adsabs/AstroCLIMB huggingface dataset:
Paper: Eclipse Timing the Milky Way’s Gravitational Potential
Authors: Sukanya Chakrabarti, Daniel J. Stevens, Jason Wright, Roman R. Rafikov, Philip Chang, Thomas Beatty, Daniel Huber
Figure caption: (a) Simulated HST WFC3 primary eclipse light curve of KIC 4144236 (blue points) and the best-fit transit model from batman (Kreidberg 2015; black curve). (b) Posterior distribution for the eclipse midpoint time T  c  from the transit modeling, demonstrating that a 0.1 s precision on T  c  is achievable with HST.
Paper: Analysis of a JWST NIRSpec Lab Time Series: Characterizing Systematics, Recovering Exoplanet Transit Spectroscopy, and Constraining a Noise Floor
Authors: Zafar Rustamkulov, David K. Sing, Rongrong Liu, Ashley Wang
Figure caption: The recovered transmission spectra of GJ 436 b (top) and TRAPPIST-1 d (bottom) recovered from the injected data using our novel pipeline. We include a cloudy TRAPPIST-1 d atmosphere model for an illustrative comparison.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Dust continuum emission at 257 GHz as observed by ALMA (color scale and contours). First contours (gray) and steps (black) are 8σ, corresponding to 3.35 mJy beam−1. The beam size is 0.″19 × 0.″13 (PA = +5°). The binary system is composed of VLA4A (right) and VLA4B (left). Coordinates are α J2000 = 03h 29m 3.ˢ75, δ J2000 = +31°16′03.″81 and α J2000 = 03h 29m 3.ˢ773, δ J2000 = +31°16′03.″81 for VLA4A and VLA4B, respectively. The blue arrows indicate the directions toward HH 11 (133°) as well as the main axis of the H2/CO jet (155°) as inferred by Lefèvre et al. (2017).
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Integrated emission from CH3OH, 13CH3OH, CH3CHO, NH2CHO, and CH3OCH3, in white contours, superposed to the dust emission in color scale. The emission is integrated in the following velocity intervals: 4–7.5 km s−1 in the left panels (V sys − ), 7.5–8.7 km s−1 in the middle panels (V sys), and 8.8–12.0 km s−1 in the right panels (V sys + ). The first contours and steps are 5σ, corresponding to 35 mJy beam−1, 19 mJy beam−1 and 29 mJy beam−1, for CH3OH; 34 mJy beam−1, 21 mJy beam−1 and 28 mJy beam−1 for 13CH3OH; 29 mJy beam−1, 19 mJy beam−1 and 26 mJy beam−1 for CH3CHO; 30 mJy beam−1, 18 mJy beam−1 and 29 mJy beam−1 for CH3OCH3; and 33 mJy beam−1, 24 mJy beam−1, and 27 mJy beam−1 for NH2CHO, respectively. The synthesized beams are reported in white in the lower-left corner of each panel. The dashed line indicates the axes connecting VLA4A and VLA4B along which the line intensity profiles shown in Figure 3 are extracted. On the right, we report the spectra in brightness temperature units, extracted at the continuum peak position of VLA4A (black star) and VLA4B (red star). From 13CH3OH spectra, we derived a systemic velocity of +7.7 km s−1 for VLA4A (black vertical dashed line) and +8.5 km s−1 for VLA4B (red vertical dashed line). Spectra are smoothed at 0.3 km s−1 resolution. On the left is reported the upper-level energy of each transition in K.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Left panel: normalized intensity profile of the NH2CHO line at 243.521 GHz (blue) and the CH3OCH3 line at 241.946 GHz (orange) extracted along the line connecting VLA4A with VLA4B. The green line shows the residuals obtained subtracting the formamide emission from the CH3OCH3 profile. The two vertical dashed lines show the position of VLA4A (black) and VLA4B (red). The offset in pixel is given with respect to the position of VLA4A. The pixel size corresponds to 25 mas. Right panel: residual line profiles of CH3OCH3 (green), CH3OH (orange), 13CH3OH (blue), and CH3CHO (magenta), after subtracting the formamide emission profile. The analyzed lines are the CH3OCH3 line at 241.964 GHz, the CH3OH line at 241.904 GHz, the 13CH3OH line at 255.204 GHz, the two detected CH3CHO lines at 242.106 GHz and 242.118 GHz, whose intensity is added, and the NH2CHO line at 243.521 GHz.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Moment 1 (intensity-weighted velocity peak) map of the lines 13CH3OH at 256.8265 GHz, CH3CHO at 242.1060 GHz, and NH2CHO at 255.058 GHz (see Table 1). The two stars indicate the VLA4A and VLA4B positions. The systemic velocities of the two protostars are indicated as horizontal lines in the wedge.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Integrated emission of all the detected lines of CH3OH, in color scale, superposed on the dust emission in white contours. The emission is integrated in the following velocity intervals: 4–7.5 km s−1 in the left panels (blue), 7.5–8.7 km s−1 in the middle panels (V sys), and 8.8–12.0 km s−1 in the right panels (red). The first contours are 10σ, corresponding to 4 mJy beam−1, and steps are 25σ, corresponding to 10.46 mJy beam−1. The synthesized beams are reported in white in the lower-right corner of each panel. On the left is reported the upper-level energy of each transition in Kelvin.