adsabs/AstroCLIMB huggingface dataset:
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Histograms of the α vir parameter by region in the Ridge, derived from 13CO (1–0) (Figure 14 shows the extent of the regions). Overplotted in black hatching is the α vir distribution of 30 Dor. The average α vir parameter is shown in the upper left corner of the panel for each region. A series of K-S tests indicate that the NE region (pink) has a different distribution than each of the other regions in the Ridge. The NE region tends toward lower values of α vir than the rest of the Ridge.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Line widths plotted against sizes of structures in the Ridge, colored by their region within the Ridge. We fit a power law with a fixed slope of a 1 = 0.5 to each region’s structures and find that the South and NE regions have the lowest intercepts, indicating low kinetic energy in these regions. The NC region has the highest intercept, indicating that it has the highest kinetic energy.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Values of α vir in the Ridge plotted against the structure’s distance to R136 (top), the nearest H II region (middle), and the nearest YSO (bottom). All three show similarly weak correlations based on Pearson’s correlation coefficients, shown in the upper left corner.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Illustration adapted from Smith et al. (2016) demonstrating how changing the location of an input illumination spot on a circular 200 μm core fiber (top row) results in different near-field (middle row) and far-field (bottom row) output patterns.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Wavelength-averaged mean differences between subsequent fiber-flat spectra for all MaNGA fibers as observed in a sequence of exposures with the telescope pointed at zenith and instrument rotated 20° between each exposure over the course of an hour. Each exposure pair is represented by a different color. Only the b1 channel is shown because the other spectrograph channels show similar behavior. The variations are again coherent across fiber blocks but appear somewhat stronger, 0.3%–0.5%, compared to the experiment with no instrument rotation, which exhibited 0.2%–0.3% variations (Figure 4). The larger deviations may result from changing angles between the fiber input and the flat-field beam as rotation sweeps the fibers around the focal plane.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Far-field intensity distributions for fibers associated with a 127 fiber MaNGA bundle, MA 176. The left panel shows far-field patterns stretched to reveal core structure. The first eight fibers (from the top right) are free-roaming single sky fibers, while the remainder are members of the bundle and as such are subject to varying stresses. The exact location of an underfilled illumination source also varied from fiber to fiber in these lab measurements and is responsible for some degree of output variation. The image on the right shows the standard deviation of the intensity variation across this sample, divided by the mean intensity profile. The innermost contour indicates that variations within the fiber cores across this set of fibers is about 9%.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Standard deviation of the difference spectrum between pairs of fiber flats observed during a simulated observing track. Each exposure pair is represented by a different color (although hard to distinguish since most points overlap) and only the b1 channel is shown since the other channels are similar. Despite the significant importance of flexure in this experiment, the 1σ scatter is nearly identical to what was observed when the instrument and telescope were stationary (Figure 5).
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Wavelength-averaged mean differences between subsequent fiber-flat spectra for all MaNGA fibers (numbered arbitrarily) as observed in a sequence of exposures with the telescope and instrument fixed. Each exposure pair is represented by a different color. The deviations are typically 0.2%–0.3%. Coherent behavior at the same fiber number locations may be caused by flexure variations of specific v-groove blocks along the pseudo-slit or subtle changes in the flat-field illumination pattern.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Wavelength-averaged mean fiber-flat differences across a simulated observing track with both telescope motion and instrument rotation. Each exposure pair is represented by a different color. Only the b1 channel is shown because the other spectrograph channels show similar behavior. Coherent block-to-block variations now reach 1%. Fiber motion and induced stresses are negligible because cabling in plugged cartridges limit fiber motion.