overall, AGN galaxies have higher metallicities than SF galaxies.
Paper: Rotation of a Stealth CME on 2012 October 5 Observed in the Inner Heliosphere
Authors: Sandeep Kumar, Dinesha V. Hegde, Nandita Srivastava, Nikolai V. Pogorelov, Nat Gopalswamy, Seiji Yashiro
Figure caption: Top panel shows the Marubashi fitting of toroidal model (TorusM03) with solar wind parameters in the magnetic cloud (red line) and observed solar wind parameters from ACE plotted with respect to time (YY/MM/DD), i.e., ∣B∣, B  x , B  y , B  z , of IMF and bulk solar wind velocity in kilometers per second from top to bottom respectively (black curve). The bottom panel shows the orientation of the fitted flux rope at L1 for TorusM03. Here, + sign shows the position of the spacecraft crossing the magnetic cloud. We measured the tilt angle counterclockwise from the negative y-axis of the GSE coordinate system.
Paper: Rotation of a Stealth CME on 2012 October 5 Observed in the Inner Heliosphere
Authors: Sandeep Kumar, Dinesha V. Hegde, Nandita Srivastava, Nikolai V. Pogorelov, Nat Gopalswamy, Seiji Yashiro
Figure caption: Top panel shows the angular width of 2012 October 5 CME in STEREO-A plotted with respect to height; here, Hc represents the transition height. Bottom panel shows GCS axis (blue dots) representing current along the axis of CME front projected on the PFSS extrapolated magnetic field at 2.5 R ⊙. The cyan color arrow shows the direction of the toroidal current in the CME derived from the flux rope type in Marubashi et al. (2017), Palmerio et al. (2018), and Martinić et al. (2022). The green arrows show the direction of the force on the CME.
Paper: Rotation of a Stealth CME on 2012 October 5 Observed in the Inner Heliosphere
Authors: Sandeep Kumar, Dinesha V. Hegde, Nandita Srivastava, Nikolai V. Pogorelov, Nat Gopalswamy, Seiji Yashiro
Figure caption: This figure shows the WSA velocity background of the CME at 21 R ⊙ from NASA/CCMC. The black rectangle specifies the inhomogeneous velocity background around the CME top front. The green arrow in the lower panel shows the deflection of the upper front of the CME due to interaction with the slow solar wind in front of it.
Paper: Rotation of a Stealth CME on 2012 October 5 Observed in the Inner Heliosphere
Authors: Sandeep Kumar, Dinesha V. Hegde, Nandita Srivastava, Nikolai V. Pogorelov, Nat Gopalswamy, Seiji Yashiro
Figure caption: Evolution of tilt with respect to time of GCS fitting of the CME of 2012 October 5 in COR2 last frame and in the HI FOV. The error bars are incorporated based on four independent fittings.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Left:  variation of the average stellar ellipticity (top) and size (bottom) as a function of focus. Each orange circle represents a single F160W WFC3-IR NGC 104 frame. Median values for 2 μm wide bins are displayed as black circles. In the range of −5 to +5 μm, we find that the ellipticity and size of the stars vary by 0.004 and 1%, respectively. Right: comparison of the ellipticity (top) and size (bottom) of the observed stars and the TinyTim models (blue and red lines). The blue and red lines are TinyTim models for an O5-type and a K7V-type star, respectively. The TinyTim model is significantly rounder and smaller than the observed stars, suggesting that it is not an accurate representation of the PSF.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Ellipticity correction for stars in the five CANDELS fields. The red circles are the measured ellipticity of stars from each coadded mosaic. The black circles are the residual ellipticities after subtracting the measured ellipticity of the PSF models from their respective stars (red circles). For all fields, the PSF model corrects for the average ellipticity (shifts the centroid of the distribution toward zero) and the spatial variation of the ellipticity (reduces the scatter). The residual e 1 and e 2 components are summarized in Table 5, and, on average, they leave residuals of ∣de 1∣ < 0.0005 ± 0.0003 and ∣de 2∣ < 0.0005 ± 0.0003, which is sufficient for our future weak-lensing study of massive overdensities.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Histogram of galaxy shape bias for the population of galaxies from the UDS field. The vertical red line shows the multiplicative shear bias (−0.025) calculated from averaged galaxy ellipticities for applied shears in the range of −0.05 to 0.05 (see Section 3.1.3 for details of the simulation). To demonstrate one method to mitigate the undersampling effect, we present a half-light radius cut of >0.″15 (blue hatched histogram). After the half-light radius cut (vertical green line), the multiplicative shear bias is reduced to 0.002.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Quadrupole-measured ellipticity (bottom panel) and size (top panel) of NGC 104 stars as a function of F160W AB magnitude. Blue circles are the median values in bins that are 1 mag wide with standard errors. The black line is a linear fit to the unbinned data. The data show that brighter stars are observed to be rounder (top panel) and brighter (bottom panel). Across the magnitude range, the ellipticity changes by ∼0.006, and the size changes by ∼2%.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Astrometric offset of stars in the Gaia catalog to stars in the mosaics from CANDELS Treasury (top panel) and our work (bottom panel). The stars have been corrected for proper motion. The CANDELS Treasury positions show a systematic offset that varies from ∼0.″1 in the center of the image to ∼0.″25 on the outskirts. This systematic variation has been corrected in our mosaic. On average, the astrometry of the UDS field is improved from 0.″13 to 0.″01.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Astrometric offset of stars in the Gaia catalog to stars in the mosaics from CANDELS Treasury (left panel) and our work (right panel). The CANDELS Treasury positions show a nearly constant offset from the Gaia positions by ∼0.″26. Our mosaic has removed the offset. On average, the astrometry of the GOODS-S field is improved from 0.″26 to 0.″02.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Comparison of galaxy colors in the optical (blue; F606W–F814W) and NIR (red; F125W–F160W). The median and standard deviation of the NIR and optical colors are 0.21 ± 0.36 and 0.33 ± 0.65, respectively. The lower variation of galaxy colors in the NIR is caused by less variation in galaxy SEDs in the bandpasses. This shows that the NIR PSF is less dependent on the SED of the galaxy than the optical PSF.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Temporal variation of the HST focus for observations in the CANDELS fields. The majority of observations are performed in the range of −5 to 5 μm. The temporal variation of the HST focus causes variations in the PSF that we account for in our PSF modeling (Section 4).