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Integrated emission of all the detected lines of 13CH3OH, in color scale, superposed on the dust emission in white contours. The emission is integrated in the following velocity intervals: 4–7.5 km s−1 in the left panels (blue), 7.5–8.7 km s−1 in the middle panels (V sys), and 8.8–12.0 km s−1 in the right panels (red). The first contours are 10σ, corresponding to 4 mJy beam−1, and steps are 25σ, corresponding to 10.46 mJy beam−1. The synthesized beams are reported in white in the lower-right corner of each panel. On the left is reported the upper-level energy of each transition in Kelvin.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Integrated emission of all the detected lines of CH3CHO, in color scale, superposed on the dust emission in white contours. The emission is integrated in the following velocity intervals: 4–7.5 km s−1 in the left panels (blue), 7.5–8.7 km s−1 in the middle panels (V sys), and 8.8–12.0 km s−1 in the right panels (red). The first contours are 10σ, corresponding to 4 mJy beam−1, and steps are 25σ, corresponding to 10.46 mJy beam−1. The synthesized beams are reported in white in the lower-right corner of each panel. On the left is reported the upper-level energy of each transition in Kelvin.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Integrated emission of all the detected lines of CH3OCH3, in color scale, superposed on the dust emission in white contours. The emission is integrated in the following velocity intervals: 4–7.5 km s−1 in the left panels (blue), 7.5–8.7 km s−1 in the middle panels (V sys), and 8.8–12.0 km s−1 in the right panels (red). The first contours are 10σ, corresponding to 4 mJy beam−1, and steps are 25σ, corresponding to 10.46 mJy beam−1. The synthesized beams are reported in white in the lower-right corner of each panel. On the left is reported the upper-level energy of each transition in Kelvin. The panels showing only the continuum contours refer to line emission partially outside the observed spectral window (spw). Please note that each line is composed of four blended transitions very close in frequency (AE, EA, EE, AE). This structure, due to the rotation in the CH3OCH3 molecule of two functional groups CH3-, leads to some contamination in the channel maps. However, we would like to stress that this velocity blending does not affect the line spatial distribution.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Integrated emission of all the detected lines of NH2CHO, in color scale, superposed on the dust emission in white contours. The emission is integrated in the following velocity intervals: 4–7.5 km s−1 in the left panels (Blue), 7.5–8.7 km s−1 in the middle panels (V sys), and 8.8–12.0 km s−1 in the right panels (Red). The first contours are 10σ, corresponding to 4 mJy beam−1, and steps are 25σ, corresponding to 10.46 mJy beam−1. The synthesized beams are reported in white in the lower-right corner of each panel. On the left is reported the upper-level energy of each transition in Kelvin. The panel showing only the continuum contours refers to line emission partially outside the observed spectral window (spw).
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Synthetic LTE spectra generated with Weeds using the gas parameter in Table 2.
Paper: The Two Hot Corinos of the SVS13-A Protostellar Binary System: Counterposed Siblings
Authors: Eleonora Bianchi, Ana López-Sepulcre, Cecilia Ceccarelli, Claudio Codella, Linda Podio, Mathilde Bouvier, Joan Enrique-Romero
Figure caption: Optimized binding geometries and energies. The energetics include zero-point-energy corrections.
Paper: Solar Energetic Particles Produced during Two Fast Coronal Mass Ejections
Authors: Xiaolei Li, Yuming Wang, Jingnan Guo, Shaoyu Lyu
Figure caption: Observations of eight CMEs between 2021 October 28 and November 2. (a) Remote-sensing observations of eight CMEs and their associated flares. First row: SDO/AIA193 images of the flares (marked by the green dashed oval). Second row: preprocessed base-difference SOHO/LASCO C2 images of the CMEs. Third row: preprocessed base-difference STEREO-A/SECCHI COR2 images of the CMEs. (b) Positions of the Sun (big yellow dot), STEREO-A (red dot), Earth (green dot with its orbit shown as the dotted circle), and Mars (orange dot) on the ecliptic plane on 2021 October 29 00:00 UT. (c) The time–elongation plot for the STEREO-A COR2, HI1, and HI2 running-difference images along the position angle of 264° where Earth is located. The front of CMEs 4, 6, 7, and 8 and the trace of Earth (green curve) are marked. The corresponding CME’s flare-onset time (magenta dashed line) and CME-driven shock arrival time (orange dash line) are marked as well.