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: The relative mean difference compared to the first exposure in the average fiber-flat spectra measured within each science IFU and plotted against their location in the focal plane. Four specific rotator angles from the “Telescope at Zenith, Instrument Rotated” experiment are shown. A degree of coherent spatial variations across the plate is apparent, suggesting that differences in the flat-field illumination and angular distribution pattern as seen by different IFUs plays a role.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Standard deviation of difference spectra between subsequent fiber flats as computed for all wavelength pixels within Δλ  c  for all MaNGA fibers in the “Instrument Fixed at Zenith” experiment. The typical 1σ scatter is 0.3%.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Fiber-flat spectra for FiberID #100 in both MaNGA spectrographs as observed in a series of five exposures taken over 1 hr with the telescope pointing at zenith and the instrument fixed. A boxcar smoothing of 50 pixels (∼55 Å) has been applied. The variation may be driven by flexure from subtle temperature changes or subtle changes in the output intensity of the calibration lamps.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: Overlay plots of the observed intensity ratios in the PDR Toolbox modeled grid of G 0 and n for p1, p3 (top and bottom panels include and exclude H2 data, respectively), and p7. The shaded region corresponds to the error on the observations. Each plot is overlaid with the contours of its corresponding corner plot.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: Overlay plots of the observed intensity ratios in the PDR Toolbox modeled grid of G 0 and n for the northern cloud, ridge, shell, and pillar. The shaded region corresponds to the error on the observations. Each plot is overlaid with the contours of its corresponding corner plot.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: The n and G 0 model phase space for [C II], [O I], 12CO, and FIR intensities. Left panel: modeled phase space with respect to [C II]/CO (3–2) vs. [C II]/FIR. Right panel: modeled phase space with respect to [C II]/[O I] vs. [O I] + [C II]/FIR. Data points are shown with colored (different regions) markers. The shaded regions correspond to the spread in the phase space as probed by the entire data set toward different regions as shown in Figure 7. The solid and dashed colored curves depict constant n and G 0 values, respectively.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: The n and G 0 model phase space for [C II], [O I], 12CO, and FIR intensities. Left panel: modeled phase space with respect to [C II]/CO (3–2) vs. [C II]/FIR. Right panel: modeled phase space with respect to [C II]/[O I] vs. [O I] + [C II]/FIR. Data points are shown in colored (different regions) markers. The shaded regions correspond to the spread in the phase space as probed by the entire data set toward different regions as shown in Figure 6. The solid and dashed colored curves depict constant n and G 0 values, respectively.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption:  p th vs. G 0 for different regions. The red, green, magenta, and dark-blue points correspond to regions studied by Young Owl et al. (2002; using FIR line analysis), Joblin et al. (2018; using high-J 12CO analysis), Pabst et al. (2022; using low-J 12CO and [C II] analysis), and this work, respectively. p3v1 and p3v2 correspond to the two velocity components of p3: −15 to 5 km s−1 and 5–20 km s−1, respectively. The black line refers to the fit by Wu et al. (2018) using mid- to high-J 12CO and [C I] analysis. The light-blue solid and dashed lines are for the analytic relation by Seo et al. (2019) and the relation divided by 3 to account for pressure equipartition, respectively.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: The n and G 0 model phase space for [C II], [O I], 12CO, and FIR intensities. Left panel: modeled phase space with respect to [C II]/CO (3–2) vs. [C II]/FIR. Right panel: modeled phase space with respect to [C II]/[O I] vs. [O I] + [C II]/FIR. Data points are shown with colored (different regions) markers. The solid and dashed colored curves depict constant n and G 0 values, respectively.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: Average IR spectra toward p1, p3, and p7 (regions shown in Figure 1). The six species presented in this work are marked with red dashed lines.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: [C II] modeled intensity map as a function of G 0 and n. The map is highlighted with the observed intensity contours, as well as marked with the model-predicted intensity values for different regions in different colors. The thickness of the contours corresponds to their observational error bars.
Paper: Destruction of Long-period Comets
Authors: David Jewitt
Figure caption: Nucleus radii independently estimated from the production rate (r 1, from Equation (5)) and the nongravitational acceleration (r 2, from Equation (7)). Yellow and red filled circles denote nuclei that survived and that were destroyed by the perihelion passage, respectively. The solid line shows r 1 = r 2. The dashed line indicates r 1 = (5/3) r 2.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: WASP-52b’s transit light curve centered on the helium triplet. Left panel: the red points show the light curve found by integrating the residual absorption in a 0.43 Å wide bin centered on the redder two lines of the He I triplet. The red line shows a fit to these data that is then resampled to a finer time resolution. The green points show the light curve in a bin width matching the FWHM of the narrowband filter used by Vissapragada et al. (2020). The green line shows a fit to these data. The orange line shows the transit light curve observed by Vissapragada et al. (2020) and the blue line shows the “continuum” optical light curve as measured by Alam et al. (2018). The red and blue vertical dashed lines indicate the first and fourth contact points of the transit models for the helium and continuum light curves, respectively. Right panel: the excess transit depth we observe with NIRSPEC as a function of the width of the bin that we integrate over. The orange square shows the 95th percentile upper limit on WASP-52b’s excess He I absorption measured by Vissapragada et al. (2020) in a 6.35 Å wide filter.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: WASP-52b’s transmission spectrum, centered on the helium triplet, whose location is shown by the vertical dashed gray lines. Top panel: transmission spectrum (in units of excess absorption) shown by the black data points. The red line shows the fit of the summation of two Gaussians to the transmission spectrum. The blue dashed lines show the contribution of the two components of this double Gaussian. This reveals a peak amplitude of 3.44% ± 0.31% (11σ) and no velocity shift (0.00 ± 1.19 km s−1). Bottom panel: residuals to the fit.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: WASP-177b’s transmission spectrum, centered on the helium triplet, which shows a peak at ﹩{1.28}_{-0.29}^{+0.30}﹩% that is redshifted by +6.02 ± 1.88 km s−1. However, given the systematics in the spectrum we do not interpret this as strong evidence for helium.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Velocity, in the stellar frame, of WASP-52b’s peak He I absorption during transit (red squares). The red error bars show the pixel size of NIRSPEC (0.11 Å, 3 km s−1) with the black error bars showing the resolution element (12 km s−1, R = 25,000). The green line shows the planet’s orbital motion given the parameters in Table 1. We note that the final spectrum at phase 0.020 is at low signal-to-noise and so do not take this as evidence for blueshifted material.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: WASP-177b’s transit light curve and the excess absorption we measure centered on the helium triplet, revealing no significant in-transit absorption. See Figure 9 for details.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Phase-resolved excess absorption centered on the helium triplet during WASP-52b’s transit. The wavelength is in the stellar rest frame. The horizontal white lines show the first and fourth contact points of WASP-52b’s optical transit (using the ephemeris of Mancini et al. 2017). The dashed white lines indicate the planet’s orbital motion.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Our bootstrapping analysis of WASP-52b’s He I absorption. The out–out (blue), in–out (orange), and in–in (green) distributions for WASP-52b in a 20 km s−1 wide bin centered on the helium triplet. For each distribution, the median, 16th, and 84th percentiles are given in the legend.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Phase-resolved excess absorption centered on the helium triplet during WASP-177b’s transit, indicating no absorption visible by eye. See Figure 4 for details.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Distributions resulting from our bootstrap analysis for WASP-177b. See Figure 11 for details.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: The GD 153 count rates for the WFC3-IR F105W filter are shown with black filled circles, while measurements from exposures collected with a number of samples (NSAMP) greater than six are marked with magenta filled circles. Error bars are also shown. The solid line indicates the mean of all measurements, while the dotted–dashed line indicates the mean of the NSAMP ≥ 6 measurements.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Same as Figure 3 but for data collected with the UVIS2-C512C-SUB (amp C; black) and UVIS2-C512D-SUB (amp D; red) subarrays.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Old (DE16; cyan) and new (CA21; red) EE corrections for UVIS1 (solid lines) and UVIS2 (dashed lines) as a function of wavelength. The EE model values from Hartig (2009a) are shown with a blue solid line, and the prelaunch values are shown with a black solid line.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: The EE fraction, flux(r)/flux(150), as a function of the aperture radius in pixels, r, for amp A (UVIS1; black) and amp C (UVIS2; red) for the F275W (top) and F814W (bottom) filters. Photometry was measured on the combined _drc images for the standard star GRW 70. See text for more details.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Same as Figure 1 but for data collected with the UVIS2-C512C-SUB (amp C; black) and UVIS2-C512D-SUB (amp D; red) subarrays.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Measured sensitivity change slopes for the wide- and medium-band filters for the UVIS1 detector (amp A) as a function of pivot wavelength. Note that for the three UV filters, the slope is the one calculated after MJD = 55,738 (see text and Table 4 for more details).
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Normalized standard deviation of WFC3-IR photometric measurements of GD 153 plotted versus the S/N. The solid line represents the expected normalized standard deviation (1/S/N).