Paper: Solar Energetic Particles Produced during Two Fast Coronal Mass Ejections
Authors: Xiaolei Li, Yuming Wang, Jingnan Guo, Shaoyu Lyu
Figure caption: In situ observation near Earth. From top to bottom: X-ray flux observed by GOES-R XRS on board GOES-17, dynamic spectra of Waves radio data, magnetic field magnitude and components in GSE coordinates (X pointing toward the Sun, Y pointing to solar east, and Z normal to the ecliptic), solar wind velocity and proton number density, proton temperature and value of plasma beta, and solar energetic proton flux detected by the Wind spacecraft. The corresponding CME’s flare-onset time (magenta dash line) and CME-driven shock arrival time (orange dash line) are marked as well.
Paper: Solar Energetic Particles Produced during Two Fast Coronal Mass Ejections
Authors: Xiaolei Li, Yuming Wang, Jingnan Guo, Shaoyu Lyu
Figure caption: In situ observation by STEREO-A. From top to bottom: dynamic spectra of Waves radio data, magnetic field magnitude and components in RTN coordinates (R, T, and N pointing to radial, transverse and normal directions), solar wind velocity and proton number density (Beacon data, to be processed), and solar energetic proton flux detected by the STEREO-A spacecraft. The corresponding CME’s flare-onset time (magenta dashed line) and CME-driven shock arrival time (orange dashed line) are marked as well.
Paper: Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7
Authors: Nicola Borghi, Michele Moresco, Andrea Cimatti
Figure caption: Example of age–star formation timescale degeneracy for a LEGA-C galaxy (ID 217260, S/N ≃ 22 pix−1) comparing the baseline index set (left plot, gray boxes) to the Vazdekis et al. (2015) τ declining models. Left: observed (gray) and synthetic (blue and red) spectra normalized at 4200 Å. The blue spectrum corresponds to the model closer to the best-fit parameters, while the red one is taken at the edge of the 1σ confidence region. Right: corner plot for stellar age, star formation timescale τ, stellar metallicity [Z/H], and [α/Fe]. The contours enclose 1σ (darker shade) and 2σ (lighter shade) confidence regions. Blue and red symbols indicate the values at which the synthetic spectra are generated.
Paper: A Massive AGB Donor in Scutum X-1: Identification of the First Mira Variable in an X-Ray Binary
Authors: Kishalay De, Deepto Chakrabarty, Roberto Soria, Michael C. B. Ashley, Charlie Conroy, Matthew J. Hankins, Mansi M. Kasliwal, Ryan M. Lau, Anna M. Moore, Robert Simcoe, Jamie Soon, Tony Travouillon
Figure caption: PGIR J-band light curve of 2MASSJ1835. The black points denote the observed J-band photometry. The black solid line shows the best-fit semiparametric Gaussian process regression model (g(t); see text). The black dashed, dotted–dashed and dotted lines denote the contribution from the long-term trend component (l(t)), primary periodic component (q(t)), and high-frequency variability component (h(t)), respectively. The best-fit period and its uncertainty are shown. The red arrow shows the SpeX observation epoch.(The data used to create this figure are available.)
Paper: A Massive AGB Donor in Scutum X-1: Identification of the First Mira Variable in an X-Ray Binary
Authors: Kishalay De, Deepto Chakrabarty, Roberto Soria, Michael C. B. Ashley, Charlie Conroy, Matthew J. Hankins, Mansi M. Kasliwal, Ryan M. Lau, Anna M. Moore, Robert Simcoe, Jamie Soon, Tony Travouillon
Figure caption: Comparison of the infrared spectrum of 2MASSJ1835 to that of an RSG (of the favored spectral type in Kaplan et al. 2007) and a late-type Mira variable (inferred from our analysis) in the IRTF Spectral Library (Rayner et al. 2009). Prominent absorption features are marked, while regions of low atmospheric transmission are shown in gray. The comparison spectra have been artificially reddened with E(B − V) = 7.0 mag based on the estimate in Kaplan et al. (2007) (see also Section 3.3).(The data used to create this figure are available.)
Paper: A Massive AGB Donor in Scutum X-1: Identification of the First Mira Variable in an X-Ray Binary
Authors: Kishalay De, Deepto Chakrabarty, Roberto Soria, Michael C. B. Ashley, Charlie Conroy, Matthew J. Hankins, Mansi M. Kasliwal, Ryan M. Lau, Anna M. Moore, Robert Simcoe, Jamie Soon, Tony Travouillon
Figure caption: Comparison of the observed pulsation period and surface composition of the infrared counterpart of Sct X-1 (shown in the red shaded region) to evolutionary tracks of AGB stars at different initial masses for solar-metallicity composition (Z = 0.0152). We show tracks for three masses as indicated in the legend (along with the corresponding stellar ages), with lines connecting the model epochs in increasing age sequence during the thermally pulsing phase. The period for the dominant pulsation mode at each stage is shown (Trabucchi et al. 2019).
Paper: A Massive AGB Donor in Scutum X-1: Identification of the First Mira Variable in an X-Ray Binary
Authors: Kishalay De, Deepto Chakrabarty, Roberto Soria, Michael C. B. Ashley, Charlie Conroy, Matthew J. Hankins, Mansi M. Kasliwal, Ryan M. Lau, Anna M. Moore, Robert Simcoe, Jamie Soon, Tony Travouillon
Figure caption: Comparison of the J-band spectrum of 2MASSJ1835 to that of a similar late-type supergiant (MY Cep) and Mira variable (HD 69243) in the IRTF spectral library. The spectra have been normalized by fitting the steep continuum with a low-order polynomial.
Paper: Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7
Authors: Nicola Borghi, Michele Moresco, Andrea Cimatti
Figure caption: Theoretical age–redshift relations for the high-σ ⋆ subsample of cosmic chronometers. Each panel shows the effect of varying each parameter to the labeled values. Red diamonds are median binned data for the high-σ ⋆ subsample of cosmic chronometers from Borghi et al. (2022). For illustrative purposes, we also show the data points of the lower σ ⋆ subsample (blue diamonds), which are about 0.5 Gyr younger, on average. When not varied, the parameters are set to the following fiducial values: t form = 3.9 Gyr, H 0 = 70 km s−1 Mpc−1, Ω m,0 = 0.3, ΩΛ,0 = 0.7, w 0 = −1, and w  a  = 0.
Paper: Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7
Authors: Nicola Borghi, Michele Moresco, Andrea Cimatti
Figure caption: Upper panel: median binned age–redshift relation for 140 passive galaxies analyzed in Borghi et al. (2022) (gray points) divided into higher (red) and lower (blue) σ ⋆ regimes. Lower panel: H(z) measurement (violet star) with statistical (inner error bar) and total (outer error bar) uncertainties. Black points are literature data from: Simon et al. (2005) (•), Stern et al. (2010) (♦), Moresco et al. (2012) (▾), Zhang et al. (2014) (▴), Moresco (2015) (◀), Moresco et al. (2016) (▶), and Ratsimbazafy et al. (2017) (■). Gray lines are theoretical relations for a standard ΛCDM (dashed) and Einstein–de Sitter (dotted) cosmology.
Paper: Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7
Authors: Nicola Borghi, Michele Moresco, Andrea Cimatti
Figure caption: Same as Figure 1, but showing the results obtained with linear fits to the unbinned age–z relations for different combinations of indices used in the analysis (as presented in Borghi et al. 2022). Gray lines are theoretical relations for a standard ΛCDM (dashed) and Einstein–de Sitter (dotted) cosmology and are shown for visual inspection purposes only. We note that the EdS model predicts a much flatter slope compared to the ones of the data, which are instead more compatible with a ΛCDM scenario, as also confirmed the H(z) measurements.
Paper: Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7
Authors: Nicola Borghi, Michele Moresco, Andrea Cimatti
Figure caption: Constraints from age–redshift relations assuming a flat ΛCDM model. Left: corner plot for H 0, Ω m,0, t form, showing 1σ (darker shade) and 2σ (lighter shade) regions. Vertical shaded bands are the cumulative 1σ confidence regions. Our results are compared with those from Riess et al. (2021) and (Planck Collaboration 2020, TT,TE,EE+lowE+lensing). Right: resulting fits (gray lines) to the observed age–redshift relations (diamonds).
Paper: Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7
Authors: Nicola Borghi, Michele Moresco, Andrea Cimatti
Figure caption: Differences as a function of redshift between stellar ages and metallicities [Z/H] of 140 LEGA-C passive galaxies obtained with Vazdekis et al. (2015) single-burst (SSP, upper panels) and exponentially declining (τ-decl., lower panels) star formation histories vs. Thomas et al. (2011) SSP models. Violet lines and shaded regions are robust linear fits and associated 2σ scatter regions, respectively.
Paper: Anomalous Flux in the Cosmic Optical Background Detected with New Horizons Observations
Authors: Tod R. Lauer, Marc Postman, John R. Spencer, Harold A. Weaver, S. Alan Stern, G. Randall Gladstone, Richard P. Binzel, Daniel T. Britt, Marc W. Buie, Bonnie J. Buratti, Andrew F. Cheng, W. M. Grundy, Mihaly Horányi, J. J. Kavelaars, Ivan R. Linscott, Carey M. Lisse, William B. McKinnon, Ralph L. McNutt, Jeffrey M. Moore, J. I. Núñez, Catherine B. Olkin, Joel W. Parker, Simon B. Porter, Dennis C. Reuter, Stuart J. Robbins, Paul M. Schenk, Mark R. Showalter, Kelsi N. Singer, Anne. J. Verbiscer, and Leslie A. Young
Figure caption: An average of the first four images in the present data set. The area is ﹩17\buildrel{\,\prime}\over{.} 4\times 17\buildrel{\,\prime}\over{.} 4.﹩ The display range is 50 DN (linear stretch starting at −5 DN). The faintest stars visible are at V = 19.1. The top of the field is at PA 139.°6.
Paper: Anomalous Flux in the Cosmic Optical Background Detected with New Horizons Observations
Authors: Tod R. Lauer, Marc Postman, John R. Spencer, Harold A. Weaver, S. Alan Stern, G. Randall Gladstone, Richard P. Binzel, Daniel T. Britt, Marc W. Buie, Bonnie J. Buratti, Andrew F. Cheng, W. M. Grundy, Mihaly Horányi, J. J. Kavelaars, Ivan R. Linscott, Carey M. Lisse, William B. McKinnon, Ralph L. McNutt, Jeffrey M. Moore, J. I. Núñez, Catherine B. Olkin, Joel W. Parker, Simon B. Porter, Dennis C. Reuter, Stuart J. Robbins, Paul M. Schenk, Mark R. Showalter, Kelsi N. Singer, Anne. J. Verbiscer, and Leslie A. Young
Figure caption: The total sky levels for the present (TF01 = Test Field 1) and seven NH21 fields are plotted as a function of the total known flux components present. A line with unit slope going through the point representing the present field is shown. This demonstrates that the total sky level in the present field decreased by the amount expected as compared to the NH21 fields, given its reduced foreground flux components.
Paper: Anomalous Flux in the Cosmic Optical Background Detected with New Horizons Observations
Authors: Tod R. Lauer, Marc Postman, John R. Spencer, Harold A. Weaver, S. Alan Stern, G. Randall Gladstone, Richard P. Binzel, Daniel T. Britt, Marc W. Buie, Bonnie J. Buratti, Andrew F. Cheng, W. M. Grundy, Mihaly Horányi, J. J. Kavelaars, Ivan R. Linscott, Carey M. Lisse, William B. McKinnon, Ralph L. McNutt, Jeffrey M. Moore, J. I. Núñez, Catherine B. Olkin, Joel W. Parker, Simon B. Porter, Dennis C. Reuter, Stuart J. Robbins, Paul M. Schenk, Mark R. Showalter, Kelsi N. Singer, Anne. J. Verbiscer, and Leslie A. Young
Figure caption: A stacked bar chart showing the amplitudes of the known sky components for the present field (leftmost bar) as compared to the seven NH21 fields. The black horizontal lines with error bars show our measured total sky values and their uncertainties for each field. The small flux from bright galaxies masked out in the LORRI field is not included in this figure.
Paper: Anomalous Flux in the Cosmic Optical Background Detected with New Horizons Observations
Authors: Tod R. Lauer, Marc Postman, John R. Spencer, Harold A. Weaver, S. Alan Stern, G. Randall Gladstone, Richard P. Binzel, Daniel T. Britt, Marc W. Buie, Bonnie J. Buratti, Andrew F. Cheng, W. M. Grundy, Mihaly Horányi, J. J. Kavelaars, Ivan R. Linscott, Carey M. Lisse, William B. McKinnon, Ralph L. McNutt, Jeffrey M. Moore, J. I. Núñez, Catherine B. Olkin, Joel W. Parker, Simon B. Porter, Dennis C. Reuter, Stuart J. Robbins, Paul M. Schenk, Mark R. Showalter, Kelsi N. Singer, Anne. J. Verbiscer, and Leslie A. Young
Figure caption: A bar chart showing the amplitudes of the anomalous sky components for the present field (blue) as compared to the seven NH21 fields.